Sixth Catalog of Orbits of Visual Binary Stars: Notes


                                                                                                                             
00000-1930   LTT 9831    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
00002+0146   WEI  45     HWE 64 is certainly identical with Weisse 45 = ADS 17156. Howe misread          
                         the sign of the declination. This was already stated in Cin. Pub v 6,           
                         nos 748 and 749, and the mean of the two measures is given in the mean          
                         results, assigned to Weisse 45. Nevertheless the pair was given                 
                         separately in the BDS and 12692 and taken over as ADS 17168. ADS 17156          
                         is misidentified. It is BD+00 5079 (9.1), 9.5, G0, with the position            
                         for 1900 (1950) as 23 55.1 (57.6) +01 13 (30).                          B__1950c
00003+1642   HJ  318     A component is PPM 116047. In Tycho catalog magnitude of A is 9.46; in          
                         Guide Star Catalogue B is GSC 1178 1031 with magnitude 12.77. Spectral          
                         types are K for A component, G5-K0 for B component. Annual proper               
                         motion for B: AR= -0.013" and DEC=-0.0005"                              FMR1999c
00006-5238   FIN 294     Spectrum: K1/2III+A/F.                                                          
00008+0630   GWP   2     XMI 101.                                                                Tob2012b
00011+6935   STTA253     B is BD+68 1417.                                                                
00011-2326   LDS2070     B is CD-24 17944.                                                               
00012-0005   TOK 359     Long-period SB.                                                         Tok2013b
00012-0312   LDS9082     Old LDS6082.                                                                    
00013+6021   STTA254     A is the semiregular variable WZ Cas.                                           
00013+0742   DU    4     HJL 325.                                                                HJL1986 
00013-7012   GLI 290     B is CPD-70 3035.                                                               
00014+3937   HLD  60     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.67 +/- 0.29, 1.79, and 1.65 Msun, respectively.             Mlk2012 
00016+6437   MLR  79     Misidentified by Muller as BD +63 2093.                                         
00016+3714   ES 2444     Aka ALI 472.                                                                    
00018-0322   LDS9083     Old LDS6083.                                                                    
00018-2548   B   630     Measures uncertain, too close.                                                  
                         G266-029. Not resolved in our images                                    Oso2004 
                         HIP 146. See Allen et al. (2000) for information on metallicity,        AlC2000 
                         age, galactic orbital parameters, etc.                                          
00019-0952   LDS5157     NLTT 58812/58813                                                        Chm2004 
00020+4530   J   864     BRT 1164.                                                                       
                         -22s and +2.4' from BD+44 4541.                                         J__1955 
                         AC: CPM pair.                                                           J__1955 
00022+5958   BU 1337     STI 1256.                                                                       
00022+2705   BU  733     85 Peg. Spectral types and masses of primary and secondary assigned by          
                         ten Brummelaar et al., based on adaptive optics observations.           TtB2000 
                         AB: Additional notes may be found in Baize (1945).                      Baz1945b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.49 +/- 0.81, 1.58, and 1.56 Msun, respectively.  Mlk2012 
                         Soderhjelm notes poor Hipparcos solution.                               Sod1999 
                         A third star has been detected by infrared speckle interferometry.      Mcy1983 
                         HIP 171. See Allen et al. (2000) for information on metallicity,        AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AC and AD: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         AC and AD: Additional notes may be found in Burnham (1894).             Bu_1894 
                         AD: Rectilinear solution by Friedman et al. (2011).                     USN2011a
00023+1609   BPM   1     [PM2000]    1692 + [PM2000]    1685.                                    Gvr2010 
00023+0732   LDS9084     Old LDS6084.                                                                    
00023-2943   B   631     zet Scl. The companion is very faint and not accurately measured. A             
                         is a spectroscopic binary.                                                      
00024+1429   GWP   4     XMI 102.                                                                Tob2012b
00024+1047   BGH   1     AB,C: HJL 326.                                                          HJL1986 
                         AB,C: SHY 377. Bayesian analysis by Shaya & Olling (2011) indicates     Shy2011 
                         very high (near 100%) probability pair is physical.                             
00025-0826   LDS5255     NLTT 2/3                                                                Chm2004 
00026+6606   STF3053     B is BD+65@1988.                                                                
00026+1841   SHY 378     AB: HIP    201 + HIP    206.                                                    
00028+1647   BPM   2     [PM2000]    2010 + [PM2000]    1993.                                    Gvr2010 
00028+0208   HJ  998     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: Rectilinear solution by Friedman et al. (2012).                     USN2012a
00031+0816   STF3054     B component is eclipsing binary of Algol-type, period 2.2604 d.         Zas2012 
00032+4508   HJ 1927     Unless the separation has decreased greatly, the measures given in the          
                         ADS would seme to refer to the nearby pair ADS 108.                     B__1963b
00032+3315   ES 2400     Pair long unconfirmed due to 1m error in published epoch-1900                   
                         coordinates (thanks to Rafael Caballero, private communication)                 
00034+1839   GWP   6     XMI 103.                                                                Tob2012b
00034-2430   LDS2076     NLTT 53/54                                                              Chm2004 
00037+1851   GWP   7     XMI 104.                                                                Tob2012b
00037+1134   BPM   3     [PM2000]    2710 + [PM2000]    2680.                                    Gvr2010 
00037-2824   CRZ   1     BDK   1. G 266-33 + 2MASS J00034227-2822410. Distance 39.5 +1.8/-1.6            
                         pc for primary, 26 +/- 3 pc for secondary. Estimated age of system              
                         0.9-1.4 Gyr. Mass of secondary estimated at 0.100-0.103 Msun.           Fah2010 
00038-1317   XMI   1     Rectilinear solution by Hurowitz et al. (2013).                         USN2013a
00042+6217   H 5  79     9 Cas.                                                                          
00042-1008   LDS3116     NLTT 86/84                                                              Chm2004 
00044+5804   OSO   1     G217-030. No common proper motion pairs, based on comparison with               
                         POSS2 red plates                                                        Oso2004 
00045+0045   GWP  10     XMI 106.                                                                Tob2012b
00045+1851   GWP   9     XMI 105.                                                                Tob2012b
00046+4206   CHR 122     B is a spectroscopic binary. Hence the system is quadruple.                     
00046-4044   GKI   2     Ba,Bb. GJ 1001BC = LHS 102BC. Spectral types L4.5 and L4.5              Red2006b
00046-7745   LDS 832     Aka TVB  18.                                                                    
00047+3416   STF3056     AB is an orbit pair, and D is an unresolved spectroscopic pair (P=68d)  Tok2019b
                         so this is a 2+2 hierarchical multiple. C is optical.                           
00049+5832   STF3057     Called a two-spectrum SB in the Bright Star Catalog Supplement.                 
                         H 1  39.                                                                MEv2010 
00049-1320   GAL 295     Object #1 in Gallo's original list.                                     Gal1912a
00050+0835   GWP  11     XMI 107.                                                                Tob2012b
00051+6323   HJ 1933     STI 1265.                                                                       
00052+4514   ES 9001     Previously known as ES 1293a.                                                   
             BU 9001     Previously known as BU  997a.                                                   
00053-0542   33 Psc      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Harper (1926).                                                          Hrp1926 
00054+1620   STTA255     B is BD+15@4934.                                                                
00054-2559   LDS3119     NLTT 158/159                                                            Chm2004 
00055+3406   HU 1201     A possible close approach about 1980.                                           
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.09 +/- 0.63, 2.52, and 1.10 Msun, respectively.  Mlk2012 
00056-0141   LDS3012     NLTT 176/175                                                            Chm2004 
00057+4549   STT 547     Premature orbits have been computed. Motion direct.                             
                         Both A and B have variable RV (ranges 45 and 25 km/s, respectively).            
                         Another star (9.9, 330") has common proper motion.                              
                         AB: Bolometric corrections and component masses determined from                 
                         M-L relation. A family of possible orbits were determined by Kiyaeva    Kiy2001 
                         (2001) for the F component relative to AB pair (Note: only the                  
                         shortest-period solution is presented in orbit catalog.)                        
                         AB: NLTT 172/173                                                        Chm2004 
                         AD and AE: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         AF: HIP    473 + HIP    428.                                                    
                         AC and AD: Rectilinear solution by Pavlovic et al. (2013).              Pal2013 
00057+4549   POP 217     AP: Rectilinear solution by Cvetkovic (2011).                           Cve2011d
00057+0626   BFR   1     NLTT 182 + 2MASS J00054171+0626300. Baron et al. (2015) estimate                
                         spectral types M4.5 +/- 0.5 and L0 +/- 1, distances 62 +38/-23 and              
                         69 +5/-22 pc, masses 0.157-0.181 and 0.079-0.085 Msun.                  BFr2015 
00059+1805   STF3060     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         Aka J  3330.                                                                    
             HD    108   Hutchings (1975 ApJ 200, 122) presented a preliminary orbit with a              
                         period of 4.6d, but subsequent  work has cast doubt on the reality of           
                         the orbit (Underhill 1994 ApJ 420, 869).                                Msn1998a
             LEP   1     AD: HJL1001.                                                            HJL1986 
                         AD: SHY 112. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AD: the visual binary at 573" is co-moving, same parallax. The D                
                         component is ~1.3m below the main sequence in the (K, V-K) color-               
                         magnitude diagram.                                                      Tok2012a
00063+5826   STF3062     One component, designated V640                                                  
                         Cas, is variable, probably due to partial eclipses. P = 1.08 d.                 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Secondary is SB, P=47.685d                                              Tok2014d
00063-4905   HDO 180     A is a spectroscopic binary.                                                    
                         Primary is planet host star, P=339d. B comp is LHS 1021. Pair bound.            
                         Photometry suggests companion K8.5-M1.5 with mass 0.59 +/- 0.02 Msun.   Egn2007 
00064+4501   UC  320     Aka BVD 170.                                                            Skf2013 
00066+2901   STT 549     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             ENG   1     A,CD: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
             LAF   1     CHARA Array Limb-darkened diameter of A :                               CIA2013c
                         R =  0.9172 +/- 0.0090 \rsun, L =   0.6078 +/-0.0090 \lsun,                     
                         Teff = 5327 +/-  39 K, M = 0.889 \msun, Age = 9.6 Gyr.                          
             BU 1338     CD: J 866.                                                                      
00066+1554   GWP  12     XMI 108.                                                                Tob2012b
                         Aka GRV1158 with quadrant flip.                                                 
00067-0706   JNN  11     Estimated age 1000-10000 Myr; masses 0.35 +/- 0.09 and 0.21 +/- 0.05            
                         Msun; a ~5.6 au.                                                        Jnn2014 
00068-2106   RSS  41     CPD-21@1                                                                        
00068-0853   BUG  15     Burgasser et al. (2012) determine that the pair comprised of LP 704-48          
                         and SDSS J000649.16-085246.3 share cpm, at a projected separation of            
                         820 +/- 120 au, based on a derived distance 30 +/- 3pc. Spectral type           
                         of the primary is M7. From near-IR spectroscopy they determine the              
                         secondary is SB, orbital period 147.6 +/- 1.5d, e = 0.10 +/- 0.07;              
                         spectral types of Ba and Bb are M8.5 +/- 0.5 and T5 +/- 1. Estimated            
                         ages of A and B are >8 and >3-4 Gyr; masses 0.092 Msun for A,                   
                         0.082-0.083 and 0.049-0.064 Msun for the M8.5 and T5 stars.             Bug2012 
                         NLTT 251 + 2MASS J00064916-0852457. Baron et al. (2015) estimate                
                         spectral types M6.0 +/- 0.5 and M9.0 +/- 0.5, distances 25 +7/-11 and           
                         37 +5/-11 pc, masses 0.102-0.133 and 0.079-0.085 Msun.                  BFr2015 
00070+0303   GWP  14     XMI 109.                                                                Tob2012b
00071+6309   MLR 105     No significant movement since first resolution.                         Drd2009 
00073+2058   HDS  12     Rectilinear solution by Hartkopf & Mason (2013).                        Hrt2013b
00074-2936   LDS2088     NLTT 296/295                                                            Chm2004 
00076+4009   STF3064     Taken to be the same as H 4  69 (= H IV 69). With error of 1deg in              
                         declination it would be the same as STF 3064 rej.                               
                         BDS 8.                                                                          
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2013).                         USN2013a
00076-2718   LDS2089     NLTT 307/308                                                            Chm2004 
00077+6022   JNN 247     G 217-32. Estimated age 35-300 Myr; masses 0.17 +/- 0.07 and 0.12 +/-           
                         0.06 Msun; a ~9.8 au.                                                   Jnn2014 
00078+5723   HJ 3241     HJ 1935.                                                                        
00079+0317   J   301     BAL 1606.                                                                       
00079-2727   LDS   5     Also known as CHM   1. WDS designation in error, apparently due to              
                         confusion between CD-28 11 and CPD-28 11.                                       
00079-3005   LDS2092     NLTT 319/320                                                            Chm2004 
00080+3123   STTA256     B is BD+30@3.                                                                   
00081+3240   HJ  610     SEI   2.                                                                Nsn2017a
00082+6217   HJ 1936     Optical pair, since relative motion reflects the proper motion of               
                         component A relative to B to high accuracy.                             Kiy2012 
00082+5933   STI   8     AB: 00083+5934SMA   3                                                           
00082+0937   LDS9085     Old LDS6085.                                                                    
00083+1329   GWP  17     XMI 110.                                                                Tob2012b
00084+2905   H 5  32     21 And = alp And = Alpheratz                                                    
                         AB: H V 32. STFB 15. A is spectroscopic binary, P = 96.7d.                      
                         AB: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
             MKT  11     Aa,Ab: Separations and magnitude differences derived by model fitting           
                         to calibrated squared visibilities, using measurements with the Mark            
                         III interferometer. Spectroscopic and photometric data are combined             
                         with astrometry from the Mark III interferometer to derive orbital              
                         elements for the SB1 by Pan et al.                                      MkT1992a
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Pan et al. (1992).                                                      MkT1992a
                         Aa,Ab: Orbit determined by fitting revised Hipparcos intermediate               
                         astrometric data. Derived component masses are 4.05 +/- 0.50 and                
                         1.71 +/- 0.20 Msun.                                                     Ren2010 
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 5.19 +/- 0.18, 4.10, and 3.09 Msun, respectively.  Mlk2012 
                         Aa,Ab: Docobo et al. (2014) use the spectroscopic elements of Pourbaix          
                         (2000), together with speckle data and the Hipparcos parallax, to       Pbx2000b
                         derive the remaining orbital elements. The resulting masses are                 
                         3.84 +/- 0.29 and 1.63 +/- 0.26 Msun.                                   Doc2014h
00085+3456   HDS  17     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.78 +/- 0.89, 2.67, and 1.10 Msun, respectively.             Mlk2012 
                         A(B) Teff = 6100+/-50(5940+/-50) K, R = 1.93+/-0.20(1.83+/-0.20) \rsun, AlW2014b
                         L = 4.63+/-0.80(3.74+/-0.70) \lsun, M = 1.35(1.25) \msun.                       
                         Sp = F8.5IV(G0IV).                                                              
00085-7134   HLN  18     Also known as TDS1309.                                                          
00085-0419   GWP  19     AB and BC were originally listed as the triple 00086-0418; now are              
                         merged with GWP 18 at the correct WDS designation.                              
00087+5006   ES  443     Identical to ES 744.                                                            
00088+8647   NLTT 324    Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by Latham             
                         et al. (2002). They derived component masses 1.06 and 0.59 Msun and an  Lat2002 
                         estimated semimajor axis of 7.00 mas.                                   Ren2013 
00088+0801   HDO   2     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Friedman et al. (2012).                         USN2012a
00089+3257   SEI   1     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
00089+2050   BEU   1     GJ 3010. Estimated age 30-300 Myr; masses 0.20 +/- 0.09 and 0.11 +/-            
                         0.06 Msun; a ~2.0 au.                                                   Jnn2014 
00090+2738   GIC   1     AB = G130-046/G130-045.                                                         
00090-5400   HDO 181     Spectroscopic binary.                                                           
                         Quoted errors in P and a are +116/-40y, +0".20/-0".06, respectively.    Ary2002b
00092+5909   AGC  15     bet Cas = 11 Cas = Caph                                                         
                         The primary is a Delta Scuti-type variable.                                     
                         Spectroscopic binary, P = 27 d.                                                 
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         NPOI Limb-darkened diameter 2.103 +/- 0.015 mas, Sp = F2III,            NOI2018 
                         R = 3.79 +/- 0.04 \rsun, Teff = 6739 +/- 88 K, L = 26.8 +/- 1.4 \lsun,          
                         M = 2.02 +/- 0.03 \msun, Age = 1.00 +/- 0.05 Gyr.                               
00092-3035   LDS2093     NLTT 410/401                                                            Chm2004 
00093+7943   STF   2     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.97 +/- 2.24, 3.22, and 2.02 Msun, respectively.             Mlk2012 
00093+5324   FYM   4     The EF pair reported by Fay (2013) is not seen in Aladin; probably an   FyM2013d
                         erroneous identification of their CG pair.                                      
             BVD  11     CD: Originally listed as separate pair (00096+5325), aka FYM 4CD.               
00093+2517   GIC   2     LDS 859 = G130-048/G130-047.                                                    
                         HIP 754. See Allen et al. (2000) for information on metallicity,        AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         A companion is a close astrometric binary.                              HIP1997d
                         AB: Primary is SB2, P=463.250d                                          Tok2014d
                         Spectroscopic orbit P=463.44d and radial velocity of B consistent       Grf2015b
                         with physicality.                                                               
00094+6357   BUP   1     V641 Cas, a VV Cep-type system.                                                 
00094+4819   LDS3128     NLTT 412/405                                                            Chm2004 
00094+1415   CHE   1     Due to poor published coordinates, identification with the coordinates          
                         in the WDS is uncertain. Chevalier's measure does not agree well with   Che1910 
                         others for this pair.                                                   Hrt2012b
00094-2759   BU  391     kap 1 Scl                                                                       
00096+3826   PTT   1     This appears to be the same as ALI 473. PTT position 00 10.0 +38 23.            
00096+0148   GWP  22     XMI 113.                                                                Tob2012b
00096+1047   GWP  21     XMI 112.                                                                Tob2012b
00096+1052   GWP  20     XMI 111.                                                                Tob2012b
00097+3107   GIC   3     G130-050/G130-049.                                                              
                         NLTT 433/431                                                            Chm2004 
00100+4623   STF   3     A small star in field: 1831.33 133.0@ 4.57"; Possibly an illusion.      Bu_1906 
                         H 2  83.                                                                MEv2010 
                         Primary is V342 And, an Algol-type eclipsing binary, P = 2.63934d.      Zas2012 
00100+1109   STF   5     34 Psc.                                                                         
00101+5847   STI1287     SMA.                                                                            
                         Daley (Dal2002c) finds a large B-V for the secondary of 1.52.                   
00101+3825   HDS  23     Da,Db: Cvetkovic et al. (2014) derive spectral types K3 and  K4,                
                         masses 0.79 and 0.72 Msun. Dynamical parallax is 11.42 +/- 0.70 mas.    Cve2014 
00103+7231   HJ 1941     See note to 00138+7233BUP   2.                                                  
00104+5831   BU  253     Ba,Bb: Rectilinear solution by Rica & Zirm (2012).                      FMR2012i
00104+4952   ES 2576     B is BD+49@17.                                                                  
00105+1716   ALP   1     2MASSI J0010325+171549                                                          
                         Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
00106-7313   I    43     There is a long gap (1931-1977) in the observations.                            
00107+5453   WOR  37     SX Cas, an eclipsing and spectroscopic binary, P = 36.6d.                       
                         Spectral types A6shell and K3III.                                               
00108+5846   BU  485     Ca,Cb: Rectilinear solution by Rica & Zirm (2012).                      FMR2012i
00108-5729   HJ 3350     Primary is BL Phe, a Beta Lyr type eclipsing binary, P = 0.81035d.      Zas2012 
00109+4807   LEP   2     NI    1.                                                                        
00109+1705   GWP  24     XMI 114.                                                                Tob2012b
00110+0058   SKF1821     Initial WDS designation (00110+0913) garbled - dec portion copied from          
                         SKF1820.                                                                        
00111+5755   HJ 1003     STI 1291.                                                                       
00112+4933   ES 2577     B is BD+48@28.                                                                  
00113+1435   LDS1072     NLTT 521/522                                                            Chm2004 
00113+0625   GWP  27     XMI 115.                                                                Tob2012b
00113-2045   LDS   1     G266-060. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 525/526                                                            Chm2004 
00114+5850   SKW   1     Aa,Ab. Primary of the Herbig Ae/Be pair LkHa 198. A family of possible  SKW2005 
                         orbits are calculated, based on various choices for initial parameters          
                         (luminosities, component masses, etc.). Neither a" nor T0 was                   
                         provided. a" was calculated from other published parameters and T0 was          
                         determined by trial and error with comparison to their Figure 3.                
00116-0305   STF   8     H 2  55.                                                                MEv2010 
00116-2748   LDS2099     kap 2 Scl                                                                       
00117+0323   FMR  29     aka UC  332.                                                                    
00121+5337   BU 1026     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 6.13 +/- 1.26, 3.41, and 3.01 Msun, respectively.  Mlk2012 
             CHR   1     AC: Rapid motion, particularly in separation.                                   
00121+3327   GII  13     Aka ITF  31.                                                                    
00122+4647   A   802     Not seen 1950-1976. Possibly a whole revolution.                                
00125+1434   LN Peg      Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
00126+2143   LDS 861     NLTT 589/592                                                            Chm2004 
00126+1118   BPM   4     [PM2000]    8713 + [PM2000]    8668.                                    Gvr2010 
00130+0257   A  2001     Apparent motion in a highly-inclined orbit.                                     
00132+1511   BUP   3     gam Peg = 88 Peg = Algenib                                                      
                         Beta CMa variable and spectroscopic binary.                                     
00132+0536   PLQ   3     Possibly same star as HDO   5 (Doolittle).                                      
00132-1711   HJ 1944     B is BD-17@16.                                                                  
00133+6919   KUI   1     AB: Nechville 6.                                                                
             JNN 248     BC: GJ 11 B. Estimated age 1000-10000 Myr; masses 0.38 +/- 0.10 and             
                         0.26 +/- 0.06 Msun; a ~17.2 au.                                         Jnn2014 
00134+3859   BRT2196     ALI 718, J 2709.                                                                
00134+3801   ES 2445     ALI 474.                                                                        
00134+2659   STT   2     Hipparcos parallax of 0".00808 yields a mass sum of 1.9 Msun,                   
                         slightly underestimated for a double star of spectral type F8V.                 
                         Dynamic parallax is 0".0053, considerably different from the                    
                         measured one.                                                           Sca2000b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.36 +/- 1.29, 4.23, and 1.10 Msun, respectively.  Mlk2012 
                         Star C (mag. 10.37, 18") is physical, according to Le Beau.             LBu1990c
00135-0009   HJ  618     BAL 641 = LDS   4.                                                              
00136+1356   LDS1073     LDS6086 = LDS9086.                                                              
00137+7702   MLR 283     Aka TDS1350.                                                                    
00137+4934   STF   9     B is BD+48@42.                                                                  
00137+1537   BPM   5     [PM2000]    9457 + [PM2000]    9535.                                    Gvr2010 
00138+7233   BUP   2     Misinterpretation of a note in Bu_1913 resulted in these three BUP              
                         components being associated with 00103+7231HJ 1941, when all three              
                         were actually measured relative to a planetary nebula (NGC 40) about            
                         3m following the HJ pair. Since one BUP component was also the primary          
                         of the MLR 282 triple system, the BUP component designations were               
                         changed to become part of the MLR multiple. The planetary nebula is             
                         now the D component in this system.                                             
00138+3612   BU 1341     AC: This is a measure of A and BD+35@27.                                        
00138+0812   TOK 360     Likely triple system.                                                   Tok2013b
                         Primary is unresolved Hipparcos acceleration solution (G-code) binary.  Tok2014d
00138-7442   HJ 3353     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2013).                         USN2013a
00139+6323   BU 1309     AB: The star is 63@703-62@1909 in Vat. Astrog. Cat. (Van Biesbroeck).   VBs1954 
                         AD: D is 63@656-62@1910.                                                        
00139+1518   LDS1074     NLTT 667/666                                                            Chm2004 
00139-0429   LDS9087     Old LDS6087.                                                                    
00140+2837   BRT 117     MLB 554.                                                                        
00140-1815   BFR   2     NLTT 687 + 2MASS J00135882-1816462. Baron et al. (2015) estimate                
                         spectral types M3.0 +/- 0.5 and L1.0 +/- 0.5, distances 42 +26/-16 and          
                         83 +7/-27 pc, masses 0.389-0.412 and 0.072-0.078 Msun.                  BFr2015 
00141+7601   STTA  1     B is BD+75@5.                                                                   
00141+3957   ES 2544     ALI 1008.                                                                       
00142-0712   MSH   1     Meshkat et al (2015) resolved a faint companion to HD 984. They derive          
                         a system age in the range 30-200 Myr. Teff for the primary is 6315 +/-          
                         89K; temperature for the secondary is 2777 +127/-130K or 2900 +/- 200K,         
                         depending on adopted scale and synthetic spectra. Spectral types are            
                         F7V and M6.0 +/- 0.5. Primary mass is 1.20 +/- 0.06 Msun; secondary             
                         mass estimates range from 74 - 90 Mjup, depending on adopted models.    Msh2015 
00143-0535   OSO   2     G031-036. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates                                                        Oso2004 
00144+3609   LDS3140     NLTT 703/704                                                            Chm2004 
00144+1643   BPM   6     [PM2000]    9941 + [PM2000]    9955.                                    Gvr2010 
00144-1424   GAL 296     Object #7 in Gallo's original list.                                     Gal1912a
00145-0747   BU  486     Irregular variable, AD Cet.                                                     
00148-2859   RSS   1     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
00150+0849   STF  12     35 Psc. A is an Algol-type system, UU Psc, P = 0.84d. Also known as             
                         CHE   2.                                                                        
                         HJL   2.                                                                HJL1986 
                         H 3  62.                                                                MEv2010 
00150-7251   BRG   1     The AstraLux PSF was strongly asymmetric for this target, hence in              
                         addition to the usual PSF fitting, we also performed a customized               
                         aperture photometry scheme in order to ensure that the PSF fitting did          
                         not provide a biased result (see paper for details). We adopt the               
                         aperture photometry values for the differential photometry, and let             
                         the errors be represented by the scatter between PSF fitting results            
                         and the aperture photometry. Note that the photometry values presented  Brg2010 
                         here should replace those in Bergfors et al. (2010).                    Jnn2012 
00152+5947   FYM 153     Purported AJ pair removed on request of author.                         FyM2014b
00152+3642   LDS3144     pa error = 359 deg.                                                     RAO2020b
00152+2722   J   868     Rectilinear solution by Rica (2014).                                    FMR2014f
                         Due to the very different parallax in Gaia DR2 for the two components   Cve2019b
                         the orbital solution of Novakovic (2007) is no longer plausible and the Nov2007b
                         linear solution is preferred. The orbit solution is retained in ORB6.           
00152+2717   KUI   2     A is a spectroscopic binary.                                                    
00152+2722   J   868     Despite having an orbit, this pair determined to be optical.            FMR2014d
00152+2454   GIC   4     G130-059/G130-060.                                                              
00153+5304   GIC   5     G217-041/G217-040.                                                              
                         NLTT 739/738                                                            Chm2004 
00153+4412   A  1256     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 6.79 +/- 3.58, 5.77, and 2.82 Msun, respectively.  Mlk2012 
                         Primary is the Algol-type eclipsing binary V348 And.                    Zas2009 
                         The A component is a close 27.7-d eclipsing pair, so the pair is at     Zas2019b
                         least triple. Based on proper motion C and D are likely optical.                
00153+1630   BPM   7     [PM2000]   10539 + [PM2000]   10566.                                    Gvr2010 
00153+0936   GWP  30     XMI 116.                                                                Tob2012b
00153-4006   WG    2     B is CPD-40@14.                                                                 
00154-1134   GAL 297     00153-1133SLE 251. Object #9 in Gallo's original list.                  Gal1912a
00155-1608   HEI 299     L722-22. Astrometric binary now resolved.                                       
                         Too poor astrometric orbit (Innes 1998) and too few resolved            Inn1988 
                         observations (cf. Heintz 1990) to give definite orbit. Present          Hei1990a
                         solution at least preferable to `X' HIP solution.                               
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 0.17 +/- 0.02, 0.39, and 0.50 Msun, respectively.             Mlk2012 
00157+3516   ALP   2     2MASSW J0015447+351603                                                          
                         Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
00159-0853   SHY 381     HIP   1266 + HIP    118.                                                        
00160+0415   NLS   1     Nielsen et al. (2012) discovered two low-mass companions to the young           
                         A0V star HD 1160. The B component is thought to be a brown dwarf,               
                         mass 33 +12/-9 Mjup. The C component is of spectral type M3.5 +/- 0.5,          
                         with estimated mass 0.22 +0.03/-0.04 Msun. The age of the system is             
                         roughly 50 +50/-40 Myr.                                                 Nls2012 
00161+0902   GWP  32     XMI 117.                                                                Tob2012b
00162+7657   STF  13     A premature orbit has been calculated.                                          
00162+1903   J   217     Measures scattered.                                                             
                         Additional notes may be found in Couteau (1952) and                     Cou1952a
                         Van Biesbroeck (1954).                                                  VBs1954 
00162-7951   GJ 3021     Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from the Geneva           
                         Extrasolar Planet Search Programs home page.                            HaI2001 
             CVN  14     Companion is a probable mid-M dwarf.                                    Cvn2006 
                         Spectral type of B component M4V +/- 1.                                 Cvn2007 
                         A second candidate companion at 39" is noted in UCAC2 as having much            
                         different proper motion, so has been ruled out as a companion. The              
                         measured proper motion of the companion between the two SofI observing          
                         epochs is (+368 +/- 68 mas, -48 +/- 68 mas). IR spectroscopy suggests           
                         a spectral type of M4-M5V for the B component.                          Mug2007b
                         Co-moving with HIP 107705 at 3.5pc.                                     Shy2011 
00164+5722   TDS1375     Aa,Ab: formerly 00165+5722, WDS designation changed when merged with            
                         HJ 1011 into triple                                                             
00164+1950   LDS 863     AB: NLTT 803/804                                                        Chm2004 
00165-2805   LDS2107     NLTT 834/835                                                            Chm2004 
00167+3910   ES 1936     ALI 719.                                                                        
00167+3638   STF  19     STT   3.                                                                        
00167+3629   STT   4     Hipparcos parallax of 0".01115 yields a mass sum of 2.75 Msun                   
                         with an uncertainty of 38% overestimated for a double star of                   
                         spectral type G0. Dynamic parallax is 0".0108, agreeing well with               
                         the measured parallax.                                                  Sca2000b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.72 +/- 0.59, 2.35, and 1.05 Msun, respectively.             Mlk2012 
00169-5239   GC 333      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Bopp et al. (1970).                                                     Evn1970 
00171+3841   CHR 123     theta And = 24 And                                                              
00171-1205   CBL 202     GWP  34.                                                                Tob2012b
00171-1406   GAL 298     Object #12 in Gallo's original list.                                    Gal1912a
00172-1921   LDS   9     B is BD-20@34.                                                                  
00174+0853   A  1803     Too close 1932, 1946-47, 1965-72. Modern measures show a close                  
                         approach about 1985. While both 18- and 36-year period orbits                   
                         have been calculated for this pair, Griffin (Docobo, private                    
                         communication) determined spectroscopically that the shorter-period             
                         high-eccentricity orbit is the correct one.                                     
                         The measure reported for 1976.622 is spurious and has been deleted              
                         from the catalogs.                                                      McA1982b
                         Large and irregular residuals preclude the correction of an orbit.      Tok1985 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 0.02 +/- 0.02, 1.48, and 1.13 Msun, respectively.  Mlk2012 
             STF  22     AB,C: H 2  50.                                                          MEv2010 
00174+0221   STF  21     HJL   3.                                                                HJL1986 
00176+1300   HJ    3     HJL   4.                                                                HJL1986 
00176-1113   GAL 299     Object #13 in Gallo's original list.                                    Gal1912a
00177+5126   TRN   8     AO Cas.  Classification is from the UV tomographic analysis of          Bgn1991 
                         Bagnuolo & Gies (1991).                                                 Msn1998a
                         The image rotator was in an unknown state, so two possible theta                
                         values are listed for the 2001.7341 observation - one for zenith up             
                         and one for north up.                                                   Trn2008 
00178+1620   TOK 646     Primary is 39 Psc. B is likely physical, as it moves in the same                
                         direction as A in DSS2 image.                                           Tok2014d
00180+2057   LDS 864     NLTT 912/910                                                            Chm2004 
00180+0931   AG    1     HJL   5.                                                                HJL1986 
00182+7257   A   803     Quadrant uncertain.                                                     Wor1967b
00182+1209   GWP  38     XMI 118.                                                                Tob2012b
00183+1646   BPM   8     [PM2000]   12613 + [PM2000]   12602.                                    Gvr2010 
00184+4401   GRB  34     AB: Proper motion of A +2892 +412. Proper motion of B +2863 +336.               
                         Premature orbits have been calculated. RV of star A possibly variable.          
                         A component is eruptive variable GX And and B component is the                  
                         eruptive variable GQ And and a SB.                                              
                         AB: NLTT 919/923                                                        Chm2004 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         PTI Limb-darkened diameter = 1.014 +/- 0.05 mas,                        PTI2001 
                         R = 0.389 +/- 0.021 \rsun.                                                      
                         VLTI Limb-darkened diameter  1.000 +/- 0.05 mas,                        LTI2003a
                         M = 0.414 +/- 0.021 \msun, R = 0.383 +/- 0.02  \rsun,                           
                         T = 3698 +/-  95 K.                                                             
                         CHARA Array Limb-darkened diameter of A : 0.988 +/- 0.016 mas           CIA2006 
                         R = 0.379 +/- 0.006 \rsun, Teff = 3730 +/-  49 K.                               
                         CHARA Array Limb-darkened diameter of A :                               CIA2012f
                         R =  0.3874 +/- 0.0023 \rsun, L =  0.02173 +/-0.00021 \lsun,                    
                         Teff = 3563 +/-  11 K, M = 0.423 \msun.                                         
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
00184+0344   HDO  12     AB: Appears to be same pair as HDO 13.                                          
00185-2757   HJ 1949     B is CD-28@75.                                                                  
00187+4347   STT   5     26 And.                                                                         
00188+5923   HJ 1012     STI 1320.                                                                       
00188-1217   GAL  15     Incorrectly entered in WDS as GAL   5.                                          
00188-1258   GIC   6     G158-057/G158-054.                                                              
00189+5923   HJ 1013     STI 1322.                                                                       
00189-1135   GAL  16     Originally entered with incorrect RA, so also known as                          
                         10187-1239GAL 422                                                               
00190+4301   ES 1483     J 1359.                                                                         
00192+5942   KR    4     A is an irregular variable, V377 Cas.                                           
00192+4330   ES 1484     BRT 67. Djurkovic calls this ES 1484BC.                                 Dju1954c
00192+0827   GWP  39     XMI 119.                                                                Tob2012b
00194-0849   HJ 1953     iot Cet = 8 Cet.  Variable?                                                     
                         NPOI Limb-darkened diameter  3.310 +/- 0.062 mas, Sp = K1III,           NOI2018 
                         R = 29.95+/- 0.725\rsun, Teff = 4645 +/- 73 K, L =376.8 +/-22.0 \lsun,          
                         M = 3.70 +/- 0.10 \msun, Age = 0.23 +/- 0.03 Gyr.                               
00196-2808   LDS  12     Proper motion -275 -1292.                                                       
00197+6046   LDS9088     Old LDS6088.                                                                    
00197+1951   GWP  40     XMI 120.                                                                Tob2012b
                         2MASS J00193931+1951050 and J00194303+1951117 are separated by only             
                         53", have very similar proper motions (e.g. Roser et al. 2010) and      XXX2010 
                         have similar estimated spectroscopic distances (23 and 21 pc,                   
                         respectively) in Riaz et al. (2006), hence it is highly likely that     Ria2006 
                         they form a physical pair.                                              Jnn2012 
00197+0624   ZUC   5     Primary is white dwarf PG 0017+061 = PHL 790.                           Zuc1992 
00199+2633   CHE   4     Chevalier's measure was correct, but his published (dx,dy) predict      Che1908 
                         different (rho,theta) than published. This was apparently due to a              
                         typographic error in dy, which was printed as -0'.0317 rather than              
                         -0'.0617. There is also an apparent trigonometric error in his value            
                         for position angle. Chevalier gives a value for theta of 154.62 deg,            
                         but all later measures in the WDS give values of about 204.0 deg. It            
                         appears his value should be 360-154.62 = 205.38 deg instead.            Hrt2012b
00200+3814   S   384     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: H 5  85.                                                            MEv2010 
00201+4244   OSO   3     G171-050. AB is not a common proper motion pair, based on astrometry            
                         and color.                                                              Oso2004 
             LDS3151     AC: NLTT 1038/1036                                                      Chm2004 
00203-3246   B  1025     Considerable motion, but no measures for more than 30 years.                    
00204+1757   OSO   4     G032-012. Not a common proper motion pair.                              Oso2004 
00206-2356   WSP  20     Planet-host star found to be close visual binary. Evans et al. (2016)           
                         find that the transiting hot Jupiter is probably orbiting the primary,          
                         and derive the following properties:                                            
                         A:      M = 1.089 +/- 0.047 Msun, R = 1.142 +/- 0.085 Rsun                      
                         planet: M = 0.378 +/- 0.022 Mjup, R = 1.28  +/- 0.15  Rjup              EvD2016 
00206+1219   BU 1015     Hipparcos parallax of 0".00883 yields a mass sum of 2.87 Msun                   
                         with an uncertainty of 75% slightly in excess for a binary of                   
                         spectral type F5. The great uncertainty concerning the sum of                   
                         masses is largely due to the consistent error in the measured                   
                         parallax. The dynamical parallax is 0".0085, agreeing well with                 
                         the observed parallax.                                                  Sca2000b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.44 +/- 1.04, 2.58, and 1.20 Msun, respectively.             Mlk2012 
00207+3159   CCA   1     WSP   1. WASP-1.  Duplicity discovered based on low-amplitude radial            
                         velocity variation. Spectral analysis plus transit light curves yields          
                         an orbital period of 2.520d. Given a spectral type for the primary of           
                         F7V, the planet has mass 0.80-0.98 +/- 0.11 Mjup and radius 1.33-2.53           
                         Rjup. Mass of the parent star is 1.06-1.39 Msun.                        CCA2007 
00207+0738   GWP  41     AB: XMI 121AB.                                                          Tob2012b
             GWP  42     AC: XMI 121AC.                                                          Tob2012b
00208+2737   CHE   7     MLB 674.  Also known as ROE 116.                                                
00210+6740   HJ 1018     STF 18.                                                                 Mlr1955c
00210+2647   CHE   9     Chevalier's measure was correct, but his published (dx,dy) predict      Che1908 
                         different (rho,theta) than published. This was apparently due to a              
                         typographic error in dx, which should be +0'.0708. Chevalier applied            
                         his declination offset from the plate center in the wrong direction,            
                         leading to an error of over 25' in the coordinates. The image for the           
                         pair at the corrected coordinates is elongated on the Aladin image;             
                         due to uncertain relative proper motion it's impossible to tell                 
                         whether his rho and theta values are correct.                           Hrt2012b
00210-3219   BRT1578     A likely plate flaw.                                                    Grv2021b
00210-7429   OGL   1     SMC139.6.72    + SMC139.6.636                                           Pli2012 
00211+6443   TDS  13     According to Milburn this pair was originally "found by Aitken          Mlb1925 
                         (private letter) in looking for MLB 244". This note went unnoticed      A__1925D
                         until long after the Tycho designation had come into usage, however;            
                         although the historical measures have been added the original TDS               
                         designation has been retained.                                                  
00212-4246   KO    1     A = LEHPM 494 (spec M6.0 +/0 1.0 V), B = DENIS-P J0021.0-4244 (spec             
                         M9.5 +/- 0.5 V). Data sources: UK Schmidt blue survey (1977.6), ESO             
                         Schmidt red (1984.8), DENIS I (1996.60), UK Schmidt red (1996.61), UK           
                         Schmidt near-IR (1999.6), 2MASS (1999.7). Mean separation (1974-1999)           
                         1.296 +/- 0.012 arcmin. The pair moved 5".7 over 22 years, 80 times             
                         the uncertainty in mean rho; concludes is CPM pair.                     Cab2007a
                         Additional 2003 measure from Spitzer Space Telescope.                   Cab2007b
00214+6700   STT   6     Orbit is very eccentric and very inclined. Scardia's geometrical                
                         elements do not differ much from those of Van Biesbroeck and Muller,            
                         but the orbit is more eccentric and has twice the period. An Hipparcos          
                         parallax of 0".00491 yields a mass sum of 6.6 Msun, overestimated for           
                         a binary system of spectral type B8.5V. The dynamical parallax is               
                         0".0054, in reasonable agreement with the measured one.                 Sca2000b
00214+2744   CHE  10     MLB 675.                                                                        
00214-7355   OGL   2     SMC138.6.56    + SMC138.6.104                                           Pli2012 
00215-6744   HJ 3361     CD-68@10.                                                                       
00215-7407   OGL   3     SMC138.8.18    + SMC138.6.78                                            Pli2012 
00216-7442   OGL   4     SMC139.8.20    + SMC139.8.81                                            Pli2012 
00217+1301   BPM   9     [PM2000]   14913 + [PM2000]   14833.                                    Gvr2010 
00218+6628   STT   7     CD: Previously listed incorrectly as AB,E, with quadrants flipped to            
                         275 deg.                                                                        
00219+1706   BPM  10     [PM2000]   15011 + [PM2000]   15046.                                    Gvr2010 
00219-2300   HJ 1957     Designated as HJ 3429 in BDS.                                           Bu_1906 
00220+4913   BWL   3     AC and AD: Colors and/or astrometry are inconsistent with a late-type           
                         common proper motion companion based on visual inspection of the field          
                         from 2MASS, SDSS, DSS1, and/or DSS2. Primary is GJ 3030.                Bwl2015 
00220+4231   RAS  16     Poorly-studied silicon star with weak magnetic field.                   Ras2014 
00221+4822   J  9001     Was a measure of a new pair designated as J  2384.                              
00222-7439   OGL   5     SMC139.7.1570  + SMC139.7.1569                                          Pli2012 
00224+1329   STF  27     42 Psc.                                                                         
00224+0640   FR    2     V Psc.                                                                          
00225+4456   A   648     Measure very doubtful. Not seen double on two later nights.             B__1963b
00226+5033   KU   67     B is BD+49@62.                                                                  
00226-3111   LDS  14     NLTT 1165/1164                                                          Chm2004 
00229+6214   ES  115     Primary is V745 Cas, a W UMa type eclipsing binary, P = 1.41057d.       Zas2012 
00229+5420   ES   42     ES 154.                                                                         
00229-1213   BUP   6     9 Cet.                                                                          
00230+6112   STI  43     HJ 1023.                                                                        
00234+2624   CHE  17     AC: Chevalier's measure was correct, but his published (dx,dy) predict  Che1908 
                         different (rho,theta) than published. This was apparently due to a              
                         typographic error in dy, which should be -0'.2783.                      Hrt2012b
00234-0121   HJ 1961     J 1433.                                                                         
00235-0343   LDS3160     AB: NLTT 1213/1214                                                      Chm2004 
00236+0947   KUI   3     LDS3162                                                                         
00239+2930   STF  28     B is BD+28@55. The variable, double-lined spectroscopic binary                  
                         BD+28@54 may belong to the system. This was previously reported as              
                         BD+28@49, but was corrected by Weis{2002, "F.G.W. Struve's              StF2002 
                         Double Stars (STF2000.0)"}                                                      
                         SHY 383. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
00240+3835   BUP   7     A is a Mira-type variable, R And.                                               
00240-0329   BU  488     Due to poor published coordinates, Chevalier's measure of this pair     Che1910 
                         was originally added to the WDS as a new discovery: 00245-0327 CHE 23   Hrt2012b
00240-7300   OGL   6     SMC136.8.38    + SMC136.8.178                                           Pli2012 
00241-7300   OGL   7     SMC136.8.41    + SMC136.8.408                                           Pli2012 
00242+1505   GWP  44     XMI 122.                                                                Tob2012b
00242-1305   VOU  83     Also single in 1958. Star confused with HU 4 (00246).                   VBs9999 
00242-7349   OGL   8     SMC138.6.4018  + SMC138.6.246                                           Pli2012 
00243+5201   HU  506     Aka V746 Cas.                                                                   
                         A premature orbit has been computed.                                            
                         Single 1934, 1953. A is SB, P = 28d:.                                           
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Additional notes may be found in van den Bos (1963).                    B__1963b
                         Also provide a solution to the usresolved ~25d companion.               Hmn2018 
00244+1322   BPM  11     [PM2000]   16681 + [PM2000]   16731.                                    Gvr2010 
00245-1217   GIC   7     LDS 3163 = G158-073/G158-074.                                                   
                         NLTT 1262/1265                                                          Chm2004 
00247-2653   LEI   1     Paper includes orbit of BC pair and estimate of mass sum.               Lei2001a
                         HST WFPC2 photometry was also transformed to standard Johnson B and V           
                         and Cousins R and I filters, yielding the following magnitudes for the          
                         A, B, and C components:                                                 Lei2000 
                            ------ A -----  ------ B -----  ------ C -----  filt                         
                            17.17 +/- 0.05  20.57 +/- 0.07  21.48 +/- 0.11   B                           
                            15.35     0.04  18.68     0.06  19.07     0.07   V                           
                            13.63     0.04  16.30     0.05  16.65     0.05   R                           
                            11.66     0.04  14.01     0.05  14.43     0.05   I                           
                         Seifahrt et al. (2008) determine mass sum of BC pair to be 0.157 +/-    Sef2008 
                         0.009 Msun; mass of A 0.115 +/- 0.010 Msun. They find no sign of the            
                         fourth component reported by Henry et al. (1999).                       Hen1999 
                         Rajpurohit et al. (2012) derive Teff, log g, radius, luminosity, and    Raj2012 
                         spectral type for the components of LHS 1070 using various models.              
                         Mean values (assuming distance = 8.8pc) are:                                    
                                 Teff (K)   log g   radius (Rsun)   log(L/Lsun)   spec                   
                             A:    2950      5.3       0.136           -2.92      M5.5                   
                             B:    2400      5.5       0.102           -3.44      M9.5                   
                             C:    2300      5.5       0.099           -3.55      L0                     
                         Koehler et al. (2012) derive masses for the A, B, and C components of           
                         0.172+/-0.010, 0.077+/-0.005, and 0.071+/-0.004 Msun, respectively.     Koh2012 
                         VLTI Limb-darkened diameter  1.149 +/- 0.11 mas,                        LTI2003a
                         M = 0.631 +/- 0.031 \msun, R = 0.702 +/- 0.063 \rsun,                           
                         T = 3520 +/- 170 K.                                                             
00247-5359   HJ 3364     B is CPD-54@89.                                                                 
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Friedman et al. (2012).                         USN2012a
00247-7240   OGL   9     SMC136.6.12    + SMC136.6.115                                           Pli2012 
00248+1925   BRT2296     J 2586.                                                                         
00249+1355   GWP  45     XMI 123. SLW  18.                                                       Tob2012b
00250+2726   CHE  24     There was a 1' error in Chevalier's determination of declination.       Che1908 
                         In addition, there was a trigonometric error in deriving theta; the             
                         correct value is 180deg - theta.                                        Hrt2012b
00250+0600   GWP  46     XMI 124.                                                                Tob2012b
00250-7244   OGL  10     SMC136.7.2977  + SMC136.7.2975                                          Pli2012 
00251+4803   CRZ   2     BDK   2. G 171-58 + 2MASS J00250365+4759191. Distance 42.2 +2.0/-1.8            
                         pc for primary, 31 +/- 6 pc for secondary. Estimated ages of                    
                         components are discrepant: 1.8-3.5 Gyr for primary, versus 0.1-0.5 Gyr          
                         for secondary. The primary is a spectroscopic binary resolved by        Hip1997a
                         Hipparcos, the secondary a close (~10au) L4+L4 pair, resolved by Reid   Red2006b
                         (2006).                                                                 Fah2010 
             HDS  56     Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 1.30 +/- 0.21, 1.85, and 1.10 Msun, respectively.  Mlk2012 
             RED  14     Ba,Bb: 2MASS J00250365+4759191. Spectral types L4 and L4                Red2006b
00251+1824   HJ  621     Rectilinear solution by Cvetkovic (2011).                               Cve2011c
00251-3646   BRG   2     Like BRG 1, this stellar binary also had an asymmetric PSF, and we              
                         therefore calculated the photometry in the same way as for that case.           
                         Note that the photometry values presented here should replace those in  Brg2010 
                         Bergfors et al. (2010).                                                 Jnn2012 
00251-7432   OGL  11     SMC139.2.27    + SMC139.3.744                                           Pli2012 
00253+3230   STF  29     SEI   4.                                                                Nsn2017a
00253-7446   OGL  12     SMC139.1.28    + SMC139.1.120                                           Pli2012 
00254+2036   A  2301     J 219.                                                                          
00254+0156   STT   8     44 Psc                                                                          
00254-7404   OGL  13     SMC138.2.19    + SMC138.7.4092                                          Pli2012 
00255-7334   OGL  14     SMC135.8.3096  + SMC135.8.3687                                          Pli2012 
00256+1536   LDS9089     Old LDS6089.                                                                    
00256-1849   HJ 1964     SEE 8.                                                                          
00257-5050   HJ 3365     B is CD-51@102.                                                                 
00259-0748   RIA   1     LHS 1074.                                                                       
00260+0027   GRV 974     Aka SLW  21.                                                                    
00260-0542   LDS3168     NLTT 1360/1359                                                          Chm2004 
00261-1037   GIC   8     LDS5273 = G158-077/G158-078.                                                    
                         NLTT 1370/1374                                                          Chm2004 
00261-7057   OGL  15     SMC137.5.17    + SMC137.5.19                                            Pli2012 
00262-4217   alp Phe     Alden's astrometric solution uses values of P, T, e adopted from the    Ald1938a
                         spectroscopic orbit (Lunt 1924).                                        Lun1924b
00263-4218   CRU9004     alp Phe = Ankaa.                                                                
00266-1924   ARA 515     Aka ITF  33.                                                                    
00267-7220   OGL  16     SMC140.1.3576  + SMC140.1.3730                                          Pli2012 
00268+0722   DOO  23     Doolittle calls this HDO 21, BDS 210. However, this seems to be a       Doo1915b
                         different pair.                                                                 
00268-3220   LDS2121     LDS5274                                                                         
                         NLTT 1416/1412                                                          Chm2004 
00269-0531   SCJ   1     B is BD-06@72.                                                                  
00269-7123   OGL  17     SMC137.8.790   + SMC137.8.846   + SMC137.8.1090                         Pli2012 
00269-8308   I   177     Spectrum of B is F.                                                             
00270+1705   BFR   3     HD 2292 + 2MASS J00265989+1704463. Baron et al. (2015) estimate                 
                         spectral types G5 and M9 +/- 1, distances 42 +28/-14 and 65 +4/-20 pc,          
                         masses 1.05 -1.12 and 0.108-0.118 Msun.                                 BFr2015 
00270-7237   OGL  18     SMC136.3.1     + SMC136.6.2735                                          Pli2012 
00271-0628   LDS3169     NLTT 1426/1425                                                          Chm2004 
00272+4959   STF  30     B is BD+49@89.                                                                  
00274+3054   HDS  62     Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Griffin (1979).                                                         Grf1979c
00274+0124   GWP  51     XMI 125.                                                                Tob2012b
00276+5120   COU2252     Transcription error resulted in 10' error in WDS designation.                   
                         00274+5130TDS1470                                                               
00276+1616   GWP  52     XMI 126.                                                                Tob2012b
00276-3157   I   438     BC: Rectilinear solution by Friedman et al. (2011).                     USN2011a
00276-7221   OGL  19     SMC140.1.4858  + SMC140.1.4878                                          Pli2012 
00277+0936   GIC   9     G001-005/G032-021.                                                              
00277-1625   YR    1     Ma,Mb = 1.362 +/- 0.033, 1.073 +/- 0.024 \msun.                         GmJ2022 
00277-7228   OGL  20     SMC136.4.4     + SMC136.4.17    + SMC136.4.36                           Pli2012 
00277-7300   OGL  21     SMC136.1.16    + SMC136.1.168                                           Pli2012 
00278+1803   BPM  12     [PM2000]   18879 + [PM2000]   18873.                                    Gvr2010 
00278-7251   OGL  22     SMC136.2.4     + SMC136.2.19    + SMC136.2.207                          Pli2012 
00279+2220   FRV   1     LP 345-25. Assuming a parallactic distance of 13.19 +/- 0.28 pc                 
                         (Gatewood & Coban 2009), Konopacky et al. (2010) derive a system mass   Gat2009 
                         of 0.121 +/- 0.009 Msun.                                                Kon2010 
                         Dupuy et al. (2010) determine system mass 0.120 +0.008/-0.007 Msun;             
                         spectral types are  M7.5 +/- 1.0  and M8.0 +1.5/-1.0.                   LiM2010 
00280-2654   LDS2123     DEA  22.                                                                        
00281-0001   HJ 1970     Designated as HJ 1972 in BDS.                                           Bu_1906 
00281-2512   B     5     AC = LDS2124                                                                    
00281-7329   OGL  23     SMC135.1.4464  + SMC138.3.12                                            Pli2012 
00282-1030   GAL 300     Object #18 in Gallo's original list.                                    Gal1912a
00283+6344   HU 1007     A premature orbit has been calculated. Motion direct.                   B__1963b
00283+1131   BPM  13     [PM2000]   19197 + [PM2000]   19238.                                    Gvr2010 
00283-7339   OGL  24     SMC138.4.5573  + SMC138.4.5757                                          Pli2012 
00283-7427   OGL  25     SMC139.3.2443  + SMC139.3.2445                                          Pli2012 
00284-2020   B  1909     Difficult visual system, with two components remaining within 0".2              
                         of each other throughout the orbit.                                             
                         Two orbit solutions (van den Bos 1956, Soedehjelm 1999). High-          B__1956b
                         eccentricity, half-period solution fits equally well but gives          Sod1999 
                         too high mass-sum (with no third component allowed by q).                       
                         1982.7657 autocorrelogram remeasured; new results listed in catalog.    McA1987b
                         Martin et al. (1998) derive component masses 1.563 +/- 0.177 and                
                         1.238 +/- 0.151 Msun.                                                   Mig1998 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.14 +/- 0.32, 2.15, and 1.05 Msun, respectively.             Mlk2012 
00287+5801   MLB 107     WDS changed from 00293+5800, BC pair merged with STI1355                        
00287+1502   ALP   3     2MASSI J0028394+150141                                                          
                         Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
00288+5756   OSO   5     G217-052. No common proper motion pairs, based on comparison with               
                         POSS2 red plates.                                                       Oso2004 
00288+0251   HJ  623     C component is galaxy NGC 125.                                                  
00289+5023   DAE   1     GJ 3036 = G172-001                                                              
                         Daemgen et al. derive a distance of 17.4 +/- 4.5 pc, a separation of    Dae2007 
                         7.4 +/- 2.2 au, and a predicted orbital period of 40 +19/-18 yr.                
                         Spectral types are M4.0 +/- 0.5 and M4.5 +/- 0.5; masses are 0.24               
                         +0.11/-0.07 and 0.19 +0.07/-0.05 Msub.                                          
00289+1835   BPM  14     [PM2000]   19589 + [PM2000]   19539.                                    Gvr2010 
00290-0933   GIC  10     G158-086/G158-087.                                                              
                         NLTT 1529/1530                                                          Chm2004 
00291+5752   MLB  39     STI 1359.                                                                       
00291-0742   MLR   2     Speckle measures show rapid motion.                                             
00292+7646   HJ 1967     Aka PKO  19.                                                                    
00293-0555   SHY 384     AB: HIP   2292 + HIP   2350.                                                    
             RAO   1     BC: Exoplanet host star. Roberts et al. (2015) estimate the spectral            
                         types of B and C as G8V and M1V.                                        Rbr2015a
                         BC: The B component is of type G5V, with mass 0.87 +/- 0.03 Msun.               
                         Based on isochrone fitting, Wittrock et al. (2016) estimate the mass            
                         of the C component at 0.48 +/- 0.03 Msun, and type likely an M dwarf.   Wtt2016 
00293-7244   OGL  26     SMC136.2.2867  + SMC136.2.2890                                          Pli2012 
00295+1413   BPM  15     [PM2000]   20020 + [PM2000]   19943.                                    Gvr2010 
00296-2845   LDS2130     NLTT 1581/1580                                                          Chm2004 
00297+5548   MLB 150     STI1361.                                                                        
00300-0357   HJ  322     12 Cet.                                                                         
00300-1058   GAL 301     Object #19 in Gallo's original list.                                    Gal1912a
00300-1657   CHM   2     NLTT  1595 +  1598.                                                             
00300-6023   JSP 855     00301-6027TDS1494                                                               
00300-7257   OGL  27     SMC136.1.2934  + SMC136.1.3498                                          Pli2012 
00301+2945   BU 1095     28 And. A is a Delta Scuti-type variable, GN And.                               
00301-3740   DAY   1     2MASS J0030-3739 + 2MASS J0030-3740. Dwarf / white dwarf binary.                
                         Spectral types M9+/-1 + DA, Teff 2000-2400 + 7600+/-175K, masses                
                         0.07-0.08 + 0.48-0.65 Msun. Minimum age of the system > 1.94 Gyr.       Day2008 
00302+5929   STI  79     Historical measures of STI1363 match STI  79 and have been included.            
00304-0947   CHE  27     This pair has opened considerably since its discovery (from 9".6 to     Che1910 
                         19"), due to the considerable proper motion of the primary. AC2000              
                         coordinates of both components from ~1901 are in good agreement with            
                         Chevalier measure, so identification with this pair appears probable.   Hrt2012b
00305-7237   OGL  28     SMC136.3.2481  + SMC136.3.2710                                          Pli2012 
00306+4919   OL   86     Aka TDS1492.                                                                    
00306+1442   OSO   6     G032-026. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates                                                        Oso2004 
00306-7358   OGL  29     SMC133.7.1599  + SMC138.1.5656                                          Pli2012 
00306-7242   OGL  30     SMC136.3.2599  + SMC136.2.3059                                          Pli2012 
00307+3208   STT  11     B is BD+31@66.                                                                  
00307-1545   HJ 1979     J 1435.                                                                         
00310+3817   ALI 480     Also known as ES 2447.                                                          
00311+5648   ES    2     BDS 269 same star.                                                              
00311-7239   OGL  31     SMC131.6.14    + SMC131.6.859   + SMC136.4.2269                         Pli2012 
00312+0631   GWP  57     XMI 127.                                                                Tob2012b
00312-3041   LDS2132     NLTT 1669/1668                                                          Chm2004 
00312-6102   HJ 3372     CD-61@81.                                                                       
00313-7311   OGL  32     SMC130.6.354   + SMC130.5.916                                           Pli2012 
00314+3335   HJ 5451     STTA  2. A is a spectroscopic binary. B is BD+32@81.                            
                         HJL1004.                                                                HJL1986 
00314+0158   LDS 865     Also known as GWP  59 or XMI 128.                                       Tob2012b
00314-1113   GAL 302     Object #21 in Gallo's original list.                                    Gal1912a
00314-4848   RST  11     lam 1 Phe. A is a spectroscopic binary.                                         
00315-6257   B     7     A: bet 1 Tuc. A is a spectroscopic binary.                                      
             I   260     C: bet 2 Tuc                                                                    
                         bet 1,2,3 Tuc form a sextuple system with cpm.                                  
                         bet 3 Tuc (mag. 5.14, A2) is the close binary B     8.                          
             SHY 114     AE: HIP   2484 + HIP   2578.                                                    
             SHY 114     AF: HIP   2484 + HIP   2729.                                                    
             SHY 114     AG: HIP   2484 + HIP   1481.                                                    
             SHY 113     FG: HIP   2729 + HIP   1481.                                                    
             SHY 117     FH: HIP   2729 + HIP   1993.                                                    
             SHY 117     FI: HIP   2729 + HIP   1910.                                                    
             SHY 113     GH: HIP   1481 + HIP   1993.                                                    
00316+1344   LDS9091     Old LDS6091.                                                                    
00317+5057   LDS3175     Coordinate correction and estimate of secondary's proper motion by              
                         Caballero (2013, private comm.)                                                 
00318+5431   STT  12     lam Cas = 14 Cas. A premature orbit has been computed.                          
                         Spectral types of primary and secondary assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
                         Corrections to Drummond et al. (2014) orbit: P=245.70 +/- 35.96y,               
                         T0=2025.54 +/- 4.65 (Drummond, private comm.)                                   
                         Uniform disk diameter  0.224 +/- 0.017 mas,                                     
                         Limb darkened diameter 0.230 +/- 0.017 mas,                                     
                         Teff = 12000+/-500 K based on LD although SED result (12800 +/- 500)            
                         thought to be more accurate due to poor binary flux correction.                 
                         Radius is 2.31 +/- 0.20 \rsun.                                          CIA2019a
00319+3705   BRT2584     ALI 248.                                                                        
00319-2750   LDS2134     NLTT 1711/1713                                                          Chm2004 
00319-7318   OGL  33     SMC130.6.16    + SMC130.6.13                                            Pli2012 
00320+1426   GRV 975     Aka SLW  29.                                                                    
00321+6715   MCY   1     Aa,Ab: Discovery designation is per Todd Henry 03/02/98.                        
                         K-band magnitudes of components 6.42 and 8.44, derived masses are               
                         0.377 +/= 0.030 and 0.138 +/- 0.007 Msun.                               Doc2008d
             VYS   2     AB: ADS 433, MLB 377. The primary is an astrometric binary, P=16y.              
                         Proper motion +1.723 -0.242. A premature orbit has been computed for            
                         the visible pair.                                                               
                         Also a flare star, V547 Cas.                                                    
                         Woitas et al. (2003) give orbital solution and determination of         Woi2003 
                         dynamical masses for this low-mass M dwarf triple.                              
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Solution includes mass determination.                                   Woi2003 
                         In the orbit catalog figure illustrating the Docobo et al. (2006)       Doc2006g
                         orbital solution, B is plotted relative to the center of mass. These            
                         adjusted measures were provided by Docobo (2007, private comm.) See             
                         also further analysis by Docobo et al. (2008), who derive a mass for    Doc2008d
                         the B component (K-band mag 7.88) of 0.177 +/- 0.014 Msun (see note to          
                         MCY 1 pair above for masses of Aa and Ab components.)                           
             GL 22       Ba,Bb: Andrade & Docobo detect a sinusoidal pattern in the motion of            
                         the B component, which they attribute to a possible 4th component of            
                         the system in a 15y orbit.  Masses under this scenerio are 0.162 +/-            
                         0.014 Msun for Ba and 0.0152 +/- 0.0053 Msun (16.0 +/- 5.6 Mjup) for            
                         Bb (assuming a circular solution) or 0.0147 +/- 0.0027 Msun (15.4 +/-   Ana2009 
                         2.8 Mjup) for Bb (assuming an elliptical solution). The Bb component            
                         may be either a giant planet or a brown dwarf.                          Ana2011 
00321+0155   GWP  60     XMI 129.                                                                Tob2012b
00321-0511   A   111     Elongations and quadrant of AB doubtful.                                B__1963b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.48 +/- 0.34, 1.75, and 0.85 Msun, respectively.  Mlk2012 
00321-1218   HDS  71     Cvetkovic et al. (2014) derive spectral types G2 and  G5, masses 1.11           
                         and 1.05 Msun. Dynamical parallax is 14.06 +/- 0.62 mas.                Cve2014 
00322-1050   LDS3176     NLTT 1727/1715                                                          Chm2004 
00322-7515   HJ 3374     B is CPD-75@48.                                                                 
00323-6304   LDS9092     Old LDS6092.                                                                    
00324+7335   LDS1509     NLTT 1681/1680.                                                                 
00324+0657   MCA   1     51 Psc. A is a triple occultation system, and a resolved                        
                         interferometric pair. B is BD+06@65.                                            
                         First detected as an occultation binary by Africano.                    Afr1976 
                         Mason et al. give Aa,Ab,B triple solution (double (Aa)-B in HIP).       Msn1997a
                         Orbit mostly dependent on Hershey pc obs; more IR speckle needed.       Hry1973 
                         The Aa,Ab components of ADS 449 apparently went through periastron              
                         some time during 1987-1990.                                             Hrt1992b
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 3.08 +/- 0.46, 3.66, and 2.40 Msun, respectively.  Mlk2012 
             STF  36     AB: H 4  70.                                                            MEv2010 
00325+0101   GWP  61     XMI 130. GRV1160.                                                       Tob2012b
00326+5513   RAS  17     SrCrEu star at about 36 pc. Secondary likely close to solar (G2-G5).    Ras2014 
00326+2018   HJ 1982     52 Psc.                                                                         
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
00327+7807   STF  34     HJL   6.                                                                HJL1986 
00327+2312   BU 1310     AC: Rectilinear solution by Friedman et al. (2012).                     USN2012a
00327+0732   GWP  62     XMI 131.                                                                Tob2012b
00327-6302   B     8     Aa,Ab: bet 3 Tuc. CPM with bet 1 and bet 2 Tuc = B     7.                       
             SHY 116     AB: HIP   2578 + HIP   2729. B component = F component of 00315-6257.           
             SHY 116     AC: HIP   2578 + HIP   1993. C component = H component of 00315-6257.           
00328+2817   STT  14     A is a spectroscopic binary. Aka H N  76.                                       
00329-7445   OGL  34     SMC134.1.90    + SMC134.8.2266                                          Pli2012 
00330+4442   LDS9093     Old LDS6093.                                                                    
                         NLTT 1759/1762                                                          Chm2004 
00330+0850   J  2710     -9s, -5' from BD+08   69.  Declinaison augmentee de 2'.                 J__1955 
00330-7335   OGL  35     SMC130.8.5777  + SMC130.8.5810                                          Pli2012 
00331-7446   OGL  36     SMC134.1.223   + SMC134.1.542                                           Pli2012 
00332+1902   GWP  63     XMI 132.                                                                Tob2012b
00332-7114   OGL  37     SMC132.7.12    + SMC132.7.25                                            Pli2012 
00334+1418   LDS9094     Old LDS6094.                                                                    
00334-7104   OGL  38     SMC132.6.11    + SMC132.6.191                                           Pli2012 
00334-7407   OGL  39     SMC133.8.4148  + SMC133.1.95                                            Pli2012 
00335+4006   HO    3     A premature orbit has been computed.                                            
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.60 +/- 0.55, 2.07, and 1.10 Msun, respectively.             Mlk2012 
00336+1712   GWP  64     XMI 133.                                                                Tob2012b
00336-0811   LDS 5280    B component of 00339-0813 LDS5281 found to be the A component of                
                         LDS5280; pairs merged, with LDS5281 made AC pair (with quadrant flip).          
00337-3500   HJ 3375     HIP 2663. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
00339+1748   GWP  65     XMI 134.                                                                Tob2012b
00340-7056   OGL  40     SMC132.5.883   + SMC132.5.916                                           Pli2012 
00344-7252   OGL  41     SMC131.7.3527  + SMC131.7.4371                                          Pli2012 
00346+6254   BU  108     AB: B component is SB, P=156.430d                                       Tok2014d
00345-0433   STF  39     AB,C: H 4  76.                                                          MEv2010 
00346-7105   OGL  42     SMC132.6.1065  + SMC132.6.1159                                          Pli2012 
00349+2627   COU 548     Originally entered as AG   4.                                                   
00350+5636   ES    3     BDS 326 identical.                                                              
00351+8337   MLR 481     00356+8338HDS  80                                                               
00351+0209   RST5182     J 3281.                                                                         
00352-0336   HO  212     13 Cet.                                                                         
                         Visual primary is 2.1d SB1 (#27 in Batten et al., 1989) and may be a    Bte1989 
                         Delta Scuti-type variable.                                                      
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         1979.5326: This measure was incorrectly attributed to ADS 2200          McA1982d
             BU  490     AB,C: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
00353-0942   CHE  28     J  1437 = 00358-0942CHE  28                                                     
00356-7342   OGL  43     SMC133.4.124   + SMC133.4.3322                                          Pli2012 
00357+0233   LAW   7     LSPM J0035+0233 = NLTT 1930. Law et al (2008) derive a distance of      Law2008 
                         14.5 +6.3/-2.4 pc and a projected separation of 6.8 +3.1/-1.0 au.               
                         Estimated spectral types are M5 and M6.0.                                       
00357-7055   OGL  44     SMC132.5.871   + SMC132.5.912   + SMC132.5.1085                         Pli2012 
00358+5241   GIC  11     G172-011/G217-059.                                                              
                         NLTT 1920/1921                                                          Chm2004 
00359-7429   OGL  45     SMC134.3.2988  + SMC134.3.3515                                          Pli2012 
00360+2959   STF  42     Hyperbolic orbit by Hopmann.                                            Hop1967 
                         sigma = areal constant in the true orbit = 0.1432 arcsec^2/yr                   
                         q = periastron distance in the true orbit = 6".123                              
                         Hopmann made small but unspecified corrections to the node and                  
                         inclination before computing residuals and ephemeris.                   Fin1970b
                         All hyperbolic orbits rejected from Fourth Orbit Catalog                Wor1983 
                         A is a spectroscopic binary.                                                    
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
00360+0514   GWP  66     XMI 135.                                                                Tob2012b
00360+1040   GWP  67     XMI 136.                                                                Tob2012b
00361+3858   J  2711     ALI 723.                                                                        
00363-3818   RST5183     A is a close 4.8-d spectroscopic pair.                                  Tok2019a
00364-7313   OGL  46     SMC130.3.8754  + SMC130.3.8886                                          Pli2012 
00365-0639   LDS3183     NLTT 1976/1977                                                          Chm2004 
00365-7246   OGL  47     SMC131.2.1420  + SMC126.6.896                                           Pli2012 
00366-4908   LDS  21     A is a spectroscopic binary, P = 3.74d. B is CD-49@138.                         
                         SHY 118. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         B component is SB, P=22d                                                Tok2006 
00366-7435   OGL  48     SMC134.2.2429  + SMC134.2.2618                                          Pli2012 
00367+1542   GWP  68     XMI 137.                                                                Tob2012b
00368+1605   KU   69     HJL   7.                                                                HJL1986 
00369+3343   H 5  17     pi And = 29 And.  H V 17. STTA  4.  BDS 263, HJ 1030 identical.                 
                         A is a spectroscopic binary, P = 143.6d. B is BD +32@102.                       
             MKT   1     Aa,Ab: Hummel et al. (1995) visual orbit is based on astrometry from    MkT1995 
                         the Mark III interferometer. Additional spectroscopic data yield                
                         masses, luminosities, radii, effective temperatures, and distance.              
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Hummel et al. (1995).                                                   MkT1995 
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 11.98 +/- 2.06, 11.18, 4.79 Msun, respectively.    Mlk2012 
             RBR   3     Aa,Ac: PA for 2001.7424 observation is measured in zenith mode. If              
                         data collected in equatorial mode, PA = 97.6. Confirmation of the pair          
                         should establish the proper value for theta.                            Rbr2007 
00372+7149   HDS  86     1997.7289: Large change in separation seen since Hipparcos epoch.       Msn1999b
00373+5801   BU 1097     Spectrum composite; A2+K.                                                       
00373-2446   BU  395     Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         HIP 2941. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.79 +/- 0.29, 1.92, and 0.91 Msun, respectively.             Mlk2012 
                         YSC 170.                                                                        
00374-2054   FAR  23     GJ 2010 = NLTT 2019. Primary is white dwarf WD 0034-211.                Far2006 
00374-3717   I   705     Many attempts, but only a few positive observations.                            
00374-3904   WHI   1     Other IDs uncertain; based on Simbad search using epoch-1950                    
                         coordinates 003456-392028 from White et al. (1991).                     Whi1991 
00374-7243   OGL  49     SMC131.3.3943  + SMC131.3.4041                                          Pli2012 
00376+1257   GWP  69     XMI 138.                                                                Tob2012b
00376+1547   GWP  70     XMI 139.                                                                Tob2012b
00378-7246   OGL  50     SMC131.2.5591  + SMC131.2.6860                                          Pli2012 
00378-7413   OGL  51     SMC128.8.65    + SMC128.8.358                                           Pli2012 
00379+1404   GWP  71     XMI 140. GRV1161.                                                       Tob2012b
00379-7256   OGL  52     SMC131.1.6657  + SMC126.7.785                                           Pli2012 
00381-7127   OGL  53     SMC132.1.1336  + SMC132.1.1337                                          Pli2012 
00381-7345   OGL  54     SMC128.5.115   + SMC128.5.276   + SMC128.7.9551                         Pli2012 
00382+0322   J  1042     BAL 1609.                                                                       
00383-7124   OGL  55     SMC132.1.1263  + SMC132.1.1284                                          Pli2012 
00384+0130   BAL 947     Probably ARG 47, BD+00@93.                                                      
00385+4300   LDS5176     old LDS6095.                                                                    
                         NLTT 2053/2057                                                          Chm2004 
00386+4738   OSO   7     G172-016. Common proper motion pair                                     Oso2004 
00386+1420   GWP  72     XMI 141.                                                                Tob2012b
00386-2118   LDS2140     NLTT 2075/2062                                                          Chm2004 
00386-3903   WHI   2     Other IDs uncertain; based on Simbad search using epoch-1950                    
                         coordinates 003609-391934 from White et al. (1991), where pair is       Whi1991 
                         listed as possibly resolved.                                                    
00387-7431   OGL  56     SMC129.7.14    + SMC129.7.603                                           Pli2012 
00388+3101   AG  430     B is BD+30@90.                                                                  
                         Not confirmed using images from the Digitized Sky Surveys               Oso2004 
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
00388-2506   HJ 1991     B is CD-25@235.                                                                 
00389-2536   HJ 1992     B is CD-26@195.                                                                 
00389-7248   OGL  57     SMC126.7.3     + SMC126.7.86                                            Pli2012 
00391-7313   OGL  58     SMC125.6.23680 + SMC125.6.24279                                         Pli2012 
00392+1329   GWP  73     XMI 142.                                                                Tob2012b
00393+3052   BU  491     del And = 31 And                                                                
                         A is a long-period spectroscopic binary, P = 15000d (?).                        
             BTM   1     Aa,Ab: Bottom et al. (2015) resolve the spectroscopic binary del And            
                         using the Palomar 5m and Stellar Double Coronograph. The physical               
                         separation is 11.55 +/- 0.13 au; the spectral type of the companion is          
                         estimated at K4 +/- 2.                                                  Btm2015 
                         Aa,Ab: Gontcharov & Kiyaeva (2002) orbit based on combination of        Gon2002b
                         ground-based catalogs with Hipparcos. They quote masses of 1.3+/-0.4            
                         and 1.3 Msun for the two components, and estimate their spectral types          
                         as K3III and white dwarf.                                                       
                         Mk III Limb-darkened diameter  4.12 mas.                                MkT1991 
                         Mk III Limb darkened diameter  4.17  +/- 0.06  mas                      MkT2001 
                         Mk III Limb-darkened diameter  4.136 +/- 0.041 mas                      MkT2003 
                         NPOI Limb-darkened diameter    4.24  +/- 0.06  mas                      NOI2001b
00394+2115   STT 550     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             LUH   3     54 Psc. AC: Common proper motion for both components was determined             
                         through comparison of relative location with that obtained by 2MASS.            
                         The B component is determined to be a possible T dwarf (T7.5 +/- 0.5)           
                         based on mid-IR colors and magnitudes. Age is determined to be 7 +/-            
                         3 Gyr and mass of C component 0.051 +/- 0.014 Msun.                     Luh2007 
                         The T dwarf is referred to by Luhman et al. as the "B" component,               
                         either because the non-physical STT 550 was not considered, or the WDS          
                         was not consulted. In any event, this component referred to in the WDS          
                         hierarchy as "C" is sometimes called "B" in the literature.                     
                         CHARA Array Limb-darkened diameter  0.790 +/- 0.027 mas,                CIA2008c
                         R =  0.947 +/- 0.032 \rsun.                                                     
00395+6151   STI 110     00394+6158MLB 378                                                               
00395+6002   HJ 1042     STI 111.                                                                        
00395+1454   GIC  12     AB: LDS 868 = G032-037/G032-038.                                                
                         NLTT 2126/2125                                                          Chm2004 
             JNN 249     Ba,Bb: G 32-37B. Estimated age 300-1000 Myr; masses 0.33 +/- 0.03 and           
                         0.19 +/- 0.01 Msun; a ~4.3 au.                                          Jnn2014 
00396+8445   HJ 1986     STTA  3. B is BD+83@11.                                                         
00398+6157   LAM   1     MLB 379. STI 114AC.                                                             
                         BDS notes AB measure 357deg, 69".87 - Burnham was unable to find any            
                         pair that matched this separation - perhaps typo for 6".98?                     
             STI 113     BD: Previously 00399+6158STI 113AB.                                             
00398-1418   GAL 303     Object #23 in Gallo's original list.                                    Gal1912a
00399+2126   STF  46     55 Psc.                                                                         
00400+7652   STTA  5     B is BD+76@16.                                                                  
00400+1336   BPM  16     [PM2000]   26418 + [PM2000]   26431.                                    Gvr2010 
00400+1016   PLQ   7     The A component has been resolved as a close spectroscopic binary.      Tok2020h
00400+0106   GWP  74     XMI 143.                                                                Tob2012b
00401+5014   V523 Cas    Multiple system including contact binary. Pribulla & Rucinski (2006)    Pbl2006 
                         estimate the mass of the contact pair at 1.130 Msun and the minimum             
                         mass of the wider component at 0.31 Msun.                                       
00403+2403   BU 1348     AC : Carries BU 1348 from ADS (562), despite earlier discovery by STF.          
                         BC : AD equated with this component.                                            
                         BC: Rectilinear solution by Mason et al. (2012).                        WSI2012 
00403-0855   GAL 304     Object #24 in Gallo's original list.                                    Gal1912a
                         Also known as FAB   3.                                                          
00403-7241   OGL  59     SMC126.6.564   + SMC126.6.565                                           Pli2012 
00404+0722   OSO   8     G001-012. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates                                                        Oso2004 
00405+5632   BU 1349     alp Cas = 18 Cas = Schedar                                                      
                         Mk III Limb-darkened diameter  5.4   +/- 0.4   mas.                     MkT1989 
                         Mk III Limb-darkened diameter  5.64 mas.                                MkT1991 
                         Mk III Limb-darkened diameter  5.72  +/- 0.08  mas                              
                         Mk III Limb-darkened diameter  5.608 +/- 0.056 mas.                     MkT2003 
                         NPOI Limb-darkened diameter    5.60  +/- 0.06  mas,                     NOI1999 
                         R = 42.1 +/- 1.7 \rsun.                                                         
                         NPOI Limb-darkened diameter    5.65  +/- 0.08  mas.                     NOI2001b
                         NPOI Limb-darkened diameter    5.903 +/- 0.036 mas,                             
                         R =   45.03 (+1.57- 1.68)  \rsun,  Teff = 4476 +/-  15 K,                       
                         L =  734.2 +/- 42.2 \lsun.                                              NOI2023 
             H 5  18     AD: H V 18. Also HJ 1993.                                                       
                         AD: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AD: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
00405-1631   BU  109     B is BD-17@108.                                                                 
00405-4829   LDS9096     Old LDS6096.                                                                    
00405-7321   OGL  60     SMC125.7.29221 + SMC125.7.29234                                         Pli2012 
00406-0023   ARG  48     BAL 646.                                                                        
00406-1502   GAL 305     Object #26 in Gallo's original list.                                    Gal1912a
00407-0421   HJ  323     B is BD-05@100.                                                                 
00408+1618   GWP  76     XMI 144.                                                                Tob2012b
00408-7125   OGL  61     SMC127.8.10    + SMC127.8.21                                            Pli2012 
00409+0810   GWP  77     XMI 145.                                                                Tob2012b
00409-7320   OGL  62     SMC125.7.29414 + SMC125.7.30547                                         Pli2012 
00410+3257   SEI   8     Listed in ADS as both #565 and #580 (00420+3304POT   8)                         
00414-7124   OGL  63     SMC127.8.1547  + SMC127.8.2057  + SMC127.8.2076                         Pli2012 
00415+5550   GIC  13     G218-007/G218-008 = GJ 1015AB.                                                  
00416+2438   WRH  28     Hynek 1. Not certainly resolved by Wilson in 1949, but successfully             
                         resolved by McAlister in 1980.                                                  
                         1983.9362: this (and presumably other) negative results may be due              
                         to a delta m between 1.5 and 3.                                         Bnu1984 
00416-0934   GRV1162     SLW  36.                                                                        
00416-5621   RNR   1     2MASS J0041353-562112. Spectral types M6.5 +/- 1 and M9.0 +/- 1.                
                         Assuming age of ~10 Myr, component masses are ~30 and ~15 Mjup;                 
                         distance 50 +21/-10 pc, orbital period 126 +86/-37y.                    Rnr2010 
00417-4729   LDS9097     Old LDS6097.                                                                    
00417-7102   OGL  64     SMC127.6.1579  + SMC127.6.1681                                          Pli2012 
00418-5630   HJ 3387     xi Phe. Variable.                                                               
00419+1751   A  2303     J 585.                                                                          
00419+1341   JMS   1     BDK   3. NLTT 2274 + 2MASS J00415453+1341351. Distance 21 +/- 8 pc for          
                         the primary, 31 +/- 6 pc for the secondary. Estimated age of system             
                         4.5-8 Gyr. Mass of secondary estimated at 0.081-0.083 Msun.             Fah2010 
                         NLTT 2274 + 2MASS J00415453+1341351. Baron et al. (2015) estimate               
                         spectral types M4.0 +/- 0.5 and M9.5 +/- 0.5, distances 23 +14/-9 and           
                         40 +6/-12 pc, masses 0.207-0.272 and 0.076-0.083 Msun.                  BFr2015 
00420-7306   OGL  65     SMC125.5.32790 + SMC125.5.33233                                         Pli2012 
00422-7435   OGL  66     SMC129.2.448   + SMC129.2.992                                           Pli2012 
00424+1721   BPM  17     [PM2000]   27917 + [PM2000]   27832.                                    Gvr2010 
00424+0410   STT  18     AB: Visual orbit (Grade 4) gives too large mass sum of 52 Msun.         Tok2014d
00426-5407   HJ 3388     B is CPD-54@159.                                                                
00427-3828   HDO 182     lam 1 Scl                                                                       
00427-6537   I   440     Probable rapid motion, as yet undefined by the measures.                        
                         Derived orbital parallax 0".00685, mass sum 4.91 +/- 2.94 Msun          Lin2004a
00427-7409   OGL  67     SMC128.1.11    + SMC128.1.217                                           Pli2012 
00428+3533   TOK  10     FF And. Primary is 2.2d SB2. Estimated period of visual pair 4400y.             
                         G-solution in HIPPARCOS.                                                Tok2006 
                         This system is noted as being triple in Tokovinin et al. (2006),        Tok2006 
                         including a close spectroscopic binary pair with approximately 1.3 mas          
                         separation and a likely wider companion at 11" separation. Due to               
                         these separations however, it is counted as single for our purposes.    Jnn2012 
00429+2047   A  2205     A premature orbit has been calculated.                                          
00431+3913   MLB1054     ALI 727.                                                                        
00431+0707   OSO   9     G001-013. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates                                                        Oso2004 
00432+0128   GWP  80     XMI 146.                                                                Tob2012b
00432-2146   LDS1078     SLW  39.                                                                        
00432-3759   UC  427     CPM candidate confirmed physical by photometry (2MASS and V mags).      Tok2013c
                         Spectral type of comoving secondary estimated as M0-1, mass 0.56 Msun.  Mug2014 
00434-0054   STF  53     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
00434-5728   HJ 3391     eta Phe.                                                                        
             MRN   1     Aa,Ab: Marion et al. (2014) estimate the companion as K1V, at about             
                         6.8au separation from the A0IV primary. They derive a minimum orbital           
                         period of ~9.5y, consistent with an astrometric companion reported by           
                         Makarov & Kaplan (2005). A followup K-band observation suggests         Mkr2005 
                         spectral type for the secondary of ~G5V.                                Mrn2014 
00435+3351   BUP 241     AB: B is BD+32@120.                                                             
             WEI  46     AC: Distances are 1321" and 1310".                                              
00436-2354   LDS2147     NLTT 2383/2381                                                          Chm2004 
00437+7211   OSO  10     G242-065. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates                                                   Oso2004 
00439+0946   J  2712     Not found by Heintz at IDS position.                                    Hei1990b
00441+5655   MLR 625     Also known as TDS1589.                                                          
00441-7238   OGL  68     SMC126.3.2852  + SMC126.3.910                                           Pli2012 
00442+3122   GRV  40     Aka HJL1007                                                                     
00442+4614   STF  52     Primary is eclipsing binary V355 And (period 4.7184 day).               Zas2010 
00443-7439   OGL  69     SMC129.2.3173  + SMC129.1.2349                                          Pli2012 
00444+3332   STF  54     STF  56.                                                                        
                         SEI   9.                                                                Nsn2017a
00444+1235   HJ    6     AG 7.                                                                           
00445-1715   B  2513     Probably BD-18@118.                                                             
00445-3607   B   640     Primary is CR Scl, eclipsing binary of W UMa-type, period 0.246537d.    Zas2013 
00446+4341   LDS5177     old LDS6098.                                                                    
00446+2007   GWP  84     XMI 147.                                                                Tob2012b
00446-1856   LDS3195     AC: NLTT 2439/2437                                                      Chm2004 
00447+4817   BU  231     omi Cas = 22 Cas                                                                
                         Primary is a spectroscopic binary, P = 1033:d.                                  
             NOI   3     Aa,Ab: Hipparcos astrometric solution adopted some elements from the    HIP1997d
                         orbit of Abt & Levy (1978).                                             AbH1978 
                         Koubsky et al. (2010) combined solution uses NPOI astrometric data      NOI2010 
                         together with radial velocities from the Dominion Astrophysical and             
                         Ondrejov Observatories. The secondary appears to be of similar mass to          
                         the primary, although the magnitude difference is nearly 3 magnitudes.          
                         One possible explanation might be that the secondary is comprised of a          
                         close pair of similar stars, possible early A dwarfs.                           
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 6.12 +/- 2.94, 7.39, and 5.62 Msun, respectively.  Mlk2012 
00448+4202   LDS5178     old LDS6099.                                                                    
00448+3940   ALI1011     MLB 810.                                                                        
00450-7234   OGL  70     SMC126.4.9807  + SMC126.4.10299 + SMC126.4.10283                        Pli2012 
00451+0533   PLQ   8     BAL2993.                                                                        
                         HJL   8.                                                                HJL1986 
00451-7310   OGL  71     SMC125.4.14538 + SMC125.4.14830                                         Pli2012 
00452+0015   LDS 836     AB: Primary is SB1, P=11.439d (Griffin 2002 Obs 121, 221).              Tok2014d
00453+1019   STF  58     B is BD+09@85.                                                                  
00454+1422   LDS1079     G032-046. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
00454-7413   OGL  72     SMC128.1.8607  + SMC128.1.10178                                         Pli2012 
00455+1232   HJ    7     Rectilinear solution by Mason et al. (2012).                            WSI2012 
00455-1253   BUP   8     18 Cet.                                                                         
00456+3628   ALI  21     Astrographic Catalogue plate defect.                                    Grv2023b
00456-7115   OGL  73     SMC127.2.1735  + SMC127.1.582                                           Pli2012 
00456-7331   OGL  74     SMC125.1.37411 + SMC125.1.37410                                         Pli2012 
00457+7459   H N 122     A: 21 Cas = YZ Cas                                                              
                         A is an Algol-type eclipsing and spectroscopic binary, P = 4.47d.               
00457-1625   MLF   1     aka HO  624                                                                     
00457-3510   LDS3191     LDS5294                                                                         
00457-7401   OGL  75     SMC128.2.9138  + SMC128.2.10100                                         Pli2012 
00458+5459   ARG   2     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
00458-4733   HDO 183     AB: PMS star, X-ray source, rapid rotation, debris disk.                Tok2014d
00458-7242   OGL  76     SMC126.3.12924 + SMC126.3.13758                                         Pli2012 
00459+3347   LAW   8     LSPM J0045+3347 = NLTT 2511. Law et al (2008) derive a distance of      Law2008 
                         14.9 +7.0/-2.6 pc and a projected separation of 4.0 +2.1/-0.6 au.               
                         Estimated spectral types are M4.5 and M5.5.                                     
00459-7359   OGL  77     SMC128.2.9204  + SMC128.2.11627                                         Pli2012 
00460+3626   HJ  627     ALI 22.                                                                         
00460-7108   OGL  78     SMC127.3.1324  + SMC127.2.2113                                          Pli2012 
00461-0539   LDS3199     NLTT 2540/2538                                                          Chm2004 
00462-2214   RST4155     Ma,Mb = 1.043 +/- 0.026, 0.990 +/- 0.024 \msun.                         GmJ2022 
00462-7250   OGL  79     SMC126.2.15522 + SMC126.2.15521                                         Pli2012 
00463+6517   HJ 1052     STI 124.                                                                        
00463-0634   HDS 101     Cvetkovic et al. (2016) estimate spectral types F2 and F9, masses 1.56          
                         and 1.20 Msun. Dynamical parallax is 9.22 +/- 1.22 mas.                 Cve2016b
00464+3057   STFA  1     STTA  6. B is BD+30@114.                                                        
                         H 5 123.                                                                MEv2010 
00464-7332   OGL  80     SMC103.5.132   + SMC103.5.864                                           Pli2012 
00466-7334   OGL  81     SMC103.5.4     + SMC103.5.25                                            Pli2012 
00467+1335   BPM  18     [PM2000]   30523 + [PM2000]   30577.                                    Gvr2010 
00467-0426   LDS9100     Old LDS6100.                                                                    
                         NLTT 2582/2586                                                          Chm2004 
00467-7228   OGL  82     SMC101.6.16943 + SMC101.6.16996                                         Pli2012 
00468-5200   HJ 3398     B is CPD-52@91.                                                                 
00469+0533   GWP  86     XMI 148.                                                                Tob2012b
00470+3848   ES  223     00471+3848ALI 729                                                               
00470-1152   CUD   1     AB: Component A is the central star of the planetary nebula NGC 246.    Skf2013 
                         Adam & Mugrauer (2014) estimate spectral type of B component as K2-K5,          
                         mass 0.85 Msun.                                                         Ada2014 
             ADA   1     AC: Adam & Mugrauer (2014) detect an additional companion to the white          
                         dwarf primary. Estimated spectral type is M5-M6, mass 0.1 Msun. All             
                         components share common proper motion.                                  Ada2014 
00471+3800   J  2713     ALI 485.                                                                        
00471-7304   OGL  83     SMC100.6.7164  + SMC100.6.7261                                          Pli2012 
00473+2416   BUP   9     AB: zet And. A is an eclipsing and spectroscopic binary, P = 17.8d.             
                         Mk III Limb-darkened diameter  4.4   +/- 0.5   mas.                     MkT1989 
                         AC is probably optical.                                                         
                         Proper motion +758 -1146.                                                       
00474+5106   H 5  82     H V 82. STTA  7. B is BD+50@142.                                                
00474+3314   BOW   1     Not found by Heintz at IDS position.                                    Hei1990b
00474+1730   BPM  20     [PM2000]   30911 + [PM2000]   30961.                                    Gvr2010 
00474+1726   BPM  19     [PM2000]   30878 + [PM2000]   30861.                                    Gvr2010 
00474-7345   OGL  84     SMC103.7.16909 + SMC128.5.14891                                         Pli2012 
00476+5533   TDS1614     WDS designation changed slightly when merged with STI1428 into triple           
00476-1812   LDS9101     Old LDS6101.                                                                    
00477+1253   STTA  8     LDS2796. B is BD+12@90.                                                         
                         AB: HJL   9.                                                            HJL1986 
00479-2921   I   261     Rapid, but as yet undefined, motion.                                            
                         1989.9437: Having had only one other measure in the last 35 years,              
                         this pair needs further observation, especially since we appear to be           
                         near periastron at this epoch.                                                  
00480+5127   STF  59     AB: H 1  40.                                                            MEv2010 
00481-7234   OGL  85     SMC101.7.31055 + SMC101.5.77                                            Pli2012 
00481-7348   OGL  86     SMC103.7.20241 + SMC103.7.6961  + SMC103.7.7536                         Pli2012 
00482+1737   GWP  87     XMI 149.                                                                Tob2012b
00482+1055   DAM 864     CD: GII 108.                                                                    
00484+0517   HEI 202     The AB pair was seen on two photographic plates by Heintz, but the              
                         companion was not visible on 164 other plates, nor was it seen on               
                         repeated checks with a micrometer. The parallax plates also yield               
                         large residuals, leading Heintz to suspect variability.                 Hei1984i
                         CHARA Array Limb-darkened diameter of A :                               CIA2012f
                         R =  0.6954 +/- 0.0041 \rsun, L =  0.26073 +/-0.00263 \lsun,                    
                         Teff = 4950 +/-  14 K, M = 0.753 \msun.                                         
00486-2357   LDS  27     NLTT 2704/2705                                                          Chm2004 
00487+4619   SMA  10     A 1-deg error in WDS designation, apparently a typo in transcribing             
                         coordinates from the original source.                                           
00487+1841   BU  495     Hipparcos parallax of 0".01628 yields a mass sum of 2.14 Msun                   
                         with an uncertainty of 28%, agreeing well for a double star of                  
                         spectral type G0. The dynamical parallax is 0".0149, in reasonable              
                         agreement with the measured one. Semi-major axis erroneously given              
                         as 0.317; a = 0.617 matches Scardia's figure, so is assumed to be               
                         the intended value.                                                     Sca2000b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.00 +/- 0.67, 2.30, and 1.05 Msun, respectively.             Mlk2012 
                         Quadruple system. The inner AB pair, BU 495, has an orbit with a 143.6          
                         +/- 4.0 yr period (Scardia et al. 2000). The CPM component C at 152"    Sca2000b
                         from AB was found by Tokovinin & Lepine (2012), who estimate the        Tok2012c
                         probability of it being physical as 0.99. The component C was resolved          
                         by Riddle et al. (2015) into a 0".67 pair Ca,Cb. The PM is too small    RAO2015 
                         to determine if the Ca and Cb share common PM, but the low density of           
                         background stars and the small separation imply that the pair Ca,Cb is          
                         physical.                                                               Rbr2015d
00487+0735   BUP  11     del Psc = 63 Psc                                                                
00489-7434   OGL  87     SMC104.8.5148  + SMC129.2.824                                           Pli2012 
00490+4435   MCT   2     Initially entered into WDS incorrectly as 00490+5535.                           
                         GJ 3058. Estimated age 50-150 Myr; masses 0.22 +/- 0.10 and 0.18 +/-            
                         0.08 Msun; a ~19.0 au.                                                  Jnn2014 
00490+1656   BUP  12     64 Psc. A is a spectroscopic binary.                                            
             64 Psc      Combined spectroscopic/interferometric solution by Boden et al. (1999)  Bod1999b
                         yields P=13.824621 days, T=JD 2450905.984.                                      
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 2.51 +/- 5.01, 2.80, and 1.10 Msun, respectively.  Mlk2012 
00491+5749   STF  60     eta Cas = 24 Cas = Achird.                                                      
                         Proper motion of A +1141 -572. PM of B = +1105 -493.                            
                         A has been reported to be a                                             Dob1927 
                         spectroscopic binary, but this is not confirmed. Doberck, Pavel, and    Pav1914 
                         Harshaw measure attributed to BC, then later to BE, was actually to     Hsw2004 
                         another faint star; confusion was due to the high proper motion of the          
                         B component and the long time span since the previous measurement.              
                         Proper Motion of E -003-001, F -010+000, G +009-005, H -006-001                 
                         System has been discussed by van de Kamp & Flather.                     Kam1955 
                         AB: H 3   3.                                                            MEv2010 
                         AB: Additional notes may be found in Simonov (1937).                    Smw1937 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.58 +/- 0.85, 1.71, and 1.60 Msun, respectively.  Mlk2012 
                         AB: Raghavan et al. (2010) do not accept the astrometric sub-system as  Rag2010 
                         real.                                                                   Tok2014d
                         CHARA Array Limb-darkened diameter  1.623 +/- 0.004 mas,                CIA2012e
                         R =  1.039 +/- 0.004 \rsun, L =  1.252 +/-0.019 \lsun,                          
                         Teff = 6003 +/-  24 K, M = 0.972 +/- 0.012 \msun,                               
                         Age =  5.4 +/- 0.9 Gyr.                                                         
                         AD: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
00492+5720   A   921     Star C (mag. 14, 4.5") is probably physical.                                    
00494-2313   PES   1     A : Teff = 5400 +/- 60 K, Age = 2.3 +/- 1.4 GYr, M = 0.856 +/- 0.014    Pes2019 
                             \msun, R = 0.769 +/- 0.016 \rsun.                                           
                         B : Teff = 1300 +/- 100K, R = 0.91 +/- 0.16 \rjup, M = 70.2 +/- 1.6             
                             \mjup.                                                                      
00494-7401   OGL  88     SMC103.8.8139  + SMC103.8.8451                                          Pli2012 
00496-5410   HJ 3402     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
00497-1841   B  2067     Primary is Hipparcos acceleration solution (G-code) binary. Is the              
                         acceleration caused by the companion, or is it a triple?  Companion             
                         not measured by HIP, could cause false acceleration? 2MASS: another             
                         companion at 6.6", 276.2deg is listed, likely bogus.                    Tok2014d
00497-7336   OGL  89     SMC103.6.31460 + SMC103.6.31513                                         Pli2012 
00498+7027   ENG   2     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
00499+3027   STTA  9     B is BD+29@139.                                                                 
00499+2743   STF  61     65 Psc = i Psc                                                                  
                         H 2  84.                                                                MEv2010 
00500-0401   RST4158     J 1440.                                                                 J__1941a
00501+1606   GWP  88     XMI 150.                                                                Tob2012b
00502+1604   GWP  89     XMI 151.                                                                Tob2012b
00502-7147   OGL  90     SMC102.4.11    + SMC102.4.92                                            Pli2012 
00503+6235   MRI  32     FMR  35.                                                                        
00503-7217   OGL  91     SMC101.4.18707 + SMC101.4.18866                                         Pli2012 
00504+5038   BU  232     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.83 +/- 2.67, 2.70, and 1.20 Msun, respectively.  Mlk2012 
00505+7538   HJ 1997     B is BD+74@31.                                                                  
00505+5930   LDS9102     Old LDS6102.                                                                    
00505+2450   LDS3203     NLTT 2805/2804                                                          Chm2004 
00506-7328   RSS   2     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
00507+6415   MCA   2     A spectroscopic binary and resolved interferometric pair. Composite             
                         spectrum: B9.5V+G0III-IV.                                                       
                         Combined spectroscopic/visual solution by Mason et al. (1997).          Msn1997b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 9.12 +/- 1.74, 8.22, and 2.40 Msun, respectively.             Mlk2012 
00508+5123   OSO  11     G172-024. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
00508+3203   A   922     No observations 1932-69. Apparently has completed nearly a revolution.          
00509+1215   GWP  91     XMI 152.                                                                Tob2012b
00511+2231   AZC   7     BC measure of 00511+2236LDS3204 now with this pair and decoupled with           
                         the former LDS3204AB.                                                           
00511-7204   OGL  92     SMC102.2.129   + SMC102.2.1604                                          Pli2012 
00511-7226   DBR 213     DBR 214.                                                                        
00512+2211   KU   70     motion direct.                                                                  
00513+5840   GIC  14     G218-015/G218-016.                                                              
00513-7413   OGL  93     SMC104.3.46    + SMC104.3.1506                                          Pli2012 
00515+5630   DAL  11     RoboAO: 2 faint companions near B at 16.7" and 15.0", likely optical.   RAO2015 
                         Star in cluster IC 1590 (NGC 281 nebula)                                Tok2014d
                         Significantly different proper motion and parallax for components, so   Jao2017 
                         non physical.                                                                   
00515-7225   OGL  94     SMC101.3.29657 + SMC101.4.5258  + SMC101.3.30856                        Pli2012 
00516+4412   YR   19     Aa,B: These observations were previously presented in Horch et al       Hor2009 
                         (2009, 2010). The data presented here are the result of a reanalysis    Hor2010 
                         using a trinary fit to include the close component YR 123Aa,Ab,                 
                         although the Aa,Ab component was not always of high enough quality to           
                         include. In the course of reanalyzing these observations, it was also           
                         noticed that the magnitude differences appearing in Horch et al (2011)          
                         for the two filters shown were reversed. The values here correct that           
                         error.                                                                  Hor2011b
00516+2237   A  1808     Orbits with periods around 110y and a ~0.13" have been computed.                
                         Motion direct.                                                                  
                         Omega for Docobo (1988) solution corrected from 322.8 to 332.8          Doc1988b
                         degrees.                                                                Ruy1995 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.31 +/- 1.64, 5.27, and 2.88 Msun, respectively.             Mlk2012 
00516+0735   GWP  93     XMI 153.                                                                Tob2012b
00516-7354   OGL  95     SMC103.1.11891 + SMC103.1.11996                                         Pli2012 
00517-1600   GWP  94     ABL  82.                                                                Tob2012b
00519+3750   GIC  15     G132-035/G132-036.                                                              
00519-1553   GWP  95     ABL  83.                                                                Tob2012b
00519-5921   HJ 3404     LDS  28.                                                                        
00520+3353   HJ  628     Possibly the same a STF  66 with an error of 2 deg in dec.                      
00520+2035   GIC  16     G069-027/G069-029.                                                              
00521-1925   RSS  44     CPD-20@105                                                                      
00522-2237   STN   3     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
00522-3534   BRT3373     A likely plate flaw.                                                    Grv2021b
00523-7224   DBR 236     DBR 237.                                                                        
00523-7252   OGL  96     SMC100.4.53934 + SMC100.4.11604                                         Pli2012 
00523-7350   OGL  97     SMC103.2.6804  + SMC103.2.6864                                          Pli2012 
00524-6930   DUN   2     lam 1 Tuc. B is CPD-70@38.                                                      
                         SHY 390. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         Both A and B are above MS by 2 mag! The parallax can't be wrong.        Tok2014d
                         RMK   1. Rectilinear solution by Letchford et al. (2018).               LRR2018a
00527-2400   BU  734     A is a spectroscopic binary.                                                    
00528+5638   BU    1     This is a trapezium system (Abt 1986) which lies at the center of the   AbH1986 
             ABH   5     cluster IC 1590 at a distance of 2.94 +/- 0.15 kpc (Guetter & Turner            
                         1997 AJ 113, 2116).  All four components were observed and appeared to          
                         be single.                                                              Msn1998a
             BU    1     AD: HJL  10.                                                            HJL1986 
00528+0111   LDS9104     Old LDS6104.                                                                    
00528-7308   OGL  98     SMC100.3.19805 + SMC100.3.19803                                         Pli2012 
00529-0038   LDS  29     NLTT 2925/2926                                                          Chm2004 
00529-0856   LDS3208     NLTT 2931/2928                                                          Chm2004 
00531+6107   BU  497     A is a spectroscopic binary.                                                    
00533+0405   A  2307     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 7.12 +/- 2.18, 3.24, and 1.40 Msun, respectively.             Mlk2012 
00534-4114   CPO  24     LDS  30.                                                                        
00535+2536   BRT 119     00535+2537POU  73                                                               
                         Primary an eclipsing binary of W UMa-type, period 0.345575 day.         Zas2013 
00535-0041   TOB 359     Pair found when 00536-0039HDO  38 misidentified.                        Dam2015c
00536-0039   HDO  38     Primary is galaxy LEDA 1137438.                                                 
00537+1758   GWP  97     XMI 154.                                                                Tob2012b
00537-3722   BRT1581     A likely plate flaw.                                                    Grv2021b
00537-7236   OGL  99     SMC101.2.48111 + SMC105.6.27571                                         Pli2012 
00540-2503   HJ 3407     B is CD-25@344, spectrum F2V.                                                   
00541+2615   LDS3210     NLTT 2989/2990                                                          Chm2004 
00542+5108   HU 1018     Rectilinear solution by Scardia et al. (2017).                          Sca2017c
00543-7358   OGL 100     SMC107.7.2     + SMC107.7.62                                            Pli2012 
00545+5619   CTT   2     B component is BD+55@196.                                                       
00545-7230   OGL 101     SMC105.5.24224 + SMC105.5.24308 + SMC105.5.25393                        Pli2012 
00546+3910   STF  72     B is BD+38@139.                                                                 
00546+1911   STT  20     66 Psc.                                                                 Wor1956b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.70 +/- 1.01, 4.39, and 2.57 Msun, respectively.  Mlk2012 
00547-6558   LDS9105     Old LDS6105.                                                                    
00547-7129   OGL 102     SMC109.6.11    + SMC109.6.145                                           Pli2012 
00547-7229   OGL 103     SMC105.5.24345 + SMC105.5.160                                           Pli2012 
00548+0857   GWP 100     XMI 155.                                                                Tob2012b
00548-6727   GLI   7     B is CPD-68@33.                                                                 
00548-7303   OGL 104     SMC106.5.28410 + SMC106.5.28476                                         Pli2012 
00548-7358   OGL 105     SMC107.7.205   + SMC107.7.460                                           Pli2012 
00549-3615   BRT1582     A likely plate flaw.                                                    Grv2021b
00550+5858   BU 1098     ups 1 Cas = 26 Cas                                                              
00550+2406   ENG   3     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2013).                         USN2013a
00550+2338   STF  73     36 And.                                     One component is                    
                         variable. A combined photometric/polarimetric/speckle spectroscopic             
                         analysis of this system was made by Tamazian et al.                     Tam2000 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Subgiant stars, spectral types G6 and K6. Calculated mass sum is 1.86           
                         +/- 0.15 Msun, in reasonably agreement with these classifications.      Mut2010b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.86 +/- 0.14, 2.29, and 1.35 Msun, respectively.  Mlk2012 
             FOX 115     AB,C: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
00552-4724   CD-48  216  HD 5388 was known to have a companion thought to be a planet candidate          
                         of minimium mass M sin i = 1.96 Mjup. Sahlmann et al. (2011) derive a           
                         combined astrometric/spectroscopic orbit, using values of P,e,T, and            
                         omega from the spectroscopic orbit of Santos et al. (2010 A&A 512,              
                         A47). They determine the orbit is nearly face-on, yielding an                   
                         estimated mass for the companion of  69 +/- 20 Mjup. Thus it can no             
                         longer be considered a planet.                                          SaJ2011b
00552-7401   OGL 106     SMC107.7.14    + SMC107.7.241                                           Pli2012 
00553-7318   OGL 107     SMC106.6.7246  + SMC106.6.7641                                          Pli2012 
00554+4611   ES 1298     The angle for 1914 has been increased 100 degrees.                              
                         The 1914 Espin measure is probably in error by 100deg.                  Cou1955c
00554+1545   LDS2801     LDS3212.                                                                        
00554+1253   GWP 103     XMI 156.                                                                Tob2012b
00556-4316   CBL 115     May be the omitted CPO  25.                                                     
00557+5748   ES  405     Motion for component B relative to A reflects the proper motion of A            
                         to within the errors. Therefore, in spite of the fact the small proper          
                         motions of these two components are similar, we consider their                  
                         physical relationship to be in doubt.                                   Kiy2012 
00557-7145   OGL 108     SMC109.8.11703 + SMC109.8.11918                                         Pli2012 
00558-1832   B   645     Probable rapid motion, but little observed.                                     
00559+5937   STI 146     Rectilinear solution by Hurowitz et al. (2013).                         USN2013a
00560-7155   OGL 109     SMC108.5.26777 + SMC108.5.26787                                         Pli2012 
00561+5406   A  1259     Rectilinear solution by Rica & Zirm (2012).                             FMR2012i
00561-8237   WHI   3     Possibly resolved                                                       Whi1991 
00564+0548   GWP 105     XMI 157.                                                                Tob2012b
00565+5928   ES 1709     STI 95 is identical                                                     Hei1983a
00566+1040   STF  76     ET Psc, W Uma (EW) type eclipsing binary, P = 0.439298 d.               Zas2011 
00566-1614   HJ 2002     Evidently a mistake in position angle by Herschel (HJ).                         
00566-5633   LPO   1     Spectral type G5?                                                               
00567+6043   BU 1028     gam Cas = 27 Cas                                                                
                         A is nova-like variable. Photocentric motion of (probably) the Aa pair          
                         detected by Gontcharov et al.                                           Gon2001 
                         1975.636: Disk unresolved in H alpha emission and H beta.               Bla1977a
                         Very small relative motion of B despite the high proper motion of A             
                         reveals this as a common proper motion companion.                               
                         AD: The D component is the A component of 00568+6022.                   Mam2017 
00568+6022   BU 1099     Theta for 1979.7703 incorrectly given as 308.6 in McAlister & Hendry    McA1982d
                         (1982). Also, the measure for 1979.7730 was a spurious preliminary              
                         measure of the observation on 1979.7703, and has been deleted.                  
                         The A component is the D component of 00567+6043.                       Mam2017 
             BAG  10     Aa,Ab: The primary is 4.24d SB2 (Young, Pub DAO Victoria 1, 287, 1921;          
                         F.C. Fekel, personal comm.). HR  266.                                           
                         Astrometric binary (P=4.85yr) discovered in residuals to speckle                
                         data for 83-year AB pair (Cole et al. 1992), as well as in residuals    CWA1992 
                         to SB orbit.                                                                    
                         The Ab component is a 4.2d pair consisting of a B9V and A7V.            Tok2021b
00568+3830   HJ 1057     mu And = 37 And                                                                 
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
00568+1525   GWP 106     XMI 158.                                                                Tob2012b
00568-7210   OGL 110     SMC108.7.49889 + SMC108.7.49890                                         Pli2012 
00569+6152   HJ 1056     Aka STI 149.                                                                    
00570+5729   ES   44     Not the same as 00591+5729STI1500                                               
00570-7315   OGL 111     SMC106.6.41340 + SMC106.6.16701 + SMC106.6.15030                        Pli2012 
00572+2325   FOX 116     eta And = 38 And. A is a spectroscopic binary, P = 115.7d.                      
             MKT   2     Hummel et al. (1993) orbital elements were derived from Mark III        MkT1993b
                         interferometer astrometry. Combined with spectroscopy by Gordon (1946           
                         ApJ, 103, 13) to yield masses and distance.                                     
                         Errors are given as "error ellipses"; these values are tabulated                
                         below. Columns include date (BY), major and minor axes of the ellipse           
                         (mas), and ellipse orientation (deg):                                           
                              1990.5359     0.57     0.04     107.1                                      
                              1990.5687     0.12     0.02     105.8                                      
                              1990.5742     0.17     0.02     105.2                                      
                              1990.6125     0.43     0.05     102.7                                      
                              1990.6262     0.12     0.03      98.5                                      
                              1990.6426     0.09     0.02      96.9                                      
                              1990.6563     0.08     0.02      93.3                                      
                              1990.6591     0.06     0.01      85.7                                      
                              1990.6646     0.24     0.02      81.0                                      
                              1990.6673     0.06     0.02      82.2                                      
                              1990.6728     0.09     0.03     100.6                                      
                              1990.6837     0.61     0.09      78.9                                      
                              1990.7056     0.08     0.02      92.4                                      
                              1990.8233     0.08     0.02      98.0                                      
                              1991.6037     0.22     0.04     105.1                                      
                              1991.6557     0.10     0.02      88.5                                      
                              1991.6584     0.12     0.03      98.1                                      
                              1991.7077     0.10     0.03      96.5                                      
                              1991.7104     0.08     0.02      99.7                                      
                              1991.7132     0.05     0.01      84.4                                      
                              1991.7460     0.08     0.02      84.3                                      
                              1992.6413     0.19     0.03      85.5                                      
                              1992.6441     0.56     0.05      96.3                                      
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 3.88 +/- 0.22, 5.02, and 2.63 Msun, respectively.  Mlk2012 
00573+6020   ARG   3     B is BD+59@149.                                                                 
00573+2518   POU  79     LDS 871.                                                                        
00573+1100   ITF  49     Aka ITF  94.                                                                    
00574+2053   J  2587     BRT2300.                                                                        
00576-7131   OGL 112     SMC109.3.163   + SMC109.3.288                                           Pli2012 
00577+0441   GWP 107     AB: XMI 159AB.                                                          Tob2012b
             GWP 108     AC: XMI 159AC.                                                          Tob2012b
00577-7326   OGL 113     SMC106.7.19223 + SMC106.7.12940                                         Pli2012 
00578-7346   OGL 114     SMC107.5.14324 + SMC107.5.14471                                         Pli2012 
00580-7306   OGL 115     SMC106.5.52673 + SMC106.5.51760                                         Pli2012 
00586+4709   BRT  73     The 1893 observation differs substantially from modern observations.            
                         Either the 1893 observation is erroneous (which we consider the most            
                         probable), or there exist perturbations in the system. The question of          
                         the physical relationship of this system remains open.                  Kiy2012 
00587-7144   OGL 116     SMC109.1.23    + SMC109.1.460                                           Pli2012 
00587-7207   OGL 117     SMC108.3.6583  + SMC108.3.6695                                          Pli2012 
00588+1044   GWP 109     XMI 160.                                                                Tob2012b
00588-7149   OGL 118     SMC109.1.85    + SMC109.1.231                                           Pli2012 
00589+3230   SEI  10     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
00589+0339   GWP 110     XMI 161.                                                                Tob2012b
00591+5824   STI1501     Rectilinear solution by Hurowitz et al. (2013).                         USN2013a
00591+5729   STI1500     Not the same as 00570+5729ES   44.                                              
00592-1211   LDS3217     NLTT 3252/3253                                                          Chm2004 
00593+0706   GWP 111     XMI 162.                                                                Tob2012b
00593-0040   A  1902     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.23 +/- 0.70, 2.54, and 1.20 Msun, respectively.             Mlk2012 
00593-7142   OGL 119     SMC109.2.9765  + SMC109.1.13352                                         Pli2012 
00594+0047   STF  80     B is BD+00@158.                                                                 
                         AB: Additional notes may be found in Holden (1972).                     Hln1972 
                         A: In addition to the linear solution for the resolved pair,                    
                         astrometric orbits have been computed for an unseen close companion to          
                         A. Dommanget give two orbits calculated from perturbations seen to the          
                         rectilinear motion.                                                     Dom1969 
00595+3202   SEI  11     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
00596-0111   A  1903     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.31 +/- 0.60, 2.11, and 0.95 Msun, respectively.  Mlk2012 
00596-7549   GLI   8     B is CPD-76@82, spectrum G0/2V.                                                 
00598+0629   KUI   4     The primary is variable, WW Psc.                                                
00599-7146   OGL 120     SMC109.1.13337 + SMC113.6.34323                                         Pli2012 
00599-7208   OGL 121     SMC108.3.14363 + SMC108.3.15476                                         Pli2012 
00599-7410   OGL 122     SMC107.1.178   + SMC107.1.218                                           Pli2012 
01000+5702   MLR 626     Also known as TDS1710.                                                          
01000-7234   OGL 123     SMC105.4.9983  + SMC105.4.11297                                         Pli2012 
01001+4443   STF  79     164 And. Both A and B are spectroscopic binaries.                               
                         H N  45.                                                                MEv2010 
                         T0 converted from negative to positive by subtracting from P.           FMR2020c
01001+1246   GWP 113     XMI 164.                                                                Tob2012b
01001-7135   OGL 124     SMC109.2.10029 + SMC109.2.10470                                         Pli2012 
01002+5809   SKF  56BC   Aka MRI  25.                                                                    
01005-1923   SHY 392     HIP   4702 + HIP   4833.                                                        
01006+6027   BAG  36     Primary is the alpha2 CVn type variable V551 Cas.                               
01006-7343   OGL 125     SMC107.4.12713 + SMC107.3.646                                           Pli2012 
01007-7250   OGL 126     SMC105.2.10999 + SMC105.2.12098                                         Pli2012 
01007-7328   OGL 127     SMC106.2.10337 + SMC106.2.11173                                         Pli2012 
01008-7400   OGL 128     SMC107.2.7090  + SMC107.2.7244                                          Pli2012 
01010-7154   OGL 129     SMC108.4.34907 + SMC108.4.34906                                         Pli2012 
01011-7119   OGL 130     SMC114.5.140   + SMC114.5.363                                           Pli2012 
01012+3704   BRT2585     ALI 254.  Also known as TDS1720.                                                
01012-5610   HJ 3412     B is CPD-56@199.                                                                
01013+1745   GWP 116     XMI 165.                                                                Tob2012b
01014+3535   COU 854     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.42 +/- 1.13, 2.60, and 1.10 Msun, respectively.             Mlk2012 
01014+1155   BU  867     Misidentified in BDS and ADS. Corrections by Baize and Couteau.                 
                         A premature orbit has been calculated.                                          
01014-7120   OGL 131     SMC114.5.22    + SMC114.5.226                                           Pli2012 
01014-7210   OGL 132     SMC113.7.22785 + SMC113.7.22807                                         Pli2012 
01015+6922   A  2901     1984.9965: This autocorrelogram was remeasured; the new results are             
                         listed in catalog.                                                              
01015+1024   GWP 117     XMI 166.                                                                Tob2012b
01016+5339   HJ 2008     01015+5339SMA  11                                                               
01016-1630   LDS9107     Old LDS6107.                                                                    
01017+4635   A   927     BRT  75                                                                         
01017+2518   HDS 134     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.80 +/- 0.47, 2.33, and 2.40 Msun, respectively.             Mlk2012 
                         A: Teff = 5625+/-75 K, log g = 3.75+/-0.25, R = 2.75+/-0.30 \rsun,      AlW2014 
                            Mv = 2.99+/-0.30, M = 1.60+/-0.20 \msun, L = 15.84+/-1.60 \lsun              
                         B: Teff = 5575+/-75 K, log g = 3.75+/-0.25, R = 2.65+/-0.30 \rsun,              
                            Mv = 3.12+/-0.30, M = 1.46+/-0.20 \msun, L = 15.83+/-1.60 \lsun              
01018-0652   LDS  33     NLTT 3377/3378                                                          Chm2004 
01019+1405   GRV 984     Typo in original WDS designation - entered as 01010+1405.                       
01020+0214   LDS3221     LDS5310.                                                                        
01020-7201   OGL 133     SMC113.6.22750 + SMC108.3.39755                                         Pli2012 
01020-7304   OGL 134     SMC106.4.40341 + SMC111.5.15843                                         Pli2012 
01021-1516   LDS9108     Old LDS6108.                                                                    
01023+8153   KNT   1     A is an Algol-type eclipsing binary, U Cep, P =19.3d.  There is                 
                         circumstellar matter.                                                           
01023+1131   PLQ  11     LDS1085.                                                                        
01023+0552   A  2003     Close, 0.2" or under. Position angles show large changes. A premature           
                         orbit has been computed.                                                        
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.79 +/- 1.16, 2.45, and 1.05 Msun, respectively.             Mlk2012 
01024+0504   HDS 135     Mean motion indicates P ~ 80 yr, rho decreasing.                        Msn1999b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.13 +/- 0.11, 1.39, and 1.35 Msun, respectively.  Mlk2012 
             WNO  50     AC: GJ 3071 + GJ 1027. CPM pair.                                        Mkr2008 
01025+0933   GWP 119     XMI 167.                                                                Tob2012b
01025-7353   OGL 135     SMC107.3.8839  + SMC112.6.180                                           Pli2012 
01026+6221   WNO  51     GJ 49 + GJ 51. CPM pair.                                                Mkr2008 
01027+0908   RAO  39     RoboAO finds 2 companions - Optical?  2MASS: B at 32.4" 145.3d, below   RAO2015 
                         the MS, optical? Tokovinin & Lepine (2012) miss AB but list an optical  Tok2012c
                         companion at 1733".                                                     Tok2014d
                         AB: A is SB2 with P = 26.2 days (Griffin & Suchkov 2003). The tertiary  Grf2003 
                         companion B at 2".8 did not move substantially in a year since its              
                         discovery by Riddle et al. (2015), but the PM of the main component A   RAO2015 
                         is small and the astrometry is not conclusive. B is located below the           
                         MS on the CMD, although still within the errors of its photometry.              
                         Considering the small field crowding, we count B as likely physical.    Rbr2015d
01028+3148   sig Psc     Combined spectroscopic/interferometric solution (Palomar Testbed        Knc2004 
                         Interferometer) by Konacki & Lane (2004), yielding distance = 112.9             
                         +/- 0.9 pc, masses 2.65 +/- 0.27 and 2.36 +/- 0.24 Msun, spectral               
                         types B9.5V, diameters 0.16 and 0.15 mas.                                       
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 8.19 +/- 0.87, 5.71, and 2.40 Msun, respectively.             Mlk2012 
01028+0049   LDS5311     Error in WDS designation - incorrect precession of Luyten coordinates?  Luy1984 
01029+5148   BU 1161     Rectilinear solution by Rica & Zirm (2012).                             FMR2012i
01029+4702   GIC  17     G172-034/G172-035. The A component is the variable star V359 And.               
                         NLTT 3437/3438                                                          Chm2004 
01029+4121   HJ 1064     39 And.                                                                         
01029+0753   OCC 480     eps Psc                                                                         
                         NPOI Limb-darkened diameter 1.74 +/- 0.10 mas,                          NOI1999 
                         R = 10.9 +/- 0.8 \rsun.                                                         
01030+4723   STT  21     A may be a spectroscopic binary.                                                
                         Measures attributed to this pair are actually of 01006+4719 = MAD   1.  Mad1856 
                         Error identified by Wilfried Knapp.                                     Bu_1883 
01030-0450   BUP  13     25 Cet.                                                                         
01031-7358   OGL 136     SMC112.7.5     + SMC112.7.92                                            Pli2012 
01032+7113   JNN 250     LHS 1182. Estimated age 1000-10000 Myr; masses 0.21 +/- 0.04 and 0.13           
                         +/- 0.02 Msun; a ~2.7 au.                                               Jnn2014 
01032+6032   MLB  43     This is a physical pair, with relative motion much smaller than the             
                         proper motions. Relative motion may be affected by a perturbation in            
                         the radial direction with a period of 25y.                              Kiy2012 
01032+2006   LDS 873     NLTT 3462/3463                                                          Chm2004 
01033-6006   HJ 3416     Spectrum F6/8III/IV.                                                            
01033-7123   OGL 137     SMC114.5.6465  + SMC114.6.10201                                         Pli2012 
01035+5019   STF  83     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2013).                         USN2013a
01035-0535   RST4162     J 1442.                                                                         
01036-5516   DLR   1     AB is a low-mass binary with masses 0.19 +/- 0.02 and 0.17 +/- 0.02             
                         Msun. At a distance of 47.2 +/- 3.1 pc the projected distance between           
                         the stars is 12au.  They are orbited by an L-type companion at 84au,            
                         which shares common proper motion.  The companion is either a 12-13             
                         Mjup planet (assuming an age of 20 Myr) or a 14-15 Mjup brown dwarf             
                         (for an age of 50 Myr).                                                 Dlr2013 
01036-7138   OGL 138     SMC114.7.13732 + SMC114.8.18665                                         Pli2012 
01037+4051   LDS3225     AB: Also known as GIC  18.                                                      
                         BC: NLTT 3481/3482                                                      Chm2004 
                         BC: Aside from the companion seen in the AstraLux images, there is an           
                         additional possible wide companion at 26" separation, as noted in the           
                         WDS. The wide components have very similar proper motions (e.g. Roser   XXX2010 
                         et al. 2010), so actual companionship seems probable.                   Jnn2012 
             BWL   5     AD:  Colors and/or astrometry are inconsistent with a late-type common          
                         proper motion companion based on visual inspection of the field from            
                         2MASS, SDSS, DSS1, and/or DSS2. Primary is G 132-50.                    Bwl2015 
01037-3024   B   649     CI Scl, Algol-type eclipsing binary, P = 14.7104 d.                     Zas2011 
                         B is a close 14.7-d spectroscopic pair.                                 Tok2019a
01037-7138   OGL 139     SMC114.7.13496 + SMC114.7.13580                                         Pli2012 
01037-7158   OGL 140     SMC113.5.9293  + SMC113.5.9288                                          Pli2012 
01038+2232   J   874     J measures a pair 1912 - 1917: 345@, 3".                                        
                         Measures and magnitude differences discordant.                          J__1949a
                         Companion has variable magnitude.                                       Cou1952a
01038+0122   STF  84     26 Cet.                                                                         
             STF  84     AB: H 4  83.                                                            MEv2010 
             BU 1355     AC: 1909 and 1921 measures disagree. BDS 494 same star.                         
01039-7255   SKF1068     OGL 141. SMC110.8.23710 + SMC110.8.23860                                Pli2012 
01040+3528   HO  213     A premature orbit has been calculated.                                          
01040-6409   B  1913     Spectrum composite: K0III/IV+A/F.                                               
01040-7134   OGL 142     SMC114.7.14379 + SMC114.6.11666                                         Pli2012 
01040-7401   OGL 143     SMC112.7.11    + SMC112.7.755                                           Pli2012 
01041+4408   UC  493     Not a CPM pair. The A component is a close double, leading to a                 
                         spurious proper motion (Skiff, private comm.).                                  
01042+2256   GIC  19     G069-044/G069-043.                                                              
                         NLTT 3529/3528                                                          Chm2004 
01044-0518   STF  85     Probably the same as STF 211 with a 1 hr error in RA.                           
01044-4703   UC  495     AB and BC are probably not CPM pairs. The proper motion of the B                
                         component was effected by a nearby bright star (Skiff, private comm.).          
01047+0401   GWP 126     XMI 168.                                                                Tob2012b
01047-3929   GJ 9037     Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from the Geneva           
                         Extrasolar Planet Search Programs home page.                            HaI2001 
01048+0135   A  2310     Position angles vary widely. A premature orbit has been calculated.             
01048-0528   STF  86     AB: H 3  73.                                                            MEv2010 
01049+3649   A  1515     Periods from 86 to 419yr have been calculated. Possibly ambiguous case          
01050+2119   LDS3228     NLTT 3570.  White dwarf pair = WD 0102+21 = EGGR 462/463                Grn1986 
01050-7132   OGL 144     SMC114.3.186   + SMC114.3.569                                           Pli2012 
01051+3814   J  1804     ALI 488.                                                                        
01051+1457   HJ 1068     72 Psc. A is a spectroscopic binary.                                            
01052+1250   HJ   10     Primary is eclipsing binary of Algol-type, period 1.62785 d.            Zas2012 
01053-7331   OGL 145     SMC111.8.20419 + SMC111.8.20441                                         Pli2012 
01055+8315   MLR 482     Also known as TDS  39.                                                          
01055+4928   ES 1206     1deg error in IDS led to similar error in WDS designation.                      
01055+1523   STF  87     NLTT 3597/3598                                                          Chm2004 
                         The B component may be a spectroscopic pair.                            Tok2019b
01055-7215   OGL 146     SMC113.2.30    + SMC113.2.126                                           Pli2012 
01056+4927   OSO  12     G172-038. Neither is a common proper motion pair, based on color and            
                         comparison with POSS2 red plates                                        Oso2004 
01056-7342   OGL 147     SMC112.5.12714 + SMC112.5.12879                                         Pli2012 
01057+3304   MLB 444     Rectilinear solution by Cvetkovic et al. (2017).                        Cve2017 
01057+2128   STF  88     psi 1 Psc                                                                       
                         AB: HJL  12.                                                            HJL1986 
                         AB: SHY 395. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AB: H 4   9.                                                            MEv2010 
             YR    6     Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 4.29 +/- 0.78, 4.29, and 2.19 Msun, respectively.  Mlk2012 
01058+0455   STF  90     77 Psc. STTA 10. B is BD+04@176.                                                
                         AB: HJL  13.                                                            HJL1986 
                         AB: H 4  68.                                                            MEv2010 
01058-2618   HJ 2014     LDS  34. HIP 5140. See Allen et al. (2000) for information on           AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
01058-5959   R     5     B is CPD-60@75.                                                                 
01058-7150   OGL 148     SMC114.1.170   + SMC114.1.1973                                          Pli2012 
01060+6120   LDS3230     Old LDS6109. Due probably to a typo in the epoch-1900 IDS coordinates,          
                         LDS3230 was originally listed in the WDS as 00055+6119.                         
01060+2456   BRT 122     J 2708.                                                                 J__1955 
01060+1111   BPM  21     [PM2000]   41785 + [PM2000]   41845.                                    Gvr2010 
01061-4643   SLR   1     bet Phe. Variable?                                                              
                         Quoted errors in P and a are +/- 5.0y and +/- 0.016", respectively.     Ary2015b
01062+4508   BRT  76     Algol-type eclipsing binary, period 5.613460 d.                         Zas2019 
01062+3211   S   393     sig 2 Psc                                                                       
                         AB: H 5  16.                                                            MEv2010 
01064+3230   LDS3231     Aka RAO 184.                                                                    
01065+5325   ES  616     One degree error in WDS designation - should be +5425.                          
01065+0154   HDO  42     Doolittle may have measured a different pair (see ADS).                 A__1932a
01065-3055   LDS2167     NLTT 3662/3663                                                          Chm2004 
01065-3441   LDS9110     Old LDS6110.                                                                    
01066+1353   SHY 396     HIP   5207 + HIP   4387.                                                        
01069-1408   GAL 306     Object #34 in Gallo's original list.                                    Gal1912a
01071+1740   BPM  22     [PM2000]   42380 + [PM2000]   42414.                                    Gvr2010 
01072+5752   STI1537     Rectilinear solution by Hurowitz et al. (2013).                         USN2013a
01072+5330   H 4  66     H IV 66.                                                                        
01072+3839   A  1516     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.62 +/- 0.59, 2.89, and 1.10 Msun, respectively.  Mlk2012 
01072-0144   STF  91     B is 2mag above the MS in (K,V-K), on MS in (J,J-K). Wrong 2MASS ptm.           
                         The B component is possibly a SB.                                       Tok2014d
01072-7121   OGL 149     SMC114.4.6097  + SMC114.4.6144                                          Pli2012 
01073+0537   GWP 130     XMI 169.                                                                Tob2012b
01073-3452   COO   6     Rectilinear solution by Friedman et al. (2012).                         USN2012a
01073-7201   OGL 150     SMC113.3.21615 + SMC113.3.21614                                         Pli2012 
01074+0101   LDS5315     Error in WDS designation - incorrect precession of Luyten coordinates?  Luy1984 
01075+4116   RAO  40     Primary is SB, P=49.480d. Estim. mass of B 0.26 Msun.                   Tok2014d
                         Triple system with inner 74.1 day spectroscopic pair (Gorynya &                 
                         Tokovinin 2014 MNRAS 441, 2316) and tertiary from Riddle et al. (2015)  RAO2015 
                         confirmed as physical by our photometry and astrometry. Observations            
                         demonstrate that photometry of B given in 2MASS is biased by proximity          
                         of bright primary, as in many other similar pairs. Their "unusual"              
                         colors derived from the 2MASS photometry are thus wrong.                Rbr2015d
01075+0244   GWP 131     XMI 170.                                                                Tob2012b
01075-4145   LDS9111     Old LDS6111.                                                                    
01076+2257   LDS9112     AB: Old LDS6112.                                                                
                         NLTT 3723/3725                                                          Chm2004 
01078-4129   RST3352     ups Phe. Variable RV suspected. The lines are poor and show a scatter           
                         of 40km/s without apparent relation to the visual motion.                       
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.16 +/- 0.34, 2.78, and 2.09 Msun, respectively.             Mlk2012 
01079-7311   OGL 151     SMC111.3.12611 + SMC111.3.12798                                         Pli2012 
01080+3915   RAO  41     Primary is SB, P=1713d.                                                 Tok2014d
01083+5455   WCK   1     Aa,Ab: mu Cas = 30 Cas. Proper motion of A +3424 -1596 (FK5).                   
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 0.01 +/- 0.01, 1.22, and 0.95 Msun, respectively.  Mlk2012 
                         Aa,Ab : 0.7400 +/- 0.0122, 0.1728 +/- 0.0035 \msun, respectively.       BdH2020 
                         Age estimated as 12.7 +/- 2.7 Gyr.                                              
             mu Cas      Aa,Ab: Astrometric orbit. Spectroscopic elements are somewhat                   
                         different from those of Lippincott: P = 23.0, T = 1954.0, e = 0.30,     Lip1981 
                         omega = 178.0 (Worek & Beardsley 1977).                                 Bey1977 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         The pair has now been resolved by infrared speckle interferometry.      Mcy1983 
                         Pierce & Lavery (1985), Karovska et al. (1986), Haywood et al. (1992),  Pie1985 
                         and McCarthy et al. (1993) all compare their observations with          Kar1986b
                         published orbits and discuss  luminosities and masses of components,    Hay1992 
                         helium abundances, etc.                                                         
                         Hipparcos astrometric solution adopts some elements from the orbit      HIP1997d
                         of Heintz & Cantor (1994).                                              Hei1994b
                         CHARA Array Limb-darkened diameter  0.973 +/- 0.009 mas,                CIA2008d
                         R =  0.791 +/- 0.008 \rsun, Teff = 5297 +/- 32,                                 
                         L =  0.442 +/- 0.014 \lsun.                                                     
                         CHARA Array Limb-darkened diameter  0.972 +/- 0.009 mas,                CIA2012e
                         R =  0.790 +/- 0.009 \rsun, L =  0.428 +/-0.007 \lsun,                          
                         Teff = 5264 +/-  32 K.                                                          
             STT 551     AB: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
01083-3535   FAR   2     SKF 328. Primary is white dwarf WD 0106-358 = GD 683.                   Far2005b
01084+0539   BUP  15     80 Psc. B is BD+04@192.                                                         
             STT 552     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
01084-5515   RST1205     zet Phe. Also known as Wurren.                                          Mam2017b
                         A is an Algol-type system, spectrum composite, P = 1.67d.                       
                         Both B and C are probably physical.                                             
                         Ling (2004) gives a derived orbital parallax 0".01176 and a mass sum    Lin2004a
                         of 7.41 +/- 5.85 Msun                                                           
01085+6331   OSO  13     G243-062. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates. PM of A = +1047 -91.                                  Oso2004 
01086+1652   GWP 135     XMI 171.                                                                Tob2012b
01086+1917   GWP 136     XMI 172.                                                                Tob2012b
01086-1011   BUP  16     eta Cet = 31 Cet. B is BD-10@239.                                               
01088+6145   ES 1945     Aka OL  113.                                                                    
01088-7119   OGL 152     SMC119.5.5     + SMC119.6.162                                           Pli2012 
01089+4512   HJ 2018     AB,C : Same as STF  92.                                                         
01091-7225   OGL 153     SMC118.8.502   + SMC113.1.14118                                         Pli2012 
01092-7127   OGL 154     SMC119.6.1012  + SMC119.6.1006                                          Pli2012 
01093+6234   LDS5179     old LDS6113.                                                                    
01094+3543   BUP9005     A component is NGC 404.                                                 Skf2013 
01094+2949   ALP   4     2MASSW J0109216+294925                                                          
                         Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
01094+0457   GWP 138     XMI 173.                                                                Tob2012b
01094-5636   HU 1342     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.71 +/- 0.86, 2.48, and 1.27 Msun, respectively.             Mlk2012 
01095+4715   STT 515     phi And = 42 And. Measure of 1985.830 made by MAPPIT.                   Han1987 
                         Scardia et al. (2001) orbit considered preliminary.  The real period    Sca2001d
                         is probably long (>400 yr).  The Hipparcos parallax is 0".00443 +/-             
                         0.00080, giving a mass sum of 6.9 Msun, slightly in excess for a                
                         binary of spectral type B7Ve. The dynamical parallax is 0".0033, in             
                         reasonable agreement with the measured one but not acceptable as it             
                         leads to an exaggerated mass sum (16.8 Msun).                                   
                         Calculated mass sum is 6.5  +/- 2.8 Msun, in reasonable agreement with          
                         spectral types B6IV and B9V, although mass is not well-constrained.     Mut2010b
01096+4635   ES 1300     Due to a typographical error in the ADS, the AE, AF, AG, AH, and AI     A__1932a
                         components of 01097+3537 were added as additional components to this            
                         pair (the AE and AI pairs as BAR  66, the others as ES 1300).                   
01096+2802   BRT 123     OL  149.                                                                        
01096-0507   LDS9114     Old LDS6114. LIT   3.                                                           
                         NLTT 3847/3849                                                          Chm2004 
01096-0711   HDS 151     This binary displays clear common proper motion, but the residual               
                         astrometry does not seem to follow a simple trajectory consistent with          
                         only orbital motion of the two visible components. In addition, the             
                         brightness difference is larger than the spectral type difference               
                         would imply at a common distance. This could indicate that the A                
                         component is itself an unresolved binary.                               Jnn2012 
01096-4616   GAA   5     AI Phe.                                                                         
                         Ma,Mb = 1.1941 +/- 0.0007, 1.2438 +/- 0.0007 \msun,                     GaA2019 
                         orbital parallax = 5.905 +/- 0.024 mas.                                         
01097+3537   BAR   1     bet And = 43 And = Mirach                                                       
                         Also, see note to 01096+4635.                                                   
01097+0856   GWP 139     XMI 174.                                                                Tob2012b
01098-2013   HJ 2023     Primary is CT Cet, a W UMa type eclipsing binary, P = 0.25649d.         Zas2012 
01099+1352   BPM  23     [PM2000]   44058 + [PM2000]   44035.                                    Gvr2010 
01100-7327   OGL 155     SMC111.2.5925  + SMC111.2.6033                                          Pli2012 
01101+5145   STT  23     AB: HJL  14.                                                            HJL1986 
01102+2447   POU 107     J 1805.                                                                         
01104-7352   OGL 156     SMC112.3.6394  + SMC117.6.1318                                          Pli2012 
01105+1326   BPM  24     [PM2000]   44379 + [PM2000]   44460.                                    Gvr2010 
01105+1019   GWP 143     XMI 175.                                                                Tob2012b
01107+8021   STF  89     B is BD+79@32.                                                                  
01107-2800   SWR   1     CPM pair                                                                Skf2004 
01108+6747   HDS 155     A spectroscopic double lined orbit has been determined as well.         Grf2012d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.02 +/- 0.23, 2.18, and 2.52 Msun, respectively.             Mlk2012 
01108+5141   DOO   3     BDS 631.                                                                        
01109+0934   HJ  634     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
01111+5509   STT 553     the Cas = 33 Cas. A is a spectroscopic binary,                                  
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
01111+3125   STT  25     82 Psc = g Psc                                                                  
01111-7228   SKF1069     OGL 157. SMC115.5.12    + SMC115.5.319                                  Pli2012 
01112+4113   A   655     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.59 +/- 0.83, 2.76, and 0.95 Msun, respectively.             Mlk2012 
01112+3743   HO  215     45 And. Also single 1903, 1906 (Doolittle), 1907 (Aitken).                      
                         A measure by Schembor (1925.60, 117.8@, 155.5", 6 - 6) belonged to      Sch1927a
                         01107+4256 ENG   4AB instead.                                                   
                         Duplicity of A is questionable.                                                 
01112+1634   GWP 144     XMI 176.                                                                Tob2012b
01114+1526   BEU   2     GJ 3076. WDS designation incorrected entered as 01224+1526.                     
                         Estimated age 10-20 Myr; masses 0.10 +/- 0.03 and 0.04 +/- 0.01 Msun;           
                         a ~5.6 au.                                                              Jnn2014 
01114-7225   OGL 158     SMC118.8.10104 + SMC118.8.10016                                         Pli2012 
01114-7323   OGL 159     SMC116.7.144   + SMC116.7.143                                           Pli2012 
01116+0446   GWP 146     XMI 178.                                                                Tob2012b
01116+1404   GWP 145     XMI 177.                                                                Tob2012b
01117+1205   LDS3242     NLTT 3967/3952                                                          Chm2004 
01119+0455   GIC  20     G002-027/G070-044 = GJ 3077A+3078B.                                             
01120+0642   GWP 149     XMI 180.                                                                Tob2012b
01120+0955   GWP 148     XMI 179.                                                                Tob2012b
01120-7231   OGL 160     SMC115.5.9132  + SMC115.5.9369                                          Pli2012 
01121+6111   KR   10     AC: Doolittle's published position angle was 91.9deg, which does not    Doo1901 
                         match anything in the field. However, an obvious star is visible at             
                         the same separation but 90deg off his theta measure. It is assumed he           
                         made an error when rotating his micrometer.                                     
             SMA9001     AD: Doolittle noted "a 13.5 mag. companion about 7" from A was          Doo1901 
                         suspected on two nights". It is assumed he saw the Smart companion.     Sma1932 
01121+4700   BU  236     Aka HJ 2024.                                                                    
01121-7400   OGL 161     SMC117.7.58    + SMC117.3.98                                            Pli2012 
01125+0228   STT  27     35 Cet                                                                          
01126+1704   NAU   1     The primary is GU Psc, a likely member of the young AB Doradus Moving           
                         Group. Spectral types are M3 +/- 0.5 and T3.5 +/- 1. Age of the system          
                         is 100 +/- 30 Myr, distance 48 +/- 5 pc.                                Nau2014 
01129+3205   STF  98     B is BD+31@196a. The primary is a double-lined spectroscopic binary,            
                         P = 2.21d. B may also be an SB (Hube, PASP 93, 490; 1981).                      
                         AB: H 4 120.                                                            MEv2010 
                         SEI  13.                                                                Nsn2017a
01130+3004   STT  26     A is a spectroscopic binary.                                                    
01131+2942   A  1260     Angle increasing, with a probable close approach about 1950.                    
01131+1141   HD  7275    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
01131-7215   OGL 162     SMC118.2.51    + SMC118.2.127                                           Pli2012 
01132-7400   OGL 163     SMC117.7.3315  + SMC117.7.3338                                          Pli2012 
01133-0152   HIP   5697  The SB1 orbit suggests mass ratio q > 0.2 and axis 0".21. The companion         
                         is probably just a bit too faint or too close to be resolved with NICI. Tok2012a
01134-3932   SHY 397     HIP   5709 + HIP   5490.                                                        
01134-7251   OGL 164     SMC115.2.45    + SMC115.2.260                                           Pli2012 
01135-3821   BRG   4     The primary star in the system is a known eclipsing binary with a               
                         period of 0.4455 days (Parihar et al. 2009 MNRAS 395, 593). Since the           
                         angular separation is inside of our inner cut-off, we count the system          
                         as a binary here for the purpose of multiplicity statistics, although           
                         it is really a triple system. To estimate the mass of the primary for           
                         the purpose of deriving the mass ratio to the tertiary component                
                         detected in our images, we use the sum of the masses corresponding to           
                         individual spectral types M1 and M3 derived for the eclipsing binary.   Jnn2012 
                         ASAS J011328-3821.1, eclipsing binary of Algol-type, period 0.44559d.   Zas2016 
01136+2825   HJ  635     Previously erroneously listed as 01126+2825.  Also known as GRV  73.            
01137+2435   STF  99     phi Psc = 85 Psc. A is a spectroscopic binary.                                  
01137+0735   STF 100     zet Psc = Revati.                                                               
                         Both A and B are spectroscopic and occultation binaries, B has P=9.08d.         
                         AB: HJL  15.                                                            HJL1986 
                         AB: H 4   8.                                                            MEv2010 
             BU 1029     BC: Delta m given in ADS is greatly overestimated.                      Wor1967b
                         BC: Rectilinear solution by Rica & Zirm (2012).                         FMR2012i
01137-5040   HJ 3421     B is CD-51@312.                                                                 
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
01139+1004   GWP 154     XMI 181.                                                                Tob2012b
01141+1698   87 Psc      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Stickland & Weatherby (1984).                                           Stc1984 
01141+0634   LDS3248     LDS5323.                                                                        
01142-4041   B  2554     Hipparcos suspected non-single.                                                 
01144-0755   STFA  3     37 Cet = LDS3250. B is BD-08@215.                                               
                         NLTT 4123/4121                                                          Chm2004 
                         AB: GJ 9045 A+B. CPM pair.                                              Mkr2008 
                         AB: H 5  24.                                                            MEv2010 
01144-7319   OGL 165     SMC116.3.3     + SMC116.3.954   + SMC116.6.11112                        Pli2012 
01145-0503   ROL   1     Primary is exoplanet host, periods 1275d, 4046d.                        Tok2014d
             RGS   1     Aa,Ab: HD 7449 has a close massive planet (P = 1270.5 +5.92/-12.1d,             
                         a =  2.33 +0.01/-0.02 au, mass >1.09 +0.52/-0.19 Mjup) as well as a             
                         more distant stellar companion. The Ab component is likely an M4-M5             
                         dwarf. Rodigas et al. (2016) estimate P = 65.7 +227/-56y, a =  17.9             
                         +32/-12.9 au, i = 59.7 +20.1/-25.8 deg, mass = 0.23 +0.22/-0.05 Msun.   Rgs2016 
01146-7402   OGL 166     SMC117.7.3320  + SMC117.7.3907                                          Pli2012 
01148+6056   BU 1100     The quadrant interpretation by Zulevic is less likely.                  Zul1972a
                         Muller corrected an error in his elements (Ephem. Cat. 1964).           Mlr1955b
                         One component is a SB, P = 5.33d.                                               
                         Only elements P, T, and a have been amended by Starikova (1977) from    Sta1977a
                         the orbit of Zulevic (1972).                                            Zul1972a
01148+4309   LDS3251     NLTT 4129/4124                                                          Chm2004 
01148-0058   BUP  18     38 Cet.                                                                         
                         A is a blue supergiant with multiple pulsation periods.                 IAU2014e
                         AC: C component is galaxy NGC 442.                                              
01149+3236   SEI  14     None of the components seen on POSS plate; may be flaws on AC Potsdam           
                         plate. The current WDS companion at the position of Scheiner's triple           
                         is probably unrelated to anything seen on the plates.                           
                         AC: SEI  15.                                                            Nsn2017a
01152-3419   LDS 837     LDS5325.                                                                        
01153+6040   LDS5180     old LDS6115.                                                                    
01153+2234   J  3226     BRT2304. Barton lists theta as 226.9; probably typo for 266.9.          Brt1939b
01155+3745   SHY 121     HIP   5881 + HIP   6278.                                                        
                         A: Ren & Fu (2013) calculated an astrometric orbit, combining                   
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Nidever et al. (2002). They derived component masses 0.95 and 0.28      Nid2002 
                         Msun and an estimated semimajor axis of 30.68 mas.                      Ren2013 
01155+0216   CHR 195     First detected as an occultation binary by Evn1983a.                            
01157+0241   GWP 157     XMI 182.                                                                Tob2012b
01157+0032   LDS5326     Error in WDS designation - incorrect precession of Luyten coordinates?  Luy1984 
01158+4702   LAW   9     LSPM J0115+4702S. Law et al (2008) derive a distance of 18.7 +9.3/-3.6  Law2008 
                         pc and a projected separation of 5.2 +2.9/-0.9 au. Estimated spectral           
                         types are M4.5 and M5.                                                          
                         In addition to the companion detected with AstraLux, it can be noted            
                         that 2MASS J01154885+4702259 has a very similar proper motion to the            
                         star J01155017+4702023 at just 27" separation (Roser et al. 2010),      XXX2010 
                         which is itself a close binary (Law et al. 2008). Thus, this is a very  Law2008 
                         likely quadruple system.                                                Jnn2012 
01158+0947   A  2102     Quadrant change. Not seen 1948 - 1954.                                          
01158-6853   HJ 3423     kap Tuc = LDS  42.                                                              
             I    27     HJ 3423 and I 27, separated by 320" are kap Tuc.                        Sca1981a
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Mass = 1.35, 0.88, 0.86, 0.80 \msun for A, B, C, D, respectively.       Tok2020d
                         Teff = 6513, 5145, 5062, 4850 K for A, B, C, D, respectively.                   
                         Physical quintuple the period of A,CD is suggested to be ~270 kyr.              
01158-7224   OGL 167     SMC118.1.5565  + SMC118.1.6020                                          Pli2012 
01160+5849   STI1550BC   Aka MRI  29.                                                                    
01160+1534   GRV 986     SLW  58.                                                                        
01162-7246   OGL 168     SMC115.2.6083  + SMC115.2.6082                                          Pli2012 
01163+1243   BPM  25     [PM2000]   47807 + [PM2000]   47744.                                    Gvr2010 
01163-2056   LDS  41     NLTT 4238/4239                                                          Chm2004 
01163-3217   LDS1091     LDS5327.                                                                        
01166+7402   HJ 2028     STTA 13.                                                                        
01166+1831   HDS 169     A: Ren & Fu (2013) calculated an astrometric orbit, combining                   
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Latham et al. (2002). They derived component masses 1.06 and 0.28 Msun  Lat2002 
                         and an estimated semimajor axis of 14.81 mas.                           Ren2013 
01166+1507   GWP 161     XMI 183.                                                                Tob2012b
01166-0230   BU 1358     39 Cet. A semiregular variable, AY Cet, and spectroscopic binary, P =           
                         56.8d. Radio flares and soft X-rays are observed, and a white-dwarf             
                         companion is revealed by IUE observations.                                      
01167-7142   OGL 169     SMC124.7.387   + SMC124.7.163                                           Pli2012 
01168+2643   BRT3257     Originally published as BRT 124.                                        Brt1928 
01170-7311   OGL 170     SMC116.3.7036  + SMC116.3.7122                                          Pli2012 
01171+1739   BPM  26     [PM2000]   48328 + [PM2000]   48320.                                    Gvr2010 
01171-7355   OGL 171     SMC117.3.682   + SMC117.3.1102                                          Pli2012 
01172+0930   GWP 164     XMI 184.                                                                Tob2012b
01172+0201   HDO  45     Rectilinear solution by Mason et al. (2012).                            WSI2012 
01175+0131   GWP 165     XMI 185.                                                                Tob2012b
01176+4018   A  1521     Rapid change, but the measures are inadequate to define the motion.             
01177+2647   BRT3258     Originally published as BRT 125.                                        Brt1928 
01177-7150   OGL 172     SMC124.8.4147  + SMC124.8.4560  + SMC124.8.4191                         Pli2012 
01178+4945   HU  520     Quadrant indeterminate.                                                         
01178+4901   HJ 2033     Ea : Also known as STF 102 ET.                                                  
01179-7314   OGL 173     SMC116.3.7181  + SMC116.3.7479                                          Pli2012 
01180+0037   GWP 167     XMI 186.                                                                Tob2012b
01181+4707   A   937     North preceding and slightly brighter of a finder pair. Narrow                  
                         apparent orbit.                                                         B__1963b
01182+5742   STI1556     Rectilinear solution by Hurowitz et al. (2013).                         USN2013a
01182+1409   BPM  27     [PM2000]   48977 + [PM2000]   49004.                                    Gvr2010 
01182-7136   OGL 174     SMC124.7.4469  + SMC124.7.4898                                          Pli2012 
01184-2332   LDS2182     Appears to be same as SKF1373. Primary is B component of 01183-2330             
                         SKF1372; pair moved to become AC pair (with quadrant flip).                     
01185+7323   A   814     Not separated about 1951 (Van Biesbroeck). Possible quadrant change.    VBs9999 
01186+3855   GIC  21     G132-069/G132-068.                                                              
                         NLTT 4342/4337                                                          Chm2004 
01186-2255   FAR  24     Primary is white dwarf WD 0116-231.                                     Far2006 
01187-0052   HJ 5453     LDS  43. HIP 6130. See Allen et al. (2000) for information on           AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
                         AB: NLTT 4362/4361                                                      Chm2004 
             EGN   1     Aa,Ab pair bound. Colors of Ab component consistent with M2-M5 dwarf,           
                         with mass 0.24 +/- 0.01 Msun.  B component is K7 dwarf and shares               
                         CPM with A. C component is likely a background star.                    Egn2007 
01187-2249   HDO  47     Probably = HDO 48.                                                              
01188+3724   STF 108     The A component is a spectroscopic binary.                                      
01188-5637   RST  29     Spectral type G5?                                                               
01191-7215   OGL 175     SMC123.7.2850  + SMC123.7.2849                                          Pli2012 
01192+5821   STI1560     B is BD+57@248.                                                         FMR9999 
01192-4338   B  1423     Zurlo et al. (2013) estimate the period of this system at ~300y, in an          
                         eccentric orbit with a semi-major axis of ~50au. The companion is               
                         likely a white dwarf.                                                   Zur2013 
01194+6418   MLB 186     TDS1841.                                                                        
01194+1158   BPM  28     [PM2000]   49715 + [PM2000]   49656.                                    Gvr2010 
01194-7129   OGL 176     SMC124.3.274   + SMC124.3.22                                            Pli2012 
01194-7246   OGL 177     SMC120.7.5025  + SMC120.8.5604                                          Pli2012 
01194-7359   OGL 178     SMC122.7.221   + SMC122.7.232                                           Pli2012 
01195+5816   ES  408     CD component also known as STI1562                                              
01195+1850   GWP 169     XMI 187.                                                                Tob2012b
01195-7205   OGL 179     SMC123.6.2701  + SMC123.6.3359                                          Pli2012 
01196-0520   A   313     Only elements P and T have been amended by Starikova (1977) from the    Sta1977a
                         orbit of Heintz (1968).                                                 Hei1968a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.39 +/- 1.07, 2.59, and 1.10 Msun, respectively.             Mlk2012 
01197+1209   CHR 196     First detected as an occultation binary by Africano.                    Afr1975 
01197-7203   OGL 180     SMC123.6.2671  + SMC123.6.3140                                          Pli2012 
01198-0031   STF 113     42 Cet.                                                                         
                         AB: Absolute quadrant for 1998.657 determined by triple-correlation             
                         techniques.                                                             Pru2002b
                         A,BC. 1985.8430: This autocorrelogram was remeasured; the new results           
                         are listed in catalog.                                                          
                         Star A (mag. 6.3, G8III) is in slow direct motion at 1.6" separation.           
                         T incorrectly given as 1992.52 by Baize (1990); should be 1993.02       Baz1990a
                         (erratum noted in Inf. Circ. 111, 1990)                                         
             FIN 337     BC: 1982.7629, 1982.7657, 1983.7106: A mistake in reduction resulted in         
                         90 degree errors for these three measures.                              McA1987b
                         BC: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.79 +/- 0.56, 3.32, and 1.20 Msun, respectively.  Mlk2012 
01198-7157   OGL 181     SMC123.5.2462  + SMC123.5.2499                                          Pli2012 
01199+0350   CHE  29     BAL2084.                                                                Hln1972 
01200+5747   STI1571     Aka LYS   5. Identity not recognized due to large pm affecting pa.              
                         Rectilinear solution by Hurowitz et al. (2013).                         USN2013a
01200-1549   HJ 2036     A is an SB. Binary or triple?                                           Tok2014d
01201+5814   H 3  23     H III 23. phi Cas = 34 Cas. A is a spectroscopic binary.                        
                         A quintuple system. C has spectral type B5/6Ia/be.                              
01201+3900   GIC  22     G132-071/G132-072.                                                              
                         NLTT 4410/4412                                                          Chm2004 
01203-0933   LDS9116     Old LDS6116.                                                                    
01203-4841   HJ 3428     B is CD-49@378.                                                                 
01204+0937   GWP 171     XMI 188. BVD  15.                                                       Tob2012b
01205+0418   J  1807     BAL 2085.                                                                       
01205-1957   TOK 203     Two astrometric orbits are derived by Goldin & Makarov (2006), the      Gln2006 
                         longest one has P = 8.93 yr, axis 55 mas, and e = 0.84.                 Tok2012a
                         Retrograde motion by 4deg since first resolution in 2011. Goldin &              
                         Makarov (2006) propose two orbits with periods ~9yr; semi-major axis    Gln2006 
                         should then be 0".15, so the system is near apastron.                   Tok2013b
01207+0333   GWP 172     XMI 189.                                                                Tob2012b
01207-7145   OGL 182     SMC124.1.101   + SMC124.1.545                                           Pli2012 
01208+1127   AG   17     LDS 878. B is BD+10@167.                                                        
                         HJL  17.                                                                HJL1986 
01208+1035   PLQ  13     B is BD+09@153.                                                                 
                         HJL  16.                                                                HJL1986 
01211+6439   S   397     35 Cas. STTA 15 = H 5  81.  B is BD+63@175.                                     
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
01211+1540   J   227     B is variable                                                           Cou1952a
01211+0736   SLE 257     The primary is a W UMa system, AQ Psc.                                          
01211-0403   LDS3267     G 271-42.                                                                       
01211-3508   LDS5330     Aka LDS9117 the old LDS6117.                                                    
01211-7251   OGL 183     SMC120.2.15    + SMC120.2.163                                           Pli2012 
01211-7305   OGL 184     SMC121.5.2620  + SMC121.5.3200                                          Pli2012 
01212+5159   NLTT 4450   Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by Latham et          
                         al. (2002). They derived component masses 1.21 and 0.26 Msun and an     Lat2002 
                         estimated semimajor axis of 35.17 mas.                                  Ren2013 
01212+4108   LDS3266     NLTT 4468/4469                                                          Chm2004 
01213+1132   BU    4     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         The Hipparcos parallax (0".00616 +/- 0.00141) yields a mass sum of      Sca2001d
                         4.7 Msun, in excess for a binary of type F1III.                                 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 9.73 +/- 6.50, 3.62, and 1.64 Msun, respectively.  Mlk2012 
01215-2908   RUC   1     BE Scl. Spectral type of resolved companion estimated at G5-8V.         Ruc2007 
01218-2408   SEE  13     Motion direct. A premature orbit has been computed.                             
01219-4003   WG    8     BRT 643.                                                                Brt1933 
01220+1848   GWP 175     XMI 190.                                                                Tob2012b
01220-6943   I   263     A premature orbit has been computed. Motion direct.                             
01221-2654   LDS2189     NLTT 4564/4566                                                          Chm2004 
01223+0331   DEA  38     NLTT 4558 + 2MASS J01221697+0331235. Baron et al. (2015) estimate               
                         spectral types G5 and L2 +/- 1, distances 58 +/-3 and 43 +13/-40 pc,            
                         masses 1.05 -1.12 and 0.071-0.076 Msun.                                 BFr2015 
01223-7332   OGL 185     SMC121.1.5     + SMC121.1.187                                           Pli2012 
01226+1200   GWP 178     XMI 191.                                                                Tob2012b
01227+1410   GWP 179     XMI 192.                                                                Tob2012b
01227+0032   LDS3270     Aka WNO  42.  G 70-55.                                                          
01227-7258   OGL 186     SMC120.1.13    + SMC120.1.32                                            Pli2012 
01228-2440   BWL  63     Bowler et al (2013) derive the following properties: age 120+/-10 Myr,          
                         distance 36+/-4 pc, masses 0.40+/-0.05 Msun and 12-14 or 23-27 Mjup.    Bwl2013 
01230-1258   GAL 307     LDS  46. Object #40 in Gallo's original list.                           Gal1912a
             KUI   6     BC: BC shares CPM with A.                                               B__1963b
01230-3035   LDS2190     According to Richard Jaworski the precise position he determine may be  Jaw2006 
                         correct if Luyten's original separation is off by an order of                   
                         magnitude (i.e., 11.8" rather than 118").                                       
01232+4905   KU    8     HU 524.                                                                         
01233+0152   LDS5332     CVR  26.                                                                        
01233-0209   LDS3271     NLTT 4616/4615                                                          Chm2004 
01233-2105   LDS2191     NLTT 4626/4625                                                          Chm2004 
01233-7256   OGL 187     SMC120.1.3850  + SMC120.1.4139                                          Pli2012 
01234+5809   STF 115     First measured by F.W. Struve in 1836 at an angular separation of       Hrt1989 
                         0".68, this system had opened to 1".2 by 1910, then steadily closed             
                         to 0".35 at the time of the first speckle measurement in 1978.                  
                         The pair reached an apparent minimum separation of 0".01 in the                 
                         spring of 1984.                                                                 
                         1983.7107  This autocorrelogram was remeasured; the new results are             
                         listed in the catalog.                                                          
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.36 +/- 0.67, 2.80, and 1.20 Msun, respectively.  Mlk2012 
01235-7356   OGL 188     SMC122.3.2     + SMC122.3.173   + SMC122.5.71                           Pli2012 
01236+3415   CRJ   4     NLTT 4619. The A component is SB, P=83.9d. Primary is G8IV. The 0.3"            
                         companion is physically associated with primary, based on multi-epoch           
                         astrometry. The estimated spectral type of the companion ~M1V, its              
                         mass > 0.297 Msun.                                                      CrJ2013 
01236+0753   GWP 180     XMI 193.                                                                Tob2012b
01237+3743   CIA  15     47 And.                                                                         
                         Mass = 1.636 +/- 0.050, 1.587 +/- 0.049 \msun for A and B.              CIA2020a
                         Radius = 1.84 +/- 0.05, 1.66 +/- 0.12 \rsun for A and B.                        
                         Teff = 7280 +/- 110, 7280 +/- 120 deg K for A and B.                            
                         Age = 1.0 Gyr, distance = 61.7 +/- 0.7 pc.                                      
01237-6217   RST  31     Spectral type G0?                                                               
01239+0050   GWP 182     XMI 194.                                                                Tob2012b
01239-7228   OGL 189     SMC120.4.3345  + SMC120.4.3627                                          Pli2012 
01240-0800   HJ 1079     44 Cet. A is a Delta Scuti-type variable, AV Cet.                               
01240-0811   BU  505     the Cet = 45 Cet.                                                               
01240-2933   LDS2192     NLTT 4676/4656                                                          Chm2004 
01241-1244   GAL 308     Object #42 in Gallo's original list.                                    Gal1912a
01242+1254   HJ   13     C component is galaxy NGC 514.                                                  
01243+0426   GWP 183     XMI 195.                                                                Tob2012b
01243-0655   BU 1163     The system is also detected as a spectroscopic binary.                  B__1951a
                         Only elements P, T, and a have been amended by Starikova (1978) from    Sta1978c
                         the orbit of van den Bos (1961).                                        B__1961e
                         This system underwent periastron in late 1988, an event now covered by          
                         speckle observations.                                                   Hrt1992b
                         A combined visual-spectroscopic orbit by Morbey (1975) gives almost     Mrb1975 
                         the same elements, but in the representation of position angles         Sod1999 
                         Soderhjelm's elements are preferable.                                           
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.59 +/- 0.41, 2.74, and 1.30 Msun, respectively.             Mlk2012 
01245+3902   STTA 17     B is BD+38@256.                                                                 
                         D is BD+38@253.                                                                 
01245+1740   BPM  29     [PM2000]   52622 + [PM2000]   52637.                                    Gvr2010 
01245-2839   LDS2194     NLTT 4694/4695                                                          Chm2004 
01245-3356   JAO   1     Aa,Ab: GJ 2022 = G274-024                                                       
                         Daemgen et al. derive a distance of 12.6 +/- 2.3 pc, a separation for           
                         the AC pair of 26.0 +/- 4.8 au, and a predicted orbital period of 330           
                         +95/-93 yr. Spectral types for both components are M5.0 +/- 0.5;                
                         masses are 0.14 +0.03/-0.02 and 0.13 +0.03/-0.02 Msun.                  Dae2007 
01246+5311   ES 2583     B is BD+52@332.                                                                 
01247-7402   OGL 190     SMC122.2.45    + SMC122.2.104                                           Pli2012 
01248-2614   RST1218     LDS 3277.                                                                       
                         NLTT 4714/4713                                                          Chm2004 
01250+1424   GWP 185     XMI 196.                                                                Tob2012b
01251+4537   A   939     Recent observations seem to rule out Muller's short-period              Mlr1955a
                         alternative.                                                                    
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.54 +/- 1.99, 3.23, and 1.45 Msun, respectively.             Mlk2012 
01252-0412   HJ  638     01252-0409BU 1361                                                               
                         J  1445.                                                                Nsn2016 
01252-7954   HJ 3443     B is CPD-80@23.                                                                 
01253-5930   HJ 3435     B is CPD-60@111.                                                                
01254+0227   GWP 186     XMI 197.                                                                Tob2012b
01256+3133   STT  30     AC: HJL  18. Aka MAD   9.                                               HJL1986 
                         AC: SHY 402. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         STTA 18.                                                                        
                         B is above MS (wrong ptm), while A and C are on it. C is SB2,           HJL2012b
                         P=14.908d (Halbwachs et al. 2012)                                       Tok2014d
01256+2331   TOK  11     Primary is 5.4d SB1. Estimated period of visual pair 880y.              Tok2006 
01257+0258   J  1899     BC: Error in coordinates listed in Jonckheere (1941), star is at        J__1941a
                         1h 23.2m, not 0h 23.2m.  Star of mag 7.3 at 131" is BD+02  207.         J__1952 
01257+0107   GWP 188     XMI 199.                                                                Tob2012b
01257+0611   GWP 187     XMI 198.                                                                Tob2012b
01258+6014   BUP  19     del Cas = 37 Cas = Ruchbah. A spectroscopic and (perhaps) eclipsing             
                         binary.                                                                         
01259+6808   BU 1101     psi Cas = 36 Cas.                                                               
             H 5  83     H V 83, SHJ 18, STF 117. C is BD+67@124.                                        
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
01260+1450   BPM  30     [PM2000]   53515 + [PM2000]   53480.                                    Gvr2010 
01261+0925   GWP 189     XMI 200.                                                                Tob2012b
01261-2618   SWR   2     CPM pair                                                                Skf2004 
01262+3435   WSI  96     Provisionally designated WSI9101.                                       Tok2010 
                         The initial observations of WSI 96 by Mason et al. (2011) are           Msn2011d
                         considered spurous. The pair resolved by Roberts et al. (2015) using            
                         AO is believed to be a different pair, whose magnitude difference               
                         would have been beyond the dm limit of speckle. The original WSI 96             
                         designation was retained, however. Spectral types of the components             
                         are estimated as F7V and M2V, masses as 1.4 and 0.4 Msun.               Rbr2015b
01263+0711   LDS9118     Old LDS6118.                                                                    
01263-0440   TOK 204     Possible physical companion at 24".4, 227deg in 2MASS.                  Tok2012a
                         Direct motion by 20deg since first resolution in 2011, at constant              
                         separation. Estimated period ~10yr. The small RV amplitude suggests an          
                         orbit in the plane of the sky.                                          Tok2013b
01264+5929   STI 213     STI1607.                                                                        
01265+1812   HDS 187     Also a spectroscopic binary with P = 3087d which cannot be the visual   Grf2015b
                         pair.                                                                           
01267-7408   OGL 191     SMC122.1.1145  + SMC122.1.1144                                          Pli2012 
01269-5023   ART   1     Low-mass wide double, discovered on 2MASS and Digital Sky Survey                
                         frames. Artigau et al. determine sectral types M6.5V +/- 0.5 and M8V    Art2007 
                         +/- 0.5, distances 63 +/- 5 and 61 +/- 6 pc. Based on evolutionary              
                         models, the masses are 0.095 +/- 0.005 and 0.092 +/- 0.005 Msun for an          
                         age > 1Gyr, or 0.020 +/- 0.003 and 0.019 +/- 0.003 Msun for and age             
                         ~30Myr. The projected separation is ~5100 au.                                   
01270+1500   GWP 190     XMI 201.                                                                Tob2012b
01270+1200   LDS3282     G002-038. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc. Also known as LIT   5.                   
                         NLTT 4817/4814                                                          Chm2004 
01270-0009   STF 125     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
01270-3058   RSS   3     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
                         SHY 403. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
01270-3233   LDS2199     Some unconfirmed early observations. A is the semiregular variable              
                         R Scl.                                                                          
01270-7405   OGL 192     SMC122.2.1199  + SMC122.2.1250                                          Pli2012 
01271-5158   SHY 404     HIP   6772 + HIP   6804.                                                        
01274-0204   J  1446     BAL 6.                                                                          
01274-2220   RST2261     CD-22@503.                                                                      
01275+1546   BPM  31     [PM2000]   54366 + [PM2000]   54359.                                    Gvr2010 
01276+6429   TDS1882     CD: Originally 01276+6430 TDS1882; primary found to be C component of           
                         01276+6429.                                                                     
01276+0402   GWP 192     XMI 202.                                                                Tob2012b
01277+6321   STI 215     MLB 382.                                                                        
01277+4524   BU  999     ome And = 48 And                                                                
                         This cannot be the close 254.9-d spectroscopic binary.                  Grf2011b
                         Although the pair has been repeatedly resolved with the CHARA Array             
                         with the Separated Fringe Packet technique, a full solution is not      CIA2010 
                         yet complete.                                                                   
             CIA   4     Aa,Ab: Combined solution by Farrington et al. (2014) yields masses              
                         0.993 +/- 0.056 and 0.888 +/- 0.058 Msun, as well as an orbital                 
                         parallax 39.12 +/- 1.97 mas (compared with the Hipparcos parallax of            
                         34.94 +/- 3.1 mas).                                                     CIA2014a
             BU   82     CD: There is a faint star between the AB and CD pairs. The change in            
                         AC is due to the proper motion of A. This is common to AB.              Bu_1894 
01277+1620   BPM  32     [PM2000]   54497 + [PM2000]   54549.                                    Gvr2010 
01277+0521   BU 1164     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.51 +/- 0.76, 2.67, and 1.05 Msun, respectively.  Mlk2012 
01278+5928   STI1618     STI 217.                                                                        
01281-5238   CVN   2     Both the B and C companions are probably background objects.            Cvn2005a
01282+1244   GWP 193     XMI 203.                                                                Tob2012b
01283+5329   STF 123     AB: Also known as HU 1651, but the 1911 Hussey measure has a quadrant           
                         flip and a large sep error.                                             Hu_1911 
01283+1731   GWP 194     XMI 204.                                                                Tob2012b
01283+1429   AG   18     B is BD+13@217.                                                                 
01283-1615   LDS3284     NLTT 4889/4888                                                          Chm2004 
01284+0758   S   398     STTA 19. B is BD+07@214.                                                        
                         HJL  19.                                                                HJL1986 
01284+0758               A hierarchical quadruple. AB is a wide binary with an estimated period  Tok2020h
                         of 300k years; the Ba,Bb pair has an estimated  period of about 200             
                         years and the close Ba1,2 pair has a spectroscopic orbit of 116d.               
01284-4319   gam Phe     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Luyten (1936).                                                          Luy1936 
01287-4710   LDS  48     Aka UC  562.                                                                    
01289+0633   PLQ  16     LDS3285.                                                                        
01290+7412   HJ 2045     LDS1529.                                                                        
                         A is above MS, B on the MS. A component possibly a close double         Mkr2005 
                         (Makarov & Kaplan 2005) but nothing on the close sub-system in SIMBAD.  Tok2014d
01291+2143   HO    9     BC: According to Griffin, the radial velocities of B and C differ by    Grf1987c
                         30km/sec. Either the pair is optical, or one component is a                     
                         spectroscopic binary.                                                           
                         AB and AD: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         AD: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
01291+1040   GWP 195     XMI 205.                                                                Tob2012b
01292+4820   BWL   6     AC: Source appears spatially extended; probably a background galaxy.            
                         Primary is G 172-56.                                                    Bwl2015 
01295+6319   MLB 330     This pair was purged from an earlier edition of the WDS as it was not           
                         found by Heintz. It has apparently been located. It and the nearby              
                         MLB 329 are in NGC 559.                                                 Hei1985a
01295+3054   BUP  20     B is BD+30@229.                                                                 
01296-2138   SEE  14     48 Cet.                                                                         
01297+4228   ZUC   6     SKF 314.                                                                        
                         Primary is white dwarf WD 0126+422 = GD 13.                             Zuc1992 
01297+2250   A  1910     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 6.11 +/- 1.86, 4.31, and 2.09 Msun, respectively.  Mlk2012 
01298+1014   CHR 197     First detected as an occultation binary by Africano.                    Afr1977b
01299+3100   ENG   6     B is BD+30@232.                                                                 
01300-2231   I   445     A,BC = LDS  51.                                                                 
01302+0609   STH   6     A: mu Psc = 98 Psc                                                              
01305-4242   I  1609     SY Phe, an Algol-type eclipsing binary, P = 5.27095d.                   Zas2012 
01306-4446   DHI   1     At a distance of 40 +/- 14pc, the projected physical separation is 130          
                         +/- 50au. Spectral types are M9.0 +/- 0.5 and L6 +/- 1. Dhital et al.           
                         conclude the pair is physical.                                          Dhi2011 
01307-1227   GAL 309     Object #45 in Gallo's original list.                                    Gal1912a
01309+5244   GIC  23     G173-002/G173-003.                                                              
                         NLTT 4991/4993                                                          Chm2004 
01312+7016   38 Cas      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Wright & Pugh (1954).                                                   Wri1954 
01315+1521   BU  506     eta Psc = 99 Psc. A is a Beta CMi-type variable.                        Baz1964 
                         NPOI Limb-darkened diameter 2.64 +/- 0.11 mas,                          NOI1999 
                         R = 26. +/- 2. \rsun.                                                           
01316-1901   HJ 2052     B is BD-19@263. BDS 796, HJ 3373 same star.                                     
01317+6103   STF 128     STI 227.                                                                        
01317+1506   CHR 198     First detected as an occultation binary by Beavers.                     Bvr1977 
01319+1603   BF Psc      Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Griffin (1975).                                                         Grf1975a
01319+1026   GWP 196     XMI 206.                                                                Tob2012b
01320-1604   GAL 310     Object #46 in Gallo's original list.                                    Gal1912a
01321+1657   STF 132     A is a spectroscopic binary, P = 36.6d.                                         
                         A: SB2. Combined orbit including RV data and Hipparcos Intermediate             
                         Astrometric data. Semimajor axis derived from photocentric a0 plus              
                         stellar evolutionary model. Derived properties for A and B:                     
                         M/Msun = 1.14 + 1.02, L/Lsun = 5.40 + 1.41, dm = 1.46 mag,                      
                         log age = 9.86.                                                         WaX2015b
                         Improved SB2 orbit for the unresolved pair.                             Kie2018 
                         A: Teff = 5367 +/- 166 K, B: Teff = 5150 +/- 228.                               
                         AB: H 4 130.                                                            MEv2010 
                         AB, AC, and AD: Optical pairs, based on study of relative motion of             
                         the components using the method of apparent motion parameters.          Kiy2008 
                         AC: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
01321+1434   BPM  33     [PM2000]   57016 + [PM2000]   57059.                                    Gvr2010 
01323-2633   ARG   4     B is CD-27@523.                                                                 
01325+1645   BPMA  1     [PM2000]   57224 + [PM2000]   57397.                                    Gvr2010 
01325+1417   LDS1102     NLTT 5103/5102                                                          Chm2004 
01326-2745   LDS2206     NLTT 5136/5135                                                          Chm2004 
01326-4944   SHY 405     HIP   7189 + HIP   7086.                                                        
01327+6336   EVS   9     Primary is the Cepheid V636 Cas.                                        Evs2016a
01327-0139   FIL   2     B is BD-02@235.                                                                 
01328+3551   STF 133     Confusion between C and D in ADS. With quadrant for CD north preceding,         
                         AC obviously has greater separation than AD.                            B__1962d
                         Identifications of several later AC and AD measures were switched to            
                         give motion consistent with earliest measures. Quadrants were flipped           
                         for CD measures, which now agree with AC and AD measures. AC has                
                         smaller separation than AD, and C is slightly brighter than D.                  
             A  1911     Ea,Eb: Originally 01238+3553; found to be E component of 01328+3551.            
01329+1954   LDS3289     NLTT 5133/5127                                                          Chm2004 
01329+1200   GWP 197     XMI 207.                                                                Tob2012b
01329-3652   GC 1881     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
01330+1027   GWP 198     XMI 208.                                                                Tob2012b
01331-0602   LDS3290     NLTT 5155/5154                                                          Chm2004 
01331-1951   LDS1103     NLTT 5163/5169                                                          Chm2004 
01332+6041   STF 131     Spectrum of B: B3IV.                                                            
01332+3231   SEI  17     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
01333-0014   UC  582     aka ITF  47.                                                                    
01333-2411   LDS2209     NLTT 5178/5160                                                          Chm2004 
01335+6039   BUP  22     B is BD+59@273.                                                                 
01337-1213   HWE   4     The linear formula by Job & Tamburini seems ruled out, as it makes      Job1969b
                         the current quadrant opposite to what is observed.                              
01338+0346   RBR  32     Suspected non-single.                                                   Hor2002b
01343-0827   A   314     Derived orbital parallax 0".00978, mass sum 4.14 +/- 2.34 Msun          Lin2004a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.85 +/- 0.99, 2.60, and 1.20 Msun, respectively.             Mlk2012 
01344+4844   ES 2587     G172-061. Not a common proper motion companion after comparison with            
                         POSS2 red plates                                                        Oso2004 
01344-1607   FAR  25     Primary is white dwarf WD 0131-163.                                     Far2006 
01345+1448   LDS9119     Old LDS6119.                                                                    
01347+0720   GWP 199     XMI 209.                                                                Tob2012b
01348+2935   BRT   5     An Algol-type system, RS Tri.                                                   
01349+1234   STF 136     AB: H 4 131.                                                            MEv2010 
01349-6909   GLI  12     B is CPD-69@74.                                                                 
01350-2955   BU 1000     AB,C triple+var solution (AB in HIP).                                   Sod1999 
                         B is 0.47d eclipsing binary (= BB Scl).                                         
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
01352-1829   RSS  49     CPD-19@169                                                                      
01354+6305   MLB 280     Also classified K1V.                                                            
01354+4123   ES 1494     Probably identical with ADS 1241 ( = ALD).                                      
01356+6117   STI 237     This and STI 239 are members of the multiple system HJ 1083.                    
01360+2646   BU  507     Morlet et al. note that this has similar position angle, separation,            
                         and delta-m as HDS 212. HDS 212 removed.                                Mor2000 
01360+0739   STF 138     D is BD+06@245.                                                                 
                         AB: H N  92.                                                            MEv2010 
01361-2954   HJ 3447     tau Scl. Arend orbit rejected from Fourth Orbit Catalog                 Ard1968 
                         ("orbit completely faulty and irreparable")                             Wor1983 
01361-3718   HJ 3448     Spectral type of A may be K. B is CD-37@605.                                    
01364+7909   STF 127     B is BD+78@50.                                                                  
01364+3209   SEI  18     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
                         The faint pair now measured for the lost SEI  18 may be this new pair.  Dam2017a
01368+4124   BUP  23     ups And = 50 And = Titawin. A is a spectroscopic binary.                        
                         AB: exoplanets with P=4.61d, 237.7d, 1302d, 3848d                       Tok2014d
             LWR   1     AD. Determined to be CPM pair from examination of POSS I and II plates          
                         (epochs 1953 and 1995), plus 2MASS. Conclude spectral type of                   
                         companion M4.5V.                                                        Lwr2002 
                         AD: Raghavan et al. (2010) consider D physical, high PM (no PM given).  Rag2010 
                         CHARA Array Limb-darkened diameter  1.114 +/- 0.009 mas,                CIA2008c
                         R =  1.631 +/- 0.014 \rsun.                                                     
             ups And     A: Combined solution, based on reduction of Hipparcos intermediate              
                         astrometric data together with spectroscopic elements from Butler       CPS1999b
                         et al. (1999).                                                          HaI2001 
             BUP  23     AB: Rectilinear solution by Rica et al. (2017).                         FMR2017b
01368+4124   STT 554     AC: Rectilinear solution by Rica et al. (2017).                         FMR2017b
01371+1209   VSC   1     = pi Psc = 102 Psc.                                                             
01372+1147   TOB9002     Measured as HJ   16 but actually an anonymous pair added here.          Tob2012b
01373+1828   GWP 204     XMI 210.                                                                Tob2012b
01374+2510   G034-039    Boden et al. (2006) give combined spectroscopic/interferometric         Bod2006 
                         solution, including PTI observations. Derive distance of 42.23 +/-              
                         0.21 pc (pi = 23.68 +/- 0.12 mas), age 9.12 +/- 0.25 Gyr, with                  
                         abundances near solar. The K0IV primary appears to have evolved off             
                         the MS and is traversing the Hertzsprung gap toward red giant phase.            
                         Masses are 1.072 +/- 0.014 and 0.8383 +/- 0.0081 Msun, luminosities             
                         2.451 +/- 0.041 and 0.424 +/- 0.023 Lsun, radii 2.048 +/- 0.081 and             
                         0.887 +/- 0.071 Rsun.                                                           
01374-8217   GLI  14     Spectrum G5III:+K1/2.                                                           
01375-1135   LDS9120     Old LDS6120.                                                                    
01376+2233   STTA 20     B is BD+21@218.                                                                 
                         Pair appears in an appendix list, not part of discoverer's regular              
                         numbering sequence.                                                             
01376+1727   GWP 205     XMI 211.                                                                Tob2012b
01376+0709   PLQ  19     HJL  21.                                                                HJL1986 
01376-0645   BRG   5     BC: Initially entered as WDS 01369-0648, the primary of BRG 5 was               
                         later found to be the B component of 01376-0645 CAB 3.                          
01376-0924   KUI   7     1982.7657: This autocorrelogram was remeasured; the new results are             
                         listed here.                                                            McA1987b
                         Combined spectroscopic/visual orbit, also yielding orbital parallax             
                         and component masses and absolute magnitudes.                           Tok1993 
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Martin et al. (1998) derive component masses 1.712 +/- 0.296 and                
                         1.140 +/- 0.226 Msun.                                                   Mig1998 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.51 +/- 0.43, 2.49, and 1.13 Msun, respectively.             Mlk2012 
01377+4825   HDS 215     Rectilinear solution by Hartkopf & Mason (2013).                        Hrt2013b
01377-5714   KRV  54     alp Eri = Achernar                                                              
                         Ma = 6.0 +/- 0.6, Mb = 2.0 +/- 0.1 \Msun, Ra = 8.14 +/- 0.26, Rb = 1.70         
                         +/- 0.08 \Rsun, Teff_a = 15539 +/- 438, Teff_b = 9064 +/- 624 K, La =           
                         3493 +/- 429, Lb = 17.5 +/- 5.1 \Lsun.                                  Krv2022 
01379-8259   TOK 426     HIP 7601 is a nearby (27pc) dwarf also known as GJ 67.1 or HR 512.              
                         According to Wichman et al. (2003 A&A, 400, 293), it is a young                 
                         spectroscopic triple detected in X-rays (1RXS J013755.4-825838). GCS            
                         also recognized the star as SB2. Spectroscopic monitoring (Tokovinin,           
                         in preparation) shows that all three components are similar stars of            
                         approximately one solar mass. Here we resolved the outer subsystem AB           
                         and observed its fast motion. In fact it was already resolved at SOAR           
                         on 2011.036 at 221.0deg and 0".044, but this low-quality observation            
                         has not been published. The available data indicate that the period             
                         of AB is 1.35years; the pair completed nearly two revolutions since             
                         its first resolution in 2011.                                           Tok2015c
01380+4600   HJ 2063     Aka A   944AB,C.                                                                
01385+7302   HJ 2054     40 Cas.                                                                         
01386-4113   CPO 110     B is CD-41@445.                                                                 
01387+0359   GWP 208     XMI 212.                                                                Tob2012b
01387-4515   HJ 3451     LDS  55.                                                                        
01388-1758   LDS 838     LUY 726-8. L 726-8 = UV Cet. Both components are active flare stars             
                         According to Harrington & Behall the mass ratio is 0.487 +/- 0.011 and          
                         the individual masses are 0.115 (0.008) 0.109 (0.008) Msun for A & B,           
                         respectively.                                                           Hrr1973 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         This pm star with flare characteristics is a difficult object.          VBs1954 
                         Magnitude uncertain due to flares.                                      USN1988b
                         AB: Kervella et al. (2016) derive a new orbit for GJ 65 and determine           
                         the following physical parameters:                                              
                            masses (Msun): A = 0.1225 +- 0.0043   B = 0.1195 +- 0.0043                   
                            radii (Rsun):      0.165  +- 0.006        0.159  +- 0.006                    
                            [Fe/H] (dex):     -0.03   +- 0.20        -0.12   +- 0.20                     
                            log (cgs):         5.092  +- 0.015        5.113  +- 0.015            Krv2016 
                         Using the parallax from Gaia DR3 and the mass ratio from Worley,        Gai2018 
                         individual masses of Ma = 0.1191 +/- 0.0018 \msun and Mb = 0.1144 +/-   Wor1973b
                         0.0017 \msun are determined for these components.                       Msn2023 
01388-5327   DUN   4     While this pair appears to have common proper motion and parallax, a            
                         linear solution has been performed and identified therein as optical.   LRR2022c
01393+5257   STF 139     Neither AB, AC or BC are physically associated.                         Kiy2015c
01393+1638   BU    5     103 Psc.                                                                        
01394-1748   HJ 2067     HJ 3380.                                                                        
01397+4602   EGB   1     ES 553.                                                                         
01397-3728   HJ 3452     B is CD-38@572.                                                                 
01398+1704   BPM  34     [PM2000]   61379 + [PM2000]   61385.                                    Gvr2010 
01398-5612   DUN   5     Some measures have been corrected by Andrew James (personal                     
                         correspondance). Note that this is p Eri, not rho Eri                           
                         (03027-0741BU   11).                                                            
                         Measures of 1947.60 and 1947.84 made by triangulation of multiple       Der9999 
                         measures.                                                                       
01399+1515   STF 142     B is BD+14@@251.                                                                
01400+2702   ALP   5     2MASSW J0140026+270150                                                          
                         Companion seen as elongated in I-band image taken at WIYN in August             
                         2002. Physical companionship to this ultracool dwarf ruled out.         AlP2007 
01400-1348   GAL 311     Object #48 in Gallo's original list.                                    Gal1912a
01402+7303   HJ 2055     AB: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
01404+3420   STF 143     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
01405-0917   LDS9121     Old LDS6121.                                                                    
01406+4035   BU 1362     tau And = 53 And. A is a spectroscopic binary. Variable?                        
01409+6410   RAO  32     AC: C component = A component of WDS 01409+6409 TDS1951.                        
01409+6409   TDS1951     Primary = C component of WDS 01409+6410.                                        
01409+1117   A  2320     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.33 +/- 0.76, 2.02, and 0.95 Msun, respectively.             Mlk2012 
01409+4952   HU  531     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.66 +/- 0.98, 2.11, and 0.79 Msun, respectively.  Mlk2012 
01409+0138   A  2404     Quadrant uncertain.                                                             
01410-0524   TOK 228     Primary is EY Cet, variable of BY Dra type, X-ray source                Tok2014d
01412-6741   LDS  56     HIP 7869. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
01413+2545   STF 145     Period of AB estimated at 7300y.                                        Tok2006 
                         Primary is SB2, P=4.435d. Aa,Ab has suspected close tertiary because            
                         K1,K2 are var, e>0. B is SB1, P=1.435d.  RoboAO find a companion to B           
                         (98deg, 4.80", dI=7.2mag), but it is considered optical.                Tok2014d
01413+1246   GWP 214     XMI 213.                                                                Tob2012b
01413+1007   STF 146     B is BD+09@203.                                                                 
                         HJL  22.                                                                HJL1986 
01414+3704   LDS3300     NLTT 5619/5621                                                          Chm2004 
01414-7909   HJ 3467     tau 1 Hyi                                                                       
01417+0712   GWP 215     XMI 214.                                                                Tob2012b
01417-7616   JSP  25     Aka TDS1958.                                                                    
01418+4237   MCY   2     An astrometric binary now resolved by infrared speckle interferometry.          
                         Discovery designation per Todd Henry 03/02/98.                                  
                         Improved pc (Delta m > 6) orbit combining pg (Lippincott 1983) and      Lip1983 
                         Hipparcos obs. Scaling by the speckle IR (Henry 1993) gives orbit size  Hen1993 
                         and mass ratio.                                                                 
                         Martin et al. (1998) derive component masses 0.795 +/- 0.159 and                
                         0.136 +/- 0.053 Msun.                                                   Mig1998 
                         The estimated magnitude difference in V (~6 mag) is too large for the           
                         companion to have been detected.                                        Hrt2009 
                         Mass of A(B) determined to be 0.95+/-0.11(0.254+/-0.019) \msun. Orbital         
                         parallax 79.08 +/- 0.63 mas.                                            Trr2022 
01419-0907   GRV1170     Aka SLW  81.                                                                    
01420+4252   ROE  64     HJL  23.                                                                HJL1986 
01423+5134   CUD   2     Component A is the central star of the planetary nebula NGC 650/1       Skf2013 
                         = Messier 76.                                                                   
01424+2609   BRT3259     Originally published as BRT 126.                                        Brt1928 
01424-0645   A     1     A premature orbit has been computed.                                            
                         Omega corrected from 24.0 to 58.9, omega from 58.9 to 24.0              Ruy1995 
01425+5000   B  2550     BD+49 440 (8.5) and 441 (9.0) are together in a high power field. Both          
                         are close pairs; brighter star is deep orange, the fainter (ADS 1341,           
                         HU 1210) is white. At present the brighter star is the easier pair,             
                         but as its duplicity was missed by Hussey, Aitken, and van Biesbroeck,          
                         then they measured CD, it must have opened out more recently.           B__1963b
01425+2016   HJ 2071     A: 107 Psc.                                                                     
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             107 Psc     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
01426+6033   BU 1363     A 3588-d spectroscopic orbit has been found for the A component.        Grf2012d
                         The primary is the E component of 01426+6033.                                   
01427+0637   J  1808     HJL  24.                                                                HJL1986 
01430+6402   STI 264     Component A is a pulsating star in the open cluster NGC 637. Since              
                         relative motions of all three components are small and in agreement             
                         with each other, we believe all three stars are members of the same             
                         cluster. It is not currently possible to determine whether of not they          
                         form a closed triple system.                                            Kiy2012 
01431+3426   COU 668     Aa,Ab: TDS1964.                                                                 
01431+2101   JNN 251     Estimated age 300-1000 Myr; masses 0.30 +/- 0.06 and 0.15 +/- 0.03              
                         Msun; a ~4.8 au.                                                        Jnn2014 
01432+6056   MLR 106     AC: STI 271.                                                                    
01433+6033   BU 1103     44 Cas. A is a spectroscopic binary.                                            
             FYM 160     AH: Fay (2013) notes an H component in their Figure 1, but does not     FyM2013d
                         include a measurement.                                                          
             ARN  32     AE: E component is primary of 01426+6033 BU 1363                                
01433-1736   HJ 3455     B is BD-18@292.                                                                 
01434-0705   STF 150     B is BD-07@283.                                                                 
01434-1127   GAL 312     Object #50 in Gallo's original list.                                    Gal1912a
01435+5318   HJ 2069     B is BD+52@417.                                                                 
01435-1038   GAL 313     Object #51 in Gallo's original list.                                    Gal1912a
01436+2802   GIC  24     G072-028/G072-029.                                                              
                         NLTT 5738/5740                                                          Chm2004 
01437+5014   CIA   6     Phi Per. Be+sdO binary, resolved by the CHARA Array. The hot subdwarf           
                         companion is detected in near-IR; flux contribution 1.5% in H (dH=4.6)          
                         and restricted fits indicate flux contribution rises to 3.3% (dV~3.7)           
                         in visible.  Combined interferometric/spectroscopic orbital solution            
                         yields masses 9.6+/-0.3 and 1.2+/-0.2 Msun for the Be primary and               
                         subdwarf secondary, respectvely. The inferred distance (186+/-3pc),             
                         kinematical properties, and evolutionary state are consistent with              
                         membership of phi Per in the alpha Per cluster.                         CIA2015a
01437+0934   BU  509     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.69 +/- 0.64, 1.83, and 0.85 Msun, respectively.             Mlk2012 
01438+1954   GWP 216     XMI 215.                                                                Tob2012b
01438+1206   HJ   18     Possibly BD+11@225. BDS 899, HJ 18. HJ position angle in 1820: 220@.            
                         Disagrees with 1912 - 1922: 143@.                                               
01441-1556   BUP  25     tau Cet = 52 Cet. Optical. Proper motion of A -1718 +856.                       
01442-0813   LDS9122     Old LDS6122. Primary is QSO, Z=0.239.                                           
01443+6652   HAU  10     HJL  25.                                                                HJL1986 
01443+5732   BU  870     A premature orbit has been computed.                                            
                         Primary is eclipsing binary V773 Cas (period 2.58734 day).              Zas2010 
                         Light curve and radial velocity combined solution determined.           Zas2017 
             ARN  55     AD: HJL1011.                                                            HJL1986 
01443+0929   KPR   1     AC: Separation may be a factor of 10 too small.                                 
             STF 155     AB: H 2  49.                                                            MEv2010 
01448+5708   B  2548     Rapid motion.                                                                   
                         This close pair precedes BD+56 338 (ADS 1371, BU 453) by 12 sec of              
                         time and is 0.6' north of it. All measures given in Pub Yerkes O. IX,           
                         pt 1 and 2, by van Biesbroeck and myself, assigned to BU 453, are               
                         obviously of the new pair. My estimates of the difference in magnitude          
                         vary between 0.4 sf and 0.7 np, which seems rather large to be error            
                         of estimation, even in so close a pair.                                 B__1963b
01449+2005   109 Psc     Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from Vogt et al.  CPS2000c
                         (2000).                                                                 HaI2001 
01449+1951   A  2322     EU Psc, Algol-type eclipsing binary,  per 1.69261 d.                    Zas2011 
                         Observed wrong star? van den Bos has 4 measures in 1962, and I have     B__1963b
                         positive measure in 1964.                                               Wor1967b
01450+6032   STI 281     AB: BKO1073AC.                                                                  
             MRI  27     AC: BKO1073AB.                                                                  
01450+5707   BU  453     Premature orbits have been calculated. Motion direct.                   Baz1972 
01450+2703   COU 750     Rapid motion.                                                                   
01450-0104   LDS9123     Old LDS6123.                                                                    
                         NLTT 5822/5818                                                          Chm2004 
01452+2317   GIC  25     G034-048/G034-049.                                                              
01454+0909   OCC9041     110 omi Psc = Torcular.                                                         
01454-3957   BRG   6     2MASS J01452133-3957204 has only been observed in one epoch, but the            
                         color and brightness of the detected companion are consistent with              
                         expectation, hence we count it as an unconfirmed binary.                Jnn2012 
01455-6035   JSP9001     Previously known as JSP  13a.                                                   
01456+1148   GWP 217     XMI 216.                                                                Tob2012b
01456-0224   J  1448     BC. Gauchet (1926) measure originally listed as CD pair, with theta     Gau1926a
                         flipped by 180deg.                                                              
01456-2503   HJ 3461     eps Scl. A premature orbit has been computed.                                   
01457+0834   BAG  38     Primary is the alpha2 CVn type variable UZ Psc.                                 
01458+1200   BPM  35     [PM2000]   64864 + [PM2000]   64876.                                    Gvr2010 
01458+0043   GWP 219     XMI 217.                                                                Tob2012b
01459+7142   HJ 1090     01459+7142FOX 119CD. WDS designation for HJ 1090 changed from                   
                         01461+7143 due to inclusion in multiple.                                        
             HJ 1089     AB: Rectilinear solution by Mason et al. (2012).                        WSI2012 
01459-4357   HJ 3463     B is CD-44@509.                                                                 
01460+8005   GW Cep      Multiple system including contact binary.                               Pbl2006 
01460+6113   STF 151     STF 151rej and Duner 1 are identical.                                           
01462+5326   HJ 2079     Confused with nearby 01463+5328 HJ 2080, as pairs are also of similar           
                         separation and position angle.                                                  
01462+3343   HU  804     A premature orbit has been computed.                                            
01463+5328   HJ 2080     Confused with nearby 01462+5326 HJ 2079, as pairs are also of similar           
                         separation and position angle.                                                  
01466+1639   GWP 221     XMI 218.                                                                Tob2012b
01467+0214   GWP 222     XMI 219.                                                                Tob2012b
01469+4234   DUP   1     Dupuy et al. (2015) resolved a low-luminosity T9/Y0 binary, using Keck          
                         laser guide star imaging. Masses are estimated as 4.6 +1.0/-1.1 and             
                         4.3 +1/0/-1.2 Mjup (for age of 1Gyr) or 16.9 +3.8/-4.0 and                      
                         15.9 +3.5/-4.4 Mjup  (for age of 10Gyr).                                Dup2015 
01474+0355   HJ 2084     Aka STT  36.                                                                    
01474-2157   GD 1400     Song et al. (2006) confirm common proper motion of this brown dwarf     Son2006 
                         and its planetary mass companion.                                               
01475-4955   RED  15     2MASS J01473282-4954478. Spectral types M8: and L2:                     Red2006b
01476+3453   CSW   1     AB: This star has a possible wide brown dwarf companion at 43"          Csw2008 
                         separation, according to Casewell et al. (2008).                        Jnn2012 
             KIR   6     BC: B component is an L0.5V brown dwarf. The spectrum of the secondary          
                         shows it to be a background M star.                                     Kir1999 
01477+6351   ENG   7     A is GJ 75 = V987 Cas. B is BD+63@241.                                          
                         AB: Rectilinear solution by Friedman et al. (2011).                     USN2011a
01477+1643   BPMA  2     [PM2000]   65958 + [PM2000]   65844.                                    Gvr2010 
01477-4358   I    52     Gomez et al. (2016) derive dynamical parallax and component masses:             
                         7.50 +/- 0.33 mas, 1.310 +/- 0.032 Msun, 1.128 +/- 0.027 Msun.          Doc2016i
                         A is a close 5.3-d spectroscopic pair.                                  Tok2019a
01478-8011   HJ 3474     tau 2 Hyi                                                                       
01479+4440   A   949     BJN  26.                                                                        
                         This measure was published as BRT 346. Note to BRT 346: This seems to           
                         be ADS 1412, although the magnitude difference is discordant.                   
                         BD+44  369, with which ADS 1412 is identified, was not seen as double.  Brt1939a
01480+4353   ES 1498     BRT 325.                                                                Brt1930 
01481-2533   FAR  26     Primary is white dwarf WD 0145-257.                                     Far2006 
01482+1657   TOK 945     4 Ari.                                                                          
01483+1203   LDS1116     LDS3311.                                                                        
                         NLTT 6012/6013                                                          Chm2004 
01483-4130   RGS   2     GJ 77. Rodigas et al. (2016) detect a companion to the old solar-type           
                         star HD 11112, and determine it is likely a gravitationally bound cool          
                         white dwarf. SED fits (pure-H and pure-He models) suggest a mass for            
                         the companion in the range 0.90-1.08 Msun, Teff 7300-9800K,                     
                         log (L/Lsun) -3.69 - -3.36, and age 2.43-3.92 Gyr.                      Rgs2016b
01486+1618   BU  510     AC: H 5  92.                                                            MEv2010 
01486-0955   JNN  17     LP 708-465.                                                                     
01487+7528   HJ 2075     LDS1540.                                                                        
01487+3306   GIC  26     G072-038/G072-037.                                                              
                         NLTT 6030/6027                                                          Chm2004 
01487-2916   HJ 3466     B is CD-29@590.                                                                 
01488-0125   STF 171     B is BD-02@300.                                                                 
01489+1411   GWP 223     XMI 220.                                                                Tob2012b
01489-2053   ARA1256     Primary is TW Cet, a W UMa type eclipsing binary, P = 0.31685d.         Zas2012 
01489-3153   LDS3316     NLTT 6087/6088                                                          Chm2004 
01491+2956   2M 0149+29  2MASSW J0149090+295613. Astrometric orbit by Harris et al. (2015)               
                         yielded the following properties: spectral types M9.5+L4, absolute J            
                         mags 11.74+13.40, masses 0.084 +/- 0.008 and 0.069 +/- 0.010 Msun.      USN2015 
01491+0236   GWP 224     XMI 221.                                                                Tob2012b
01493+4754   CHR   4     Aa,Ab: Although this new component is indicated as Aa,Ab we have not            
                         firmly established whether it is associated with the A or B component           
                         of the wide pair.                                                       McA1987b
                         B is a spectroscopic binary. The system appears to be quintuple.                
             STF 162     AB: Rectilinear solutions by Zirm & Rica (2014)                         Zir2014b
                         and Genet et al. (2015).                                                GnR2015a
                         Despite the linear solution, proper motion and parallax favor a         Grv2020a
                         physical connection. Long period and/or high eccentricity possible.             
01493+1808   GWP 225     XMI 222.                                                                Tob2012b
01496+1741   GWP 226     XMI 223.                                                                Tob2012b
01496-1041   ENG   8     53 Cet = chi Cet. LDS2222.                                                      
                         SHY   8. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
01497-1414   HU  422     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.42 +/- 0.46, 2.45, and 1.20 Msun, respectively.             Mlk2012 
01498-3824   GC 2219     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
             HDO 186     Additional notes may be found in Herschel (1847).                       HJ_1847b
01499+8053   STT  34     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 14.28 +/- 6.95, 4.72, and 2.24 Msun, respectively.            Mlk2012 
01499+1324   LDS1118     Also known as LDS6124 and LDS9124. Richard Jaworski first               Jaw2006 
                         recognized that these systems were the same.                                    
01500-0408   A  2602     Gomez et al. (2016) derive dynamical parallax and component masses:             
                         15.65 +/- 1.62 mas, 0.748 +/- 0.037 Msun, 0.748 +/- 0.037 Msun.         Doc2016i
01501+3538   ALI  28     No stars seen at AC catalog locations - probably plate flaws.                   
01501+2217   STF 174     1 Ari. Spectrum composite; K1III+A6V. Spectroscopic binary?                     
                         H 1  73.                                                                MEv2010 
01502+1600   BPM  36     [PM2000]   67462 + [PM2000]   67449.                                    Gvr2010 
01503+1146   GWP 227     XMI 224.                                                                Tob2012b
01504+2942   MLB1059     Aka MLB 448.                                                                    
01505-2042   ARA1257     A likely plate flaw.                                                    Grv2021a
01509+1626   BPM  37     [PM2000]   67854 + [PM2000]   67921.                                    Gvr2010 
01509+1031   GWP 228     XMI 225.                                                                Tob2012b
01510+2107   STF 175     AB: H 2  56.                                                            MEv2010 
01511+1135   BPM  38     [PM2000]   68017 + [PM2000]   67969.                                    Gvr2010 
01512+2439   HO  311     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.19 +/- 1.30, 3.38, and 1.40 Msun, respectively.             Mlk2012 
01513+6451   STF 163     B is BD+64@244.                                                                 
01513-3800   LDS9125     Old LDS6125.                                                                    
01514+4329   HJ 2089     B is BD+42@388.                                                                 
01515+0457   STF 177     Formerly, BD+04@320. Corrected by Weis.                                 StF2002 
01515-0744   HIP   8653  Small acceleration of 2 mas yr-2, possibly single.                      Tok2012a
01515-1020   BNU   1     Aa,Ab: zet Cet = 55 Cet = Baten Kaitos. A is a long-period                      
                         spectroscopic binary, P = 1652d, and has been resolved by speckle               
                         interferometry. B is BD-11@360.                                                 
01515-1858   LDS9126     Old LDS6126.                                                                    
01516+1618   BPM  39     [PM2000]   68302 + [PM2000]   68249.                                    Gvr2010 
01518-5458   SHY 128     AC: HIP   8687 + HIP   7387.                                                    
01519+6426   GIC  27     G244-037/G244-036 = GJ 3117A/3118B.                                             
01520+1049   STF 178     H 1  56.                                                                MEv2010 
                         Additional notes may be found in Couteau (1952).                        Cou1952a
01521+5430   SMA  24     Also known as STI1703.                                                          
01522+6627   STF 167     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
01522-5220   CVN   3     CPM pair. The spectral type of the B component is M9.5 +/- 1,                   
                         Teff = 2100 +/- 200K; age ~30 Myr, mass 25 +/- 10 Mjup.                 Cvn2005a
01523-0620   LDS9127     Old LDS6127.                                                                    
01525+1710   GWP 232     XMI 226.                                                                Tob2012b
01526+3127   HJ  645     SEI  20.                                                                Nsn2017a
01528+4016   MLB 999     BRT 2198.                                                                       
01528+1544   BPM  40     [PM2000]   69032 + [PM2000]   69018.                                    Gvr2010 
01528+0117   GWP 233     XMI 227.                                                                Tob2012b
01530-2805   HJ 3472     SWR   3. CPM pair                                                       Skf2004 
01531+2935   BUP  27     alp Tri = 2 Tri = Mothallah. A is a spectroscopic binary, P = 1.77d.            
01532+3719   STF 179     H 1  89.                                                                MEv2010 
01533+4044   HJ 1094     55 And.                                                                         
01534+7003   STF 169     Primary is V776 Cas, a W UMa type eclipsing binary, P = 0.44042d.       Zas2012 
01535+1918   STF 180     gam Ari = 5 Ari = Mesarthim. According to R.G. Aitken, Robert Hooke     A__1935f
                         noted this as a double in 1664. Hooke wrote: "I took notice that it     Hoo1665 
                         consisted of two small stars very near together; a like instance to             
                         which I have not else met in all the heavens."                          HFC1928 
                         A is a variable of the Alpha CVn type.                                          
                         AB: H 3   9.                                                            MEv2010 
                         Uniform disk diameter  0.336 +/- 0.019 mas,                                     
                         Limb darkened diameter 0.346 +/- 0.019 mas,                                     
                         Teff = 11000 +/- 1100 K based on LDD.                                           
                         Radius is 1.97 +/- 0.12 \rsun.                                          CIA2019a
             BU  512     Primary is C component of STF 180. WDS designation changed from                 
                         01538+1918 and components labelled CD.                                          
01536+6324   PTT   3     OL 114, STI 317 are identical.                                                  
01536+0311   xi Psc      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin & Herbig (1981).                                                Grf1981b
01539+5611   RBR  33     Suspected non-single.                                                   Hor2002b
01541-7729   JSP  31     Apparent rapid retrograde motion, but measures sparse.                          
01543+6542   GIC  28     G244-042/G244-041.                                                              
01543-1543   GAL 314     Also known as LDS1120.                                                          
                         Object #55 in Gallo's original list.                                    Gal1912a
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
             CHM   3     AC. NLTT 6398 + 6395.                                                           
01544-2250   LDS3322     NLTT 6400/6399                                                          Chm2004 
01544-4230   phi Phe     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
                         Chemically peculiar late-B star, initially thought to be a triple,              
                         with spectroscopic period 41.4d and astrometric period 878d. Using              
                         Coralie spectra from 2000-2010, Korhonen et al. (2013 A&A 553, A27)             
                         find a spectroscopic period of 1126d. Spectroscopic data by Pourbaix            
                         et al. (2013) exclude the 40d period, but are insufficient to refine            
                         the Korhonen solution. Their spectroscopic elements are combined                
                         with the Hipparcos astrometry to refine the initial astrometic orbit.   Pbx2013 
01546+2049   MKT   3     bet Ari = Sheratan. Astrometry from Mark III interferometer is combined         
                         with spectroscopy (Tomkin & Tran 1987) by Pan et al. (1990) to          Tom1987b
                         determine orbital elements, masses, and distance. Masses agree well     MkT1990 
                         with empirical mass-luminosity relation.                                        
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Pan et al. (1990).                                                      MkT1990 
                         Martin et al. (1998) derive component masses 2.067 +/- 0.203 and                
                         1.281 +/- 0.178 Msun.                                                   Mig1998 
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.19 +/- 0.13, 3.51, and 1.82 Msun, respectively.             Mlk2012 
01549+1124   BPM  41     [PM2000]   70299 + [PM2000]   70233.                                    Gvr2010 
01551+2847   STF 183     According to Scardia et al. (2001), orbital elements are well defined;  Sca2001d
                         only the period is still rather uncertain. The Hipparcos parallax               
                         (0".00727 +/- 0.00189) gives a mass sum of 3.8 Msun +/- 82%, in excess          
                         for a binary of type F2. The dynamical parallax (0".0074) agrees well           
                         with the observed one.                                                          
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 4.82 +/- 2.85, 3.45, and 1.35 Msun, respectively.  Mlk2012 
01551-1204   LDS9128     Old LDS6128.                                                                    
01553-2134   DON  26     CD-22@641.                                                                      
01554+0257   A  2407     A premature orbit has been computed.                                            
01555+7637   LDS1545     Aka LOC  67.                                                                    
01556+0146   BU 1367     A 2408.                                                                         
                         Rectilinear solution by Rica & Zirm (2012).                             FMR2012i
01559+0151   STF 186     Spectroscopic binary?  Spectrum composite; F7V+G0V.                             
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.22 +/- 1.22, 2.56, and 1.07 Msun, respectively.             Mlk2012 
01560+5728   STI1717     Apparently the same as MRI  41.                                                 
01560+0529   GWP 236     XMI 228.                                                                Tob2012b
01560+0046   RST5186     BD+00@311a.                                                                     
01560-5137   HJ 3473     chi Eri                                                                         
01561+6035   AG  301     HJL  26.                                                                HJL1986 
01561+3745   HJ 1097     ALI 494.                                                                        
01562+3715   BU 1368     Bb: b is BD+36@349.                                                             
             STFA  4     56 And. B is BD+36@354.                                                         
01563+0829   GWP 237     AB: XMI 229AB.                                                          Tob2012b
             GWP 238     AC: XMI 229AC.                                                          Tob2012b
01564+3650   J  2719     ALI 259.                                                                        
01568+3931   ALI1022     Not found by Heintz at IDS position.                                    Hei1990b
01568+3802   TOB9001     BC: A measure by Espin incorrectly attributed to this pair led to its           
                         earlier designation as 01569+3759ES  228CD.                                     
01568+2303   BVD  21     RoboAO resolved the B component (201.1deg, 0.199", dI=1.61 mag) but             
                         the pair was not accepted as real.                                      Tok2014d
01570+3101   A   819     A premature orbit has been computed.                                            
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.97 +/- 1.00, 2.49, and 1.20 Msun, respectively.  Mlk2012 
                         AB,C: HJL  27.                                                          HJL1986 
01571+1517   BPM  43     [PM2000]   71640 + [PM2000]   71653.                                    Gvr2010 
01571+1414   BPM  42     [PM2000]   71596 + [PM2000]   71608.                                    Gvr2010 
01572+1644   GWP 241     XMI 230.                                                                Tob2012b
01572-1015   GAL 315     LDS  60. Object #56 in Gallo's original list.                           Gal1912a
                         HIP 9094. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 6529/6530                                                          Chm2004 
                         CHARA Array Limb-darkened diameter  0.611 +/- 0.081 mas,                CIA2008c
                         R =  2.18  +/- 0.29  \rsun.                                                     
                         CHARA Array Limb-darkened diameter of A :                               CIA2013c
                         R =  2.1425 +/- 0.0687 \rsun, L =   2.6056 +/-0.1041 \lsun,                     
                         Teff = 5013 +/-  62 K, M = 1.133 \msun, Age = 7.8 Gyr.                          
01575+5558   ES 1811     STI1732.                                                                        
                         Vatican zone coordinates yield 1911.9, 295.2, 5.61, showing Espin's             
                         distance is too small and that there is no change so far.               VBs1954 
01576+4205   YSC 125     There is some evidence of a very faint third component in this system           
                         with separation of 0.45 arcsec.                                         Hor2011b
                         Improved SB2 orbit. A: Teff = 5789 +/- 21 K, B: Teff = 4544 +/- 164.    Kie2018 
             NLTT 6522   Orbit determined by fitting revised Hipparcos intermediate astrometric          
                         data. Derived component masses 0.99 +/- 0.11 and 0.75 +/- 0.05 Msun.    Ren2010 
01577-3625   LDS  62     LDS5359. TSN  72.                                                               
01579+2336   H 5  12     H V 12. STTA 21. 9 Ari = lam Ari. A is a Beta Lyrae-type and                    
                         spectroscopic binary.  B is BD+22@289.                                          
                         AB: HJL  28.                                                            HJL1986 
01579+0924   GWP 243     XMI 231.                                                                Tob2012b
01579-2851   LDS  61     NLTT 6581/6583                                                          Chm2004 
01581+4123   S   404     Same as STF 190 rej, SHJ 404, H IV 104, H 4 104, H IV 128, H 4 128.             
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
01583+0250   GWP 245     XMI 232.                                                                Tob2012b
01583-8218   I   311     Composite spectrum: G8/K0(V)+(G).                                               
01584+2547   A  2011     B is strongly above MS, very red in V-K (wrong 2MASS ptm?). Hipparcos           
                         does not resolve AB, but has X-solution and suspected non-single.       Tok2014d
01584-2304   LDS3330     NLTT 6605/6606                                                          Chm2004 
01585+3643   J  1809     ALI 262.                                                                        
01586+3834   LPL   1     La Palombara et al. (2012) detect a companion to the hot subdwarf               
                         BD+37 442, using the XMM Newton satellite. The companion is thought to          
                         be a white dwarf or neutron star, likely powered by accretion from the          
                         wind of the primary.                                                    LPl2012 
01586-5332   HU 1557     Primary is CI Eri, an Algol-type eclipsing binary, P = 1.23819d.        Zas2012 
01588+1702   GWP 247     XMI 233.                                                                Tob2012b
01588-0949   J  1449     BD-10  410. Previously published declination corrected by +4'.          J__1949a
                         GAL 316. Object #57 in Gallo's original list.                           Gal1912a
01588-2212   HJ 2103     B is BD-22@329.                                                                 
01588-6134   alf Hyi     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
01589-5652   LDS  63     LDS6106 = LDS9106 (incorrectly listed in the WDS as 00593-5652).                
                         B is CPD-57@385 = CD-57@396.                                                    
01590-1640   LDS9129     Old LDS6129.                                                                    
01590-2255   H 2  58     H II 58. A is a W UMa-type system, AA Cet.                                      
01591+3313   ENG   9     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: Rectilinear solution by Friedman et al. (2011).                     USN2011a
01591+1523   GWP 248     XMI 234.                                                                Tob2012b
01598+1543   BPM  44     [PM2000]   73241 + [PM2000]   73209.                                    Gvr2010 
02000+1334   LDS5181     old LDS6130.                                                                    
02003-0138   BAL   9     J  3333.                                                                Nsn2016 
02004-0831   HJ 3476     AB: A is AR Cet, probably a semi-regular variable.                              
02005-0240   BRG   8     The companion to 2MASS J02002975-0239579 has yet to be tested for               
                         common proper motion, but since its color and brightness are                    
                         consistent with expectation and its separation is small (~0.32"), it            
                         is counted as a physical companion here.                                Jnn2012 
02005-6246   HJ 3479     B is CPD-63@142.                                                                
02006+2753   J  3257     A is an Algol-type binary, X Tri, P = 0.97d.                                    
02011+3518   STF 197     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
02011-1741   LDS5362     NLTT 6759/6757                                                          Chm2004 
02012-0729   GWP 250     ABL   1.                                                                Tob2012b
02012-3000   CUS   1     Assuming a primary mass of 1.02 +/- 0.19 Msun, the derived flux ratio           
                         (~0.028 in H and K) gives a mass of ~0.5 Msun for the secondary.        Cus2012 
02013+1227   BPM  45     [PM2000]   74159 + [PM2000]   74128.                                    Gvr2010 
02013-0752   GWP 251     ABL   2.                                                                Tob2012b
02015+1830   BPM  46     [PM2000]   74328 + [PM2000]   74271.                                    Gvr2010 
02019+7332   JNN 252     GJ 3125. Estimated age 30-300 Myr; masses 0.12 +/- 0.07 and 0.06 +/-            
                         0.04 Msun; a ~5.0 au.                                                   Jnn2014 
02019+2415   POU 157     ID uncertain. Nothing at Pourteau's coordinates.                        Pou1933 
02020+7054   BU  513     48 Cas. A is a spectroscopic binary, same period as the visual pair.            
                         Suspected sub-periods of 39 yr (Baize) and 26 yr (Muller) are not       Baz1941b
                         confirmed by later measures.  The radial velocities of the primary may  Mlr1949c
                         show a trace of a period of about 4 yr (Heintz).                        Hei1981e
                         See Baize & Petit catalog of doubles with variable component.           Baz1989d
                         Masses and bolometric magnitudes are derived for the two components             
                         based on assumed spectral types and available parallaxes.                       
                         1980.7205: This measure was incorrectly attributed to ADS 1958 in               
                         McAlister et al. (1983).                                                McA1983 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.96 +/- 0.42, 3.07, and 2.00 Msun, respectively.  Mlk2012 
02020+0246   STF 202     alp Psc = Alrescha. Both components are listed as Alpha CVn variables           
                         of small amplitude, and both may have variable RV.                      Sca1983f
                         See Baize & Petit catalog of doubles with variable component.           Baz1989d
                         Absolute quadrant for 1998.657 determined by triple-correlation                 
                         techniques                                                              Pru2002b
                         Chevalier identified this star as alp Psc, but gave an incorrect        Che1911 
                         declination, leading to its initial designation as 02020+0320 CHE 32.   Hrt2012b
             PWL   1     AC: SHY 132. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
             STF 202     AB: H 2  12.                                                            MEv2010 
02021+0355   OSV   1     LDS5363.                                                                        
02021-1321   GAL 317     Object #59 in Gallo's original list.                                    Gal1912b
02022+7530   STF 185     Primary is V779 Cas, an Algol-type eclipsing binary, P = 6.35340d.      Zas2012 
02022-1441   GWP 253     ABL   4.                                                                Tob2012b
02022-1808   GWP 252     ABL   3.                                                                Tob2012b
02022-4550   SHY 410     HIP   9495 + HIP   9672.                                                        
02022-6236   TOK  70     HIP 9499. A is SB, no orbit, dRV=70.7 (Nordstrom et al. 2004).          Nrd2004 
02023-2634   LDS  65     NLTT 6825/6826                                                          Chm2004 
02025-1410   GWP 254     ABL   5.                                                                Tob2012b
02026+5941   CIA  53     V780 Cas.                                                                       
02026-1719   GWP 255     ABL   6.                                                                Tob2012b
02027-3019   HJ 3478     B is CD-30@717.                                                                 
02030+3317   STF 201     eps Tri = 3 Tri                                                                 
02031-0725   STF 209     B is BD-08@371.                                                                 
02031-1229   GWP 256     ABL   7.                                                                Tob2012b
02032+5514   BLL   4     A is a semi-regular variable, XX Per. B is BD+54@445.                           
02034+3919   MLB  10     AB: Also known as SMA  27.                                                      
02035+6408   HJ 1101     STI 337 (three Vat1926 measures from STI 337 merged 2008/06/25)                 
02035+1744   BPM  47     [PM2000]   75525 + [PM2000]   75508.                                    Gvr2010 
02035-0455   TOK 873     also known as VSC   2.                                                  Hor2024 
02037+2556   STF 208     10 Ari. Malkov et al. (2012) derive dynamical, photometric, and                 
                         spectroscopic masses 2.94 +/- 0.84, 2.35, and 1.29 Msun, respectively.  Mlk2012 
02038+7013   MLR 375     1983.0663: This autocorrelogram was remeasured; the new results are             
                         listed in the catalog.                                                  McA1987b
02038-0020   H 5 102     H V 102. 61 Cet. Spectrum composite; G5II-III+G5V.                              
02039+8221   HJ 2090     The measure in BDS by Cogshall belongs to some other pair.              Bu_1906 
                         1904.69, 243.9@, 3.52" (Van Biesbroeck).                                VBs1914 
02039+4220   STF 205     H III 5, SHJ 26. gam And = Almach. A quadruple system.                          
                         Star A (mag 2.3, K3II) forms with BC the pair STF 205, separation 10".          
                         Star B is SB, P = 2.67 d (Maestre & Wright, ApJ 131, 119, 1960).                
                         See discussion by Morgan et al. (1978).                                 BLM1978 
                         A,BC: H 3   5.                                                          MEv2010 
                         Mk III Limb-darkened diameter  7.84 mas.                                MkT1991 
                         Mk III Limb-darkened diameter  7.814 +/- 0.078 mas.                     MkT2003 
             STT  38     BC: See discussion by Morgan et al.                                     BLM1978 
                         BC: Poor agreement between two theta measures.                          Mlr1956d
                         BC: Additional notes may be found in Muller (1954).                     Mlr1954a
02039+1231   BPM  48     [PM2000]   75778 + [PM2000]   75779.                                    Gvr2010 
02039-4525   RST2272     Primary is SB2, P=0.851 y. Aa,Ab UR in speckle. Koen et al. (2002               
                         MNRAS 331, 45) find 311d photometric period.                            Tok2014d
02042+5257   HJ 2104     B is BD+52@501.                                                                 
02042+4641   ADM   1     HTP  32. HAT-P-32. Primary is exoplanet host star.                      Adm2013 
02042-1039   GAL 318     Object #62 in Gallo's original list.                                    Gal1912b
02044+1230   CHE  36     CHE  37.                                                                        
02046+2525   LTT 17328   Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from the Geneva           
                         Extrasolar Planet Search Programs home page.                            HaI2001 
02046+1757   GWP 257     XMI 235.                                                                Tob2012b
02051+7717   SHJ  22     47 Cas.                                                                         
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
             47 Cas      Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
02051-1737   BEU   3     PM = +1318-174.                                                                 
02053+2906   CHE  38     CD: Originally 02053+2907 CHE  38AB, until C component of 02053+2906            
                         found to be prmary of 02053+2907.                                               
             WAK  14     CE: Originally 02053+2907 WAK  14AC.                                            
02053-2803   LDS  67     NLTT 6979/6980                                                          Chm2004 
02054-5910   HJ 3481     B is CPD-59@185.                                                                
02055+7607   BU  785     49 Cas.                                                                         
02055+0056   LDS5365     Error in WDS designation - incorrect precession of Luyten coordinates?  Luy1984 
02056+1444   BPM  49     [PM2000]   76857 + [PM2000]   76899.                                    Gvr2010 
02057-2423   I   454     CPD-24@891. C is CPD-24@889.  AB,C = LDS  68.                                   
                         AB,C: SHY 135. Bayesian analysis by Shaya & Olling (2011) indicates     Shy2011 
                         very high (near 100%) probability pair is physical.                             
             WSI   7     Aa,Ab: Tokovinin et al. (2014) derive a combined spectroscopic/                 
                         interferometric orbit of the Aa,Ab pair, as well as a new orbit of the          
                         AB pair. Resulting component masses for Aa, Ab, B, and C are 0.74,              
                         0.72, 0.57, and 0.78 Msun, respectively.                                Tok2014b
02058+1241   CHE  42     There are no obvious errors in applying the offset from Chevalier's     Che1910 
                         plate center, but there are no appropriate pairs near his coordinates,          
                         nor at coordinates found by reversing the sign of either or both                
                         offsets. The pair is likely lost.                                       Hrt2012b
02062-1808   GWP 258     ABL   8.                                                                Tob2012b
02065+5703   BAR  23     J 880.                                                                          
02068+2542   HO  312     11 Ari.                                                                         
02069-1126   SLW  99     Aka ABL   9.                                                                    
02070+4512   WOR   1     AB: Rectilinear solution by Hartkopf & Mason (2015).                    WSI2015 
             BKO  12     AC: Rectilinear solution by Hartkopf & Mason (2015).                    WSI2015 
             LMP  27     AD: Rectilinear solution by Hartkopf & Mason (2015).                    WSI2015 
                         There is an unresolved (P=897d) spectroscopic companion to A.           Tok2019b
02070-1017   GAL 319     Object #63 in Gallo's original list.                                    Gal1912b
02070-4406   JNN 149     2MASS J02070176-4406380 and J02070198-4406444 are separated by only 7"          
                         and have similar estimated spectroscopic distances (13 and 21 pc,               
                         respectively) in Riaz et al. (2006), hence it is likely that they form  Ria2006 
                         a physical pair.                                                        Jnn2012 
02074-5941   HJ 3484     B is CPD-60@183.                                                                
02076+1355   ZHN   2     BDK   4. G 73-26 + SDSS J020735.60+135556.3.   Distance 26 +/- 10 pc            
                         for primary, 35 +/- 5 pc for secondary. Estimated age of system 3-4             
                         Gyr. Mass of secondary estimated at 0.079-0.081 Msun.                   Fah2010 
02076-0037   LDS3346     NLTT 7066/7064                                                          Chm2004 
                         HJL  29.                                                                HJL1986 
02079+1343   GWP 259     XMI 236.                                                                Tob2012b
02080+2814   CHE  55     MLB 452.                                                                        
02080-0951   GAL 320     Object #64 in Gallo's original list.                                    Gal1912b
                         Rectilinear solution by Hurowitz et al. (2013).                         USN2013a
02081+1336   FAR  27     SKF  23.  Primary is white dwarf WD 0205+133.                           Far2006 
02082+1509   LDS5183     old LDS6131.                                                                    
02083+2543   ALP   6     2MASSW J0208183+254253                                                          
                         Further observations are required to determine the physical/optical             
                         nature of this triple.                                                  AlP2007 
02084+2819   KUI 118     G072-058. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 7087/7088                                                          Chm2004 
02085-0641   HDS 285     Possible sub-diffraction-limited component, but the astrometry is not           
                         consistent between the two observations.                                Hor2011b
02087-0026   STF 218     Same as STF 220.                                                                
02087-1005   HU   16     HD 13191, W UMa-type eclipsing binary, period 0.31542 d.                Zas2018 
02089+4927   BWL   9     Colors and/or astrometry are inconsistent with a late-type common               
                         proper motion companion based on visual inspection of the field from            
                         2MASS, SDSS, DSS1, and/or DSS2. Primary is GJ 3136.                     Bwl2015 
02090+5745   STI1791     AB. WDS designation changed from 02099+5744 when it was determined              
                         that TDS2135 comprised the primary of this wider pair.                          
02091+5104   STF 213     C easily seen 8" north following. Magnitude about 10.5, not 12.5.       B__1963b
02091+4341   LDS3349     NLTT 7117/7118                                                          Chm2004 
02091+4048   STF 215     A is an eclipsing binary, BX And.                                               
02091+1511   GWP 260     XMI 237.                                                                Tob2012b
02093-1958   GWP 261     ABL  10.                                                                Tob2012b
02094+2556   H 6  69     H VI 69. 14 Ari. STTA 23.                                                       
                         AC: HJL1012.                                                            HJL1986 
02094-1011   HJ 2116     Richard Jaworski, in analysis of SuperCOSMOS data, has determined that  Jaw2005 
                         component C is the galaxy NGC 833, D is the galaxy NGC 835, E is the            
                         galaxy NGC 838 and F is the galaxy NGC 839. Thus, in the pairing "CD"           
                         both components are galaxies and not stars.                                     
02095+3459   MKT   4     bet Tri.                                                                        
                         Hummel et al. (1995) visual orbit based on astrometry from Mark III     MkT1995 
                         interferometer. Additional spectroscopic data yield component masses,           
                         luminosities, radii, effective temperatures, and distance.                      
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Hummel et al. (1995).                                                   MkT1995 
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.11 +/- 0.18, 5.26, and 1.82 Msun, respectively.             Mlk2012 
02096+4251   ES   48     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
02097+2021   STF 221     AB: H 3  68.                                                            MEv2010 
02097+0857   GWP 262     XMI 238.                                                                Tob2012b
02098-4052   TOK 427     HIP 10096 is SB2 according to GCS. The separation corresponds to a              
                         period of ~5yr.                                                         Tok2015c
02099+3449   HU 1034     Not seen 1948, 1951. No observations since that time.                           
02103+3322   STF 219     SEI  24.                                                                Nsn2017a
02104+3911   HJ 1109     C is a nebula.                                                                  
02104-5049   ESG   1     Gl 86. Magnitudes are K magnitudes of Lagrange et al. (2006).                   
                         Lagrange et al. (2006) give two possible orbital solutions, based on    Lgr2006 
                         different assumed masses (70 Mjup and 0.5 Msun) for the secondary.              
                         Semi-major axes converted from au (47.58 and 18.42 au, respectively)            
                         to arcseconds assuming an Hipparcos-based distance of 10.9 pc.                  
                         JHK photometry of primary from 2MASS, that of secondary transformed             
                         from NACO to 2MASS filters.                                                     
                         2001.7454: PA is measured in zenith mode. If data collected in                  
                         equatorial mode, PA = 112.1.                                            Rbr2011d
                         Farihi et al. (2013) derive a mass of 0.59 +/- 0.01 Msun and                    
                         Teff = 8180 +/- 120K for the white dwarf companion to GJ 86. Monte              
                         Carlo simulations yield the following orbital constraints:                      
                         P = 120-481y, T0 = 1933-2067, e = 0.00-0.61, i = 114.7-122.6deg,                
                         a = 2.57-6.47" (27.8-69.8 au) Omega = 63.7-76.1deg, omega=0-358deg.             
                         The upper ranges of P and a are considered less likely.                 Far2013 
             GJ 86       A: Combined solution, based on reduction of Hipparcos intermediate              
                         astrometric data together with spectroscopic elements from Queloz       Que2000 
                         et al. (2000).                                                          HaI2001 
02106+1027   GWP 263     XMI 239.                                                                Tob2012b
02107-1507   FAR  28     Primary is white dwarf WD 0208-153.                                     Far2006 
02109+3902   STF 222     59 And.                                                                         
                         H 4 129.                                                                MEv2010 
02109+1341   STF 224     H N 105; BDS 1146 is identical.                                                 
02110+0317   GWP 264     XMI 240.                                                                Tob2012b
02112+2604   BRT3260     Originally published as BRT 127.                                        Brt1928 
02113+4407   ES 2590     Rectilinear solution by Hartkopf & Mason (2015).                        WSI2015 
02114+1848   GWP 265     XMI 241.                                                                Tob2012b
02115+5739   BU  874     5 Per.                                                                          
02117-0531   GWP 266     ABL  11.                                                                Tob2012b
02117-1927   GWP 267     ABL  12.                                                                Tob2012b
02120+0422   SKF1518     A is also a double-lined binary (5.9d) so this is a physical triple.    Tok2019b
02122+4440   RUC   2     Aa,Ab. GZ And. Spectral type of Ab component estimated at M3-4V.        Ruc2007 
             HJ 2117     A is a W UMa-type binary, GZ And.                                               
                         Neither AC, BC or CD are physically associated.                         Kiy2015c
02123-0908   GWP 268     ABL  13.                                                                Tob2012b
02124+3018   STF 227     iot Tri = 6 Tri. A is a spectroscopic binary, P = 14.73d. B is also an          
                         SB, P = 2.24d. One component is variable: TZ Tri.                               
             TZ Tri      Koresko et al. (1998) PTI solution has period fixed at spectroscopic    Krs1998 
                         value of Kaye et al. (1995).                                            Eat1995b
             STF 227     H 2  34.                                                                MEv2010 
                         T0 converted from negative to positive by subtracting from P.           FMR2020c
02124+1249   LDS1126     NLTT 7300/7301                                                          Chm2004 
02124-0223   HDO  56     Not found. There must be a large error in the Hd place. Burnham         Bu_1909 
                         could not find it anywhere in the vicinity.                                     
02124-0455   GWP 269     ABL  14.                                                                Tob2012b
02124-7023   R    15     HLN   3.  B is CPD-70@131.                                                      
02125-0804   BRT 357     Also known as LDS3357.                                                          
02127+1614   GWP 270     XMI 242. SLW 100.                                                       Tob2012b
02128+7941   S   405     STTA 22. A is a Delta Scuti-type variable and spectroscopic                     
                         binary, P = 4.12d. B is BD+78@71.                                               
                         AB: H 5  84.                                                            MEv2010 
02128+0309   GWP 271     XMI 243.                                                                Tob2012b
02128-0224   STF 231     66 Cet. B is BD-03@335.                                                         
                         Aka SHJ  29 = H 4  25.                                                          
                         AB: NLTT 7323/7321                                                      Chm2004 
                         HIP 10305. A is SB2, period 94.788d, resolved by speckle (TOK 39).              
                         A is evolved. B = HIP 10303.                                            Tok2011a
02129+5712   STTA 24     AB and AC: Optical pair, based on study of relative motion of the               
                         components using the method of apparent motion parameters.              Kiy2008 
                         AC: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
02129-0349   GWP 272     ABL  15.                                                                Tob2012b
02130+0851   MCA   5     xi 1 Cet = 65 Cet. Also a spectroscopic binary.                                 
                         A 1985.8375 measure attributed to this pair by Mcalister actually               
                         actually belonged to 02157+2503COU  79.                                 McA1987b
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin & Herbig (1981).                                                Grf1981b
                   5     1985.8375: A measure at this date, belonging to 02157+2503 = COU  79,           
                         was erroneously attributed to MCA 5 in McAlister et al. (1987). This    McA1987b
                         measure has been moved to COU 79 and averaged with a re-reduced                 
                         measure from these data published by Hartkopf et al. (1996).            Hrt1996a
02131+5805   SHY 145     AC: HIP  10332 + HIP  12685.                                                    
02132+4414   CHR   5     60 And. A spectroscopic binary.                                                 
                         The negative results obtained during 1976 - 1980 are apparently due to          
                         a large magnitude difference.                                           Hrt1984 
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Griffin & Herbig (1981).                                                Grf1981b
                         Mk III Limb-darkened diameter  2.907 +/- 0.048 mas.                     MkT2003 
02132+4030   SHY 136     AB: HIP  10339 + HIP  10321. B component is V450 And.                           
             HEL   5     Ba,Bb: V450 And. Helminiak et al. (2016) resolve this SB and BY Dra             
                         type variable, and derive a combined astrometric/spectroscopic orbit.           
                         The secondary is shown to be an M-type star, rather than brown dwarf.           
                         Resulting best-fit masses are 1.141 and 0.279 Msun (median values               
                         1.113 +/- 0.065 and 0.277 +/- 0.021 Msun), respectively. Best-fit               
                         parallax is 37.24 mas (median 37.34 +/- 0.55 mas).                      Hel2016 
02133+3649   JNN  18     Estimated age 30-300 Myr; masses 0.26 +/- 0.06 and 0.09 +/- 0.03 Msun;          
                         a ~2.8 au.                                                              Jnn2014 
02135+5926   STI 351     STI1807                                                                         
02135-0502   GWP 273     ABL  16.                                                                Tob2012b
02135-2546   HJ 2120     B is CD-26@800.                                                                 
02136+5104   BAG   1     Aa,Ab: 6 Per. A is a long-period spectroscopic binary, now resolved by          
                         speckle interferometry.                                                         
                         SB1, P = 4.5 yr. Halbwachs (1981) predicts maximum separation 0".047.   HJL1981 
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Christie (1936).                                                        Crs1936 
             STT 555     AB: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
02136-0945   GWP 274     ABL  17.                                                                Tob2012b
02137-0302   H 6 110     H VI 110. B is BD-03@341.                                                       
02138-1933   RSS  54     CPD-20@248                                                                      
02140+4729   STF 228     Spectral types and masses of components assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
                         Scardia says the quadrant unambiguous for their 2004 theta values of            
                         105.8; this does not agree with other determinations of magnitude               
                         difference, however.                                                    Sca2005a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.34 +/- 0.36, 2.52, and 2.47 Msun, respectively.             Mlk2012 
02140+1652   GWP 275     XMI 244.                                                                Tob2012b
02142+0555   GWP 276     XMI 245.                                                                Tob2012b
02142-1811   GWP 277     ABL  18.                                                                Tob2012b
02144+3454   HU  807     Motion in separation, with little angular change. Close 1950-1960.              
02144-1441   GWP 278     ABL  19.                                                                Tob2012b
02145+6631   MCA   6     55 Cas. Composite spectrum star: B9V + G0II-III, delta m = 0.2 mag      Bnu1984 
                         (Markowitz 1969)                                                        Mrz1969 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.70 +/- 1.31, 6.94, and 2.57 Msun, respectively.             Mlk2012 
02145+5912   STI1812     SMA  31.                                                                        
02145-1103   LDS5373     SLW 102.                                                                        
02146-0142   GWP 279     ABL  20.                                                                Tob2012b
02147+3024   STF 232     H 2  35.                                                                MEv2010 
02147+1657   GWP 280     XMI 246.                                                                Tob2012b
02149+5829   STF 230     B spectrum B9IV.                                                                
02149+1353   GWP 281     XMI 247.                                                                Tob2012b
02150+5903   MLR 447     Also known as TDS2174.                                                          
02152-3507   SHY 415     HIP  10483 + HIP  10385.                                                        
02154+1126   GWP 282     XMI 248.                                                                Tob2012b
02155+5231   GC 2695     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin & Radford (1977).                                               Grf1977c
02155+1220   GWP 283     XMI 249.                                                                Tob2012b
02156+4223   GIC  29     G133-079/G134-019.                                                              
                         NLTT 7438/7440                                                          Chm2004 
02157+6740   ENG  10     B is BD+66@193.                                                                 
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
             SHY  10     BC: HIP  10529 + HIP  11167.                                                    
02157+2503   COU  79     21 Ari. Couteau & Morel (1982) computed masses disagree with spectral   Cou1982d
                         type. Authors suggest 3rd component (mass ~1 Msun) as possible                  
                         explanation. 1985.8375: This measure was erroneously attributed to              
                         02130+0851 = MCA 5 by McAlister et al. (1987). The data were re-reduced McA1987b
                         by Hartkopf et al., giving similar results. The measure has now been    Hrt1996a
                         replaced by the mean of the two separate reduction results.                     
                         1986.567: The separation of this partially resolved pair was                    
                         calculated under the assumption of zero or otherwise known magnitude            
                         difference. Pair passed periastron earlier than predicted; now the              
                         orbit is definitive                                                     Tok1985 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.09 +/- 0.30, 3.04, and 1.17 Msun, respectively.             Mlk2012 
02157+1046   STF 237     AB: HJL  30.                                                            HJL1986 
02157-0217   GWP 285     ABL  21.                                                                Tob2012b
02157+1657   GWP 284     XMI 250.                                                                Tob2012b
02158-1814   HTG   1     Orbit poorly covered, period rather indeterminate.                      Hei1978c
                         Additional notes may be found in Burnham (1894).                        Bu_1894 
02159+1416   GWP 286     XMI 251.                                                                Tob2012b
02159+0638   A  2013     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.60 +/- 0.37, 1.51, and 0.79 Msun, respectively.             Mlk2012 
02160-0929   BRG  10     This likely triple system has only been observed in one epoch, hence            
                         it remains unconfirmed. The brightnesses and colors of all components           
                         are however consistent with expectation for a physical triple.          Jnn2012 
02160-1626   GWP 287     ABL  22.                                                                Tob2012b
02161+1651   GWP 288     XMI 252.                                                                Tob2012b
02161+1630   BPM  50     [PM2000]   83035 + [PM2000]   83004.                                    Gvr2010 
02162-2302   I   457     ADS 1744a.                                                                      
02163-0949   STF 242     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
02164-0731   SLW 106     = GWP 289 = ABL  23.                                                            
02164-1233   SLW 105     = ABL  24.                                                                      
02164-1632   GWP 290     ABL  25.                                                                Tob2012b
02165-2227   LDS3364     NLTT 7520/7519                                                          Chm2004 
02165-5131   DUN   6     phi Eri. B is CPD-52@284.                                                       
             SHY 137     AC: HIP  10602 + HIP   9685.                                                    
             SHY 137     AD: HIP  10602 + HIP   7699.                                                    
             SHY 133     CD: HIP   9685 + HIP   7699.                                                    
             SHY 143     CE: HIP   9685 + HIP  12225.                                                    
             SHY 130     DF: HIP   7699 + HIP   6485.                                                    
02167-0430   GWP 291     ABL  26.                                                                Tob2012b
02167-3100   LDS  71     NLTT 7535/7528                                                          Chm2004 
02167-6324   TOK  71     HIP 10621. NOMAD: PM(B)=(0,-30), PM(A)=(18,60).                                 
                         D is HIP 10754.                                                         Tok2011a
02168+4346   GNS   1     Based on 2MASS and AstraLux images, Ginski et al. (2012) conclude the           
                         companion is a background object.                                       Gns2012 
02169+5703   STTA 25     B is BD+56@470.                                                                 
02169+0448   GWP 292     XMI 253.                                                                Tob2012b
02169-2322   BRG  11     The companion to 2MASS J02165488-2322133 has not yet been confirmed to          
                         share a common proper motion, but the color and brightness of it are            
                         well consistent with a physical companion, hence it is counted as such          
                         in the statistics.                                                      Jnn2012 
02171+3413   DOR  66     del Tri = 8 Tri. A is a double-lined spectroscopic binary, P = 10.02d.          
                         Proper motion +1154 -245.                                                       
             MKT   5     Aa,Ab: PM = +1154 -245. del Tri.                                                
                         Hummel et al. 1995) visual orbit based on astrometry from Mark III      MkT1995 
                         interferometer. Additional spectroscopic data yield component masses,           
                         luminosities, radii, effective temperatures, and distance.                      
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Hummel et al. (1995).                                                   MkT1995 
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 1.57 +/- 3.14, 1.92, and 1.05 Msun, respectively.  Mlk2012 
02172+5838   YSC  87     Ba,Bb: Originally 02171+5839 YSC  87, but found to correspond to B              
                         component of 02172+5838.                                                        
02172-2849   LDS3365     NLTT 7557/7558                                                          Chm2004 
02173+3351   VIG   1     Primary is gam Tri. The B and C components are background stars, the D          
                         component ambiguous.                                                    Vig2012 
02174+2845   STF 239     HJL  32.                                                                HJL1986 
                         Aka H 4  40 = SHJ  31.                                                          
02174+2708   GIC  30     AC: G035-037/G036-007.                                                          
02176+2214   STF 244     HJL  33.                                                                HJL1986 
02176-5400   RSS  55     CD-54@487                                                                       
02178+5638   A  1272     V438 Per, a W UMa type eclipsing binary, P = 3.50939d.                  Zas2012 
02179+1941   TOK  72     HIP 10710. Primary is astrometric binary (Makarov & Kaplan 2005)        Mkr2005 
02179+1614   GWP 293     XMI 254.                                                                Tob2012b
02180+5616   UC   29     Primary appears to be a close pair.                                     Cbl2010c
02180+3116   A   959     Primary is eclipsing binary of W UMa type, period 0.31069d.             Zas2017b
02180+1958   GWP 294     XMI 255.                                                                Tob2012b
02180+0145   GC 2770     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Harper (1935).                                                          Hrp1935 
                         Combined astrometric/spectroscopic orbit by Fekel et al. (2007). For    Fek2007 
                         primary, derive mass = 1.15 Msun, radius = 1.64 +/- 0.07 Rsun,                  
                         Luminosity = 3.0 +/- 0.1 Lsun. Spectral types are G0IV and ~M0V.                
                         SB1. Combined orbit including RV data and Hipparcos Intermediate                
                         Astrometric data. Semimajor axis derived from photocentric a0 plus              
                         stellar evolutionary model. Derived properties for A and B:                     
                         M/Msun = 1.20 + 0.53, L/Lsun = 2.76 + 0.04, dm = 4.60 mag,                      
                         log age = 9.65.                                                         WaX2015b
02180-1229   LDS  73     NLTT 7592/7593                                                          Chm2004 
02181+5731   BU 1170     7 Per = chi Per                                                                 
                         S   409 = H 6  19.                                                              
02182+5715   STI1836     BKO 165.                                                                        
02182+3920   A   207     Scardia et al. (2001) orbit preliminary as all the orbital elements     Sca2001d
                         are still rather uncertain. Hipparcos parallax (0".01200 +/- 0.00311)           
                         seems to be overestimated and leads to a mass sum 0f 0.46 Msun,                 
                         unacceptable for a system of type F5. Scardia (1982) classified the     Sca1982a
                         star as type F9. Dynamical parallax is 0".0065; the corresponding mass          
                         sum is 2.87 Msun.                                                               
02184+5758   STI1839     STI1844.                                                                        
02184-0636   GWP 295     ABL  27.                                                                Tob2012b
02186+4017   STF 245     ALI1193.                                                                        
             EGG   2     Aa,Ab: This system has spectral type F2 from SIMBAD and parallax of             
                         10.26 +/- 2.92 mas from van Leeuwen (2007). A previous orbit was        VlF2007 
                         calculated by Cvetkovic (2008) with period of 109 years and semimajor   Cve2008c
                         axis of 0.344 arcsec. However, our new observation shows that the               
                         system has a much shorter period and smaller semimajor axis. However,           
                         our orbit yields roughly the same total mass, with large uncertainty.           
                         The system appears to have executed nearly a full orbit since the               
                         first speckle observations taken of it in 1985 by McAlister et al.              
                         (1987). More data will be needed to confirm this orbital trajectory,            
                         but if correct, the smaller period makes the system much more                   
                         attractive for future study.                                            Hor2015b
02186-2940   B    34     AV For, Algol-type eclipsing binary, P = 1.8797 d.                      Zas2011 
02187+3429   STF 246     H III 42, BDS 1165.                                                             
                         HJL  34.                                                                HJL1986 
                         H 3  42.                                                                MEv2010 
02187+0412   BU  437     Some observations erroneously ascribed to STF 247, even Struve's                
                         discovery, seems to belong to this pair, whose delta-m = 2 is less              
                         than Burnham's estimate.                                                Hei1992a
02188+5714   BKO 168     AC: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
02188+0840   GWP 296     XMI 256.                                                                Tob2012b
02188+1440   GWP 297     XMI 257.                                                                Tob2012b
02190+2839   HJ 1115     10 Tri.                                                                         
02191-0651   HJ  327     AC: The C component is the galaxy NGC 883.                                      
02193-0259   JOY   1     Aa,Ab: The primary is omi Cet = VZ Cet = 68 Cet = Mira , prototype of           
                         the Mira-type variables. "Orbits" have been computed for the visual             
                         pair, but are most likely false. B has in the past been identified as a         
                         Cepheid, VZ Cet; however, it appears that the component seen as                 
                         variable is the Joy component, recently determined to be a White Dwarf. Skl2010 
                         Recent papers (in particular 1995 PhD thesis by Harold L. Chambers II)          
                         suggest that the visible companion is not the star itself, but the              
                         accretion disc around it (material captured from Mira's stellar wind).          
                         Rapid fluctuations of brightness are described by Warner (1972 MNRAS            
                         159, 95).                                                                       
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Aa,Ab: Pair seen but not measured.                                      Cou1958c
                         Aa,Ab: Additional notes may be found in Couteau (1963).                 Cou1963a
             H 6   1     H VI 1. C is BD-03@355.                                                         
02198-2352   HJ 2130     B is CD-24@1022.                                                                
02200-2213   BRT1373     CD-22@784.                                                                      
02201-1703   GWP 298     ABL  28.                                                                Tob2012b
02204+2456   POU 175     Also known as KU    9.                                                          
02204+1617   BPM  51     [PM2000]   85486 + [PM2000]   85504.                                    Gvr2010 
02204+0135   GWP 299     XMI 258.                                                                Tob2012b
02205+1733   BPM  52     [PM2000]   85552 + [PM2000]   85616.                                    Gvr2010 
02209-0954   GWP 300     ABL  29.                                                                Tob2012b
02209-5632   RST  51     CD-57@470.                                                                      
02210-1650   GWP 301     ABL  30.                                                                Tob2012b
02211+4246   STF 248     Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Combined spectroscopic/visual solution, yielding masses, etc.           Trr1995a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.39 +/- 0.49, 1.78, and 0.85 Msun, respectively.             Mlk2012 
02212+5651   BU 1171     Not seen in 1951 with 82-inch (Van Biesbroeck).                         VBs9999 
02212+3653   GIC  31     AB,C: NLTT 7710/7708                                                    Chm2004 
02213-1057   HJ 3495     B is BD-11@445.                                                                 
02215-1251   GWP 302     ABL  31.                                                                Tob2012b
02215-1354   GWP 303     ABL  32.                                                                Tob2012b
02216+2338   STF 254     POU 178.                                                                        
02219+0824   GWP 304     XMI 259.                                                                Tob2012b
02220+0445   TOK 231     Primary is SB1, P= 79.700 d. Companion at 53" is possibly a white       Tok2012c
                         dwarf (Tokovinin & Lepine 2012)                                         Tok2014d
02220-0034   GWP 305     ABL  33.                                                                Tob2012b
02222-0348   GWP 306     ABL  34.                                                                Tob2012b
02224+5551   BU  875     9 Per. Variable, V474 Per.                                                      
02225+2830   FAR  29     Primary is white dwarf WD 0219+282.                                     Far2006 
02225-0536   GWP 307     ABL  35.                                                                Tob2012b
02225-2349   LAF  27     TOK  40.                                                                        
                         Astrometric binary with 26.5 yr orbit has massive secondary with q~1.   Tok2012a
                         Tokovinin (2013) derived a combined spectroscopic/interferometric               
                         solution, including echelle spectroscopy and speckle interferometry.            
                         The B component is a close binary (tentative period 3.7d); masses of A          
                         and Ba+Bb are nearly equal.                                             Tok2013a
                         Astrometric binary with large acceleration, where the massive                   
                         companion B is in fact a close pair of M dwarfs.                        Tok2013b
             kap For     Gontcharov & Kiyaeva (2002) photocentric (astrometric) orbit based on   Gon2002a
                         combination of ground-based catalogs with Hipparcos.                            
02226+1531   LDS3375     G004-016. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 7795/7794                                                          Chm2004 
02229+5835   BLL   7     A is the semi-regular variable, S Per.                                          
02229+4129   TRN  10     The image rotator was in an unknown state, so two possible theta                
                         values are listed for the 2001.7451 observation - one for zenith up             
                         and one for north up.                                                   Trn2008 
             HD  14633   Rodgers (1974 M.S. Thesis, Univ. Toronto) made a preliminary orbital            
                         analysis (P =15.3 d) but the variations appear to be more complicated           
                         than originally claimed (Bolton & Rodgers 1978 ApJ 222, 234).           Msn1998a
02229-1718   GWP 308     ABL  36.                                                                Tob2012b
02229-5106   EHR   1     CPM pair.                                                               Ehr2010 
02230+0443   GWP 309     XMI 260.                                                                Tob2012b
02231+7021   MLR 377     A premature orbit has been published.                                           
                         Omega corrected from 0.0 to 180.0 by Ruymaekers & Nys (1995)            Ruy1995 
02231+0246   GWP 310     XMI 261.                                                                Tob2012b
02232+6050   MZA  42     DN Cas.                                                                         
02232-2952   BU  738     T incorrectly listed as 1953.489 by Scardia et al. (1990); should be    Sca1990a
                         1953.849 (erratum noted in Inf. Circ. 112, 1990)                        Sca1990b
                         Parabolic orbit.                                                        Fin1969b
                         sigma = areal constant in the true orbit = 0.0199 arcsec^2/yr                   
                         q = periastron distance in the true orbit = 0".4991                             
02233+2230   LDS3378     NLTT 7840/7842                                                          Chm2004 
02233+1525   AG   38     LDS 879. B is BD+14@387.                                                        
                         AB: NLTT 7845/7843                                                      Chm2004 
                         AB: SHY 417. Bayesian  analysis by Shaya & Olling (2011) indicates      Shy2011 
                         very high (near 100%) probability pair is physical.                          .  
                         HIP 11137. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AB: HJL  35.                                                            HJL1986 
02233+1452   GWP 311     XMI 262.                                                                Tob2012b
02236-1056   RST4203     Also known as OL  111.                                                          
02238+4920   STF 256     Also known as STF 243.                                                          
02239+5751   MLR 656     Also known as HDS 311.                                                          
02239+5522   BU 1373     The primary is the Cepheid variable V440 Per.                           Evs2016a
02239+3330   STF 258     Also known as STF 253.                                                          
02242+1016   CHR 199     First detected as an occultation binary by Evans.                       Evn1980 
02244-2253   LDS3382     NLTT 7922/7928                                                          Chm2004 
02245-0145   STF 265     HJL  36.                                                                HJL1986 
02246+5959   STF 255     STI 360.                                                                        
02246+2537   ALP   7     2MASSI J0224367+253704                                                          
                         Further observations are required to determine the physical/optical             
                         nature of this pair.                                                    AlP2007 
02246-4050   GC 2912     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Barker et al. (1967).                                                   Evn1967 
02247+4008   LDS3381     NLTT 7887/7890                                                          Chm2004 
02249+5153   ES  764     B is BD+51@567.                                                                 
02249+3039   UC  733     AC: Candidate on Tokovinin list, now reconfirmed as CPM. The primary            
                         hosts an exoplanet.                                                     Tok2013c
02250-1501   GWP 312     ABL  37.                                                                Tob2012b
02252+1217   BRT1170     1deg error in WDS designation, apparently an error in transcribing              
                         coordinates from the original source.                                           
02253-0802   GWP 314     ABL  39.                                                                Tob2012b
02253-1242   GWP 313     ABL  38.                                                                Tob2012b
02255-1834   GWP 315     ABL  40.                                                                Tob2012b
02256+5017   BUP  31     65 And.                                                                         
02257+6133   STF 257     The primary is SB1 V559 Cas, P = 1.58 d.                                        
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
02257+0846   GWP 316     XMI 263.                                                                Tob2012b
02257-2119   HJ 3500     HIP 11324. B = HIP 11323. Both components are below the MS, the true            
                         parallax should be 12.6 mas (as for the B-component in Hipparcos).      Tok2011a
02258-1038   HJ 2140     Identical with HJ 2134, 4 minutes west.                                         
02259+1747   JNN  19     LP 410-22.                                                                      
02260+4228   LDS3383     Aka SLN  57.                                                                    
02260-1520   H 3  80     H III 80. A is a variable of the Alpha CVn type, AB Cet, and a                  
                         spectroscopic binary.                                                           
02262+3428   HDS 318     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.48 +/- 0.19, 1.81, and 1.80 Msun, respectively.             Mlk2012 
                         The spectroscopic orbit of this pair has been computed.                 Grf2018e
                         Orbital parallax 21.02 +/- 1.5 mas. Mass-A is 0.99 +/- 0.15 \msun.      ATl2021 
                         Mass-B is 0.95 +/- 0.13 \msun.                                                  
                         Mass-A is 1.08 +/- 0.07 and Mass-B is 0.96 +/- 0.06 \msun.              EEA2021 
02262-0833   GWP 318     ABL  42.                                                                Tob2012b
02262-1602   GWP 317     ABL  41.                                                                Tob2012b
02263+0618   VIG   2     The B component appears to be a faint background star.                  Vig2012 
02265+5417   STF 260     HJL  37.                                                                HJL1986 
02268+5853   HD  14947   Garmany & Stencel (1992 A&AS 94, 211) include this star in Per OB1.     Msn1998a
02268+1034   STTA 27     B is BD+09@322. A is VW Ari, a Delta Scuti-type variable.                       
02269+3733   ADM   2     WSP  33. WASP-33. Primary is del Sct-type variable and exoplanet host.  Adm2013 
02270-0326   GWP 319     ABL  43.                                                                Tob2012b
02272+0309   GWP 320     XMI 264.                                                                Tob2012b
                         HIP 11417. SB, no orbit. NOMAD: PM(B)=(-12,-68), V=14.73.               Nrd2004 
                         Primary is SB2, P=5.997d, but the mass ratio is unknown.                Tok2014d
02273+5433   LAW  10     LSPM J0227+5432. Law et al (2008) derive a distance of 18.6 +9.5/-3.4   Law2008 
                         pc and a projected separation of 13.2 +7.2/-2.2 au. Estimated spectral          
                         types are M4.5 and M5.                                                          
02273-0304   GWP 321     ABL  44.                                                                Tob2012b
02274+3059   INN   1     Rotation periods 12.1d (AG Tri, 13.7d wrong) and 4.7d.                  Skf2013 
02274+1807   GWP 322     XMI 265.                                                                Tob2012b
02278+0426   A  2329     Using the Hipparcos parallax value of 60.22 +/- 1.75 mas, the orbital           
                         elements of Andrade (2007) yield a mass sum of 1.25 +/- 0.14 Msun.      Ana2007 
                         Masses of the two K7V components are estimated at 0.63 +/- 0.01 and             
                         0.62 +/- 0.01 Msun.                                                             
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.37 +/- 0.12, 1.25, and 0.65 Msun, respectively.             Mlk2012 
02279+4710   BWL  10     AB: Primary is a probable member of the AB Dor moving group.            Bwl2015 
02280+0248   GWP 324     XMI 266.                                                                Tob2012b
02280-0520   GWP 323     ABL  45.                                                                Tob2012b
                         WDS designation corrupted at some point to 02280-0303. Corrected.               
02280-3349   SHY 140     HIP  11477 + HIP  11448.                                                        
02281+3251   ES 2407     GCB 6.                                                                          
02282+5423   STF 267     B is BD+53@530.                                                                 
02282+2952   STF 269     STT  41. May also be H 1  21.                                                   
02284-0404   GWP 325     ABL  46.                                                                Tob2012b
02286+5521   ES  872     There is a difference of 18 degrees in the measured angles. The Espin           
                         measure appears correct.                                                Es_1910b
02286-0704   A   447     WSP  77.                                                                        
02287+1850   GWP 326     XMI 267.                                                                Tob2012b
02287-3114   TOK  73     HIP 11537. The V-photometry is affected by small separation. B is red           
                         in the V-K color, variable? Astrometric binary in HIPPARCOS (Makarov            
                         and Kaplan), possibly new triple?                                       Mkr2005 
                         PMS star (Torres et al. 2006).                                          TrC2006 
                         SIMBAD: PMS star and X-ray source 1RXS J022843.6-311332.                Tok2011a
                         Companion is partially resolved in 2MASS images, for that reason the            
                         star is not found in the 2MASS point-source catalog. Pre-main-sequence          
                         star according to SIMBAD.                                               Tok2012a
                         A hierarchical quadruple. The resolved pair has an estimated period of  Tok2020h
                         3000 years while their are two closer spectroscopic components, one             
                         with a period of 22d while the other is 1146d.                                  
02288+3215   WOR   2     Tamazian et al. derive a dynamical mass sum of 1.40 +/- 0.25 Msun       Tam2005 
                         and classify the stars as K6-7V and M0V. Absolute magnitudes of                 
                         the two components are estimated at +8.0 and +8.6, leading to                   
                         individual masses of 0.65 and 0.61 Msun, in good agreement with                 
                         the dynamical mass sum.                                                         
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.46 +/- 0.20, 1.25, and 0.55 Msun, respectively.             Mlk2012 
02288-0826   GWP 327     ABL  47.                                                                Tob2012b
02290-0302   GWP 328     ABL  48.                                                                Tob2012b
02291+6724   STF 262     iot Cas. The primary is an unresolved binary, also an Alpha CVn                 
             CHR   6     type variable, P = 1.74 d, and an astrometric, spectroscopic, and               
                         spectrum variable (Rakos 1962; Klock, AJ 70, 176, 1965). The RV         Rak1962 
                         variation has not been confirmed.                                               
                         Heintz (1962) also detected this pair as a submotion to the visual      Hei1962 
                         orbit of the AB pair with a period of 52 years and an amplitude of              
                         0".11. Star C (mag. 8.4, dG4) is probably physical, but Hopmann         Hop1960b
                         (1960) computed a hyperbolic orbit for it, as there is some RV                  
                         difference between C and A.   q = periastron distance in the true               
                         orbit = 6".7056. All hyperbolic orbits were rejected from the                   
                         Fourth and subsequent orbit catalogs.                                   Wor1983 
                         Soderhjelm gives Aa,Ab,B,C quadruple solution (AB in HIP). High         Sod1999 
                         mass-sum, strangely well-behaved speckle obs at  Delta m=4?                     
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Drummond et al. (2003) give solution for Aa,Ab incorporating motion of  Dru2003 
                         the AB pair. The authors conclude that the motion of B relative to              
                         the CHR pair appears to be rectilinear. Masses of the CHR components            
                         are derived.                                                                    
                         1985.8540: This autocorrelogram was remeasured; the new results are             
                         listed in the catalog.                                                  McA1987b
             STF 262     AB: H 1  34.  AC: H 3   4.                                              MEv2010 
                         AC: Hyperbolic orbit.                                                   Hop1960b
02291+2331   VBS   6     The inclination must be high.                                                   
02294+5532   STF 268     A is a spectrum variable and shell star.                                        
02296+6039   STF 263     A is a possible Beta Cep variable, V528 Cas.                                    
02297-0030   GWP 329     ABL  49.                                                                Tob2012b
02297+0134   GWP 330     XMI 268.                                                                Tob2012b
02297-0955   GAL 321     Object #69 in Gallo's original list.                                    Gal1912b
02305+2514   STF 271     AB: H N  12.                                                            MEv2010 
02307-0407   GWP 331     ABL  50.                                                                Tob2012b
02308+5533   STF 270     AB: HJL  38.                                                            HJL1986 
                         Is there a wobble in the PA of AB?                                      Tok2014d
02309+0158   GWP 332     XMI 269.                                                                Tob2012b
02310+1358   GWP 333     XMI 270.                                                                Tob2012b
02310+0823   GIC  32     G004-024/G073-059.                                                              
02312+0811   LDS3396     Aka NSN 527.                                                                    
02313-1310   GAL 322     Object #70 in Gallo's original list.                                    Gal1912b
02315+0106   SHY 422     BC: HIP  11736 + HIP  12728.                                                    
02318+8916   STF  93     alp Umi = 1 UMi = Polaris. Cepheid variable and spectroscopic binary,           
                         P = 30y. A close companion has been suspected. The close pair,                  
                         measured three time from 1937-1939 by R.H. Wilson using an eyepiece     WRH1941b
                         interferometer, was not seen again until Evans et al. (2006) resolved   Evs2006 
                         it with HST.  Wilson's measures agree with the combined astrometric/            
                         spectroscopic solution by Gerasimovic (1936), although both orbit and   Ger1936 
                         measures are called into dispute by the more recent orbit of Wielan et  Wln2000 
                         al. (2000), whose solution includes mass estimates, etc.                        
                         NPOI Limb-darkened diameter 3.28 +/- 0.02 mas,                          NOI1999 
                         R = 46. +/- 3. \rsun.                                                           
                         An earlier orbit by Wyller (1957) was rejected from Fourth Orbit        Wye1957 
                         Catalog ("amplitude below noise level")                                 Wor1983 
                         Component B = BD+88@@@7. See discussion of this system by Roemer.       Re_1965 
                         While Hipparcos parallax of A 7.56 +/- 0.48 from the original mission   HIP1997a
                         and 7.54 +/- 0.011 mas from the re-reduction, the HST-FGS parallax of   VlF2007 
                         B = 6.26 +/- 0.24 mas implies that that A is high luminosity and        BdH2018 
                         pulsating in the second overtone if AB is physical, i.e., the distance          
                         to B is the same as A.                                                          
                         The C component was observed by Burnham in the late 19th century, then  Bu_1894 
                         not seen again until the early 21st century by Daley and Ashcroft.      Dal2006a
                         The extremely large magnitude makes the pair too close for most large           
                         astrometric surveys.                                                            
                         The D component has also been recently recovered in 2MASS data.         TMA2003 
                         According to Jim Daley, the R-I color for C is 0.56 and for D it is             
                         0.67. The V-I color for D is 1.08.                                      Dal2006b
                         Published measures precessed to J2000 are here "X" coded. Measures      CIA2024c
                         precessed back to date of observation to maintain consistency with              
                         other cataloged measures.                                                       
                         Mean diameter of the primary is 3.143 +/- 0.027 mas. At the Gaia                
                         distance of 136.90 +/- 0.34 pc this corresponds to 46.27 +/- 0.42 \rsun         
                         and the mass of the Cepheid is 5.13 +/- 0.28 \msun.                             
                         AB: H 4   1.                                                            MEv2010 
02318-0021   GWP 334     ABL  51.                                                                Tob2012b
02319+5742   BU 1314     V425 Per. Variable in light and radial velocity.                                
02319+0108   LDS9132     Old LDS6132. Primary is confirmed quasar: Z = 1.26.                             
02320+1822   STF 273     H N 106.                                                                MEv2010 
02320-1955   BRT 297     LDS3400.                                                                        
02321-1515   GWP 335     ABL  52.                                                                Tob2012b
                         sig Cet. B is BD-15@@447.                                                       
                         SHY 141. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
02322+5415   HJ 2142     Neither AB, AC or BC are physically associated.                         Kiy2015c
02323+4630   BRT 330     Since precise position has been corrected from previous precise         WSI2002 
                         position null detection not relevant.                                           
02324-1849   GWP 336     ABL  53.                                                                Tob2012b
02327+6127   STI 368     Both visual components were observed and appeared to be single.         Msn1998a
             MZA   8     EL and EM pairs were originally 02326+6128 MZA   8AB and AC, until              
                         match of E component of 02327+6127 to primary of 02326+6128 noticed.            
02327+0704   GWP 337     XMI 271.                                                                Tob2012b
02328+0021   GRV1174     SLW 119.                                                                        
02328-3421   LDS9133     Old LDS6133.                                                                    
02329+3433   GC 3048     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
02329+1502   TOK  12     Estimated period of visual pair 160y.                                   Tok2006 
                         Primary is SB2, P=19.4161d (Katoh et al. 2013 AJ 145, 41)               Tok2014d
02330+4852   HJ 2144     B is BD+48@694.                                                                 
02331-7738   BVD  25     B is CPD-78@59.                                                                 
02332+7013   RBR  34     Suspected non-single.                                                   Hor2002b
02332-2207   DON  35     CD-22@863.                                                                      
02333+5219   STT  42     Distance small, measures often discordant.                                      
                         1982.7604: This autocorrelogram was remeasured; the new results are             
                         listed in catalog.                                                      McA1987b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.00 +/- 1.28, 4.13, and 2.19 Msun, respectively.  Mlk2012 
02333-1933   GWP 338     ABL  54.                                                                Tob2012b
02333-7554   HJ 3522     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
02335+5732   HJ 2143     B is BD+56@657.                                                                 
02338-2814   HJ 3506     ome For.                                                                        
02340-1812   BRG  13     There is insufficient motion between the two epochs of observation of           
                         2MASS J02335984-1811525 to establish common proper motion of the                
                         binary, but the components are nearly equal brightness and color, and           
                         reside at a relatively small separation of ~0.85" hence it is almost            
                         certainly a physical pair.                                              Jnn2012 
02342+0916   GWP 339     XMI 272.                                                                Tob2012b
02342+0139   LDS9134     Old LDS6134.                                                                    
02343+4017   AG   42     STF 275.                                                                        
02344+3542   J  1810     ALI 35.                                                                         
02344+2040   A  2218     Identification error in ADS. Pair is BD+20 426, not BD+19 375.          Cou1970c
02344-4259   HJ 3510     Spectrum: G3/5III/IV.                                                           
02347-0752   BUP  32     77 Cet.                                                                         
02350-1522   GWP 340     ABL  55.                                                                Tob2012b
02351-1046   GAL 323     Object #71 in Gallo's original list. Aka J  1452.                       Gal1912b
02352+0407   TOK 649     Resolved using ANDICAM2. Primary SB?                                    Tok2014d
02353+4017   A  1818     Baize suspected another close pair in the region.                               
02353-0334   MUG   2     Followup spectroscopy confirmed the B component is a dwarf; estimated   Mug2005 
                         mass is 0.286 +- 0.017 Msun. Primary is planet host star. Colors of B   Egn2007 
                         component consistent with M1-M4 dwarf with mass 0.31 +/- 0.02 Msun.     Met2009 
                         HIP 12048. The B component estimated mass 0.29Msun.                             
                         2001.7454: PA is measured in zenith mode. If data collected in                  
                         equatorial mode, PA = 183.7.                                            Rbr2011d
                         CHARA Array Limb-darkened diameter  0.490 +/- 0.049 mas.                CIA2009a
                         R =  2.05 +/- 0.21 \rsun, L =   2.3 +/-  0.1 \lsun,                             
                         Teff = 4982 +/- 254 K.                                                          
             79 Cet      A: Combined solution, based on reduction of Hipparcos intermediate              
                         astrometric data together with spectroscopic elements from Marcy et al. CPS2000b
02354-0228   GWP 341     ABL  56.                                                                Tob2012b
02355+5948   HIP  12062  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Latham et al. (2002). They derived component masses 0.96 and 0.45 Msun  Lat2002 
                         and an estimated semimajor axis of 35.47 mas.                           Ren2013 
02356+6106   RAO   7     Primary is close astrometric binary; also SB?                           Tok2014d
02356+3719   STF 279     AB: H N  47.                                                                    
02358+3441   AG  304     15 Tri. B is BD+34@471.                                                         
02359+6338   CTT   3     The B component is BD+62@423.                                                   
02359+1515   GWP 342     XMI 273.                                                                Tob2012b
02359+0536   STF 281     nu Cet = 78 Cet                                                                 
                         The A component is a 714d spectroscopic binary. B is not a binary, so           
                         this is a physical triple.                                              Grf2015a
02359-2830   SWR   4     CPM pair                                                                Skf2004 
02360-0750   BUP  33     80 Cet.                                                                         
02360-1312   GWP 343     ABL  57.                                                                Tob2012b
02360-2331   GIZ   1     GJ 1048.  Discovered by Gizis et al. (2001) on 2MASS images. The A      Giz2001 
                         component is K2V; conclude secondary is L1, mass ~0.077 Msun.                   
                         Seifahrt et al. (2004) combine 2MASS measure with earlier UK Schmidt    Sef2004 
                         near-IR southern survey data to show stars have similar proper motion,          
                         so are likely physical companions.                                              
02361+0653   GKI   1     AB: This object was misidentified as HD 61660 by McAlister (1978).      McA1978c
                         PTI Limb-darkened diameter = 0.941 +/- 0.07 mas,                        PTI2001 
                         R = 0.729 +/- 0.064 \rsun.                                                      
                         VLTI Limb-darkened diameter  0.936 +/- 0.07 mas,                        LTI2003a
                         M = 0.790 +/- 0.039 \msun, R = 0.708 +/- 0.05  \rsun.                           
                         CHARA Array Limb-darkened diameter of A :                               CIA2012f
                         R =  0.7949 +/- 0.0062 \rsun, L =  0.26790 +/-0.00239 \lsun,                    
                         Teff = 4662 +/-  17 K, M = 0.767 \msun.                                         
             PLQ  32     AC: GJ 105. Proper motion of A +1811 +1451 (FK5). Spectroscopic binary          
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         HIP 12114. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
02362-1656   GWP 344     ABL  58.                                                                Tob2012b
02363+4012   BAZ   2     V377 And, Algol-type eclipsing binary, period 4.0632 d.                 Zas2018 
02363-0500   GWP 345     ABL  59.                                                                Tob2012b
02363-6329   B  1435     Spectral type F6?                                                               
02366+1231   GWP 346     XMI 274.                                                                Tob2012b
02366+1227   MCA   7     31 Ari. This system has a small Delta m (~0.1 in the blue, 0.3 in the           
                         red) as determined from lunar occultation measures by Africano et al.   Afr1978 
                         Measures in 1982.7659, 1984.7046, and 1988.6544 were based on           Hrt1994 
                         reprocessing of archival video data.                                    Hrt2000a
                         Martin et al. (1998) derive component masses 11.001 +/- 1.969 and               
                         9.407 +/- 1.707 Msun.                                                   Mig1998 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 19.08 +/- 2.57, 2.95, and 1.13 Msun, respectively.            Mlk2012 
02368+1723   BPM  53     [PM2000]   95004 + [PM2000]   94927.                                    Gvr2010 
02368-1929   ARA 523     BRT1374.                                                                Brt1935b
02369+5953   STF 277     V791 Cas, a Beta Lyr type eclipsing binary, P = 2.88680d.               Zas2012 
02370+2439   STFA  5     30 Ari. STTA 29. A is 1.1d SB1; AB has estimated period of 34,000y.     Tok2006 
                         B is BD+24@375.                                                                 
                         HJL  39.                                                                HJL1986 
                         SHY 142. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         H 5  49.                                                                MEv2010 
                         Primary is SB2, P=1.109d. B is exoplanet host, P=335d. A is F6III, but          
                         on the MS.                                                              Tok2014d
             RAO   8     BC: Exoplanet host star. Roberts et al. (2015) estimate the spectral            
                         types of B and C as F8V and M1V.                                        Rbr2015a
02370-3435   MUG  12     Primary is GJ 9088 = lam 2 For. Spectral type of comoving secondary             
                         estimated as M5-6, confirmed by follow-up spectroscopy. Mass of                 
                         secondary ~0.11 Msun.                                                   Mug2014 
02371+6232   MLR  31     No significant movement since first resolution.                         Drd2009 
02371+1740   GWP 347     XMI 275.                                                                Tob2012b
02371-0926   ITF  62     BD: Originally 02368-0926ITF  62.                                               
02371+0055   LDS5388     Error in WDS designation - incorrect precession of Luyten coordinates?  Luy1984 
02371-2951   LDS3405     NLTT 8520/8519                                                          Chm2004 
02374-5233   EHR   2     Primary is eta Hor. Physical/optical nature ambiguous.                  Ehr2010 
             TOK 186     Aa,Ab: The Marion et al. (2014) measure is in good agreement with the   Mrn2014 
                         Hartkopf et al. (2012) discovery observation, but hints at a            Tok2014a
                         significantly eccentric and/or inclined orbit. A face-on, circular              
                         orbit with a semimajor axis of 3.6au would have a period of ~3.7y,              
                         which is in line with the 3.0y astrometric period found by Goldin &             
                         Makarov (2007).                                                         Gln2007 
02376+2250   LDS1132     NLTT 8503/8502                                                          Chm2004 
02378+1737   BPM  54     [PM2000]   95638 + [PM2000]   95705.                                    Gvr2010 
02380+1418   GWP 348     XMI 276.                                                                Tob2012b
02381-0541   SLW 126     Aka ABL  60.                                                                    
02382+4604   A  1278     A premature orbit has been computed.                                            
02382-1123   STF 288     H 3  79.                                                                MEv2010 
02383-3012   UC  766     CPM candidate confirmed physical by photometry (2MASS and V mags).      Tok2013c
02386+0327   KUI   9     HR 775 in Cetus. Some scatter in measured position angles.                      
02387-5257   COO  14     Spectrum: F8IV/V + G/K.                                                         
             SHY 424     AC: HIP  12326 + HIP  12361.                                                    
02388+3325   STF 285     H 1  21.                                                                MEv2010 
02389+1526   AG   43     HU 1043.                                                                        
02389-5450   HJ 3520     B is CPD-55@444.                                                                
02390+6235   STTA 28     B is BD+61@445.                                                                 
02390+1452   STF 287     H N 107.                                                                MEv2010 
02392-0016   GWP 350     ABL  62.                                                                Tob2012b
02392-0933   GWP 349     ABL  61.                                                                Tob2012b
02394-0318   GWP 351     ABL  63.                                                                Tob2012b
02396-1152   FIN 312     eps Cet = 83 Cet. Pourbaix gives combined solution for this resolved            
                         SB2, yielding orbital parallaxes and component masses.                  Pbx2000b
                         Arenou give combined solution of astrometric orbits and DSBs. Paper             
                         includes masses and distances.                                          Are2000 
                         Systematic errors are clearly present and the period remains in doubt.  Fin1954c
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.68 +/- 0.35, 2.39, and 2.40 Msun, respectively.             Mlk2012 
                         Docobo & Andrade (2013) derive a dynamical parallax of 41.43 +/- 0.68           
                         mas and component masses 1.37 +/- 0.09 and 1.03 +/- 0.08 Msun. See              
                         paper for extensive notes on this system.                               Doc2013d
                         CHARA Array Limb-darkened diameter of A :  2.126 +/- 0.014 mas,         CIA2007 
                         R =  0.735 +/- 0.005 \rsun.                                                     
02398-1522   GWP 352     ABL  64.                                                                Tob2012b
02398-3354   LDS3413     HIP 12411. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
02399+0009   A  1928     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.83 +/- 0.56, 2.33, and 1.05 Msun, respectively.             Mlk2012 
02399-2429   TOK 205     A faint companion near the detection limit is found, our measures are           
                         uncertain. The estimated long period P ~ 100 yr suggests that the               
                         Hipparcosacceleration of 17 mas yr-2 is spurious.                       Tok2012a
                         The tentative resolution on 2011.84 at 78deg, 0".34, dK=3.8 is not              
                         confirmed here, with new good-quality images. The star has constant RV          
                         so could be single.                                                     Tok2013b
02401+1148   FAR  30     Primary is white dwarf WD 0237+115.                                     Far2006 
02401+0255   UC  771     CPM candidate confirmed physical by photometry (2MASS and V mags).      Tok2013c
02402+0436   HDS 347     Mean motion indicates P ~ 90 yr, rho increasing.                        Msn1999b
02404-1914   RST2285     Despite being nearby the WDSS pair 0240239-191332 appears unrelated.            
02405-1341   GAL 324     Object #74 in Gallo's original list.                                    Gal1912b
02406+3420   WNO  43     Aa,Ab: Identified as WNO  13 by Routley.                                USN1972 
             GIC  33     AB = G074-039/G074-040. AC = G074-039/G074-041.                                 
                         AB: NLTT 8633/8634                                                      Chm2004 
02407+6117   STF 284     A is a Beta CMa-type variable, V482 Cas.                                        
             CHR 208     Both visual components were observed: A was resolved (CHR 208Aa,Ab),            
                         B appeared to be single.  Gies & Bolton (1986) found a large scatter    Gie1986 
                         in radial velocities (but could not find a suitable period), and this           
                         suggests that at least one component may be a spectroscopic binary.     Msn1998a
02407+2704   STF 289     33 Ari. A spectroscopic binary.                                                 
                         HJL  41.                                                                HJL1986 
                         H 4   5.                                                                MEv2010 
02407+2637   STT  43     Scardia et al. (2001) orbit considered preliminary because the arc of   Sca2001d
                         the observed orbit is only 90 degrees and is placed completely around           
                         aphelion. The Hipparcos parallax of 0".01385 +/-  0.00125 gives a mass          
                         sum of 3.1 Msun, an overestimate for a star of type F7V. The dynamical          
                         parallax of 0".0149 agrees well with the measured one.                          
02410+6539   STF 282     AB: HJL  40.                                                            HJL1986 
02410+3905   A  1820     AB: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
02410-2506   LDS3414     NLTT 8688/8689                                                          Chm2004 
02412-0042   STF 295     84 Cet. A is a Delta Scuti-type variable.                                       
                         CHARA Array Limb-darkened diameter of A :                               CIA2013c
                         R =  1.2080 +/- 0.0288 \rsun, L =   2.1332 +/-0.0825 \lsun,                     
                         Teff = 6356 +/-  46 K, M = 1.168 \msun, Age = 2.1 Gyr.                          
02413+2659   L    55     Since precise position has been corrected from previous precise         WSI2013 
                         position null detection not relevant.                                           
02413-0432   BWL  12     Colors and/or astrometry are inconsistent with a late-type common               
                         proper motion companion based on visual inspection of the field from            
                         2MASS, SDSS, DSS1, and/or DSS2. Primary is G 75-35.                     Bwl2015 
02413-5725   BRG  14     2MASS J02411909-5725185 is yet to be confirmed as a common proper               
                         motion binary, but the color and brightness of the companion are well           
                         consistent with it being bound.                                         Jnn2012 
02414+3629   HJ  328     Aka ALI 269.                                                                    
02415+4053   COU1511     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.86 +/- 1.13, 2.54, and 1.05 Msun, respectively.             Mlk2012 
02415+1115   GWP 353     XMI 277.                                                                Tob2012b
02415-7128   B  1923     Actually a quadruple. Both A (1852d) and B (108d) are spectroscopic     Tok2022e
                         binaries.                                                                       
02418-5300   JFF   1     Aka CAB   6.                                                                    
02420+4248   HJ 1123     B is BD+42@588, spectrum B9IVp(Hg,Mn,Eu).                                       
02420-1824   GWP 354     ABL  65.                                                                Tob2012b
02421+1351   LDS3416     NLTT 8720/8721                                                          Chm2004 
02421-0134   OL    9     Since precise position has been corrected from previous precise         WSI2004b
                         position null detection not relevant.                                           
                         Aka RST4211.                                                                    
02422+4242   HJ 1124     Aka BKO 172.                                                                    
02422+4012   MCA   8     12 Per. SB2 resolved by speckle interferometry by McAlister (1977).     McA1977 
                         Elements P = 331.0d, T, e, and longitude of periastron for McAlister    McA1978a
                         solution are from the spectroscopic orbit by Colacevich (1941).         Cla1941 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Colacevich (1941).                                                              
                         Martin et al. (1998) derive component masses 1.125 +/- 0.169 and                
                         1.389 +/- 0.193 Msun.                                                   Mig1998 
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Bagnuolo et al. (2006) solution combines speckle data with data from    Bgn2006 
                         the CHARA Array. Authors derive orbital parallax 41.19 +/- 0.21 mas,            
                         masses 1.382 +- 0.019 and 1.240 +- 0.017 Msun, and a magnitude                  
                         difference 0.409 +/- 0.013 mags in K' (2136 nm). Values for omega and           
                         Omega are switched in their Table 3.                                            
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.59 +/- 3.80, 2.58, and 1.07 Msun, respectively.             Mlk2012 
02422-2445   LDS3418     NLTT 8753/8759                                                          Chm2004 
02423+1639   BPM  55     [PM2000]   98625 + [PM2000]   98718.                                    Gvr2010 
02423+1415   GWP 355     XMI 278.                                                                Tob2012b
02424+3837   EVT   1     Aa,Ab: Exo-planet host                                                  Tok2014d
02424+2001   BLA   1     Aa,Ab: mu Ari = 34 Ari. Occultation binary, known to have variable              
                         radial velocity.                                                        Bag1984b
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 3.64 +/- 0.47, 5.77, and 2.24 Msun, respectively.  Mlk2012 
02424+0247   GWP 356     XMI 279.                                                                Tob2012b
02424-0214   LDS9135     Old LDS6135.                                                                    
02424-1358   LDS3419     NLTT 8758/8757                                                          Chm2004 
02425+4016   STF 292     B is BD+39@611.                                                                 
                         H 4  64.                                                                MEv2010 
02425+1045   CHR 200     First detected as an occultation binary by Blow et al.                  Blw1982a
02426-5048   iot Hor     Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from Kurster      CPS2000e
                         et al. (2000).                                                          HaI2001 
             HD  17051   No comoving objects found within separation/magnitude range listed.             
                         However, Chauvin et al. (2006) note finding at least one faint          Cvn2006 
                         background object.                                                              
02426-7947   TOK 362     This 0.6" pair with dK=1.1 is obvious and should have been resolved             
                         both by visual observers and by Hipparcos, yet there are no                     
                         indications of previous resolution in the literature. The declination           
                         of -79deg may have something to do with the missed companion, as the            
                         southern sky is less well surveyed for binaries.                        Tok2013b
02427+3932   J  2401     Jonckheere says is two faint condensations of a nebula. Galaxy           .      
                         UGC 2180.                                                               J__1962a
02427+1434   GWP 357     XMI 280.                                                                Tob2012b
02427-1513   GWP 358     ABL  67.                                                                Tob2012b
02428+4249   HJ 2155     B is BD+42@605.                                                                 
02431+0330   GWP 359     AB: XMI 281AB.                                                          Tob2012b
             GWP 360     AC: XMI 281AC.                                                          Tob2012b
02433+1926   BAG  20     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin et al. (1985).                                                  Grf1985b
                         Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
                         However, this is a Hyades non-member                                    Grf1988 
                                                                                                 Grf2013c
02433+1718   BPM  56     [PM2000]   99282 + [PM2000]   99285.                                    Gvr2010 
02433+0314   STF 299     gam Cet = 86 Cet = Kaffaljidhma. AC is a CPM pair, according to Alden.  Ald1924 
                         AB: Additional notes may be found in Muller (1946).                     Mlr1946a
02434-3756   TOK 187     Triple. The A-component is 0.955d SB2; the tertiary is resolved with            
                         speckle. As A is located some 1.7m above the main sequence, the object          
                         can be closer than indicated by the Hipparcos parallax of 24.6 mas.     Tok2012a
02434-6643   FIN 333     Probably an ambiguous case, although only one solution has been                 
                         tested.                                                                         
                         More speckle obs needed to define orbit.                                        
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 14.55 +/- 4.04, 2.67, and 1.20 Msun, respectively.            Mlk2012 
02435+2742   35 Ari      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Abt & Levy (1978).                                                      AbH1978 
02435+1611   BPM  57     [PM2000]   99396 + [PM2000]   99434.                                    Gvr2010 
02438-2754   BU  261     Aka HDO  59.                                                                    
02440-0601   TOK  75     HIP 12764. A is SB, no orbit, dRV= 2.5). Contradictory photometry of    Nrd2004 
                         B, it is too close in 2MASS (5"). NOMAD: PM(B)=(-99,-71) V=7.79 (??)            
                         Considering the brightness of B and  N*=15, it is almost certainly      Tok2011a
                         physical. A new triple system. See Bonavita & Desidera (2007).          Bnv2007 
02442+4914   STF 296     the Per = 13 Per. A premature orbit has been computed.                          
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Data appear equally well fit by rectilinear solution - see catalog.             
                         CHARA Array Limb-darkened diameter  1.103 +/- 0.009 mas,                CIA2012e
                         R =  1.319 +/- 0.011 \rsun, L =  2.235 +/-0.040 \lsun,                          
                         Teff = 6157 +/-  37 K, M = 1.138 +/- 0.010 \msun,                               
                         Age =  4.0 +/- 0.4 Gyr.                                                         
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: H 3  58.                                                            MEv2010 
                         AC and BC: Rectilinear solution by Hurowitz et al. (2013).              USN2013a
02442-2530   FIN 379     Aa,Ab: More than one revolution apparently has occurred.                        
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 1.55 +/- 0.22, 2.20, and 1.02 Msun, respectively.  Mlk2012 
             BSO   1     HIP 12780. A is visual binary FIN 379, 0.1". B = HIP 12779.             Tok2011a
02443+5704   STF 293     AB: Additional notes may be found in van den Bos.                       B__1963b
02443+1600   GWP 361     XMI 282.                                                                Tob2012b
02445-1859   GWP 362     ABL  68.                                                                Tob2012b
02446+7912   BVD  26     Primary is V405 Cep.                                                            
02446+2928   STF 300     H 1  74.                                                                MEv2010 
02447+6128   KRV   3     Classical Cepheid DF Cas.                                                       
02448+4231   LDS3424     NLTT 8830/8829                                                          Chm2004 
02448+1536   KIR   7     A close double dwarf pair,spectral types M5V and M5.5V.                 Kir1999 
02449+5456   ES   50     Initially assigned as TDS  94. Corrected 11/27/01.                              
02449+1007   TOK   1     Aa,Ab: mu Cet = 87 Cet. Considered somewhat uncertain by Tokovinin.             
                         Not resolved by McAlister on several occasions.                                 
                         A preliminary spectroscopic orbit with a period of 1202 days has been           
                         published by Abt (1965).                                                AbH1965 
02449-1336   GWP 363     ABL  69.                                                                Tob2012b
02451-1834   tau 1 Eri   Despite a large acceleration of 26 mas yr-2, no RV variability was              
                         found in the GCS from two measures.                                     Tok2012a
02452-4344   CPO  29     LDS  78.                                                                        
             BRG  15     Aa,Ab: 2MASS J02451431-4344102 is a member of an approximately equal-           
                         brightness binary with ~50" separation, in addition to being a close            
                         binary discovered with AstraLux.                                        Jnn2012 
02452-6700   GLI  18     Spectrum: F5/6III/IV.                                                           
02455-6342   HDO 306     gam Hor. A spectroscopic binary.                                                
02456-7114   HDS 357     Primary is CN Hyi, a W Uma type eclipsing binary, period 0.45611d.      Zas2012 
02457+4456   LDS5393     old LDS6136.                                                                    
                         AB: NLTT 8869/8870                                                      Chm2004 
             GIC  34     AC = G078-004/G078-003 = GJ 3178A+3179B.                                        
02457-3943   B  2077     Astrometric orbit for primary, P=2.303y (Golden & Makarov 2007). PM(A)  Gln2007 
                         moves almost towards B, so the increased separation is not reflex PM.   Tok2014d
02460-0457   BU   83     A premature orbit has been calculated.                                          
                         A: Dommanget (1972) astrometric orbit calculated from perturbations     Dom1972a
                         seen to rectilinear motion.                                                     
02461+1250   GWP 364     XMI 283.                                                                Tob2012b
02462+0536   RAO   9     AB: Primary is HIP 12925. A 13.8m star at 221.7deg, 494.3" appears to           
                         share common proper motion, but the probability of physicality is only          
                         36%. It is likely this star is another member of the Tuc-Hor moving             
                         group.  HIP 12925 and 12862 also appear to be a co-moving pair.         Tok2013c
                         AB: The primary is a spectroscopic binary.                              Tok2014d
                         Quadruple system with 3-tier hierarchy: a close spectroscopic pair              
                         with yet unknown period, Robo-AO companion D at 1".89, and CPM                  
                         companion C at 494" (Tokovinin & Lepine 2012). Yet another star,        Tok2012c
                         HIP 12862, at 0.9deg, also shares common PM and parallax. The stars             
                         are young and belong to the Tucana–Horlogium moving group (Zuckerman    .     
                         et al. 2011 ApJ 732, 61). Our photometry places D slightly above the            
                         MS. D was  independently discovered by Brandt et al. (2014) by high-    Bdt2014 
                         contrast imaging at Subaru. They measured it on 2012.0 at 252.9 deg     RAO2015 
                         and 1".893, in excellent agreement with Riddle et al. (2015).           Rbr2015d
             TOK 651     AC: Tuc-Hor moving group? Additional CPM companions at 725" and 1536".  Tok2014d
                         AD: Too wide to be a companion at 3271", but CPM, common parallax. F            
                         is a rapid rotator (Vsini=109km/s), on main sequence.                           
02462-0619   GWP 365     ABL  70.                                                                Tob2012b
02463+1427   GWP 366     XMI 284.                                                                Tob2012b
02464+0301   GWP 367     XMI 285.                                                                Tob2012b
02470-0952   A  2608     The northern pair, CD, is slightly fainter                              Hei1985a
02470-1320   RST3371     Variable: CU Eri.                                                               
02472+3611   ALI  38     No star seen at AC catalog location of the purported secondary                  
                         - probably a plate flaw.                                                        
02473+1812   BPM  58     [PM2000]  102021 + [PM2000]  102010.                                    Gvr2010 
02473+1803   GWP 368     XMI 286.                                                                Tob2012b
02473+1717   A  2222     CD: Aitken gives the magnitude of B as 13.8. I could not see it at all          
                         on the first two nights, glimpsed it on the fourth, and made a very             
                         uncertain measure on the third. Variable?                               B__1962d
02474-1733   GWP 369     ABL  71.                                                                Tob2012b
02475+1922   STF 305     A premature orbit has been computed.                                            
02476+5357   STF 301     A is a long-period spectroscopic binary, P = 675d.                              
02476+1014   HJ  655     Hipparcos identified the B component as a candidate for Hyades          HIP1998 
                         membership. However, re-reduction of the Hipparcos parallax places      VlF2007 
                         the B component elsewhere, so this is an optical pair.                  Grf2013c
02478-0411   GWP 370     ABL  72.                                                                Tob2012b
02479-0529   GWP 371     ABL  73.                                                                Tob2012b
02480-0108   GRV 993     SLW 134.                                                                        
02480-0940   GAL 325     Object #76 in Gallo's original list.                                    Gal1912b
02480-2836   RED  20     One companion is ~10" from CD-29 1020 = 2MASS J02481094-2835382.  To            
                         the SW at a milar distance is 2MASS J02480263-2835465. There are no             
                         USNO-B1 proper motions for the fainter stars, but comparison of                 
                         Digitized Sky Survey UKST and 2MASS images show little evidence of              
                         significant relative motion. IR colors are consistent with a K0/M3/M6           
                         triple at 60pc. System appears non-hierarchical, with projected                 
                         separations of ~600au between each component.                           Red2007a
02481-1244   GAL 326     Object #77 in Gallo's original list.                                    Gal1912b
02482+2704   LDS1138     HIP 13081. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
             LDS1138     NLTT 8997/8996                                                          Chm2004 
02483+1532   BPM  59     [PM2000]  102707 + [PM2000]  102652.                                    Gvr2010 
02486+1344   GRV 146     NI    4.                                                                        
                         Primary is BQ Ari, a W UMa type eclipsing binary, period 0.282335d.     Zas2011 
02487+3107   GJ 9102     1981.6875: HD 17433 was misidentified as Gliese 113 by Balega et al.    Bag1984b
                         (1984). It is uncertain whether this observation is of HD 17433 or of           
                         GJ 113 = HD 17382.                                                              
02488-0301   GWP 372     ABL  74.                                                                Tob2012b
02489+3823   ALD  10     First measure probably 90@ in error.                                    Ali1955 
02490-1029   BRG  16     The system is precisely at the 3 sigma threshold for statistically              
                         significant exclusion of the background star hypothesis. By chance,             
                         the AB astrometry is just below the criterion (2.7 sigma) and BC is             
                         just above (3.1 sigma), so in principle the BC pair is inconsistent             
                         with chance alignment, if the pair does share a common proper motion            
                         with  A. However, the proper motion of the system has of course been            
                         determined based on A, so until the AB physical connection has been             
                         demonstrated to the required accuracy, the 3.1 sigma confidence of the          
                         BC pair is irrelevant. Hence, we label the entire system as                     
                         undetermined for now, although it is obviously very likely that the             
                         whole system is indeed bound.                                           Jnn2012 
02490-1432   KPP2871     Aka TOI 1201.                                                                   
02491-1712   GWP 373     ABL  75.                                                                Tob2012b
02491-3224   B  1031     bet For                                                                         
02493+1728   STF 311     pi Ari = 42 Ari. A is a spectroscopic and occultation binary.                   
                         AB: H 1  64.                                                            MEv2010 
02493-1033   STF 315     Rectilinear solution by Hartkopf & Mason (2013), however, the close     Hrt2013b
                         parallax and proper motion argues for an orbital solution.              Izm2019 
                                                                                                         
02494+4336   LDS3429     LDS9137. LDS6137.                                                               
                         NLTT 9035/9037                                                          Chm2004 
02495+5705   MCA   9     V480 Per.                                                                       
02496-0932   GWP 374     ABL  76.                                                                Tob2012b
02497+1209   CHR 201     First detected as an occultation binary by Evn1983a.                            
02498-0220   GWP 376     ABL  78.                                                                Tob2012b
02498-0346   GWP 375     ABL  77.                                                                Tob2012b
02498-2015   HJ 3533     B is BD-20@523.                                                                 
02498-2434   BU  877     gam 1 For. AB =? LDS  80. Separation and position angle (sf)                    
                         agree, as does the DM number from LDS catalog. The quoted primary               
                         magnitude of the LDS pair is much fainter, however - possibly a poor            
                         measure of CB instead?                                                          
02499+0856   STF 313     B component is EE Cet, a W UMa type eclipsing binary, P = 0.37992d.     Zas2012 
02499-0206   GWP 377     ABL  79.                                                                Tob2012b
02500+2716   MCA  10     Aa,Ab: 41 Ari = Bharani. Aa is a spectroscopic binary and resolved              
                         interferometer pair.                                                            
             STT  47     AB: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
             H 5 116     AC: H V 116.                                                                    
                         AC: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
             H 6   5     AD: H VI 5. D is BD+26@470.                                                     
02501+1646   GWP 378     XMI 287.                                                                Tob2012b
02502+7255   HJ 2157     Also known as STF 298.                                                          
                         Primary is V793 Cas, an Algol-type eclipsing binary, period 1.652303d.  Zas2011 
02502+1343   SHY 426     HIP  13223 + HIP  13122.                                                        
02502+0641   AG   55     AB,C: HJL  42.                                                          HJL1986 
02502-3551   HJ 3536     eta 2 For                                                                       
02504+3551   LDS3430     Old LDS6138. LDS9138.                                                           
                         NLTT 9076/9097                                                          Chm2004 
02505+1113   BPM  60     [PM2000]  104291 + [PM2000]  104261.                                    Gvr2010 
02505-0414   GWP 379     ABL  80.                                                                Tob2012b
02506+3819   BUP  34     16 Per.                                                                         
02507+5554   STF 307     eta Per = 15 Per = Miram. A is a spectroscopic binary. B is BD+55@712.          
                         Mk III Limb-darkened diameter  5.381 +/- 0.055 mas.                     MkT2003 
                         NPOI Limb-darkened diameter    5.260 +/- 0.073 mas,                             
                         R =  173.10 (+9.69-10.80)  \rsun,  Teff = 4082 +/-  30 K,                       
                         L = 7508.  +/- 864  \lsun.                                              NOI2023 
02507+1910   TOK  76     HIP 13269. The 2MASS PSC companion at 17.2" is likely an artifact (not          
                         detected in J and H bands). A is an astrometric binary.                 Tok2011a
02507+1601   BPM  61     [PM2000]  104457 + [PM2000]  104476.                                    Gvr2010 
02508-3956   SHY 427     AB: HIP  13271 + HIP  13499.                                                    
02509+0331   PLQ  36     LDS3432.                                                                        
02510+1317   GWP 381     XMI 289.                                                                Tob2012b
02510+1329   GWP 380     XMI 288.                                                                Tob2012b
02510-2100   SEE  20     tau 2 Eri = 2 Eri = Angetenar                                                   
02511+6025   STF 306     Spectroscopic binary, also classified Oe5V and O7.5.                            
                         AC: See BDS 1430.                                                               
                         AG: G component = A component of 02512+6023.                                    
             STI 398     EF: previously 02512+6025STI 298AB, merged with STF 206 system.                 
                         fh: previously 02512+6025STI 298bc, merged with STF 206 system.                 
02512+6023   D  9001     See BDS 1431.                                                                   
02513+0303   HO  218     Position angle and distance changing rapidly but                                
                         period not established. Needs speckle.                                          
02514-1526   GWP 382     ABL  81.                                                                Tob2012b
02514-2139   DON  43     Gomez et al. (2016) derive dynamical parallax and component masses:             
                         8.24 +/- 0.22 mas, 1.110 +/- 0.014 Msun, 1.045 +/- 0.013 Msun.          Doc2016i
02516+6033   BU 1374     B component spectral type B0III                                         AbH2000 
                         CD: Also known as STI 400.                                                      
02516+4803   HJ 2160     AB: Rectilinear solution by Cvetkovic et al. (2017).                    Cve2017 
02517+5921   GIC  35     G246-014/G246-013.                                                              
02518+5819   BLL   8     A is a spectroscopic binary. B is BD+57@652.                                    
02518-2117   SEE  21     This very close visual system was discovered at a separation of 0".36   See1898b
                         and has closed steadily for over 90 years. It is unknown at this                
                         point whether the system is still approaching periastron or has                 
                         begun to widen.                                                         Hrt1993 
02520-5347   BRT2020     CD-54@578.                                                                      
02521+1536   GWP 383     XMI 290.                                                                Tob2012b
02521-6054   HJ 3540     CD-61@515.                                                                      
02522+1520   BPM  62     [PM2000]  105424 + [PM2000]  105482.                                    Gvr2010 
02525+2505   LDS1140     NLTT 9175/9176                                                          Chm2004 
02525-1246   LWR   4     EP Eri                                                                          
02527-1105   GWP 384     ABL  84.                                                                Tob2012b
02529+5300   STF 314     AB,C: H 1  38.                                                          MEv2010 
02529+1040   AG   56     HD 17906, W UMa-type eclipsing binary, period 0.4238 d.                 Zas2018 
02531-1212   GAL 327     Object #78 in Gallo's original list.                                    Gal1912b
02532+4155   LDS9139     Old LDS6139.                                                                    
02532-1007   GWP 385     ABL  85.                                                                Tob2012b
02533+2714   ALP   8     2MASSI J0253202+271333                                                          
                         Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
02536-0745   GWP 386     ABL  86.                                                                Tob2012b
02536-3826   TOK 652     Primary is psi For                                                      Tok2014d
02537+3820   BU  524     AB: 20 Per. Barnard gives this as 20 Per = BU 520.                      Bar1898b
                         Star A is a suspected variable of Delta Scuti type. A suspected                 
                         spectroscopic 3.5 yr period is not confirmed (Scarfe & Fekel 1978).     Scf1978 
                         A measure on 1979.5326 was incorrectly attributed to ADS 2200 by                
                         McAlister & Hendry (1982); it actually belongs to ADS 490.              McA1982d
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Aristidi et al. (1999) orbit includes mass determination.               Ari1999 
                         Docobo et al. (2001) orbit includes mass determination.                 Doc2001c
                         Calculated mass sum is 3.88 +/- 0.58 Msun, a bit high for a pair of             
                         mid-F dwarfs.                                                           Mut2010b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.88 +/- 0.60, 2.99, and 1.38 Msun, respectively.  Mlk2012 
             STF 318     AB,C: HJL  43.                                                          HJL1986 
                         AB,C: H 3  60.                                                          MEv2010 
02542+3644   ES 2555     ALI 274.                                                                        
02542-1225   GWP 387     ABL  87.                                                                Tob2012b
02543+5246   LAB   1     Aa,Ab: tau Per = 18 Per. Spectrum composite; G4III+A4V. A is a                  
                         long-period spectroscopic binary, resolved by speckle interferometry.   Lab1974 
                         Speckle observations have resolved the pair and invalidate an                   
                         astrometric solution by Kamper (1969).                                  Kam1969a
                         van de Kamp & Andersen orbit rejected from Fourth Orbit Catalog         Kam1969a
                         ("amplitude below noise level")                                         Wor1983 
                         Time of 1989 mideclipse determined as JD = 2447542.31+/-0.01d.          DSH1991 
                         Eclipse duration is 2.09d. Inclination of orbit is 88.74deg.                    
                         Time of 1989 mideclipse determined as JD = 2447542.34d. Their model     REG1992 
                         results give 16 \rsun, 2.4 \msun, Sp G8IIIa and Teff = 5160+/-150 for           
                         the primary and 2.2 \rsun, 1.8 \msun, Sp A3/4V and Teff = 8970+/-150            
                         for the secondary. The mass ratio is 1.1+/-0.2.                                 
                         Time of 1989 mideclipse determined as JD = 2447542.302/-0.007d.         Smk1990 
                         Eclipse duration is 1.936+/-0.029d. P = 1515.869+/-0.059d.                      
                         Time of 1984 mideclipse determined as JD = 2446026.48+/-0.05d.          XXX1986 
                         Eclipse duration is 2.3-3.1d.                                                   
                         Zeta Aurigae-type binary.                                                       
                         The elements P, T, e, and longitude of periastron for the McAlister     McA1981c
                         (1981) orbit are from the orbit by Colacevich (1941).                   Cla1941 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Demircan & Selam (1992).                                                Dmr1992 
                         The 52" distant, visual double BC may be physical.                              
02544+0946   HJ  658     HIP 13543. B is a known close binary A 2341 of 1.3" separation,                 
                         partially resolved in the ANDICAM images in K and V bands.              Tok2011a
02544-0030   GWP 390     AB: ABL  88AB.                                                          Tob2012b
             GWP 391     AC: ABL  88AC.                                                          Tob2012b
02544+0635   GWP 388     XMI 291.                                                                Tob2012b
02544+1754   GWP 389     XMI 292.                                                                Tob2012b
02546+1306   BPM  63     [PM2000]  107057 + [PM2000]  107037.                                    Gvr2010 
02548+4332   HJ 2162     Star C is A of HJ 2163, BDS 1479.                                               
02548+2916   BRT 130     1deg error in WDS designation, apparently an error in transcribing              
                         coordinates from the original source. Appears to be the same as COU 677.        
02548-0640   GWP 393     ABL  89.                                                                Tob2012b
02548+1401   GWP 392     XMI 293.                                                                Tob2012b
02548-2754   HDO  58     Aka HDO  61.                                                                    
02549+1913   GWP 394     XMI 294.                                                                Tob2012b
02549-0709   JNN  21     The primary is an SB2 binary with an 11.8 day period (Torres et al.             
                         2002 AJ, 123, 1701). Since the angular confirmed to share a common              
                         proper motion) for the purpose of multiplicity statistics, although it          
                         is really a triple system. To estimate the mass of the primary for the          
                         purpose of deriving the mass ratio to the tertiary component detected           
                         in our images, we adopt the mass ratio of 0.58 derived from the                 
                         spectroscopic orbit and use the mass corresponding to an M3 spectral            
                         type for the primary.                                                   Jnn2012 
02550-1402   GAL 328     Object #81 in Gallo's original list.                                    Gal1912b
02552-0800   EGN   2     Pair likely unbound.                                                    Egn2007 
02552-4549   CPO 113     This is ESO 247-11, B is an interacting galaxies.                       Dam2010 
02553-0348   GWP 396     ABL  91.                                                                Tob2012b
02553-1209   GWP 395     ABL  90.                                                                Tob2012b
02555+0731   GWP 397     XMI 295.                                                                Tob2012b
02556+2652   STF 326     Parabolic orbit by Hopmann (1967).                                      Hop1967 
                         sigma = areal constant in the true orbit = 0.05215 arcsec^2/yr                  
                         q = periastron distance in the true orbit = 2".827                              
                         Data appear equally well fit by rectilinear solution - see catalog.             
02556+1311   HU 1047     Close, position angles scattered. No positive observations since 1937.          
02557-1223   GAL 329     Object #82 in Gallo's original list.                                    Gal1912b
02558+3429   LDS9140     BC: Old LDS6140.                                                                
                         NLTT 9308/9312                                                          Chm2004 
02558+1909   A  2342     Closing in with little angular change.                                          
02558-1606   GWP 398     ABL  92.                                                                Tob2012b
02559+1455   BPMA  3     [PM2000]  107836 + [PM2000]  107938.                                    Gvr2010 
02559-1521   LDS3441     NLTT 9361/9360                                                          Chm2004 
02560+1221   GWP 399     XMI 296.                                                                Tob2012b
02561+2003   HER   6     AC: Additional notes may be found in Herbig (1962).                     Her1962 
             CVN   6     Ca,Cb: COR   1Aa,Ab previously cataloged is actually this pair.                 
02562+2359   JNN 253     Estimated age 1000-10000 Myr; masses 0.07 +/- 0.02 and 0.07 +/- 0.01            
                         Msun; a ~0.4 au.                                                        Jnn2014 
02563+5852   STF 321     B is BD+58@531.                                                                 
02563-1816   GWP 400     ABL  93.                                                                Tob2012b
02564+1534   BPM  64     [PM2000]  108162 + [PM2000]  108210.                                    Gvr2010 
02564-1722   LDS3442     NLTT 9390/9388                                                          Chm2004 
02565+6322   MLB 390     Also known as STI 405.                                                          
02565+5526   LDS5401     Duplicity first noted by Ross: Ross 364-5.                              Ros1926 
02567+4248   LDS9141     old LDS6141. A is possibly the same as A of LDS2815.                            
                         AB: NLTT 9354/9355                                                      Chm2004 
02570+1244   BPM  65     [PM2000]  108547 + [PM2000]  108528.                                    Gvr2010 
02571-1244   GWP 401     MBL   1.                                                                Tob2012b
02572+1157   GWP 402     XMI 297.                                                                Tob2012b
02572+0153   A  2413     Component variable?                                                     Hln1963 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         According to Scardia et al. (2001), this orbit is now well defined and  Sca2001d
                         will certainly change little in the future; only the period is still            
                         slightly uncertain. The Hipparcos parallax is 0".02012 +/- 0.00150.             
                         This gives a mass sum of 2.1 Msun +/- 29%, agreeing very well with              
                         expected values for a system of type G0. Compared to the orbit                  
                         calculated by Scardia in 1980, the total mass of the system, whose      Sca1980e
                         uncertainty was then 55%, is now much better defined. The dynamical             
                         parallax is 0".0193, well in agreement with the measured parallax.              
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.64 +/- 0.52, 2.04, and 1.05 Msun, respectively.             Mlk2012 
02572-2458   BU  741     Rica (2012) derived a dynamical parallax of 45.0 mas (compared with     FMR2012g
                         44.51 +/- 2.09 mas from Hipparcos) and a mass sum (using the Hipparcos          
                         parallax) of 1.5 +/- 0.3 Msun.                                                  
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.46 +/- 0.44, 1.66, and 0.79 Msun, respectively.  Mlk2012 
02573+3156   DCH 116     21 Per.                                                                         
02578+4431   STF 328     Statistically the same parallax within the errors would indicate the            
                         components are physical.                                                        
02579+6400   STI 409     PTT 7.                                                                          
02579+0025   STF 332     HJL  44.                                                                HJL1986 
02581+6912   STF 317     BDS mentions a third star 15 sec f at 102.4@.                                   
02582+0310   GWP 403     XMI 298.                                                                Tob2012b
02583-0002   GWP 404     MBL   2.                                                                Tob2012b
02583-4018   PZ    2     the Eri = Acamar. A is a spectroscopic binary.                                  
02584-0135   A   208     C is BD-02@528.                                                                 
02585-1453   GWP 405     MBL   3.                                                                Tob2012b
02586+2408   BU 1173     Star C (mag. 13, 4.6") is probably physical.                                    
02586+1741   HO  498     Last star in a row of four. STT 49 20' n, 1.9m f.                       Ho_1899a
02586+1302   GWP 406     XMI 299.                                                                Tob2012b
02586-1628   GWP 407     MBL   4.                                                                Tob2012b
02588+4322   LDS2816     B is BD+42@664.                                                                 
02590-0746   GRV 996     SLW 141.                                                                        
02592+2120   STF 333     eps Ari. Variable velocity suspected.                                           
                         Rica (2012) derived a mass sum (using the Hipparcos parallax 9.81 +/-   FMR2012g
                         0.79 mas) of 7.4 +/- 1.8 Msun.                                                  
02594+6034   TRN  14     The image rotator was in an unknown state, so two possible theta                
                         values are listed for the 2001.7451 observation - one for zenith up             
                         and one for north up.                                                   Trn2008 
                         Position angle ambiguity solved by Jesus Maiz Apellaniz.                        
02595+3916   BRT2202     ALI 763.                                                                        
02596+3849   MLB1002     ALI 764.                                                                        
02596+0508   BAL2603     J 1811.                                                                         
02596-1436   LDS3445     NLTT 9570/9569                                                          Chm2004 
02596-2516   LDS3446     zet For                                                                         
                         NLTT 9579/9563                                                          Chm2004 
02598+3856   LAW  11     LSPM J0259+3855 = NLTT 9527. Law et al (2008) derive a distance of      Law2008 
                         18.8 +9.3/-3.4 pc and a projected separation of 17.6 +9.4/-2.8 au.              
                         Estimated spectral types are M4.5 and M5.5.                                     
03001+6244   STI 417     MLB 391.                                                                        
03001+3911   ALI 765     A is the eclipsing binary ST Per.                                               
03001+1139   BPM  66     [PM2000]  110407 + [PM2000]  110416.                                    Gvr2010 
03002-1110   BRT2627     J 1454.                                                                         
03006+4753   A  1529     Round 1951 - 1954.                                                              
03007+5700   KR   15     Heintz gives the correct identification and position.                   Hei1983a
03008+1527   BPM  67     [PM2000]  110893 + [PM2000]  110922.                                    Gvr2010 
03009+5940   STTA 31     B is BD+59@581.                                                                 
03009+5221   STF 331     Both components are spectroscopic binaries.                                     
                         H 3  36.                                                                MEv2010 
03011+4453   HJ 2167     AB: HJL  45.                                                            HJL1986 
03012-1816   GWP 408     ABL  94.                                                                Tob2012b
03013+6035   MLR 108     V1018 Cas, an Algol-type eclipsing binary, period 4.12781d.             Zas2011 
03013-0636   GWP 409     ABL  95.                                                                Tob2012b
03014+1607   BPM  68     [PM2000]  111250 + [PM2000]  111338.                                    Gvr2010 
03014+0615   HDS 385     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.20 +/- 0.32, 1.76, and 1.82 Msun, respectively.             Mlk2012 
                         Teff for A & B : 5670 +/- 100 and 5580 +/- 100 K                        Mda2018 
                         R    for A & B : 0.877+/-0.08 and 0.821+/-0.07 \rsun                            
                         L    for A & B : 0.71 +/-0.06 and 0.59 +/-0.09 \lsun                            
                         M    for A & B : 0.99 +/-0.19 and 0.96 +/-0.15 \msun                            
                         Age = 11.5 +/- 2 Gyr.                                                           
03014-1409   GWP 410     ABL  96.                                                                Tob2012b
03015+6029   ALV   1     RAFGL 4029 IRS 1. Massive YSO, member of cluster of IR sources.         Alv2004 
03015+3225   STF 336     SEI  26.                                                                Nsn2017a
03019-1633   RST2292     AB: LDS3448.                                                                    
                         A : M = 0.257+/-0.014 \msun, R = 0.268+/-0.027 \rsun.                   WJG2019b
                         B : M = 0.215+/-0.014 \msun, R = 0.236+/-0.027 \rsun.                   WJG2019b
                         C : M = 0.161+/-0.014 \msun, R = 0.197 /-0.027 \rsun.                   WJG2019b
03021+0005   GAU   2     BAL 652.                                                                        
03023+4124   STF 337     B is below MS in both (V,V-K) and (J,J-K) CMDs: wrong plx(B)=39.9mas!           
                         Wrong PM(B) in HIP?                                                     Tok2014d
03023+1820   A  2414     A premature orbit has been computed.                                            
03023+0405   alp Cet     Menkar                                                                          
                         1975.634: Disk possible marginally resolved (0".014 +/- 0".005) at 400          
                         and 425 nm.                                                                     
                         1975.639: Disk possible marginally resolved at 460 nm.                  Bla1977a
03023-7154   FIN 360     the Hyi. Not seen for certain 1962-1969, and not observed since.                
                         Needs speckle.                                                                  
03024+4204   BRT1135     LDS2824.                                                                        
03025-1516   HJL1114     IR Eri. A combined interferometric/spectroscopic solution by                    
                         Halbwachs et al. (2016) yields masses 0.982 +/- 0.010 and 0.8819 +/-            
                         0.0089 Msun.                                                            HJL2016 
03027-0741   BU   11     rho 2 Eri = 9 Eri. Note: this is not p Eridani (= 01398-5612DUN   5).           
03030-0205   STF 341     Primary is possible SB? On Keck RV program, but only small RV var.      Tok2014d
                         A 1136d spectroscopic solution for the B component has been found       Tok2019g
                         making this a triple system.                                                    
03031-0049   GWP 413     ABL  97.                                                                Tob2012b
03032-0215   J  1455     BAL 21.                                                                         
03033-1848   GWP 414     ABL  98.                                                                Tob2012b
03034-0804   LDS5409     A possible wide companion to 2MASS J03032132-0805153 at 172" with               
                         similar proper motion is noted in WDS.                                  Jnn2012 
03035+2304   HDS 389     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.50 +/- 0.27, 1.91, and 1.79 Msun, respectively.  Mlk2012 
                         Primary is SB, P(AB)=2152d=5.89y.  Metchev & Hillenbrand (2009)         Met2009 
                         resolve AB and list two faint optical(?) companions at 4", dK~5.        Tok2014d
                         Teff for A & B : 6140 +/- 100 and 5300 +/- 100 K                        Mda2018 
                         R    for A & B : 1.234+/-0.05 and 0.820+/-0.05 \rsun                            
                         L    for A & B : 1.94 +/-0.08 and 0.48 +/-0.10 \lsun                            
                         M    for A & B : 1.18 +/-0.22 and 0.84 +/-0.12 \msun                            
                         Age =  3.5 +/- 1.5 Gyr.                                                         
03036+3627   BUP  37     The COU 869Aa companion was suspected by Burnham.                       Bu_1913 
03036-1001   GWP 415     ABL  99.                                                                Tob2012b
03036-2536   BRG  17     One or both of the stars in this system must be highly variable. The            
                         magnitude differences between the primary and secondary vary from 5.14          
                         mag to 1.72 mag between different observations in Bergfors et al.       Brg2010 
                         (2010) and here. In contrast to the individual note on this system in           
                         Bergfors et al., we assume here that the designation LTT 1453 refers            
                         to the primary star.                                                    Jnn2012 
                         First noted as a likely binary by Makarov & Kaplan (2005), based on     Mkr2005 
                         significant differences between Hipparcos and Tycho proper motions,             
                         then later resolved as part of the Astralux Lucky imaging survey by             
                         Bergfors et al. (2010) and Janson et al. (2012). Their 2008 and 2010    Brg2010 
                         measures, together with measures from 2011 reveal a constant            Jnn2012 
                         separation but a P.A. changing by ~3 deg/yr.                            Bwl2015 
03038+0608   KPP3161     A : Teff =  6113 +/-   40 K, M = 1.06 +/- 0.06 \msun.                   XXX2020a
                         B : Teff = 18200 +/- 3000 K, M = 1.12 +/- 0.15 \msun.                           
03039+1514   BPM  69     [PM2000]  112964 + [PM2000]  112917.                                    Gvr2010 
03041+3509   POP  11     Popovic coordinate offset was apparently in error.                      Pop1969c
03042+6142   LDS9142     Old LDS6142.                                                                    
03044+2118   JNN  23     The close (~0.40") companion to 2MASS J03042184+2118154 is counted as           
                         an unconfirmed binary companion, since it has not yet been tested for           
                         common proper motion.                                                   Jnn2012 
03045+3844   SMA  33     ALI 766.                                                                        
03046-5119   DUN  10     B is CD-51@706.                                                                 
                         SHY 433. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         HIP 14307 and 14313 form a 38" pair belonging to the FG-67 sample.              
             TOK 428     AC: AC is not co-moving. C=HIP14257 has different parallax              Tok2014d
             TOK 428     Ba,Bb: The component B is resolved here at 0".19. The estimated                 
                         period of Ba,Bb is ~25yr. No motion is seen in 2 months. The subsystem          
                         Ba,Bb is also manifested by asymmetric line profiles (Tokovinin, in             
                         preparation). The A component has never been observed at high angular           
                         resolution.                                                             Tok2015c
03047+6346   STF 335     B is BD+63@388.                                                                 
03048+5330   WRH  29     Aa,Ab: gam Per = 23 Per. SB2. Spectrum composite: G8III+A2V.            WRH1955 
                         zeta Aurigae-type binary.                                                       
                         1975.781: Uncertain angle readout                                       Bla1977a
                         Analyses of the spectroscopic/interferometric orbit are given by        McA1982a
                         McAlister (1982) and Popper & McAlister (1987). Elements P, T, e for    Ppp1987 
                         the McAlister (1982) orbit are from the spectroscopic orbit by                  
                         McLaughlin (1948).                                                      MLa1948 
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         McAlister (1982).                                                       McA1982a
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         1998.657: Absolute quadrant determined by triple-correlation technique  Pru2002b
                         The physical nature of visual companion B (57", mag. 11) is uncertain.          
                         Aa,Ab: Malkov et al. (2012) derive dynamical and spectroscopic masses           
                         5.80 +/- 88.31 and 4.72 Msun, respectively.                             Mlk2012 
                         NPOI Limb-darkened diameter  3.894 +/- 0.018 mas, Sp = G8III,           NOI2018 
                         R =31.21 +/- 1.195 \rsun, Teff = 4589 +/- 58 K, L =389.6 +/-35.5 \lsun,         
                         M = 3.64 +/- 0.25 \msun, Age = 0.23 +/- 0.05 Gyr.                               
03048-0603   GWP 416     ABL 101.                                                                Tob2012b
03049+3446   HU  812     Hussey position angle 1902: 199.4@. Probably wrong quadrant.            Hu_1905a
                         HIP 14342. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
03052-0156   GWP 417     ABL 102.                                                                Tob2012b
03052-3725   BRG  18     This target, like BRG  23, gives conflicting information about whether          
                         the AB pair is physically bound. The brightness and color are fully             
                         consistent with B being an M3.5 companion to the M2.0 primary.                  
                         Furthermore, the separation is only 0.2", and the whole field is                
                         otherwise empty. This indicates physical companionship. However, the            
                         deviation from the expectation of a background source is only 1.1               
                         sigma, and the companion has moved 3.6 times closer to the background           
                         expectation than its original position where the motion has a 14 sigma          
                         confidence. This, by contrast, suggests a chance alignment. Since the           
                         magnitude of motion is not inconsistent with what could be expected             
                         for orbital motion of a real physical pair, we keep it as binary in             
                         our analysis, but we note that further observations will be necessary           
                         in order to resolve this issue satisfactorily.                          Jnn2012 
03054+2515   STF 346     52 Ari. AB: Malkov et al. (2012) derive dynamical, photometric, and             
                         spectroscopic masses 9.10 +/- 6.84, 6.89, and 3.39 Msun, respectively.  Mlk2012 
03054-1432   GWP 418     ABL 103.                                                                Tob2012b
03055+0234   BAL1630     OL  183.                                                                        
03056+1150   GIC  36     G005-013/G005-012.                                                              
03056-0238   GWP 419     ABL 104.                                                                Tob2012b
03058+3202   ES  326     BC: SEI  27.                                                            Nsn2017a
03059+1302   BPMA  4     [PM2000]  114294 + [PM2000]  114392.                                    Gvr2010 
03061+7925   STF 320     Spectroscopic binary? Spectrum composite; M1III+F7IV.                           
03063-1243   LDS3452     NLTT 9888/9881                                                          Chm2004 
03064+1545   ALP   9     2MASSW J0306268+154514                                                          
                         Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in February 2003.          AlP2007 
03069+4022   A  1532     Also known as V568 Per.                                                         
                         A is a 1325d spectroscopic double which cannot be this pair.            Tok2019b
03071+3757   BRT2203     ALI 513.                                                                        
03072-0520   GWP 423     ABL 105.                                                                Tob2012b
03073-1346   CRJ   7     Crepp et al. (2015) determine effective temperatures for the A and B            
                         components of 5680 +/- 40 and 978 +20/-43K. Spectral types are G3V and          
                         T5.5 +/- 1, masses 0.95 +/- 0.02 and >51.9 +3.6/-4.3 Mjup,                      
                         ages 4.6-10 Gyr.                                                        CrJ2015 
03074+5831   RAFGL 437   Shows subarcsecond monopolar nebula extending towards SE at PA                  
                         135 +/- 10deg.                                                          Alv2004 
03075-7859   HJ 3568     A is a spectroscopic binary.                                                    
03076-4702   TOK 206     The companion with q = 0.29 is resolved with NICI but unresolved with           
                         speckle,  being too faint in the optical.                               Tok2012a
03077+3637   ENG  11     B is BD+36@631.                                                                 
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
03078+2533   TOK 234     The B component was suspected of duplicity (0".253, 240.5deg,                   
                         dI=2.7mag) by RoboAO, but the pair was not accepted as real             Tok2014d
03078+1223   BPM  70     [PM2000]  115596 + [PM2000]  115589.                                    Gvr2010 
03078-2750   VIG   3     Optical/physical nature of the faint companion is undefined.            Vig2012 
03079-2813   LDS  86     AB: NLTT 9987/9985                                                      Chm2004 
03080-0135   GWP 425     ABL 107.                                                                Tob2012b
03080-0537   GWP 424     ABL 106.                                                                Tob2012b
03082+4057   LAB   2     Aa,Ab: bet Per = 26 Per = Algol , prototype of the Algol-type binaries.         
                         The eclipse phenomena, known since historical times (although the time          
                         of minimum brightness was first measured by Montanari on 8 Nov 1670)            
                         was first explained as an eclipsing binary by Goodericke as early as            
                         1782. According to R.G. Aitken, this was verified when it was noted as  A__1935f
                         the second spectroscopic binary based on photographic spectra                   
                         obtained by Prof. H.C. Vogel at Potsdam in November, 1889. Belopolsky           
                         discovered a variation in the radial velocity with a period of order            
                         1.8 years, later resolved by Labeyrie and his speckle camera in 1973;   Lab1974 
                         the magnitude difference is about 2.5.                                          
                         The binary, a radio and X-ray source, is triple (and possibly                   
                         quadruple, but the variation with the 32 yr period is more probably an          
                         apsidal rotation of the eclipsing pair).                                        
                         The spectroscopic data were discussed by Hill et al. (1970, 1971).      HlG1970 
                         ADS lists several distant, faint, and probably optical companions.      HlG1971 
                         Elements P, T, e, and omega for Labeyrie et al. (1974) orbit adopted    Lab1974 
                         from the spectroscopic orbit of Hill et al. (1971).                             
                         Analysis of the spectroscopic/interferometric orbit is given by                 
                         Bonneau (1979)                                                          Bnu1979 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Hipparcos astrometric solution adopts some elements from the orbits of  HIP1997d
                         Pan et al. (1993) and                                                   MkT1993a
                         Gatewood et al. (1995).                                                 Gat1995 
                         Peterson et al. (2011) orbits of both the outer (LAB   2Aa,Ab) and      Ptn2011 
                         inner (CSI   1Aa1,Aa2) are based on VLBI measures combined with                 
                         speckle and radial velocity data. Assuming masses of the primary and            
                         secondary of 3.70 and 0.79 Msun, respectively, they derive a mass for           
                         the tertiary of 1.51 +/- 0.02 Msun.                                             
             BU  526     AB: Additional notes may be found in Burnham (1894).                    Bu_1894 
03084+4020   BRT2204     ALI 1031.                                                                       
03084+2620   OSO  14     G037-026. Not a common proper motion pair, based on color               Oso2004 
03084-2410   LDS  87     NLTT 10008/10007                                                        Chm2004 
03084-7033   HLN  19     DAM 782.                                                                        
03087+1736   COU2680     BD+17@499a.                                                                     
03087-1432   GWP 426     ABL 108.                                                                Tob2012b
                         Not a double star, but an edge-on galaxy: USNO-B1.0 proper motion is    Skf2012 
                         spurious.                                                                       
03088-0952   GWP 427     ABL 109.                                                                Tob2012b
03090+4415   STF 351     B is BD+43@637.                                                                 
03090+1740   COU 358     BD+17 501a. Mistaken identification with BD+17 501 led to earlier               
                         incorrect WDS designation as 03088+1801.                                        
03091+4937   BUP  38     iot Per. Proper motion of A +1263 -091.                                         
03092+0728   STFA  6     STTA 32. B is BD+06@487.                                                        
03094-3004   LDS3460     NLTT 10074/10076                                                        Chm2004 
03095+4544   HDS 404     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 0.90 +/- 0.09, 0.87, and 0.75 Msun, respectively.             Mlk2012 
03095+4451   ES 2596     kap Per = 27 Per = Misam. A is a spectroscopic binary.                          
03096+0512   A  2030     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.41 +/- 0.32, 2.11, and 1.05 Msun, respectively.             Mlk2012 
03096-0054   CHE  75     Aka BAL 281.                                                                    
03098-1238   GWP 428     ABL 110.                                                                Tob2012b
03099-0654   UX Eri      Multiple system including contact binary. Pribulla & Rucinski (2006)    Pbl2006 
                         estimate the mass of the contact pair at 1.901 Msun and the minimum             
                         mass of the wider component at 0.59 Msun.                                       
03099-8332   HJ 3582     Spectral type of A : F2IIISrEuSi:  Estimated orbital period ~100,000y.  Soz2017 
03101+0210   RST5197     Aka TDS2463.                                                                    
03101-6355   HJ 3559     B is CPD-64@231.                                                                
03104+0238   OL  177     Not found by Heintz at IDS position. Position corrected.                Hei1990b
03104-0004   GWP 429     ABL 111.                                                                Tob2012b
03105+5040   LDS9143     Old LDS6143.                                                                    
03107+2226   LDS3461     NLTT 10112/10110                                                        Chm2004 
03107-4023   LDS9144     Old LDS6144.  Recognized to be the same as LDS5414 by John Greaves.     Grv2006c
03108+3724   LDS9145     Old LDS6145.                                                                    
                         NLTT 10082/10091                                                        Chm2004 
03110+1648   SPF   1     L dwarf 2MASS J03105986+1648155 resolved into close components at L/T           
                         boundary. Approximate orbital period 72 +/- 4 years, distance 25 +/- 4          
                         pc, system mass ~30-60 Mjup. Spectral types of both components are              
                         estimated at L9 +/- 1.                                                  Spf2010 
03112+2225   H 5 117     Also known as STF 359.                                                          
                         AC: Rectilinear solution by Friedman et al. (2011).                     USN2011a
03113+3937   BLL  10     ome Per = 28 Per                                                                
03117+8128   STF 327     A is a spectroscopic binary.                                                    
03118+3525   GIC  37     G095-014/G095-013.                                                              
03119+6131   HDS 407     A is also a 59d spectroscopic binary.                                   Tok2019b
03121-2859   HJ 3555     alp For = 12 Eri = Dalim. The magnitude of B is uncertain and has been          
                         suspected to vary. Another century is needed for apastron coverage.             
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         A is GJ 127. B is possible SB. Variability of RV(B) is based on                 
                         historic RV (Eggen, van den Bos)                                        Tok2014d
03121-6420   HJ 3562     B is CPD -64@231.                                                               
03122+3713   STF 360     A premature orbit has been calculated. Data appear equally well fit by          
                         rectilinear solution - see rectilinear elements catalog.                        
                         A is SB1, P=415d. B is possible long-period SB.                         Tok2014d
03123-2727   LDS  88     NLTT 10222/10227                                                        Chm2004 
03124-4425   JC    5     Ma,Mb = 1.365 +/- 0.031, 1.134 +/- 0.024 \msun.                         GmJ2022 
03124-1157   GWP 432     AB: ABL 112AB.                                                          Tob2012b
             GWP 433     AC: ABL 112AC.                                                          Tob2012b
03124-4425   JC    8     Variable RV of AB, not explained by the visual motion, has been                 
                         reported (Eggen 1965), but Heintz's mass ratio does not support         Egg1965b
                         the presence of a fourth body.                                          Hei1979a
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.59 +/- 0.73, 2.18, and 3.82 Msun, respectively.  Mlk2012 
             HJ 3556     AB,C: Star C (mag. 9.2, 3.5") is in slow retrograde motion.                     
                         Heintz (1979) gives AB orbit, attempts AC orbit with P=987yr.           Hei1979a
                         The motion of AC is not directed away from PM(A), hence physical.       Tok2014d
03125-3449   LDS  89     LDS5418.                                                                        
03127+7133   STT  50     A premature orbit has been calculated.                                          
                         Bespalov (1961) has a = 1".618, Finsen & Worley (1970) assume this      Bsp1961 
                         is a misprint.                                                          Fin1970b
03128+3720   WZ    6     ES 2556.                                                                        
03128-0112   HJ  663     94 Cet.                                                                         
                         AB: B is PMS star and SB1 (P=2.026y). Planet (P= 1.2y=535.7d) around            
                         A. Is this true planet or Ba,Bb effect?                                 Tok2014d
                         CHARA Array Limb-darkened diameter  0.788 +/- 0.026 mas,                CIA2008c
                         R =  1.930 +/- 0.067 \rsun.                                                     
             TOK 654     AF: CPM companion HD 20619 = GJ 135: 7.03V, G1.5, HD 20169 at 133'              
                         from AB (0.7 pc)                                                        Tok2014d
03130+3254   LDS9146     AB: Old LDS6146.                                                                
                         B is deeply below MS, blue in V-K and J-K. White dwarf?  WDS: too fast          
                         motion of AB, optical? Hyades cluster. CfA: RV var?                     Tok2014d
                         Hyades cluster. The 2MASS companion B can be physical.                  Tok2014d
                         Previous AD companion, TOK 655, is the same as the known AB pair. The   Dam2015d
                         Luyten measure was poor.                                                        
03130-0343   GWP 434     ABL 113.                                                                Tob2012b
03132+1710   BPM  71     [PM2000]  119048 + [PM2000]  119061.                                    Gvr2010 
03134-0852   GWP 438     ABL 114.                                                                Tob2012b
03135+4417   ES  559     Also known as LDS9147, LDS6147, and LDS2836. These were all recognized          
                         by John Greaves (personal corres.) to be the same pair.                         
                         NLTT 10231/10232                                                        Chm2004 
03136+3909   STF 364     HJL  46.                                                                HJL1986 
03141+5934   TRN  15     CC Cas. Classification in Mason et al. (1998) is from the tomographic   Msn1998a
                         analysis of Hill et al. (1994 A&A 282, 455).                                    
                         The image rotator was in an unknown state, so two possible theta                
                         values are listed for the 2001.7452 observation - one for zenith up             
                         and one for north up.                                                   Trn2008 
03141+0832   GIC  38     G079-015/G079-016.                                                              
03144-0227   GWP 440     ABL 115.                                                                Tob2012b
03146-0940   GWP 441     ABL 116.                                                                Tob2012b
03147-3533   GAA   4     TZ For, a detached eclipsing binary.  A combined spectroscopic/                 
                         interferometric orbit by Gallenne et al. (2016) yields a semimajor              
                         axis of 0.5564 +/- 0.0001 au, distance 185.9 +/- 1.9 pc, and the                
                         following component parameters:                                                 
                         mass (Msun):        2.057 +/- 0.001     1.958 +/- 0.001                         
                         radius (Rsun):      8.28  +/- 0.22      3.94  +/- 0.17                          
                         luminosity (Lsun):  1.57  +/- 0.02      1.36  +/- 0.03                  GaA2016 
03149-1400   HJ 3558     HJ 3551 is identical.                                                           
03150+0101   GIC  39     G077-035/G077-034. See Allen et al. (2000) for  information on          AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
03151+1618   HU 1055     The companions C, D, and E, given in the ADS, do not exist. They                
                         should be under ADS 2426.                                               B__1963b
03154-6930   R    22     Also appears to be R    27.                                                     
03158+5057   HU  544     A = V572 Per: eclipsing binary of Algol-type, period 1.21317 days.      Zas2015
03158-0849   SHY 154     HIP  15197 + HIP  15244. Primary is zet Eri = Zibal.                            
03160+4853   LDS9148     Old LDS6148.                                                                    
                         NLTT 10355/10353                                                        Chm2004 
03160+3441   HO  503     A spectroscopic binary and ellipsoidal variable, V423 Per.                      
03162+1302   BPMA  5     [PM2000]  120872 + [PM2000]  120882.                                    Gvr2010 
03165-0642   GWP 443     ABL 117.                                                                Tob2012b
03165-3541   SHY 439     AB: HIP  15239 + HIP  15432.                                                    
             SHY 439     AC: HIP  15239 + HIP  15152.                                                    
             SHY 439     AD: HIP  15239 + HIP  15933.                                                    
             SHY 441     BC: HIP  15432 + HIP  15152.                                                    
03166+4943   ES  463     Aka OL  150.                                                                    
03166+3238   STF 370     According to Burling, the long unconfirmed system, 03064+3153HJ 5456,           
                         may also be this pair.                                                  Bur2005 
                         SEI  29.                                                                Nsn2017a
03167+4237   LDS9149     Old LDS6149.                                                                    
03167+2639   TOR   4     Formerly known as PAN   1.                                                      
03167-0332   TOK  78     HIP 15247. A is SB without orbit, dRV= 6.6.                             Nrd2004 
03168+7830   STF 345     Also known as STF 340.                                                          
03168+0501   A  2032     HIP 15253. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
03172+4522   PRV   2     GJ 3213. Pravdo et al. (2006) derive masses 0.370 +/- 0.034 and                 
                         0.195 +/- 0.021 Msun.                                                   Prv2006 
03174+0739   BU 1039     Hyades vB 1. BU 1039AB, with rho = 2".2 and Delta m = 6.0 is outside            
                         the detection window.                                                   Msn1993a
                         AC: HJL  47.                                                            HJL1986 
                         AC: SHY 155. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
03175+6540   STT  52     A premature orbit has been calculated.                                          
03175-0107   GWP 445     ABL 118.                                                                Tob2012b
03175-1222   J  1456     BRT2628.                                                                Brt1947 
03176-1412   GWP 446     ABL 119.                                                                Tob2012b
03177+6108   STI 441     03175+6108SMA  36                                                               
03177+3838   STT  53     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.51 +/- 0.99, 2.40, and 1.05 Msun, respectively.             Mlk2012 
03178-7029   R    28     Aka RSS  62.                                                                    
03180-6656   EHR   3     Physical/optical nature undefined.                                      Ehr2010 
03182-6230   BNU   2     Aa,Ab: zet 2 Ret. B has common proper motion, +1370 +660, and is                
                         CPD-63@217 = zet 1 Ret.                                                         
                         Aa,Ab: Likely a spurious pair. Last measured 1978 and unresolved by             
                         SOAR on 3 occasions 2008-2012.                                          Tok2010 
                                                                                                 Tok2012d
                                                                                                 Tok2014a
                         Aa,Ab is suspicious, 1 observation in WDS, not binary in Raghavan et    Rag2010 
                         al. (2010). Jones et al. (2002) do not detect SB with precise RV at     CPS2002b
                         the AAT.                                                                Tok2014d
             ALB   1     AB = LDS  92.  HIP 15371. See Allen et al. (2000) for information       AlC2000 
                         on metallicity, age, galactic orbital parameters, etc.                          
                         AB: SHY  16. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
03184-0056   AC    2     95 Cet. According to Eggen this pair shares common proper motion with   Egg1960 
                         BD -01 474 at 11'.                                                              
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
03184-0708   LDS3473     HIP 15396. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 10536/10548                                                        Chm2004 
03184-2231   SEE  23     15 Eri. CD-22@1146. Motion direct.                                              
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.33 +/- 0.80, 3.35, and 1.20 Msun, respectively.             Mlk2012 
03185+4721   MET   1     V522 Per.                                                               Met2004a
03185+1511   LDS9150     Old LDS6150. HIP 15394. See Allen et al. (2000) for information on      AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
03186+0827   LUH   6     AC: LSPM J0318+0827S + 2MASS J03184214+0828002.                         Luh2012b
03187+1527   LDS9151     Old LDS6151. SLE  41.                                                           
03187-1834   HJ 3565     A is a spectroscopic binary.                                                    
03188-0028   ABT   3     BAL 656.                                                                        
03188-0321   GWP 447     ABL 120.                                                                Tob2012b
03189-0101   BU 1177     Gomez et al. (2016) derive dynamical parallax and component masses:             
                         10.03 +/- 0.77 mas, 0.906 +/- 0.033 Msun, 0.886 +/- 0.032 Msun.         Doc2016i
03190-1549   GWP 448     ABL 121.                                                                Tob2012b
03192-5306   HJ 3571     CD-53@674.                                                                      
03193-0232   GWP 449     ABL 122.                                                                Tob2012b
03194+6156   JNN 254     G 246-33. Estimated age 35-300 Myr; masses 0.29 +/- 0.11 and 0.17 +/-           
                         0.07 Msun; a ~10.8 au.                                                  Jnn2014 
03194+0322   STT 557     AB: kap 1 Cet = 96 Cet. Variable? A is a spectroscopic binary.                  
                         B is BD+02@521.                                                                 
03195-2145   JC    1     tau 4 Eri = 16 Eri. A is an irregular variable.                                 
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
03199-0321   GWP 450     ABL 123.                                                                Tob2012b
03200+6539   BUP  43     Shell star. Light and spectrum variable, BK Cam. May also be a long-            
                         period spectroscopic binary.                                                    
03200+3845   BRT2205     MLB 819. ALI 774.                                                               
03201-2851   LDS  93     van den Bergh reports a third star at 38@, 105.6".                      Bgh1958 
                         A is exoplanet host, P=592d. B = HIP 15526 hosts exoplanets with                
                         P=29.1d, 85.1d.                                                         Tok2014d
                         B is CD-29@1229.                                                                
                         NLTT 10636/10635                                                        Chm2004 
                         SHY 157. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
03202-1457   LDS3479     NLTT 10629/10617                                                        Chm2004 
03202-1632   GWP 452     ABL 124.                                                                Tob2012b
03203+1944   STF 376     H 2  76.                                                                MEv2010 
03203+1625   SLE  42     Hipparcos suspected non-single.                                                 
03206+0902   GIC  40     G079-029/G079-030 = GJ 9114AB.                                                  
                         HIP 15572. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         Primary is SB1, P=321.6d                                                Tok2014d
03207+8459   STF 319     Schiller measures 1910.87,331.1@,42.32",7.7-9.2.                        Shr1913 
03207+1736   HJ 3245     See BDS for components.                                                         
03210-0054   LDS5420     LDS5420A was B component of 03211-0054ITF  55AB, LDS5420B was ITF 55C           
                         Pairs merged; ITF 55AB --> 03210-0054ITF 55AD (with quadrant flip),             
                         ITF 55AC --> 03210-0054ITF 55BD (also with quadrant flip).                      
03211-2632   SWR   5     CPM pair                                                                Skf2004 
03212+2109   COU 259     tau 1 Ari = 61 Ari. A is an irregular variable.                                 
03213+4302   A  1706     LDS2842.                                                                        
03214+4320   VIG   4     Optical/physical nature of the faint companion is undefined.            Vig2012 
03216-0841   GWP 454     ABL 126.                                                                Tob2012b
03217+0845   STF 380     A premature orbit has been calculated.                                          
03219+4904   WEB   1     B is BD+48@892.                                                                 
03220+1715   LDS3483     G006-003. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 10701/10698                                                        Chm2004 
03220-1636   LDS3485     NLTT 10725/10724                                                        Chm2004 
03226-0210   GWP 456     ABL 127.                                                                Tob2012b
03226-3011   LDS3487     LDS5422.                                                                        
                         NLTT 10762/10761                                                        Chm2004 
03227+1717   BPM  72     [PM2000]  124803 + [PM2000]  124860.                                    Gvr2010 
03227+1037   GIC  41     BC: 03328+1040 UC  997.                                                         
03228-0042   GWP 457     ABL 128.                                                                Tob2012b
03229+2949   STF 379     H III 91, BDS 1688.                                                             
                         H 3  91.                                                                MEv2010 
03230-0548   GWP 458     ABL 129.                                                                Tob2012b
03232+4554   LDS9152     Old LDS6152.  HD 20835. See Allen et al. (2000) for information on      AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
03232-1404   GWP 459     ABL 130.                                                                Tob2012b
03233-0337   GWP 460     ABL 131.                                                                Tob2012b
03233-0748   BU  531     CHARA Array Limb-darkened diameter of A :                               CIA2013c
                         R =  2.4214 +/- 0.0764 \rsun, L =   4.0279 +/-0.1529 \lsun,                     
                         Teff = 5261 +/-  65 K, M = 1.056 \msun, Age = 7.2 Gyr.                          
03233-5000   HJ 3573     LDS  94. A is CD-50@1015, B is CD-50@1014 (Roman).                              
03234-0710   GWP 461     ABL 132.                                                                Tob2012b
03234-1015   HJ 2188     STF 387.                                                                        
03236+0453   BU 1178     A is a spectroscopic binary.                                                    
                         Greenwich measure of 1921 erroneous. No certain change since 1890.      B__1963b
03236-4005   I   468     glimpsed?                                                               I__1948a
                         Soderhjelm (1999) gives possible orbit from two widely spaced visual    Sod1999 
                         observations + Hipparcos data.                                                  
03236-8116   SHY 161     AC: HIP  15803 + HIP  17184.                                                    
03237-0609   GWP 462     ABL 133.                                                                Tob2012b
03238+2432   LDS1144     NLTT 10780/10781                                                        Chm2004 
03240-0007   GRV 997     = GWP 464 = ABL 135.                                                    Tob2012b
03240-2613   HJ 3572     B is CD-26@1270.                                                                
                         SWR   6. CPM pair                                                       Skf2004 
03242+2347   LDS 884     AB,C: NLTT 10804/10808                                                  Chm2004 
03242-1048   GWP 463     ABL 134.                                                                Tob2012b
03243+4952   BUP  44     alp Per = 33 Per = Mirfak                                                       
03244-1539   A  2909     There are many negative observations. Needs speckle.                            
                         HIP 15868. A is the close pair A 2909, 0.1". The 2MASS PSC companion            
                         at 17" is called C in the WDS.                                          Tok2011a
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 0.62 +/- 0.11, 2.10, and 1.01 Msun, respectively.  Mlk2012 
                         CfA: SB? P=9115d? =25y?  UR at SOAR from 2008.6 to 2012.9, in           Mlr1955a
                         contradiction with orbit of Muller (1955).                              Tok2014d
                         A spurious orbit of this ghost pair has been computed which is          Doc2016d
                         contradicted by the many non-resolutions.                               Tok2019d
03245+4626   LDS9153     Old LDS6153.                                                                    
03248-1533   GWP 466     ABL 136.                                                                Tob2012b
03249+1552   BPM  73     [PM2000]  126226 + [PM2000]  126261.                                    Gvr2010 
03249-0356   GWP 467     ABL 137.                                                                Tob2012b
03253+1158   BPM  74     [PM2000]  126464 + [PM2000]  126473.                                    Gvr2010 
03256-1855   GWP 468     ABL 138.                                                                Tob2012b
03257+0551   JNN 255     AB: GJ 3224. Estimated age 300-1000 Myr; masses 0.25 +/- 0.06 and 0.14          
                         +/- 0.01 Msun; a ~6.3 au.                                               Jnn2014 
                         AC: Estimated age 300-1000 Myr; masses 0.48 +/- 0.25 and 0.45 +/- 0.24          
                         Msun; a ~48.1 au.                                                       Jnn2014 
03259+4540   COU1682     TDS2544.                                                                        
03261+1229   A   829     Probably ambiguous case, but only one solution has been tested.                 
03262+2950   ALP  10     2MASSW J0326137+295015                                                          
                         Further observations are required to determine the physical/optical             
                         nature of this pair.                                                    AlP2007 
                         Astrometric orbit by Harris et al. (2015) yielded the following                 
                         properties: spectral types L3.5+L7, absolute J mags 12.99+14.5,                 
                         masses 0.061 +/- 0.010 and 0.044 +/- 0.008 Msun.                        USN2015 
03262-1817   GWP 469     ABL 139.                                                                Tob2012b
03263+1709   JNN 256     Estimated age 1000-10000 Myr; masses 0.24 +/- 0.03 and 0.16 +/- 0.03            
                         Msun; a ~20.6 au.                                                       Jnn2014 
03264+3520   HDS 430     Cvetkovic et al. (2016) estimate spectral types F7 and G8, masses 1.30          
                         and 0.97 Msun. Dynamical parallax is 15.60 +/- 0.44 mas.                Cve2016b
03265+5909   GIC  42     G246-036/G246-035.                                                              
03266+2843   CHR   9     Aa,Ab: This is UX Ari, an RS CVn type binary that is not eclipsing.             
                         Peterson et al. (2011) orbits of both the outer (CHR   9Aa,Ab) and      Ptn2011 
                         inner (CIA  10Aa1,Aa2) are based on VLBI measures combined with                 
                         speckle and radial velocity data. Assuming masses of the primary and            
                         secondary of 1.10 and 0.95 Msun, respectively, they derive a mass for           
                         the tertiary of 0.75 +/- 0.01 Msun.                                             
             CIA  10     Aa1,Aa2: Orbit of Hummel et al. (2017) corrected for apparent 0.5d      Hmm2017b
                         error in T0 (2456238.134d changed to 2456237.634d). Also, they were             
                         unaware of the wide CPM companion, so erroneously refer to the close            
                         pair as Aa,Ab and the CHR pair as AB.                                           
                         Aa1,Aa2: Mass of Aa1 & Aa2 = 1.30(0.06) & 1.14(0.06) \msun.             Hmm2017b
                         Teff = 4560(100) & 5670(100) for Aa1 & Aa2. Diameters = 0.97(0.02) &            
                         0.35(0.02) mas. Orbital parallax = 19.20(0.28) mas.                             
             TOK  13     AB: AB is CPM, estimated period 20,000y. Primary is 6.4d SB2.                   
                         The spectrum shows 3 components (Fekel, 1986 private communication),            
                         two of which are identified with the 6.44-day system described by               
                         Carlos & Popper (1971), while the third is possibly the component       Ppp1971 
                         listed here.                                                                    
                         Evolved or bad 2MASS photometry.                                        Tok2006 
03266+1406   BPM  75     [PM2000]  127254 + [PM2000]  127284.                                    Gvr2010 
03269+1609   BPM  76     [PM2000]  127466 + [PM2000]  127423.                                    Gvr2010 
03269-2344   RSS   4     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
03271+1845   CHR  10     Resolution of an occultation binary.                                            
03272+0944   HDS 433     1975.629: Marginally resolved at 450 nm?                                Bla1977a
                         Hierarchical quadruple, including 51y, 145d, and 7.14d pairs                    
                         (HDS 433AB; MKT 15Aa,Ab; and MKT 15Aa1,Aa2; respectively). The 7d pair          
                         is eclipsing.  Nemravova et al. (2016) combine spectroscopy,            Nem2016 
                         photometry, and interferometry to derive orbits of all three pairs,             
                         yielding the following component parameters:                                    
                         Parameter       Aa1              Aa2               Ab                           
                         Mass (Msun)     2.252 +- 0.027   2.125 +- 0.027    3.89 +- 0.25                 
                         Radius (Rsun)   1.700    0.035   1.618    0.039    2.81    0.28                 
                         Teff (K)        10700    160     10480    130     14190    150                  
                         Mbol (mag)      0.923    0.079   1.120    0.075   -1.14    0.22                 
                         (Note: Nemravova et al. refer to the pairs as AC; AB; and Aa,Ab.                
                         However, the HDS pair was assigned components A and B at discovery.)    HIP1997a
03276+5847   RAFGL 490   Extended emission seen in H-band, no subarcsecond structure resolved.   Alv2004 
03276+0954   J   305     May be the same as GJ 3226, which is not in the WDS. At the SIMBAD      Dam2017c
                         precise position of GJ 3226 a measure from Gaia-DR1 is 117.1 deg @              
                         1.530", quite close to the measures of J   305.                                 
03278+5627   STI1984     The relative motion is small but fairly certain; it is smaller than             
                         the proper motions of both components. Therefore, although the                  
                         component proper motions are of the same order, we consider this to be          
                         a physical pair.                                                        Kiy2012 
03278-2352   LDS3496     NLTT 11000/10999                                                        Chm2004 
03279+5625   MLB 116     Triple star with weak hierarchy. Motions of all components relative to          
                         each other are small. If we trust the relatively large pm for A from            
                         the WDS, the system is physically bound; however there is an                    
                         appreciable discrepancy between this pm and the value given by                  
                         Kharhenko & Rezer (2001, Kinemat. Fiz. Nebesn. Tel 17, 409). Therefore          
                         we are not yet able to determine with confidence whether or not the             
                         components are physically bound.                                        Kiy2012 
03279-1948   GC 4128     Hipparcos astrometric solution assumed circular orbit (e = omega = 0);  HIP1997d
                         Cluster Melotte 25 #EGG21.                                                      
03280+2631   LDS1146     NLTT 10977/10976                                                        Chm2004 
03280+2028   STF 394     AB: H 3  77.                                                            MEv2010 
03282+5628   ES 1777     Relative and proper motions are of the same order, making it                    
                         impossible to judge whether the pair is physically bound.               Kiy2012 
03282+0409   A  2417     BC is also known as V1221 Tau.                                                  
03282-1335   GAL 330     Object #94 in Gallo's original list.                                    Gal1912b
03282-3551   I    58     chi 3 For                                                                       
                                                                                                         
03284+2248   BAG   2     Aa,Ab: 66 Ari. A is a spectroscopic and occultation binary.                     
                         Agreement is poor between this observation and the only other                   
                         measurement, by Balega (1988, private communication).                   Hrt1992b
03284-1425   GWP 470     ABL 140.                                                                Tob2012b
03286-1537   LDS3498     NLTT 11020/11021                                                        Chm2004 
                         Also known as GJ 3228A, this star has a wide binary companion at 16"    VVO1991 
                         separation (e.g., Weis 1991).                                           Jnn2012 
03289+4039   ES 2598     LDS6169.                                                                        
03289-2723   LDS9154     Old LDS6154.                                                                    
                         LHS1549-50.                                                                     
03291+5956   STF 385     CS Cam.                                                                         
03291+0118   MET   2     RX J0329.1+0118                                                                 
03292-0226   GWP 471     ABL 141.                                                                Tob2012b
                         This is the galaxy LEDA 1092357.                                        Dam2017c
03294+4931   BU 1179     34 Per.                                                                         
                         Magnitude 11.6 of Burnham is underestimate; mine are similar to the             
                         photometric values of Kuiper (1.93)                                     Baz1954a
03294-2406   GAA  18     AK For                                                                          
03294-6256   HJ 3580     kap Ret. LDS 100.                                                               
03295-1558   GWP 472     ABL 142.                                                                Tob2012b
03296+2431   SAR   1     HBC 347 = V1224 Tau.                                                            
03297+5955   HLM   2     Aka HLM  42.                                                                    
03297-0850   GAL 331     Object #95 in Gallo's original list.                                    Gal1912b
03298+8402   STF 343     STF 347.                                                                        
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
03300+5527   STF 390     Aka H N  66.                                                                    
03301+1258   BPMA  6     [PM2000]  129571 + [PM2000]  129567.                                    Gvr2010 
03301-1019   GWP 473     ABL 143.                                                                Tob2012b
03302+7402   LDS1572     G221-010/G221-011.                                                              
                         NLTT 10954/10953                                                        Chm2004 
                         Aka GIC  43.                                                                    
             FAR  31     NLTT 10954. Primary is white dwarf WD 0324+738.                         Far2006 
03304-1257   GWP 474     ABL 144.                                                                Tob2012b
03305+5418   LEP  15     NI    7.                                                                        
03305+2006   STF 399     AB: H 4  89 (aka, H IV 89)                                              MEv2010 
                         A component SB1, P=32.5y. Is AB a real physical pair, or just two               
                         members of Hyades?                                                      Tok2014d
03307-1926   HDS 441     Cvetkovic et al. (2016) estimate spectral types G2 and G5, masses 1.11          
                         and 1.05 Msun. Dynamical parallax is 24.78 +/- 1.48 mas.                Cve2016b
03309+7041   JNN 257     LHS 1553. Estimated age 1000-10000 Myr; masses 0.31 +/- 0.03 and 0.17           
                         +/- 0.02 Msun; a ~7.9 au.                                               Jnn2014 
03309+1256   5 Tau       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Harper (1924).                                                          Hrp1924 
03309-6200   TOK 190     The double-lined SB detected in GCS is resolved by speckle. Its                 
                         estimated orbital period of 4 yr explains the acceleration.             Tok2012a
03311+2744   STFA  7     STTA 34. B is BD+27@513.                                                        
                         HJL  49.                                                                HJL1986 
03311+1544   HDS 443     1997.7181  Large change in separation seen since Hipparcos epoch.       Msn1999b
03312+1947   STF 403     AB: H 1  55.                                                            MEv2010 
03313+6644   OSO  15     G246-038. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates. PM = +1193 -1066.                                     Oso2004 
03313+2734   SHY 445     BC: HIP  16410 + HIP  16742.                                                    
03313-5955   JSP  47     CD-60@724.                                                                      
03314+5842   STI1991     STI1997.                                                                        
03314+0131   HJ 2194     Rectilinear solution by Friedman et al. (2011).                         USN2011a
03316+4752   STT  56     Primary also is classified B8.5VeShell.                                         
03317+1331   BPM  77     [PM2000]  130670 + [PM2000]  130734.                                    Gvr2010 
03318+3803   ES 2458     ALI 517 is the same pair.                                               Hei1980a
03319+3536   ES 2559     BRT 3235.                                                                       
03319-2537   VIG   5     The B component appears to be a faint background star.                  Vig2012 
03320+6735   STT  54     B is BD+67@@274.                                                                
03320+1820   LDS3501     NLTT 11140/11139                                                        Chm2004 
03320-0223   BRT 363     A likely plate flaw.                                                    Grv2021b
03321+4801   BAG  40     Primary is the rotationally variable star V396 Per.                             
03321+4340   COU1688     AB: A premature orbit has been calculated with very sparse data, since          
                         most of the observations are negative.                                          
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.58 +/- 1.35, 2.16, and 0.95 Msun, respectively.  Mlk2012 
             LDS9155     AC: Old LDS6155. HIP 16467. See Allen et al. (2000) for information on  AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
                         NLTT 11124/11125                                                        Chm2004 
03322+1133   AG   68     H IV 44. Also known as STF 409.                                                 
                         H 4  44.                                                                MEv2010 
03323-0705   STF 411     B is BD-07@619 (Roman).                                                         
                         B component spectral type F9IV                                          AbH2000 
03326+2844   JNN  24     This is a close triple system discovered with AstraLux, where in                
                         particular the tertiary component is difficult to fit for. Since the            
                         relative positions of the BC pair components are therefore clearly              
                         dominated by noise scatter in both separation and position angle, we            
                         set the error of each epoch to the scatter among the data points and            
                         make no assessment of orbital motion for the BC pair (although by               
                         contrast, clear orbital motion is seen of the pair with respect to the          
                         A component).                                                           Jnn2012 
                         Estimated age 10-20 Myr; masses 0.07 +/- 0.01 and 0.04 +/- 0.01 Msun;           
                         a ~8.7 au.                                                              Jnn2014 
03327+3540   CHR 261     This object is a new addition to older Hyades member lists added by             
                         Schwan (1991 A&A, 243, 386), although Griffin (1992 private comm.)              
                         doubts that this object is actually a cluster member. While its status          
                         is not definitive, subsequent confirmation or suspected duplicity (by           
                         another technique) makes the discovery measurement somewhat more                
                         probable.                                                               Msn1993a
03327-0553   GWP 476     ABL 145.                                                                Tob2012b
03328-0247   GWP 477     ABL 146.                                                                Tob2012b
03329-0927   BLA   2     eps Eri = 18 Eri = Ran. Macintosh et al (2003) made a K-band search for MBA2003 
             MBA   1     extrasolar planets in the dust surrounding eps Eri, using Keck, NIRC2,          
                         and AO. The relative motions for these 10 objects between 2001 Dec and          
                         2002 Aug were all well below expected motions for true companions,              
                         leading to conclusion all these faint companions are background stars.          
03332+4615   ES  560     NLTT 11174/11176                                                        Chm2004 
03334+2322   STT  57     STTA 35 = S   429.                                                              
03335+5846   STF 396     B is BD+58@618. Spectrum of A: Am(A3/A7/F0).                                    
03336-0735   GWP 478     ABL 147.                                                                Tob2012b
03336-1904   RSS  66     CPD-19@376                                                                      
03337+5752   CHR 117     Cf orbit in McAlister et al. (1992).  High-space-velocity binary.       McA1992 
                         See Balega et al. (2001) for further discussion of Li abundance.        Bag2001 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.47 +/- 0.38, 3.40, and 1.13 Msun, respectively.             Mlk2012 
03339+3205   HJ  334     STT 540.                                                                        
                         SEI  30.                                                                Nsn2017a
                         Rectilinear solution by Friedman et al. (2012).                         USN2012a
03339-3105   B    52     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.62 +/- 1.43, 2.46, and 1.20 Msun, respectively.             Mlk2012 
03342+4837   BU  787     Burnham notes: "Hussey measures a third star, 175.8deg, 12.70arcsec     Hu_1903b
                         (1898.70) 1n. I could not see this on one night with the 40-inch, but           
                         measured 11m star in nearly the same direction, 175.6deg, 36.78arcsec           
                         (1899.13) 1n."                                                          Bu_1906 
                         C does not exist.                                                       B__1960b
                         AB: Rectilinear solution by Cvetkovic (2011).                           Cve2011c
                         Despite having an orbit, an optical pair based on parallax an proper    Izm2019 
                         motion.                                                                 Mlk2022 
03342+4651   HDS 452     V578 Per, eclipsing binary of bet Lyr type, period 0.97077d.            Zas2016 
03343+6348   MLB 190     Also known as WFC  16.                                                          
03343+2625   OL  152     COU 687.                                                                        
03344+2428   STF 412     7 Tau. Only P, T, and a were redetermined by Vlaicu & Vasile (1961);    Vla1965 
                         the remaining elements were from the orbit of Luyten (1934).            Luy1934c
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.04 +/- 1.54, 4.91, and 2.09 Msun, respectively.  Mlk2012 
                         AB,C: H 4  88.                                                          MEv2010 
03344-1940   GWP 480     ABL 148.                                                                Tob2012b
03345+1948   STF 414     H III 78. STT  58.                                                              
                         H 3  78.                                                                MEv2010 
                         One or both components may be variable.                                 SHS2023f
03346-1613   GAL 332     Object #96 in Gallo's original list.                                    Gal1912b
03346-3104   LDS3508     NLTT 11300/11288                                                        Chm2004 
03348+2126   BRT3261     AB: Also known as TDS2588.                                                      
                         AB: Additional notes may be found in Couteau (1952).                    Cou1952a
             J   932     AB,C: Additional notes may be found in Jonckheere (1949) and            J__1949b
                         Couteau (1952).                                                         Cou1952a
03349-1604   GAL 353     Object #97 in Gallo's original list. ARA  17.                           Gal1912b
03350+6002   STF 400     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.96 +/- 1.62, 2.62, and 1.30 Msun, respectively.  Mlk2012 
03350+3201   STF 410     A is an ellipsoidal variable, IX Per.                                           
03351-2309   ARA1976     Rectilinear solution by Mason & Hartkopf (2016).                        Msn2016a
03352+0543   TOK 657     CPM, common parallax, both on MS.                                       Tok2014d
03353+1549   BPM  78     [PM2000]  133139 + [PM2000]  133157.                                    Gvr2010 
03354+3948   MLB1064     ALI 1035.                                                                       
03355-3218   LDS3510     NLTT 11346/11349                                                        Chm2004 
03356+4253   LDS9156     Old LDS6156.                                                                    
                         AD: NLTT 11280/11270                                                    Chm2004 
03357-1644   GWP 484     ABL 149.                                                                Tob2012b
03361-0320   J  1457     HD 22393.                                                               J__1941a
03362+4220   A  1535     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.99 +/- 0.69, 2.06, and 0.95 Msun, respectively.             Mlk2012 
03368+2106   LDS3511     NLTT 11370/11371                                                        Chm2004 
03368+0035   STF 422     A premature orbit has been computed. The primary is a variable of the           
                         RS CVn type, V711 Tau., and also a spectroscopic binary, P = 2.8 d.             
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         H 3  45.                                                                MEv2010 
03369-4957   SEE  29     The astrometric orbit of the stars comprising the A component was               
                         generated by a fit to individual data points available in Hipparcos             
                         Intermediate Astrometry Data.                                           Mkr2007a
                         Primary is possible SB.                                                 Tok2014d
             TOK 207     Likely triple. The inner pair produces RV variability and acceleration,         
                         the outer companion at 2".7 is discovered with NICI.                    Tok2012a
03370-2808   LDS 840     NLTT 11423/11421                                                        Chm2004 
03372+3710   BRT3236     ALI 283.                                                                        
03373-8517   R    39     Also appears to be R    48.                                                     
03374-8051   HJ 3607     B is CPD-81@89.                                                                 
03375+3107   GC 4314     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
03376+1751   LDS3512     NLTT 11415/11416                                                        Chm2004 
03376-0103   GWP 486     ABL 150.                                                                Tob2012b
03377+7235   HJ 2190     C component is galaxy NGC 1343.                                                 
03377-0801   GWP 487     ABL 151.                                                                Tob2012b
03378+4046   COU1517     AB Per, an Algol-type eclipsing binary, P = 7.1601d.                    Zas2012 
03378+1526   HD  22522   This star was misidentified as BD+17 0593 = SAO 93525 in the first              
                         speckle catalog.                                                        McA1984b
03379+8017   MLR 456     Also known as TDS2606.                                                          
03379+1950   LDS3515     G006-022. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 11424/11425                                                        Chm2004 
03381-1133   OL  151     Aka HEI 315.                                                                    
03382-5947   DUN  14     B is CPD-60@261.                                                                
                         SHY 448. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
03383+4448   S   430     STTA 37.  B is BD+44@759.                                                       
                         AB: HJL  50.                                                            HJL1986 
03388+5055   ES  953     Appears to be the lost HJ 2197.                                         Dam2015b
03388-1607   LDS3517     NLTT 11485/11486                                                        Chm2004 
03390+4232   RAO  47     Triple system consisting of an astrometric binary with period of 3 yr           
                         (Goldin & Makarov 2007) and Robo-AO tertiary B at 1".76. Considering    Gln2007 
                         the fast PM(A), the fixed position of AB during 1 year would appear to          
                         confirm it as a physical binary. B is located well below the MS,                
                         although its photometry has a large uncertainty. If it is a physical            
                         component with unusual colors, the system merits further study.         Rbr2015d
03392+5632   JNN 258     G 175-2. Estimated age 1000-10000 Myr; masses 0.60 +/- 0.10 and 0.38            
                         +/- 0.03 Msun; a ~24.7 au.                                              Jnn2014 
03393+5632   JNN 258     Aa,Ab: Originally 03392+5632; merged with 03393+5632.                           
03395-1017   GWP 494     ABL 153.                                                                Tob2012b
03396+3747   GRV 185     Primary is V736 Per, Algol-type eclipsing binary, period 3.76674d.      Zas2013 
03396+2530   LDS9158     old LDS6158. This is the common proper motion pair Wolf 204,5.                  
03396+1823   TOK  14     AB has estimated period 5000y; primary is 8.7d SB2.                     Tok2006 
             LDS9159     AC: Old LDS6159.                                                                
                         NLTT 11499/11500                                                        Chm2004 
             JAO   9     Ba,Bb: Referred to as G 006-026BC by Jao et al. (2016), but the C       Jao2016 
                         component is the Luyten companion. Combined astrometric/spectroscopic           
                         solution yields component masses 0.474 +/- 0.053 and 0.436 +/- 0.049            
                         Msun, plus an orbital parallax  of 26.34 +/- 0.2 mas. There is an               
                         error in their Table 3: a" = 0.0225 +/- 0.0008" (Jao, private comm.)            
03397-0331   GWP 495     ABL 155.                                                                Tob2012b
03397-1612   GWP 496     ABL 154.                                                                Tob2012b
03397-2727   LDS 841     NLTT 11538/11539                                                        Chm2004 
03398+3328   ES  327     Also known as GJ 9119 B, this star is a wide companion to GJ 9119 A at          
                         about 14" as noted in e.g. the WDS catalog. It is however single in             
                         the separation range covered by the AstraLux data.                      Jnn2012 
                         A is also a 183d spectroscopic binary.                                  Tok2019b
03398+0515   J  1812     BAL 2608.                                                                       
03400+6352   STTA 36     A,BC: HJL  51.                                                          HJL1986 
                         A,BC: SHY 160. Bayesian analysis by Shaya & Olling (2011) indicates     Shy2011 
                         very high (near 100%) probability pair is physical.                             
03401+3407   STF 425     H 2  52.                                                                MEv2010 
                         The B component was resolved at Palomar (0.580"). Genet et al. (2013)           
                         detect a wobble in the motion of AB, with P~107y, alpha~0.18"                   
                         suggesting M2~0.5 Msun                                                  Tok2014d
                         AB: known binary, which shows apparently a non-Keplerian motion. Rica           
                         Romero & Zirm (2014) proposed that the motion was caused by an unseen   FMR2014c
                         companion and calculated an astrometric orbit for it with P = 107 yr,           
                         eccentricity 0.61, and photocenter semimajor axis 0".179. Our                   
                         observations were able to resolve the predicted subsystem Aa,Ab. For            
                         the time of our observations the orbit predicts a companion position            
                         angle of 43.3 deg, in excellent agreement with the position angle of            
                         44 +/- 1.3 deg measured here. The ratio of the predicted displacement           
                         to the measured separation of 0".50 is r = 0.32 = q/(1+q). Hence, the           
                         mass ratio q = 0.47 (the contribution of the light from Ab to the               
                         photo-center is neglected). The mass of Aa is estimated at 1.16 Msun            
                         from its absolute magnitude, leading to 0.54 Msun for Ab. The absolute          
                         magnitude of Ab corresponds to a smaller mass of 0.33 Msun. This                
                         discrepancy, if confirmed, can be explained by Ab being a close pair            
                         of M-dwarfs, as happens in other known multiple systems, e.g., in kap   Tok2013a
                         For (Tokovinin 2013).                                                   Rbr2015d
                         AB: Rectilinear solutions by Rica & Zirm (2014)                         FMR2014c
                         and Genet et al. (2015).                                                GnR2015a
03402-1936   GC 4392     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
03403-0805   STF 433     B is BD-08@698.                                                                 
03404-1502   GWP 497     ABL 156.                                                                Tob2012b
03405-1925   GWP 498     ABL 157.                                                                Tob2012b
03406+2846   STF 427     H N  23.                                                                MEv2010 
                         V1268 Tau, Algol-type eclipsing binary, P = 8.161235 d.                 Zas2011 
03407+0643   A  1934     Companion not seen in 1934.                                                     
03409+1435   BPM  79     [PM2000]  137052 + [PM2000]  137046.                                    Gvr2010 
03409-1237   STF 436     B is BD-13@712.                                                                 
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
03413+4554   BU 1181     Motion in separation. The period may be fairly short. Needs speckle.            
                         Additional notes may be found in van den Bos (1963).                    B__1963b
                         Known triple system. Inner binary has been known for over a century     Bu_1894d
                         (Burnham 1894); its first orbit was computed by Riddle et al. (2015).   RAO2015 
                         They also detected a third component C which was confirmed by                   
                         examination of 2MASS images. The close binary is detectable in our Ks           
                         images, but the PSFs of the stars are overlapping and we are unable to          
                         make a consistent measurement with fitstars. We are able to extract             
                         the astrometry of the AC pair and consider it as likely physical.       Rbr2015d
03414-0934   GWP 501     ABL 159.                                                                Tob2012b
03414-1421   GWP 499     ABL 158.                                                                Tob2012b
03416+2655   LDS6095     Also known as GRV 187.                                                          
03418+6239   BLL  12     A is a semi-regular variable, U Cam. B is BD+62@594.                            
03418+5317   A   985     Primary is the eclipsing binary CV Cam, P = 0.97326 day.                Zas2010 
03419-5542   JNN  25     2MASS J03415581-5542287 and J03415608-5542408 are separated by only             
                         12" and have similar estimated spectroscopic distances (14 and 20 pc,           
                         respectively) in Riaz et al. (2006), hence it is likely that they form  Ria2006 
                         a physical pair. 2MASS J03415581-5542287 is a close (~0.61") binary in          
                         our data, so the system is likely triple in reality, although common            
                         proper motion of all components has yet to be proven.                   Jnn2012 
03422+6313   BD Cam      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin (1984).                                                         Grf1984c
03422+5436   HJ 2198     B is BD+54@704.                                                                 
03423+3141   COU 691     A premature orbit has been computed.                                            
03424+3358   STF 431     40 Per = o Per. A spectroscopic binary. Spectrum of B: A1Vn.                    
                         H 3  39.                                                                MEv2010 
03424-1200   GWP 503     ABL 160.                                                                Tob2012b
03424-8001   HJ 3612     Spectrum: G0/2III/IV. B is CPD-80@94.                                           
03425+3256   HJ  336     Also known as STF 432.                                                          
                         Rectilinear solution by Friedman et al. (2012).                         USN2012a
03425+1416   BPM  80     [PM2000]  138169 + [PM2000]  138144.                                    Gvr2010 
03425+1216   JNN  26     Since the two epochs of observation were acquired over a baseline of            
                         only a few months, there is not yet sufficient motion to confirm                
                         common proper motion of the companion that was detected with AstraLux.          
                         However, the separation between components is rather small (~0.86"),            
                         and the fact that the companion is clearly detected in z' but too               
                         faint in i' implies that it must be very red, as expected for a real            
                         companion. Hence, we count it as a binary system for statistical                
                         purposes.                                                               Jnn2012 
                         Primary is an active M4.0Ve star, age 60-300 Myr. Bowler et al (2015)           
                         confirm B is physically bound and detect slight orbital motion. The             
                         projected separation is 19.8 +/- 0.9 au. Spectral type of B is                  
                         L0 +/- 1, mass 35 +/- 8 Mjup.                                           Bwl2015 
03425+0202   BAL1260     HJL  52.                                                                HJL1986 
03426+1718   GC 4435     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
03426-2445   RST2317     TDS2636.                                                                        
03427+1448   BPM  81     [PM2000]  138368 + [PM2000]  138396.                                    Gvr2010 
03427-2428   LDS3527     NLTT 11680/11682                                                        Chm2004 
03429+4747   BUP  46     del Per = 39 Per. A possible variable of the Alpha CVn type.                    
03430+4554   JNN 259     NLTT 11633. Estimated age 1000-10000 Myr; masses 0.28 +/- 0.03 and              
                         0.20 +/- 0.04 Msun; a ~21.8 au.                                         Jnn2014 
03430+2515   LDS1148     NLTT 11651/11648.                                                               
03431+2541   STF 435     H 3  88.                                                                MEv2010 
03435+7247   LDS1579     Rectilinear solution by Hurowitz et al. (2013).                         USN2013a
03435-4549   PRB   1     Primary is WD 0341-45 = VY Hor, secondary (not found in Aladin) is              
                         BPM 31492. Possible CPM pair, according to Probst (1983).               Prb1983 
03438+4236   ENG  14     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
03439+1640   GIC  44     AB = G006-029/G006-028 = GJ 9122AB.                                             
                         AB: NLTT 11693/11688                                                    Chm2004 
                         AB: SHY  17. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
03439-7100   HJ 3603     B is CPD-71@@218.                                                               
03440+3822   STF 434     B is BD+37@@821.                                                                
03440-1836   GWP 505     ABL 161.                                                                Tob2012b
03441+3207   DCH   3     HMW 72. Monitored for photometric variability 1998-2003 by Cohen et             
                         al. (2004). Range of variability dI = 0.527 mag, no periodicity found.  CHW2004 
03442+3207   STF 437     H 3  37.                                                                MEv2010 
                         SEI  31.                                                                Nsn2017a
03442-6448   LDS 104     bet Ret. A is a spectroscopic binary. B has separation of 1480". B is           
                         CPD-65@272.                                                                     
             bet Ret     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Jones (1928).                                                           Jon1928a
03443+3217   BU  535     38 Per = omi Per = Atik. Ellipsoidal and spectroscopic binary.                  
03443+3208   DCH   4     HMW 73. Monitored for photometric variability 1998-2003 by Cohen et             
                         al. (2004). Range of variability dI = 1.271 mag; multiple periods,              
                         average = 7.582d. Photometry may be contaminated by nearby star.        CHW2004 
03444+3210   DCH   5     HMW 10/78 = LLRL 10/45. Monitored for photometric variability                   
                         1998-2003  by Cohen et al. (2004). Range of variability dI = 0.030 mag          
                         for A component, 4.816 mag for B. No periodicity found for either               
                         component. Photometry of B may be contaminated by nearby companion.     CHW2004 
03444+3207   DCH   7     HMW 136. Monitored for photometric variability 1998-2003 by Cohen et            
                         al. (2004). Range of variability dI = 0.789 mag, no periodicity found.  CHW2004 
03444+3206   DCH   6     HMW 39. Monitored for photometric variability 1998-2003 by Cohen et             
                         al. (2004). Range of variability dI = 0.251 mag; multiple periods,              
                         average = 9.667d.                                                       CHW2004 
03444+2812   A  1826     Not seen on three nights 1964-1982.                                             
03444+1637   BPM  82     [PM2000]  139475 + [PM2000]  139465.                                    Gvr2010 
03445+3212   DCH   8     HMW 13 = LLRL 12. Monitored for photometric variability 1998-2003 by            
                         Cohen et al. (2004). Range of variability dI = 0.048 mag, no                    
                         periodicity found.                                                      CHW2004 
03445+3211   DCH  10     HMW 86. Monitored for photometric variability 1998-2003 by Cohen et             
                         al. (2004). Range of variability dI = 0.318 mag, no periodicity found.  CHW2004 
03445+3210   DCH   9     HMW 75 = LRLL 40. Monitored for photometric variability 1998-2003 by            
                         Cohen et al. (2004). Range of variability dI = 0.337 mag, nonperiodic.  CHW2004 
03445+3209   DCH  12     HMW 12 = LLRL 29. Monitored for photometric variability 1998-2003 by            
                         Cohen et al. (2004). Range of variability dI = 0.181 mag; multiple              
                         periods, average = 2.237d.                                              CHW2004 
03445+3208   DCH  13     HMW 42 = LRLL 86. Monitored for photometric variability 1998-2003 by            
                         Cohen et al. (2004). Range of variability dI = 0.097 mag; multiple              
                         periods, average = 6.532d.                                              CHW2004 
03445-1322   GAL 354     Object #99 in Gallo's original list.                                    Gal1912b
03446+3210   BU  880     AB: HMW 1 = LRLL 1. Monitored for photometric variability 1998-2003 by          
                         Cohen et al. (2004). Range of variability dI = 0.455 mag, no                    
                         periodicity found.                                                      CHW2004 
                         SEI  32.                                                                Nsn2017a
             STF 439     AB,C: H 3  38.                                                          MEv2010 
03446+3209   DCH  11     AB: HMW 27/28 = LLRL 16/33. Monitored for photometric variability               
                         1998-2003 by Cohen et al. (2004). Range of variability dI = 0.097 mag           
                         for A, 1.462 mag for B. Multiple periods seen for A, average = 2.656d.          
                         Photometry of B may be contaminated by nearby companion.                CHW2004 
03446+3209   HER  20     CD: HM 107 = LLRL 165. Monitored for photometric variability 1998-2003          
                         by Cohen et al. (2004). Range of variability dI = 0.328 mag, no                 
                         periodicity found. Photometry may be contaminated by nearby star.       CHW2004 
03446+3208   HER   7     Additional notes may be found in Herbig (1962).                         Her1962 
03446+3207   DCH  14     HMW 11 = LRLL 6. Monitored for photometric variability 1998-2003 by             
                         Cohen et al. (2004). Range of variability dI = 0.094 mag; multiple              
                         periods, average = 1.687d.                                              CHW2004 
03446+2754   STTA 38     Optical with BU 1041BC, which is BD+27@558, at 03 44.7 +27 55.                  
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             BU 1041BC   The B component has both an astrometric and a spectroscopic orbit       Gln2007 
                         which are not associated with the optical BC pair.                      Grf2015c
03446-5416   HJ 3592     See claimed A was a close pair in 1897, but no trace of it was seen     See1898c
                         subsequently by van den Bos, Dawson, and Innes.                         Daw1918a
03447+3211   HER  21     HM 98 = LRLL 166. Monitored for photometric variability 1998-2003 by            
                         Cohen et al. (2004). Range of variability dI = 0.960 mag, no                    
                         periodicity found. Photometry may be contaminated by nearby star.       CHW2004 
03447+3210   DCH  15     HMW 99 = LRLL 221. Monitored for photometric variability 1998-2003 by           
                         Cohen et al. (2004). Range of variability dI = 2.136 mag, no                    
                         periodicity found.                                                      CHW2004 
03447+3209   DCH  16     HMW 14 = LRLL 9. Monitored for photometric variability 1998-2003 by             
                         Cohen et al. (2004). Range of variability dI = 0.109 mag; multiple              
                         periods, average = 2.539d.                                              CHW2004 
03447+3208   DCH  17     HMW 111 = LLRL 52. Monitored for photometric variability 1998-2003 by           
                         Cohen et al. (2004). Range of variability dI = 0.187 mag, no                    
                         periodicity found. Photometry may be contaminated by nearby star.       CHW2004 
03447+2449   ITO   7     Pleiades HII 405.                                                               
03447+2414   LDS6103     A component is Pleiades star Melotte 22 HII 430.                                
03448+4602   BAG   8     Combined astrometric/spectroscopic solution by Balega et al. (2002),    Bag2002b
                         including determination of component masses.                                    
                         The Balega (2002) orbit predicts a separation of 0.055" in mid-2006,    Bag2002b
                         opening rapidly to 0".197 in late 2007. Perhaps T0 is not quite                 
                         correct?                                                                Hrt2009 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.54 +/- 0.13, 1.54, and 0.79 Msun, respectively.             Mlk2012 
                         A(B) Teff = 5350+/-50(4400+/-50) K, R = 0.95+/-0.06(0.58+/-0.06) \rsun, AlW2014c
                         L = 0.56+/-0.01(0.10+/-0.02) \lsun, M = 0.83+/-0.05(0.60+/-0.05) \msun.         
03448+2417   HL    6     Primary is Pleiades star Celaeno = 16 Tau.                                      
03448-7002   LFR   1     SHY 450. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
03449+2407   HL    7     Primary is Pleiades star Electra = 17 Tau.                                      
                         Uniform disk diameter  0.472 +/- 0.025 mas,                                     
                         Limb darkened diameter 0.478 +/- 0.025 mas,                                     
                         Teff = 14700 +/- 800 K based on LDD.                                            
                         Radius is 5.91 +/- 0.47 \rsun.                                          CIA2019a
03452+4235   ES 2601     nu Per = 41 Per                                                                 
03452+2450   HL    8     Primary is Pleiades star 18 Tau.                                                
03452+2428   HJ 3251     Primary is Pleiades star Taygeta = 19 Tau = 19 Pleiadum.                        
                         A is a spectroscopic and occultation binary.                                    
03454+2402   HL   10     Primary is Pleiades star.                                                       
03454-2752   BU 1003     A premature orbit has been computed. Motion direct and increasing as            
                         the pair closes in. However, there are no measures in the last twenty           
                         years.                                                                          
03457+2438   YAM   1     Pleiades cluster member. Primary is the BY Dra type variable V855 Tau.  Yam2013 
03457+0603   HJ 2204     29 Tau. A is a spectroscopic binary.                                            
03458+2422   HL   11     Primary is Pleiades star Maia = 20 Tau.                                         
03458+2309   STF 444     Spectroscopic binary, P = 7.15d.                                                
03459+2433   HL   12     Primary is Pleiades star Asterope = 21 Tau.                                     
03459+2402   HL   13     Primary is Pleiades star.                                                       
03460+7302   MLR 457     Same as HDS 476.                                                                
03460+2734   CTI7214     V1274 Tau.                                                                      
03460+2432   HL   14     Primary is Pleiades star 22 Tau.                                                
03460+1721   BPM  83     [PM2000]  140561 + [PM2000]  140577.                                    Gvr2010 
03461-1522   GWP 508     ABL 163.                                                                Tob2012b
03461-1708   GWP 507     ABL 162.                                                                Tob2012b
03461-6405   HJ 3600     B is CPD-64@271.                                                                
03462+2434   POU 309     LDS6108.                                                                        
                         Both components are Pleiades variables. A = Melotte 22 HII 879 = V813           
                         Tau, while B = Melotte 22 HII 883 = V789 Tau.                                   
03462+1710   HJ 3252     This star has a possible wide companion at about 8" as noted in the             
                         WDS. It is however single in the separation range covered by the                
                         AstraLux data.                                                          Jnn2012 
03463+2411   BU  536     In the Pleiades. The motion so far is retrograde and rectilinear.       Hzg1958 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Both elliptical orbit and rectilinear trajectory were calculated by             
                         Popovic & Pavlovic (1995). See also rectilinear catalog.                Pop1995d
03463+2357   HL   15     Primary is Pleiades star 23 Tau = Merope.                                       
03463-1235   GAL 355     Object #103 in Gallo's original list.                                   Gal1912b
03464+7523   STF 418     Same as PRZ   4. Coordinates of PRZ   4 correct and retained.                   
03464+2435   ITO   8     AB: Pleiades HII 996.  Primary is the BY Dra-type variable V1045 Tau.   Ito2011 
             LDS6110     AC: Possibly common with LDS6108.                                               
03464+1143   LEP 119     LHS 1589 = NLTT 11793. Lepine et al. determine a photometric distance   Lep2007b
                         of 81 +/- 18 pc; masses are estimated at 0.25 and 0.20 Msun.                    
03465+2508   ITO   9     Pleiades HII 1015.                                                              
03465+2426   ITO  10     Pleiades HII 1032.  Primary is V1171 Tau. Both companions are                   
                         background stars.                                                       Yam2013 
03465+2415   CHR  12     Pleiades cluster member.                                                        
                         1985.8488: This measure is from reanalysis of archival data.  Not               
                         listed as an SB by Abt et al. (1965), but it may show measurable        AbH1965b
                         velocity variation at some phases of a possibly eccentric orbit.        Msn1993b
                         Aa,Ab: Observed 20 times 1982-1998 and resolved 4 times 1983-1989,              
                         with separations decreasing from 0.236" to 0.160". Motion indicates a           
                         ~40-year period orbit.                                                  Hrt2009 
03466+2950   BRT 233     MLB 683.                                                                        
03466+2458   MET  34     Pleiades cluster member. The companion is a background star.            Yam2013 
03466+2255   RDR   2     Primary is an F6 Pleiades member (HII 1132). Based on common motion             
                         over 4 years, Rodriguez et al. (2012) conclude the B component is               
                         either a companion to the primary or (less likely) a nearby comoving            
                         Pleiades member. Assuming they comprise a physical pair, the companion          
                         is a brown dwarf, with mass estimated at 0.06 +/- 0.01 Msun,                    
                         temperature 2600 +/- 100K.                                              Rdr2012b
03467+2402   LDS6111     A component is a Pleiades variable = Melotte 22 HII 1124 = V814 Tau.            
03467-1231   GAL 356     Object #104 in Gallo's original list.                                   Gal1912b
03470+4126   STF 443     HIP 17666. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AB: NLTT 11792/11791                                                    Chm2004 
                         Proper motion of A +596 -1249. Proper motion of B +594-1259. B is a             
                         single-lined spectroscopic binary, P = 48.65d. A common proper motion           
                         companion, G095-059, mag. 13.4, lies more than 2 degrees away.                  
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: HJL  53.                                                            HJL1986 
03470+2431   CHR 124     Occultation binary. Has variable radial velocity. Pleiad.                       
03471+2449   BU  537     Variable, V534 Tau.                                                             
03473+2424   BOV  18     Geissler et al (2012) conclude companion is an M8 brown dwarf, the              
                         first substellar companion discovered around a Pleiades star.  Mass             
                         estimates range from 0.052 to 0.063 Msun, depending on distance, etc.   Gei2012 
                         Pleiades cluster member. The companion shares common proper motion.     Yam2013 
03473+2348   HL   18     Primary is Pleiades star.                                                       
03473+2344   HL   19     Primary is Pleiades star.                                                       
             BOV  17     CF: 03471+2343BOV  17 = HL  19C, system merged.                                 
03474+2435   HL   20     Primary is Pleiades star.                                                       
03474+2355   STF 450     POU 311. Primary is Pleiades star.                                              
03474+2255   HD 23610    Hipparcos astrometric solution assumed circular orbit (e = omega = 0);  HIP1997d
                         Cluster Melotte 22 #1407.                                                       
03475+2417   HL   22     Primary is Pleiades star.                                                       
03475+2406   STFA  8     Primary is Pleiades star Alcyone = 25 Tau = eta Tau = V647 Tau.                 
                         STTA 42.                                                                        
                         A is an occultation and spectroscopic binary.                                   
                         B, at 03 47.4 +24 07, is an occultation binary.                                 
                         C is V647 Tau.                                                                  
                         BC: HJL1029.                                                            HJL1986 
                         BD: HJL1028.                                                            HJL1986 
                         CD: HJL1027.                                                            HJL1986 
03476+2337   HL   24     Primary is Pleiades star.                                                       
03478+3501   ES  235     Primary is eclipsing binary of Algol-type, period 1.92873d.             Zas2014 
03478+3212   HR 1164     Orbit determined by fitting revised Hipparcos intermediate astrometric          
                         data. Derived component masses 1.44 +/- 0.09 and 1.15 +/- 0.08 Msun.    Ren2010 
03479+3336   STF 448     HJ 5457. A is a spectroscopic binary. Also, one component is variable.          
03479+2555   BRT2520     Heintz finds no pair in the field, and believes identity with J 27      Hei1985a
                         (03470+2855) is possible.                                                       
03479+2407   BU  538     AB. Identification of a 2000.8 measure by Lampens et al. (2007)         Lmp2007 
                         originally attributed to 03481+2409 COU  80 was corrected by the                
                         author; it actually was of this pair.                                           
03480+6840   KUI  13     See discussion by van de Kamp & Chao-Yuan Yang.                         Kam1967 
             WNO  16     AD: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         BD: Rectilinear solution by Hartkopf & Mason (2015).                    WSI2015 
03480+4032   TOK 240     Primary is an exoplanet host, P=1565d                                   Tok2014d
03480-7048   HJ 3606     B is CPD-71@223.                                                                
03481+2409   COU  80     Pleiad.                                                                         
                         Identification of a 2000.8 measure by Lampens et al. (2007) originally  Lmp2007 
                         attributed to this pair was corrected by the author; it actually was            
                         of 03479+2407 BU  538AB.                                                        
03482+2419   CHR 155     Included in the Pleiades cluster survey of Abt et al. (1965), who did   AbH1965b
                         not detect variable RV. Pearce & Hill (1975 Pub DAO, 14, 319) did               
                         notice velocity variation at the 1% level, and Liu et al. (1997) found  Liu1997 
                         the system to be a SB2, although large velocity difference may imply a          
                         closer companion than this.                                             Msn1993b
03482+2219   EQ Tau      Multiple system including contact binary. Pribulla & Rucinski (2006)    Pbl2006 
                         estimate the mass of the contact pair at 1.752 Msun and the minimum             
                         mass of the wider component at 0.49 Msun.                                       
03483+2325   HL   25     Pleiades H 722. Primary was misidentified as SAO 76125 in the first             
                         speckle catalogue.                                                      McA1984b
03483+1109   STF 452     30 Tau.                                                                         
                         H 3  66.                                                                MEv2010 
03483-0943   GWP 517     ABL 164.                                                                Tob2012b
03484+5202   HU  546     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.17 +/- 0.43, 1.53, and 1.20 Msun, respectively.             Mlk2012 
03486+3039   SHY 453     HIP  17796 + HIP  18204.                                                        
03486-3737   DUN  16     f Eri. One component is a possible Beta Lyrae-type system.                      
03489+6445   STT  62     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.82 +/- 0.52, 2.75, and 1.20 Msun, respectively.             Mlk2012 
03489+2351   HL   27     Primary is Pleiades star 26 Tau.                                                
03490+5120   LDS9160     Old LDS6160. NLTT 11871/11873.                                                  
03491+4358   V376 Per    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
03491+2347   TRR  16     V1282 Tau.                                                                      
                         Ma,Mb = 0.978 +/- 0.024, 0.897 +/- 0.022 \msun. Orbital parallax is             
                         7.310 +/- 0.026 mas. Spectroscopic dm (518.7 nm) = 0.63.                Trr2020b
03492+3651   J  2721     BRT 2586. ALI 288.                                                              
03492+2408   CHR 125     Aa,Ab: Pleione, 28 Tau = BU Tau. Shell star and suspected long-period           
                         spectroscopic binary (Hoffleit 1982) . Pleiades cluster member.         Hof1982 
                         Frequently unresolved, probably due to large Delta m.                   Msn1993b
                         For their measure, Roberts et al. reports that the "The close                   
                         proximity of the two star's PSFs prevented accurate measurement of the          
                         astrometry and photometry."                                             Rbr2007 
                         Aa,Ab: Observed 3 times 1987-1991 (all observations noted as weak),     Rbr2007 
                         then unresolved until a 2002 (0.24") measure at 900nm                   Hrt2009 
             RBR   4     AF: 2002.0924: PA is measured in zenith mode. If data collected in              
                         equatorial mode, PA = 119. Confirmation of the pair should establish            
                         the correct value for theta.                                            Rbr2007 
03492+2403   STF 453     Primary is Pleiades star Atlas = 27 Tau = Melotte 22 #2168                      
                         Position angles scattered. Distances range from "single" to 0.6". Some          
                         question duplicity. A is a long-period spectroscopic binary.                    
             MKT  12     Aa1,Aa2: Hipparcos astrometric solution assumed circular orbit (e =             
                         omega = 0).                                                             HIP1997d
                         Pan et al. (2004) orbit is based on Mark III and PTI measures. A        PTI2004 
                         distance to the Pleiades of 135 +/- 2 pc is determined. Masses for the          
                         components are calculated as 4.90 +/- 0.28 and 3.65 +/- 0.08 Msun.              
                         Zwahlen et al. (2004) orbit is based on published Mark III and PTI      Zwa2004 
                         measures, plus additional Mark III and NPOI astrometric data and                
                         ELODIE echelle spectra. This combined spectroscopic/interferometric             
                         solution yields masses of 4.74 +/- 0.25 and 3.42 +/- 0.25 Msun; the             
                         distance 132 +/- 4 pc found agrees with "traditional" Pleiades                  
                         distances obtained through MS fitting techniques.                               
                         Aa1,Aa2: Malkov et al. (2012) derive dynamical, photometric, and                
                         spectroscopic masses 5.68 +/- 0.79, 6.68, and 3.31 Msun, respectively.  Mlk2012 
                         Uniform disk diameter  0.464 +/- 0.043 mas,                                     
                         Limb darkened diameter 0.469 +/- 0.043 mas,                                     
                         Teff = 13500 +/- 300 K based on LDD.                                            
                         Radius is 5.98 +/- 0.67 \rsun.                                          CIA2019a
03493+5707   S   436     STTA 39. B is BD+56@847.                                                        
                         HJL1030.                                                                HJL1986 
03493-1656   GWP 519     ABL 165.                                                                Tob2012b
03494+5214   ES  770     B is BD+51@781.                                                                 
03494+2423   STTA 40     AB: LDS6116. B is BD+23@560. A is Pleiades star and occultation double          
             HL   30     BC: Primary is Pleiades star.  Also known as STU   2BC.                         
             HL   30     BD: Also known as STU   2BD.                                                    
03495+5239   STF 446     Also known as STF 454. Another classification: B0Ib. The primary is             
                         slightly variable; the system is a member of the cluster NGC 1444.1             
03495+1255   AG   74     Primary is V1128 Tau, a 10th magnitude W UMa type eclipsing binary,             
                         with period 0.3053725d.                                                 Zas2011 
03496+6318   CAR   1     Also known as MOAI 1.                                                           
                         1995.948: Theta corrected from published value of 213 deg (Aristidi,            
                         private communication)                                                          
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.76 +/- 0.61, 3.36, and 1.82 Msun, respectively.             Mlk2012 
03496+3859   HU 1067     A RW Aur-type variable, XY Per. Both components may vary.                       
                         dm estimates on a number of nights. quadrant reversed on 1936 Jan 17,           
                         indicating primary is responsible for variation. Beyer (AN 263, 71,             
                         1937) established the irregular character of the variation.             VBs1954 
03496-0220   YR   23     Triple. The RV amplitude of 9.5 km s-1 and double lines seen in GCS             
                         cannot be caused by the visual system YR 23 with estimated period of            
                         ~50 yr which could however be responsible for dmu.                      Tok2012a
                         The Hipparcos parallax, individual magnitudes and standard relations    Tok2018a
                         for main-sequence stars leads to masses of 1.14, 0.96 and 0.80 \msun            
                         for A and the unresolved Ba and Bb pair.                                        
                         Ba,Bb is estimated to have a dM in V band of 1.2 and a maximum                  
                         separation of 26 mas.                                                           
03497+2343   HL   32     Primary is Pleiades star.                                                       
03497+2320   YAM   2     BC: Pleiades cluster member. The companion is a background star.        Yam2013 
                         Pair initially 03495+2323 YAM 2; merged with 03497+2320 LDS6118.                
03498+2421   HL   33     Primary is Pleiades star.                                                       
03498+2342   ITO  11     Pleiades HII 2462.                                                              
03499+2313   ITO  12     Pleiades HII 2506.                                                              
             YAM   3     Pleiades cluster member. The companion is probably a background star.   Yam2013 
03500+2351   STT  64     A is a spectroscopic binary, P = 16.72d, spectrum B9.5VpSiSrCr. Pleiad          
03501+4458   CHR 126     A spectroscopic binary.                                                         
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         P'edoussaut et al. (1987).                                              Ped1987 
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Pedoussaut et al. (1987).                                               Ped1987 
03501+0637   TOK  80     HIP 17936. The magnitude difference in the 2MASS PSC dK=1.8 is                  
                         suspect (5" separation), dK=3.4 is measured with ANDICAM.               Tok2011a
03502+3449   ES  277     AB: Rectilinear solution by Hartkopf & Mason (2015).                    WSI2015 
03502-1335   FAR  32     NLTT 11972. Primary is white dwarf WD 0347-137.                         Far2006 
03503+2535   STT  65     One star variable?                                                      Wor1967b
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.15 +/- 0.39, 3.39, and 3.91 Msun, respectively.             Mlk2012 
03503-0131   SHY 164     AE: HIP  17950 + HIP  16933. E component = A component of 03379-0231.           
                         AB: Hipparcos identified the pair as a candidate for Hyades membership. HIP1998 
                         However, radial velocity classifies this as not a Hyades member.        Grf2013c
03504+7120   HJ 2200     gam Cam                                                                         
03505-1219   GAL 357     Object #105 in Gallo's original list.                                   Gal1912b
03506+2431   YAM   4     Pleiades cluster member. Primary is V1174 Tau.                          Yam2013 
03506-4234   EGN   3     Pair bound, with projected separation 73au. Mass of secondary                   
                         0.15 +/- 0.01 Msun; spectral type M4-M6.                                Egn2007 
03507-1206   GAL 358     Object #106 in Gallo's original list.                                   Gal1912b
03508+4546   FMR  63     Typographical error in initial WDS designation (03508+4946)                     
03510+1414   JLM   1     Erroneously labelled as JML 1; changed upon request of discoverer.              
03511+3548   BRT3238     ALI 51.                                                                         
03511+1551   BPM  84     [PM2000]  144054 + [PM2000]  144088.                                    Gvr2010 
03513+2621   A  1830     The few observations do not define the nature of the motion.                    
03514+2538   HEI   9     Primary is eclipsing binary of Algol-type, period 1.26292 d.            Zas2012 
03514-1610   GWP 523     ABL 166.                                                                Tob2012b
03517+7030   HJ 1139     B is BD+70@263.                                                                 
03517+2433   LDS5437     A component is a Pleiades variable = Melotte 22 HII 3096 = V1054 Tau.           
                         B component is flare star V383 Tau.                                             
03518+3453   ARN  58     Also known as GRV 196.                                                          
03518-0306   GWP 524     ABL 167.                                                                Tob2012b
03520+2440   BOV  27     AB: Assuming a Pleiades parallax of 7.43 +/- 0.17 mas (distance 134.6           
                         pc; Soderblom et al. 2005, AJ 129, 161), Schaefer et al. (2014) find a          
                         total mass of 1.42 +/- 0.10 Msun. The revised Hipparcos parallax of             
                         8.32 +/- 0.13 (120.2 pc; van Leeuwen 2009, A&A 497, 209) gives a total          
                         mass of 1.01 +/- 0.05 Msun, which is not consistent with the                    
                         corresponding photometric masses of the components.                     Sfr2014 
03520+0632   KUI  15     31 Tau.                                                                         
                         AB: Additional notes may be found in Van Biesbroeck (1954) and          VBs1954 
                         Couteau (1955).                                                         Cou1955c
03525+3546   ES 2334     BRT 3239. ALI 52.                                                               
03525-0403   GWP 525     ABL 168.                                                                Tob2012b
03526-0829   RST4762     The few measures do not define the motion.                                      
03527-0522   HJ  338     30 Eri.                                                                         
03529+3532   ES 2459     BRT 3240.                                                                       
03529-0633   GWP 528     ABL 169.                                                                Tob2012b
03530+1158   BPM  85     [PM2000]  145369 + [PM2000]  145423.                                    Gvr2010 
03530-1332   GWP 529     ABL 170.                                                                Tob2012b
03534+1743   BPM  86     [PM2000]  145657 + [PM2000]  145663.                                    Gvr2010 
03535+3538   ES 2460     Identical to ALI 54 and BRT 3237                                        Hei1983a
03535+3307   RBR  36     Suspected non-single.                                                   Hor2002b
03535-1229   GAL 359     Object #107 in Gallo's original list.                                   Gal1912b
03535-1440   GWP 531     ABL 171.                                                                Tob2012b
03536+2718   OCC9003     The OCC2010 solution is ambiguous and one is arbitrarily "T" coded              
                         until the true solution is determined.                                          
03536+2146   OL  184     TDS2678. Appears to be the same as 03549+2148 OL  200. IDS notes that           
                         OL  200 is possibly identical to 03559+2146 HU  815, but they appear            
                         to be different pairs.                                                          
03537+5316   A  1293     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.00 +/- 0.24, 1.94, and 1.05 Msun, respectively.             Mlk2012 
03539-1751   GWP 532     ABL 172.                                                                Tob2012b
03541+3153   STF 464     zet Per = 44 Per. A is a spectroscopic binary.                                  
                         AD: H 6  96.                                                            MEv2010 
03543-0257   STF 470     32 Eri. A is a spectroscopic binary.                                            
                         AB: H 2  36.                                                            MEv2010 
03544+0116   TOK  81     RoboAO finds a companion to B (233deg, 3.05", dI=5.88mag), but it is            
                         thought to be optical.                                                  Tok2014d
03544-0649   A   461     Less than 0.1" in 1954 - 1961. It appears that a revolution has been            
                         completed.                                                                      
03544-4021   FIN 344     Spectroscopic binary.                                                           
                         1989.9438: This is the first observation of this system since those of          
                         Finsen in the 1960's, and is considerably closer than any of his                
                         results.  It is known that in some instances Finsen's rho values                
                         appeared systematically larger than those of speckle; further                   
                         observations of this system will determine whether such is again the            
                         case.                                                                   Hrt1993 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 4.24 +/- 0.59, 4.58, and 4.88 Msun, respectively.  Mlk2012 
03545+3203   LEI   6     Member of Taurus-Auriga molecular cloud.                                Dae2015 
03545+0510   STTA 41     A is a Delta Scuti-type variable, V479 Tau. B is BD+04@@600.                    
                         A,BC(60") is probably physical.                                                 
             A  1831     BC: Less than 0.1" in 1954 - 1955 with 82-inch.                                 
                         A premature orbit has been computed. Motion direct.                             
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
03546+3519   HJ  669     AC: Rectilinear solution by Hartkopf & Mason (2015).                    WSI2015 
03546+2507   HAT   1     30' error in WDS designation.                                                   
                         Member of Taurus-Auriga molecular cloud.                                Dae2015 
03546+2131   LDS1149     Old LDS6161. LDS9161.                                                           
03547+5200   TOR   5     Formerly known as PAN   2.                                                      
03547+1529   BPM  87     [PM2000]  146665 + [PM2000]  146678.                                    Gvr2010 
03547-1811   GWP 533     ABL 173.                                                                Tob2012b
03548-3542   TOK  82     HIP 18305. NOMAD: PM(B)=(-89,+19), V=11.48(??).                                 
                         PM(A)=(+108,+218).                                                      Tok2011a
03549-1426   GAL 360     Object #109 in Gallo's original list.                                   Gal1912b
03553-0237   BRT1928     BAL 25.                                                                         
03553-1921   GWP 534     ABL 174.                                                                Tob2012b
03554+3103   HO  325     A is a RW Aur-type variable, X Per, and also a long-period                      
                         spectroscopic binary.                                                           
03557-2236   I   722     CD-22@1398.                                                                     
03558+5225   TOR   6     Formerly known as PAN   3.                                                      
03558+5224   STF 462     HJ 2206.                                                                        
03561-4509   CPO 121     LDS 108.                                                                        
03561-4746   HU 1361     HIP 18402. B is definitely physical, but it is too red in the                   
                         (Kabs,V-K) CMD. Infrared companion? Nothing on B in SIMBAD.             Tok2011a
03562+5939   ENG  16     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             HDS 497     AD: CfA: P=12625d=34.6y? Abt & Willmarth (2006): RV=-22.18 const.       AbH2006 
03563-1935   GWP 535     ABL 175.                                                                Tob2012b
03564+4404   LDS5186     NLTT 12174/12173                                                        Chm2004 
03565-3642   BAS   2     This is the X Ray source EUVE J0356-36.6.                                       
03566+6951   LDS1583     A is also a 1539d spectroscopic binary.                                 Tok2019b
03566+5042   S   440     43 Per. A is a spectroscopic binary. B is BD+50@861.                            
             CIA  16     Aa,Ab                                                                           
                         Mass = 1.434 +/- 0.014, 1.409 +/- 0.014 \msun for A and B.              CIA2020a
                         Radius = 1.67 +/- 0.06, 1.60 +/- 0.10 \rsun for A and B.                        
                         Teff = 6790 +/- 120, 6770 +/-  90 deg K for A and B.                            
                         Age = 1.4 Gyr, distance = 38.7 +/- 0.2 pc.                                      
                         AB: H 5  41.                                                            MEv2010 
03569+2005   OCC1090     OCC9087.                                                                        
03571-0828   RST4764     Rapid retrograde motion.                                                        
03572-0706   OSW   7     Typographical error in WDS - initially entered as 03572-0025, with dec          
                         portion copied from OSW 8.                                                      
03573-1054   GWP 536     ABL 176.                                                                Tob2012b
03575-0110   BU  543     A premature orbit has been computed. A is a flare suspect.                      
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         NLTT 12237/12236                                                        Chm2004 
03576+5712   ES 1820     Doubtful this system is physically bound, since relative motion is              
                         larger than pm of A.                                                    Kiy2012 
03578+4932   KU   82     B is BD+49@1068.                                                                
03579+5142   SCA 176     Scardia (2017) measured an 8" pair located near the close (0".4) pair   Sca2017b
             COU2358     COU2358. Proper motions for the COU pair and the primary of the SCA     Cou1988b
                         pair were similar, so they were merged into one multiple system, with           
                         an 18" pair added to link them. This wide pair was given the same SCA           
                         176 discoverer designation and assigned components AB. The components           
                         for the COU pair were changed to Aa,Ab, those of the 8" pair to BC.             
03579+4001   STF 471     eps Per = 45 Per. A is a Beta Lyrae-type binary.                                
                         AB: H 2  22.                                                            MEv2010 
03580-1331   HJ 3608     gam Eri = 34 Eri = Zaurak. Variable?                                            
                         The faint pair, presumeably the original system, was recovered in       Dal2009 
                         2009, which appears to have common proper motion. All subsequent                
                         measures of the HJ 3608 were of a more distant pair with linear                 
                         motion relative to the primary, presumeably optical.                            
                         Mk III Limb-darkened diameter  9.332 +/- 0.173 mas.                     MkT2003 
03583+2757   ARG  58     AG 75.                                                                          
03583-1659   GWP 537     ABL 177.                                                                Tob2012b
03584+2538   LDS5459     Also known as LDS9162.                                                          
                         NLTT 12251/12250                                                        Chm2004 
03586-0239   BU 1042     B is BD-03@651.                                                                 
03587+1646   LDS5462     GWP 538. Luyten's original 1960 measure listed theta = 144deg, 90deg    Luy1984 
                         different from the angle found by Bernal. Agreement on coordinates,     ABl2012a
                         separation, and magnitude difference led to the conclusion Luyten made          
                         a trigonometry error in his reduction.                                          
03590+3547   TRN  16     = ksi Per = Menkib.                                                             
                         The image rotator was in an unknown state, so two possible theta                
                         values are listed for the 2001.7342 observation - one for zenith up             
                         and one for north up.                                                   Trn2008 
                         Uniform disk diameter  0.216 +/- 0.016 mas,                                     
                         Limb darkened diameter 0.245 +/- 0.010 mas,                                     
                         Radius is 10.1 +/- 1.3 \rsun.                                           CIA2018e
03590+0947   HU   27     The value of omega for Ling's (2001) orbit was incorrectly given as     Lin2001b
                         263.1 in IAU Inf. Circ. 144.                                                    
                         Ling (2004) derived an orbital parallax 0".01239 and a mass sum of      Lin2004a
                         1.94 +/- 0.82 Msun.                                                             
03590-0056   HEI 215     Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
                         However, radial velocity classifies this as not a Hyades member.        Grf2013c
03591-0656   LDS3545     NLTT 12296/12294                                                        Chm2004 
03591-2312   FAR   3     FAR  33. Primary is white dwarf WD 0357-233.                            Far2005b
03592+8020   JNN  27     A companion to 2MASS J03591438+8020019 was detected on two separate             
                         occasions with AstraLux, in both cases the detection is rather                  
                         tentative, but since it is detected twice with consistent properties            
                         we count it as a genuine detection. However, due to the poor quality            
                         of the fit and the fact that the two epochs of observation are only             
                         separated by 3 months, we do not try to acquire two epochs of                   
                         astrometry, but merely quote the astrometry as the mean (and standard           
                         deviation) of the two epochs.                                           Jnn2012 
03593+5714   MZA  43     MY Cam.                                                                         
03596-1019   HU   29     Motion in a highly-inclined orbit.                                              
03597+4809   STT  68     A is an Algol-type binary, IQ Per. B is BD+47@921.                              
03597-1147   GWP 540     ABL 178.                                                                Tob2012b
03597-1301   GAL 361     Object #110 in Gallo's original list.                                   Gal1912b
03598+1133   STF 478     LDS5464.                                                                        
03599+1325   LDS1150     Aka LDS5465.                                                                    
04005+1935   KOH   1     Metchev & Hillenbrand say pair probably physical, based on proximity.   Met2004b
                         Member of Taurus-Auriga molecular cloud.                                Dae2015 
04005-4145   DON  58     B is above the MS in (V,V-K). Tuc-Hor moving group? (Kiss et al., 2011          
                         MNRAS 411, 117)                                                         Tok2014d
04005-5120   TOK  83     HIP 18713. NOMAD: PM(B)=(+44,+43). PM(A)=(+162,-39).                    Tok2011a
04007+2023   BD+19  641  Hyades vB 9                                                                     
                         SB with P > 7 yr according to Griffin et al. (1988).                    Grf1988 
04008+1812   BUP  49     A is a spectroscopic binary. B is BD+17@664.                                    
04008+0505   A  1937     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.32 +/- 1.76, 2.84, and 2.00 Msun, respectively.             Mlk2012 
04009+2312   STF 479     H N 93.                                                                         
04009-1027   STF 487     B is BD-10@814.                                                                 
04018+2303   LDS5476     Aka RAO 114.                                                                    
04021-3429   BU 1004     HIP 18824. See Allen et al. (2000) for information on metallicity,      AlC2000 
             LDS3551     age, galactic orbital parameters, etc.                                          
             BU 1004     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             LDS3551     AD: Holberg et al. (2013): D at 64" is CPM, WD(DA9.9)                   Hbg2013 
04022+2808   STF 481     AD: Declination difference 11.18".                                              
                         AD: Component D is 04039+2808VBS   9.                                           
04024-2832   DAW  79     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.29 +/- 0.72, 2.25, and 1.07 Msun, respectively.             Mlk2012 
04025+0638   HDS 510     Cvetkovic et al. (2016) estimate spectral types K2 and K3, masses 0.81          
                         and 0.79 Msun. Dynamical parallax is 13.24 +/- 0.28 mas.                Cve2016b
04025-6121   LDS 109     Jenkins et al. (2010 A&A 515, 17): RV(A) var with P>6.5yr, M2min=66     CPS2002b
                         Mjup. However, Jones et al. (2002) do not detect RV variation.          Tok2014d
04027+3210   HJ  670     SEI  34.                                                                Nsn2017a
04029+1228   BPM  88     [PM2000]  152895 + [PM2000]  152883.                                    Gvr2010 
04030-3322   BRT1587     A likely plate flaw.                                                    Grv2021b
04031-1149   GAL 362     Object #113a in Gallo's original list.                                  Gal1912b
04032+2553   DCH  45     HBC 356/357 = V1067 Tau.                                                        
                         Member of Taurus-Auriga molecular cloud.                                Dae2015 
04033+3516   OSO  16     Not a common proper motion pair, based on comparison with POSS2 red             
                         plates. PM of A = +1732 -1356.                                          Oso2004 
04033+1820   BPM  89     [PM2000]  153212 + [PM2000]  153228.                                    Gvr2010 
04036-3611   WHI   5     Listed as possibly resolved by White et al. (1991).                     Whi1991 
04037-1545   A  2913     1989.9413: This system closed steadily from its discovery at 0".45 in           
                         1915 to 0".22 in 1959; this is the first observation in 30 years so it          
                         is unknown whether the pair has passed through periastron.              Hrt1993 
04038+3758   ES 2085     A is V380 Per.                                                                  
04038-4429   LCL 120     AB: B is CD-44@1388.                                                            
                         AB: Additional notes may be found in Herschel (1847).                   HJ_1847a
             SHY 458     AC: HIP  18958 + HIP  18888.                                                    
04039+2808   VBS   9     An Algol-type binary, RW Tau.                                                   
                         This is the D component of 04022+2808.                                          
04040+3932   L    51     Not found in Heintz at IDS position.                                    Hei1987a
04042+2324   OSO  17     Not a common proper motion pair, based on comparison with POSS2 red             
                         plates                                                                  Oso2004 
                         Suspected non-single.                                                   Hor2002b
04043-1231   GAL 363     Object #116 in Gallo's original list.                                   Gal1912b
04044+2406   MCA  13     36 Tau. A is an occultation binary, first detected by Dunham et al.     Dnh1973 
                         Now resolved by speckle interferometry.                                         
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 16.02 +/- 8.21, 11.83, 2.92 Msun, respectively.    Mlk2012 
04044+2025   RED   1     1996.0656: RHy ID and coordinates from Reid (1992).                     Red1992 
                         LP ID from Luyten et al. (1981)                                         Luy1981 
                         Candidate Hyades member; Reid considers definite binary.                Red1997 
04045+1512   BPM  90     [PM2000]  154069 + [PM2000]  154068.                                    Gvr2010 
04046+5504   HO  221     Both A and B are above the MS. AC: reflex PM(A), likely optical.        Tok2014d
04047+2205   STT 558     AB: 37 Tau.                                                                     
04047-0303   LDS3555     NLTT 12486/12488                                                        Chm2004 
04049-3527   CHR 224     AC. Surprisingly, no record of this wide companion to the 0".8 pair             
                         I 152 is listed in the WDS, despite 17 observations spanning 90+ years          
                         since Innes' discovery in 1896.  Misidentification appears ruled out,   I__1897b
                         since both the Innes pair and the new component are seen on two                 
                         separate occasions.                                                     Hrt1996b
04050+3705   KU   83     AB: HJL  55.                                                            HJL1986 
04050-0600   BFR   4     BD-06 813 + 2MASS J04050209-0600409. Baron et al. (2015) estimate               
                         spectral types K0 and M6.5 +/- 1, distances 68 +/-10 and 86 +2/-37 pc,          
                         masses 0.925-1.014 and 0.096-0.114 Msun.                                BFr2015 
04053+2201   CHR 158     Aa,Ab: 39 Tau. Variable?                                                        
                         Aa,Ab: Observed 7 times 1985-1998, then resolved at 0.22" in 1988       McA1993 
                         (note: "uncertain"), unresolved in 2002 (3.6m AO), and finally          Rbr2005 
                         resolved at 0".41 in late 2003                                          Hrt2009 
04056+1255   BPM  91     [PM2000]  154891 + [PM2000]  154924.                                    Gvr2010 
04057+2248   COU 151     Metchev & Hillenbrand say the AB pair is probably physical, based on            
                         proximity.                                                              Met2004b
04058+7117   LDS1589     NLTT 12426/12424                                                        Chm2004 
04059+3438   ES  238     A measure in 1946 gives distance as 7.2".                                       
04063+3548   BRT3241     ALI 57.                                                                         
04063+1952   BAG   4     A preliminary circular orbit is determined                              Bag2001 
04064+4325   A  1710     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.72 +/- 0.73, 2.49, and 0.95 Msun, respectively.             Mlk2012 
04065+1422   S   443     B is BD+13@643.                                                                 
04066+2018   BNV   2     V1300 Tau. DAE 17. Member of Taurus-Auriga molecular cloud.             Dae2015 
                         Primary is F8-G1, mass = 1.14 +/- 0.05 Msun, age = 25 +25/-10 Myr,              
                         Teff = 5970-6100K. Secondary is M8-L1, mass = 32 +18/-14 Mjup,                  
                         Teff = 2537 +95/-182K.                                                  Bnv2014 
04066-6019   R    40     B is CPD-60@292. Spectral type of B may be G8.                                  
04067+1309   BPM  92     [PM2000]  155660 + [PM2000]  155680.                                    Gvr2010 
04067+0324   HJ 2221     A component: V = 11.8; B-V = +0.9; Spectral type: K-M.                          
                         B component: V = 13.5; B-V = +0.8; Spectral type: M                     FMR2000a
04068+5035   HU  547     Variable of unknown type.                                                       
04069+3327   STT  71     A is an Algol-type eclipsing binary, AG Per, P = 2.03d.                         
04070-1000   SHY 165     AB: HIP  19206 + HIP  21489.                                                    
             HDS 521     Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 1.68 +/- 0.48, 2.13, and 1.96 Msun, respectively.  Mlk2012 
04070-2200   HU 1363     1994.8069: Quadrant determined by speckle imaging analysis.             Hor1996 
04072+2731   TOK 241     Makarov & Kaplan (2005) note as astrometric companion to A, but there   Mkr2005 
                         is RV data for A to support this astrometric sub-system.                Tok2014d
04073-2429   BEU   5     Rectilinear solution by Miles & Mason (2016) and                        Msn2016b
                         Mason et al. (2018). Despite linear solution, based on proper motion    Msn2018a
                         and parallax appears to be physical.                                            
04075-5234   TOK  15     Astrometric binary in Hipparcos catalog. Estimated period of visual             
                         pair 6y. Primary is 2.5d SB1. G-solution in HIPPARCOS.                  Tok2006 
                         Triple system, consisting of 2.5d SB and 0".1 tertiary companion                
                         discovered by Tokovinin (2006) and previously revealed by Hipparcos     Tok2006 
                         acceleration and RV trend. It is not resolved here; apparently it               
                         closed in.                                                              Tok2013b
04076+3804   STT 531     A: V491 Per. CPM with BD+37@882 (50 Per), 12' distant.                  Cou1955c
                         Premature orbits have been calculated. Motion retrograde.                       
                         G039-001. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
             ALC   1     AE: Also known as BU  545CA.                                                    
                         AE: SHY  19. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         E: 50 Per = V582 Per.                                                           
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
04077+1510   STF 495     A is a Delta Scuti-type variable. A = Hyades vB 11, B = Hyades vB 12.           
                         AB pair, with rho = 3".8 is outside our detection window.               Msn1993a
04077+1413   LDS5187     old LDS6164.                                                                    
04078+6220   ES 2603     SZ Cam                                                                          
             STF 485     The classification is from Chocol (1980 Bull. Astron. Inst. Czech. 31,          
             CHR 209     321).  The discovery of speckle companion CHR 209 Ea,Eb with a period           
             WSI  20     of some 60 y confirms the third body model advocated by  Mayer et al.           
             HZG   2     (1994 A&A 288, L13) based on the appearance of the spectrum and                 
             HLM   3     variations in the time of light curve minimum (they suggest a third             
                         body period of 50.7 y).  Another light curve solution is given by               
                         Harries et al. (1998 MNRAS 295, 386).  The B component was also                 
                         observed and appeared to be single. Classification of the B component           
                         is from the WDS.                                                        Msn1998a
                         This complex multiple system has had numerous identification errors             
                         due to various difficulties. The diagram of Lewis in his catalog of     L__1906b
                         the Struve pairs, which seemed a good first step, was hampered by the           
                         quadrant error of the pair he designated Ca. This quadrant error was            
                         repeated in the ADS, IDS, and in earlier editions of the WDS. In the            
                         ADS (where this pair is listed as #2984, but note that #2989 is part            
                         of this system, too) the errors multiplied. The pair Holmes AF (WDS             
                         designation HLM   3AF) is apparently the same as STF 485Ac. Inspection          
                         of scanned images of this region of the sky have allowed the                    
                         Hertzsprung pairs (HZG   2) whose components are given within                   
                         quotation marks in the ADS to be identified. Of the HZG pairs, the              
                         "CD" pairing is the same as STF 484AC and the "CE" pairing is the               
                         same as STF 484AB. The ADS note to the "AJ" pairing of HZG   2 is a             
                         typographical error. The correct position angle is 77 degrees, which            
                         corresponds to the AD (now AO) pair. Below outlines the changes from            
                         the WDS 2001.0 to the current version.                                          
                                                                                                         
                         ES 2603Aa ---> ES 2603AB                                                        
                         STF 485Ab ---> STF 485AC                                                        
                         STF 485Ac ---> STF 485AD                                                        
                         STF 485AB ---> STF 485AE                                                        
                         STF 485BE ---> STF 485EF                                                        
                         STF 485   ---> STF 485EG (formerly STF 485B to STF 484A)                        
                         STF 484AB ---> STF 484GH                                                        
                         STF 484AC ---> STF 484GI                                                        
                         STF 485Bb ---> STF 485EC                                                        
                         HLM   3AF ---> STF 485AD                                                        
                         STF 485AD ---> STF 485AO                                                        
                         STF 485   ---> STF 485AL (formerly STF 485A to HLM   3A)                        
                         HLM   3AB ---> HLM   3LM                                                        
                         HZG   2AC ---> STF 484AI                                                        
                         HZG   2AD ---> STF 484AG                                                        
                         HZG   2AE ---> STF 484AH                                                        
                         HZG   2AG ---> HZG   2AN                                                        
                         HZG   2BC ---> STF 484EI                                                        
                         HZG   2BE ---> STF 484EH                                                        
                         HZG   2CD ---> STF 484GI                                                        
                         HZG   2CE ---> STF 484HI                                                        
                         HZG   2JK ---> HZG   2OP                                                        
                         HZG   2   ---> HZG   2JK                                                        
                         SLV   3   ---> STF 485AF                                                        
                         CHR 209Ba ---> CHR 209Ea,Eb                                                     
             CHR 209     Ea,Eb: The primary of this pair is the Beta Lyrae-type O9/B0 eclipsing          
                         system SZ Cam, with a period of 2.698d. The Gorda et al. (2007) orbit   Grd2007a
                         is based on changes in the period of SZ Cam to determine P, omega, e,   Grd2007b
                         and T, and speckle measures to derive i, Omega, and a. They derive a            
                         distance of 1125 +/- 135 pc, which exceeds by 30% the 800pc distance            
                         to the open cluster NGC 1502; they conclude that SZ Cam is not a                
                         member of the cluster. The mass of the eclipsing pair (Ea) is 28.5              
                         +/- 0.5 Msun, that of the third body (Eb) 23.4 +/- 2.4 Msun.                    
                         Eb is also a close binary.                                                      
             STF 484     GH: STI 492.                                                                    
04079+1750   DAE  18     V1302 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04080+4311   AG  308     B is BD+42@897.                                                                 
04080+0119   HJ 2223     BAL 1262.                                                                       
04082+1957   DAE  19     V1196 Tau.                                                              Dae2015 
04083+1327   BPM  93     [PM2000]  156773 + [PM2000]  156823.                                    Gvr2010 
04087+2553   OCC 777     Griffin (2013) notes that the magnitude and parallax of this pair               
                         suggest a star of luminosity class III, rather than the published               
                         spectral type of G8II. He derived a spectroscopic orbit of P=2224.4             
                         +/- 2.3 days, e=0.477 +/- 0.009.                                        Grf2013g
04088+1126   LDS5188     LDS5508.                                                                        
04089+2911   BU 1232     Only elements P, T, and a in the Starikova (1980) orbit have been       Sta1980b
                         amended from the orbit of Muller (1978).                                Mlr1978a
                         Griffin et al. (1988) find this to be a SB but doubt its                Grf1988 
                         membership in the Hyades in spite of its inclusion by                   Sym1965 
                         Wayman et al. (1965).                                                   Msn1993a
                         Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
                         However, this is a Hyades non-member                                    Grf1988 
                                                                                                 Grf2013c
04089+2306   STF 494     H N  17.                                                                MEv2010 
04090-5153   HJ 3625     B is CPD-52@499.                                                                
04091+2901   KOH   3     Young member of Taurus-Auriga molecular cloud.                          Dae2015 
04091+2839   HO  326     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 9.61 +/- 4.45, 2.43, and 1.10 Msun, respectively.             Mlk2012 
04091-1624   SKF 950     GWP 556.                                                                Tob2012b
04092+2105   ALP  11     2MASSI J0409095+210439                                                          
                         Physical companionship of B component to this ultracool dwarf ruled             
                         out based on I-J color, using I-band photometry taken at WIYN in                
                         August 2002. C component seen as elongated; its physical companionship          
                         also ruled out.                                                         AlP2007 
04093+1835   LDS1154     NLTT 12637/12636                                                        Chm2004 
04093-0756   A   469     Only elements P and T in the Starikova (1984) orbit have been amended   Sta1984 
                         from the orbit of Baize (1981).                                         Baz1981b
                         Typographical error in semimajor axis for Brendley & Mason (2007)       USN2007b
                         orbit corrected from 2".435 to 0".2986.                                         
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 8.49 +/- 6.33, 3.80, and 2.09 Msun, respectively.             Mlk2012 
04094+2328   POU 412     LDS5509.                                                                        
04094+0546   LAW  12     LSPM J0409+0546 = NLTT 12648. Law et al (2008) derive a distance of     Law2008 
                         19.9 +9.1/-3.8 pc and a projected separation of 4.9 +2.7/-0.7 au.               
                         Estimated spectral types are M4.5 and secondary later than M6.                  
04094-0125   BAL 290     J  3334.                                                                Nsn2016 
04095-0742   BRT 533     Not found by Heintz at IDS position.                                    Hei1990b
04095-1729   ENG  17     B is BD-17@806.                                                                 
04096+3139   HO  327     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         SEI  36.                                                                Nsn2017a
                         AB: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
04096-6023   R    41     B is CPD-60@297.                                                                
04096-8151   RST2345     A semi-regular variable, U Men. Hipparcos suspected non-single.                 
04097+1154   BPM  94     [PM2000]  157774 + [PM2000]  157781.                                    Gvr2010 
04097+0006   GRV 207     HJL  56.                                                                HJL1986 
04099+2446   ITO  16     V1306 Tau. Young member of Taurus-Auriga molecular cloud.               Dae2015 
04100+8042   STF 460     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 7.24 +/- 2.42, 5.27, and 4.54 Msun, respectively.             Mlk2012 
04100+0944   LDS1155     LIT  10.                                                                        
04102-0217   FIL  10     BAL  27.                                                                        
04105+5751   HDS 529     Pair originally X coded due to lack of resolution, however, elsewhere   Msn1999b
                         it is noted as a "very close double" so uncertain. Ambiguity from old   MCK1956 
                         reference recently found.                                               Dam2015a
04107+3808   WNT   2     IRAS 04073+3800 = Parsamian 13. Weintraub (1992) suggests that both     Wnt1992 
                         the northern and southern components are double, with separations of            
                         about 5" and 8", respectively.                                                  
04107-0452   A  2801     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.83 +/- 0.33, 2.34, and 1.05 Msun, respectively.             Mlk2012 
                         Docobo et al. (2017) derive an orbital parallax of 16.18 +/- 0.23 mas           
                         and component masses 1.203 +/- 0.059 and 1.114 +/- 0.054 Msun. Age of           
                         of the system is estimated at 5 Gyr.                                    Doc2017d
04108-1252   PHB   1     LP 714-37                                                                       
                         Phan-Bao et al. (2005) derive distance 18.1 +/- 2.2 pc, spectral types  PhB2005 
                         M5.5 and M7.5, masses 0.11 +/- 0.01 and 0.09 +/- 0.005 Msun.                    
                         Phan-Bao et al. (2006) derive spectral types, absolute K-band mags,     PhB2006 
                         masses of components as follows:                                                
                         A   M5.5 +/- 0.5    9.11 +/- 0.25   0.11 +/- 0.01 Msun                          
                         B   M8.0 +/- 0.5   10.05 +/- 0.30   0.09 +/- 0.01 Msun                          
                         C   M8.5 +/- 0.5   10.35 +/- 0.30   0.08 +/- 0.01 Msun                          
04111-1826   UPT   1     No change in angle; distance decreased 2" in 70 years.                  B__1951a
04112+2630   STF 502     LDS5514 (both AB and BC).                                                       
04112+1538   CHR 202     First detected as an occultation binary by Radick & Lien.               Rad1982a
04113+0531   ENG  18     45 Tau.  Hyades vB 14.  CPM companion with rho = 124".1 is outside              
                         detection window. An additional component was noted as spectroscopic    Grf1988 
                         by Griffin et al. (1988).                                               Msn1993a
04119+2338   CHR  14     Observed under poor seeing conditions. Griffin & Gunn (1981) found a    Grf1981d
                         2.4-day SB.                                                             Msn1993a
04120-0916   A   471     Motion increasing, but only three measures since 1933.                          
04123+6908   HJ 1141     A 13.3 magnitude star is 20" preceding.                                         
04125+3538   HJ  341     ALI 59. BU gives 1880 position +35 25.                                          
04125-3609   HJ 3628     B is CD-36@1632.                                                                
04128+1937   KOH   4     V1307 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04130+5237   PRV   1     GJ 164. Discovered by Palomar 5m/STEPS astrometry and confirmed                 
                         using HST/NICMOS, the combined solution by Pravdo et al. (2004)                 
                         yielded an absolute parallax of 0".0820 +/- 0".008, spectral types of           
                         M4.5V and M6-8V and masses 0.170 +/- 0.015 and 0.095 +/- 0.015 Msun.            
                         Inclination = 57 +13/-17, omega = 133 +45/-20 deg.                      Prv2004 
                         Combined AO+STEPS analysis of this M dwarf binary yields a total mass           
                         0.343 +/- 0.026 Msun, individual masses 0.257 +/- 0.020 and 0.086 +/-           
                         0.007 Msun. Metallicity is at least solar.                              Mtc2009 
                         Inclination = 57 +13/-17, omega = 133 +45/-20 deg.                              
                         GJ 164 = LHS 1642. A known close binary system with a well-determined           
                         orbit (Pravdo et al. 2004; Martinache et al. 2009). Its separation is   Prv2004 
                         smaller than 100 mas at all times, and it therefore remains unresolved  Mtc2009 
                         by AstraLux. We do detect one other point source in the field of view,          
                         but it is a suspected background contaminant based on its blue color,           
                         with dz'= 5.8 +/- 0.1 mag and di' = 5.3 +/- 0.1 mag.                    Jnn2014 
04130-2832   HWE  10     Rectilinear solution by Hartkopf et al.  (2012).                        Hrt2012a
04132+5032   CHR  15     Ross 29.  Van Maanen (1941) suspected this star to be a binary, but     Maa1941 
                         these are the first measurements of a companion.                        McA1987b
04132+2258   HU  302     A premature orbit has been computed.                                            
04135+2816   KSA 102     Primary is variable star V1096 Tau.                                             
04135+1813   BPM  95     [PM2000]  160209 + [PM2000]  160214.                                    Gvr2010 
04135-2554   LDS3564     NLTT 12805/12807                                                        Chm2004 
04136+0743   A  1938     46 Tau. Hipparcos astrometric solution adopted some elements from the   HIP1997d
                         orbit of Heintz.                                                        Hei1984b
                         Combined spectroscopic/astrometric solution of SB1. Calculated masses           
                         1.38 +/- 0.26 and 0.82 +/- 0.21 Msun.                                   Mut2010b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.17 +/- 0.14, 2.77, and 2.55 Msun, respectively.             Mlk2012 
04139+0916   BU  547     47 Tau.                                                                         
                         Spectral types of primary and secondary assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
04140+8216   LUH   7     LHS 1643 + WISE J041328.73+821854.7. Companion is likely not physical,          
                         based on proper motion.                                                 Luh2012b
04140-1222   GAL 364     Object #120 in Gallo's original list.                                   Gal1914 
04141-3155   TS    1     The triply eclipsing TESS multiple TIC 168789840. Pair A has a period   TS_2021 
                         of 1.570d and masses of 1.25 +/- 0.05 and 0.56 +/- 0.04 \msun. Pair B           
                         has a period of 1.306d and masses of 1.30 +/- 0.08 and 0.66 +/- 0.03            
                         \msun. Pair C has a period of 8.217d and masses of 1.23 +/- 0.10 and            
                         0.59 +/- 0.07 \msun. The estimated period of AC is 3.7y and AC,B of 2           
                         kyr.                                                                            
04142+5149   HU  212AC   Also known as SCA 183.                                                  Sca2018b
04142+2813   GHE   1     Aa,Ab: V773 Tau.  Orbital elements and dynamical mass determinations            
                         were published by Tamazian et al. (2002).                               Tam2002 
                         Aa,Ab: The combined solution by Boden et al. (2012) yields a mass and   Bod2012 
                         luminosity for the Ab component of 2.35 +/- 0.67 Msun and 2.6 +/- 0.6           
                         Lsun. This mass is higher than expected, and suggests the Aa,Ab pair            
                         may instead be a multiple system.                                               
                         Young member of Taurus-Auriga molecular cloud.                          Dae2015 
04142-4608   RST2338     Half-period solution equally good, but gives large mass-sum.                    
                         More speckle obs needed (the only existing one erroneous?).                     
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.72 +/- 0.26, 2.26, and 1.07 Msun, respectively.             Mlk2012 
                         Gomez et al. (2016) derive dynamical parallax and component masses:             
                         20.75 +/- 0.42 mas, 1.245 +/- 0.012 Msun, 0.954 +/- 0.009 Msun.         Doc2016i
04143-2742   SWR   7     CPM pair                                                                Skf2004 
04144+1523   BPM  96     [PM2000]  160726 + [PM2000]  160650.                                    Gvr2010 
04144-1015   STF 516     39 Eri.                                                                         
                         AB: H N  24.                                                            MEv2010 
04144-6228   HJ 3638     alp Ret. Possible spectroscopic binary.                                         
04145+2851   GRV 208     2MASS J04143060+2851298 and J04143109+2851518, both from the Riaz et            
                         al (2006) sample, are separated by only 23" and although the estimated  Ria2006 
                         spectroscopic distances of 55 and 72 pc are not fully equal, they are           
                         consistent to within the 37% error. In addition, they have very                 
                         similar proper motions (e.g. Roser et al. 2010) and thus probably form  XXX2010 
                         a physical pair.                                                        Jnn2012 
04148+2813   GHE   2     FO Tau.  Orbital elements and dynamical mass determinations were                
                         published by Tamazian et al. (2002).                                    Tam2002 
                         M_Aa = 0.35 +0.06-0.05 \msun, M_Ab = 0.34 +/- 0.05 \msun.               Tof2024 
04148+2753   GHE   3     HBC 368 = V1098 Tau = LkCa 3. Torres et al. (2013) find that both               
                         components of this 0".5 pre-MS pair are spectroscopic binaries, with            
                         periods for Aa,Ab and Ba,Bb of 12.942 and 4.068d, respectively.         Trr2013 
04148+2648   DAE  21     CX Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
04148+2646   DAE  20     FP Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
04148-6212   HJ 3641     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2013).                         USN2013a
04149+5824   LDS9165     Old LDS6165.                                                                    
04149+4825   STT  73     mu Per = 51 Per. A is a Beta Lyrae-type system.                                 
                         The elements P, T, and e of Alden (1925) were adopted from the          Ald1925 
                         spectroscopic orbit of Cannon (Pub. DAO Ottawa 2, 365, 1915).                   
             H 6  20     H VI 20. SHJ 364.                                                               
04152+5052   AG  309     B is BD+50@944.                                                                 
04153+2044   KOH   6     Metchev & Hillenbrand say the pair is probably physical, based on               
                         proximity.                                                              Met2004b
                         V1199 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04153-0739   STF 518     A: omi 2 Eri = 40 Eri = Keid                                                    
                         LDS 114 = STFB 1. Proper motion of A -2224 -3423.                               
                         C is a flare star, DY Eri, and a strong X-ray source.                           
                         AE: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         BC: NLTT 12868/12869                                                    Chm2004 
                         BC at 83" is physical, and is a Delta Scuti star showing coronal X-ray          
                         emission.                                                                       
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         HIP 19849. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         BC: Additional notes may be found in Worley (1956).                     Wor1956b
                         B: M = 0.575 +/- 0.018 \msun, C: M = 0.2041 +/- 0.0064.                 Msn2017d
                         P = 230.09 +/- 0.68 y.                                                          
                         VLTI uniform disk diameter of A:       1.405 +/- 0.038 mas,             LTI2009 
                         VLTI limb-darkened disk diameter of A: 1.437 +/- 0.039 mas,                     
                         R = 0.770 +/- 0.021 \rsun, Teff = 5269 +/-  35 K,                               
                         M = 0.877 +/- 0.044 \msun.                                                      
                         CHARA Array Limb-darkened diameter of A :                               CIA2012f
                         R =  0.8061 +/- 0.0036 \rsun, L =  0.40782 +/-0.00319 \lsun,                    
                         Teff = 5143 +/-  14 K, M = 0.816 \msun.                                         
                         B: Teff = 17,200 +/- 110 K, log g = 7.957 +/- 0.020, R = 0.01308 +/-    BdH2017b
                         0.00020 \rsun, M = 0.565 +/- 0.031 \msun, l = 0.01349 +/- 0.00054               
                         \lsun. Inferred cooling age 122 Myr. Assuming a pre-WD progenitor of            
                         1.8 \msun with a lifetime of 1.7 Gyr gives a total system age of ~1.8           
                         Gyr. It has a thin outer hydrogen layer.                                        
                         AD, AE: Rectilinear solutions by Friedman et al. (2011).                USN2011a
                         BD, BE: Rectilinear solutions by Mason & Hartkopf (2016).               Msn2016a
04155+0611   STTA 45     AB: H VI 98. A is V774 Tau. B is BD+05@613, and a suspected variable.           
                         AB: SHY  21. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AB: H 6  98.                                                            MEv2010 
                         Toyota et al. (2009) monitored the RV of both the A and B components            
                         every 1-2 months between 2003 Mar - 2007 Nov, using a high-dispersion           
                         echelle (precision ~10 m/s). Standard deviations of the RVs of both             
                         components are <40 m/s and velocities show no periodic variation.               
                         These results rejects the association of a planet of mass > 1.8 Mjup            
                         with either star.                                                       Toy2009 
04157+2049   CIA  62     Aa,Ab : M_Aa = 1.0714+/- 0.0038\msun, M_Ab = 0.9682 +/- 0.0031 \msun,           
                         pi_orb = 20.411 +/- 0.026 mas, A_dia = 0.186 mas, B_dia = 0.163 mas.    CIA2024d
             TOK 659     Hyades, vB162.  primary is SB2, P=55.130d                               Tok2014d
                         The 55.1-day SB of Griffin & Gunn (1981) is outside our detection       Grf1981d
                         window.                                                                 Msn1993a
             RED   2     1996.1230: RHy ID and coordinates from Reid (1992).                     Red1992 
                         LP ID from Luyten et al. (1981).                                        Luy1981 
                         Candidate Hyades member; Reid considers definite binary.                Red1997 
04158+4524   STF 512     HJL  58.                                                                HJL1986 
04158+3100   KOH   7     V952 Per. Member of Taurus-Auriga molecular cloud.                      Dae2015 
04158+1524   BUP  51     A: 48 Tau = V1099 Tau                                                           
04159+3142   STT  77     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 4.90 +/- 3.64, 2.97, and 1.10 Msun, respectively.  Mlk2012 
             STTA 43     AB,C: HJL  59.                                                          HJL1986 
04162+1648   RED   3     1995.8821: RHy ID and coordinates from Reid (1992).                     Red1992 
                         LP ID from Luyten et al. (1981).                                        Luy1981 
                         Candidate Hyades member; Reid considers possible binary.                Red1997 
04163+3644   YSC 128     Also a 7.3d spectroscopic binary.                                       Tok2019b
04163+0710   WSI 97      This is a single-lined nearby binary. Using the radial velocities               
                         measured by D. Latham (2012, private communication), we computed a              
                         combined orbit (the previous visual orbit reported by Riddle et al.     RAO2015 
                         (2015) had a wrong period). The inclination is close to 180deg and had          
                         to be fixed in order to match the RV amplitude.                         Tok2015c
04163-6057   GLE   1     Variable: TT Ret. A premature orbit has been computed.                          
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
04164+0710   WSI  97     Provisionally designated WSI9102.                                       Tok2010 
04165+0041   J  1458     BAL 971.                                                                        
04165-5918   JSP  56     eps Ret                                                                         
                         The companion is a possible white dwarf.                                Cvn2006 
                         Companion confirmed as DA white dwarf.                                  Cvn2007 
                         Optical spectroscopy suggests the companion is a mid- to late-B                 
                         (B3-B9) dwarf.                                                          Mug2007b
04166+2447   LDS1158     NLTT 12896/12897                                                        Chm2004 
04170+1941   HO  328     Only elements P and T in the Starikova (1980) orbit were amended from   Sta1980b
                         the orbit of Heintz (1978).                                             Hei1978a
                         Additional notes may be found in Van Biesbroeck (1954) and              VBs1954 
                         Couteau (1963).                                                         Cou1963a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 6.92 +/- 2.37, 2.74, and 1.20 Msun, respectively.             Mlk2012 
04171+6408   STF 503     BD is +63  489a.                                                                
04171+0409   BAL2119     J 1814.                                                                         
04173+4613   STTA 44     B is BD+45@904.                                                                 
04173+2035   LDS5535     HJL1032.                                                                HJL1986 
04176+2833   SAR   2     HBC 371 = LkCa 5.                                                               
04176+1658   LDS3568     This cannot be the close 3079-d or 5.609-d spectroscopic binaries of    Grf2012b
                         Griffin. The 3079-d pair has an estimated separation of 0.06", but              
                         delta-mag may be considerable.                                                  
04176+1657   HD  27130   Hyades vB 22.  The 5.6-day SB of Griffin et al. (1985) is outside our   Grf1985b
                         detection window.                                                       Msn1993a
04177-6315   RMK   3     the Ret                                                                         
                         Rectilinear solution by Letchford et al. (2018).                        LRR2018a
04179+5847   STF 511     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.60 +/- 1.54, 3.37, and 2.09 Msun, respectively.             Mlk2012 
04179-3348   I   270     ups 4 Eri = 41 Eri. Duplicity of AB doubtful.                                   
                         A is a spectroscopic binary, and possible variable.                             
             HMM   2     Aa1,Aa2: close SB resolved by VLTI. A combined spectroscopic/                   
                         interferometric orbit by Hummel et al. (2017) yields component masses           
                         3.17 +/- 0.07 and 3.07 +/- 0.07 Msun, luminosities 100.6 +/- 4.3 and            
                         87.4 +/- 3.3 Lsun, and an orbital parallax of 18.05 +/- 0.17 mas.       Hmm2017 
04180+1815   CIA  63     V1232 Tau.                                                                      
                         M_A = 1.1028 +/- 0.0011 \msun, M_B = 1.01736 +/- 0.00091 \msun,                 
                         pi_orb = 21.4783 +/- 0.0078 mas, A_dia = 0.199 mas, B_dia = 0.179 mas.  CIA2024d
                         Hyades vB 23. The 75.6-day SB of Batten & Wallerstein (1973) is         Bte1973 
                         outside our detection window.                                           Msn1993a
04180-0031   SKF 848     Pair originally published as BVD 45, but with incorrect sign given to   Bvd2010b
                         declination. Pair later "rediscovered" and published with correct               
                         declination; this latter discoverer designation has been maintained.            
04181+0446   TOB9003     Measured as BAZ   3 = STF1063 but with an error of -3h in RA!           Tob2012c
04181-1448   LDS9166     Old LDS6166.                                                                    
                         NLTT 12975/12973                                                        Chm2004 
04182+5018   b Per       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Hill et al. (1976).                                                     HlG1976 
04182+2248   STF 520     Measured separation too large, estimated at probably 0.30".             Cou1955c
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 14.33 +/- 9.16, 3.42, and 1.20 Msun, respectively.            Mlk2012 
04183-3000   LDS3571     NLTT 12992/12990                                                        Chm2004 
04184+2135   MCA  14     51 Tau. Hyad (vB 24). B is BD+21@619. A is a long-period spectroscopic          
                         binary, resolved by speckle interferometry. Analysis of the                     
                         spectroscopic/interferometric orbit is given by McAlister (1977).       McA1977 
                         1978.1490:  Theta was incorrectly given as 325.5 degrees                McA1980b
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         A new orbit with a period of 11.3 years was determined by Dombrowski    Dmb1991 
                         (1991).                                                                 Msn1993a
                         Torres et al. (1997) derive a combined spectroscopic/astrometric        Trr1997a
                         solution, yielding an orbital parallax 0.01792 /- 0.00058 and masses            
                         1.80 +/= 0.13 and 1.46 +/- 0.18 Msun.                                           
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Deutsch & Lowen (1971).                                                 Deu1971 
                         Aa,Ab: Martin et al. (1998) derive component masses 1.756 +/- 0.343             
                         and 0.953 +/- 0.247 Msun.                                               Mig1998 
                         Pourbaix (2000) gives a combined solution for this resolved SB2,        Pbx2000b
                         yielding orbital parallaxes and component masses.                               
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 2.96 +/- 0.47, 2.99, and 1.45 Msun, respectively.  Mlk2012 
04184-2347   RST2344     BRT2832.                                                                Brt1947 
04185+2828   GHE   4     Aka V410 Tau.                                                                   
04185+2817   HAT   4     AB: Additional notes may be found in Herbig (1962).                     Her1962 
04186+1606   BPM  97     [PM2000]  163490 + [PM2000]  163456.                                    Gvr2010 
04187+2819   SKW   2     V892 Tau.                                                                       
                         Circumbinary disk approximately five times larger than the binary               
                         separation.                                                             Mnr2008 
                         Total mass estimated to be 6.0 +/- 0.2 \msun. Orbit is nearly coplanar          
                         with circumbinary disk. Mild inner and outer disk misalignment may be           
                         due to interaction with the eccentric binary.                           Lon2021 
04187+2819   SKN   1     Measure of 1990.725 made by the VLA at radio wavelengths.               Skn1993 
04187-5252   SHY 462     AB: HIP  20109 + HIP  20074.                                                    
04188+2820   KSA 104     Primary is variable star V1023 Tau.                                             
04189+0146   STTA 49     B is BD+01@734.                                                                 
04190-0725   STF 527     H 2  80.                                                                MEv2010 
04192+6135   STF 513     Same as STF 507.                                                                
04192+1100   BPM  98     [PM2000]  163846 + [PM2000]  163809.                                    Gvr2010 
04193-4416   HJ 3643     B is CD-44@1505.                                                                
04195+3800   HDS 552     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.74 +/- 0.86, 2.77, and 1.45 Msun, respectively.             Mlk2012 
04195+2808   DAE  23     Member of Taurus-Auriga molecular cloud.                                Dae2015 
04196+3355   HJ  674     The discovery observation of 220 deg may be in error. The AC2000                
                         catalog include one measurement for 1924.381: 22.3 deg and 16.1".               
                         Proper motion of B is mu(AR) = +0.004+-0.007, mu(DEC) = -0.022+-0.002   FMR2000b
04196-2847   SHY 463     HIP  20184 + HIP  19926.                                                        
04197+1416   GIC  45     G008-027/G008-026 = Melotte 25 VA 174 + 170.                                    
04198+1538   BLM   1     gam Tau = 54 Tau = Prima Hyadum. SB resolved by speckle interferometry.         
                         This object was misidentified as HR 1349 by McAlister (1978).           McA1978c
                         Observed under rather poor seeing conditions. Morgan et al. (1982)      BLM1982 
                         also report a large magnitude difference.                               Msn1993a
04199+3145   J   934     Jonckheere gives the 1950 position: 04 17.0 +31 43.                     J__1958 
                         Couteau corrects the position.                                          Cou1953a
04199+1631   STT  79     Hyad (vB 29). SB according to Griffin et al. (1988).                    Grf1988 
                         1978.6183: The date of this observation was given incorrectly as                
                         1977.6183 by McAlister & Fekel (1980).                                  McA1980b
                         Observed under poor seeing conditions.                                  Msn1993a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.57 +/- 1.41, 2.25, and 1.07 Msun, respectively.             Mlk2012 
04200+1402   BUP  53     57 Tau. A is a Delta Scuti-type variable, V483 Tau.                             
04201+1953   LDS1164     LDS9167 (old LDS6167).  NLTT 13024 = LP 414-169                         Chm2004 
                         NLTT 13024/13026                                                        Chm2004 
04202+3336   FAR   4     Primary is white dwarf WD 0416+334 = GD 60. Aka SKF 316.                Far2005b
04203+3150   HJ 5460     SEI  40.                                                                Nsn2017a
04203+1833   LDS5540     Companion at 264" agrees with Luyten's astrometry, but star at 307" is  Luy1984 
                         in much better magnitude and proper motion agreement. This pair added           
                         as AC pair, until proper identification can be determined.                      
04204+3434   BU 1382     54 Per.                                                                         
04204+2721   SHJ  40     phi Tau = 52 Tau. STTA 48 = H 5  13. B is BD+26@712.                            
04205-0119   RST4769     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.54 +/- 0.98, 3.17, and 2.00 Msun, respectively.             Mlk2012 
04206+2429   COU 704     Probably the A component of POU 442.                                            
04207+1514   JNN 261     LP 475-7. Estimated age 1000-10000 Myr; masses 0.45 +/- 0.04 and 0.21           
                         +/- 0.03 Msun; a ~7.4 au.                                               Jnn2014 
04208+3009   KOH   8     Member of Taurus-Auriga molecular cloud.                                Dae2015 
04209+1352   CIA  60     Hyad - Melotte 25 VA 201 = vB 34.                                               
                         Aa,Ab : M_Aa = 1.363 +/- 0.010 \msun, M_Ab = 1.3323 +/- 0.0099 \msun,           
                         pi_orb = 21.174 +/- 0.073 mas, A_dia = 0.265 mas, B_dia = 0.257 mas.    CIA2024d
                         The combined spectroscopic/interferometric solution by Konacki et al.   Knc2004 
                         (2004) uses data from the Palomar Testbed Interferometer and assumes            
                         the eccentricity = 0.0 and the K-band brightness ratio = 1.0. Results           
                         include P = 3.0591080 +/- 0.000011 d, T = 44497.185696 +/- 0.0026 MJD,          
                         derived masses 1.38 +/- 0.13 and 1.39 +/- 0.13 Msun, spectral types             
                         F6V, and diameters 0.25 mas.                                                    
                         Aa,Ab is resolved with PTI, orbit (Konacki & Lane 2004). The B          Knc2004 
                         component is a white dwarf (Barstow et al. 2001), DA3.1; mass 0.98      Bas2001 
                         Msun.  Shaya & Olling (2011): co-moving HIP 1996 at 0.75pc, prob.       Shy2011 
                         0.96: another Hyades star?                                              Tok2014d
             HD  27483   Mel 25 VA 201: Malkov et al. (2012) derive dynamical, photometric, and          
                         spectroscopic masses 3.04 +/- 6.10, 2.70, and 3.17 Msun, respectively.  Mlk2012 
04209-1156   GAL 365     Object #125 in Gallo's original list.                                   Gal1914 
04210+5015   S   445     STTA 47. B is BD+49@1161.                                                       
04211+5532   STTA 46     B is BD+55@869.                                                                 
04215+1704   BPM  99     [PM2000]  165579 + [PM2000]  165489.                                    Gvr2010 
04215-2055   LDS9168     Old LDS6168.                                                                    
                         AC: NLTT 13102/13095                                                    Chm2004 
                         AC: SHY 167. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
04215-2544   BU  744     Star A is SB1, P = 4.0 d, tho this may be spurious,                     Wor1983 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.42 +/- 1.00, 2.96, and 1.35 Msun, respectively.  Mlk2012 
04216-1559   LDS9169     Old LDS6169.                                                                    
                         NLTT 13109/13110                                                        Chm2004 
04217+1046   TOK  84     HIP 20366. Small PM(A)=(-31,-12). NOMAD: PM(B)=(+39,-63), V=13.95.      Tok2011a
04218+1949   KNT   2     LDS2228. The variable U Tau.                                                    
04218+1929   SIG   1     LP 415-20 = Bryja 262.  Spectral types M7.0, M9.5. Probable Hyades              
                         member. Estimated orbital period 23 +7/-6 yrs.                          Sig2003 
                         Konopacky et al. (2010) derive a distance of 21. +/- 5. pc and a                
                         system mass of 0.09 +/- 0.06 Msun.                                      Kon2010 
04219+5749   BRG  34     XO-3. Bergfors et al. (2013) estimate spectral types F5V and G0-M2.5V.  Brg2013 
04219+1530   CHX   1     IRAM 04191+1522. Primary is a Class 0 protostar, resolved into 7.8"             
                         pair in 1.3mm continuum observations at Submillimeter Array (SMA).      ChX2012 
                         Chen et al. quote position angle as "SE/NW"; followup check on Aladin           
                         by cataloguer suggests angle approximately 290deg.                              
04220+2826   ISM   1     RY Tau, a T-Tauri star.                                                         
04220+2818   ITO  21     V987 Tau. Member of Taurus-Auriga molecular cloud.                      Dae2015 
04220+2658   SMN   9     FS Tau.                                                                         
                         Measure of 1989.5 made by triangulation of multiple measures and was            
                         in a red filter.                                                                
                         Tamazian et al. (2002) solution includes a mass determination based on  Tam2002 
                         an estimated distance.                                                          
                         AB: Additional notes may be found in Simon et al. (1992).               Smn1992 
04220+1932   GHE   6     Components A, Ba, and Bb of this system are also commonly designated            
                         as N, Sa, and Sb, respectively, due to the north-south orientation of           
                         the wider pair.                                                                 
                         AB: Measure of 1982.5 made by the VLA at radio wavelengths.             Scw1984 
                         Measure of 1983.75 made by the VLA at radio wavelengths.                Scw1986 
                         Measures of Johnston et al. and Loinard et al. made by the VLA at       Jnt2003 
                         radio wavelengths.                                                      Loi2003 
                         AB: Rho and theta errors for Ghez et al. (1995), Furlan et al. (2003),  Ghe1995 
                         and Roddier et al. (2000) measures have been added/updated as noted by  Fun2003 
                         Koehler et al. (2008). Koehler et al. derive a preliminary orbit for    Rod2000 
                         the AB pair, yielding a system mass of 5.57 +0.11/-0.29 Msun.           Koh2008b
                         A,Ba: The 2000.886 Duchene et al. (2002) theta value was corrected by   Dch2002 
                         Duchene et al (2006). Also, the Duchene et al. (2006) theta value for   Dch2006 
                         2005.801 was changed by 90deg to correct for the orientation of the             
                         camera (Schaefer, priv. comm. cited by Koehler et al. 2008)             Koh2008b
             KRS   2     Ba,Bb: Tamazian derives a total system mass of 2.82 +/- 0.74 Msun,      Tam2005 
                         consistent with the IRC model of Koresko et al. (1997).                 Krs1997 
                         T Tau Sa-Sb orbit gives range 1991-2001 for T, 0.09-0.87 for e,                 
                         11-60 for i. Values for P and a are lower limits.                       Sfr2006 
                         Duchene et al. (2006) derive masses for the Ba and Bb components of     Dch2006 
                         2.73 +/- 0.31 and 0.61 +/- 0.17 Msun, respectively.                             
                         Ba,Bb: The 2000.886 Duchene et al. (2002) theta value was corrected by  Dch2002 
                         Duchene et al (2006)                                                    Dch2006 
                         The 2002.829 Schaefer et al. (2006) measure is a reanalysis of data     Sfr2006 
                         from Beck et al. (2004).                                                Bck2004 
                         Koehler et al. (2008) derive a system mass of 2.96 +0.15/-0.24 Msun     Koh2008b
                         and individual masses of 2.13 +0.14/-0.20 and 0.83 +0.10/-0.11 Msun             
                         for the Ba and Bb components, respectively.                                     
                         Ba,Bb: The Schaefer et al. (2014) orbit, combined with a VLBA parallax          
                         of 6.90 +/- 0.09 mas (147.6 +/- 0.6pc; Loinard et al. 2007, ApJ 671,            
                         546) yields a total mass for Ba+Bb of 2.70 +/- 0.22 Msun.               Sfr2014 
                         Ba,Bb: Csepany et al. (2015) generated new orbital parameters for T             
                         Tau N-S (KRS   2Ba,Bb), but their grid search yields a wide range of            
                         possible solutions (P 475-27000y, a 0.57-16.8", etc.)                   Cse2015b
                         Based on the new orbit and the Gaia parallax the masses of Ba(Bb) is    Sfr2020 
                         is 2.049(0.430) +/- 0.137(0.055) \msun. Using the slightly grater               
                         distance from the VLBA parallax the result is 2.268(0.476) +/-                  
                         0.147(0.060) \msun. The brightnesa of Ba and Bb are both variable.              
04220+1405   HD  27628   Hyades vB 38 = V775 Tau. The 2.14-day SB of Abt (1961) is outside our   AbH1961 
                         detection window.                                                       Msn1993a
             BUP  54     60 Tau. A is a specroscopic binary and variable, V775 Tau.                      
04221+2826   KSA 105     V1071 Tau = LkCa 21. Young member of Taurus-Auriga molecular cloud.     Dae2015 
04221-2849   BWL  15     Pair is a 0".7 equal-flux K7V2 binary. Torres et al. (2006 A&A 460,             
                         695) found strong Halpha emission and lithium absorption. Age is                
                         consistent with that of the Pleiades, so an age range of 50-200 Myr             
                         is adopted for this system.                                             Bwl2015 
04221+1934   KOH   9     Young member of Taurus-Auriga molecular cloud.                          Dae2015 
04224+1118   PAT   5     The 3-year SB of Griffin et al. (1988) is outside our detection         Grf1988 
                         window.                                                                 Msn1993a
                         The double-lined spectroscopic solution of this 1043.5-d pair           Grf2012b
                         determined by Griffin.                                                          
04226+2538   STF 528     chi Tau = 59 Tau                                                                
                         H 4  10.                                                                MEv2010 
                         The secondary is SB2 (F8+G6), with period 17.6 days for Ba,Bb; RV               
                         residuals indicate the presence of a more distant Bc companion. Based           
                         on spectroscopic observations obtained at CfA 1988-2004, Torres (2006)          
                         derived an orbit for Bab,Bc with period 9.447 +/- 0.017 yr. Mass for            
                         the A component is determined to be 2.60 +/- 0.5 Msun. Inclination              
                         angle for the Ba,Bb orbit is 53.5 +/- 0.5deg, yielding masses 1.19 and          
                         1.02 Msun for Ba and Bb. Bc appears to be over-massive; based on                
                         infrared excess this could be well explained as an equal-mass binary            
                         composed of late-type stars of masses ~0.70 Msun (spectral type ~K4).           
                         Total mass of B is 3.6 Msun.  Torres estimates the Bab,Bc semi-major            
                         axis at about 83.6 mas and the magnitude difference dV~3.3mag                   
                         (dK~1.5mag), making the pair potentially resolvable by speckle                  
                         interferometry.                                                         Trr2006b
04227+1503   STT  82     Hyades vB 40A. The primary is SB1, P = 4.00 d (Sanford 1921).           San1921 
                         Primary is SB2, P=4.0002d (Griffin 2012)                                Grf2012b
                         Also a wider companion (LDS 1166 AC, rho = 62", M = 17.8).                      
                         The 255.5-year binary, ADS 3169 = STT 82 AB is outside our detection            
                         window, although part of a peak is seen at the edge of the window at            
                         the expected position angle, according to the orbit in the Worley &             
                         Heintz (1983) orbit catalog. A wider companion (LDS 1166AC, rho = 62",  Wor1983 
                         M = 17.8) and the 4d SB are also outside our detection window.          Msn1993a
                         A component of pair determined to be a 4.0-d spectroscopic binary.      Grf2012b
04228+1647   HD  27685   Hyades vB 39. Spectroscopic binary with P > 7 yr, according to Griffin  Grf1988 
                         et al. (1988).                                                          Msn1993a
04230+1732   CHR 262     del 1 Tau = 61 Tau = Secunda Hyadum. The primary is a long-period               
             BUP  55     spectroscopic and occultation binary.                                           
                         Mk III Limb-darkened diameter  2.338 +/- 0.033 mas.                     MkT2003 
                         CHARA Array Limb-darkened diameter  2.408 +/- 0.038 mas.                CIA2009a
                         R =  12.3 +/- 0.4 \rsun, Teff = 4826 +/- 51 K.                                  
                         This system, first announced in Mason et al. but considered of          Msn1993a
                         uncertain veracity, has been included. While its status is not                  
                         definitive, subsequent confirmation or suspected duplicity (by another          
                         technique) makes the discovery measurement somewhat more probable.              
                         1991.8995: This is a particularly unexpected result, given the four             
                         previous epochs at which our observations have shown no indications of          
                         duplicity.  All four of the earlier observations were reanalyzed using          
                         the same procedures employed here, but no additional supporting                 
                         evidence of duplicity was found.  If this additional component is               
                         confirmed,  vB 41 will be the second K0 giant binary that has been              
                         resolved in the Hyades (HR 1411 being the other).  The common proper            
                         motion companion at a separation of 195".5 is far outside our window            
                         of observation, and the 530-day spectroscopic component of Griffin &            
                         Gunn (1977) would have an angular separation below the diffraction      Grf1977d
                         limit of the KPNO 4-m telescope.                                        Msn1993a
                         Aa,Ab : If real, this pair could be the 530.1-d spectroscopic binary    Grf2012b
                         of Griffin.                                                                     
04231-0117   BU  402     Aka OL  201.                                                                    
04232+7510   MLR 459     Also known as TDS 138.                                                          
04232-1135   GAL 366     Object #127 in Gallo's original list.                                   Gal1914 
04233+1123   STF 535     A premature orbit has been computed.                                            
                         Ruymaekers & Nys (1995) noted discrepancies in the orbit of Popovic     Ruy1995 
                         (1982), and calculated elements from their Thiele-Innes elements.       Pop1982a
04233-0500   HJ  342     Same as STF 539 and H IV 117.                                                   
                         AB: H 4 117.                                                            MEv2010 
04233-2138   B  2571     CPD-21@545.                                                                     
04234+1940   V988 Tau    Hyades vB 43. Hipparcos astrometric solution adopted some elements      HIP1997d
                         from the orbit of Griffin et al. (1985).                                Grf1985b
                         The 1.6-year SB of Griffin et al. is outside our detection window.      Msn1993a
04234+1647   HD  27749   Hyades vB 45.  The 8.418-day SB of Abt & Levy (1985) is outside our     AbH1985 
                         detection window.                                                       Msn1993a
04234+1546   TOK 876     V989 Tau.                                                                       
04235+2059   CHR  16     An occultation binary, now resolved.                                            
04236+4226   STT  80     1977.7420: The date of this observation was given incorrectly as                
                         1978.7420 by McAlister & Fekel (1980).                                  McA1980b
04236+2503   MTZ   2     FU Tau                                                                          
04237+1538   MET   3     Metchev & Hillenbrand say the pair is probably optical, based on                
                         proximity.                                                              Met2004b
04238-0414   BUG   7     SDSS J042348.57-041403.5                                                        
                         Estimated spectral types are L6.5 + T2, effective temperatures 1490             
                         +/- 100 and 1250 +/- 80 K. Masses are estimated at 0.039-0.062 and              
                         0.029-0.051 Msun, and the orbital period (assuming the semi-major axis          
                         = 1.26 * rho) is ~19yr.                                                 Bug2006a
04239+0928   HU  304     66 Tau.                                                                         
                         Spectral types and masses of components assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.81 +/- 1.40, 6.11, and 4.43 Msun, respectively.             Mlk2012 
04239-1102   GAL 367     Object #128 in Gallo's original list.                                   Gal1914 
04240+2418   STF 534     62 Tau.                                                                         
                         AB: H 4 109.                                                            MEv2010 
04241+1727   BUP  56     del 2 Tau = 64 Tau. Hyades vB 47. A is spectroscopic binary.                    
04242+1445   HDS 564     1991.8992: Noted as a possible spectroscopic binary by Griffin et al.   Grf1988 
                         (1988), it is uncertain whether the system we detect here is also               
                         producing the radial velocity variation.                                Msn1993a
                         Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
                         The spectroscopic solution of this ~42000-d pair determined by Griffin, Grf2012b
                         its gamma velocity "removing any remaining doubt about the systems      Grf2013c
                         credentials as a Hyades member."                                                
04242-5704   RMK   4     Rectilinear solution by Letchford et al. (2018), however, common                
                         parallax and proper motion argues for their orbital solution.           LRR2018a
04244+3419   STF 533     AB: H 4  72.                                                            MEv2010 
                         Primary is V590 Per, a Beta Lyr type eclipsing binary, P = 5.6866d.     Zas2012 
04245+5051   TOK 245     AC: The physical nature of C is not certain: CPM, but the PM is small.  Tok2014d
             COU2459     AB: Rectilinear solution by Hartkopf & Mason (2013).                    Hrt2013b
04245+2244   BU 1235     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.22 +/- 2.00, 2.88, and 1.35 Msun, respectively.             Mlk2012 
04245+1653   PAT   6     Noted as a possible spectroscopic binary by Griffin et al.              Grf1988 
                         (1988).                                                                 Msn1993a
                         Hyades vB 52. Mass of B 0.49 Msun (Metchev & Hillenbrand 2009).         Met2009 
04246+3358   STT  81     AB: 56 Per.                                                                     
04247+0442   HJL1115     Hyades vB 140. The 156.4-day SB of Griffin et al. (1985) is outside     Grf1985b
                         our detection window.                                                   Msn1993a
                         A combined interferometric/spectroscopic solution by Halbwachs et al.           
                         (2016) yields masses 0.9808 +/- 0.0040 and 0.7269 +/- 0.0019 Msun.      HJL2016 
                         Mass = 0.9798 +/- 0.0019, 0.72697 +/- 0.00094 \msun for A and B.        HJL2020 
                         orbital parallax = 16.703 +/- 0.034 mas.                                        
04247-0845   STF 544     Primary is SB1, P=1248d = 3.41y. RV(B)=var?                             Tok2014d
04247+0442   HJL1115     A combined interferometric/spectroscopic solution by Halbwachs et al.           
                         (2016) yields masses 0.9808 +/- 0.0040 and 0.7269 +/- 0.0019 Msun.      HJL2016 
04248+1552   PAT   7     SB with P > 7 yr according to                                           Grf1988 
                         Griffin et al. (1988).                                                  Msn1993a
                         The spectroscopic solution of this 5688-d pair determined by Griffin.   Grf2012b
04248-5037   RST1273     HIP 20606. Both components A,B are above the MS, young? B is too red in         
                         the (Kabs,V-K) CMD, infrared companion? Planetary companion to A = HD           
                         28254 is detected with RV. No relevant references in SIMBAD.            Tok2011a
                         A is exoplanet host, P=1116d.  Roell et al. (2012 A&A 542, A92) list B          
                         as physical, confirmed by Naef et al. (2010 A&A 532, A15).              Tok2014d
04249-3445   I    59     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
04251+8603   WFC  23     HJL  57.                                                                HJL1986 
04252+2545   TOK 247     Not Hyades member: different PM and RV. (Griffin 2013).                 Grf2013c
04252+1716   AST   4     V805 Tau.                                                                       
                         The visual A consists of an M3.5V main sequence star (A) and an                 
                         unresolved WD (D) with a period of 20.82d. B consists of a pair of              
                         unresolved M dwarfs with an orbital period of 0.75d. V band fits of the         
                         masses of A, B and C are 0.46, 0.40 and 0.38 \msun, respectively. K             
                         band fits of the masses of A, B, C and D are 0.60, 0.46, 0.44 and 0.53,         
                         respectively.                                                           AST2021 
04252-6415   HJ 3656     B is CPD-64@333.                                                                
04253-0932   GAL 368     Object #129 in Gallo's original list.                                   Gal1914 
04254+2218   STF 541     A: kap 1 Tau = 65 Tau = K Tau                                                   
                         A,CD: H 6   8.                                                          MEv2010 
                         AB: HJL1034.                                                            HJL1986 
             STF 541     04253+2215STF 541CD and 04254+2218STFA  9AB were found to                       
             STFA  9     be the same wide pair, so designations for these two                            
                         multiple systems were combined, as follows:                                     
                         04253+2215STF 541AB   --> 04254+2218STF 541CD                                   
                         04253+2215STF 541AB,C --> 04254+2218STF 541A,CD                                 
                         04253+2215STF 541AB,D --> 04254+2218STF 541B,CD                                 
                         04254+2218STFA  9AB   --> 04254+2218STF 541AB                                   
                         04254+2218STFA  9Aa   --> 04254+2218STF 541AE                                   
                         04254+2218STFA  9Bb   --> 04254+2218STF 541BF                                   
                         A : kap 1 Tau = 65 Tau = K Tau. Occult. binary, Hyades member (vB 54)           
                         B : kap 2 Tau = 67 Tau. Delta Scuti variable, Hyades cluster member.            
                         CD : J 2722. This faint pair is between kap 1 and kap 2 Tau.                    
                         Pairs STFA  9AB (rho = 339"), STFA  9Aa (rho = 141") and STFA  9Bb              
                         (rho = 107") are all far outside our detection window.                  Msn1993a
04255+1756   KUI  17     del 3 Tau = 68 Tau. A is spectroscopic binary and variable, V776 Tau.           
             H 6 101     H VI 101. There is a wide faint pair noticed by John Herschel, 320@             
                         Class VI.                                                               H__1867 
                         The B, C, D, and E components all fall outside our detection window.    Msn1993a
04256+1556   FIN 342     Aa,Ab: Hyad (vB 57). HR 1391 = 70 Tau.                                          
                         Combined spectroscopic/astrometric solution. Orbital parallax 0.02144   Trr1997b
                         +/- 0.00067, masses 1.363 +/= 0.073 and 1.253 +/- 0.075 Msun.                   
                         Quadrant determinations made at several epochs by McAlister et al.      McA1988 
                         (1988) have shown that this system is best represented by an eccentric          
                         orbit of period 6.3 years, rather than a circular 13-year orbit.                
                         1977.7421  Theta was incorrectly given as 6.0 degrees by McAlister &            
                         Fekel 1980).                                                            McA1980b
                         This resolved spectroscopic binary (with P = 6.28 yr) is discussed by   McA1988 
                         McAlister et al. (1988) and by Dombrowski (1991).                       Dmb1991 
                         The published measure for 1988.6582 (McAlister et al. 1990) is          McA1990 
                         is spurious. The data leading to this measure are actually the same as          
                         those for HR 1331 (= McA 14) for the same epoch. These two stars were           
                         observed in immediate sequence but with different microscope                    
                         objectives, and the final reductions calculated two results from the            
                         same data set, but with different scale factors; the HR 1331 measure            
                         for 1988.6582 is the correct one.  Reanalysis of the correct data for           
                         FIN 342 gives the 25 mas result shown here. Peterson (1992, private             
                         communication) pointed out the inconsistency of our originally                  
                         published measure with respect to our previous orbital analysis of              
                         this Hyades binary (McAlister et al. 1988).                             Hrt1992b
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Aa,Ab : New spectroscopic solution determined by Griffin.               Grf2012b
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 2.50 +/- 0.47, 2.48, and 1.13 Msun, respectively.  Mlk2012 
04257+6340   HJL1033     SHY 464. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
04257-0214   BU  403     Linear elements fit nicely at present, but this is a physical pair and          
                         an orbit can be computed at some future date.                                   
                         Rectilinear solution by Hartkopf et al.  (2012).                        Hrt2012a
04258+1800   COU2682     Spectroscopic binary with P > 15 yr, according to Griffin et al.        Grf1988 
                         (1988).                                                                 Msn1993a
                         The spectroscopic solution of this 15650-d pair determined by Griffin.  Grf2012b
04258+1733   RED   4     1996.1449: RHy ID and coordinates from Reid (1992).                     Red1992 
                         Candidate Hyades member; Reid considers definite binary.                Red1997 
04259+1852   BU 1185     Hyad (vB 58).                                                                   
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         1982.7579: This autocorrelogram was remeasured; the new results are     McA1987b
                         listed here.                                                                    
                         The 27.67-year binary (see Dombrowski 1991) ADS 3210  was observed at   Dmb1991 
                         a time when atmospheric seeing was rated as poor.  Also noted as a SB   Grf1988 
                         in Griffin et al. (1988).                                               Msn1993a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.01 +/- 0.36, 2.00, and 0.98 Msun, respectively.             Mlk2012 
04260+4515   ES  567     B is BD+44@946.                                                                 
                         Measures attributed to BC are all AC. Component designation changed.            
04261-1059   GAL 369     Object #130 in Gallo's original list.                                   Gal1914 
04262+3313   HJ  676     AC: SEI  44.                                                            Nsn2017a
04263+3443   HU  609     Only elements P and T have been amended from the orbit of               Sta1978c
                         Heintz (1967).                                                          Hei1967d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 12.01 +/- 10.65, 3.16, and 1.20 Msun, respectively.           Mlk2012 
                         A is also a 141d spectroscopic binary. B is a possible                  Tok2019b
                         spectroscopic binary (~1600d), too.                                             
04263+2249   BUP  58     ups Tau = 69 Tau. A is an occultation binary.                                   
04263+2128   TOK  16     Hyades vB 62. Primary is 8.55d SB1 (Griffin & Gunn 1978); estimated     Grf1978b
                         period of visual pair 9300y. Unresolved by Patience et al.              Tok2006 
                         The SB  is outside our detection window.                                Msn1993a
04263+1538   HD  28052   Hyades vB 141. A CPM companion with rho = 134".4 is outside our         Msn1993a
                         detection window.  Also, noted as a 14.24-year SB by Abt (1965).        AbH1965 
04263+1537   BUP  59     71 Tau. A is a long-period spectroscopic binary,                                
                         P = 5200d, and occultation pair. V777 Tau.                                      
                         Peirce noted a close companion to A component (1868.13, 70deg) which            
                         he said was "much closer than 80 Tau". His 1868.13 separation                   
                         measure for 80 Tau (= 04301+1538 STF 554) was 0".75.                    Pei1882 
04263+1400   HJ 3256     LDS5558.                                                                        
04264+2249   HD  28024   Hyades vB 60. A CPM companion with rho = 110".2 is outside our                  
                         detection window.                                                       Msn1993a
04264+1651   HD  28068   Hyades vB 63. A spectroscopic binary B with P ~ 7 yr, according to      Grf1985b
                         Griffin et al. (1985).                                                  Msn1993a
04268+1525   LDS2236     LDS5559.                                                                        
04268+1052   PAT   8     1991.8990: This K dwarf is noted as a binary with a period in excess            
                         of 16 years in Griffin et al. (1988), and it is likely that we have     Grf1988 
                         detected the spectroscopic companion.                                   Msn1993a
                         The spectroscopic solution of this 6950-d pair determined by Griffin.   Grf2012b
04268+0843   HJ  678     This is not BD+08  690, according to Heintz.                            Hei1992a
                         AB: Rectilinear solution by Friedman et al. (2012).                     USN2012a
04268-0143   UC 1168     Candidate on Tokovinin list, now reconfirmed as CPM.                    Tok2013c
                         AB is CPM according to Hartkopf et al. (2013).  A is on Keck RV         UC_2013b
                         program, RV trend.                                                      Tok2014d
04269+2607   LEI   2     Measure of 1987.8 made by triangulation of multiple measures and was            
                         in a red filter.                                                                
             SMN  10     Ca,Cb: Called FV Tau-c by Simon, therefore given component designation          
                         of Ca,Cb. Relationship to LEI  02 uncertain.                            Smn1992 
                         Measure of 1987.8 made by triangulation of multiple measures and was            
                         in a red filter.                                                                
                         aka COR   3Ca,Cb                                                                
                         FV Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
04270+1907   STF 546     HJL  60.                                                                HJL1986 
                         H 2  54.                                                                MEv2010 
04270-7238   B  2091     Composite spectrum: G8III+(A/F).                                                
04271+2542   THB   1     Preliminary orbital elements give total mass 2.8 +/- 1.5 Msun.          Thb1995b
                         Tamazian et al. (2002) solution includes mass determination based on    Tam2002 
                         estimated distance.                                                             
                         DF Tau orbit by Schaefer et al. (2006) gives range 1974-2022 for T,     Sfr2006 
                         0.05-0.76 for e. Values for P and a are lower limits.                           
                         Assuming a distance of 140 pc, Schaefer et al. (2014) derive a total            
                         mass 1.17 +/- 0.13 Msun. The orbital period of 43.7y closely matches            
                         the 44yr timescale of photometric variations; this is consistent with           
                         a suggestion by Lamzin et al. (2001 A&A 372, 922) that the variability          
                         is caused by the circumstellar accretion rate onto the primary being            
                         modulated by the orbital motion of the companion.                       Sfr2014 
04271+1812   STF 545     AB: H 4  74.                                                            MEv2010 
04275+1113   BU 1186     A is variable.                                                                  
04275-1707   HU  440     Primary is HH Eri, eclipsing binary (Algol-type), P=8.5d.               Tok2014d
04275-2427   I   413     Baize (1993) value of omega incorrectly listed as 96.0, same as Omega.  Baz1993b
04276+1927   RED   5     1995.6986: RHy ID and coordinates from Reid (1992).                     Red1992 
                         LP ID from Luyten et al.(1981).                                         Luy1981 
                         Candidate Hyades member; Reid considers definite binary.                Red1997 
04277+2631   GIC  47     LDS1171.  G008-035/G039-014.                                                    
                         NLTT 13302/13303                                                        Chm2004 
04278+1001   STF 549     AB: H 4  75.                                                            MEv2010 
04280+2137   BUP  60     A is a spectroscopic and occultation binary.                                    
04281-1033   GAL 370     Object #131 in Gallo's original list.                                   Gal1914 
04282+5303   RUC   3     AO Cam. Spectral type of resolved companion later than M5V.             Ruc2007 
04282+0600   LDS9170     Old LDS6170.                                                                    
04283-1400   GAL 371     Object #132 in Gallo's original list.                                   Gal1914 
04284+1622   RCH   2     Measure of 1998.921 made by triangulation of multiple measures.         Rch2002 
04284+1444   CIA  25     76 Tau.                                                                         
04284-0736   GRV1248     Both A and B have approximately the same radial velocity.               Grv2019b
04284-6543   HJ 3662     B is CPD-65@@345.                                                               
04285+1742   GUE   5     The spectroscopic solution of this 7022-d pair determined by Griffin.   Grf2012b
04285+1458   BPM 100     [PM2000]  170962 + [PM2000]  171001.                                    Gvr2010 
04285+0505   HJ 2233     BAL 2614.                                                                       
04286+1944   HD  28291   Hyades vB 69.  The 41.66-day SB of Griffin et al. (1985) is outside     Grf1985b
                         our detection window.                                                   Msn1993a
04286+1911   BUP  61     eps Tau = 74 Tau = Ain                                                          
                         Mk III Limb-darkened diameter       2.67  +/- 0.04  mas.                MkT2001 
                         Mk III Limb-darkened diameter       2.671 +/- 0.032 mas.                MkT2003 
                         NPOI Limd-darkened diameter         2.41  +/- 0.11  mas.                NOI2001b
                         CHARA Array Limb-darkened diameter  2.734 +/- 0.031 mas.                CIA2009a
                         R =  13.4 +/- 0.2 \rsun, Teff = 4827 +/- 44 K.                                  
                         NPOI Limb-darkened diameter  2.592 +/- 0.050 mas, Sp = G8III,           NOI2018 
                          R =12.53 +/- 0.28 \rsun, Teff = 4880 +/- 77 K, L = 80.3 +/- 4.4 \lsun,         
                          M = 2.69 +/- 0.11 \msun, Age = 0.55 +/- 0.10 Gyr.                              
04287+2714   KON   2     Estimated masses 0.15 and 0.06 Msun. Primary spectral type M5.25        Kon2007b
04287+2613   HDS 576     Cvetkovic et al. (2014) derive spectral types M0 and  M0, masses 0.46           
                         and 0.46 Msun. Dynamical parallax is 25.86 +/- 0.27 mas.                Cve2014 
04287+1552   STFA 10     AB: the 2 Tau = 78 Tau = Chamukuy. Hyades vB 72 = HR 1412.                      
                         Pair appears in an appendix list, not part of discoverer's regular              
                         numbering sequence. B is BD+15@631.                                             
                         Also variable, probably of  Delta Scuti type.                                   
                         The 140.7-day SB of Ebbighausen (1959 Pub. DAO, 11, 235) is outside             
                         our detection window.                                                   Msn1993a
                         UBAD 2.1 relative astrometry measures computed. Table 1 mean positions  USN2022 
                         for 2017.0 and Table 2 mean dates computed as well when appropriate.            
             MKT  13     Aa,Ab: Data from lunar occultation, spectroscopy, and Mark III                  
                         astrometry are combined by Torres et al. to generate orbital elements.  Trr1997c
                         Distance and component masses and absolute magnitudes are derived from          
                         these elements.                                                                 
                         Period is fixed for the Armstrong et al. (2006) orbit. The resulting    MkT2006 
                         component masses are 2.15 +/- 0.12 Msun and 1.87 +/- 0.11 Msun.                 
                         Aa,Ab: Orbit determined by fitting revised Hipparcos intermediate               
                         astrometric data. Derived component masses are 2.03 +/- 0.87 and                
                         1.78 +/- 0.76 Msun.                                                     Ren2010 
                         Aa,Ab: Combined spectroscopic/astrometric solution, using data from             
                         Mark III interferometer plus high-resolution spectroscopy from ELODIE,          
                         HERMES, and CfA. Torres et al. (2011) determine an orbital parallax of  Lmp2011 
                         20.90 +/- 0.14 mas and component masses 2.86 +/- 0.06 and 2.16 +/-              
                         0.02 Msun. Effective temperatures for both components are 7800 +/-              
                         170K, absolute magnitues are 0.33 +/- 0.03 and 1.44 +/- 0.03 mag.               
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 4.46 +/- 0.29, 3.81, and 2.00 Msun, respectively.  Mlk2012 
             MCA  15     Ba,Bb:The primary of 04286+1558 was found to be the B component of              
                         physical pair 04287+1552; systems were merged.                                  
                         the 1 Tau = 77 Tau. Hyad (vB 71). Physical companion to the 2 Tau.              
                         A spectroscopic, occultation, and interferometric binary.                       
                         First detected as an occultation binary by White.                       Wit1979 
                         1979.698, 1979.857:  possible third component                           Heg1983 
                         This is a long period interferometric companion in addition to the              
                         spectroscopic component suggested by Griffin & Gunn (1977) to have a    Grf1977d
                         period of about 16 years.  An estimate of Delta m = 0.76 was made by    Dmb1991 
                         Dombrowski (1991).                                                      Msn1993a
                         Masses and distance of the 2 Tau are derived from spectroscopic                 
                         elements, adopting astrometric elements from Pan et al. (1992)          MkT1992e
                         Combined spectroscopic/astrometric solution by Torres et al. (1997).    Trr1997c
                         Distance (from relative proper motions and orbital parallax of the 2            
                         Tau) 47.6 +/- 1.9 pc, masses 2.91 +/= 0.88 and 1.31 +/- 0.14 Msun.              
                         CHARA Array Limb-darkened diameter of B  2.305 +/- 0.043 mas.           CIA2009a
                         R =  11.7 +/- 0.2 \rsun, Teff = 4811 +/- 50 K.                                  
                         Ba,Bb : New spectroscopic solution determined by Griffin.               Grf2012b
                         Ba,Bb: Malkov et al. (2012) derive dynamical and spectroscopic masses           
                         4.14 +/- 0.35 and 2.88 Msun, respectively.                              Mlk2012 
             BPMA  7     BC: [PM2000]  171052 + [PM2000]  171309.                                Gvr2010 
04288+1617   BPMA  8     [PM2000]  171281 + [PM2000]  171421.                                    Gvr2010 
04289+3022   STF 548     AB: B=HIP 20907 is bluer than A, below the MS. A is 1.7mag above. But           
                         they are physical: CPM, parallax, same RV! Primary is SB1, P=460.7d.    Tok2001 
                         A,B have same RV (Tokovinin & Gornya 2001), both rotate fast            Tok2014d
04289-0236   BRT 366     A likely plate flaw.                                                    Grv2021b
04290+1610   HU 1080     Hyad (VB 75); RV possibly variable, as noted by Wilson (1948).          WOC1948 
                         The spectroscopic solution of this 14697-d pair determined by Griffin.  Grf2012b
                         B is also a close 21.3-d pair.                                                  
                         M_A = 1.341 +/- 0.025 \msun, M_Ba = 1.210 +/- 0.021 \msun, M_Bb =       Trr2019b
                         0.781 +/- 0.014 \msun. Orbital parallax = 21.75 +/- 0.11 mas.                   
04290+1338   SIG   2     LP 475-855. Spectral types M7.5, M9.5. Probable Hyades member.                  
                         Estimated orbital period 86 +20/-19 yrs.                                Sig2003 
04292-1206   LDS3591     NLTT 13376/13372                                                        Chm2004 
04293+1733   HD  28394   Hyades vB 77.  The 238.9-day SB of Griffin et al. (1985) lies outside   Grf1985b
                         our detection window.                                                   Msn1993a
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin et al. (1985).                                                  Grf1985b
04293-3124   SIG   4     Aka 2MASS 0429-3123AB. Significant H\alpha emission. Appears to be      JLB2017 
                         young, but not a member of any known moving group or association.               
                         Parallax = 58.71 +/- 1.25 mas.                                                  
04294+2701   KON   3     Estimated masses 0.1 and 0.06 Msun. Primary spectral type M6.0          Kon2007b
04294-3335   HJ 3652     Primary is CT Eri, a Beta Lyr type eclipsing binary, P = 0.63420d.      Zas2012 
04295+2617   SMN  11     Measure of 1990.25 made by triangulation of multiple measures and was           
                         in a red filter.                                                                
                         AB: Additional notes may be found in Simon et al. (1992).               Smn1992 
             WHT   2     AC: Primary is the Orion-type variable FW Tau. Multi-epoch astrometry           
                         by Kraus et al. (2014) confirm the AC pair is co-moving, and estimate           
                         mass of the companion at 10 +/- 4 Mjup for a system age of 1-5 Myr.     KsA2014 
             HER   8     AD: Additional notes may be found in Herbig (1962).                     Her1962 
04295+1752   BGH   2     LDS 2244. Variable, V921 Tau. B is +17@  734.                                   
                         HJL1035.                                                                HJL1986 
04295+0025   BAL 972     RST 5206.                                                                       
04296+0350   BAL2121     J 2725.                                                                         
04297+2633   HAT   6     AB: Additional notes may be found in Herbig (1962).                     Her1962 
                         DI Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
             ITO  13     BC: B component is the Orion-type variable DH Tau = HBC 38. Colors of           
                         both B and C are consistent with T Tauri stars. The B component has a           
                         lower effective temperature than A (2700-2800K, vs 3580K), and is               
                         redder. The stars are probably early and late M stars; mass of the              
                         companion is estimated at 30-50 Mjup.                                   Ito2005 
                         Kraus et al. (2014) estimate mass of the companion at 18 +/- 4 Mjup.    KsA2014 
04298-0949   LDS3592     NLTT 13393/13392                                                        Chm2004 
04299+2607   HER   9     Aka IQ Tau. Additional notes may be found in Herbig (1962).             Her1962 
04300+8320   HR 1304     Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Prieur et al. (2006).                                                   Pru2006 
04300-6955   OGL 193     LMC157.7.150   + LMC157.7.333                                           Pli2012 
04301+1814   JOY   2     A RW Aur-type variable, UX Tau.                                         Her1962 
04301+1538   STF 554     80 Tau. Hyad. Star A is SB1, P = 30.5d                                  Hei1981e
                         Spectral types and masses of components assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
04301+1538   STF 554     The 1897 measure by Burnham was "... made under not the best            Bu_1900 
                         conditions ..." and "... is difficult to reconcile ...". Aitken did             
                         not include it in the ADS. It was, then, not in the IDS list of         A__1932a
                         measures transferred to Washington in 1964, so this measure was lost    IDS1963A
                         for many years and recently found by G. Torres, and the observation     Trr2019 
                         of this high eccentricity binary was made shortly after periastron              
                         passage, which resulted in the unexpected result.                               
                         Ma = 1.63 (+0.30 or -0.13) \msun, Mb = 1.11 (+0.21 or -0.14) \msun,             
                         orbital parallax = 20.984+/-0.060 mas.                                          
04302+3516   TTH   1     HBC 40 = LkHA 101. Herbig Ae/Be star imaged at multiple wavelengths             
                         shows evidence of a companion at ~180 mas to the East-Northeast of the          
                         primary. Derived physical parameters for A and B for three possible             
                         distances are:                                                                  
                            160pc: L/Lsun =  1300 and  340   R/Rsun = 1.9 and 1.0                        
                            340pc: L/Lsun =  5900 and 1500   R/Rsun = 4.1 and 2.1                        
                            800pc: L/Lsun = 30000 and 8500   R/Rsun = 9.7 and 5.0                Tth2002 
04302-0303   PRB   2     Primary is WD 0427-03 = NLTT 13402, secondary is LP 655-33. Possible            
                         CPM pair, according to Probst (1983).                                   Prb1983 
04302-6753   TOK  85     HIP 20998. Not observed, but J-K=2.92 for B in the 2MASS PSC, hence             
                         optical.                                                                Tok2011a
04303+1950   PAT  10     Noted as a probable SB in                                               Grf1988 
                         Griffin et al. (1988).                                                  Msn1993a
                         Member of the Hyades (vB 81) and "probable SB" according to Griffin et  Grf1988 
                         al. (1988). This WDS pair PAT 10 was resolved by speckle.               Tok2012a
                         The spectroscopic solution of this 4023-d pair determined by Griffin.   Grf2012b
04306+1612   LDS2246     Hyades vB 82. A is possibly variable. B is BD+15@640.                           
                         The primary was noted as a possible occultation binary by Peterson      Pts1981a
                         et al. (1981).                                                          Msn1993a
                         HJL1036.                                                                HJL1986 
04306+1545   HD  28545   Hyades vB 182.  The 358.4-day SB of Griffin & Gunn (1981) is outside    Grf1981d
                         our detection window.                                                   Msn1993a
04306+1542   BUP  62     81 Tau = LDS2247. Hyades vB 83.  B is BD+15@638.                                
                         AB: HJL1037.                                                            HJL1986 
             ARN  36     The CPM B companion with rho = 161".8 is outside our detection window,          
                         as are C and D.                                                         Msn1993a
             CIA  65     Ca,Cb : M_Ca = 0.9717+/- 0.0056\msun, M_Cb = 0.6859 +/- 0.0028 \msun,           
                         pi_orb = 20.318 +/- 0.042 mas, A_dia = 0.159 mas, B_dia = 0.118 mas.    CIA2024d
                         D component is primary of 04309+1547 TDS2876. Pair does not appear to    .      
                         be physical, so systems not merged.                                             
04306+1344   HD  28556   Hyades vB 84. A CPM companion with rho = 111".9 lies far outside our            
                         detection window with a large Delta m of 5.8.                           Msn1993a
04306+1343   BUP  63     83 Tau.                                                                         
04307+2601   SMN  12     Measure of 1990.77 made by triangulation of multiple measures and was           
                         in a red filter.                                                        Smn1992 
04307-1627   HJ 3653     B is BD-16@879.                                                                 
04308+1609   PAT  11     Hyades. The 0".3 binary PAT 11 was not resolved by speckle. The GCS did         
                         not detect RV variability despite large scatter of 4.8 km s-1 in their          
                         three measures.                                                         Tok2012a
04309+2442   SMN  13     ZZ Tau. Sfr2003 astrometry for 1995.081 and 1996.124 was based on               
                         interpolation of one-dimensional data by Simon.                         Smn1996a
                         The first ZZ Tau orbit by Schaefer et al. (2006) gives range 1994-1999  Sfr2006 
                         for T, 0.35-0.88 for e, 115-134 for i, 111-129 for Omega, 268-336 for           
                         omega.  Values of P and a are lower limits.  The second orbital                 
                         solution includes a lunar occultation measure by Simon et al. (1995).   Smn1995 
                         Assuming a distance of 140 pc, Schaefer et al. (2014) derive a total            
                         mass of 0.83 +/- 0.16 Msun.                                             Sfr2014 
04309+1547   TDS2876     D component of 04306+1542. ARN  36AD does not appear to be physical,            
                         so systems not merged.                                                          
04309-0849   KO    2     CPM pair; A = LP 655-23 (spec early M), B = 2MASS J0430516-084901               
                         (M8.0V). Mean separation (1953-2000) 0.328 +/- 0.004 arcmin. Data               
                         sources: Palomar Sky Survey red (1953.2), UK Schmidt blue (1982.8), UK          
                         Schmidt red (1985.9), 2MASS (1998.7), DENIS I (1998.9), UK Schmidt              
                         near-IR (2000.0). Masses of components estimated at 0.26 +/- 0.04 and           
                         0.086 +/- 0.004 Msun.                                                   Cab2007b
                         A known component of the wide binary Konigstuhl 2AB with a separation           
                         of 20" (Caballero 2007), 2MASS J04305203-0849193 is single closer in,   Cab2007b
                         in the AstraLux images.                                                 Jnn2012 
04310+7724   MLR 461     Also known as TDS 142.                                                          
04310-6911   OGL 194     LMC156.6.7     + LMC156.6.6                                             Pli2012 
04311+0647   STT  84     HJL  61.                                                                HJL1986 
04311-4522   TOK 208     Possibly triple. The new companion at 1".6 should not produce RV                
                         variability by 3.8 km s-1.                                              Tok2012a
04312+5858   STI2051     A is an astrometric binary. B (mag. 12.44, 8", DC) is a white dwarf,            
                         in slow retrograde motion about the mass-center. A very large proper            
                         proper motion brought this pair close to a 13th magnitude star which            
                         was measured as the C component by Pauwels & Lampens.                   Pws1993 
                         Also known as HDS 584.                                                          
                         B: Teff = 7122 +/- 122 K, R = 0.0114 +/- 0.0004 \rsun, M = 0.675 +/-    BdH2017b
                         0.051 \msun.                                                                    
                         AB: Rectilinear solutions by Cvetkovic (2015)                           Cve2015b
                         and Cvetkovic et al. (2016).                                            Cve2016 
                         Despite the linear solution, based on proper motion and parallax                
                         is physical.                                                                    
04312+0621   LDS9171     Old LDS6171.                                                                    
04313-6959   OGL 195     LMC157.7.2247  + LMC157.7.2249                                          Pli2012 
04314+4001   STF 552     H N  44.                                                                MEv2010 
04314-0934   GAL 372     Object #136 in Gallo's original list.                                   Gal1914 
04314-1339   STF 560     B is BD-13@905.                                                                 
04315+1706   SAR   3     HBC 392 = V1074 Tau. SB2.                                               Sar1998 
                         Member of Taurus-Auriga molecular cloud.                                Dae2015 
04316+1743   HD  28634   This is a 2.31-year spectroscopic binary, according to Griffin et al.   Grf1985b
                         (1985).                                                                 Msn1993a
             vA 627      VVO 394. Hipparcos astrometric solution adopted some elements from the  HIP1997d
                         orbit of Griffin et al. (1985). Hyad.                                   Grf1985b
                         Perturbation orbit by McArthur et al. (2011) is based on HST FGS        AST2011 
                         astrometry, plus radial velocities from Griffin et al. (1985). Derived  Grf1985b
                         masses are 0.83 +/- 0.05 and 0.42 +/- 0.05 Msun.                                
04316-7037   OGL 196     LMC158.1.29    + LMC158.1.122                                           Pli2012 
04317+2330   POU 458     LDS 886 = LDS1173.                                                              
04317+1814   HER  10     AB: Additional notes may be found in Herbig (1962).                     Her1962 
                         XZ Tau.                                                                         
             GHE   9     Aa,Ab: Dodin et al. (2016) generated the following preliminary orbital          
                         elements: P = 155-256y, a = 27.2-37.2au, i <47deg, e = 0.29-0.64.       Dod2016 
                         Carrasco-Gonzalez et al. (2009) found a close companion to the Aa       CGo2009 
                         component at 7mm wavelength (~6deg, 0.09", dm 0.4 +/- 0.3 mag).                 
                         However, subsequent observations by Forgan et al. (2014) and the ALMA   Fgn2014 
                         Partnership (2015) found no evidence of this additional component and   ALM2015 
                         concluded it was a false detection.                                             
04317+1538   WOR  16     The A component is a known Hyad.                                                
             LDS1174     The C component may or may not be a physical companion, possibly                
                         sharing CPM only as a member of the cluster.                                    
04318+2424   CHN   3     Formerly known as LEI  15.                                                      
04319-0851   HJ 2234     B is BD-09@917.                                                                 
04320+5355   STF 550     1 Cam. A spectroscopic binary.                                                  
                         AB: H N  67.                                                            MEv2010 
04320+1822   CHN   4     Formerly known as LEI  16.                                                      
                         AB: Additional notes may be found in Herbig (1962).                     Her1962 
             HER  11     AD: Additional notes may be found in Herbig (1962).                     Her1962 
04320-6939   OGL 197     LMC157.5.2454  + LMC157.5.2477                                          Pli2012 
04322+3630   AG   80     ALI 293.                                                                        
04322+1820   KSA 107     Primary is variable star V827 Tau.                                              
04322+1757   MSR   1     HBC 397 = V1075 Tau.                                                    Msr2005 
04323+2423   GHE  10     Aka V928 Tau.                                                                   
04323+2422   KON   4     Estimated masses 0.07 and 0.06 Msun. Primary spectral type M6.5         Kon2007b
04323-6918   OGL 198     LMC156.7.3411  + LMC156.7.3620                                          Pli2012 
04324+0128   HDO 307     Aka BAL 1273.                                                           Hei1983a
04325+2420   HAT   7     A and B are FY Tau and FZ Tau.                                                  
                         Additional notes may be found in Herbig (1962).                         Her1962 
04325+2044   RED   6     1996.0902  RHy ID and coordinates from Reid (1992).                     Red1992 
                         LP ID from Luyten et al. (1981).                                        Luy1981 
                         Candidate Hyades member; Reid considers possible binary.                Red1997 
04325+1732   LEI   3     Aa,Ab: GG Tau.                                                                  
                         Tamazian (2002) solution includes mass determination based on an        Tam2002 
                         estimated distance.                                                             
                         Aa,Ab: Kohler (2011) derives orbits both coplanar and not coplanar              
                         with the disk; only his "most plausible" orbit is tabulated in the              
                         orbit catalog. Elements are as follows: P = 403 +67/-32 y, a = 0".429,          
                         i = 132.5 +1.0/-2.5 deg, Omega = 131 +13/-8 deg, e = 0.44 +0.02/-0.03,          
                         T = 2463400 +1470/-5420, omega = 19 +9/-10.                             Koh2011 
             CHN   5     AB: formerly known as LEI   3.                                                  
             DIF   1     Ab1,Ab2: Di Folco et al. estimate spectral types for Ab1 and Ab2 of M2V         
                         and M3.5V, respectively. Assuming the close pair is coplanar with the           
                         outer diskof the system, the stars were separated by 5.1au in Dec 2012. DiF2014 
04326+2628   GIC  48     LDS1176 = G008-040/G039-021.                                                    
                         NLTT 13455/13456                                                        Chm2004 
                         HD 283702. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
04326-0313   H 6  64     H VI 64. Probably a variable of Delta Scuti type,                               
                         DZ Eri. B is BD-03@810.                                                         
04327+2553   GHE  11     Aa,Ab: Measure of 1990.77 made by triangulation of multiple measures            
                         and was in a red filter.                                                Smn1992 
             JOY   3     AB: A RW Aur-type variable, UZ Tau.                                             
                         Measure of 1990.77 made by triangulation of multiple measures and was           
                         in a red filter.                                                        Smn1992 
                         AB: Additional notes may be found in Herbig (1962).                     Her1962 
04327+1855   DAE  26     V1203 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04327+1803   SAR   4     HBC 403 = V1076 Tau.                                                            
04328+1600   CHR 152     This is probably the spectroscopic system found by Griffin et al.       Grf1988 
                         (1988) to have a period in excess of 15 years.                          Msn1993a
                         The spectroscopic solution of this 9377-d pair determined by Griffin.   Grf2012b
04329+0007   LDS 121     BC: NLTT 13492/13491 = LSPM J0432+0006. Law et al (2008) derive a       Law2008 
                         distance of 16.5 +8.2/-2.7 pc and a projected separation of                     
                         76.2 +38.7/-11.8 au. Estimated spectral types are M4.5 and M5.5.                
04330-3817   BU  747     RZ Cae, Algol-type eclipsing binary, P = 2.486955 d.                    Zas2011 
04331+2410   GHE  13     Ab1,Ab2: Second and third Schaefer et al. (2006) orbits for Elias 12    Sfr2006 
                         Na-Nb include a lunar occultation measure by Simon et al. (1995)        Smn1995 
                         Schaefer et al. (2012) derive spectral types, Teff, luminosities, and           
                         masses for the Aa, Ab1, and Ab2 components (assuming a distance of              
                         140pc for M and L) as follows:                                                  
                            Aa:  K7       4060K  1.05 +/-0.20 Lsun  1.040+/-0.016 Msun (Mtotal)          
                            Ab1: M2       3560   0.447+/-0.058      0.564+/-0.018                        
                            Ab2: M2-M2.5  3560   0.356+/-0.038      0.476+/-0.017                Sfr2012 
                         Aa,Ab: V807 Tau. Young member of Taurus-Auriga molecular cloud.         Dae2015 
             HAT   9     AB: Additional notes may be found in Herbig (1962).                     Her1962 
             GHE  12     Ba,Bb: GH Tau. Young member of Taurus-Auriga molecular cloud.           Dae2015 
04331-1208   STF 564     The pair GAL 145 is identical                                           Hei1983a
04331-4646   SKF1205     The pair also show matching radial velocities, but primary is a SB1.    TrC2006 
04332+2434   SAR   5     HBC 405 = V830 Tau.                                                             
04332-6829   OGL 199     LMC155.5.3403  + LMC155.6.576                                           Pli2012 
04333+6847   LDS9172     Old LDS6172.                                                                    
04333+5921   TOR   7     Formerly known as PAN   4.                                                      
04333+5248   MLR 695     Aa,Ab: Also known as HDS 591.                                                   
             ES 2607     B is BD+52@844.                                                                 
04333+2505   LDS5190     old LDS6173.                                                                    
04334+4304   SHJ  44     57 Per. STTA 50 = H 6  99.                                                      
04335+7232   HJ 2228     AB: A is a spectroscopic binary.                                                
                         Also an unresolved 4.194d spectroscopic binary.                         Mug2017b
             LDS1595     AC: Initially merged with AB under mistaken belief was same pair.               
04335+1801   STF 559     H N 132.                                                                MEv2010 
04336+2610   GHE  14     Aa,Ab: IS Tau. Young member of Taurus-Auriga molecular cloud.           Dae2015 
04336+2421   POU 460     AB: Haro 6-22. Both components variable (A: 13.9-15.5, B: 14.1-16.1)            
                         according to Wenzel (1957 Nach. astr. Zentralst. 11,28)                 Her1962 
                         A is GK Tau. B is GI Tau.                                                       
04336-6249   HJ 3670     B is CPD-63@343.                                                                
04337+1824   DAE  27     V1323 Tau.                                                              Dae2015 
04337+1752   CHN   7     Formerly known as LEI  17.                                                      
                         HN Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
04338+1451   CIA  51     rho Tau = 86 Tau.                                                               
                         Hipparcos astrometric solution assumes circular orbit (e = omega = 0);  HIP1997d
                         Hyades VA 725 = vB 95.  1.337-year SB according to Abt (1965).          AbH1965 
04339-0644   BU  881     46 Eri. A is variable EH Eri, P = 3.8d, small amplitude.                        
04340+1510   CHR  17     This rapidly moving system within the wide binary ADS 3317 is probably  Grf1988 
                         the spectroscopic system with P ~13 yr found by Griffin et al. (1988).  Msn1993a
                         New spectroscopic solution determined by Griffin.                       Grf2012b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.27 +/- 0.34, 1.66, and 0.95 Msun, respectively.             Mlk2012 
04340-5503   B  2092     alp Dor. Hyad (vB 96).                                                          
                         High mass-sum, illustrative solution only, speckle/spectroscopic orbit          
                         needed, cf. Griffin et al. (1988).                                      Grf1988 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 5.51 +/- 1.51, 4.25, and 2.69 Msun, respectively.  Mlk2012 
             HJ 3668     AB,C: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
04342+2612   SMN  14     Measure of 1990.77 made by triangulation of multiple measures and is            
                         in a red filter.                                                        Smn1992 
04343+1830   SAR   6     HBC 407 = V1077 Tau.                                                            
04344+6928   HJ 1145     Aka TDS2898.                                                            Skf2016a
04344+1630   OL  107     The ES pair formerly listed at 04350+1631 (= ADS 3313)                          
                         is identical to this pair.                                              Hei1980a
04345-6859   OGL 200     LMC156.4.9     + LMC156.4.130   + LMC155.1.775                          Pli2012 
04345-6958   OGL 201     LMC157.2.3089  + LMC157.2.3113                                          Pli2012 
04346-6948   OGL 202     LMC157.3.2891  + LMC157.3.2890                                          Pli2012 
04346-7015   OGL 203     LMC151.5.4     + LMC151.5.38    + LMC151.6.4891                         Pli2012 
04348+3206   SEI  49     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
04349-7651   HJ 3691     B is CPD-77@176.                                                                
04350-1246   GAL 373     Object #143 in Gallo's original list.                                   Gal1914 
04352+1822   SAR   7     TAP 51  = V1078 Tau.                                                            
04352-0944   STF 570     B is BD-10@958.                                                                 
                         H 3 100.                                                                MEv2010 
04353+2254   KSA 108     Primary is variable star FF Tau.                                                
04353+2232   HER  23     HAT  11.                                                                        
04354+1045   RED   7     Identification with GCS2 uncertain.                                             
                         1996.8130  RHy ID and coordinates from Reid (1992).                     Red1992 
                         LP ID from Luyten et al. (1981).                                        Luy1981 
                         Candidate Hyades member; Reid considers definite binary.                Red1997 
04356+2408   HRM   1     AB = DCH  56. IRAS 04325+2402.                                                  
04356+1206   TOK  17     Hyades vA 771.                                                                  
                         Primary is 1.9d SB2. Estimated period of visual pair 400y.              Tok2006 
04357+2411   CHN   8     Formerly known as LEI  19.                                                      
04357+1953   L     4     First resolved by Lewis in 1902, this system was unconfirmed for        GrO1932A
                         several decades despite numerous attempts, notably those of Aitken              
                         with the 36inch between 1910 and 1922. In the ADS, Aitken concluded     A__1932b
                         "It is very doubtful whether the star is double". The system was                
                         subsequently removed from the WDS, until its resolution by Prieur et            
                         al. over 90 years after its discovery.                                  Pru2002b
04357+1010   CHR  18     Aa,Ab: 88 Tau. A is an Alpha CVn-type variable, and spectroscopic               
                         binary, now resolved by speckle interferometry.                                 
                         B is BD+09@606.                                                                 
                         1997.071: Absolute quadrant determined by triple-correlation                    
                         techniques                                                              Pru2002b
             88 Tau      Lane et al. (2007) combine PHASES astrometry with speckle and radial    Lne2007 
                         velocity data to derive an orbit for the Aa,Ab components of the                
                         nearby sextuple 88 Tau, as well as the Aa1,Aa2 and Ab1,Ab2 subsystems.          
                         The parallax of the system is determined at 0".01973 +/- 0".00034,              
                         with semimajor axes for Aa,Ab; Aa1,Aa2; and Ab1,Ab2 of 12.17 +/- 0.17,          
                         0.0689 +/- 0.0012, and 0.0997 +/- 0.0021 au, respectively. Other                
                         derived quantities for the four components are as follows:                      
                                Star     Mass (Msun)        M_K (mag)      Spec Type                     
                                Aa1    2.06  +/- 0.11     0.69 +/- 0.26      A6m                         
                                Aa2    1.361 +/- 0.073    2.20 +/- 0.28      F5V                         
                                Ab1    1.069 +/- 0.069    2.31 +/- 0.27      G2-3:V                      
                                Ab2    1.057 +/- 0.068    2.00 +/- 0.27      G2-3:V                      
             SHJ  45     STTA 52.                                                                        
                         AB: H 6  31.                                                            MEv2010 
04358-6655   OGL 204     LMC152.7.209   + LMC152.7.891                                           Pli2012 
04359+2352   KOH  15     V1324 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04359+2254   LEI  21     Primary is V1025 Tau.                                                           
             HAT  12     C component is HP Tau.                                                          
04359+1631   BU  550     alp Tau = 87 Tau = Aldebaran. A is an unclassified variable.                    
                         Mk III Limb-darkened diameter 21.21 mas.                                MkT1991 
                         Mk III Limb-darkened diameter 21.099 +/- 0.211 mas.                     MkT2003 
             STFB  2     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         Incorrectly listed as STFA  2.                                                  
             STFA  2     AC: H 6  66.                                                            MEv2010 
             STFB  2     AC: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
04359-0332   LDS9174     Old LDS6174.                                                                    
04360-0337   STF 571     AB: H 3  95.                                                            MEv2010 
04361+5525   HIP  21433  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Tokovinin et al. (1994). They derived component masses 0.88 and 0.24    Tok1994c
                         Msun and an estimated semimajor axis of 28.68 mas.                      Ren2013 
04362+0814   A  1840     Observations suggest eccentricity >0.80 and period 150-200y.            Mlr1956a
                         Star C (mag. 9, 6") is probably physical.                                       
04363+5502   RAO  35     Triple, consisting of a 2.6 day spectroscopic binary (Gorynya &                 
                         Tokovinin 2014 MNRAS 441, 2316) and the Robo-AO and 2MASS companion at          
                         5".7. The field is crowded and PM(A) is small. Our photometry places B          
                         slightly above the MS. The star is young and active according to                
                         Guillout et al (2009 A&A 504, 829) and we retain B as likely physical.  Rbr2015d
04363+4722   S   451     STTA 51. B is BD+47@1012.                                                       
04363-0321   BUP  64     nu Eri = 48 Eri. A is a Beta CMa-type variable.                                 
04363-6655   OGL 205     LMC152.7.23    + LMC152.7.88                                            Pli2012 
04364+3413   HU  610     Only elements P, T, and a have been amended by Starikova (1978) from    Sta1978c
                         the orbit of Baize (1961).                                              Baz1961b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.70 +/- 1.07, 2.11, and 0.95 Msun, respectively.             Mlk2012 
04365-0559   LDS9175     Old LDS6175.                                                                    
04365-0611   LDS 843     Aka LDS9175.                                                                    
04366+1930   LDS3597     The primary is a BY Draconis-type variable.                                     
04366+1845   RUC   4     RZ Tau. Spectral type of resolved companion M3-5V or possibly later.    Ruc2007 
04367+4116   58 Per      Wyller orbit rejected from Fourth Orbit Catalog                         Wye1957 
                         ("not confirmed by subsequent observations")                            Wor1983 
04367+4105   STF 563     H 3  65.                                                                MEv2010 
04367+1155   LDS1181     Hyades vB 210.                                                                  
                         NLTT 13608/13606                                                        Chm2004 
04367-6733   OGL 206     LMC153.7.3072  + LMC153.7.3092                                          Pli2012 
04368+2708   GIC  49     LDS1180 = G008-044/G039-027 = GJ 171.2AB. A component is the variable           
                         V833 Tau = Melotte 25 301.                                                      
                         NLTT 13601/13599                                                        Chm2004 
                         Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
04368-6205   HJ 3679     A is a long-period variable, R Dor.                                             
04372+3108   KOH  16     V961 Tau. Member of Taurus-Auriga molecular cloud.                      Dae2015 
04372+1108   GIC  50     LDS1182 = G083-024/G083-023.                                                    
04372-6658   OGL 207     LMC152.7.3126  + LMC152.7.3127                                          Pli2012 
04373+1748   BPM 101     [PM2000]  178584 + [PM2000]  178531.                                    Gvr2010 
04373-6853   OGL 208     LMC155.1.4867  + LMC155.1.5999                                          Pli2012 
04373-6905   OGL 209     LMC149.7.8     + LMC149.7.35    + LMC149.5.668                          Pli2012 
04374+0034   STTA 53     B is BD+00@801.                                                                 
                         Pair appears in an appendix list, not part of the discoverer's                  
                         regular numbering sequence.                                                     
                         SHY 465. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
04375+1509   CHR 153     1991.9021: Reprocessing of archival speckle data have confirmed this            
                         already strong detection and have shown a change in theta of 15 deg in          
                         2.7 yr. CHR 153 cannot be the 734.2-d spectroscopic system of Griffin   Grf2012b
                         et al. (1988). In the Hyades.                                           Msn1993a
                         The preliminary orbital solution is clearly in error as the visual      Ole2003b
                         companion was better fit by linear motion and it previously appeared in Hrt2012a
                         the linear catalog. However, with more observations an orbit solution           
                         was possible.                                                           Tok2021b
04376-0228   WAL  32     After analysis of proper motions, radial velocities, etc. conclude              
                         that A (= 51 Eri) and C (= GJ 330) comprise a wide physical binary and          
                         are members of the young bet Pic moving group. Distance is ~30pc and            
                         estimated orbital period is ~60,000y; pair form a very fragile system.  Fgl2006 
                         C component is GJ 3305; A and C are members of bet Pic moving group.    Zuc2001b
             BU   88     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             KAS   1     Ca,Cb: Better known as GJ 3305, this binary is part of the beta Pic             
                         moving group (Zuckerman et al. 2001), and is also bound to 51 Eri in a  Zuc2001b
                         wide orbit (Feigelson et al. 2006) with a projected separation of 66".  Fgl2006 
                         The binarity of GJ 3305 was first reported by Kasper et al. (2007),     Kas2007b
                         and has been observed with AstraLux on several occasions.               Jnn2012 
                         Ca,Cb: Montet et al (2015) derive a combined spectroscopic/astrometric          
                         orbital solution, yielding masses 0.67 +/- 0.05 and 0.44 +/- 0.05               
                         Msun, luminosities 0.112 +/- 0.007 and 0.043 +/- 0.005 Lsun, and an             
                         age of 37 +/- 9 Gyr.                                                    Mtt2015 
04379-6701   OGL 210     LMC152.2.1     + LMC152.2.31                                            Pli2012 
04379-6915   OGL 211     LMC149.7.39    + LMC149.7.80                                            Pli2012 
04380-1302   STF 576     B is BD-13@938.                                                                 
04381+1457   LDS5582     LDS6138.                                                                        
04382+2813   BEU   6     GJ 3304 = G039-029.  Daemgen et al. (2007) derive a distance of 14.5    Dae2007 
                         +/- 3.8 pc, a separation of 11.4 +/- 3.4 au, and a predicted orbital            
                         period of 76 +36/-35 yr. Spectral types are M4.0 +/- 0.5  and M4.5 +/-          
                         0.5; masses are 0.23 +0.10/-0.07 and 0.20 +0.07/-0.05 Msun.                     
                         Estimated age 60-300 Myr; masses 0.28 +/- 0.06 and 0.19 +/- 0.05 Msun;          
                         a ~13.4 au.                                                             Jnn2014 
04382+1603   PAT  12     Aa,An. CPM companion (rho = 140".5) is outside our detection window.    Msn1993a
04382+1602   BUP  65     89 Tau.                                                                         
04382+1231   BUP  66     Hyades vB 104. 90 Tau. A is a spectroscopic binary.                             
                         Two CPM companions (rho = 44" and 120") fall outside detection window.  Msn1993a
             MRN   2     Aa,Ab: Marion et al. (2014) estimate the companion to this Hyades               
                         member as K4V.  Assuming a face-on, circular orbit with a semi-major            
                         axis of 11.1 mas (0.52 au), the minimum period would be ~84d.           Mrn2014 
04382-1315   TOK 660     Resolved using ANDICAM2. PM(A) is small, B is considered physical from          
                         photometry and low crowding                                             Tok2014d
04382-1418   KUI  18     53 Eri = Sceptrum.                                                              
04384+2611   ITO   6     AC: Itoh et al. (2008) estimate that if the AC pair is physical, the            
                         H-band magnitude of C suggests a mass of order 1 Mjup. Followup                 
                         astrometry and spectroscopy is needed to confirm its companionship.     Ito2008b
04385+2656   STF 572     AB: One component is a spectroscopic binary.                                    
                         Has an orbital solution and while proper motion is close, parallax      Izm2019 
                         indicates it is non-physical.                                                   
04385+2611   SMN  15     Aka HV Tau.                                                                     
04385+2611               Measure of 1990.77 made by triangulation of multiple measures                   
                         and is in a red filter.                                                 Smn1992 
04385+1752   BPM 102     [PM2000]  179567 + [PM2000]  179474.                                    Gvr2010 
04386-0921   TOK 387     HIP 21265 is an X-ray source and an SB2 according to GCS (only one              
                         observation). It is resolved here at 56mas, which corresponds to a              
                         period of ~5yr.                                                         Tok2015c
04387-6822   OGL 212     LMC148.5.112   + LMC148.5.706                                           Pli2012 
04388+2147   JNN 262     G 8-48. Estimated age 300-1000 Myr; masses 0.12 +/- 0.04 and 0.10 +/-           
                         0.03 Msun; a ~21.9 au.                                                  Jnn2014 
04388-2702   TOK 661     CA: Resolved using ANDICAM2. Tuc-Hor moving group. PM(C) is small,              
                         physical from ptm only.                                                 Tok2014d
04388-7015   OGL 213     LMC151.4.44    + LMC151.4.45                                            Pli2012 
04389+1406   HD  29461   Hyades vB 106.  This is SB with P ~ 10 yr according to Griffin et al.   Grf1988 
                         (1988).                                                                 Msn1993a
04389+1406   MET  41     This optical companion cannot be 3760d spectroscopic binary of Griffin  Grf2012b
04389-1207   HDS 599     Cvetkovic et al. (2014) derive spectral types A1 and  F2, masses 2.28           
                         and 1.56 Msun. Dynamical parallax is 15.50 +/- 0.75 mas.                Cve2014 
04390+2149   LDS1183     NLTT 13673/13674                                                        Chm2004 
04391+0752   BUP  67     B is BD+07@680.                                                                 
04392+2553   TER   1     IRAS 04361+2547.                                                                
04393+3331   JNN 263     Estimated age 1000-10000 Myr; masses 0.32 +/- 0.16 and 0.20 +/- 0.10            
                         Msun; a ~2.6 au.                                                        Jnn2014 
04393+2545   SMN  16     GN Tau.                                                                         
04393+2221   LKCA 15     Sallum et al. (2015) resolve three planetary companions to LkCa 15.             
                         Companion b has a best-fit orbital semi-major axis 14.7 +/- 2.1 au,             
                         that of companion c is 18.6 +2.5/-2.7 au. Companion d is only seen in           
                         the L' band, so less information can be gleaned.                        Sll2015b
04393+1555   STFA 11     A: sig 2 Tau = 92 Tau. A is a spectroscopic binary.                             
                         B: sig 1 Tau = 91 Tau. B is BD+15@665, SB and occultation binary.               
04394-6938   OGL 214     LMC150.4.33    + LMC150.4.139                                           Pli2012 
04395-1141   GAL 374     Object #147 in Gallo's original list.                                   Gal1914 
04395-4507   I  1489     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.49 +/- 0.82, 1.60, and 0.79 Msun, respectively.             Mlk2012 
04396-2115   BU 1236     AC: SHY 467. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
04397+0952   HDS 601     Also a 610d spectroscopic binary.                                       Tok2019b
             GIC  51     LDS1184.  AB = G083-028/G083-029 = GJ 9162AB.                                   
04397-6722   OGL 215     LMC153.3.3746  + LMC153.3.4025                                          Pli2012 
04399+5305   BU 1043     3 Cam. A is an eclipsing binary of the W UMa-type.                              
04399+1940   RED   8     1996.0929  RHy ID and coordinates from Reid (1992). Candidate Hyades    Red1992 
                         member; Reid considers possible binary.                                 Red1997 
04399+1631   BU 1044     Measures made by CHARA/USNO in 1991, 1993, 1995, 1996 and 1998 of               
                         04404+1631 = CHR 154 were actually of this pair. Those measures have            
                         been included here.                                                             
04400+5328   BU 1295     2 Cam.                                                                          
                         The high-eccentricity solution for AB by Valbousquet (1980) is          Val1980b
                         questioned by Heintz (1962) on grounds of a mass discrepancy.           Hei1962 
                         The equinox-1900 position was incorrectly given as 04320+5310 in                
                         McAlister & Hendry (1982).                                              McA1982d
                         Argument of periastron flipped for Tok2021b orbit since WDS refers to           
                         fainter star as primary.                                                        
             STF 566     A is the D component of 04404+5328.                                             
04400+3534   HJ  681     ALI 64.                                                                         
04400+2556   KON   5     Estimated masses 0.1 and 0.06 Msun. Primary spectral type M5.75         Kon2007b
04403-6924   OGL 216     LMC149.2.6     + LMC149.2.26                                            Pli2012 
04404+5328   D     4     AD: D component is primary of 04400+5328BU 1295AB. AD not physical, so          
                         systems not merged.                                                             
04404+1631   CHR 154     Measures made by CHARA/USNO in 1991, 1993, 1995, 1996 and 1998 were             
                         actually of 04399+1631 = BU 1044. Measures X coded here but retained            
                         to maintain original catalog pedigree.                                          
04404-1940   STN   9     54 Eri. A semiregular variable, DM Eri. No very positive observations           
                         as a visual double. Needs speckle.                                              
04404-2935   DAW  81     BC: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
04406-4152   HDO 190     AB: alp Cae. A is a Delta Scuti-type variable.                                  
                         AB: Physical/optical nature undefined.                                  Ehr2010 
04407+2519   KON   6     Estimated masses 0.15 and 0.08 Msun. Primary spectral type M5.5         Kon2007b
04407-2812   TOK 209     Resolved with NICI, uncertain measure. Not resolved with speckle.       Tok2012a
                         Direct motion by 16deg since first resolution at Gemini on 2011.80;             
                         estimated period is 15 yr.                                              Tok2013b
04408-3951   RSS   5     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
04408-6741   OGL 217     LMC146.8.31    + LMC146.8.30                                            Pli2012 
04409+0058   STF 583     AB: H 2  81.                                                            MEv2010 
04410-6935   OGL 218     LMC150.4.7439  + LMC150.4.8170                                          Pli2012 
04413+3242   JNN 264     Estimated age 300-1000 Myr; masses 0.54 +/- 0.04 and 0.40 +/- 0.06              
                         Msun; a ~58.9 au.                                                       Jnn2014 
04414+2715   KOH  20     V1328 Tau.                                                              Dae2015 
04413+2054   LWR   5     V834 Tau                                                                        
04415-4328   Anon        EQ 0439-4333. ID as EQ 0439-4333 is uncertain, as it was based on a             
                         Simbad search using epoch-1950 coordinates 043955-433318 from White et  Whi1991 
                         al. (1991).                                                                     
04416-4302   WHI   6     Possibly resolved.                                                      Whi1991 
04417+2302   KSA  29     Primary is of spectral type M8.5 and shows evidence of a circumstellar          
                         disk and active accretion. The Ab companion is estimated as type                
                         M9.5-L0, mass 5-10 Mjup. Todorov et al. (2010) also resolved the B              
                         component into a 0.23" pair.                                            Tod2010 
04418+2658   KOH  21     Member of Taurus-Auriga molecular cloud.                                Dae2015 
04419-6714   OGL 219     LMC146.5.3639  + LMC146.5.3827                                          Pli2012 
04421+2523   LEI  24     V955 Tau.                                                                       
             GHE  15     The measures and component designations of the Ba and Ca pair were              
                         assigned incorrectly and were correctly re-assigned 5/22/02. The                
                         designations LEI  24Ba <---> GHE  15Ca were flipped and the                     
                         designation LEI  25Aa became LEI  24Aa.                                         
04422+3731   STF 577     CfA: SB? Not clear if it is A or B.                                     Tok2014d
04422+2257   MCA  16     Aa,Ab: tau Tau = 94 Tau. Occultation binary and short-period SB.                
                         Hough suspected duplicity due to a slow occultation. Finally resolved           
                         by McAlister in 1980.                                                   McA1983 
                         1983.9337, 1983.9391: Interferometric observations are incompatible     Jef1963 
                         with the large delta m reported by Jeffers et al. (1963).               Bnu1984 
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 12.44 +/- 4.14, 7.48, and 6.92 Msun, respectively. Mlk2012 
                         Uniform disk diameter  0.220 +/- 0.016 mas,                                     
                         Limb darkened diameter 0.226 +/- 0.016 mas,                                     
                         Teff = 18500 +/- 800 K based on LDD.                                            
                         Radius is 2.27 +/- 0.20 \rsun.                                          CIA2019a
             S   455     STTA 54 = H 6   7.                                                              
04422+0259   A  2424     Position angles uncertain.                                                      
04423+8103   LDS1596     NLTT 13589/13587                                                        Chm2004 
04423+0932   TOB 369     Aka GWP 610.                                                                    
04423-2943   LDS 126     NLTT 13802/13804                                                        Chm2004 
04423-6657   OGL 220     LMC145.7.3953  + LMC145.7.4003                                          Pli2012 
04426+2516   KSA 111     Primary is variable star DP Tau.                                                
04427-2147   LDS3608     NLTT 13805/13809                                                        Chm2004 
04428-7030   OGL 221     LMC144.7.6     + LMC144.7.441                                           Pli2012 
04429+1843   LDS2266     BC: HJL1038.                                                            HJL1986 
                         RV(A)=+14.5, not Hyades member! On Lick RV program.  B is SB2,          HJL2012b
                         P=56.445d (Halbwachs et al. 2012)                                       Tok2014d
04430+5712   A  1014     Only elements P, T, and a have been amended by Starikova (1978) from    Sta1978c
                         the orbit of Baize (1958).                                              Baz1958 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.27 +/- 0.48, 2.37, and 1.10 Msun, respectively.             Mlk2012 
04431+3356   HJ  348     Also known as STF 580.                                                          
04431-0725   A   476     KP Eri, Algol-type eclipsing binary, P = 7.447126 d.                    Zas2011 
04431-6844   OGL 222     LMC148.2.7773  + LMC148.2.7774  + LMC148.2.7791                         Pli2012 
04432-5436   TOK  87     HIP 21960.                                                                      
04432-6723   OGL 223     LMC146.3.22    + LMC146.3.117                                           Pli2012 
04433+5931   A  1013     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 5.20 +/- 2.40, 3.42, and 1.82 Msun, respectively.             Mlk2012 
04434+1558   BPM 103     [PM2000]  183754 + [PM2000]  183745.                                    Gvr2010 
04436-0848   STF 590     55 Eri. B is a Delta Scuti-type variable, DW Eri., BD-09@969. Spectral          
                         type F4IIIpSr. Both components are spectroscopic binaries.                      
                         H 3  99.                                                                MEv2010 
04441+1739   LDS2268     NLTT 13828/13829.                                                               
04441+0205   HL    1     This is a measure of HL 04441+0204 and A 3006 04440+0204                        
04442-6959   OGL 224     LMC143.8.7618  + LMC143.8.8368                                          Pli2012 
04443+2017   KOH  22     V1205 Tau.                                                              Dae2015 
04444+1952   KOH  23     V1333 Tau.                                                              Dae2015 
04444+1109   BUP  68     Hyades vB 111.  A may be variable. Two CPM companions with rho = 74".7          
                         and rho = 10".0, both outside our detection window.                     Msn1993a
04445+3953   COU1524     Primary is eclipsing binary V592 Per (period 0.71572 day).              Zas2010 
04448-6946   OGL 225     LMC143.6.9637  + LMC143.6.10050                                         Pli2012 
04449+2717   KOH  24     Member of Taurus-Auriga molecular cloud.                                Dae2015 
04449+1757   LDS2271     LDS5590.                                                                        
04450+1605   BPM 104     [PM2000]  185037 + [PM2000]  185149.                                    Gvr2010 
04453-6943   OGL 226     LMC143.6.9561  + LMC143.6.9815                                          Pli2012 
04454+2955   NI   12     BVD  47.                                                                        
04454+2421   POU 477     Also known as GRV 215.                                                          
04454-5949   FIN  89     A is the Mira-type variable, T Dor.                                             
04454-7006   OGL 227     LMC143.8.7703  + LMC143.8.7822                                          Pli2012 
04455-0512   HJ   27     B is BD-05@1021.                                                                
04455-2226   DON  77     CD-22@1801.                                                                     
04455-7018   OGL 228     LMC144.3.38    + LMC144.3.177                                           Pli2012 
04458+3515   ES 2410     ALI 65.                                                                         
04459+1911   AG  311     B is BD+18@714.                                                                 
04460+1616   BPM 105     [PM2000]  185978 + [PM2000]  185928.                                    Gvr2010 
04460+1142   BUP  69     A is possibly a spectroscopic binary.                                           
04464+4221   COU2031     1985.740:  The separation of this partially resolved pair was                   
                         calculated under the assumption of zero or otherwise known magnitude            
                         difference.                                                             Tok1985 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.53 +/- 0.35, 2.85, and 1.05 Msun, respectively.             Mlk2012 
                         Combined spectroscopic/interferometric orbit. Resulting masses are              
                         1.75 +/- 0.08 and 1.32 +/- 0.08 Msun. Spectral types are estimated as           
                         G3IV and F6V.                                                           Doc2014i
04465+1528   HD  30246   Hyades vB 142.                                                          Grf1988 
                         Noted as a SB in Griffin et al. (1988).                                 Msn1993a
04465+1528   MET  42     This optical companion cannot be 989.8-d SB of Griffin.                 Grf2012b
04466+4002   BRT2206     ALI 1040.                                                                       
04468+1745   PAT  15     This pair is noted as a slow spectroscopic binary in Griffin et al.     Grf1988 
                         (1988).                                                                 Msn1993a
04468+1744   LDS1187     LDS5601.                                                                        
04468+0901   PAT  16     This pair is a spectroscopic binary with P ~ 7 yr according to Griffin  Grf1988 
                         et al. (1988).                                                          Msn1993a
                         Hyades. The 0".1 pair PAT 16 was not resolved with speckle; its                 
                         estimated period is 7 yr.                                               Tok2012a
                         The spectroscopic solution of this 2446-d pair determined by Griffin.   Grf2012b
04468-2618   VIG   6     The B component appears to be a faint background star.                  Vig2012 
04469+1700   DAE  35     DQ Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
04469-1117   JNN  28     2MASS J04465175-1116476 has a companion that has not yet been tested            
                         for common proper motion. Since the brightness and color match                  
                         expectations, the system counts as an unconfirmed binary.               Jnn2012 
04469-4630   LDS9177     Old LDS6177.                                                                    
04469-6036   GAL   6     AL Dor.                                                                         
                         Ma,Mb = 1.1029 +/- 0.0004, 1.1018 +/- 0.0005 \msun,                     GaA2019 
                         orbital parallax = 15.200 +/- 0.056 mas.                                        
             TOK 388     First resolution of HIP 22229 at 0".043, dI=1.2. The measure is                 
                         uncertain, but the elongation is confirmed with 2-ms exposure and is            
                         not seen in other observed stars, so it is not caused by vibration.             
                         This is a triple system containing an eclipsing binary AL Dor                   
                         (Algol-type) with an eccentric orbit (Bulut & Demirkan, 2007 MNRAS,             
                         378, 179). The separation implies an orbital period of the outer                
                         system ~5yr                                                             Tok2015c
04470-6954   OGL 229     LMC143.2.264   + LMC143.2.1526                                          Pli2012 
04472+2027   KU   85     Also known as STF 593.                                                          
04472+1332   LDS1188     LDS5603.                                                                        
04472-1715   ARG  11     B is BD-17@951, spectrum G2/3V.                                                 
04476+1816   PAT  17     This pair is a spectroscopic binary with P >5 yr according to Griffin   Grf1988 
                         et al. (1988).                                                          Msn1993a
                         The spectroscopic solution of this 4822-d pair determined by Griffin.   Grf2012b
04476-0534   GRE   1     IRAS 04451-0539 = PDS 11.                                               Gre1992 
04477+4014   A  1545     Primary is V593 Per, a Beta Lyr type eclipsing binary, P = 3.2437d.     Zas2012 
04477-6945   OGL 230     LMC143.3.10488 + LMC143.3.11560                                         Pli2012 
04478+3643   GAA   2     AW Per. This Cepheid is an SB with an orbital period of ~40 yr. First           
                         discovered by Miller & Preston (1964 PASP 76, 47), it took several              
                         years to derive the first orbit from radial velocity data (Evans 1989           
                         AJ 97, 1737). It is likely that this companion is itself a binary, as           
                         argued by Evans and by Evans et al. (2000 AJ 120, 407), because the             
                         magnitude difference between the Cepheid and its companion is not               
                         consistent with equal masses and predictions from evolutionary tracks.          
                         Unfortunately, Gallenne et al. (2015) note they did not have enough             
                         angular resolution and sensitivity to detect this third companion. The          
                         properties of the brightest companion were studied based on IUE                 
                         spectra by Evans (1994 ApJ 436, 273; 1995 ApJ 445, 393), who found its          
                         spectral type to be B8.3V. This is in agreement with their detection            
                         with a flux ratio f = 1.22 +/- 0.30%, i.e., a spectral type in the              
                         range B6-B9V (using d = 853 pc from a P-L relation and K = 4.63 mag     .   
                         for the Cepheid). They estimate the companion mH = 9.6 +/- 0.3 mag      .     
                         (using for the Cepheid at theirgiven phase mH = 4.84 +/- 0.01 mag from  .     
                         Monson & Pierce (2011 ApJS 193, 12). Massa & Evans (2008 MNRAS 383,             
                         139) also determined the angular separation of the component for                
                         another epoch, which will allow an estimate all the orbital elements,           
                         (see also Gallenne et al. 2013 EAS Pub. Ser. 64, 197). Gallenne et al.          
                         (2015) derived a maximum sensitivity limit at 3sigma of 0.62%, i.e.,            
                         dmH> 5.5 mag, so can therefore exclude any additional components with   .     
                         a spectral type earlier than B9V.                                       GaA2015 
                         Spectroscopic binary orbit with P = 13954d determined.                  Grf2016c
04478+2925   CHN  10     Additional notes may be found in Herbig (1962).                         Her1962 
                         DS Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
04478-3043   LDS3620     NLTT 13968/13970                                                        Chm2004 
04479+2755   KOH  26     V1337 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04479+1902   LDS3619     LDS5604.                                                                        
04480+5645   BU 1387     4 Cam.                                                                          
04480+5307   STF 587     H 4  73.                                                                MEv2010 
04480-4154   TOK 490     AD: D component is the primary of 04490-4128 RST1285.                           
04481+7810   MLR 464     Also known as TDS 148.                                                          
04483-7036   OGL 231     LMC137.8.142   + LMC137.8.140                                           Pli2012 
04485+1056   HJ  684     CD: Also known as STF 601.                                                      
04486+1748   STF 598     HJL  62.                                                                HJL1986 
04486-6648   OGL 232     LMC138.6.5554  + LMC138.6.5870                                          Pli2012 
04487+2106   HD 284787   Hyades vB 115.  This pair is a spectroscopic binary SB with P ~ 4 yr    Grf1988 
                         according to Griffin et al. (1988).                                     Msn1993a
04487-6830   OGL 233     LMC141.4.9     + LMC141.4.22                                            Pli2012 
04488+5308   STF 586     Same position, and in field of, STF 587.                                        
04488-6124   JSP  60     AC, 180deg, 8" 14th mag noted.                                          Hln1966 
04488-6902   OGL 234     LMC142.4.13828 + LMC142.4.14777                                         Pli2012 
04489-6951   OGL 235     LMC136.7.1220  + LMC136.7.2869                                          Pli2012 
04491+1408   BPM 106     [PM2000]  189268 + [PM2000]  189301.                                    Gvr2010 
04491+0513   STTA 55     B is BD+04@755.                                                                 
04492+2448   HD 283882   Hyades vB 117.  The 11.93-day SB of Griffin & Gunn (1978) is outside    Grf1978b
                         our detection window.                                                   Msn1993a
             CIA  61     Aa,Ab : M_Aa = 0.8252+/- 0.0029\msun, M_Ab = 0.7816 +/- 0.0025 \msun,           
                         pi_orb = 20.174 +/- 0.072 mas, A_dia = 0.134 mas, B_dia = 0.127 mas.    CIA2024d
04492-3505   TOK 210     The companion is close to the detection limit, but it is considered to          
                         be real. The measurement is uncertain.                                  Tok2012a
                         Retrograde motion by 5deg since resolution on 2011.78; period is about          
                         20y. Measurements are uncertain because of large dm. The "blue" color           
                         of the companion is caused by measurement error.                        Tok2013b
04492-6736   OGL 236     LMC139.2.2     + LMC139.2.1                                             Pli2012 
04492-6901   OGL 237     LMC142.4.13837 + LMC142.4.14005                                         Pli2012 
04493+3235   CHR  19     A spectroscopic binary with P = 7.05d.                                          
                         Fekel et al. (2013) derive a new spectrosopic orbit with P=7.051d and           
                         e (adopted) = 0.0. Estimated masses are 1.95 and 1.2 Msun. Differences          
                         between early DAO and more recent data suggest the possibility of a             
                         3rd component in the system. It in uncertain whether this corresponds           
                         to the never-confirmed speckle companion, however.                      Fek2013a
04493+2934   RAS  18     Magnetic star; primary is A0 silicon star. Companions A8-F0.            Ras2014 
                         LSC  31. V473 Tau.                                                              
04494+4828   JNN 265     G 81-34. Estimated age 30-300 Myr; masses 0.27 +/- 0.14 and 0.18 +/-            
                         0.09 Msun; a ~13.5 au.                                                  Jnn2014 
04497+1554   HJ 3261     96 Tau. BU  551A,BC.                                                            
04498+0658   STT 560     pi 3 Ori = 1 Ori = Tabit. Obviously an optical pair. A spectroscopic            
                         binary and possibly a variable of Delta Scuti type.                             
                         CHARA Array Limb-darkened diameter  1.526 +/- 0.004 mas,                CIA2012e
                         R =  1.323 +/- 0.004 \rsun, L =  2.822 +/-0.030 \lsun,                          
                         Teff = 6516 +/-  19 K, M = 1.283 +/- 0.006 \msun,                               
                         Age =  1.3 +/- 0.2 Gyr.                                                         
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
04499+2230   LDS9178     Old LDS6178. G085-017. See Allen et al. (2000) for information on       AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
                         NLTT 14005/13996                                                        Chm2004 
04500+2230   KOH  27     V1341 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04501+6632   STF 584     May be H 2  92.                                                         Bu_1906 
04501-6635   OGL 238     LMC138.4.30    + LMC138.4.63                                            Pli2012 
04502-0413   SLW 172     GWP 619.                                                                Tob2012b
04502-3113   B  1474     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.59 +/- 1.09, 1.93, and 0.91 Msun, respectively.             Mlk2012 
04503+0657   H 6  83     H VI 83.                                                                        
04503-4119   HJ 3697     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2013).                         USN2013a
04503-6649   OGL 239     LMC138.3.160   + LMC138.3.161   + LMC138.3.468                          Pli2012 
04504+1712   HD  30676   Hyades vB 119                                                           Grf1988 
                         This pair is noted as a SB in Griffin et al. (1988).                    Msn1993a
04504+1712   CIA  64     M_A = 1.262 +/- 0.042 \msun, M_B = 0.822 +/- 0.016 \msun,                       
                         pi_orb = 23.16 +/- 0.22 mas, A_dia = 0.156 mas, B_dia = 0.126 mas.      CIA2024d
04505+0103   A  2622     A premature orbit has been computed.                                            
04505-3834   GC 5916     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
04506+1505   CHR  20     Hyad (vB 120). Preliminary circular orbit, speckle/spectroscopic                
                         orbit needed, cf. Griffin et al. (1988).                                Grf1988 
                         1991.9023: This may be the spectroscopic system found by Griffin et             
                         al., but more observations are needed to determine the orbital motion.  Msn1993a
                         New spectroscopic solution determined by Griffin.                       Grf2012b
                         This is a Hyades binary for which Griffin (2012) published an SB2       Grf2012b
                         orbit. We combined his RVs with the speckle data, resulting in a very           
                         accurate period. The combined orbit corresponds to a mass sum of 2.1            
                         Msun and an orbital parallax of 22mas, in good agreement with the HIP2          
                         parallax of 23.69 +/- 0.87mas.                                          Tok2015c
                         Orbital parallax is 21.30 +/- 0.75 mas. Mass of the primary is                  
                         1.129 +/- 0.169 \msun. Mass of the secondary is 1.090 +/- 0.160 \msun.  Doc2018h
                         M1    = 1.065 +/- 0.018 \msun,   M2 = 1.008 +/- 0.016 \msun,                    
                         R1    = 0.968 +/- 0.012 \rsun,   R2 = 0.878 +/- 0.013 \rsun,                    
                         Teff1 = 5656  +/- 56 K,        Teff2 = 5489 +/- 60 K,                           
                         orbital parallax = 21.86 +/- 0.15 mas.                                  Trr2024 
04506-6711   OGL 240     LMC139.4.89    + LMC139.4.1334                                          Pli2012 
04507-4540   HJ 3699     old LDS6179.                                                                    
04508+1613   HD  30738   Hyades vB 121                                                                   
                         The 5.751-day SB of Griffin & Gunn (1978) is outside our detection      Grf1978b
                         window.                                                                 Msn1993a
04508-4013   I  1492     Variable, Y Cae.                                                                
04509+3746   TOK 249     Cmp? Crowded field (N*=81), small PM, hence B can be optical.           Tok2014d
04509-5328   DUN  18     iot Pic                                                                         
             SHY 172     AC: HIP  22531 + HIP  22562.                                                    
             SHY 173     BC: HIP  22534 + HIP  22562.                                                    
                         In addition to the three visual components, which are physical, the A   Tok2020h
                         component has two spectroscopic components with periods of 1.6d and             
                         1003d. The B component also has a spectroscopic component with a period         
                         of 208d making this a physical sextuple. The AB visual pair has an              
                         estimated period of 6k yr and the wide AB,C pair has an estimated               
                         period of 600k years.                                                           
04511-2731   TOK  88     HIP 22538. The original Hipparcos gives parallax 13.9 mas. A is X-ray           
                         source 1RXS J045103.5-273115.                                           Tok2011a
04512+1104   BU  883     Hyad (vB 122).                                                                  
                         Mass-sum calls for sp subsystem, but RV-ampl <1km/s according to                
                         Griffin et al. (1988).                                                  Grf1988 
                         AO photometric analysis by ten Brummelaar et al. (2000) includes mass           
                         determination.                                                          TtB2000 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.58 +/- 0.49, 2.36, and 2.24 Msun, respectively.  Mlk2012 
                         Argument of periastron flipped for Sod1999 orbit since WDS refers to            
                         fainter star as primary.                                                        
                         AB,C: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB,C: Rectilinear solution by Hurowitz et al. (2013).                   USN2013a
04512-2213   BRT1378     CD-22@1851.                                                                     
04512-6843   OGL 241     LMC134.7.16981 + LMC134.7.17012                                         Pli2012 
04513-3040   BRT2856     A likely plate flaw.                                                    Grv2021b
04513-6804   FIN 362     Only one observation, with many negative results. Duplicity                     
                         questionable. Needs speckle.                                                    
04514+1850   BUP  70     97 Tau = LDS1190. A is a Delta Scuti-type variable, V480 Tau.                   
                         B is BD+18@742.                                                                 
04515+5550   LDS5615     relative motion of AB is 0.1"/yr, too fast. optical?                    Tok2014d
04515-3454   FIN 320     Appears to have completed a revolution if the quadrants are correct.            
                         Period about 40y.                                                               
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.50 +/- 1.29, 3.59, and 2.19 Msun, respectively.             Mlk2012 
                         Docobo & Andrade (2013) derive a dynamical parallax of 13.78 +/- 0.41           
                         mas and component masses 1.85 +/- 0.21 and 1.58 +/- 0.18 Msun. See              
                         paper for extensive notes on this system.                               Doc2013d
04515-6653   OGL 242     LMC138.3.7274  + LMC138.3.7555                                          Pli2012 
04515-6933   OGL 243     LMC136.5.13108 + LMC136.5.13830                                         Pli2012 
04516-6841   OGL 244     LMC134.7.20843 + LMC134.7.21738                                         Pli2012 
04518+3047   JOY   4     A is the RW Aur-type variable, UY Aur.                                  Her1962 
                         Hioki et al. (2007) calculate a period of 1640 +/- 90 yr and a total    Hio2007 
                         mass of 1.73 +/- 0.29 Msun.                                                     
04518+1339   BU  552     Hyad (vB 124).                                                          Wor1963a
                         The primary is 143d SB (Griffin et al. 1985).                           Grf1985b
                         The spectroscopic system of Griffin et al. would be too close for us            
                         to resolve by speckle interferometry.                                   Msn1993a
                         A: Ren & Fu (2013) calculated an astrometric orbit, combining                   
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Turner et al. (1986). They derived component masses 1.42 and 0.55 Msun  TrD1986 
                         and an estimated semimajor axis of 15.67 mas.                           Ren2013 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.67 +/- 1.47, 2.30, and 1.00 Msun, respectively.  Mlk2012 
                         A faint component (about mag. 13, 45") is unobserved since 1906; its            
                         physical nature is unknown.                                                     
04519-3414   BVD  48     AC: SHY 470. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
04519-6058   JSP  62     CD-61@974.                                                                      
04519-6635   OGL 245     LMC138.4.6967  + LMC138.4.6968                                          Pli2012 
04521-6706   OGL 246     LMC138.1.8041  + LMC138.1.8261                                          Pli2012 
04525-3631   LDS9180     Old LDS6180.                                                                    
04526+4302   ES 1526     BC: BRT 111                                                                     
04526-2646   LDS3625     NLTT 14126/14125                                                        Chm2004 
04527-2546   TOK 662     With plx(A), B is on the MS, likely physical.                           Tok2014d
04527-6936   OGL 247     LMC136.4.307   + LMC136.4.140                                           Pli2012 
04527-7043   OGL 248     LMC137.1.262   + LMC137.1.650                                           Pli2012 
04531-0117   S   457     B is BD-01@743.                                                                 
04531-0853   BRT 369     A likely plate flaw.                                                    Grv2021b
04533+1401   BPM 107     [PM2000]  194282 + [PM2000]  194455.                                    Gvr2010 
04534-0925   RST4256     BRT 2834.                                                                       
04535-5551   LDS 131     See note to 05287-6527 SHY  27AD.                                               
04537-4539   GRV1249     Both A and B have approximately the same radial velocity.               Grv2019b
04538-6831   OGL 249     LMC134.3.20577 + LMC134.3.20575                                         Pli2012 
04540-6943   OGL 250     LMC136.3.223   + LMC136.3.524                                           Pli2012 
04540-7022   OGL 251     LMC137.3.14145 + LMC137.3.18362                                         Pli2012 
04541+8125   MLR 490     Also known as TDS 152.                                                          
04541+6621   alp Cam     Fullerton (1990) presents high quality profiles that indicate the       Ful1990 
                         presence of line profile variations; his associated radial velocity             
                         measurements do not confirm any of the periods suggested by Zeinalov &          
                         Musaev (1986 SvAL 12, 125) and Musaev & Snezhko (1988 SvAL 14, 68).     Msn1998a
04542+4935   STF 603     AB: H N  77.                                                            MEv2010 
04543+0722   STF 612     HD 31208. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AB: HJL  64.                                                            HJL1986 
04544-6720   OGL 252     LMC132.6.11391 + LMC132.6.12002                                         Pli2012 
04545-0314   RST5501     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.79 +/- 1.45, 3.77, and 1.20 Msun, respectively.             Mlk2012 
04547+1221   TOK 251     A is exoplanet host, P=466d. RV(A)=+12.1, not Hyades                    Tok2014d
04547-0257   J  1348     GCB 7. BRT 370.                                                                 
04548+1126   MCA  17     6 Ori.                                                                          
04549+1009   ENG  19     7 Ori = pi 1 Ori. B is BD+09@682.                                               
04549+0836   STT  90     V1834 Ori, Algol-type eclipsing binary, P = 1.51058 d.                  Zas2011 
04549-6934   OGL 253     LMC136.4.18656 + LMC136.4.18660                                         Pli2012 
04550+3411   HJ  351     AB: Rectilinear solution by Friedman et al. (2011).                     USN2011a
04551+5516   BU 1187     5 Cam.                                                                          
04551+3535   MLB 923     Not found by Heintz at IDS position.                                    Hei1985a
04551-6718   OGL 254     LMC132.4.88    + LMC132.4.1271                                          Pli2012 
04552+1827   DAE  39     V1349 Tau.                                                              Dae2015 
04552-6656   OGL 255     LMC131.7.14509 + LMC131.7.14673                                         Pli2012 
04552-6908   OGL 256     LMC135.3.30074 + LMC135.3.30071                                         Pli2012 
04552-7923   HJ 3733     B is CPD-79@163.                                                                
04554-7109   OGL 257     LMC130.7.31    + LMC130.7.349   + LMC130.7.1118                         Pli2012 
04555+1711   BPM 108     [PM2000]  197155 + [PM2000]  197180.                                    Gvr2010 
04556+3018   MSR   3     HBC 426 = V396 Aur.                                                     Msr2005 
04556+1653   HJ 3263     Rectilinear solutions by Cvetkovic (2015)                               Cve2015b
                         and Cvetkovic et al. (2016).                                            Cve2016 
04557+1742   DAE  40     V1350 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04557-6637   OGL 258     LMC131.4.8     + LMC131.4.7                                             Pli2012 
04558+3033   BNS   1     HBC 78 = MWC 93 = AB Aur                                                        
04558-3100   LDS3628     NLTT 14212/14213                                                        Chm2004 
04558-6741   OGL 259     LMC132.1.137   + LMC132.1.297                                           Pli2012 
04558-7056   OGL 260     LMC130.6.29    + LMC130.6.186                                           Pli2012 
04559+0440   LDS9181     Old LDS6181.                                                                    
             EGN   4     Aa,Ab pair bound. Ab component is likely an early M dwarf with mass             
                         0.43 +/- 0.02 Msun                                                      Egn2007 
                         Aa,Ab: A is on Keck program, RV var.                                    Tok2014d
04560+3021   SFN   1     Aa,Ab: Steffen (2000, 2001) combined solutions each yield values for    Sfn2000 
                         the masses, as well as an orbital parallax.                             Sfn2001 
                         Simon et al. (2013) derive masses 0.86 +/- 0.11 and 0.55 +/- 0.05 Msun          
                         and distance 187.7 +/- 3.9 pc for this pre-MS binary.                   Smn2013 
             KSA  31     HBC 427 = V397 Aur.                                                     Msr2005 
04560-6938   OGL 261     LMC128.5.315   + LMC128.5.772                                           Pli2012 
04560-7040   OGL 262     LMC129.8.308   + LMC129.8.309                                           Pli2012 
04561-7116   OGL 263     LMC130.8.10926 + LMC130.8.11364                                         Pli2012 
04562+2554   GIC  52     G039-042/G039-041.                                                              
                         NLTT 14180/14179                                                        Chm2004 
04563+5206   STF 608     AB,C: HJL  65.                                                          HJL1986 
04563+2415   LDS6148     Also known as GRV 220.                                                          
04564+1331   BU  553     omi 2 Ori = 9 Ori                                                               
04564-0510   SHJ  48     62 Eri. B is BD-05@1093.                                                        
                         AB: H 6 106.                                                            MEv2010 
04566+0422   TOB9004     Measured as BAL2622 but actually an anonymous pair added here.          Tob2012c
04566-6629   DON  89     Variable.                                                                       
04566-7027   OGL 264     LMC129.7.22    + LMC129.7.188                                           Pli2012 
04567+3917   HU 1091     V560 Aur, Algol-type eclipsing binary, P = 1.528311 d.                  Zas2011 
04567-7106   OGL 265     LMC130.7.12419 + LMC130.7.12474                                         Pli2012 
04568+1825   BPM 109     [PM2000]  199012 + [PM2000]  199066.                                    Gvr2010 
04569-6721   OGL 266     LMC132.3.14233 + LMC132.3.14300                                         Pli2012 
04570+1716   BPMA  9     [PM2000]  199271 + [PM2000]  199591.                                    Gvr2010 
04570+1517   MET   4     Metchev & Hillenbrand say the C component is probably optical, based            
                         on proximity.                                                           Met2004b
04572+3838   ES 2338     ALI 780.                                                                        
04573+5345   D     5     7 Cam. A premature orbit has been computed for AB. The primary is SB1,          
                         P = 3.884 d (Lucy & Sweeney).                                           Lcy1971 
                         Drummond linear elements have been modified.                            Dru2014 
             STF 610     AB,C: Star C (mag. about 11.3, 26") may be physical.                            
             D     5     AB: Rectilinear solution by Drummond (2014).                            Dru2014 
04573+1524   HEI  38     KOH  36.                                                                        
                         Young member of Taurus-Auriga molecular cloud.                          Dae2015 
04573-7055   OGL 267     LMC130.6.14234 + LMC130.6.16118                                         Pli2012 
04574+0100   A  2624     Aa,Ab : Hipparcos identified the pair as a candidate for Hyades         HIP1998 
                         membership. However, it is not.                                         Grf1988 
                                                                                                 Grf2013c
04574+0100   SHY 471     AB: HIP  23044 + HIP  23266. B component = A component of 05003+0100.           
04575-2358   LDS3630     NLTT 14263/14262                                                        Chm2004 
04576+1356   BPM 110     [PM2000]  200066 + [PM2000]  200068.                                    Gvr2010 
04576+0344   BAL2132     A likely plate flaw.                                                    Grv2021b
04576-0545   STF 624     B is BD-05@1103.                                                                
04576-6950   OGL 268     LMC128.6.11701 + LMC128.6.11986                                         Pli2012 
04578+2357   BU 1045     99 Tau.                                                                         
04580-2248   I   473     CD-22@1917.                                                                     
04580-6735   OGL 269     LMC124.7.79    + LMC132.2.17928                                         Pli2012 
04581+0141   STF 622     A,BC: H 1  68.                                                          MEv2010 
04582+8015   OSO  18     GD 288. Not a common proper motion pair, based on comparison with               
                         POSS2 red plates                                                        Oso2004 
04582+2503   BU 1390     98 Tau. A is a spectroscopic binary.                                            
04582+1423   BPM 111     [PM2000]  201029 + [PM2000]  201109.                                    Gvr2010 
04583+0027   FR   11     V1198 Ori.                                                                      
04584-6739   OGL 270     LMC124.8.20199 + LMC124.8.20752                                         Pli2012 
04585-2749   RST 117     CPD-28@715.                                                                     
04585-6834   OGL 271     LMC126.6.46772 + LMC126.6.46857                                         Pli2012 
04587-7053   OGL 272     LMC130.3.25    + LMC130.3.4226                                          Pli2012 
04588-7027   OGL 273     LMC129.2.10    + LMC129.7.17168                                         Pli2012 
04589+6435   GNO   1     Distance is estimated at about 10.5 +/- 1.4 pc, giving a projected              
                         component separation of ~5 au. Estimated orbital period ~70 yr, for an          
                         assumed age of 1 Gyr.  Spectral types are estimates at T8.5 and T9;             
                         total system mass ~25 Mjup.                                             Gno2011 
04590+1433   SHJ  49     STTA 58 = H 5 113. B is BD+14@795. Probably same as BDS 2461, H V 57.           
                         AB: H 5  57.                                                            MEv2010 
04590-1623   BU  314     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.87 +/- 0.28, 2.66, and 2.36 Msun, respectively.  Mlk2012 
                         AB,C: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB,C: Rectilinear solution by Hurowitz et al. (2013).                   USN2013a
04591+6322   HU 1090     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 12.31 +/- 4.18, 2.27, and 1.10 Msun, respectively.            Mlk2012 
04591+1123   BPM 112     [PM2000]  202364 + [PM2000]  202525.                                    Gvr2010 
04593+3753   STF 616     ome Aur = 4 Aur                                                                 
                         AB: H 2  14.                                                            MEv2010 
04595-4927   HJ 3715     Primary is VW Pic, a W UMa type eclipsing binary, P = 0.42576d.         Zas2012 
04595-6802   OGL 274     LMC125.6.10758 + LMC125.6.10639                                         Pli2012 
04595-6958   OGL 275     LMC128.2.17    + LMC128.2.402                                           Pli2012 
04596+3135   HO  222     Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
                         However, radial velocity classifies this as not a Hyades member.        Grf2013c
                         The colors from Tycho photometry are also not consistent with a         Fab2000a
                         physical pair.                                                                  
04597+1555   BUP  73     Hyades vB 128                                                                   
                         A CPM companion with rho = 106".4 is outside our detection window.      Msn1993a
04597-6940   OGL 276     LMC128.4.12    + LMC128.4.92                                            Pli2012 
04598-1016   63 Eri      Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Vennes et al. (1998).                                                   Ven1998 
04599+5327   A  1303     A premature orbit has been computed.                                            
                         T corrected from 200.74 to 2000.74 by Ruymaekers & Nys (1995)           Ruy1995 
04599+0031   J    47     Despite having an orbit, an optical pair based on parallax and proper   Mlk2022 
                         motion.                                                                 Izm2019 
05001-6217   B  1942     Composite spectrum: G5/8III + F/G.                                              
05001-6953   OGL 277     LMC128.2.32346 + LMC128.2.32381                                         Pli2012 
05002+1811   GIC  53     LDS1198. G083-047/G083-048.                                                     
05003+3924   CHR 159     5 Aur.                                                                          
05004+6925   STF 606     B is BD+69@289.                                                                 
05005+0506   STT  93     Hyperbolic orbit by Janova (1966).                                      Jnv1966 
                         sigma = areal constant in the true orbit = 0.00576 arcsec^2/yr                  
                         q = periastron distance in the true orbit = 0".366                              
05006+0337   STF 627     B is BD+03@736.                                                                 
05007-0204   VIG   7     Optical/physical nature of the six faint companions (B-G) is undefined. Vig2012 
05007-6856   SKF1044     OGL 278. LMC126.1.9 + LMC126.1.100                                      Pli2012 
05008+3913   STF 621     Same as AG   83.                                                                
05008+3811   SEI  52     Secondary not seen on POSS plate; may be either variable star or flaw           
                         on AC Potsdam plate.                                                            
05009-7052   OGL 279     LMC130.4.19979 + LMC130.4.21083                                         Pli2012 
05010-0818   BRT 372     A likely plate flaw.                                                    Grv2021b
05010-6948   OGL 280     LMC128.3.14335 + LMC128.3.14552                                         Pli2012 
05012+3430   COU1229     Primary is V410 Aur, a W UMa type eclipsing binary, P = 0.36636d.       Zas2012 
05013+5015   STF 619     Rectilinear solution by Scardia et al. (2017).                          Sca2017c
                         Very different proper motion. Despite having an orbit,                  Kis2009 
                         an optical pair based on parallax.                                      Mlk2022 
05015+3733   BRT2207     ALI 523.                                                                        
05015-7107   OGL 281     LMC122.7.267   + LMC122.7.1784                                          Pli2012 
05016+6105   HU 1093     Primary is possible astrometric pair?                                   Tok2014d
05016-7056   OGL 282     LMC122.6.146   + LMC122.6.918                                           Pli2012 
05017+2640   A  1844     Masses and bolometric magnitudes are derived for the two components     Msn1999a
                         of this system by Maosn et al. (1999), based on assumed spectral types          
                         and available parallaxes.                                                       
                         Visual separations systematically too small.                                    
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.83 +/- 0.31, 2.12, and 1.00 Msun, respectively.  Mlk2012 
             S   461     STTA 59 = STFA 12.                                                              
             BAG  21     Ca,Cb: SB2, P=186.28d                                                   Tok2014d
05017+2050   HU  445     Quadrant uncertain, Delta m at least 0.3.                               B__1963b
                         Only elements P and T have been amended by Starikova (1977) from the    Sta1977a
                         orbit of Baize (1957).                                                  Baz1957a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 0.15 +/- 0.04, 1.78, and 1.05 Msun, respectively.             Mlk2012 
05019-7638   RST2368     Rectilinear solution by Hartkopf et al.  (2012).                        Hrt2012a
05020+4349   BU  554     AB: eps Aur = 7 Aur = Almaaz. Strand orbit rejected from Fourth Orbit   Str1959 
                         Catalog ("amplitude below noise level")                                 Wor1983 
                         Mk III Limb-darkened diameter  2.17  +/- 0.03  mas.                     MkT2001 
                         Mk III Limb-darkened diameter  2.096 +/- 0.086 mas.                     MkT2003 
                         NPOI Limb-darkened diameter    2.28  +/- 0.09  mas.                     NOI2001b
                         NPOI Limb-darkened diameter  2.210 +/- 0.012 mas, Sp = A2I,             NOI2018 
                         Teff = 7977 +/-292 K, M = 2.16 +/- 0.39 \msun, Age = 0.62 +/- 0.22 Gyr.         
             eps Aur     A is a enigmatic supergiant eclipsing system. Also a spectroscopic and          
                         eclipsing binary                                                        Fin1970b
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Heintz & Cantor (1994).                                                 Hei1994b
05020+0137   STF 630     A,BC: H 3  52.                                                          MEv2010 
05021+6910   BU  313     The AB component, BU 313 AB, originally in the BDS and IDS, was                 
                         removed by Worley following multiple unresolved observations. The new           
                         Hipparcos binary (AB), is almost certainly not the Burnham AB star,             
                         which was seen at 10", 250 deg, and had a Delta-M of 5.0.                       
                         AC: Burnham (BDS) notes 1874 observation made with 6-in telescope but           
                         says no 10" companion was found during subsequent searches with either          
                         the 36-inch or 40-inch.                                                 Bu_1906 
05022+3116   RUC   5     V402 Aur. Spectral type of resolved companion later than M5V.           Ruc2007 
05023-1932   LPM 201     NLTT 14407/14408                                                        Chm2004 
05023-5605   LDS 135     B is CPD-56@767.                                                                
                         Primary is SB1; Jenkins et al. (2010 A&A 515, 17) estimate P(Aa,Ab)             
                         ~6.5y, M2min=55 Mjup.                                                   Tok2014d
05023-6821   OGL 283     LMC125.1.12039 + LMC125.1.12040                                         Pli2012 
05024+1628   BPM 113     [PM2000]  207217 + [PM2000]  207230.                                    Gvr2010 
05024-6454   GLI  32     B is CPD-65@416.                                                                
05025+4105   MKT   6     zet Aur = Saclateni. The first of the zeta Aurigae-type binaries (K4IB          
                         + B5V). This object was misidentified as rho Aur by McAlister (1978).   McA1978c
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Wright (1970).                                                          Wri1970 
                         Bennett et al. (1996) orbit is combined solution, using astrometry      MkT1996 
                         from the Mark III interferometer, spectroscopy from HST Goddard High            
                         Resolution Spectrograph, and published photometry to determine masses,          
                         radii, etc. Positions of component stars on theoretical H-R diagram             
                         are compared to current evolutionary models.                                    
                         Errors to individual measures are given as "error ellipses"; these              
                         values are tabulated below, together with filters used. The columns             
                         include date (BY), major and minor axes of the ellipse (in mas),                
                         ellipse orientation (deg), and filter effective wavelengths (nm):               
                              1989.7857   1.63    0.31    98.1   800,550,450                             
                              1989.7994   0.56    0.14    86.9   800,550,450                             
                              1989.8213   0.58    0.12    84.5   800,550,450                             
                              1989.8240   0.73    0.15    78.6   800,550,450                             
                              1989.8350   0.50    0.12    85.3   800,550,450                             
                              1989.9281   0.48    0.17    96.1   800,550,450                             
                              1989.9363   1.24    0.27    86.1   800,550,450                             
                              1990.7029   1.14    0.16   104.0   800,550,500                             
                              1990.8124   0.56    0.17    97.5   800,550,500                             
                              1990.8179   0.69    0.14    91.7   800,550,500                             
                              1991.7488   2.00    0.20   111.9   800,550,500                             
                              1991.7871   0.65    0.12    92.4   800,550,500                             
                              1991.8364   0.32    0.09    94.1   800,550,500                             
                              1991.9048   0.21    0.07    86.4   800,550,500                             
                              1992.0855   1.31    0.15    90.4   800,550,500                             
                              1992.0965   1.50    0.25    73.5   800,550,500                             
                              1992.7700   0.63    0.14    99.5   800,550,500                             
                              1992.7946   0.65    0.11    98.5   800,550,500                             
                              1992.7974   0.44    0.08   104.2   800,550,500                             
                              1992.8932   1.82    0.24   111.3   800,550,500                             
                              1992.9206   1.39    0.27    99.0   800,550,500                             
                              1992.9452   1.23   0.23    101.9   800,550,500                             
                         Malkov et al. (2012) derive dynamical and spectroscopic masses                  
                         8.40 +/- 3.79 and 10.96 Msun, respectively.                             Mlk2012 
05025-2115   DON  91     Good period, indeterminate a/e/i, more obs needed!                      Hei1978c
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
05027-3309   HJ 3718     B is CD-33@2076.                                                                
05028-4909   RST 120     AB: Physical/optical nature undefined.  Primary is eta 1 Pic.           Ehr2010 
             EHR   6     AC: Physical/optical nature undefined.                                  Ehr2010 
05028-7020   OGL 284     LMC121.6.34935 + LMC121.6.34941                                         Pli2012 
05029+1433   BPM 114     [PM2000]  208075 + [PM2000]  208110.                                    Gvr2010 
05031+4933   BU  315     ID uncertain. Listed as BD+49 1288 in ADS, but no obvious 10" pair at   A__1932a
                         those coordinates. X-coded measures of a 45" pair refer to a wide               
                         companion to BD+49 1288.                                                        
05031+2523   MSR   5     HBC 429 = V836 Tau.                                                     Msr2005 
                         Young member of Taurus-Auriga molecular cloud.                          Dae2015 
05031+2135   OCC 230     iot Tau.                                                                        
05031-6944   OGL 285     LMC120.6.45262 + LMC120.6.45347                                         Pli2012 
05033+2125   LAW  13     Ba,Bb: LSPM J0503+2122 = NLTT 14406. Law et al (2008) derive a          Law2008 
                         distance of 13.7 +6.5/-2.5 pc and a projected separation of                     
                         4.4 +2.3/-0.7 au. Estimated spectral types are M4.5 and M5.5.                   
                         Ba,Bb: LP 359-186. Estimated age 1000-10000 Myr; masses 0.38 +/- 0.03           
                         and 0.16 +/- 0.01 Msun; a ~8.3 au.                                      Jnn2014 
05033-1722   B  2583     LPM 202. L 736-49.                                                              
05034+6027   S   459     bet Cam = 10 Cam. STTA 57 = H 6  36.                                            
05034-7104   OGL 286     LMC122.7.14740 + LMC122.7.14741                                         Pli2012 
05035+1449   BPM 115     [PM2000]  209034 + [PM2000]  208947.                                    Gvr2010 
05036+6305   STF 618     LDS 889. STTA 56. D is BD+62@721.                                               
                         AB: HJL  66.                                                            HJL1986 
05037-0232   J   307     Reality of BC is in doubt.                                                      
05037-6834   OGL 287     LMC118.6.42400 + LMC118.6.42472                                         Pli2012 
05038+1457   BPM 116     [PM2000]  209491 + [PM2000]  209477.                                    Gvr2010 
05039-6738   OGL 288     LMC124.1.32825 + LMC124.1.32850                                         Pli2012 
05042-6956   OGL 289     LMC120.7.16863 + LMC120.7.18028                                         Pli2012 
05043+4013   ES 1718     Espin incorrectly identified this pair as BD+40 1144 in 1919, but       Es_1919 
                         corrected this to +40 1158 in 1925. Error in transcribing to catalog;   Es_1925a
                         WDS designation originally 05041+4023 = VIG   7, corrected when                 
                         matched with 05043+4013TDS3056.                                                 
05043+2319   J  1816     POU 523.                                                                        
05043-6946   OGL 290     LMC120.6.17556 + LMC120.6.17583                                         Pli2012 
05044+6237   HU 1094     Stein measure 1901.3, 289@, 4.2", 9.5-9.9. For this position            A__1932a
                         Hussey finds no such pair.                                              Hu_1905b
05044-3529   JC    9     gam 1 Cae. The secondary is variable (IBVS 2736, 1985).                         
05044-6706   OGL 291     LMC115.8.111   + LMC115.8.177                                           Pli2012 
05045+1622   BPM 117     [PM2000]  210663 + [PM2000]  210510.                                    Gvr2010 
05045-2402   LDS3638     NLTT 14472/14466                                                        Chm2004 
05046+5852   STF 625     A,BC: H 2  53.                                                          MEv2010 
05047+7404   STT  89     Judged single by Hussey, Burnham, and Aitken, and not inserted in ADS.          
                         Rediscovered by Kuiper in 1935 (PASP 47, 230). Obvious in 1938.         Baz1942b
05047-0925   GAL 375     Object #161 in Gallo's original list.                                   Gal1914 
05047-2017   WHC   2     CPD-20@742.                                                                     
05049+1520   BPMA 10     [PM2000]  211239 + [PM2000]  211233.                                    Gvr2010 
05050-6740   OGL 292     LMC116.8.65    + LMC116.8.164                                           Pli2012 
05051+0608   HD 32662    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
05053+6923   HJ 2244     B is BD+69@295.                                                                 
05054-6905   SKF1072     OGL 293. LMC119.5.40836 + LMC119.5.40603                                Pli2012 
05055-5728   SHY  22     HIP  23693 + HIP  23708.                                                        
05056+2304   STT  97     See long note in BDS. Single in 1889.                                   Bu_1906 
                         Recovered in 1976 by McAlister.                                         McA1978b
                         Primary is V1154 Tau, an Algol-type eclipsing binary, period 1.76788d.  Zas2011 
05056-7056   OGL 294     LMC122.3.16    + LMC122.3.89                                            Pli2012 
05057+0628   PAT  18     This pair is a spectroscopic binary with P ~ 2 yr, according to         Grf1988 
                         Griffin et al. (1988).                                                  Msn1993a
                         The spectroscopic solution of this 631.08-d pair determined by          Grf2012b
                         appears to be a closer pair.                                                    
                         Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
                         It appears to match on grounds of proper motion and photometry but      Grf1988 
                         still appears slightly off based on radial velocities.                  Grf2013c
05061+5858   STFA 13     A: 11 Cam. B: 12 Cam =  BD+58@805. B is a spectroscopic binary,                 
                         P = 80.2d, spectrum K0III.                                                      
05062-6247   TOK  91     HIP 23742. ANDICAM confirms the 2MASS PSC photometry of B in K-band.            
                         B is well below the MS in the CMDs.                                     Tok2011a
05063+3738   ES 2339     Aka BRT2587 and ALI 528.                                                        
05063+3722   SEI  60     ALI 527.                                                                        
05064-1649   GAL 376     Object #164 in Gallo's original list. Aka POC9001.                      Gal1914 
05064-6700   OGL 295     LMC115.7.14821 + LMC115.7.14818                                         Pli2012 
05065+5521   KRV  28     Classical Cepheid CK Cam.                                                       
05066+0152   HJ 2250     Rectilinear solution by Hartkopf & Mason (2015).                        WSI2015 
05066-6830   OGL 296     LMC118.4.12    + LMC118.4.529                                           Pli2012 
05067+5136   BU 1046     9 Aur. A is a spectroscopic binary.                                             
             H 6  35     AC: H VI 35.                                                                    
05067+3748   SEI  61     ALI 529.                                                                        
05067+1427   GC 6239     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
                         Spectroscopic solution to these astrometric pairs given by Griffin      Grf2013a
                         (2013). Periods match "tolerably well," other common elements less so.          
05067-6725   OGL 297     LMC116.6.12552 + LMC116.6.14377                                         Pli2012 
05068-0439   STF 642     66 Eri. A is a spectroscopic binary.                                            
05069-6718   OGL 298     LMC116.5.13203 + LMC116.5.16702                                         Pli2012 
05069-6728   OGL 299     LMC116.6.12514 + LMC116.6.14626                                         Pli2012 
05070+1650   HJ 3267     LDS1199. Possibly the same as STF 672.                                          
05070-3939   HJ 3725     B is CD-39@1789.                                                                
05071-7042   OGL 300     LMC121.1.12614 + LMC121.1.12789                                         Pli2012 
05074+2715   DOO  30     J 3259.                                                                         
05074+1839   A  3010     104 Tau.                                                                        
                         Two orbit solutions (Eggen 1956). Observations of this close pair       Egg1956 
                         are so scattered that both orbits are highly conjectural.                       
                         A measure on 1977.9196 was incorrectly attributed to ADS 3701 in                
                         McAlister & Hendry (1982); it actually belongs to ADS 4020.             McA1982b
                         Visual and speckle observations at 0".1 sep ruled out as spurious by            
                         constant RV (Duquennoy & Mayor 1991).                                   Duq1991 
                         Precise velocities are stable to better than 100 m/s over 388 days,     Nid2002 
                         so there are no "hot jupiters" and a 2-year period is excluded with     Tok2010b
                         high confidence.                                                                
                         104 Tau is a G4V dwarf at 16 pc resolved into equal components at 0.1"          
                         by R. Aitken in 1912. The WDS contains 16 resolutions of this pair.     A__1927a
                         Apart from Aitken himself, it has been resolved on multiple occasions           
                         by R.H. Wilson in 1934-1971, by W. Finsen (1953-1955) and by others,    WRH1941a
                         although in other instances those observers found it to be single.      Fin1953d
                         The measures suggest a near-circular orbit seen face-on with a semi-            
                         major axis on the order of 0.1" or 1.5 au. Assuming a mass sum of 2             
                         Msun, the orbital period should be around 1.3 yr; in fact, two orbits           
                         with periods 1.19 yr and 2.38 yr were published by Eggen (1956). This   Egg1956 
                         binary should be an easy target for speckle interferometry at 4-m               
                         telescopes. It was observed 10 times from 1976.9 to 1980.7 with                 
                         speckle and, surprisingly, found unresolved on all occasions,                   
                         excluding any short-period orbits. Later, however, two measures were            
                         made by the author at a 1-m telescope with a phase-grating                      
                         interferometer. The first resolution in 1984.8 at 0.04" was tentative   Tok1985 
                         (below the diffraction limit), but the second in 1985.7 was secure,     Tok1988 
                         being an average of two observations. It was followed by the speckle            
                         resolution at 4-m telescope in 1988.17, after which the pair            Mca1993 
                         disappeared again. It was found unresolved in 2012.                     Tok2012b
                         The star is well studied. Two statistical surveys of binaries within            
                         25 pc consider it to be single (Duquennoy & Mayor 1991; Raghavan et     Duq1991 
                         al. 2010). Heintz & Borgman (1984) state that measures cannot be        Rag2010 
                         fitted by any orbit and conclude: "Although this alleged visual binary  Hei1984i
                         (ADS 3701) has three published orbits, it is probably spurious".                
                         Several independent RV studies have shown that this star is not a               
                         spectroscopic binary. Precise RVs measured by Nidever et al. (2002)     Nid2002 
                         are stable to better than 100 m s-1 over 388 days, excluding orbital            
                         periods from one to two years with high confidence. Data with lower             
                         precision show a constant RV of +21 km/s over many years (Duquennoy &           
                         Mayor 1991; Abt & Willmarth 2006; Raghavan et al. 2010). The star is    AbH2006 
                         located about 1m above the main sequence, supporting the thesis of an           
                         equal-component binary. If the orbit is seen face-on, the RV variation          
                         would be small, especially if the components are of equal brightness            
                         (blended lines move in opposite directions, the centroid stays                  
                         constant). However, the lines in this star remain narrow and the                
                         speckle non-resolution during 3.8 yr firmly excludes a face-on orbit.           
                         Remember that 104 Tau is bright (no identification errors possible)             
                         and that the components are supposedly equally bright, hence easy to            
                         resolve by speckle. If this star is single (as everything seems to              
                         suggest), we cannot dismiss its multiple resolutions with micrometer,           
                         eyepiece interferometer, and speckle as spurious; occasional image              
                         doubling (or at least elongation) must be real.                         Tok2012b
                         Ghost binary.                                                           Tok2012b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 0.65 +/- 0.09, 2.12, and 1.02 Msun, respectively.             Mlk2012 
                         In the WDS summary line this carries an "X" code (non double), but              
                         still retains all the historical measures.                                      
05074-6641   OGL 301     LMC115.4.42    + LMC115.4.508                                           Pli2012 
05076+1631   BPM 118     [PM2000]  215983 + [PM2000]  215874.                                    Gvr2010 
05076+0928   STT 561     AB: 16 Ori. A is a spectroscopic binary.                                        
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
05076-7018   OGL 302     LMC121.3.45664 + LMC121.2.45533                                         Pli2012 
05076-8852   HJ 4047     1900: 06 56.4.                                                                  
05078+3024   JOY   5     RW Aur, prototype of its class.                                         Her1962 
05078+1622   BPM 119     [PM2000]  216289 + [PM2000]  216084.                                    Gvr2010 
05078-0505   BUP  74     bet Eri = 67 Eri = Cursa. STF 647.                                              
05079+6849   HJ 1152     BDS 2479 has an error of 30', making it identical with HJ 1152                  
                         (Van Biesbroeck).                                                       VBs1914 
05079+2142   S   466     105 Tau. B is BD+21@764. A is a spectroscopic and occultation binary.           
                         H 6 105.                                                                MEv2010 
05079+1519   BPM 120     [PM2000]  216579 + [PM2000]  216575.                                    Gvr2010 
05079+0830   STT  98     14 Ori. One component, probably the primary, is SB; the RV range in the         
                         combined light is 22 km/s.                                                      
                         According to Eggen, the system shares common proper motion with         Egg1963 
                         ADS 3712 = STF 643 (mags. 9.5-9.5, 3", K2), which is 6' distant.                
05080+3703   HJ 3265     AB: SEI  69.                                                            Nsn2017a
                         AC: SEI  70.                                                            Nsn2017a
05080-2648   MUG  13     Spectral type of comoving secondary estimated as M4-5, mass 0.17 Msun.  Mug2014 
05080-6934   OGL 303     LMC120.4.70309 + LMC120.4.70525                                         Pli2012 
05081+3701   COU1530     Also known as HDS 673.                                                          
05081+3658   HJ 3266     SEI  73.                                                                Nsn2017a
05081+3609   HJ  692     SEI  71.                                                                Nsn2017a
05081+2416   EDG   2     103 Tau. A is a spectroscopic and occultation binary.                           
             H 5 114     H V 114.                                                                        
05083+7538   JNN 266     G 248-32. Estimated age 1000-10000 Myr; masses 0.21 +/- 0.04 and 0.15           
                         +/- 0.03 Msun; a ~3.1 au.                                               Jnn2014 
05080+2214   ARU   2     Mistakenly added to WDS as BD+22 0834; however, Argue et al. measure    Aru1984 
                         was of AGK3 +22 0834 = BD+22 1589 = 07085+2159 OCC 337.                         
05083-0840   STF 649     AB: H 4  43 = H N  46.                                                  MEv2010 
05084+5525   GC 6249     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
05085+1418   LDS5662     LDS6166.                                                                        
05085-1036   GAL 377     Object #165 in Gallo's original list.                                   Gal1914 
05085-4113   HJ 3728     NLTT 14574/14573                                                        Chm2004 
                         HIP 23926. B = HIP 23923. A is above the MS, evolved (despite sp. type          
                         G3V). The pair was observed with NICI in 2010. Both A and B have large          
                         PM, PM(A)=(-77,+284). The original Hipparcos parallax of B is 8.5mas,           
                         obviously wrong. IRAS source.                                           Tok2011a
                         Moutou et al. (2011 A&A 527, A63): exoplanet around A, P~2800d +drift   Tok2014d
05085-7058   OGL 304     LMC114.6.224   + LMC114.6.480                                           Pli2012 
05087+3703   SEI  78     ALI 302.                                                                        
05087+1251   BPM 121     [PM2000]  218040 + [PM2000]  218004.                                    Gvr2010 
05087-6846   MLO  13     AC: Identification uncertain.                                                   
05088-6800   OGL 305     LMC117.3.18237 + LMC117.3.18886                                         Pli2012 
05090+1238   BPM 122     [PM2000]  218603 + [PM2000]  218372.                                    Gvr2010 
05092-6701   OGL 306     LMC115.2.14607 + LMC115.2.14813                                         Pli2012 
05093+0950   BUP  75     13 Ori. Hyades vB 130.                                                          
                         Two CPM companions with rho = 88".6 and rho = 168".0, both outside              
                         our detection window.                                                   Msn1993a
05094-6857   OGL 307     LMC111.5.43680 + LMC111.5.44857                                         Pli2012 
05096+2947   STTA 61     HJL1040.                                                                HJL1986 
                         SHY 474. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AB: Primary is SB2, P=1469.4d (Halbwachs et al. 2012)                   HJL2012b
05097+1536   STT  99     15 Ori. Round (Hussey). May not be double.                                      
05097-7009   OGL 308     LMC113.5.47798 + LMC113.5.47799                                         Pli2012 
05098+2802   BU 1047     BC: Van Biesbroeck in 1953 noted "no evidence of change in 65 years."           
                         However, the pair is now apparently in rapid motion in a highly-                
                         inclined orbit.                                                         Wor1967b
                         BC. The star was noted as a spectroscopic binary by Griffin et          Grf1988 
                         al. (1988).                                                                     
                         Hipparcos identified the pair as a non-Hyades member, however, the      HIP1998 
                         results invesigating proper motion, photometry and radial velocity      Grf1988 
                         yield a more ambiguous finding. The jury is still out!                  Grf2013c
             STF 645     A,BC: HJL  67.                                                          HJL1986 
                         A,BC: H 3  90.                                                          MEv2010 
05099-6715   OGL 309     LMC116.4.13354 + LMC116.4.13836                                         Pli2012 
05100+4009   ES  169     Aka BRT 112.                                                                    
05100+3754   SEI  81     ADS 3729a.                                                                      
05100+1054   J   323     A is probably variable.                                                 J__1952 
05100-0704   STF 651     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
05100-6722   OGL 310     LMC108.6.14    + LMC116.3.15651                                         Pli2012 
05101+2733   BGH  21     NLTT 14576/14572                                                        Chm2004 
                         HJL1041.                                                                HJL1986 
                         SHY 175. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         Secondary is SB1, P=2273.8d (Halbwachs et al. 2012)                     HJL2012b
05101-0204   BAL 296     1deg error in IDS led to similar error in WDS designation.                      
05101-2341   WSI 121     Both 2MASS J05100427-2340407 and J05100488-2340148 are binaries in the          
                         AstraLux images, so since they are separated by only 27" on the sky             
                         and have very similar proper motions (e.g. Roser et al. 2010), this is  XXX2010 
                         likely a quadruple system in reality. Common proper motion remains to           
                         be confirmed for both of the close components.                          Jnn2012 
                         Aa,Ab: Rectilinear solution by Miles & Mason (2016) &                   Msn2016b
                         Mason et al. (2018).                                                    Msn2018a
05101-6929   OGL 311     LMC111.8.8839  + LMC119.8.34937                                         Pli2012 
05101-7008   OGL 312     LMC113.5.48001 + LMC113.5.48018                                         Pli2012 
05102+1400   S   468     Also known as STF 650.                                                          
05102+0439   GWP 650     This is also known as V1396 Ori (ZZ Cet type var).                              
05103+3718   STF 644     One component is a spectroscopic binary.                                        
                         AB: H 1  45.                                                            MEv2010 
                         AB: Additional notes may be found in van den Bos (1963).                B__1963b
05103-0736   A   484     Position angles uncertain but near 130@-310@.                                   
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.20 +/- 0.18, 2.28, and 1.10 Msun, respectively.             Mlk2012 
05104+3741   SEI  84     Also known as ALI 531.                                                          
05105-1854   HJ 3727     CPD-19@760.                                                                     
05108-6716   OGL 313     LMC108.5.27    + LMC108.5.171                                           Pli2012 
05108-6740   OGL 314     LMC108.8.34    + LMC108.8.462                                           Pli2012 
05111+3718   BLL  13     B is BD+37@1072.                                                                
05112-0833   RUC  18     Multiple system including contact binary ER Ori. Pribulla & Rucinski            
                         (2006) estimate the mass of the contact pair at 2.510 Msun and the      Pbl2006 
                         minimum mass of the wider component at 0.93 Msun.                               
05113-6707   OGL 315     LMC107.8.492   + LMC107.8.1389                                          Pli2012 
05114-0101   BAL 297     Duplicity suspected by Baillaud but no measure.                         Bal1944 
05115+5305   HJ 2251     HJ gives position angle as 319.9@.                                              
05115-5519   HJ 3738     B is CPD-55@759.                                                                
05115-6753   OGL 316     LMC109.5.9247  + LMC109.5.9566                                          Pli2012 
05117+0031   HU   33     One component is a spectroscopic binary. Variable, V1085 Ori.                   
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 5.26 +/- 4.75, 9.35, and 2.57 Msun, respectively.             Mlk2012 
05119+3544   HJ  358     SEI  92.                                                                Nsn2017a
05119-0907   BUP  76     B is BD-09@1093.                                                                
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
05119-4253   HJ 3734     LDS 137.                                                                        
05119-6830   OGL 317     LMC110.5.14459 + LMC110.5.14649                                         Pli2012 
05120+0650   STTA 62     B is BD+06@865.                                                                 
                         Pair appears in an appendix list, not part of the discoverer's regular          
                         numbering sequence.                                                             
05121-6511   TOK  92     HIP 24221.                                                              Tok2011a
                         A is SB without orbit, dRV=56.7                                         Nrd2004 
05123-1152   STF 655     iot Lep = 3 Lep                                                                 
                         AB: H 3  67.                                                            MEv2010 
05123-6708   LDS 140     Aka MLO  15.                                                                    
05126-1727   S   470     B is BD-17@1046.                                                                
05130+1242   BPM 123     [PM2000]  226150 + [PM2000]  226362.                                    Gvr2010 
05130-6941   OGL 318     LMC112.4.1006  + LMC112.4.1258                                          Pli2012 
05130-7028   JNN  32     There is a companion to 2MASS J05130132-7027418 in the AstraLux images          
                         which has a brightness and color that is consistent with a physical             
                         companion. It counts as an unconfirmed binary here, since it has not            
                         yet been tested for common proper motion.                               Jnn2012 
05131-5959   HJ 3743     Large parallax error in HIP! Primary is possible SB.                    Tok2014d
05133+0252   STF 654     rho Ori = 17 Ori. A is long-period spectroscopic binary, P = 1031.4d.           
                         A: Ren & Fu (2013) calculated an astrometric orbit, combining           Ren2013 
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Bertiau (1957).                                                         BFC1957 
                         AB: H N  21.                                                            MEv2010 
05134+3829   CHR 256     mu Aur = 11 Aur. Hipparcos stochastic double solution.                          
05134+2411   POU 586     POU 588.                                                                        
05134+0341   TOK 211     The 1".25 companion discovered with NICI is hardly the one that                 
                         produced the acceleration of 17 mas yr-2.                               Tok2012a
05135+1608   BPM 124     [PM2000]  227301 + [PM2000]  227493.                                    Gvr2010 
05135+0158   STT 517     Star C (mag. 13, 7") may be physical.                                           
                         Trajectory appears quasi-linear.                                        Mlr1956a
05135-5534   HJ 3742     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2013).                         USN2013a
05136-7025   OGL 319     LMC113.3.8348  + LMC113.3.9695                                          Pli2012 
05137-0856   MLL   2     Aka BRT3264.                                                                    
05138-1641   GAL 378     Object #171 in Gallo's original list.                                   Gal1914 
05139+3958   HU 1100     ES 280.                                                                         
                         J  3306.                                                                Nsn2016 
05139-5648   HJ 9001     Previously known as HJ 5450a.                                                   
05140+5126   HU  821     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
05140-6827   OGL 320     LMC110.4.6684  + LMC110.4.7756                                          Pli2012 
05142+2535   BRT3263     Originally published as BRT 136.                                        Brt1928 
05142-6701   OGL 321     LMC107.2.166   + LMC107.2.193                                           Pli2012 
05143+6949   STF 638     H 2  92.                                                                MEv2010 
05143+1953   KIR   1     AB. Using data from 2MASS and IRTF, Kirkpatrick et al (2001) derive     Kir2001b
                         spectral types K4V and M6V, conclude is probably a physical pair with           
                         separation 225 au.                                                              
05143-1550   GJ 193      The acceleration is due to the 2.2 yr SB with estimated axis of 55 mas          
                         and q > 0.14. The companion is too faint and close to be resolved with          
                         NICI or speckle. The system is triple with a faint common-proper-motion         
                         (CPM) companion at 14".6.                                               Tok2012a
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by Nidever            
                         et al. (2002). They derived component masses 0.98 and 0.22 Msun and     Nid2002 
                         an estimated semimajor axis of 57.81 mas.                               Ren2013 
05143-1723   FEN   3     Aka OL  127.                                                                    
05145+1707   BPM 125     [PM2000]  229086 + [PM2000]  229142.                                    Gvr2010 
05145-0812   STF 668     bet Ori = 19 Ori = Rigel. The companion is a spectroscopic binary and           
                         suspected visual double, although it remains unconfirmed. Magnitudes            
                         of B and C very uncertain. Changed from IDS values (10.4 for B, C, and          
                         BC). AD pair first mentioned by Mitchel in 1846 (Sidereal Messenger,            
                         May 1847) but no astrometry included.  See extensive notes by Burnham.  Bu_1906 
                         Intensity Interferometer Limb-darkened diameter 2.55 +/- 0.05 mas.      HBr1974 
                         NPOI Limb-darkened diameter  2.606 +/- 0.009 mas, Sp = B8I,             NOI2018 
                         R =74.1  +/- 6.7  \rsun, Teff = 10556 +/-133 K,                                 
                         L = 61515 +/- 11486 \lsun.                                                      
             bet Ori     1975.631: Possible binary (450 and 656 nm).                             Bla1977a
                         1975.636: Possible binary (400, 500, 600, and 750 nm).                  Bla1977a
             STF 668     A,BC: H 2  33.                                                          MEv2010 
05145-6957   HJ 3754     B is CPD-70@376.                                                                
05146+7628   HU 1097     B may be variable.                                                              
05147+3707   SEI 115     Primary not seen on POSS plate; may be flaw on AC Potsdam plate.                
05147-0704   STF 667     H 1  54.                                                                MEv2010 
05149+3309   HJ  694     Aka HJ  361.                                                                    
05150+3813   BRT2208     ALI 788.                                                                        
05150+0108   OL   95     The south following of two faint stars.                                 B__1963b
05151-3639   HJ 3740     B is CD-36@2133.                                                                
05152+0826   STF 664     Same as CHE  79. Verified by DAL04.                                             
05152-1404   LDS3648     Luyten gives a separation of 130", but this appears to be a             Luy1978 
                         typographical error; if identification is correct, rho ~13"; this               
                         secondary corresponds to a high proper motion CPM companion.                    
05153+4710   A  1031     A 1998.8317 measure by Mason et al. (2001) was actually of STT 98.      Msn2001b
                         Also known as V390 Aur.                                                         
05154+3241   STF 653     14 Aur. A is the Delta Scuti-type variable KW Aur, and is also a                
                         spectroscopic binary.                                                           
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: SEI 124.                                                            Nsn2017a
                         AC: H 4  19.                                                            MEv2010 
05154-6700   OGL 322     LMC107.2.14205 + LMC107.3.195                                           Pli2012 
05155+2217   COU 158     108 Tau.                                                                        
05155-7001   OGL 323     LMC112.1.64694 + LMC112.1.64780                                         Pli2012 
05156+7857   LDS1604     NLTT 14588/14589                                                        Chm2004 
05156-6139   JSP9002     Previously known as JSP  71a.                                                   
05156-7049   OGL 324     LMC105.5.15    + LMC105.5.761                                           Pli2012 
05157+3738   SEI 126     AC: WLY  18AC.                                                          Nsn2017a
05157-4927   GC 6457     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
05159+3425   ES  170     AB: SEI 130.                                                            Nsn2017a
05160-7002   OGL 325     LMC103.8.32853 + LMC103.8.32837                                         Pli2012 
05160-7214   JAO   3     Also known as LHS1749. Parallax = 46.08 +/- 1.40 mas.                   TSN2010 
05162-1121   CHR 225     It in uncertain whether the pair resolved here is the known G8III+A0V           
                         composite spectrum binary (Hoffleit & Warren 1991). The small apparent  Hof1991 
                         change in theta over the 4-year span between observations does not              
                         appear consistent with our estimated period of ~15 or so years;                 
                         however, the magnitude difference between the components is small, so           
                         we are unable to rule out a 180 deg quadrant flip or perhaps an                 
                         eccentric orbit.                                                        Hrt1996b
                         Docobo et al. (2014) use the spectroscopic elements of Carquillat &             
                         Prieur (2007), together with speckle data and the Hipparcos parallax,   Crq2007 
                         to derive the remaining orbital elements. The resulting masses are              
                         1.92 +/- 0.26 and 2.50 +/- 0.29 Msun.                                   Doc2014h
05163+3419   TRN  17     Aa,Ab is an AO artifact as per Turner and Roberts.                      Trn2010 
                         Aa,Ab: Additional notes may be found in Turner et al. (2008).           Trn2008 
             SEI 136     AB: AE Aur. Nova remnant, probably not double.                                  
                         The companion indicated by the Potsdam Astrographic catalogue is non            
                         existing. There's the remark: Very doubtful.                            VBs1960 
05164-1531   GAL 172     J  1468.                                                                J__1962a
05164-7124   OGL 326     LMC106.5.13    + LMC106.5.66                                            Pli2012 
05165+3635   SEI 137     SEI 138.                                                                        
05165-2106   DON  97     Variable dm?                                                            Hln1965 
05165-6947   OGL 327     LMC103.6.11600 + LMC103.6.11652                                         Pli2012 
05167+4600   ANJ   1     Aa,Ab: 13 Aur = alp Aur = Capella.  Composite spectrum; G5IIIe+G0III.           
                         aka "The Interferometrist's Friend."                                            
                         Separations from Anderson (1920) have been modified as described in     AnJ1920 
                         Merrill (1922).                                                         Mrr1922 
                         Measures of Kulagin made by a transit interferometer; quadrants were            
                         flipped for all his measures.                                           Kul1970 
                         See discussion in Labeyrie et al. (1974).                               Lab1974 
                         Combined spectroscopic/interferometric orbit by Heintz (1974):          Hei1974a
                         P = 104.0237 d, a = 0.0547", eccentricity neligibly small. Ascending            
                         node revised according to Heintz's astrometry                                   
                         1969.1348: This position angle was incorrectly published as 303.0               
                         degrees in Balega & Tikhonov (1977).                                    Bag1977 
                         1978.915, 1978.929, 1979.082: Observations on these three dates                 
                         overlap in two papers by Koechlin et al. (1979, 1983), with only        Koe1979 
                         slight changes.  Values from the later paper are given in the catalog.  Koe1983 
                         1984.9309, 1985.1062, 1985.1994: Estimates of the position angle and            
                         angular separation are deduced from the elongation of the central               
                         speckle peak in the autocorrelation.                                    Bnu1986 
                         Colors and spectral types determined by speckle photometry are                  
                         given by Bagnuolo & Sowell (1988).                                      Bgn1988 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Observations by Hummel et al. (1994) were made through narrow band      MkT1994 
                         filters centered at 800, 550, and 450 nm. Colors were derived from all          
                         1988-1992 data, so are listed at the mean epoch of 1991.9.  This paper          
                         also includes a new orbit. Finally, errors are given as "error                  
                         ellipses"; these values are tabulated below.  Columns include date              
                         (BY), major and minor axes of the ellipse (in mas), and ellipse                 
                         orientation (in degrees).                                                       
                              1988.7973     0.95     0.11      96.                                       
                              1988.8000     0.42     0.03      93.3                                      
                              1988.8028     0.22     0.03      85.7                                      
                              1988.8055     0.15     0.02      88.2                                      
                              1990.9411     0.09     0.02      86.6                                      
                              1990.9548     0.13     0.05      88.6                                      
                              1991.7159     0.73     0.08     124.1                                      
                              1991.7214     0.37     0.06     179.6                                      
                              1991.7241     0.23     0.05     156.5                                      
                              1991.7871     0.07     0.01      93.7                                      
                              1991.8364     0.07     0.02      91.6                                      
                              1991.8665     0.04     0.01      94.5                                      
                              1991.8857     0.06     0.02      88.4                                      
                              1991.8939     0.10     0.05     149.3                                      
                              1991.9021     0.16     0.05      77.9                                      
                              1991.9733     0.10     0.03      87.6                                      
                              1991.9870     0.09     0.02      77.5                                      
                              1992.0006     0.50     0.07      83.0                                      
                              1992.0417     0.24     0.05      73.4                                      
                              1992.0445     0.09     0.02      83.8                                      
                              1992.0691     0.25     0.05      74.6                                      
                              1992.0855     0.22     0.02      93.5                                      
                              1992.0965     0.10     0.02      78.5                                      
                              1992.7399     0.33     0.05     111.1                                      
                              1992.7426     0.42     0.04     118.5                                      
                              1992.7454     0.21     0.06     110.6                                      
                              1992.7481     0.40     0.09     121.2                                      
                              1992.7508     0.62     0.08     121.3                                      
                              1992.7536     0.71     0.16     103.9                                      
                              1992.7563     0.76     0.12     121.9                                      
                              1992.7755     0.05     0.01     105.9                                      
                              1992.8357     0.19     0.02     118.1                                      
                              1992.8658     0.09     0.04      78.1                                      
                              1992.8658     0.14     0.04      91.8                                      
                              1992.8686     0.09     0.02      69.5                                      
                              1992.8686     0.14     0.07      92.9                                      
                              1992.8823     0.07     0.02      88.8                                      
                              1992.8932     0.11     0.02     116.4                                      
                              1992.9206     0.43     0.07      98.8                                      
                              1992.9452     0.15     0.03     113.0                                      
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Hummel et al. (1994).                                                   MkT1994 
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         Branham (2008) derives combined interferometric/spectroscopic orbit,    Bnh2008 
                         using a semidefinite programming technique. The resulting masses are            
                         3.049 +/- 0.513 and 2.569 +/- 0.432 Msun; he also determines a value            
                         for the parallax of 74.85 +/- 1.53 mas.                                         
                         Aa,Ab: Following an extensive review of historical spectroscopic and            
                         astrometric measurements of Capella, Torres et al. (2009) derived a     Trr2009 
                         new combined-solution orbit, assuming a circular orbit. They determined         
                         an orbital parallax of 76.67 +/- 0.17 mas (distance 13.042 +/-                  
                         0.028 pc), an age of 540-590 Myr, and the following physical                    
                         parameters for the two components:                                              
                         Mass (Msun):       2.466 +/- 0.018     2.443 +/- 0.013                          
                         Radius (Rsun):     11.87     0.56      8.75      0.32                           
                         Teff (K):          4920      70        5680      70                             
                         Luminosity (Lsun): 79.5      4.8       72.1      3.6                            
                         Mv (mag):          0.315     0.017     0.186     0.016                          
                         Aa,Ab: Weber & Strassmeier (2011) derived new spectroscopic elements,   WbS2011 
                         assuming the period determined by Torres et al. (2009). The new         Trr2009 
                         solution yielded masses of 2.573 +/- 0.009 and 2.488 +/- 0.008 Msun.            
                         Aa,Ab: A combined solution by Torres et al (2015) yields the following  Trr2015 
                         physical parameters for Aa and Ab:                                              
                             mass (Msun):       2.5687 +/- 0.0074     2.4828 +/- 0.0067                  
                             Teff (K):          4970       50         5730       60                      
                             Radius (Rsun):     11.98      0.57       8.83       0.33                    
                             log g (cgs):       2.691      0.041      2.941      0.032                   
                             Luminosity (Lsun): 78.7       4.2        72.7       3.6                     
                             a(AU):                      0.74272 +/- 0.00069                             
                             Distance (pc):              13.159      0.015                               
                             Age (Myr):                  590-650                                         
                             [Fe/H}:                     -0.04       0.06                                
             HJ 2256     AF: H VI 30.                                                                    
                         AF: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             SHY  23     AM: HIP  24608 + HIP  26779.                                                    
             SHY  23     AN: HIP  24608 + HIP  26801.                                                    
                         MN is 05413+5329AB.                                                     Dam2017i
             ST    3     Capella HL, the distant (723") double companion to Capella with                 
                         common proper motion. A premature orbit has been computed.                      
                         Capella H is variable with a period of about 17.9d and an amplitude     Skf2019g
                         amplitude of about 0.03 magnitudes.                                             
             HJ 2256     AF: H 6  30.                                                            MEv2010 
05171-7128   OGL 328     LMC106.6.13434 + LMC106.6.13435                                         Pli2012 
05172+3747   HJ 3271     SEI 149.                                                                Nsn2017a
05172+3320   STF 666     H 2  48.                                                                MEv2010 
05173+5335   ES 2610     A is R Aur, variable 6.5-13.8. B is BD+53@880, F8V.                             
05174+3500   SEI 155     J   184.                                                                Nsn2016 
05175+2008   STF 674     A is the Algol-type binary CD Tau, eclipsing SB2, P = 3.44d.                    
                         AB has estimated period of 11000y.  B has spectral type dK2.            Tok2006 
05175+0354   BAL2142AC   Optical/physical nature ascertained from Gaia DR2.                      FMR2019b
05175-3454   KIR  12     omi Col.                                                                        
05175-7031   OGL 329     LMC104.7.15822 + LMC104.7.16197                                         Pli2012 
05176-0651   H 5  25     tau Ori = 20 Ori. H V 25.                                                       
05176-1513   S   473     B is BD-15@1000.                                                                
05177-1809   SEE  49     See's 1897 angle should read 196.7.                                     B__1953a
05179+3724   SEI 162     The discrepant measure by Scheiner (1908) is apparently due to a        Sei1908 
                         typographical error in the AC Potsdam Astrographic Catalog, as the              
                         correct position of the secondary is off by exactly 24" in dec.                 
                         Matches to other AC plates from 1929 and 1930 agree well with the               
                         Aladin image, as well as more recent observations.                              
05181-3402   TOK  61     Aa,Ab: Estimated masses 1.04 and 0.15 Msun; sep 43.6 au, period 260 y.  Tok2010c
             HJ 3745     HIP 24711. B = HIP 24712.                                               Tok2011a
05181-7654   TOK 663     Resolved using ANDICAM2. B is not in PPMX.                              Tok2014d
05182+3739   BU 9002     Previously known as BU 885 1/2.                                                 
05182+3322   STT 103     16 Aur. A is a long-period spectroscopic binary. P = 434.8d.                    
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Christie (1936).                                                        Crs1936 
05182-6809   OGL 330     LMC102.7.16903 + LMC102.7.16902                                         Pli2012 
05183-7143   OGL 331     LMC106.7.13197 + LMC106.7.13239                                         Pli2012 
05184-3108   LDS3651     NLTT 14861/14860                                                        Chm2004 
05185+3800   SEI 171     ALI 536.                                                                        
05185-6933   OGL 332     LMC103.5.107911+ LMC103.5.110011                                        Pli2012 
05186+4020   SMA  50     IDS and old-WDS location in error. Nothing at 05194+4020 (Heintz),      Hei1987a
                         but probably identical to a pair at this location.                              
                         SLE  64.                                                                        
05187+3331   ES   59     A pair found many years ago with the 3in refractor. The distant double          
                         comes was found with the 13in reflector at the Oxford Univ. Obs. and            
                         the comes C with the 17 1/4. AB was measured by Burnham in 1882.        Es_1902a
05187+0359   STF 682     BAL 2143.                                                                       
                         HIP 24774. The B-companion could possibly be a semi-resolved binary.            
05187-7122   OGL 333     LMC106.5.14568 + LMC106.5.14749                                         Pli2012 
05188+5250   STF 657     Same as STF 660.                                                                
05188-1808   SEE  50     A is a spectroscopic binary.                                                    
05189-6810   OGL 334     LMC102.7.22886 + LMC102.7.22769                                         Pli2012 
05189-6948   OGL 335     LMC103.6.38675 + LMC103.3.2                                             Pli2012 
05189-6957   OGL 336     LMC103.7.31356 + LMC103.7.31945                                         Pli2012 
05190-2829   BUG   8     2MASS J05185995-2828372                                                         
                         Estimated spectral types are L6: + T4:, effective temperatures ~1600            
                         and ~1330 K. Masses are estimated at 0.042-0.077 and 0.031-0.074 Msun,          
                         and the orbital period (assuming the semi-major axis = 1.26 * rho) is           
                         ~10yr.                                                                  Bug2006a
05191+4006   STFB  3     lam Aur = 15 Aur                                                                
                         AC and AD: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         AD: H 5  22.                                                            MEv2010 
                         DE: H 5  88AC. = H V 88.                                                Dam2017i
                         AC: Rectilinear solution by Friedman et al. (2011).                     USN2011a
05191-6803   OGL 337     LMC102.3.50    + LMC102.3.51                                            Pli2012 
05192+3548   SEI 179     A is an irregular variable, V348 Aur.                                           
05192+2008   STF 680     Spectrum composite; G8II-III+G1IV-V (BSC).                                      
05192+1212   BPM 126     [PM2000]  237882 + [PM2000]  238008.                                    Gvr2010 
05192-0304   A    53     HIP 24819. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AB: NLTT 14867/14868                                                    Chm2004 
05192-1800   FEN   4     Aka ARA 331.                                                                    
05193-1045   STF 688     BDS 2665, H III 94 same star. B is BD-10@1152.                                  
                         H 3  94.                                                                MEv2010 
05193-1831   S   476     AB: B is BD-18@1056.                                                            
05193-2845   LDS3653     NLTT 14889/14887                                                        Chm2004 
05194+3359   HO   18     18 Aur.                                                                         
05196-0107   BAL 303     RST 4779.                                                                       
05197+3614   WEI   8     AB: SEI 189.                                                            Nsn2017a
05197+3526   SEI 186     SEI 187.                                                                        
05197+2511   STF 679     HJL  68.                                                                HJL1986 
05199-0723   JNN  34     2MASS J05195412-0723359 and J05195513-0723399, both from the Riaz et            
                         al. (2006) sample, are separated by only 16" and have comparable        Ria2006 
                         estimated distances (59 and 70 pc), as well as quite similar proper     XXX2010 
                         motions (e.g. Roser et al 2010), and thus likely form a physical pair.  Jnn2012 
05200+4546   GIC  54     G096-032/G096-031.                                                              
                         NLTT 14857/14855                                                        Chm2004 
05200-1550   KPP2710     Mass = 0.683+/-0.018 \msun for A; = 0.58+/-0.01 for B.                  Bnv2020 
                         Teff = 4750 +/- 65 K for A; = 11,000 +/- 500 for B.                             
05201+3236   SEI 194     J 1089.                                                                         
05201-7100   OGL 338     LMC105.3.5578  + LMC105.3.5594                                          Pli2012 
05202-6810   OGL 339     LMC102.2.30    + LMC102.2.37                                            Pli2012 
05203+2510   STF 683     Chevalier's measure was incorrectly identified as STF 694, so never     Che1910 
                         added to the WDS; correct ID was determined based on his coordinates.   Hrt2012b
05204-0802   STF 692     AB,C: H 4  87.                                                          MEv2010 
05206-1031   GAL 379     Object #176 in Gallo's original list.                                   Gal1914 
05206-7024   OGL 340     LMC104.3.8821  + LMC104.3.9924                                          Pli2012 
05207+5848   GIC  46     G191-030/G191-029 or GJ 3342A/3343B.  A 1hr typographical error in RA           
                         led to this pair being initially entered in the WDS as 04205+5852.              
                         LDS6183.                                                                        
05207+3726   SEI 201     Fullerton et al. (1991) describe profile and radial velocity            Ful1991 
                         variations that suggest that this star is a short-period, radial                
                         pulsator.  Underhill (1995 PASP 107, 513) also discusses radial                 
                         velocity measurements.                                                  Msn1998a
05209+2402   STF 686     POU 650.                                                                        
05210+7113   HJ 1154     The ADS incorrectly added the CD component of 05061+5858 (STFA 13) as   A__1932a
                         an additional component of this pair.                                           
05213-6835   OGL 341     LMC101.3.42767 + LMC101.3.42931                                         Pli2012 
05217+3322   LDS6184     NLTT 14919/14920                                                        Chm2004 
05217+1854   KU   87     B is BD+18@832.                                                                 
05217+1240   STT 105     Not seen since 1971. Needs speckle.                                             
                         Additional notes may be found in van den Bos (1963).                    B__1963b
05218+3231   HU  614     A is the Mira-type variable UV Aur.                                             
05218-2446   HJ 3752     Spectrum composite; G7II-III+A7IV-V.                                            
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
05219+4203   AG  314     B is BD+41@1166.                                                                
05222+2008   J   144     OL  204.                                                                        
05222+0524   STT 106     HJL  69.                                                                HJL1986 
05223-7109   OGL 342     LMC105.2.15955 + LMC105.2.16304                                         Pli2012 
05224-6934   OGL 343     LMC103.4.118812+ LMC103.4.118814                                        Pli2012 
05225+4621   ES 1231     AC: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
05225-7044   OGL 344     LMC105.4.45008 + LMC105.4.45010                                         Pli2012 
05226+7914   STF 634     STTA 60.  B is BD+79@168.                                                       
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
05226+0236   A  2641     Only elements P and T have been amended by Starikova (1978) from the    Sta1978c
                         orbit of Baize (1957).                                                  Baz1957b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.27 +/- 0.35, 1.39, and 0.95 Msun, respectively.             Mlk2012 
05228+4755   GIC  55     G096-035/G096-034. See Allen et al. (2000) for information on           AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
                         NLTT 14943/14940                                                        Chm2004 
05228+3658   SEI 220     AB: SEI 221.                                                                    
05228+0333   STF 696     23 Ori. B is BD+03@872.                                                         
                         H 4  84.                                                                MEv2010 
05229-4219   TOK  93     HIP 25148. A is SB without orbit, dRV= 3.7                              Nrd2004 
                         and also an astrometric binary (Makarov & Kaplan 2005).                 Mkr2005 
                         The companion at 66 mas is at the diffraction limit, the NICI                   
                         measurement is not accurate. The pair can be resolved by speckle.       Tok2012a
                         Aa,Ab: The tentative resolution at Gemini om 2011.70 is confirmed here,         
                         with 25deg of direct motion.                                            Tok2013b
05229-7143   OGL 345     LMC165.7.83    + LMC165.7.149                                           Pli2012 
05230-0850   JNN  36     This star has been classified as a probable T Tau star in Alcala et             
                         al. (1996 A&AS 119, 7).                                                 Jnn2012 
05230-1613   GAL 380     Object #177 in Gallo's original list.                                   Gal1914 
05231+3110   STF 691     B is BD+31@947.                                                                 
                         SEI 227.                                                                Nsn2017a
05231+0103   STF 700     H 1  75.                                                                MEv2010 
                         V1804 Ori, Algol-type eclipsing binary, P = 2.22878 d.                  Zas2011 
05232-2642   HIP  25180  Large RV amplitude (31.7 km s-1) hints at short orbital period, but             
                         only small dmu = 3 mas yr-1 is detected by Hipparcos. Triple?           Tok2012a
05232-3145   HJ 3757     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2013).                         USN2013a
05232-7112   OGL 346     LMC164.8.18917 + LMC164.8.18916                                         Pli2012 
05233+3445   SEI 229     FOX 140.                                                                        
05233+3409   MLB1037     HJ  363.                                                                        
05233-0825   STF 701     H 2 102.                                                                MEv2010 
05234-7128   OGL 347     LMC165.6.20315 + LMC165.6.20368                                         Pli2012 
05235+5733   BU 1393     16 Cam. A is a spectroscopic binary.                                            
05235+1602   STF 697     B is BD+15@804.                                                                 
05237+6841   GIC  56     LDS5192. G248-038/G249-007.                                                     
05237+3606   SEI 233     SEI 234.                                                                        
05238-7018   OGL 348     LMC163.6.62323 + LMC163.6.62352                                         Pli2012 
05239+1743   BPM 127     [PM2000]  247544 + [PM2000]  247826.                                    Gvr2010 
05239-0052   WNC   2     A,BC: Primary is SB2, P=22.58d                                          Tok2014d
             A   847     BC: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.74 +/- 0.51, 2.47, and 1.13 Msun, respectively.  Mlk2012 
05239-6832   OGL 349     LMC160.6.38837 + LMC160.6.39333                                         Pli2012 
05240+3238   COU1090     Primary is V424 Aur, an Algol-type eclipsing binary, P = 1.8368d.       Zas2012 
05240-0940   GAL 381     Object #178 in Gallo's original list.                                   Gal1914 
05243+0222   STF 702     BDS 2709, H I 75 same star.                                                     
05244+1723   S   478     111 Tau. A is a spectroscopic binary. B is BD+17@919.                           
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
             WNO  52     AC: HJL1043.                                                            HJL1986 
                         AC: GJ 202 + GJ 201. CPM pair.                                          Mkr2008 
                         AC: SHY  25. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
             S   478     AB: H 5 110.                                                            MEv2010 
05245-0224   MCA  18     eta Ori = 28 Ori. Quintuple; primary is a double-lined spectroscopic            
                         triple with periods 7.99 d (Aa1,Aa2) and 9.2 yr (Aa,Ab). The close              
                         pair eclipses, and shows an 8-hour pulsation in one of the components.          
                         Aa is also eclipsing binary (period 7.9904 day).                        Zas2010 
                         Aa,Ab.  McAlister (1976) orbit uses the elements P, T, e, and the       McA1976 
                         longitude of  periastron for the 9-year orbit, from a spectroscopic             
                         orbit by Ziska & Beardsley (1981), and assumes the orbit is edge-on;    Bey1981 
                         semi-major axis and node are based on a single speckle observation.             
                         The ascending node has been reversed.                                           
                         The visual companions are star B (mag. 4.8, 1.5") in slow retrograde            
                         motion, and C (mag. 9.4, 115").                                                 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         1985.8542: This measurement of the Aab,c component of eta Ori,                  
                         overlooked in the original analysis of this run, was discovered during          
                         preparation of a paper on absolute quadrant determinations by Bagnuolo  Bgn1992 
                         et al. (1992)                                                           Hrt1992b
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 25.82 +/- 24.95, 24.50, 22.65 Msun, respectively.  Mlk2012 
             DA    5     AB: Rectilinear solution by Hartkopf et al.  (2012).                    Hrt2012a
05245-0224   MCA 18      Aa,Ab has an SB1 orbit with P=9.44yr. The orbit given here uses only            
                         the speckle data, however.                                              Tok2015c
             H 6  67     H VI 67.                                                                        
05246+0149   S   479     B is BD+01@1003.                                                                
05246-0535   SKF 248     There is a possible companion at 7.8" noted in the WDS, but inside the          
                         AstraLux field of view, the star appears single.                        Jnn2012 
05247+6323   STF 677     AB: CfA: RV var? Can be a sub-system in A or B.                         Tok2014d
                         Now a 3 tier quadruple system since we resolved the secondary                   
                         component of the binary STF 677AB into a new 0".18 pair Ba,Bb and               
                         confirmed that the Robo-AO tertiary C at 7" is physical. We find C to           
                         be slightly below the MS, within errors. Although the relative motion           
                         of AC is fast, it is not directed away from PM(A) as would be the case          
                         for a distant background star; it is produced by the orbital motion of          
                         the inner binary AB. The presence of an inner subsystem in the binary           
                         AB was suspected previously from its variable RV (Nordstrom et al.              
                         2004). The estimated masses of Ba and Bb, 0.98 and 0.65 Msun,           Nrd2004 
                         respectively, remove the discrepancy between the mass sum of 3.05 Msun          
                         calculated for the AB system from its grade 4 orbit by Hartkopf et al.  Hrt2008 
                         (2008) and the expected mass sum. Although such discrepancies are not           
                         uncommon for low-quality orbits, in this case it serves as an indirect          
                         confirmation of Ba,Bb. Estimated period of Ba,Bb is ~20 yr.             Rbr2015d
05247+3723   BU  888     sig Aur = 21 Aur                                                                
05247+2009   J   145     OL  185.                                                                        
05248-1642   GAL 382     Object #179 in Gallo's original list.                                   Gal1914 
05248-5219   I   345     the Pic. A is a spectroscopic binary.                                           
                         Quoted errors in P and a for the Argyle et al. (2002) solution are      Ary2002b
                         +259/-54y, +0".20/-0".01, respectively.                                         
                         1989.9388: This system has also decreased in separation steadily                
                         since the 1920's, and was last resolved visually in 1983.               Hrt1993 
05249+1658   BPM 128     [PM2000]  249674 + [PM2000]  249613.                                    Gvr2010 
05249-7105   OGL 350     LMC164.7.34239 + LMC164.7.34339                                         Pli2012 
05250-0249   H 6  68     H VI 68. B is BD-02@1238.                                                       
05251+1212   BPM 129     [PM2000]  250160 + [PM2000]  250278.                                    Gvr2010 
05251+0621   BUP  78     gam Ori = 24 Ori = Bellatrix                                                    
05251-6818   OGL 351     LMC159.8.17075 + LMC159.8.17418                                         Pli2012 
05251-6833   OGL 352     LMC160.6.45288 + LMC160.6.46200                                         Pli2012 
05252+3451   STF 698     Spectrum composite; K1pIII-IV+F6V. B is BD+34@1030.                             
                         Same as WZ    9. Verified by Daley.                                     Dal2001b
                         AB: H 4 101.                                                            MEv2010 
05252+3434   BU  191     AB: SEI 243.                                                            Nsn2017a
05252+0155   STF 708     H 1  52.                                                                MEv2010 
05252-1119   STF 710     B is BD-11@1168.                                                                
05255-0033   A   848     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         1977.9196: This measure was incorrectly attributed to ADS 3701 in               
                         McAlister & Hendry (1982), with an incorrect position angle.            McA1982b
05256+3803   STF 699     AB: SEI 244.                                                            Nsn2017a
05256+3652   SEI 246     Not found by Heintz at IDS position.                                    Hei1987a
                         Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
05256-6005   HJ 3764     CD-60@1161.                                                                     
05257-0909   DAE   2     NLTT 15049 = LP 717-36.  Daemgen et al. (2007) derive a distance of     Dae2007 
                         20.2 +/- 4.7 pc, a separation of 10.9 +/- 2.5 au, and a predicted               
                         orbital period of 58 +/- 21 yr. Spectral types are M3.5 +/- 0.5 and             
                         M4.0 +/- 0.5; masses are 0.36 +/- 0.09 and 0.28 +0.11/-0.08 Msun.               
                         Parallax = 49.07 +/- 1.40 mas. Possible member of the AB Dor moving     JLB2017 
                         group.                                                                          
05257-6931   OGL 353     LMC161.1.5     + LMC161.1.38                                            Pli2012 
                         Also known as SKF1046.                                                          
05257-7123   OGL 354     LMC165.5.38071 + LMC165.5.38133                                         Pli2012 
05258-7124   OGL 355     LMC165.5.16733 + LMC165.5.16837                                         Pli2012 
05258-7308   GLI  34     Incorrectly assigned precise coordinates of 04026-7109 GLI  25,                 
                         leading to incorrect matches against 2MASS, UCAC4, etc.                         
05259+5033   LDS3656     NLTT 15008/15009                                                        Chm2004 
05260-0938   GAL 383     Object #182 in Gallo's original list.                                   Gal1914 
05260-1942   HJ 3759     B is BD-19@1172. Spectrum F5/7V.                                                
05260-6846   OGL 356     LMC160.2.87    + LMC160.2.86                                            Pli2012 
05262+3808   SEI 250     ALI 798.                                                                        
05262-0223   TOB9005     Measured as DOO  33 but actually an anonymous pair added here.          Tob2012c
05263+2836   BAR  26     bet Tau = 112 Tau = gam Aur = Elnath                                            
05263-6754   OGL 357     LMC159.4.67    + LMC159.4.1007                                          Pli2012 
05264+1324   BPM 130     [PM2000]  253244 + [PM2000]  253203.                                    Gvr2010 
05264-1210   GAL 384     Object #183 in Gallo's original list.                                   Gal1914 
05264-4323   HJ 3763     B is CD-43@1846.                                                                
05264-7121   OGL 358     LMC165.4.21895 + LMC164.1.435                                           Pli2012 
05265+0256   STF 712     AB: H 1  53.                                                            MEv2010 
05266+3524   STF 705     SEI 257.                                                                Nsn2017a
05266+3138   SEI 259     Secondary not seen on POSS plate; may be either variable star or flaw           
                         on AC Potsdam plate. Damm (2016) misidentified SEI 259; that pair has           
                         been given the designation DAM1282.                                     Dam2016c
05266+0652   SHY 478     HIP  25453 + HIP  25483.                                                        
05267+0045   LEO  57     BAL 981.                                                                        
05267-6827   OGL 359     LMC160.4.4940  + LMC160.4.5097                                          Pli2012 
05268+3557   SEI 258     Secondary not seen on POSS plate; may be either variable star or flaw           
                         on AC Potsdam plate.                                                            
05268+0306   KNT   3     psi 2 Ori = 30 Ori. A is a variable, P = 2.52d.                                 
                         a spectroscopic binary.                                                         
05268-6817   OGL 360     LMC159.1.14589 + LMC159.1.14662                                         Pli2012 
05269+3141   DAM1282     Misidentified by Damm (2016) as SEI 259.                                Dam2016c
05271+3410   BLL  14     A is a semiregular variable, S Aur.                                             
05271-6913   OGL 361     LMC161.3.12128 + LMC161.3.12137                                         Pli2012 
05272+1758   MCA  19     115 Tau. A is an occultation binary which has been resolved by                  
                         speckle interferometry.                                                         
                         First detected as an occultation binary by Africano.                    Afr1978 
                         1982.7551: All archival data for this system were reprocessed using             
                         more powerful algorithms than earlier available, resulting in four new          
                         unresolved measures as well as the new 1991 measurement. In addition,           
                         new rho and theta values have been determined for the observations      McA1989 
                         originally published from 1986.9-1988.3 (McAlister et al. 1989),        McA1990 
                         1988.7-1989.2 (McAlister et al. 1990), and 1990.3--1990.8 (Hartkopf     Hrt1992b
                         et al. 1992).  A preliminary orbit gives a period  of ~15.3 years and           
                         a semi-major axis of 0".080.                                            Hrt1994 
                         1988.2518: This date was incorrectly given as 1988.2490 in McAlister            
                         et al. (1989).                                                          McA1989 
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 6.46 +/- 2.35, 8.01, and 4.79 Msun, respectively.  Mlk2012 
05273+3426   D     7     AB = 05275+3425 TOB  35                                                         
                         AB: SEI 263.                                                            Nsn2017a
                         CD: SEI 261.                                                            Nsn2017a
05274-6943   OGL 362     LMC162.3.103719+ LMC162.3.104199                                        Pli2012 
05275-6825   OGL 363     LMC160.4.32945 + LMC160.4.33386                                         Pli2012 
05275-6903   OGL 364     LMC161.4.20865 + LMC161.4.21143                                         Pli2012 
05275-6939   OGL 365     LMC162.4.41184 + LMC162.4.41229 + LMC161.2.25632                        Pli2012 
05276+3429   BUP  79     phi Aur = 24 Aur. D is BD+34@1049.                                              
05276+2156   HJ  365     114 Tau. A is an occultation binary.                                            
                         AC: H 5 115.                                                            MEv2010 
05276+1126   HER  12     Additional notes may be found in Herbig (1962).                         Her1962 
05276-2055   SEE  53     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.60 +/- 2.71, 3.13, and 1.35 Msun, respectively.             Mlk2012 
05276-6120   JSP  79     CD-61@1111.                                                                     
05276-6908   HJ 3771     Measure difficult because of nebula which involves principal star.      Daw1922 
05277-7022   OGL 366     LMC163.3.13645 + LMC163.3.27818                                         Pli2012 
05278+1707   BPM 131     [PM2000]  256139 + [PM2000]  255999.                                    Gvr2010 
05278-0400   A   319     Possible that two different pairs were measured in generating 1962.924          
                         mean, but pair faint for Washington, so scatter may result from that.   Wor1967b
                         Algol-type eclipsing binary, period 5.27357 d.                          Zas2019 
05278-1447   GAL 385     Object #185 in Gallo's original list.                                   Gal1914 
05278-7109   OGL 367     LMC164.2.6335  + LMC164.2.5522                                          Pli2012 
05279+3447   HDS 721     The classification is from Mammano et al. (1977 A&A 59, 9), and                 
                         because the stars are are classified as B-type we have not included             
                         this system in our distributions for the O-stars.  Harries et al.               
                         (1998 MNRAS 295, 386) discuss the inner double-lined system and                 
                         evidence of a near tertiary in a 294-day orbit.  The distant, fourth            
                         star was detected both by us (on the suggestion of B. Schaeffer) and    HIP1997a
                         Hipparcos.                                                              Msn1998a
                         Primary is IU Aur, a Beta Lyr type eclipsing binary, P = 1.81147d.      Zas2012 
05280+3346   S   483     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
05281+4021   ES 2615     B is BD+40@1296.                                                                
05281+3519   SEI 266AE   A likely plate flaw.                                                    Grv2021b
05281+3425   STF 707     AE: SEI 270.                                                            Nsn2017a
05282+3349   ES  282     Not found by Heintz at old ES location (05296+3350).                    Hei1983a
                         Also known as TDS3205.                                                          
05282+0223   J    49     Too close 1951 with probable quadrant change (van Biesbroeck).          VBs1954 
05282-2046   BU  320     bet Lep = 9 Lep = Nihal                                                         
05283+0358   HJ 2266     BAL 2148.                                                                       
05284+8605   STF 573     B is BD+85@71.                                                                  
05284+3552   SEI 279     Primary not seen on POSS plate; may be flaw on AC Potsdam plate.                
05284+3549   SEI 273     B component spectral type A0:V:                                         AbH2000 
05284+3546   SEI 276     SEI 276AC incorrectly identified in WSI2008. This is actually the new           
                         pair WSI  40BD which is the same as ALI  74 with a quadrant flip.               
05284+3523   HJ 6999     SEI 271.                                                                Nsn2017a
05284+3447   SEI 272     MLB 1040.                                                                       
05285-1131   GAL 386     Object #186 in Gallo's original list.                                   Gal1914 
05285-7104   OGL 368     LMC164.2.33139 + LMC164.2.33650                                         Pli2012 
05287-0823   HJ 2268     Same as STF 722.                                                                
05287-6527   RST 137     The primary is AB Dor, a rapidly rotating, spotted star which shows             
                         both X-ray flares and microwave emission.                                       
             CLO  10     Aa,Ab: Close et al. discovered a companion to the A component at a      Clo2005 
                         separation of 0".156, which they refer to as the A and C components             
                         (the companion was labelled as C when detected as an astrometric                
                         reflex motion of AB Dor in observations by VLBI and Hipparcos).                 
                         Based on the astrometric orbit and the AO resolution, the mass of the           
                         Ab companion is estimated at 0.090 +/- 0.005 Msun, just above the mass          
                         of a brown dwarf. AO spectroscopy yields a spectral type of M8 +/- 1.           
                         Mass of Aa & Ab = 0.90(0.08) & 0.090(0.008) \msun. Model comparison     Azu2017 
                         gives age of Aa & Ab = 40-50 Myr & 25-120 Myr.                                  
             SHY  27     AC: HIP  25647 + HIP  31878. C component = C component of 06225-6013            
                         and 06380-6132.                                                                 
                         AD: HIP  25647 + HIP  22738. D component = A component of 04535-5551.           
                         AE: HIP  25647 + HIP  26373. E component = A component of 05369-4758            
                         = D component of 06225-6013.                                                    
             CLO  10     Ba,Bb: Close et al. also resolved the B component into a 66mas pair.    Clo2005 
                         Spectral types of Ba and Bb are estimated by Janson et al. at M5 and    Jnn2007 
                         M5-6, masses at 0.13-0.2 and 0.11-0.18 Msun.                                    
                         Aa is a rapidly-rotating spotted star (0.09 mag variability in V).      Boc2008 
                         Close et al. (2007) find spectral types for Aa, Ab, Ba, and Bb of K1,   Clo2007b
                         M5.5 +/- 1.0, M3.5 +/- 1.5, M4.5 +/- 1.5. Masses are 0.865 +/- 0.034,           
                         0.090 +/- 0.005, <0.25, <0.15 Msun; the system age is 75 +/- 25 Myr             
                         and the distance 14.9 +/- 0.1 pc.                                               
                         Ba,Bb: Wolter et al. (2014) made a multiwavelength study of AB Dor              
                         Ba,Bb. They derive effective temperatures 3260-3360 and 3200-3300K for          
                         Ba and Bb, respectively. Predicted system mass is 0.45-0.71 Msun,               
                         age 50-100 Myr.  (Ed note: Inclination for Wolter et al orbit (182deg)  WoU2014 
                         appears to be off by 90deg; changed to 92deg in orbit catalog)                  
                         Ba,Bb: Azulay et al. (2015) derive an orbit for AB Dor B, yielding a            
                         parallax of 66.4 +/- 0.5 mas, as well as component masses for Ba and            
                         Bb of 0.28 +/- 0.05 and 0.25 +/- 0.05 Msun.                             Azu2015 
05289+1233   LDS6186     NLTT 15139/15142                                                        Chm2004 
             TOK  94     HIP 25662. Mini-cluster. A is SB and astrometric pair (Vogt et al.)     CPS2002 
                         P = 1427d, M2 = 0.18 Msun. The system is thus a new quadruple.          Tok2011a
                         AB: Primary is SB1O, P=1426.7d (Katoh et al. 2013 AJ 145, 41)           Tok2014d
05290+3629   SEI 292     No star matching the position of the purported primary is seen on POSS          
                         plates, although another star is found at ~127deg, 15" from the SEI             
                         secondary. It is uncertain whether this pair is the SEI pair, although          
                         none of the stars in the vicinity appear to have large proper motion.           
05290+1707   BPM 132     [PM2000]  258672 + [PM2000]  258702.                                    Gvr2010 
05290-0442   WEB   4     A is the Mira-type variable S Ori. B is -04@1144.                               
05290-2237   HDO  69     HDO  71.                                                                        
05291+1152   BGR   1     GW Ori.                                                                         
05292-6749   OGL 369     LMC166.5.30    + LMC166.5.499                                           Pli2012 
05293+2509   STF 716     118 Tau.                                                                        
                         AB: H 2  75.                                                            MEv2010 
05293-2517   WHI   7     Listed as possibly resolved by White et al. (1991).                     Whi1991 
05294+3126   SHY 481     AC: HIP  25711 + HIP  25614.                                                    
05294+1152   HER   1     This is the T-Tauri variable V649 Ori = HBC 86.                                 
                         1980.95: Marginal evidence for additional component with separation             
                         0".47, pos. angle 36 or 216 deg.                                        Bai1985b
05294-0716   H 5 101     H V 101.                                                                        
05294-6849   OGL 370     LMC167.8.42748 + LMC167.8.42773                                         Pli2012 
05295+1257   JOY   8     Additional notes may be found in Herbig (1962).                         Her1962 
05296+3045   KU   88     B is BD+30@910.                                                                 
05296+1534   LDS6187     NLTT 15154/15153                                                        Chm2004 
05296+0309   STF 721     A,BC: H 4  45.                                                          MEv2010 
05297+6355   MLR 128     Also known as TDS 174.                                                          
05297+3523   HU  217     A is the Beta Lyrae-type system, LY Aur, P = 4.00d.                             
                         The classification is from Drechsel et al. (1989 A&A 221, 49). Howarth          
                         et al. (1997 MNRAS 284, 265) give Delta m for both spectroscopic and            
                         astrometric components.                                                 Msn1998a
05297+3327   S   484     B is BD+33@1063.                                                                
05297-0106   STF 725     31 Ori. A is the variable CI Ori.                                               
05298+1825   HJ 3275     STTA 64.                                                                        
05298-6904   OGL 371     LMC168.5.10887 + LMC168.5.10884                                         Pli2012 
05298-7154   OGL 372     LMC172.8.80    + LMC172.8.234                                           Pli2012 
05300+1214   HER  13     Additional notes may be found in Herbig (1962).                         Her1962 
05301+2933   STF 719     AC: H 4 110.                                                            MEv2010 
05301-3228   B  1946     Not seen for certain 1951-1967.                                                 
05302+4145   A  1720     A measure by A 1907.8, 259@, 1.9".                                              
05302+2438   POU 688     Aka KPP 122.                                                                    
05302-4705   HJ 3767     A,BC: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
05303-0247   J     7     Magnitude of A noted as 9.7 in 1909 and 8.7 in 1910. Other variations           
                         observed since then.                                                    J__1952 
05303-2331   B  2587     Spectrum: Fm delta Del.                                                         
05303-5359   JNN  38     The AstraLux images resolve this system into a likely triple, where             
                         all components have brightnesses and colors consistent with a                   
                         physically bound system. Since it has only been observed in one epoch,          
                         common proper motion has not yet been established.                      Jnn2012 
05303-6653   HJ 3779     AC: Whole in nebulous haze.                                             Hln1965 
05305+3239   ES  335     SEI 313.                                                                Nsn2017a
05307+5521   MLR 687     Also known as TDS 175.                                                          
05308+3950   STTA 63     B is BD+39@1321.                                                                
05308+0557   STF 728     32 Ori. The motion is still practically rectilinear, as represented     B__1956b
                         in formulae by van den Bos (1956) and Cester  (1964).                   Ces1964a
                         Uniform disk diameter  0.196 +/- 0.015 mas,                                     
                         Limb darkened diameter 0.200 +/- 0.015 mas,                                     
                         Teff = 15700 +/- 500 K based on SED.                                            
                         Radius is 2.33 +/- 0.25 \rsun.                                          CIA2019a
                         H 1  25.                                                                MEv2010 
                         Probably optical.                                                       B__1962d
05308-0022   A   852     Appears to be in rapid motion. This is the variable V1093 Ori.                  
05308-0034   CBL 228     GWP 684.                                                                Tob2012b
05308-1251   BRT2644     RST 3426. BRT identifies this as BD-12@1187.                                    
05310+0440   A  2646     AB: Rectilinear solution by Rica & Zirm (2012).                         FMR2012i
05311+4255   A  1721     Too close 1924-1931. This interval may mark a possible quadrant change          
05312+0318   STF 729     33 Ori = n 1 Ori. 1945.16 : Measure unpublished in orbit quotation.             
                         AB: H 1  22.                                                            MEv2010 
05312-7134   OGL 373     LMC172.6.6648  + LMC172.6.6645                                          Pli2012 
05314-0336   ENG  20     Proper motion of A +774 -2090. B is BD-03@1122, PM -013-041.                    
05314-0724   TUV   1     Primary is an F5V W UMa eclipsing binary, while B is redder and about           
                         1 mag fainter. At the derived distance of 600-800 pc, the physical              
                         separation of A and B would be more than 1000 au. The authors conclude          
                         it is unlikely the stars are bound.                                     Tuv2008 
05314-7110   OGL 374     LMC171.7.13103 + LMC171.7.13105                                         Pli2012 
05315+5439   STF 711     AB: HJL  70.                                                            HJL1986 
05315-6749   OGL 375     LMC166.4.145   + LMC166.4.337                                           Pli2012 
05316-0953   LDS 145     LDS 844 = LDS6188.                                                              
05316-1512   GAL 387     Object #188 in Gallo's original list.                                   Gal1914 
05317+1720   BPM 133     [PM2000]  263884 + [PM2000]  263996.                                    Gvr2010 
05317+0006   TOK  96     HIP 25905.  A is SB without orbit.                                      Nrd2004 
05318-7128   OGL 376     LMC172.5.13529 + LMC172.5.13581                                         Pli2012 
05319+7548   LDS1612     BVD 302.                                                                        
05319-7620   HJ 3795     gam Men                                                                         
05320+1118   V1410 Ori   Noted as possible binary (separation > 0".020) by Baines et al. (2006)  Bns2006 
05320-0018   HEI  42     del Ori = Mintaka. A is an Algol-type system, as well as a close                
                         visual binary.                                                                  
                         Aa,Ab: Orbital elements are also given by Levato et al. (1988). This    Lev1988 
                         close visual pair has increased in separation from 0".20 to 0".29               
                         between 1979 and 1994. The spectral classification for the C component  Lev1991b
                         is from Morrell & Levato (1991).                                        Msn1998a
                         Aa spectral type O9.5II+B2V. Ab spectral type B0IV.                     Opl2023 
             STFA 14     C is a spectroscopic binary.                                                    
                         Ca is spectral type B3V, Cb is spectral type A0V.                       Opl2023 
                         AC: H 5  10.                                                            MEv2010 
05321-0305   JNN  39     V1311 Ori.                                                                      
                         2MASS J05320450-0305291 is identified as a beta Pic member in da Silva          
                         et al. (2009 A&A 508, 833). It is also known as V1311 Ori.              Jnn2012 
05321-0506   DOO  34     Doolittle identifies this as BDS 2801, but evidently it is a different          
                         pair.                                                                   Doo1923 
05321-1452   GAL 388     Object #190 in Gallo's original list.                                   Gal1914 
05322+1703   STF 730     A is a spectroscopic binary.                                                    
                         H N 124.                                                                MEv2010 
05322-0431   RAS  19     Includes the rotationally variable star V1101 Ori. Companion estimated          
                         as close to G5V; mass of system perhaps 7 Msun.                         Ras2014 
05323+0217   A  2509     Not seen 1913-1936, when about 100@ of orbital motion took place.               
                         Rectilinear solution by Rica & Zirm (2012).                             FMR2012i
05324+0132   SKF1047     These two T Tauri stars are V1884 Ori + V1883 Ori.                      Skf2012 
05324-0624   ENG  21     B is BD-06@1211.                                                                
05324-1458   GAL 389     Object #191 in Gallo's original list.                                   Gal1914 
05326+1700   BPM 134     [PM2000]  265797 + [PM2000]  266129.                                    Gvr2010 
05327-0136   BU 1048     A is variable.                                                                  
05327-1749   HJ 3766     alp Lep = 11 Lep = Arneb                                                        
                         NPOI Limb-darkened diameter 1.77 +/- 0.09 mas,                          NOI1999 
                         R = 74.  +/- 22. \rsun.                                                         
05327-6758   OGL 377     LMC166.3.14    + LMC166.3.52                                            Pli2012 
05330-2415   DAW  85     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.69 +/- 0.65, 1.66, and 0.79 Msun, respectively.             Mlk2012 
05330-6414   28 Dor      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Lunt (1924).                                                            Lun1924 
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Lunt (1924).                                                            Lun1924 
05331+2002   A  2434     HIP 26018. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc. Aka J  2606.                             
05331-0143   STF 734     H V 119.                                                                        
                         AC: H 5 119.                                                            MEv2010 
05332+1557   TOK  97     HIP 26027. Two companions are seen in the ANDICAM images.               Tok2011a
05332-6501   TOK  98     HIP 26030.                                                              Tok2011a
05333+4449   AST   3     G 96-45 = GJ 1081.                                                              
05334+1220   GIC  59     G097-049/G097-048 = Ross 43.                                                    
                         NLTT 15271/15272                                                        Chm2004 
05334-6847   OGL 378     LMC167.2.15319 + LMC167.2.15443                                         Pli2012 
05335-2420   HJ 3770     AB closed down from 12" in 1835 to 3.8" in 2MASS. Physical?             Tok2014d
05336-6956   OGL 379     LMC169.2.19326 + LMC169.2.19557                                         Pli2012 
05337+0157   LWR   6     V371 Ori                                                                        
05340-6814   OGL 380     LMC166.1.16552 + LMC166.1.16697                                         Pli2012 
05341-0102   H 5 118     H V 118. Wendell noted a possible companion to the south of A in                
                         1869.08, although "separation doubtful".                                Wen1882 
05341-1422   HLD  76     There must be some error in my single night's distance of AB in 1958.   B__1963b
05342+1019   LDS6189     This is the common proper motion pair Ross 45.                                  
05342-7120   OGL 381     LMC172.4.30962 + LMC172.4.31134                                         Pli2012 
05343+0346   STT 110     38 Ori                                                                          
05344+3549   AG   95     SEI 328.                                                                Nsn2017a
05344+0227   J  2002     BAL 1675.                                                                       
05345+3727   SEI 330     The 05345+3727SEI 330 system is actually 2 close doubles (33" apart).           
                         Most of the confirming measures were of the other, previously                   
                         uncataloged pair, 05345+3726SEI 332. Thanks to Ed Wiley for bringing            
                         this to our attention.                                                          
05346-0528   REP  51     V1438 Ori                                                                       
05346-0543   JNN  40     V1000 Ori.                                                                      
                         2MASS J05343767-0543044 has been classified as a likely member of the   Jnn2012 
                         ~1 Myr Orion OBIc/d association (Stassun et al. 1999 AJ 117, 2941).             
                         The companion that was detected with AstraLux has not yet been                  
                         confirmed to share a common proper motion, but its brightness and               
                         color are consistent with what would be expected for a physical                 
                         companion, hence it is counted as such in the statistical analysis.     Jnn2012 
05346-6836   OGL 382     LMC167.3.17320 + LMC167.3.18302                                         Pli2012 
05347-0520   REP  53     V1441 Ori = JW 63. Correia et al. (2014) derive the following                   
                         properties: spectral types M0.5 +/- 0.5 and M3.0 +/- 1.0, Teff 3777             
                         +/- 72 and 3415 +/- 145K, radii 2.2 +/- 0.3 and 1.7 +/- 0.2 Rsun.               
                         Masses and ages are determined for several published PMS tracks.        Cor2013 
05347-0534   REP  55     V1118 Ori                                                                       
05347-0545   SKF2420     MGM1241. IZ Ori.                                                        Kkl2016 
05347-6857   OGL 383     LMC167.1.20073 + LMC167.1.20205                                         Pli2012 
05348+0929   MCA  20     phi 1 Ori = 37 Ori. This speckle observation probably represents the            
                         known spectroscopic binary with P = 8.4y.                                       
05348-0524   GET   1     V1454 Ori                                                                       
05348-0525   REP  56     JW 81. Correia et al. (2014) derive the following properties:                   
                         spectral types M1.0 +/- 0.5 and M3.5 +/- 1.0, Teff 3705 +/- 72 and              
                         3442 +/- 72K, radii 2.0 +/- 0.3 and 1.1 +/- 0.1 Rsun.                           
                         Masses and ages are determined for several published PMS tracks.        Cor2013 
05348-0536   MDF   5     V2034 Ori.                                                                      
05348-0600   STF 745     H 3  13.                                                                Bu_1906 
05348-3240   JNN  41     All components of this triple system have colors and brightnesses               
                         consistent with expectation for physical companions. Common proper              
                         motion has however not yet been demonstrated.                           Jnn2012 
05349+0006   OL  178     Aka RST5217.                                                                    
05349-0007   STF 741     H 3  76.                                                                MEv2010 
05349-0523   REP  60     V1458 Ori = JW 128. Correia et al. (2014) derive the following                  
                         properties: spectral types M3.0 +/- 1.0 and M3.0 +/- 1.0, Teff 3415             
                         +/- 145 and 3415 +/- 145K, radii 2.4 +/- 0.2 and 2.2 +/- 0.2 Rsun.              
                         Masses and ages are determined for several published PMS tracks.        Cor2013 
05349-0530   REP  61     V1460 Ori                                                                       
05350+1544   HEI  43     Heintz reports a third star at 283 deg, 40".                            Hei1980a
05350-0518   MDF   8     V2120 Ori.                                                                      
05350-0522   MDF   2     V404 Ori.                                                                       
05350-0524   GET   3     AB: JW 176. Correia et al. (2014) derive the following properties:              
                         spectral types M1.0 +/- 0.5 and M1.0 +/- 0.5, Teff 3705 +/- 72 and              
                         3705 +/- 72K, radii 2.9 +/- 0.2 and 3.2 +/- 0.5 Rsun.                           
                         Masses and ages are determined for several published PMS tracks.        Cor2013 
05350-0529   REP  66     V1320 Ori                                                                       
05350-0600   STF 747     STFA 15. B is BD-06@1233.                                                       
                         AB: H 3  14.                                                            MEv2010 
05351+2006   J  2606     Jonckheere unable to recover.                                           J__1962a
05351+0956   STF 738     lam Ori = Meissa                                                                
                         Both A and B components were observed and appeared to be single. The            
                         AB pair may not be physical (Lindroos). The photometry-based            Lnd1985 
                         classification of the C component is from Lindroos, who also gives a            
                         distance of 430 pc.                                                     Msn1998a
                         Classification of the B component is from Hoffleit & Warren (1991).     Hof1991 
                         AB: The image rotator was in an unknown state, so two possible theta            
                         values are listed for the 2001.7428 observation - one for zenith up             
                         and one for north up.                                                   Trn2008 
                         AB: H 2   9.                                                            MEv2010 
                         Uniform disk diameter  0.219 +/- 0.015 mas,                                     
                         Limb darkened diameter 0.228 +/- 0.009 mas,                                     
                         Teff = 36,000 +/- 900 K, Radius is 10.2 +/- 1.3 \rsun.                  CIA2018e
05351-0124   RAS  20     SrCrEu star; secondary probably early-K. System may belong to the               
                         Orion OB1 association.                                                  Ras2014 
05351-0508   JNN  42     V1321 Ori.                                                                      
                         This star has been classified as a probable T Tau star in Alcala et             
                         al. (1996 A&AS 119, 7). It is also known as V1321 Ori.                  Jnn2012 
05351-0523   GET   4     AB: V1274 Ori = JW 248. Correia et al. (2014) resolved a close (0".14)          
                         faint (dm=3mag) companion to the primary, and derive the following              
                         properties for Aa and B: spectral types M1.0 +/- 0.5 and M7.5 +/- 1.5,          
                         Teff 3705 +/- 72 and 2795 +/- 295K, radii 3.5 +/- 0.4 and 2.4 +/- 0.8           
                         Rsun. Masses and ages are determined for several published PMS tracks.  Cor2013 
05351-0532   MGM1501     LM Ori.                                                                 Kkl2016 
05351-0534   SKF2257     MGM1454. V982 Ori.                                                      Kkl2016 
05351-0551   MGM1171     V2134 Ori.                                                              Kkl2016 
05352+1014   STT 111     The primary is a single-lined spectroscopic binary, P = 1857d.                  
05352+0954   BYN   1     Separation and position angle calculated from tabulated RA and DEC of           
                         components. Quoted date and telescope aperture are rough means of all   ByN2007a
                         listed information in Barrado y Navascues et al. (2007).                ByN2007b
05352-0513   MGM2239     V2327 Ori.                                                              Kkl2016 
05352-0515   MGM2193     V2359 Ori.                                                              Kkl2016 
05352-0516   REP  72     Ba,Bb: V1492 Ori                                                                
05352-0517   REP  77     AB: V1329 Ori                                                                   
             KOH  98     DE: V1327 Ori                                                                   
05352-0521   REP  74     Ba,Bb: JW 391. Correia et al. (2014) derive the following properties:           
                         spectral types M0.0 +/- 0.5 and M7.0 +/- 1.0, Teff 3850 +/- 53 and              
                         2880 +/- 140K, radii 2.0 +/- 0.1 and 1.4 +/- 0.2 Rsun.                          
                         Masses and ages are determined for several published PMS tracks.        Cor2013 
05352-0522   GET  20     FG: V1496 Ori                                                                   
05352-0523   GET   9     DE: V1487 Ori                                                                   
             GET  25     NO: V1330 Ori                                                                   
             PRS   8     PQ:SMN   3Da,Db                                                                 
05352-0524   PRS   9     Aa,B:  Aka GET  28.                                                     Skf2016a
                                Aka PAD   1.                                                     Dam2017k
05352-0529   REP  76     V1495 Ori                                                                       
05352-0534   MDF   4     V2265 Ori.                                                                      
05352-0537   REP  79     V1500 Ori                                                                       
05352-0538   REP  80     V409 Ori                                                                        
05353-0515   REP  84     V1334 Ori                                                                       
05353-0520   HJ 1157EF   Aka POP 205.                                                                    
05353-0522   GET  45     NO: V1333 Ori                                                                   
             PRS  18     Ka,Kb: DAE  13Oa,Ob                                                             
05353-0523   STF 748     A: the 1 Ori A = 41 Ori A = V1016 Ori                                           
                         B: the 1 Ori B = 41 Ori B = BM Ori                                              
                         C: the 1 Ori C = 41 Ori C                                                       
                         D: the 1 Ori D = 41 Ori D                                                       
                         Trapezium. the Ori A, B, and C were first noted as a triple by          G__1617 
                         Galileo on 4 February 1617. It was independently found as a triple in           
                         by Christian Huygens, who is often given credit for recognizing this            
                         multiple system. the Ori D was found by Abbe Jean Picard, as            A__1935f
                         documented by a manuscript drawing of 20 March 1673. The D component            
                         was independently found by Huygens in 1684.                                     
                         A and B are both Algol-type systems, C is an RW Aur-type system.                
                         Common proper motion with the multiple system STF 16.                           
                         Stahl et al. (1996 A&A 312, 539) find that the H-alpha profiles of the          
                         C component vary with a 15.4-day cycle which they suggest is related            
                         to the star's rotational period; photospheric line radial velocity              
                         variations are small. All 4 of the Orion Trapezium stars were observed          
                         with the speckle camera (A = HD 37020; B =  HD 37021; C = HD 37022;             
                         D = HD 37023) and all appeared to be single. Classifications of the             
                         B and D components are from the WDS.  The spectral classification for   Lev1991b
                         the A component is from Morrell & Levato (1991).                        Msn1998a
                         AB: H 3   1.                                                            MEv2010 
                         AC: C component = D component of 05354-0525 STFA 17.                            
             WGT   1     Ca,Cb: The longer-period Kraus et al. (2007) solution gives a dynamic           
                         parallax 2.304 +/- 0.066 mas, the shorter-period solution gives 2.585           
                         +/- 0.074 mas. Mass sums are 47.8 +/- 4.2 and 44.8 +/- 3.9 Msun,                
                         respectively. Based on evolutionary models, spectral types for Ca and           
                         Cb are O5.5 and O9.5, masses are 34.0 and 15.5 Msun.                    Kss2007 
                         The Kraus et al. (2009) solution is based on VLTI data from 2007-2008,          
                         plus speckle (1997-2008) and radial valocity data. They derive a                
                         dynamic distance of 410 +/- 20pc and a system mass of 44 +/- 7 Msun.    Kss2009 
                         Ca,Cb: From their combined astrometric/spectroscopic solution, Balega           
                         et al. (2015) derive the following properties for the system:                   
                            total mass (Msun): 45.5 +/- 10.0                                             
                            mass ratio:        0.36     0.05                                             
                            distance (pc):     414      7                                                
                            flux ratio:        0.30     0.05                                             
                         Resulting properties for the two components are:                                
                            mass (Msun):       33.5 +/- 5.2      12.0 +/- 3.0                            
                            log L:             5.21     0.01     4.70     0.15                           
                            Spectral types:    O6Vp              B0V                                     
                            Teff               39000    1000     30000    1000                           
                            radii (Rsun):      8.91     0.50     8.24     0.50                   Bag2015 
             STF 748     CH: Additional notes may be found in Burnham (1894).                    Bu_1894 
             KSS   1     D component of ADS 4186 = the 1 Ori D                                           
05353-0523   PTR   1     Ab is a 4 solar mass PMS F star.                                        Gvt2018 
05353-0523   GVT   1     Be is a 4-6 solar mass B star.                                          Gvt2018 
05353-0523   GVT   1     Dc is a 5-7 solar mass B star.                                          Gvt2018 
05353-0523   DAE 130     Oa,Ob: The elongated shape of JW 519's primary suggests the primary to          
                         be binary itself. The photometry for JW 519, however, is based on the           
                         assumption of a single central object since separate components cannot          
                         be identified.                                                          Dae2012 
             GET  43     TU: the 1 Ori G                                                                 
             REP 110     Xa,Xb: AF Ori                                                                   
05353-0524   GET  38     FG: AC Ori                                                                      
05353-0531   MDF   3     V2360 Ori.                                                                      
05353-0533   REP  81     V1504 Ori                                                                       
05354-0450   DA    4     AB + TOK 430Aa,Ab: This is HIP 26237, HD 37018, HR 1892, 42 Ori, a              
                         young star in Orion which has not been observed at high angular                 
                         resolution so far, according to INT4 (Hartkopf et al. 2001). We         Hrt2001d
                         resolved the known binary DA 4AB and discovered the spectacular                 
                         subsystem Aa,Ab at 0".16.                                               Tok2015c
05354-0509   KOH 101     V1344 Ori                                                                       
05354-0510   MGM2300     V2377 Ori.                                                              Kkl2016 
05354-0515   MDF   7     V1281 Ori.                                                                      
05354-0524   PRS  34     AB: V1524 Ori                                                                   
             GET  56     CD: V494 Ori                                                                    
             GET  57     GH: V1231 Ori                                                                   
05354-0525   STFA 16     A: the 2 Ori A = 43 Ori. Spectroscopic binary, P = 21d.                         
                         B: the 2 Ori B = BD-05@ 1320.                                                   
                         C component is primary of 05355-0525 S   490.                                   
             STFA 17     AD: This is the the 1 / the 2 Ori system                                        
                         D component = C component of 05353-0523 STF 748.                                
             CHR 249     The A component (CHR 249 Aa,Ab) was resolved on 3 occasions, but the            
                         distant STFA 17B component was observed to be single.  Hipparcos        HIP1997b
                         results confirm the Aa,Ab pair.  The spectral classification for        Lev1991b
                         the B component is from Morrell & Levato (1991).                        Msn1998a
                         Classification of the C component is from Hoffleit et al. (1983).       Hof1983 
05354-0527   REP  89     JW 709. Correia et al. (2014) derive the following properties:                  
                         spectral types M0.5 +/- 0.5 and M0.5 +/- 0.5, Teff 3777 +/- 72 and              
                         3777 +/- 72K, radii 1.8 +/- 0.1 and 1.7 +/- 0.2 Rsun.                           
                         Masses and ages are determined for several published PMS tracks.        Cor2013 
05343-0530   DCH 112     WZ Ori                                                                          
05347-0523   DCH 102     IX Ori                                                                          
05350-0530   DCH 103     Ca,Cb: KZ Ori                                                                   
05351-0518   DCH 104     V2144 Ori                                                                       
05352-0522   DCH 106     Qa,Qb: V1487 Ori                                                                
05353-0518   DCH 109     Ca,Cb: V1509 Ori                                                                
05353-0523   DCH 110     Oa,Ob: MT Ori                                                                   
05354-0525   GVT   2     Ac is a 8-12 solar mass companion.                                      Gvt2018 
05354-0525   GVT   2     Bb is a 1.6 +/- 0.7 solar mass companion.                               Gvt2018 
05354-0525   GVT   2     Cb is a 1.7 +/- 0.2 solar mass companion.                               Gvt2018 
05354-0527   DCH 111     Ca,Cb: V1523 Ori                                                                
05354-0532   REP  91     V1528 Ori                                                                       
05354-0535   CHN  14     Also known as AG Ori. The secondary = V2378 Ori.                                
05354-0555   STF 752     iot Ori = 44 Ori = Hatysa. A is a spectroscopic binary, P = 29.1d.              
                         The classification is from Stickland et al. (1987).                     Stc1987 
             CHR 250     The A component was resolved (CHR 250 Aa,Ab); the B component was also          
                         observed but appeared to be single.                                     Msn1998a
                         Aa1 is spectral type O8.5III, Aa2 is B0.8III and Ab is B2IV.            Opl2023 
                         Classification of the B component is from Hoffleit & Warren (1991).     Hof1991 
             STF 752     AB: H 3  12.                                                            MEv2010 
05355-0422   STF 750     H 2  26.                                                                MEv2010 
05355-0459   MGM2472     V2475 Ori.                                                              Kkl2016 
05355-0504   SKF2481     MGM2398.                                                                Kkl2016 
05355-0505   MGM2367     V2502 Ori.                                                              Kkl2016 
05355-0509   KOH 104     V360 Ori                                                                        
05355-0510   RBB   7     MGM2285. V419 Ori.                                                      Kkl2016 
05355-0515   DCH 113     V1432 Ori                                                                       
05355-0516   PBS   2     NU Ori, not nu Ori.                                                             
             GVT   3     Ab is a 4 +/- 1 solar mass companion.                                   Gvt2018 
05355-0519   REP  96     JW 867. Correia et al. (2014) derive the following properties:                  
                         spectral types M0.5 +/- 0.5 and M1.5 +/- 0.5, Teff 3777 +/- 72 and              
                         3632 +/- 72K, radii 2.2 +/- 0.1 and 2.2 +/- 0.1 Rsun.                           
                         Masses and ages are determined for several published PMS tracks.        Cor2013 
05355-0524   GET  60     V1288 Ori                                                                       
05355-0525   S   490     Variable, V361 Ori. Primary is C component of 05354-0525 STFA 16AC              
05356+3801   AG   98     HDS 746.                                                                        
05357-0451   HLD 173     45 Ori.                                                                         
05357-0528   KOH 105     AN Ori                                                                          
05358-0059   STF 751     B is BD-01@966.                                                                 
05358-0529   HLB   1     T Ori.                                                                          
05359+3530   SHY 483     AB: HIP  26290 + HIP  26322.                                                    
             SHY 476     BC: HIP  26322 + HIP  24934.                                                    
05359-0538   DA    3     A is a spectroscopic binary and light variable.                                 
05360+3614   SEI 349     Heintz equates this with ALI 308.                                       Hei1985a
05360-0616   JNN  43     V1178 Ori.                                                                      
                         Also known as V1178 Ori, this star has been classified as a probable T          
                         Tau star in Alcala et al. (1996 A&AS 119, 7). It has a companion that           
                         is as of yet unconfirmed with regards to common proper motion, but              
                         since the brightness and color are well consistent with expectations            
                         for a real companion, system is counted as binary in the statistics.    Jnn2012 
05360-7136   OGL 384     LMC172.3.13633 + LMC172.3.13778                                         Pli2012 
05361-1302   LDS3666     NLTT 15358/15357                                                        Chm2004 
05362-0112   BUP  81     eps Ori = 46 Ori = Alnilam. Possibly variable.                                  
05362-1349   WEI   9     B is BD-13@1193.                                                                
05362-2842   SHY 484     HIP  26309 + HIP  26453.                                                        
05363-0018   RAS  21     Triple includes the alpha2 CVn type variable star V1130 Ori.  Spectral          
                         types of B estimates as A7; uncertainty in magnitude does not allow             
                         estimate of specral type for C. Member of Orion OB1 association.        Ras2014 
05364+3408   STF 737     B is BD+34@1106.                                                                
                         SEI 353.                                                                Nsn2017a
05364+2200   STF 742     A premature orbit has been computed.                                            
                         The node and longitude of periastron have been corrected.                       
                         H 1  70.                                                                MEv2010 
05364-7056   OGL 385     LMC171.3.62055 + LMC171.3.62082                                         Pli2012 
05365+2556   CHR 203     First detected as an occultation binary by Schmidtke et al.             Smk1989 
05365+1120   TOK 255     V2689 Ori.                                                                      
05365-0643   J   798     Center of nebula NGC 1999 = H IV 33. Couteau did not find the           J__1912d
                         Jonckheere AC component. The two components may in fact be the same.    Cou1960a
                         Same as COU2713.                                                                
                         The A component is the RW Aur-type variable V380 Ori.                           
05366-0604   STF 754     A is a spectroscopic binary.                                                    
                         H 3  13.                                                                MEv2010 
05366-1029   GAL 390     Object #193 in Gallo's original list.                                   Gal1914 
05367-0634   SKF2301     MGM 845. V846 Ori.                                                      Kkl2016 
05367-6904   OGL 386     LMC175.5.5552  + LMC175.5.5551                                          Pli2012 
05367-6930   I  1151     An S Doradus-type variable, R127, in the LMC.                                   
05368-1003   GAL 391     Object #194 in Gallo's original list.                                   Gal1914 
05369-4758   HDS 751     See notes to 05287-6527 SHY  27AE and 06225-6013 SHY  34AD.             Shy2011 
05370+2044   GJ 209      Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from Vogt et al.  CPS2000c
                         (2000).                                                                 HaI2001 
05370-0137   HDO  76     According to Burnham (1906) original measure is labelled "doubtful".    Bu_1906 
05370-6851   OGL 387     LMC174.8.25249 + LMC174.8.25968                                         Pli2012 
05371+2655   BOW   4CD   Aka ITF   4.                                                                    
05371-3932   YMG  11     AT Col.                                                                         
05372+7928   MLR 492     Also known as TDS 187.                                                          
05372+1014   BPM 135     [PM2000]  278391 + [PM2000]  278458.                                    Gvr2010 
05372-2424   B    84     HIP 26404. AB = B 84 = ADS 4227, 3". The pair is optical according to           
                         the CMDs (B is too red, above the MS). Small PM(A)=(+13,-14). However,          
                         the field is not crowded, N*=14, an optical companion at 3.5" is                
                         unlikely. Is B an IR companion? No relevant references in SIMBAD.       Tok2011a
05373+6409   HU 1107     19 Cam.                                                                         
05373-6857   OGL 388     LMC174.8.25010 + LMC174.8.31202                                         Pli2012 
05375+3147   WZ   10     SEI 356.                                                                Nsn2017a
05375-7138   OGL 389     LMC179.7.17322 + LMC179.7.17360                                         Pli2012 
05376+3705   RAO 499     V432 Aur.                                                                       
05376+2659   ITF   3     Aka ITF  35.                                                                    
05377+1618   BPM 136     [PM2000]  280129 + [PM2000]  280138.                                    Gvr2010 
05377-5330   HJ 3786     Spectrum of A is F/G.                                                           
05378-5434   HJ 3787     B is CPD-54@866.                                                                
05379+0058   STTA 65     Pair appears in an appendix list, not part of the discoverer's regular          
                         numbering sequence.                                                             
05380+1631   BPMA 11     [PM2000]  280939 + [PM2000]  280294.                                    Gvr2010 
05381-0011   STF 758     CD : Same as STF 765.                                                           
                         CD: H 3 111.                                                            MEv2010 
05382-0649   AUN   1     V1787 Ori.                                                                      
05382-4606   HJ 3784     HIP 26501. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
05383-7135   OGL 390     LMC179.6.5087  + LMC179.6.5328                                          Pli2012 
05384+4301   A  1563     Less than 0.1" with 82-inch 1953, 1954.                                         
                         A premature orbit has been computed.                                            
05384+3401   SMR  56     Pair initially designated SMR 55 in error, designation already in use.          
05384+1124   BPM 137     [PM2000]  282231 + [PM2000]  282180.                                    Gvr2010 
05384-6951   OGL 391     LMC176.7.81530 + LMC176.7.81923                                         Pli2012 
05386+3030   BU 1240     26 Aur. Composite spectrum; B9.5V+F9III. Light variability suspected.           
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Only elements P and T have been amended by Starikova (1977) from the    Sta1977a
                         orbit of Baize (1956).                                                  Baz1956 
                         Romero (2008) estimates masses of the A and B components as 2.1 +/-     FMR2008 
                         1.0 and 3.0 +/- 0.4 Msun, respectively; spectral types are G8III and            
                         A1IV or B9.5V.                                                                  
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 6.87 +/- 22.98, 5.45, and 4.82 Msun, respectively. Mlk2012 
             STF 753     Romero (2008) analyzes the optical/physical nature of the C component;  FMR2008 
                         the spectral is determined to be about A6V and it appears to be                 
                         gravitationally bound to the AB pair, with an estimated orbital period          
                         of ~46,000 years.                                                               
                         AB,C: H 3  64.                                                          MEv2010 
             BU   90     Romero (2008) derives a proper motion for D (+0.4 +/- 2.1 mas/yr in     FMR2008 
                         RA, -12.6 +/- 1.6 mas/yr in Dec) based on that of the AB pair plus the          
                         relative motion of AB,D between the years 1856 and 2002. He also                
                         concludes that D is optical, with a spectral type estimated at K1III            
                         and distance of ~870pc (both determinations corrected for reddening).           
05386-0233   STF 761     AB: B is BD-02@1323.                                                            
                         Primary = F component of 05387-0236 STF3135AB,F.                                
                         BC: H 2  10.                                                            MEv2010 
05386-0244   PLT   1     A is TX Ori, B is TY Ori.                                               Plt1934 
05386-1655   UC 1338     CPM candidate confirmed physical by photometry (2MASS and V mags).      Tok2013c
05387-0236   STF3135     Rabe measures principal stars STF 761 and STF 762.                      Rab1923 
                         1914, 324@, 209.79". This new WDS entry created 02/18/98.                       
                         Spectral types of primary and secondary assigned by ten Brummelaar et   TtB2000 
                         al., based on adaptive optics observations.                                     
             BU 1032     sig Ori = 48 Ori. A is the variable V1030 Ori. This is the brightest            
                         pair in a trapezium system with at least five components, including             
                         components C (mag. 8.79, 11", A2V), D (mag. 6.62, 13", B2V), and the            
                         helium-rich star E, BD-02@1327. A has also been reported to be a short          
                         period SB2.                                                                     
                         Heintz (1974) gives formulae for the motions AB,C and AB,D.             Hei1974b
                         The suspected small RV variation of AB was not confirmed in David               
                         Dunlap Obs. spectra.                                                            
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         The AB pair has decreased in position angle from 171 deg to 125 deg             
                         between 1975 and 1994.  Fullerton (1990) describes three spectral       Ful1990 
                         components in the He I 5876 A profile which suggests that one of the            
                         stars is a double-lined spectroscopic binary  (see Bolton, 1974 ApJ             
                         192, L7).  Classifications of the B, C, and D components are from       Hof1991 
                         Hoffleit & Warren (1991), while the classification for the E            Lev1991b
                         component is from Morrell & Levato (1991).                              Msn1998a
                         AB: Additional notes may be found in Worley (1956).                     Wor1956b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 27.34 +/- 40.70, 25.32, 21.87 Msun, respectively.  Mlk2012 
             sig Ori     Aa,Ab: Simon-Diaz et al. (2015) derive a new spectroscopic orbit for            
                         the primary (sig Ori Aa,Ab) as well as astrometry and photometry for            
                         the AB pair. New values for mass, log g, age, Teff, etc are derived             
                         for Aa, Ab, and B.                                                      SiD2015 
             NOI   6     Aa,Ab: Schaefer et al. (2016) resolved the primary of sig Ori A and             
                         derive a new combined solution, as well as a new orbit of the AB pair.          
                         Derived masses for Aa, Ab, and B are 16.99 +/- 0.20, 12.81 +/- 0.18,            
                         and 11.54 +/- 1.15 Msun, respectively. They also derive a parallax of           
                         2.5806 +/- 0.0088 mas, corresponding to distance 387.51 +/- 0.12 pc.    NOI2016b
                         Spectral type of Aa 09.5V, Ab B0.5V                                     Opl2023 
             STF 762     AB,C: H 2  11.                                                          MEv2010 
                         Sigma Ori E (V1030 Ori) has a strong magnetic field and a magnetosphere IAU2014a
                         with two clouds of plasma constrained by magnetic and centrifugal               
                         forces which co-rotate with the 1.19d period of the star which results          
                         in eclipse features.                                                            
                         Note that the C component was first resolved by Dawes while D and E     Da_1835 
                         were first resolved by Mayer. However, the discovery designation is     MyC1784 
                         maintained due to the long standing historical designations.                    
             STF3135     AB,F: F component = primary of 05386-0233 STF 761.                              
             RAS  22     Ea,Eb: Helium star V1030 Ori, type B2; spectral type of Eb estimated            
                         as late-A.                                                              Ras2014 
             CAB  26     Ha,Hb: [W96] 4771-899 = Mayrit 528005                                           
             BOY  24     Ja,Jb: sig Ori IRS 1 = Mayrit 3020                                      Boy2009 
05387-6906   RMC 136     30 Dor cluster in Large Magellanic Cloud. Due to space limitations,             
                         component designations have been converted from the letter/number               
                         format (e.g., a1 or k10) adopted by Weigelt and collaborators to the    Wgt1985 
                         upper/lower case letter format (e.g., Aa or Kj) used in the WDS. The    Ner1988 
                         order of these components has not been changed, however. Of the 13      Peh1992 
                         companions discovered by Herschel, Dawes, and Innes, only the pair              
                         originally designated I  1152AB matches one of these close                      
                         interferometric pairs with any certainty; it has been merged with               
                         RMC 136Aa,Ac. Component designations for the others were adjusted.              
                         Results are tabulated from the combined data set only. RMS errors from          
                         comparing data sets are 0".011 in separation, 1.6 deg in position               
                         angle, 0.28 in magnitude difference.                                    Peh1992 
05388+1548   BPM 138     [PM2000]  283526 + [PM2000]  283334.                                    Gvr2010 
05388-0242   CAB  28     V595 Ori.                                                                       
05389+1651   BPMA 12     [PM2000]  283738 + [PM2000]  283905.                                    Gvr2010 
05389-0713   49 Ori      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Abt (1965).                                                             AbH1965 
05389-1334   GAL 392     Hipparcos suspected non-single.                                                 
                         Object #196 in Gallo's original list.                                   Gal1914 
05391+1747   BPM 139     [PM2000]  284438 + [PM2000]  284293.                                    Gvr2010 
05391-5008   HJ 3789     B is CD-50@1871.                                                                
05391-7100   OGL 392     LMC178.6.14067 + LMC178.6.15179                                         Pli2012 
05391-7149   OGL 393     LMC179.8.23263 + LMC179.8.23619                                         Pli2012 
05391-7157   OGL 394     LMC180.5.22705 + LMC180.5.23355                                         Pli2012 
05392+2317   STF 755     124 Tau. C is a spectroscopic binary.                                           
05393-6750   OGL 395     LMC173.4.13898 + LMC173.4.14451                                         Pli2012 
05394+1658   BPMA 13     [PM2000]  285302 + [PM2000]  285761.                                    Gvr2010 
05394+1649   BPMA 14     [PM2000]  285537 + [PM2000]  286099.                                    Gvr2010 
05394+1618   BPM 140     [PM2000]  285398 + [PM2000]  285298.                                    Gvr2010 
05394-7001   SKF1049     OGL 396. LMC176.1.34431 + LMC176.1.34425                                Pli2012 
05395+1644   BPMA 15     [PM2000]  285719 + [PM2000]  285027.                                    Gvr2010 
05395-0334   VIG   8     Optical/physical nature of the two faint companions is undefined.       Vig2012 
05396+1531   BPM 141     [PM2000]  286142 + [PM2000]  286564.                                    Gvr2010 
05396-3404   HDO 193     alp Col = Phact                                                                 
05397-0259   CAB  48     V511 Ori.                                                                       
05398+1537   BPM 142     [PM2000]  286537 + [PM2000]  286571.                                    Gvr2010 
05398-0241   CAB  32     V1147 Ori.                                                                      
05398-6859   OGL 397     LMC175.4.34483 + LMC175.4.34571                                         Pli2012 
05399+5145   ES  893     SMA  57.                                                                        
05399+1634   BPM 143     [PM2000]  286991 + [PM2000]  286795.                                    Gvr2010 
05400+1658   BPM 145     [PM2000]  287347 + [PM2000]  287190.                                    Gvr2010 
05400+1626   BPM 144     [PM2000]  287202 + [PM2000]  287554.                                    Gvr2010 
05401-7133   OGL 398     LMC179.6.15460 + LMC179.6.15507                                         Pli2012 
05402+1015   SHY 487     HIP  26680 + HIP  26646.                                                        
05402-6912   OGL 399     LMC175.3.9920  + LMC175.3.9955                                          Pli2012 
05403+3757   SEI 367     ALI 546.                                                                        
05403+1521   SHY  28     BC: HIP  26690 + HIP  26844.                                                    
05403-7112   OGL 400     LMC178.1.26335 + LMC178.1.115                                           Pli2012 
05404+2448   WNO  45     Identified as WNO  16 in USN1976. Discovered by B.Y. Riepe              USN1976 
                         and also known as Riepe's double.                                               
                         GJ 1083 = G 100-28 = V780 Tau. Estimated age 1000-10000 Myr; masses             
                         0.20 +/- 0.04 and 0.13 +/- 0.02 Msun; a ~4.9 au.                        Jnn2014 
05404+1643   BPM 146     AB: [PM2000]  288389 + [PM2000]  288781.                                Gvr2010 
             BPM 147     BC: [PM2000]  288781 + [PM2000]  288600.                                Gvr2010 
05405-7027   OGL 401     LMC177.2.57937 + LMC177.2.58437                                         Pli2012 
05406+1638   BPM 148     [PM2000]  289234 + [PM2000]  289578.                                    Gvr2010 
05406-7151   OGL 402     LMC179.8.11252 + LMC179.8.11284                                         Pli2012 
05407+1704   BPMA 16     [PM2000]  289597 + [PM2000]  289795.                                    Gvr2010 
05407-0157   STF 774     AB: zet Ori = 50 Ori = Alnitak. A premature orbit has been computed.            
                         Spectral types of AB: O9.5Ibe and B0III.                                        
                         Levato et al. (ApJS, 68, 319, 1988) and Fullerton (1990, PhD thesis,    Lev1988 
                         U. Toronto) report small RV variations (<35 km/sec), not confirmed.     Ful1990 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Spectral type of Aa O9.5Ib, spectral type of Ab B0.5IV                  Opl2023 
                         Both A and B components were observed and appeared to be single.        Msn1998a
                         Classification of the B component is from Hoffleit &  Warren (1991).    Hof1991 
                         AC: Star C (mag. about 9, 60") may be physical.                                 
             NOI   1     Aa,Ab: Combined spectroscopic/astrometric solution, using NPOI                  
                         interferometric measures with radial velocities from disentangled               
                         spectra to determine first dynamical mass for an O-type supergiant.             
                         Mass of the O9.5Ib primary is 24.8 +/- 5.6 Msun, that of the B0/1               
                         secondary is 16.4 +/- 4.9 Msun.                                         NOI2011 
                         Aa,Ab: Hummel et al. (2013) calculated a combined interferometric/              
                         spectroscopic orbit of zet Ori. Derived masses are 14.0 +/- 2.2 and             
                         7.4 +/- 1.1 Msun; orbital parallax is 3.4 +/- 0.2 mas, but as this is           
                         based on rather low velocity amplitudes, the photometric distance               
                         (2.6 +0.4/-0.3 mas) is considered more robust. Based on photometric             
                         distance, spectral types for Aa, Ab, and B are O9.5Iab, B1IV, and               
                         B0III, respectively. Masses for Aa and Ab are 33 +/- 10 and 14 +/- 3            
                         Msun, considerably larger than the dynamical values.                    Hmm2013 
                         Intensity Interferometer Limb-darkened diameter 0.48 +/- 0.04 mas.      HBr1974 
                         Uniform disk diameter  0.546 +/- 0.029 mas,                                     
                         Limb darkened diameter 0.485 +/- 0.019 mas,                                     
                         Radius is 21.5 +/- 5.4 \rsun.                                           CIA2018e
             STF 774     AC: H 4  21.                                                            MEv2010 
05408+1657   BPMA 17     [PM2000]  289777 + [PM2000]  290265.                                    Gvr2010 
05408+1539   BPM 149     [PM2000]  289939 + [PM2000]  289977.                                    Gvr2010 
05408-0806   CON  14     AB: MGM 369.                                                            Kkl2016 
05409+1625   BPM 150     [PM2000]  290186 + [PM2000]  289998.                                    Gvr2010 
05410+3106   J   937     Aka MNG   1.                                                            Dam2016a
05410+1620   BPM 151     [PM2000]  290443 + [PM2000]  290760.                                    Gvr2010 
05411+3550   ALV   2     SH 2-235 IRS 1. Luminous YSO in SH 2-235 molecular cloud.               Alv2004 
05411-7023   OGL 403     LMC177.3.13891 + LMC177.3.13893                                         Pli2012 
05412+1632   BPM 152     AB: [PM2000]  290981 + [PM2000]  291008.                                Gvr2010 
             BPM 153     AC: [PM2000]  290981 + [PM2000]  290861.                                Gvr2010 
             BPM 154     BC: [PM2000]  291008 + [PM2000]  290861.                                Gvr2010 
05412+1631   BPM 155     [PM2000]  291034 + [PM2000]  290895.                                    Gvr2010 
05413+5329   ENG  22     LDS 890.                                                                        
                         AB: NLTT 15439/15446                                                    Chm2004 
                         AB: HJL  72.                                                            HJL1986 
                         AB: SHY  29. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AB: This is MN of 05167+4600.                                           Dam2017i
05413+2929   STF 764     A is a spectroscopic binary. B is BD+29@954.                                    
                         Primary is eclipsing binary of Beta Lyr -type, period 0.674 d.          Zas2012 
                         H N  75.                                                                MEv2010 
05413+1706   BPMA 19     [PM2000]  291462 + [PM2000]  291073.                                    Gvr2010 
05413+1704   BPMA 18     [PM2000]  291452 + [PM2000]  291820.                                    Gvr2010 
05413+1632   BU 1007     126 Tau. The variable radial velocity indicates a spectroscopic                 
                         subsystem; the RV range of the blended light is about 50 km/s.                  
                         Single night's measure in 1960 apparently does not refer to this pair.          
                         Observed delta m definitely larger than given in ADS.                   Wor1967b
                         Spectral types of primary and secondary assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 17.71 +/- 23.89, 9.78, and 6.41 Msun, respectively.           Mlk2012 
05413-2621   HJ 3788     B is CD-26@2394.                                                                
05414+1527   BPM 156     [PM2000]  291745 + [PM2000]  292018.                                    Gvr2010 
05415-0840   CON  16     AB: MGM 222.                                                            Kkl2016 
05416+1629   BPM 157     [PM2000]  292234 + [PM2000]  292274.                                    Gvr2010 
05416-7024   OGL 404     LMC177.3.26963 + LMC177.3.26962                                         Pli2012 
05416-7111   OGL 405     LMC178.1.32870 + LMC178.1.33290                                         Pli2012 
05417+1644   BPM 158     [PM2000]  292535 + [PM2000]  292075.                                    Gvr2010 
05417-0254   BU 1052     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.67 +/- 2.70, 2.57, and 1.58 Msun, respectively.             Mlk2012 
05418+1541   BPM 159     [PM2000]  292945 + [PM2000]  292733.                                    Gvr2010 
05418-0155   ALV   3     NGC 2024 IRS 2.                                                         Alv2004 
05420+3401   SEI 374     Aka TOB  37.                                                                    
05420+1640   BPM 160     [PM2000]  293486 + [PM2000]  293135.                                    Gvr2010 
05421+3245   HJ  369     Measure does not agree with HJ, but so identified by Doolittle.         Doo1923 
05421+1522   BPM 162     [PM2000]  293889 + [PM2000]  293594.                                    Gvr2010 
05421+1519   BPM 161     [PM2000]  293806 + [PM2000]  293833.                                    Gvr2010 
05422-7119   OGL 406     LMC179.4.27320 + LMC179.4.30768                                         Pli2012 
05423+3247   HJ  370     SEI 376.                                                                Nsn2017a
05423+1704   BPM 164     AB: [PM2000]  294490 + [PM2000]  294334.                                Gvr2010 
             BPM 165     AC: [PM2000]  294490 + [PM2000]  294161.                                Gvr2010 
             BPM 166     BC: [PM2000]  294334 + [PM2000]  294161.                                Gvr2010 
05423+1646   BPM 163     [PM2000]  294407 + [PM2000]  294228.                                    Gvr2010 
05423+1557   BPM 167     [PM2000]  294597 + [PM2000]  294432.                                    Gvr2010 
05424+7920   STF 695     AB: HJL  71.                                                            HJL1986 
05424+2051   OCC9039     OCC9108.                                                                        
05424+1640   BPM 168     [PM2000]  294701 + [PM2000]  294561.                                    Gvr2010 
05425+4053   WEI  10     B is BD+40@1384.                                                                
05426-6810   OGL 407     LMC181.7.13965 + LMC181.7.14774 + LMC181.7.15836                        Pli2012 
05427+1705   BPMA 20     [PM2000]  295643 + [PM2000]  296373.                                    Gvr2010 
05427+1651   BPM 169     [PM2000]  295609 + [PM2000]  295407.                                    Gvr2010 
05427+1643   BPM 170     [PM2000]  295816 + [PM2000]  295876.                                    Gvr2010 
05427+0241   LDS6192     HIP 26907. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
05428+3322   STF 773     AC: DOO   8.                                                                    
05428+1806   CHR 213     First detected as an occultation binary by Edwards et al.               Evn1980 
05428-7222   OGL 408     LMC180.1.10    + LMC180.1.12050                                         Pli2012 
05429+1650   BPM 171     [PM2000]  296510 + [PM2000]  296883.                                    Gvr2010 
05429+0001   STF 782     B is BD-00@1060.                                                                
05429-0648   A   494     Suspected RV variation not confirmed (Heintz 1981). The faint pair      Hei1981a
                         CD (mag. 10-13, 1.0") is 100" distant from AB.                                  
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.77 +/- 0.28, 2.78, and 1.30 Msun, respectively.  Mlk2012 
05431+3933   BRT2210     ALI 1059.                                                                       
05431+1701   BPM 172     [PM2000]  296994 + [PM2000]  297084.                                    Gvr2010 
05431-3516   FAB  19     Originally inserted as a new solution to HDS 763, it now appears that           
                         both pairs are real.                                                            
                         AC: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
05432+1559   BPM 173     [PM2000]  297486 + [PM2000]  297074.                                    Gvr2010 
05435+1642   A  2436     Rectilinear solution by Rica & Zirm (2012).                             FMR2012i
05435+1526   BPM 174     AB: [PM2000]  298316 + [PM2000]  298293.                                Gvr2010 
             BPM 175     AC: [PM2000]  298316 + [PM2000]  298674.                                Gvr2010 
             BPM 176     BC: [PM2000]  298293 + [PM2000]  298674.                                Gvr2010 
05435-0753   A   495     Angle decreasing. No measures 1963-1988, during which period nearly             
                         two quadrants were described.                                                   
05436+6633   HU 1109     A is reported to be variable, type unknown.                                     
05436+1510   BPM 177     [PM2000]  298697 + [PM2000]  298487.                                    Gvr2010 
05436+1506   BPM 178     [PM2000]  298805 + [PM2000]  299090.                                    Gvr2010 
05436+1300   A   117     A 14.5 magnitude star is 26" from A in 191@.                            B__1963b
05438+1650   BPM 180     [PM2000]  299538 + [PM2000]  299218.                                    Gvr2010 
05438+1543   BPM 179     [PM2000]  299328 + [PM2000]  299117.                                    Gvr2010 
05438-6811   OGL 409     LMC181.2.42    + LMC181.2.240                                           Pli2012 
05439+1620   BPM 181     [PM2000]  299743 + [PM2000]  299422.                                    Gvr2010 
05439-6827   OGL 410     LMC182.5.20806 + LMC182.5.21242                                         Pli2012 
05440+1616   BPM 183     [PM2000]  300068 + [PM2000]  300159.                                    Gvr2010 
05440+1611   BPM 184     [PM2000]  300096 + [PM2000]  300502.                                    Gvr2010 
05440+1549   BPM 185     [PM2000]  300192 + [PM2000]  300353.                                    Gvr2010 
05440+1548   BPM 182     [PM2000]  300036 + [PM2000]  299690.                                    Gvr2010 
05441+1556   BPM 186     [PM2000]  300517 + [PM2000]  300475.                                    Gvr2010 
05441+0249   HJ 2277     BAL 1677.                                                                       
05441-0229   A  2918     B is BD-02@1354.                                                                
05441-7116   OGL 411     LMC186.8.7     + LMC178.1.20316                                         Pli2012 
05441-7121   OGL 412     LMC179.4.38816 + LMC179.4.40244                                         Pli2012 
05442+1644   BPM 187     [PM2000]  300711 + [PM2000]  300977.                                    Gvr2010 
05442+1544   BPM 188     [PM2000]  300888 + [PM2000]  300602.                                    Gvr2010 
05443+1546   BPM 189     [PM2000]  301137 + [PM2000]  300719.                                    Gvr2010 
05444+1551   BPM 190     [PM2000]  301700 + [PM2000]  301872.                                    Gvr2010 
05444-0528   SHY 489     HIP  27069 + HIP  26588.                                                        
05445-2227   H 6  40     AB: gam Lep = 13 Lep.H VI 40. LDS 148.                                          
                         AB: NLTT 15560/15558                                                    Chm2004 
                         AB: B = AK Lep.                                                         Tok2014d
             H 5  50     BC: H V 50. C is CPD-22@883.                                                    
05446+6320   STI 579     Rectilinear solution by Hurowitz et al. (2013).                         USN2013a
05446+1607   BPM 195     [PM2000]  302614 + [PM2000]  302673.                                    Gvr2010 
05446+1545   BPM 191     [PM2000]  302270 + [PM2000]  302653.                                    Gvr2010 
05446+1536   BPM 192     [PM2000]  302289 + [PM2000]  302408.                                    Gvr2010 
05446+1532   BPM 193     [PM2000]  302321 + [PM2000]  302640.                                    Gvr2010 
05457-1447   A  3018     Rectilinear solution by Rica & Zirm (2012).                             FMR2012i
05460+3717   BLL  16     Rectilinear solution by Friedman et al. (2011).                         USN2011a
05466+0110   RAG   1     Primary is exoplanet host, P=14.3d, 2135d. Benedict et al. (2010)       AST2010 
                         astrom. orbit for planet c, 1.05mas axis.                               Tok2014d
                         CHARA Array Limb-darkened diameter  0.573 +/- 0.049 mas,                CIA2008c
                         R =  2.44  +/- 0.22  \rsun.                                                     
05447+1607   BPM 196     [PM2000]  302752 + [PM2000]  302935.                                    Gvr2010 
05447+1546   BPM 194     [PM2000]  302592 + [PM2000]  302169.                                    Gvr2010 
05447+1538   BPM 197     [PM2000]  302856 + [PM2000]  302664.                                    Gvr2010 
05447+0350   STF 788     AB: H 2  61.                                                            MEv2010 
05447-4618   HJ 3797     B is CD-46@1983.                                                                
05448+1617   BPM 198     [PM2000]  302916 + [PM2000]  302938.                                    Gvr2010 
05448+1539   BPM 199     [PM2000]  302951 + [PM2000]  303127.                                    Gvr2010 
05449+1645   BPM 200     [PM2000]  303487 + [PM2000]  303652.                                    Gvr2010 
05450+1604   BPM 201     [PM2000]  303785 + [PM2000]  303699.                                    Gvr2010 
05451+1605   BPM 206     [PM2000]  304191 + [PM2000]  304389.                                    Gvr2010 
05451+1556   BPM 204     AB: [PM2000]  304185 + [PM2000]  304317.                                Gvr2010 
             BPM 205     BC: [PM2000]  304317 + [PM2000]  304322.                                Gvr2010 
05451+1532   BPM 202     [PM2000]  303972 + [PM2000]  304218.                                    Gvr2010 
05451+1144   BPM 203     [PM2000]  304093 + [PM2000]  304082.                                    Gvr2010 
05454+1123   BPM 207     [PM2000]  305302 + [PM2000]  305441.                                    Gvr2010 
05454-0037   HER  14     Additional notes may be found in Herbig (1962).                         Her1962 
05456-1503   ENG  23     B is BD-15@1153.                                                                
05457+1636   BPM 208     [PM2000]  306501 + [PM2000]  306641.                                    Gvr2010 
05457-6833   OGL 413     LMC182.3.133   + LMC182.3.280                                           Pli2012 
05459+2555   STT 116     DE: Also known as TAR   1.                                                      
05460+1048   A  2711     May be a short period binary, but the few measures do not even permit           
                         certain determination of the direction of motion.                               
05460-0416   STF 790     Composite spectrum; K1III+G0IV.                                                 
05460-3218   mu Col      Additional radial velocity measurements by Fullerton (1990)             Ful1990 
                         and Penny et al. (1993) confirm the lack of                             Pny1993 
                         variability.                                                            Msn1998a
05461-6920   OGL 414     LMC183.2.41    + LMC183.2.263                                           Pli2012 
05462-2100   BRT 302     ARA1281.                                                                        
05462-7027   OGL 415     LMC185.7.75526 + LMC185.7.75527                                         Pli2012 
05463+3736   GCB  66     A is the short-period variable EU Tau.                                          
05464-6835   OGL 416     LMC182.3.18716 + LMC182.3.18717                                         Pli2012 
05465+7437   YSC 148     Docobo et al. (2014) use the spectroscopic elements of Latham et al.            
                         (2002), together with speckle data and the Hipparcos parallax, and      Lat2002 
                         derive possible solutions for both direct and retrograde motion. The            
                         resulting masses are 0.99 +/- 0.09 and 0.63 +/- 0.08 Msun.              Doc2014h
05465-6903   OGL 417     LMC183.4.105   + LMC183.4.1756                                          Pli2012 
05466+0110   GC 7226     Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from the Geneva           
                         Extrasolar Planet Search Programs home page.                            HaI2001 
05467+4322   ES 1530     BRT 90.                                                                         
05467+0005   BU  559     This system, listed in the ADS as #4374 was purged from an earlier              
                         edition of the WDS probably as it was buried in reflection nebulae              
                         NGC 2068.                                                                       
05468+3700   ALI 309     MLB 826.                                                                        
05469+0931   J   251     HJL  73.                                                                HJL1986 
05470+1600   BPM 209     [PM2000]  310850 + [PM2000]  310780.                                    Gvr2010 
05471+0023   PAD  24     MGM3385.                                                                Kkl2016 
05471+0022   PAD  25     MGM3374.                                                                Kkl2016 
05472+2153   HU   39     Measures scattering around 45 degrees, with variation in distance               
                         evident. Motion in a highly-inclined orbit?                                     
05472+1429   CHR 160     131 Tau.                                                                        
05472-2430   HJ 3798     B is CD-24@3430.                                                                
05473+3222   J   902     This pair is 1.36s f and +30.7" nf of BD+32@1087.                               
05473-5104   LGR   1     Primary is bet Pic, secondary is probably a giant planet. Estimated             
                         mass of companion 9 +3/-2 Mjup, assuming a distance of 19.3 +/- 0.2pc           
                         and an age 12 +8/-4 Myr.                                                Lgr2009a
                         Planetary companion later confirmed, with multiple measurements.                
                         Member of the bet Pic moving group.                                     Zuc2001b
                         Assuming an age of 12 +8/-4 Myr (Bonnefoy et al. 2013 A&A 555, A107),           
                         Absil et al. (2013) estimate the mass of bet Pic b at 8.0 +3.2/-2.1             
                         Mjup. Using the revised age of 21 +/- 4 Myr by Binks & Jeffries (2014           
                         MNRAS 438, L11) leads to a mass of 10.6 +1.2/-1.8 Mjup.                 Abs2013 
                         Nielsen et al. (2014) find a semi-major axis of 9.1 +5/-0.5 au and a            
                         period of 21 +21/-2 y; the planet appears to have reached maximum               
                         elongation and is moving back toward the star, with minimum angular             
                         separation expected ~2018. The primary mass is 1.76 +0.18/-0.17 Msun.   Nls2014 
05473-6832   OGL 418     LMC182.3.18737 + LMC182.3.18800                                         Pli2012 
05473-7119   OGL 419     LMC187.5.29667 + LMC187.5.29853                                         Pli2012 
05474+2858   HJ  709     First distance probably in error (Doolittle).                           Doo1923 
                         Two faint stars measured near the position given for HJ 709, BDS 2951.          
                         Neither fits the earlier descriptions by Herschel, Burnham, and                 
                         Doolittle, but these do not agree among themselves, either.             B__1962d
05474-1032   MCA  22     An eclipsing binary and spectroscopic triple, V1031 Ori, with the               
                         (presumably) wider pair now resolved by speckle interferometry.                 
                         Zasche et al. (2014) derive a combined solution, including                      
                         interferometry plus times-of-minimia variation in the eclipsing-binary          
                         primary.                                                                Zas2014b
05476+1736   BU 1401     Probably STF 767 rej.                                                           
05477+1354   HJ 3279     133 Tau.                                                                        
05479+3510   HO   19     SEI 385.                                                                Nsn2017a
05479+2441   STTA 66     B is BD+24@965.                                                                 
05479-6847   OGL 420     LMC189.7.12    + LMC189.7.52                                            Pli2012 
05480+0627   STF 795     52 Ori. One component is a spectroscopic binary.                                
                         H 1  20.                                                                MEv2010 
05482+0137   A  2657     Only elements P, T, and a have been amended by Starikova (1978) from    Sta1978c
                         the orbit of Baize (1961).                                              Baz1961b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.86 +/- 2.35, 4.13, and 1.45 Msun, respectively.             Mlk2012 
05483-6948   OGL 421     LMC184.3.24360 + LMC184.3.24357                                         Pli2012 
05483-7002   OGL 422     LMC184.1.30453 + LMC184.1.30754                                         Pli2012 
05484+2052   STT 118     A is a spectroscopic binary. A premature visual orbit has been                  
                         computed.                                                                       
05485+2118   GIC  60     G100-037/G100-038.                                                              
05485-7127   OGL 423     LMC187.4.56    + LMC187.4.1142                                          Pli2012 
05486-7013   OGL 424     LMC185.4.18027 + LMC185.4.18356                                         Pli2012 
05487+1549   BPM 210     [PM2000]  317297 + [PM2000]  317306.                                    Gvr2010 
05488+1254   BPM 211     [PM2000]  317402 + [PM2000]  316980.                                    Gvr2010 
05488-6552   HJ 3815     B is CPD-65@506.                                                                
05489+2101   BU   93     B is BD+20@1112.                                                                
05489-3910   WG   42     A likely plate flaw.                                                    Grv2021b
05489-7157   OGL 425     LMC188.4.9     + LMC188.4.10                                            Pli2012 
05490+6342   TDS 197     Rectilinear solution by Cvetkovic et al. (2019).                        Cve2019b
05490+3451   SEI 386     J 1114.                                                                         
05490+2434   MCA  23     132 Tau.                                                                        
05490+0108   GRE   2     IRAS 05464+0106 = PDS 17.                                               Gre1992 
05490-1105   GAL 393     Object #205 in Gallo's original list.                                   Gal1914 
05490-7150   OGL 426     LMC187.1.114   + LMC187.1.697                                           Pli2012 
05491-6108   HJ 3810     B is CPD-61@532.                                                                
05492+3911   BU  192     tau Aur = 29 Aur                                                                
             H 5  21     H V 21.                                                                         
05492+2941   BRT2521     Rectilinear solutions by Cvetkovic (2015)                               Cve2015b
                         and Cvetkovic et al. (2016).                                            Cve2016 
05495+1239   BUP  84     134 Tau.                                                                        
05495-7047   OGL 427     LMC186.4.38205 + LMC186.4.38233                                         Pli2012 
05495-7100   OGL 428     LMC186.3.12362 + LMC186.3.12420                                         Pli2012 
05495-7123   OGL 429     LMC187.4.309   + LMC187.4.264                                           Pli2012 
05496+2244   CHR 205     First detected as an occultation binary by Africano.                    Afr1975 
05496-1429   BU   94     BDS 3207 probably same star.                                                    
05496-6836   OGL 430     LMC189.6.10983 + LMC189.6.10979                                         Pli2012 
05497-0427   SCJ   3     B is BD-04@1249.                                                                
05497-6843   OGL 431     LMC189.7.11539 + LMC189.7.11612                                         Pli2012 
05498+3258   S   500     B is BD+32@1099.                                                                
                         Although the field is crowded and the PM is small, it is CPM. With PM           
                         of 20 mas/yr it would move by 3.6" in 180yr since 1825.                 Tok2014d
05498-7225   TOK 431     First resolution, estimated period 12 yr.                               Tok2013b
05499+3147   STF 796     AB: H 1  67.                                                            MEv2010 
05499+2259   ARN  91     AC: Secondary of 05500+2258 ARN 91 found to be primary of 05499+2259            
                         POU 789. Pairs merged, with quadrant flip to ARN 91.                            
05500+2551   OL  165     Aka COU 765.                                                                    
05502+2658   RUC  19     Primary is V781 Tau.                                                            
05503-6854   OGL 432     LMC189.8.10709 + LMC189.8.12244                                         Pli2012 
05505-5246   B  1493     Spectrum composite; K0-1III+A4V+A.                                              
05506+5655   H 4 125     H IV 125. 29 Cam.                                                               
05507-6838   OGL 433     LMC189.3.372   + LMC189.3.990                                           Pli2012 
05507-7159   OGL 434     LMC188.4.11434 + LMC188.4.11429                                         Pli2012 
05510+2758   BU 1054     136 Tau. A possible occultation binary. Misidentified by Burnham,       Bu_1894 
                         corrected by van den Bos.                                               B__1960b
05510-3546   WFC  31     bet Col = Wazn                                                                  
05510-6954   HJ 3820     B is CPD-69@@535.                                                               
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
05514+3535   HJ  710     Points to a 14th magnitude star 30".                                            
05514+3207   ES  415     A is variable.                                                                  
05514-1108   GAL 394     Object #206 in Gallo's original list.                                   Gal1914 
05515+3909   H 5  90     nu Aur = 32 Aur. H V 90.                                                        
05515+1548   BPM 213     [PM2000]  328749 + [PM2000]  328867.                                    Gvr2010 
05515+1544   BPM 214     [PM2000]  328857 + [PM2000]  328714.                                    Gvr2010 
05515+1217   BPM 212     [PM2000]  328544 + [PM2000]  328831.                                    Gvr2010 
05516-6918   OGL 435     LMC190.2.201   + LMC190.2.474                                           Pli2012 
05517+3838   BRT2211     ALI 811.                                                                        
05518-4434   BLR   1     DENIS J055146.0-443412.2. NTT/SofI IR spectro-imager observations by            
                         Billeres et al. (2005) resolved the first wide ultracool binary dwarf;          
                         spectral types are M8.5 + L0.                                           Blr2005 
05520-0715   J  1913     Previously published coordinates corrected by +3'. Pair is +5s, +4'             
                         from BU 95.                                                             J__1949a
05521-6922   OGL 436     LMC190.2.13    + LMC190.2.123                                           Pli2012 
05522+1658   BPM 215     [PM2000]  331791 + [PM2000]  331753.                                    Gvr2010 
05522+1542   BPM 216     [PM2000]  332058 + [PM2000]  332011.                                    Gvr2010 
05522-6826   OGL 437     LMC189.4.9311  + LMC189.4.10038                                         Pli2012 
05523+3235   SEI 414     Identification of SEI 414 is uncertain,but is appears to correspond to          
                         the A and C components of 05523+3235.                                           
05523+1509   BPM 217     AB: [PM2000]  332310 + [PM2000]  332065.                                Gvr2010 
             BPM 218     BC: [PM2000]  332065 + [PM2000]  331572.                                Gvr2010 
05523+1431   BPM 219     AB: [PM2000]  332440 + [PM2000]  331988.                                Gvr2010 
             BPM 220     AC: [PM2000]  332440 + [PM2000]  332891.                                Gvr2010 
05523+1253   COU2704     BD: Couteau erroneously calls this AD.                                  Cou1958c
05524+3752   SEI 402     ALI 549.                                                                        
05524+3618   AG  101     SEI 409.                                                                Nsn2017b
05524+1711   BPM 221     [PM2000]  332860 + [PM2000]  332448.                                    Gvr2010 
05524+0151   BU 1404     56 Ori.                                                                         
05524-6940   OGL 438     LMC191.4.203   + LMC191.4.204                                           Pli2012 
05525+3235   SEI 424     AB: Appears to be the same pair as SEI 420.                                     
05525+3233   SEI 421     SEI 423.                                                                Nsn2017b
05525+1548   BID   1     A is a Mira-type variable, Z Tau.                                               
05525-0217   HDS 787     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.29 +/- 0.28, 2.19, and 1.20 Msun, respectively.             Mlk2012 
05526+1510   BPM 222     [PM2000]  333540 + [PM2000]  333628.                                    Gvr2010 
05526+1402   J   948     BRT 1185.                                                                       
05526-3738   I    64     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
05527+3731   ES 2341     ALI 550.                                                                        
05528+3233   SEI 428     Hipparcos suspected non-single.                                                 
05528+2946   STF 808     AC: HJL  74.                                                            HJL1986 
05529+3427   SHY 492     AC: HIP  27791 + HIP  28872.                                                    
05530+3624   HJ 5540     ALI 312. SEI 427.                                                               
05531+4127   ARG  61     B is BD+41@1290.                                                                
05531+1501   BPM 223     [PM2000]  335794 + [PM2000]  336159.                                    Gvr2010 
05531-6845   OGL 439     LMC189.2.9876  + LMC189.2.10434                                         Pli2012 
05531-7125   OGL 440     LMC194.5.537   + LMC194.5.1400                                          Pli2012 
05532+1424   J   656     OL 153 and GCB 13 are the same as this star                             Hei1985a
05533+1611   BPM 224     [PM2000]  336700 + [PM2000]  336469.                                    Gvr2010 
05534-0333   A  2919     Change in angle for AB doubtful, but separation certainly smaller.              
                         Error or misprint of 10deg in my angle for 1960 appears probable.       B__1960a
                         Probably optical.                                                       B__1962d
                         A faint pair 10s p 3' s.                                                        
                         The faint pair must be 10s following.                                   Dam2012 
05535+4434   ES 1379     Rectilinear solution by Cvetkovic et al. (2017).                        Cve2017 
05537+1245   BPM 225     [PM2000]  338633 + [PM2000]  339014.                                    Gvr2010 
05538-2218   BRT1382     CD-22@2561.                                                                     
05539+1653   BPM 226     [PM2000]  339901 + [PM2000]  340312.                                    Gvr2010 
05540+1552   BPM 228     [PM2000]  340363 + [PM2000]  340293.                                    Gvr2010 
05540+1225   LDS 891     NLTT 15772/15768                                                        Chm2004 
05540+1146   BPM 227     [PM2000]  340157 + [PM2000]  340110.                                    Gvr2010 
05541+0140   RST5219     Pre-main sequence star HBC 515, located in the Orion L1622 cometary             
             HBC 515     cloud. The primary appears to be comprised of two ~equal brightness             
                         weakline T Tauri stars of spectral type K2V. The B component dominates          
                         the system at mid-infrared wavelengths, suggesting that it is a                 
                         protostar still embedded in the nascent cloud of HBC 515.  The C and D          
                         components (L1622-6 and L1622-6N) are also T Tau stars and likely               
                         physically associated.                                                  Rep2010 
05542+1545   BPM 229     [PM2000]  341008 + [PM2000]  341038.                                    Gvr2010 
05542-2909   FIN 382     Angle decreasing.                                                               
05543+1555   BPM 230     [PM2000]  341566 + [PM2000]  342144.                                    Gvr2010 
05543+0143   CHN  19     HBC 190 = LkHa 336. Pre-main sequence stars in the Lynds 1622 star-             
                         forming cloud. Kun et al. (2008) derives effective temperatures, ages,  Kun2008 
                         and masses for both components based on model fitting and their                 
                         visible and IR data, assuming a distance of 400pc.                              
05543-2553   I  1614     B is CD-25@2770.                                                                
05543-7128   OGL 441     LMC194.5.8083  + LMC194.4.81                                            Pli2012 
05544+3836   WEI  11     B is BD+38@1326.                                                                
05544+2017   KNG   1     chi 1 Ori                                                                       
                         Combined astrometric/spectroscopic solution by Irwin et al. (1992)      Irw1992a
                         2002.161: This observation agrees with the orbit of Han & Gatewood      HaI2002 
                         (2002).                                                                         
                         Koenig et al. (2002) derive masses of 1.02+-0.08 and 0.15+-0.01 Msun.   Kng2002 
                         CHARA Array Limb-darkened diameter  1.051 +/- 0.009 mas,                CIA2012e
                         R =  0.979 +/- 0.009 \rsun, L =  1.081 +/-0.018 \lsun,                          
                         Teff = 5961 +/-  36 K, M = 1.029 +/- 0.029 \msun,                               
                         Age =  2.0 +/- 1.8 Gyr.                                                         
05544+0152   REP   6     L1622-10. Pre-main sequence stars in Lynds 1622 star-forming cloud.             
                         Kun et al. (2008) derives effective temperatures, ages, and masses for  Kun2008 
                         the A and B components based on model fitting and their visible and IR          
                         data, assuming a distance of 400pc.                                             
05544-7023   OGL 442     LMC192.3.122   + LMC192.3.1429                                          Pli2012 
05545-7044   OGL 443     LMC193.4.680   + LMC193.4.1614                                          Pli2012 
05546-7012   OGL 444     LMC192.4.133   + LMC192.4.1646                                          Pli2012 
05547+1351   S   502     STTA 68. B is BD+13@1027.                                                       
                         Both components were observed and appeared to be single.                Msn1998a
05548+3612   SEI 435     Duplicity not apparent on POSS plate; one component may be either a             
                         variable star or a flaw on AC Potsdam plate.                                    
                         A likely plate flaw.                                                    Grv2021b
05549+3836   COU2181     TDS3420.                                                                        
05549+1359   BPM 232     [PM2000]  344577 + [PM2000]  344421.                                    Gvr2010 
05549+1345   BPM 231     [PM2000]  344453 + [PM2000]  344387.                                    Gvr2010 
05549+0702   STF 817     H 4  98.                                                                MEv2010 
05549-7528   TOK 102     HIP 27957. Several other components are seen in the ANDICAM field,              
                         N*=35.                                                                  Tok2011a
05550+1616   BPMA 21     AB: [PM2000]  344770 + [PM2000]  344112.                                Gvr2010 
             BPMA 22     BC: [PM2000]  344112 + [PM2000]  344444.                                Gvr2010 
05551+1203   BPM 233     [PM2000]  345570 + [PM2000]  345715.                                    Gvr2010 
05552+0724   KAR   1     alp Ori = 58 Ori = Betelgeuse. Irregular variable, spectrum                     
                         M1-2Ia-Iab. Two close companions have been reported, detected by                
                         speckle interferometry.                                                         
                         Mk III Uniform-disk diameter 49.401 +/- 0.237 mas (800 nm).             MkT1991 
             H 6  39     H VI 39.                                                                        
05553+1516   BPM 234     [PM2000]  346272 + [PM2000]  346598.                                    Gvr2010 
05553+1220   BPM 235     [PM2000]  346508 + [PM2000]  346532.                                    Gvr2010 
05556+5328   STT 120     B is BD+53@963.                                                                 
05557-3806   SHY 493     HIP  28036 + HIP  26990.                                                        
05558+4651   LDS3680     NLTT 15797/15796                                                        Chm2004 
05560+3949   ES 2153     ADS 4527a.                                                                      
                         Aka HDS 799.                                                            Dam2016a
05561+1356   S   503     AB: B is BD+13@1037.                                                            
                         AB, AC, and AD: Optical pair, based on study of relative motion of the          
                         components using the method of apparent motion parameters.              Kiy2008 
                         AC: Additional notes may be found in Burnham (1894).                    Bu_1894 
05561+1302   BPM 236     [PM2000]  350375 + [PM2000]  351046.                                    Gvr2010 
05562+3143   HJ  714     SEI 444.                                                                Nsn2017b
05562+1755   BPM 237     [PM2000]  350997 + [PM2000]  351100.                                    Gvr2010 
05563+4353   ES 1531     AB: Barton identifies BRT 91 as same star.                              Brt1926b
05563+3140   HJ  715     SEI 445.                                                                Nsn2017b
05564+1634   BPM 238     [PM2000]  352134 + [PM2000]  351978.                                    Gvr2010 
05565-2631   B    94     1989.9362: This system was last resolved visually in 1978, and appears          
                         to be continuing to approach periastron.                                Hrt1993 
05566+1129   BPM 239     [PM2000]  353046 + [PM2000]  352711.                                    Gvr2010 
05566-7110   OGL 445     LMC193.2.5397  + LMC193.2.5487                                          Pli2012 
05567+1231   BPM 240     [PM2000]  353373 + [PM2000]  353196.                                    Gvr2010 
05567-7012   OGL 446     LMC199.5.36    + LMC199.5.193                                           Pli2012 
05568+1413   BPM 241     [PM2000]  354005 + [PM2000]  353928.                                    Gvr2010 
05569+3615   SEI 447     Secondary not seen on POSS plate; may be either variable star or flaw           
                         on AC Potsdam plate.                                                            
05569+2121   CHR 214     First detected as an occultation binary by Evans & Edwards.             Evn1983a
05569-1836   B  1953     J  1469. Identified by Jonckheere as BOS 1953 in his 1962 catalog.      J__1962a
05569-0700   HJ   33     AB: J  1915AC.                                                                  
             AOT  24     AC: J  1915AB.                                                                  
             AOT  24     BC: J  3228. J  1915BC.                                                 J__1962a
05570+1022   BPM 242     [PM2000]  355093 + [PM2000]  355331.                                    Gvr2010 
05570-7152   OGL 447     LMC194.1.135   + LMC194.1.687                                           Pli2012 
05571+1014   ARG  63     B is BD+10@939a.                                                                
05573+3601   HU 1235     Measure does not confirm apparent motion shown in IDS.                  Wor1967b
05573-2720   HJ 3818     Spectrum: G8/K0IIICNpv.                                                         
05574-6852   OGL 448     LMC196.1.80    + LMC196.1.833                                           Pli2012 
05575-3517   HJ 3819     gam Col.                                                                        
05576-6831   OGL 449     LMC196.3.15    + LMC196.3.93                                            Pli2012 
05576-7004   OGL 450     LMC198.8.6317  + LMC198.8.6316                                          Pli2012 
05578-1413   GAL 395     Object #208 in Gallo's original list.                                   Gal1914 
05578-7125   OGL 451     LMC194.4.4587  + LMC194.4.4769                                          Pli2012 
05580-6835   OGL 452     LMC196.3.66    + LMC196.3.65                                            Pli2012 
05581-3548   RSS  94     HIP 28241. No V-photometry for B in either WDS or SIMBAD.               Tok2011a
             TOK 212     A triple system consisting of the 0".54 inner pair resolved with NICI           
                         and the physical companion B at 11".                                    Tok2012a
05581-7000   OGL 453     LMC198.8.5791  + LMC198.8.5806                                          Pli2012 
05581-7108   OGL 454     LMC200.7.2     + LMC200.7.32                                            Pli2012 
05584+0150   H 5 100     H V 100. 59 Ori. A Delta Scuti-type variable, V1004 Ori, and also a             
                         spectroscopic binary.                                                           
05584-0439   LDS3684     AD: NLTT 15871/15867                                                    Chm2004 
             A   322     Pair bound. Primary is G0. B component estimated mass 0.50 +/- 0.02             
                         Msun, spectral type M0-M2.                                              Egn2007 
05586+2133   BRT2336     J 2588.                                                                         
05586-7147   OGL 455     LMC194.1.3678  + LMC194.1.3680                                          Pli2012 
05587-0110   LDS5668     LDS6194.                                                                        
05587-6856   OGL 456     LMC196.1.6419  + LMC196.1.6507                                          Pli2012 
05588+7134   STF 793     Rectilinear solution by Hartkopf & Mason (2015).                        WSI2015 
05588+2121   JNN 267     LHS 6097. Estimated age 1000-10000 Myr; masses 0.20 +/- 0.04 and 0.10           
                         +/- 0.01 Msun; a ~8.1 au.                                               Jnn2014 
05588+0033   KUI  22     60 Ori. A is a spectroscopic binary.                                            
05589+1735   BPM 243     [PM2000]  364266 + [PM2000]  364720.                                    Gvr2010 
05589+1248   STT 124     1980.1560: This measure was incorrectly attributed to STF 784 in                
                         McAlister et al. (1983).                                                McA1983 
05589-3422   GC 7577     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
05590+1321   HJ 3280     Probably J  1916.                                                       Nsn2016 
05590-1729   LDS 150     LDS5193.                                                                        
05590-7040   OGL 457     LMC199.8.4949  + LMC199.8.4969                                          Pli2012 
05592+7749   MLR 470     Also known as HDS 811.                                                          
05594-0642   HDS 826     YSC 187.                                                                        
05595+5853   ES 9002     Previously known as ES   66a.                                                   
05595+5417   ENG  24     33 Aur = del Aur                                                                
05595+4457   H 6  88     AB: bet Aur = 34 Aur = Menkalinan.  H VI 88. An Algol-type system,              
                         P = 3.96d. According to R.G. Aitken, this is the third binary           A__1935f
                         recognized by spectroscopic methods. It was identified as such by Miss          
                         Maury at the Harvard College Observatory in early 1890.                         
             KOE   1     Aa,Ab: Visual orbit by Hummel et al. (1995) based on astrometry from    MkT1995 
                         Mark III interferometer. Additional spectroscopic data yield component          
                         masses, luminosities, radii, effective temperatures, and distance.              
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Hummel et al. (1995).                                                   MkT1995 
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 4.70 +/- 9.41, 3.85, and 2.19 Msun, respectively.  Mlk2012 
05595+1522   HEI 112     BC: AB is 34 deg at 49", J 2735 is not AB and not in BD according to            
                         Heintz.                                                                 Hei1983a
05596+1130   BPM 244     [PM2000]  367567 + [PM2000]  367897.                                    Gvr2010 
05597+3713   STT 545     37 Aur = the Aur = Mahasim. A is a variable of the Alpha CVn type.              
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: H 5  89.  AD: H 6  34.                                              MEv2010 
                         AC: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
05599+5834   GIC  61     G192-011/G192-012 = GJ 3371A+3372B. The A component is the variable             
                         star EG Cam.                                                                    
05599+1234   BPM 245     [PM2000]  368722 + [PM2000]  369058.                                    Gvr2010 
05599-3703   B  1044     HIP 28403.                                                              Tok2011a
06001+3756   BRT2212     ALI 558.                                                                        
06001+1648   BPM 246     [PM2000]  369652 + [PM2000]  369271.                                    Gvr2010 
06002-1231   LDS3686     NLTT 15922/15921                                                        Chm2004 
06003+4436   BU 1055     Composite spectrum; K2III+K0III.                                                
             H 5  91     AC: H V 91. Incorrected identified as H 6  91 in BDS.  Error noted by   Bu_1906 
                         MacEvoy (2010).                                                         MEv2010 
06003-3102   HJ 3823     AB,C triple solution by Soderhjelm (1992), who notes the Hipparcos      Sod1999 
                         data are unuseable. Speckle observations needed to strengthen orbit.            
             TOK   9     CE: As suggested by Tokovinin et al. and after consultation with the    Tok2005 
                         author, the measure of Prieto was moved from AB to CE, as AB was        Pri1997a
                         unresolved at the time of the observation. This measure of CE predates          
                         the discovery by eight years.                                                   
                         AC. 1997.0952: In this multiple system, our observation failed to               
                         detect the closer pair HU 1399 AB, where the secondary has magnitude            
                         9.2 and approximate separation 0".5.                                    Hor1997 
                         Tokovinin (2005) notes that a 1996 measure of the AB pair by Prieto     Tok2005 
                         (1997) may actually have been of CE, as AB was unresolvable at this     Pri1997a
                         epoch (250deg, 0".09).                                                          
06004-4401   JNN  46     The two components resolved by AstraLux have nearly equal brightnesses          
                         and colors. Hence, this counts as an unconfirmed binary, since the              
                         system has only been observed in one epoch so far.                      Jnn2012 
06004-6822   OGL 458     LMC204.5.13    + LMC204.5.31                                            Pli2012 
06005+3519   EVS  49     CO Aur                                                                          
06007+6809   LDS1201     NLTT 15858/15857                                                        Chm2004 
06007-1838   FEN   5     Aka J  3229.                                                                    
06008-6937   OGL 459     LMC198.4.3862  + LMC198.4.4499                                          Pli2012 
06010+2734   SMK   1     Aa,Ab: Resolved by two occultation events at favorable aspects.         Smk1989 
06011+2320   H 4  48     H IV 48.                                                                        
06014-0745   A   663     Aka OL  166.                                                                    
06015+2308   SKF1612     RW Gem.                                                                         
06016-7228   OGL 460     LMC202.8.4625  + LMC202.8.4814                                          Pli2012 
06017+2224   CHR 161     Listed by Appleby (1980 JBAA, 139, 1139) as having anomalous behavior.  McA1993 
06018+1618   BPM 247     [PM2000]  376705 + [PM2000]  376243.                                    Gvr2010 
06018-1036   BU   16     3 Mon. A is a spectroscopic binary.                                             
06018-4110   HJ 3827     CPD-41@872.                                                                     
06020+1358   BPM 248     [PM2000]  377571 + [PM2000]  377156.                                    Gvr2010 
06022-4401   TOK 104     HIP 28604. The B-companion could be a close binary (PSF fit).                   
                         NOMAD: PM(B)=(+2,+10), V=14.30.                                         Tok2011a
06023-7157   OGL 461     LMC202.5.4896  + LMC202.5.5006  + LMC202.5.5007                         Pli2012 
06024+0939   A  2715     mu Ori = 61 Ori. Alden (1942) orbit is visual. P, T, e in Osvald's      Ald1942 
                         (1964) astrometric orbit are taken from a revised visual orbit by       Osv1964 
                         Alden (cf Osvald's paper); the revised a = 0.254". The different types          
                         of orbits cause the longitude of the node to be in opposite quadrants.          
                         Star A is an Alpha CVn variable and SB1, P = 4.45 d; star B is SB2,             
                         P = 4.78 d (F. Fekel 1980).                                             Fek1980b
                         See discussion by Morgan et al. (1978).                                 BLM1978 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Only elements P and T have been amended by Starikova (1977) from the    Sta1977a
                         orbit of Alden (1942).                                                  Ald1942 
                         Combined spectroscopic/astrometric solution by Fekel et al. (2002) for  Fek2002 
                         the wide pair of this quadruple system, plus spectroscopic orbits for           
                         both short-period pairs. The solution includes mass and distance                
                         determinations.                                                                 
             mu Ori      Muterspaugh et al. (2008) combine PHASES astrometry with speckle and    Mut2008 
                         radial velocity data to derive an orbit for the AB pair of this                 
                         quadruple system, as well as the Aa,Ab and Ba,Bb subsystems. Listed             
                         solution assumes L_Aa > L_Ab and L_Ba > L_Bb; other assumptions result          
                         in some changes of angular elements.  The parallax of the system is             
                         determined at 21.69 +/- 0.13 mas (distance 46.11 +/- 0.28 pc), with             
                         semimajor axes for AB; Aa,Ab; and Ba,Bb of 12.620 +/- 0.057, 0.07659            
                         +/- 0.00058, and 0.07780 +/- 0.00036 au, respectively. Other derived            
                         quantities for the four components are as follows:                              
                                Star     Mass (Msun)        M_K (mag)                                    
                                 Aa    2.38  +/- 0.11     1.03 +/- 0.26                                  
                                 Ab    0.652 +/- 0.097   >4.58                                           
                                 Ba    1.389 +/- 0.019    1.72 +/- 0.26                                  
                                 Bb    1.356 +/- 0.019    2.02 +/- 0.26                                  
06024-6902   OGL 462     LMC205.5.171   + LMC205.5.477                                           Pli2012 
06026+0014   J  1362     BAL 988.                                                                        
                         J  2589.                                                                J__1962a
06026-0028   BAL 678     RST 4794.                                                                       
06029+2553   A   120     Change doubtful.                                                        B__1963b
06030+0945   MLL  10     Probably identical with ADS 4627, J 1323.                                       
06031+1248   BRT1193     B component spectral type F9V                                           AbH2000 
06032+5813   A  1315     A premature orbit has been computed.                                            
06032+3743   BRT2213     ALI 559.                                                                        
06032+1922   LDS6195     See Allen et al. (2000) for information on metallicity, age, galactic   AlC2000 
                         orbital parameters, etc.                                                        
                         AB: NLTT 15973/15974                                                    Chm2004 
                         HIP 28671. Close triple.                                                Tok2011a
06033-7045   OGL 463     LMC200.4.3454  + LMC200.4.3453                                          Pli2012 
06033-7122   OGL 464     LMC201.4.30    + LMC201.4.134                                           Pli2012 
06034+2738   STF 830     Neither AB or BC are physically associated.                             Kiy2015c
06034+1156   BPM 249     [PM2000]  382594 + [PM2000]  382195.                                    Gvr2010 
06035+1941   MCA  24     64 Ori. A spectroscopic binary and occultation triple, with the wider           
                         pair, presumably, now resolved. Fekel & Scarfe report periods of                
                         14.57d and 13.03y.                                                      Fek1986 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 8.90 +/- 3.35, 7.95, and 3.31 Msun, respectively.             Mlk2012 
06036+0419   STF 837     Identical with STF 833. BAL2649.                                                
06037+2741   HJ 5467     Doubtful this system is physically bound, since relative and proper             
                         motions are of the same order.                                          Kiy2012 
06038+1816   STF 835     Same as HDS 824.                                                                
06038-7055   OGL 465     LMC200.3.3701  + LMC200.3.3806                                          Pli2012 
06039-7047   OGL 466     LMC200.4.3466  + LMC200.4.3890                                          Pli2012 
06040+3138   A   214     AC: SEI 455.                                                            Nsn2017b
06040+2734   HAU  17     Optical pair, since relative motion is equal to the difference in               
                         proper motions of the components within the errors.                     Kiy2012 
06041+2316   KUI  23     1 Gem. Primary 9.6d SB1 (#377 in Batten et al., 1989), secondary spec   Bte1989 
                         type K1III (Strassmeier & Fekel 1990), and reported to be an            Fek1990 
                         occultation binary. Mass sum close to expected.                                 
                         Evidently both visual components are giants with one, probably the              
                         later type component, double once more.                                         
                         Identification of the ascending node of the visual pair in the third            
                         quadrant is confused by the submotion and therefore not entirely                
                         certain.                                                                        
06041-7155   OGL 467     LMC202.4.13    + LMC202.4.72                                            Pli2012 
06042-0643   CIA  55     V696 Mon.                                                                       
06042-4109   HJ 3831     AC: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
06043-7021   OGL 468     LMC207.6.75    + LMC207.6.284                                           Pli2012 
06044+1731   BPM 250     [PM2000]  386053 + [PM2000]  386110.                                    Gvr2010 
06045+5134   STT 128     Possibly variable.                                                              
06045+4416   LEP  22     AB: HJL1044.                                                            HJL1986 
                         AB: A has planet 263d, 3.3 Mjup.                                        Tok2014d
             MUG  11     BC: Second-epoch observation of BC indicates the C component is                 
                         co-moving; hence HD 40979 is a triple-star system, with the exoplanet           
                         host star being the primary. Assuming a system age of 1 Gyr, I-band             
                         magnitudes yield masses 0.833 +/- 0.011 and 0.380 +/- 0.025 Msun for            
                         B and C. Spectral types are estimated at K3 and M3, respectively.       Mug2007b
                         BC: NLTT 15983, X-ray source.  Detection limits for BC (Mugrauer et             
                         al. 2007) show BC is CPM.  Mugrauer measure I(B)=7.98, I(C)=11.3,       Mug2007b
                         estimate masses 0.83 and 0.38 for B,C.                                  Tok2014d
06046+3014   STF 834     B is BD+30@1097.                                                                
06046-6921   OGL 469     LMC205.2.218   + LMC205.2.553                                           Pli2012 
06047-4505   HJ 3834     HIP 28790. E is HIP 28764.                                                      
                         AE: SHY 183. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
06048-4828   DUN  23     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         A is V575 Pup, var. RS CVn type, X-ray source, young, possible SB. B            
                         suspected binary (0.035") in 2008 at SOAR, but not confirmed by                 
                         further speckle data.  Castor moving group?                             Tok2014d
                         A is a close 2.5-d spectroscopic pair.                                  Tok2019a
06049-0521   BNW   4     Incorrectly identified as H 5 14 in BDS. Error noted by MacEvoy (2010). MEv2010 
06049-3434   BWL  20     AB: Deep AO imaging by Quantz et al. (2012 ApJ 754, 127) did not                
                         reveal any planetary companions down to dL'~11 at 0".5, corresponding           
                         to planetary masses near 1 Mjup. HiCIAO observations by Bowler et al.           
                         (2015) reached a sensitivity of dH=13.5 at 1" and identified a wide             
                         candidate companion at 7".1. Folowup astrometry at Keck showed it to            
                         be a background star. Primary is AP Col.                                Bwl2015 
06050+0410   66 Ori      Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Griffin (2006).                                                         Grf2006 
06052-1419   STF 843     Position corrected.                                                             
06053+7400   STT 121     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.15 +/- 1.21, 2.78, and 1.10 Msun, respectively.             Mlk2012 
06053-7056   OGL 470     LMC208.6.10    + LMC208.6.33                                            Pli2012 
06054+2459   BRT3266     Originally published as BRT 139.                                        Brt1928 
06054-6829   OGL 471     LMC204.4.7103  + LMC204.4.7242                                          Pli2012 
06055+1448   BPMA 23     [PM2000]  389828 + [PM2000]  390203.                                    Gvr2010 
06057-0637   BRT 375     Not found by Heintz at IDS position.                                    Hei1990b
06058+1237   BPM 251     [PM2000]  390772 + [PM2000]  390804.                                    Gvr2010 
06059+4815   ES 1234     The primary is a double-lined spectroscopic binary.                             
06061+3523   ENG  25     B is BD+35@1335.                                                                
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
06062+0629   STF 841     Rectilinear solution by Hartkopf & Mason (2015).                        WSI2015 
06063-2754   SKF 425     This star is likely a binary companion to the nearby K1-type star               
                         HD 41842 at 20" separation, as noted in the WDS.                        Jnn2012 
06064-1951   LDS3691     NLTT 16076/16077                                                        Chm2004 
06066+2620   EVS   4     Classical Cepheid AA Gem.                                                       
06066+1310   BPMA 24     [PM2000]  393185 + [PM2000]  392334.                                    Gvr2010 
06066+0431   VBS  12     The primary is Ross 413.                                                        
                         G106-025. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
06067+3611   ALI 317     No star seen at AC catalog location of the purported secondary                  
                         - probably a plate flaw.                                                        
06067-6933   OGL 472     LMC206.4.145   + LMC206.4.751                                           Pli2012 
06073-7242   OGL 473     LMC211.6.39    + LMC203.3.4778                                          Pli2012 
06074-0400   STF 850     Aka BRT 562.                                                                    
06075-2244   DON1065     CD-22@2776.                                                                     
06075-7033   OGL 474     LMC207.2.28    + LMC207.2.540                                           Pli2012 
06077-6925   OGL 475     LMC212.8.17    + LMC212.8.18                                            Pli2012 
06078-0623   PBS   4     The AD and AF pairs were erroneously given the discoverer designation,          
                         already assigned to another system.                                             
06079-4209   FIN  70     pi 2 Col. Position angle uncertain. Many attempts, but few                      
                         successful observations. Needs speckle.                                         
06079-6937   OGL 476     LMC206.4.4928  + LMC206.4.4929                                          Pli2012 
06081-2525   B    99     Last position angle uncertain. Not resolved by Finsen in 1960-62.               
                         Motion retrograde.                                                              
06083+1400   STF 844     B is BD+14@1161.                                                                
             ARN  64     AC: C component = U component of 06085+1358.                                    
06084+1141   BPM 252     [PM2000]  399162 + [PM2000]  399489.                                    Gvr2010 
06085+1358   STF 848     There has been considerable confusion in component identification for           
                         this complicated multiple. Components K, J, M, O, and Q were actually           
                         H, G, F, I, and J, respectively; pairs labelled PR, PS, PT, and PU              
                         were actually JR, RS, ST, and SU, respectively. Three CE measures               
                         actually were of JI, while one other was of DH. It is believed (but             
                         not guaranteed!) that components are now identified consistently.               
                         BD: Hipparcos suspected non-single.                                             
                         AB: H 1  57.                                                            MEv2010 
             JRN  23     SU: U component = C component of 06083+1400.                                    
06086+0722   STF 852     BD+07@1145a.                                                                    
06087+1724   STF 849     STF 828.                                                                        
06089+2138   ALV   4     AFGL 5180 IRS 1. Near center of CO outflow; extensive nebulosity.       Alv2004 
06090+0230   STF 855     B is BD+02@1140.  Same as STF 858.                                              
06091+3116   HJ  379     SEI 456.                                                                Nsn2017b
06092+6424   MLB 259     Rectilinear solution by Pavlovic et al. (2013).                         Pal2013 
06093+2839   A   121     164" in 247@ from BD+28@1026.                                                   
06093+2424   COU  85     Aka STJ  45. The COU pair was earlier and incorrectly associated with           
                         06093+2426 = STT 134.                                                           
06093-3550   WHH   1     Member of AB Dor group. Wahhaj et al. (2011) conclude the AB pair is            
                         physical, while the faint C component is a background object. The               
                         spectral type of B is L4 +/- 1, masses of A and B 0.4 +/- 0.05 Msun             
                         and 31 +/- 8 Mjup.                                                      Whh2011 
06095+2246   OL  206     BRT2344.                                                                        
06095+1400   BPM 253     [PM2000]  402672 + [PM2000]  402676.                                    Gvr2010 
06096+0540   STF 859     B is BD+05@1116. Same as STF 863.                                               
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
06097+4308   WEB   5     B is BD+43@1465.                                                                
06097+2307   BU 1241     3 Gem. B is variable.                                                           
06097-7046   OGL 477     LMC208.4.80    + LMC208.4.91                                            Pli2012 
06098+4632   BRT  92     The pair ES 1323 (= ADS 4740) is identical                              Hei1980a
06098-2246   RST3442     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.13 +/- 0.32, 2.92, and 1.17 Msun, respectively.             Mlk2012 
06098-7130   OGL 478     LMC209.6.4465  + LMC209.6.4729                                          Pli2012 
06100+1431   BPM 254     [PM2000]  404386 + [PM2000]  404061.                                    Gvr2010 
06100-0420   A  3021     Evidently, the same as J  2015.                                                 
06102+2423   POU1086     Aka POU1096.                                                            Bko2010b
06102-7057   OGL 479     LMC208.3.194   + LMC208.3.192                                           Pli2012 
06102-7445   EGN   5     Pair bound. B component is likely an M3.5-M6.5 dwarf with mass                  
                         0.14 +/- 0.01 Msun.                                                     Egn2007 
                         Jones et al. (2002): no detection of SB                                 CPS2002b
06103+1554   H 6 114     H VI 114.                                                                       
06104+2234   LAW  14     LSPM J0610+2234 = NLTT 16144. Law et al (2008) derive a distance of     Law2008 
                         17.0 +7.5/-2.9 pc and a projected separation of 4.6 +2.1/-0.8 au.               
                         Estimated spectral types are M5 and secondary later than M6.                    
06104+1034   BRT3374     Unnumbered pair, following BRT1195 in Barton's list.                    Brt1935a
06105+2421   POU1098     AB: Aka POU1106.                                                        Bko2010b
             POU1099     AC: Aka POU1107.                                                        Bko2010b
06105+2300   BU 1058     4 Gem.                                                                          
06106-2152   NAJ   1     Secondary is brown dwarf.                                                       
                         Pair is comprised of an M1 dwarf and a T dwarf.                         Kir1999 
06106-4701   GRV1250     Both A and B have approximately the same radial velocity.               Grv2019b
06107+3057   COU1102     KLT   2. KELT-2. Primary hosts a transiting hot Jupiter, P=4.11d.               
                         Beatty et al. (2012) determine the primary is a slightly evolved F7             
                         dwarf, the secondary a K2V. Masses are 1.314 +0.063/-0.060 and ~0.78            
                         Msun, radii 1.836 +0.066/-0.046 and ~0.70 Rsun. The orbital period is           
                         estimated at ~3500y.                                                    KLT2012 
06107-0951   STF 869     B is BD-09@1351, and is reported to be a variable of unknown type.              
06109+2037   J  1922     STF 864.                                                                        
06109+1020   KAM   1     Ross 79.                                                                        
                         Reported double by van de Kamp (1950 AJ 55, 160). Spectral type is              
                         given as M4 by Kuiper (1940 ApJ 92, 126). Pair difficult to measure             
                         with 12inch; delta m estimated at 3 mags. Motion questionable.          Wor1956b
06109+0621   J  2738     V2783 Ori. Primary is eclipsing binary of Algol-type, period 4.21618d.  Zas2014 
06109-0722   GCB  15     Listed in IDS at +07 degrees rather than -07, so not found by Heintz.   Hei1995 
                         Moved to correct location.                                                      
06111+1544   BPM 255     [PM2000]  408406 + [PM2000]  408514.                                    Gvr2010 
06111-5817   FIN  96     AO Pic, Algol-type eclipsing binary, P = 2.23415 d.                     Zas2011 
06113-0038   LDS6196     ALC   5. Incorrectly listed as 06113+0038.                                      
06113-7302   SKF1074     OGL 480. LMC211.8.3926  + LMC211.1.10                                   Pli2012 
06115+5702   ARG  13     B is BD+57@944.                                                                 
                         Additional notes may be found in Fox (1946).                            Fox1946 
06115-7049   OGL 481     LMC208.4.5070  + LMC208.4.5091                                          Pli2012 
06115-7214   JNN  48     Since the separation between the components of this system is very              
                         small (~0.16"), it is almost certainly a physical binary, although              
                         common proper motion has yet to be demonstrated.                        Jnn2012 
06116+4843   STF 845     41 Aur.                                                                         
                         H 3  82.                                                                MEv2010 
06116+2329   POU1127     Aka POU1136.                                                                    
06116+0146   J  1924     BAL 1304.                                                                       
06116-0410   GNO   3     Gellino et al. (2014) derive spectral types for this brown dwarf pair           
                         of L9 and T1.5; masses are 64.8 +/- 0.4 and 52.1 +/- 12.0 Mjup, and             
                         effective temperatures are 1300 +/- 26 and 1096 +/- 20K. Approximates           
                         ages for the two components are 1.5-4.0 and 1.0-2.0 Gyr.                Gno2014 
06116-7031   OGL 482     LMC214.7.10    + LMC214.7.67                                            Pli2012 
06117-0440   AC    3     A variable, V638 Mon.                                                           
06117-6909   OGL 483     LMC212.3.57    + LMC212.3.58                                            Pli2012 
06118-2030   RSS 102     CPD-20@1192                                                                     
06118-6927   OGL 484     LMC212.1.8     + LMC212.1.31                                            Pli2012 
06119+1413   J  2016     xi Ori = 70 Ori. A is a spectroscopic binary, P = 45.1d.                        
06120+1947   CHR 163     68 Ori. B is BD+19@1252.                                                        
             H 6  72     H VI 72.                                                                        
06122+0640   J  1925     Aka J  1927.                                                                    
06122-3036   HUE   1     At an assumed distance of 31 +/- 6 pc, the projected separation is              
                         11 +/- 2 au. Spectral types are estimated as T5-7 for both components;          
                         estimated masses of each component are ~30Mjup (for an age of 1Gyr) or          
                         ~60Mjup (for an age of 5Gyr).                                           Hue2015 
06122-6532   DUN  26     B is CPD-65@566.                                                                
                         SHY 496. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
             TOK 106     HIP 29444. B is HIP 29439.                                                      
06123-7031   OGL 485     LMC214.7.4713  + LMC214.7.4718                                          Pli2012 
06124+2359   J  1102     Found to be single in 1958 and 1960 by Couteau. Probable positional     Cou1958c
                         error.                                                                  Cou1961a
06128-7023   OGL 486     LMC214.6.4957  + LMC214.6.5063                                          Pli2012 
06129+1759   SH 2-255    IRS 1 and IRS 3 are both in a cluster of IR sources.                    Alv2004 
06130-2203   BRT 304     CD-22@2857.                                                                     
06131+4431   BRT 113     Single, distant companion.                                              Brt1938 
06132-2742   TSN   2     May be physically associated with the Brown Dwarf 2MASS                 TSN2014b
                         J06085283-2753583 separated by 3529" @ 78.0 degrees.                            
06134+0556   J   969     PAN   5.                                                                        
06134-7017   OGL 487     LMC214.5.3916  + LMC214.5.4537                                          Pli2012 
06136+1505   BPM 256     [PM2000]  418424 + [PM2000]  418656.                                    Gvr2010 
06136-1527   GAL 396     Object #220 in Gallo's original list.                                   Gal1914 
06137-0019   BAL 686     HJL  75.                                                                HJL1986 
06137-2815   JNN  49     This binary consists of two components with almost equal brightnesses           
                         and colors. Although common proper motion has not yet been                      
                         demonstrated, it thus counts as binary in the statistical analysis.     Jnn2012 
06138+3509   GCB  16     ALI  85.                                                                        
06138-2352   JNN  50     The close binary pair resolved by AstraLux is likely itself a wide              
                         companion to the nearby G5-type star HD 43162 at 25" separation, as             
                         noted in the WDS. Hence the system is likely triple, although common            
                         proper motion has not yet been deomnstrated.                            Jnn2012 
06139-3030   HJ 3840     SWR   9.                                                                        
06140+3726   BRT2214     ALI 563 is identical                                                    Hei1983a
06141+2359   STTA 70     Also known as FRK   5. B is BD+23@1258.                                         
06141+2129   BRT2347     J 2591.                                                                         
06141+0149   J  1821     RST 5222. BAL 1307.                                                             
06142+1124   BPM 257     [PM2000]  421303 + [PM2000]  421205.                                    Gvr2010 
06142-1436   LDS 847     NLTT 16269/16270                                                        Chm2004 
06142-7213   OGL 488     LMC210.2.3931  + LMC210.2.4978                                          Pli2012 
06143+1430   S   509     B is BD+14@1210.                                                                
06144+0052   BAL 992     J  1931.                                                                        
06145+3824   AG  108     ALI 817.                                                                        
06145+1754   KUI  24     A spectroscopic binary.                                                         
                         Additional notes may be found in Couteau (1955).                        Cou1955c
06145+1148   STTA 71     B is BD+11@1075.                                                                
06145-4521   CPO 133     B is CD-45@2390.                                                                
06146+0051   BAL 993     J  1932.                                                                        
06147+1435   STF 877     B is a spectroscopic binary.                                                    
06147+0714   J  1933     BRT2115. The 1901 Barton and Jonckheere measures were both generated    Brt1938 
                         from probably spurious data in the Astrographic Catalog.                J__1962a
06147-0427   A   505     Aitken's estimate of companion magnitude is of course much too faint.   B__1963b
06148+1909   HJ 2302     71 Ori.                                                                         
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
06148+1232   BPM 258     [PM2000]  423906 + [PM2000]  424046.                                    Gvr2010 
06148-7020   OGL 489     LMC214.3.122   + LMC214.3.950                                           Pli2012 
06149+2230   BU 1008     eta Gem = 7 Gem = Propus. The primary is a semiregular variable,                
                         occultation binary, and SB1, P = 8.17 yr.                               MLa1944 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Mk III Limb-darkened diameter 11.789 +/- 0.118 mas.                     MkT2003 
                         Rectilinear solution by Scardia et al. (2018).                          Sca2018b
06149-0617   HJ  384     gam Mon = 5 Mon                                                                 
                         NPOI Limb-darkened diameter  3.097 +/- 0.034 mas, Sp = K1III,           NOI2018 
                         R = 50.82 +/- 1.58 \rsun, Teff = 4810 +/- 66 K, L = 1247 +/- 96  \lsun,         
                         M = 4.19 +/- 0.14 \msun, Age = 0.17 +/- 0.02 Gyr.                               
06150-7025   OGL 490     LMC214.3.59    + LMC214.3.277                                           Pli2012 
06150-7236   OGL 491     LMC211.4.3772  + LMC211.4.3798                                          Pli2012 
06151+1355   BPM 259     [PM2000]  425229 + [PM2000]  425385.                                    Gvr2010 
06152-7028   OGL 492     LMC214.2.11    + LMC214.2.253                                           Pli2012 
06154+1856   VAS   7     VSK   1.                                                                        
06154+1614   BPM 260     [PM2000]  426446 + [PM2000]  426575.                                    Gvr2010 
06154-0902   A   668     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 6.97 +/- 2.42, 4.79, and 3.09 Msun, respectively.             Mlk2012 
06155+1902   CXT   2     J  2740.                                                                        
06155+1157   J  1363     BRT 1197.                                                                       
06155+0232   BAL1687     Not found by Heintz at IDS position.                                    Hei1985a
06156+6609   STTA 69     BC is BD+66@436. MLR 316.                                                       
06156+3609   STF 872     AB: HJL  76.                                                            HJL1986 
                         AB: RoboAO finds on 2013.62 Aa,Ab at 1.30", 204d, dI=5.1, rejected as           
                         uncertain.                                                              Tok2014d
06157+6000   BUP  86     40 Cam.                                                                         
06157+1316   BPM 261     [PM2000]  427745 + [PM2000]  427700.                                    Gvr2010 
06159+0110   RST5225     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.62 +/- 0.81, 2.84, and 1.35 Msun, respectively.             Mlk2012 
06162-1321   BRG  22     In Bergfors et al. (2010), we detected a close binary companion to      Brg2010 
                         2MASS J06161032-1320422 at 190 mas separation. In a re-observation of           
                         the target from February 2010, there is no resolved companion detected          
                         but only a slightly extended primary PSF, hence the binary separation           
                         probably decreased in the meantime.                                     Jnn2012 
06163-5913   DUN  27     B is CPD-59@618.                                                                
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             LDS 157     AC: C=WD 0615-591, DB3.2 type.  Mass=0.61 Msun (Holberg et al. 2013)    Hbg2013 
06164+1216   KUI  26     74 Ori.                                                                         
06164-7036   OGL 493     LMC214.1.3275  + LMC214.1.3458                                          Pli2012 
06165+2318   J   341     A = EPIC 202073186, eclipsing binary of Algol-type, period 1.22483d.    Zas2015 
                         AC: Aka COU2715.                                                                
06167+3852   J   591     Single 1931 (Giacobini). Position may be erroneous.                     Gcb1934 
                         Aka BTG   1AC.                                                                  
06168+3832   BRT2215     ALI 818.                                                                        
06168-1359   GAL 397     Object #221 in Gallo's original list.                                   Gal1914 
06169+2414   POU1187     J 1936.                                                                         
06171+1551   H 5  23     H V 23. B is BD+15@1138.                                                        
06171+0957   FIN 331     75 Ori.                                                                         
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 3.13 +/- 0.24, 3.73, and 2.09 Msun, respectively.  Mlk2012 
06171-2243   HJ 3845     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Friedman et al. (2012).                         USN2012a
06172+3312   COU1406     The variable VW Aur.                                                            
06172+1204   BPMA 25     [PM2000]  434066 + [PM2000]  433779.                                    Gvr2010 
06172-3715   EHR   8     Physical/optical nature ambiguous.                                      Ehr2010 
06173+3700   MLB1011     ALI 564.                                                                        
06173+0506   ENG  26     AB: B is BD+05@1165.                                                            
             CAT   1     Aa,Ab. Catala et al. (2006) calculate masses 0.96 +/- 0.18 and 0.67     Cat2006 
                         +/- 0.04 Msun.                                                                  
                         The 27 yr pair CAT 1 with computed visual (Hartkopf et al. 2012) and    Hrt2012a
                         SB orbits is responsible for dmu. Triple with the CPM companion                 
                         LEP 24 AE at 103".                                                      Tok2012a
             PRV   3     Ea,Eb: GJ 231.1B. Pravdo et al. (2006) derive masses 0.25 +/- 0.6 and           
                         0.12 +/- 0.02 Msun.                                                     Prv2006 
                         Ea,Eb: NLTT 16333. Estimated age 1000-10000 Myr; masses 0.39 +/- 0.06           
                         and 0.15 +/- 0.02 Msun; a ~11.9 au.                                     Jnn2014 
06174+5725   TOK 259     Primary is SB2, P=958d (Griffin 2011).                                  Grf2011b
06175-1537   GAL 398     Object #223 in Gallo's original list.                                   Gal1914 
06178+2612   AG  322     B is BD+26@1167.                                                                
06179+0919   OPI   9     J 2419. KRU 2.                                                                  
06180+2152   KRU   1     J  1938.                                                                        
06181+1423   HO  229     J  2018.                                                                        
06184+3633   CHE  81     AC: ALI 320.                                                                    
06184+1256   BPM 262     [PM2000]  439525 + [PM2000]  439378.                                    Gvr2010 
06185+1611   BPM 263     [PM2000]  439937 + [PM2000]  440011.                                    Gvr2010 
06185+1610   BPM 264     [PM2000]  440156 + [PM2000]  440111.                                    Gvr2010 
06186+2151   HU  451     TDS3722.                                                                        
06186-2922   I  1116     Spectrum: A2(m)A7/8-F2.                                                         
06187+0903   GC 8096     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin (1986).                                                         Grf1986b
06188-7052   OGL 494     LMC215.4.3953  + LMC215.4.3954                                          Pli2012 
06192+1448   HJ 3281     Woods measures this pair 1909.98, 262.4@, 5.72".                        Woo1913 
                         Another pair?                                                                   
06192-5803   CVN  15     AB Pic. Spectral type for B component L1 +2/-1.                         Cvn2005c
06193-0250   OL   66     BRT 536.                                                                Brt1931 
06193-1232   HO  231     This pair was listed as HJ 3847, but with an error of two degrees in            
                         declination.                                                                    
06193-2458   S   516     AB: B is CD-24@3914.                                                            
06194+2316   H 5  55     H V 55. There has been considerable confusion between this pair and             
                         06199+2316, with this being labelled the AC pair and the others                 
                         additional components of this system.                                           
06194+1326   STTA 73     B is BD+13@1200, and is a spectroscopic binary. Pair appears in an              
                         appendix list, not part of discoverer's regular numbering sequence.             
06194+1219   BPM 266     [PM2000]  444117 + [PM2000]  443589.                                    Gvr2010 
06194+1159   BPM 265     [PM2000]  444041 + [PM2000]  443892.                                    Gvr2010 
06195+1220   STF 892     Rectilinear solution by Friedman et al. (2011).                         USN2011a
06196+5901   UZ Lyn      Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
06196+1219   BPM 267     [PM2000]  445356 + [PM2000]  445120.                                    Gvr2010 
06197-0749   CHR  22     7 Mon.                                                                          
06198-3930   HJ 3849     B is CD-39@2525.                                                                
06199+2316   BNW   3     See note to 06194+2316. B component is BD+23 1309.                              
06200+2826   BU  895     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 4.90 +/- 11.16, 3.28, and 1.74 Msun, respectively. Mlk2012 
06200-1038   A  2925     Apparently a rapid binary. In the "red rectangle", a bi-polar nebula.           
                         See Meaburn et al. (1983) for a discussion of the observational         Mea1983 
                         history of this object.                                                         
06202-1044   TOK 108     HIP 30114.                                                              Tok2011a
06203-3004   SMY   1     zet CMa = 1 CMa = Furud. A is a long-period spectroscopic binary.               
                         P = 675d. B is CD-29@3008.                                                      
06204+2940   BRT3273     Barton calls this RMK 4, and this is copied in ADS, But RMK 4 is        Brt1926a
                         properly CPD-57@659.                                                    Bu_1932A
06206+2511   STTA 74     B is BD+25@1222.                                                                
06206+2327   POU1237     J  1822.                                                                        
06206+1803   STTA 75     B is BD+18@1179.                                                                
06208+1216   BPM 268     [PM2000]  450815 + [PM2000]  451412.                                    Gvr2010 
06208+0106   J  2019     BAL1310.                                                                        
06212+2108   S   513     STTA 76.  BC: STT 137.                                                          
                         Jorissen's BF and BG pairs are S 513 BT and BS, respectively.                   
06212-3507   SWR  10     CPM pair                                                                Skf2004 
06214+2203   L    58     Lewis measured an unidentified pair near this position: 1910.19,        GrO1932A
                         120.5@, 1.22", 9.0-9.5, n=1. ADS identifies this pair as JDS 1198 and   Bu_1932A
                         notes that Lewis' measure was not included in the Greenwich catalog.            
                         Aka L    37.                                                                    
06214+0216   A  2667     One component variable?                                                 Mlr1956a
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Algol-type eclipsing binary, period 5.5640 d.                           Zas2019 
                         No doubt about quadrant in these measures.                              VBs1954 
06214-1146   STF3116     A is a Cepheid, FR CMa.                                                         
06215+6224   STF 878     AB: Rectilinear solution by Friedman et al. (2012).                     USN2012a
06215+1618   LDS 894     NLTT 16409/16412                                                        Chm2004 
06215-1625   GAL 399     Object #227 in Gallo's original list.                                   Gal1914 
06220-0202   BAL 319     J 2741.                                                                         
06221+5922   CHR 128     4 Lyn.                                                                          
             WAL  45     AE: No good match to Wallenquist's estimated 0deg, 70" astrometry for   Wal1947 
                         this pair. Since he gives dm values for AB,C, AB,D, and AB,E, it is             
                         apparently not the AD pair at ~0deg, 100". Best guess is that there is          
                         a typographical error and he meant 30deg, 70", in reasonable agreement          
                         in astrometry and photometry with a pair at 31deg, 77".                         
06221+2645   DBR  22     DBR  90.                                                                        
06221+2203   L    59     Aka J  1941.                                                                    
06221-3326   del Col     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Jones (1928).                                                           Jon1928b
06225-0259   HJ  387     J 1471.                                                                         
06225-3107   LDS5675     Aka LDS 159.                                                            Dam2016a
06225-6013   SHY  34     AB: HIP  30314 + HIP  31878. B component = C component of 05287-6527            
                         and 06380-6132.                                                         Shy2011 
                         AB: AB Dor moving group. A is PMS star.  Shaya & Olling (2011) list 5   Shy2011 
                         co-moving companions, 1 to 5.8pc separations.                           Tok2014d
                         AD: HIP  30314 + HIP  26373. D component = A component of 05369-4758            
                         = E component of 05287-6527.                                                    
06226+2647   DBR  16     DBR  93.                                                                        
06227+1314   BPM 269     [PM2000]  460119 + [PM2000]  459988.                                    Gvr2010 
06227-1757   BUP  88     bet CMa = 2 CMa = Mirzam. Prototype of its class of variable.                   
                         Intensity Interferometer Limb-darkened diameter 0.52 +/- 0.03 mas.      HBr1974 
                         B is BD-17@1466.                                                                
06229+4517   LDS3698     NLTT 16424/16420                                                        Chm2004 
06229-3337   HIP  30338  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Udry et al. (1998).                                                     Udr1998 
06230+2231   BU 1059     mu Gem = 13 Gem = Tejat. A is an irregular variable.                            
                         Mk III Limb-darkened diameter 15.118 +/- 0.151 mas.                     MkT2003 
06233+2209   OL  207     TDS3789.                                                                        
06233-2827   WFC  34     SWR  11.                                                                        
06234+1432   J  1254     C is an Algol-type system, FI Ori.                                              
06234-0952   GAL 400     Object #232 in Gallo's original list.                                   Gal1914 
06234-2235   LDS 160     NLTT 16468/16466                                                        Chm2004 
06235+4717   ES 1236     V Aur. BD is +47@1291a.                                                         
06235-1246   GAL 401     Object #233 in Gallo's original list.                                   Gal1914 
06236+1205   BPM 270     [PM2000]  464759 + [PM2000]  464294.                                    Gvr2010 
06236+1147   BPM 271     [PM2000]  464830 + [PM2000]  464559.                                    Gvr2010 
06236-0938   JNN 270     Estimated age 1000-10000 Myr; masses 0.32 +/- 0.19 and 0.12 +/- 0.05            
                         Msun; a ~33.5 au.                                                       Jnn2014 
06237-7505   JNN  51     Although not yet confirmed to share a common proper motion, the                 
                         companion to 2MASS J06234024-7504327 is both relatively close ~0.57"            
                         and has consistent brightness and color to what should be expected for          
                         a physical companion, and is catagorized as such.                       Jnn2012 
06238+0436   STF 900     eps Mon. A is a spectroscopic binary, P = 331d? B is BD+04@1237.                
                         AB: H 3  29.                                                            MEv2010 
06239+0111   BAL1313     J 1943.                                                                         
06240-2137   B  2110     CPD-21@1254.                                                                    
06240-3642   DUN  28     AC : Identified as optical and linear soltion published.                LRR2022c
06240-5242   MAM   2     alp Car = Canopus.                                                              
                         Intensity Interferometer Limb-darkened diameter 6.6  +/- 0.8  mas.      HBr1974 
06241+2505   J  1942     J 2424 is identical                                                     Hei1983a
06243+6006   STF 887     STI 598.                                                                        
06243+1322   BRT1201     C component spectral type A2Va                                          AbH2000 
             ABH  45     The measures previously listed as BD, BE, BF, and BG appear to have     AbH2000 
                         been actually measured from A. All were moved and new matches made.             
06244+1119   BPM 272     [PM2000]  469241 + [PM2000]  469171.                                    Gvr2010 
06244-1613   S   518     B is BD-16@1468.                                                                
                         H 4  80.                                                                MEv2010 
06247+5940   STTA 72     AC: H 6  23.                                                            MEv2010 
06247+2503   GC 8261     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin (1986).                                                         Grf1986a
06247+2107   J   688     A = EPIC 202093968, eclipsing binary of Algol-type, period 2.470 days.  Zas2015 
06247-0544   HJ   38     BDS gives 1900: 06h 17.9m, -05@40'.                                     Bu_1906 
06248+4405   GIC  57     G101-037/G101-032.  Transcription error led to this pair being entered          
                         in the WDS as 05249+4410. Giclas noted "These stars show very nearly    Gic1971 
                         the same proper motion. The separation is 1.2 degrees."                         
06248+0005   J  2427     BAL 1003.                                                                       
06249+3150   AG  111     SEI 457.                                                                Nsn2017b
06249+1424   A  2722     A = HD 44905 = EPIC 202059360, eclipsing binary of Beta Lyrae type,     .      
                         period 3.674801 days.                                                   Zas2015 
06251+1614   BPM 274     [PM2000]  472953 + [PM2000]  472934.                                    Gvr2010 
06251+1534   BPM 273     [PM2000]  472815 + [PM2000]  472067.                                    Gvr2010 
06252+0705   EVS  11     Primary is the Cepheid T Mon.                                           Evs2016a
06253+0256   BAL1693     J 2743.                                                                         
06253+0130   FIN 343     Docobo & Andrade (2013) derive a dynamical parallax of 4.61 +/- 0.16            
                         mas and component masses 2.77 +/- 0.36 and 2.32 +/- 0.30 Msun. See              
                         paper for extensive notes on this system.                               Doc2013d
06254-1406   GAL 402     Object #236 in Gallo's original list.                                   Gal1914 
06255+2327   BAG   5     First detected as an occultation binary by Schmidtke & Africano.        Smk1984 
                         Also known as CHR  23.                                                          
                         Calculated mass sum is 2.53 +/- 1.3 Msun, not well-constrained due to           
                         the short fraction of the orbit covered.                                Mut2010b
06255+2320   MCA  26     An occultation and interferometric binary.                                      
                         First detected as an occultation binary by Africano.                    Afr1975 
                         1979.7709: This negative result was incorrectly attributed to ADS 5103          
                         in McAlister & Hendry (1981).                                           McA1981b
06255+1213   BPM 275     [PM2000]  475095 + [PM2000]  475644.                                    Gvr2010 
06256+3648   BRT2588     ALI 322.                                                                        
06257+1624   TOR   9     Formerly known as PAN   6.                                                      
06258+3627   BRT3245     ALI 323. A is an irregular variable, KS Aur.                                    
06259+5153   STF 896     B is BD+51@1189.                                                                
06259+1747   J   900     AB are lobes of the planetary nebula PN G194.2+02.5 = HD 45043.         Skf2013 
                         As A component is a PN, the quoted magnitude is integrated flux.                
06259+1640   BPMA 26     [PM2000]  477116 + [PM2000]  475748.                                    Gvr2010 
06259+0944   OPI  11     AC: Opik (1927) measure was originally entered in the WDS incorrectly   Opi1927 
                         as 40" rather than 4'. This resulted in an incorrect component match            
                         by Harshaw (2013).                                                      Hsw2013b
06260+2800   RUC   6     AH Aur. Spectral type of resolved companion M3-5V or possibly later.    Ruc2007 
06262+1845   BU 1191     A is a spectroscopic binary, P = 6.99d. It is also one of the                   
                         brightest BY Dra-type variables known, OU Gem.                          B__1963b
06264-2908   COO 266     DAW 121.                                                                        
06265+6557   MLB1066     LDS2521.                                                                        
06265+2011   J  1823     SLE 744.                                                                        
06265-0740   JNN  52     The motion in the 2MASS J06262932-0739540 system is not yet sufficient          
                         to determine whether the two components share a common proper motion,           
                         but since the separation is small (~0.47") and colors and brightnesses          
                         of the components are consistent with expectation, it is likely that            
                         they form a physical pair. The system counts as binary in the                   
                         statistical analysis.                                                   Jnn2012 
06265-2649   HJ 3859     SWR  12.                                                                        
06266+1531   STT 140     Same as CHE  82.                                                                
06266-2108   B  2113     CPD-21@1283.                                                                    
06267-0731   STF 914     BDS 3401 probably same star. B is BD-07@1428.                                   
                         H 3  43.                                                                MEv2010 
06268+5825   S   514     5 Lyn. A is a spectroscopic binary.                                             
                         Also known as STF 894 and H VI 102.                                             
                         AC: H 6 102.                                                            MEv2010 
06269+2951   HJ  388     Rectilinear solution by Friedman et al. (2011).                         USN2011a
06272-4302   GRV1251     Both A and B have approximately the same radial velocity.               Grv2019b
06273+1453   CHR 251     The classification is from Conti & Leep (1974).                         Cti1974 
                         The star was resolved in the single observation we made.                Msn1998a
06273+0532   SLE 285     There appears to be a ~36" error in the declination of the primary by           
                         Soulie (1983).                                                          Sle1983 
06274+0354   BAL2169     J 1947.                                                                         
06274+0211   BAL1694     J 1946.                                                                         
06274-2544   B   114     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.50 +/- 0.27, 1.74, and 0.85 Msun, respectively.             Mlk2012 
                         Gomez et al. (2016) derive dynamical parallax and component masses:             
                         24.21 +/- 0.20 mas, 0.797 +/- 0.003 Msun, 0.752 +/- 0.003 Msun.         Doc2016i
06275+2432   AG  112     ADS notes that Anderson's 1913 distance measure (3".36) has been        A__1932b
                         rejected.                                                               AnR1913 
06275+1124   BPM 276     [PM2000]  486225 + [PM2000]  486846.                                    Gvr2010 
06276+1721   BPM 277     [PM2000]  486731 + [PM2000]  486189.                                    Gvr2010 
06276-1112   GAL 403     Object #237 in Gallo's original list.                                   Gal1914 
06276-2524   BRT2874     CPD-25@1447.                                                                    
06277+2249   J  1092     AB: Rectilinear solution by Cvetkovic et al. (2018).                    Cve2018 
06277+0034   BAL1009     J 1948. J 1996.                                                                 
06278+2047   SHJ  70     B is BD+20@1426.                                                                
                         AB: H 5  52.                                                            MEv2010 
06280-0446   BUP  89     10 Mon.                                                                         
                         AB: H 5  14.                                                            MEv2010 
06282+1712   BPM 278     [PM2000]  490130 + [PM2000]  490048.                                    Gvr2010 
06282+0516   STF 915     Variable, V648 Mon.                                                             
                         AB: H 2  89.                                                            MEv2010 
06283+3716   DBR 101     DBR 113.                                                                        
06283-0111   JNN  53     The companion that was detected in the AstraLux images has not yet              
                         been confirmed as a physical companion through common proper motion.            
                         However, the two components have nearly equal brightness and colors,            
                         and a relatively small separation of ~1.4" hence it is very likely              
                         that it is a real physical binary, and it is counted as such here for           
                         statistical purposes.                                                   Jnn2012 
06283-1303   BNS   2     FS CMa = MWC 142                                                                
06284+3116   AG  113     HJL  77.                                                                HJL1986 
                         AB: SEI 459.                                                            Nsn2017b
06284-0428   J  1949     B is BD-04@1533.                                                                
06284-0647   J  1473     OL 139 is probably identical                                            Hei1983a
06286+3030   GAA   3     RT Aur. The binary nature of this short-period Cepheid is still                 
                         uncertain, however Gallenne et al. (2015) believe they might have               
                         detected it  for the first time. See notes in that paper regarding              
                         previously published hints of binarity. Removing this possible                  
                         companion from their interferometric data, they estimated the                   
                         detection limit. They reached a minimum dynamic range of 0.47%,                 
                         corresponding to dmH> 5.8 mag. This limit excludes the presence of      .     
                         any additional companion with a spectral type earlier than F0V.         GaA2015 
06286-7854   HJ 3888     B is CPD-78@233.                                                                
06287-0240   TOR  10     Formerly known as PAN   7.                                                      
06287-3222   BU  753     Variable.                                                                       
06288-0702   STF 919     bet Mon = 11 Mon. Found double by Benedetto Castelli on 30 January              
                         1617. A,B, and C are shell stars.                                               
                         AB: H 2  17.  BC: H 1  10.                                              MEv2010 
06289-1408   GAL 404     Object #239 in Gallo's original list.                                   Gal1914 
06290+8210   MLR 494     AB: Also known as TDS3864.                                                      
06290+2013   BTZ   1     Aa,Ab: nu Gem = 18 Gem. Probably a spectroscopic binary, now resolved.          
                         1975.780: Oblate correlation peak, under very poor seeing.              Bla1977a
                         A negative result on 1979.7709, incorrectly attributed to ADS 5103 in           
                         McAlister & Hendry (1981), actually belongs to HR 2304.                 McA1981b
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 7.03 +/- 2.32, 8.95, and 4.79 Msun, respectively.  Mlk2012 
             BU 1192     Ba,Bb: Round 1955 (Van Biesbroeck and Finsen) but uncertain whether     VBs9999 
                         measures pertain to Ba,Bb or Aa,Ab.                                     Fin1956a
06291+4131   FAR   5     Primary is white dwarf WD 0625+415 = GD 74.                             Far2005b
06291-0311   TOR  11     Formerly known as PAN   8.                                                      
06291-4022   DUN  29     B is CD-40@2487.                                                                
                         Identified as optical and linear solution also published.               LRR2022c
06292+0239   BAL1695     KUI.                                                                            
06293+3439   MLB1047     ES 2467 is identical                                                    Hei1980a
06293-0248   B  2601     Ross 614, aka GJ 234. Possibly first resolved by van den Bos.           B__1951a
                         Good resolved solution with the aid of scattered visual and IR speckle          
                         observations. Mass-ratio calculated from pc orbit size.                         
                         Star B is the flare star V577 Mon; star A is also suspected to flare.           
                         Lippincott (1955) orbit is based on the astrometric elements            Lip1955 
                         combined with Baade's observation of the companion in 1955.                     
                         Combined solution from astrometry, spectroscopy, and parallax.                  
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         1986.952: combination of NS and EW 1-D IR speckle data for 1986.952     Cpb1994 
                         1991.896: combination of data from 1991.894 and 1991.897                Cpb1994 
                         1992.143: combination of data from 1992.141 -- 1992.146                 Cpb1994 
                         Solution includes mass and orbital parallax determination.              Sgr2000 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 0.30 +/- 0.02, 0.27, and 0.41 Msun, respectively.  Mlk2012 
06296+7258   HJ 2309     See note in ADS.                                                        A__1932b
                         AC: Additional notes may be found in Heintz (1963).                     Hei1963b
06296-0231   TOR  12     Formerly known as PAN   9.                                                      
06297-4649   LDS 163     TSN  76.                                                                        
06298-5014   R    65     AB and CD form the multiple system DUN 30 (12").                                
                         Difficult a/e/i- correlation, more obs needed.                                  
06299+0707   STT 142     The primary is a spectroscopic binary. The pair formerly listed as              
                         J 2004 appears to be identical, with distance doubled.                          
06300+1507   BPM 279     [PM2000]  499321 + [PM2000]  498872.                                    Gvr2010 
06300-1056   GAL 405     Object #241 in Gallo's original list.                                   Gal1914 
06300-1840   DE0630-18   DENIS J063001.4-184014. Primary is M8.5, secondary is probably a                
                         massive brown dwarf.                                                    SaJ2015 
06300-1924   WSI 123     Rectilinear solution by Miles & Mason (2016)                            Msn2016b
                         and Mason et al. (2018).                                                Msn2018a
06302+1807   BPM 280     [PM2000]  500040 + [PM2000]  500281.                                    Gvr2010 
06302+1116   BPM 281     [PM2000]  500138 + [PM2000]  500537.                                    Gvr2010 
06302-2228   BRT1388     CD-22@3140.                                                                     
06303-5252   TOK 435     Aa,Ab: HIP 30995 is an SB2 according to GCS. The new companion at 0".2          
                         with dI = 4.1~mag is unlikely to correspond to the SB2, so the system           
                         is probably triple.                                                     Tok2015c
06305+2940   DAE   9     WSP  12. WASP-12. Bergfors et al (2013) estimate spectral types G0V     Brg2013 
                         and K0-M0V. WASP-12b is one of the largest and hottest transiting               
                         planets; period 1.09d. Bergfors 6 is a point source ~3 mags fainter,            
                         at a separation of 1". Based on color, the companion is an M0-M1 main-          
                         sequence star. Relative photometry suggests Bergfors 6 is ~50% closer           
                         to Earth than is WASP-12, and that their consistent radial velocities           
                         are coincidental. If Bergfors 6 is a binary M dwarf system near                 
                         conjunction, however, it could lie at a similar distance to WASP-12             
                         and the system could be gravitationally bound.                          Csf2012 
             BEC   1     BC: Bechter et al. (2014) resolved the 1" companion to WASP 12 into 2           
                         ~equal magnitude stars, separated by 84 mas. Both components appear to          
                         be physically associated with the primary. Spectral types of B and C            
                         components M3V, masses 0.38 +/- 0.05 and 0.37 +/- 0.05 Msun.            Bec2014 
06305+0420   STF 920     AB: H 3  98.                                                            MEv2010 
06305-1457   HJ 3864     KL CMa, Algol-type eclipsing binary, P = 1.76222 d.                     Zas2011 
06306-0205   LDS5677     LDS6198.                                                                        
06307+2025   JRN  29     AC = SLE 756.                                                                   
06307-4649   CPO 137AB   A likely plate flaw.                                                    Grv2021b
06308+5810   STT 562     6 Lyn. B is BD+58@933.                                                          
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         CHARA Array Limb-darkened diameter  0.853 +/- 0.013 mas,                CIA2018c
                         R =  5.12 +/- 0.16 \rsun, L = 14.2 +/- 0.9 \lsun,                               
                         Teff = 4949 +/-  58 K.                                                          
06308+3811   COU1874     TDS3883.                                                                        
06310+5351   STF 908     STI2145.                                                                        
06310+5003   BWL  21     Colors and/or astrometry are inconsistent with a late-type common               
                         proper motion companion based on visual inspection of the field from            
                         2MASS, SDSS, DSS1, and/or DSS2. Primary is GJ 3395.                     Bwl2015 
06311+2143   WEI  12     BDS 3400 is the same star?                                                      
06311-3817   SWR  13     CPM pair                                                                Skf2004 
06312+1656   STT 143     A is a spectroscopic binary.                                                    
06312+1115   STF 921     B is BD+11@1205.                                                                
                         H N   2.                                                                MEv2010 
06312+0956   A  2816     Primary is V727 Mon, a Beta Lyr type eclipsing binary, P = 0.79848d.    Zas2012 
06312-1039   GAL 406     Object #245 in Gallo's original list.                                   Gal1914 
06314+1646   BPM 282     [PM2000]  504691 + [PM2000]  504499.                                    Gvr2010 
06314+0749   A  2817     B has a spectroscopic subcomponent with a period of 213d. The combined  Tok2020h
                         solution of AB yields masses of 1.12 and 1.46 \msun for A and B,                
                         respectively. The orbital parallax is 14.05 +/- 0.33 mas.                       
06315+6244   STI 606     Aka ES 1890.                                                                    
06315+0212   BAL1697     J 1952.                                                                         
06316+2343   POU1398     POU1400.                                                                        
06317+0546   STF 926     AB: H 3  75.                                                            MEv2010 
06319+4542   ARG  14     Also known as WFC  36.                                                          
06319+0457   GAN   3     A is a Beta CMa-type variable.                                                  
             SLE 293     AI: H 6  65.                                                            MEv2010 
06319+0039   GIC  62     G106-055/G108-010.                                                              
06319-0938   A   670     Rapid direct motion.                                                            
06319-2325   SEE  68     zet 1 CMa. A is a Beta CMa-type variable.                                       
                         The A component is a Beta Cep pulsating star with a 0.21d period.       IAU2014d
06319-3245   JSP 105     CPD-32@1200.                                                                    
06320+3432   GIC  63     AB = G103-036AB.                                                                
                         AB: NLTT 16624/16625                                                    Chm2004 
06320-5845   HJ 3874     mu Pic                                                                          
06321+0458   STF 927     AB: Incorrectly identified as H 2  37 in BDS. Error noted by MacEvoy.   MEv2010 
                         Algol-type eclipsing binary, P = 3.094 d.                               Zas2011 
06321-0006   GAU3871     RST 4811.                                                                       
06322+0833   GCB  69     Not found by Heintz, who thinks in may be nearby J   692.               Hei1995 
06322+0639   EVS   5     Classical Cepheid CS Mon.                                                       
06322+0450   TRN  20     The image rotator was in an unknown state, so two possible theta                
                         values are listed for the 2001.8661 observation - one for zenith up             
                         and one for north up.                                                   Trn2008 
06322-6519   HD 47121    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
06323+1747   STF 924     BDS 3424 probably same star. Spectrum of B: F6IV/V.                             
                         The A component is an occultation double.                                       
                         AB: H 4  28.                                                            MEv2010 
                         Toyota et al. (2009) monitored the RV of both the Aa and B components           
                         every 1-2 months between 2003 Mar - 2007 Nov, using a high-dispersion           
                         echelle (precision ~10 m/s).  The Aa component is a suggested SB                
                         (Wright et al. 2003 AJ 125, 359). Observed RVs varied betwwen -400 and          
                         +280 m/s, but showed no significant periodic variation. B exhibits              
                         rapid rotation, so RV could not be measured to high precision.          Toy2009 
06323+0543   J   661     Aka J  1957.                                                            J__1953b
06324+1627   BPM 283     [PM2000]  508893 + [PM2000]  508685.                                    Gvr2010 
06324+1312   AG  326     1894: No companion seen. 1903: Probably double but too close to                 
                         measure. Heintz finds a faint companion at 4@, 12th mag., which does    Hei1967b
                         not fit the AG description.                                                     
06324+0110   J  2022     RST 5235. BAL 1316. J 1955 has been abandoned.                                  
06325+3227   RAO 500     WW Aur.                                                                         
06325+1720   VAS   8     VSK   2.                                                                        
06325+1539   BPMA 27     [PM2000]  509309 + [PM2000]  510100.                                    Gvr2010 
06325-1946   B  1959     CPD-19@1324.                                                                    
06327+2053   HJ 2320     H N 141.                                                                MEv2010 
06327+1716   VAS   9     VSK   3.                                                                        
06328-1110   CHR 129     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         McClure (1983).                                                         Mcr1983 
06330+0851   SLE 534     The close pair 06328+0851 J  2745 was found to be part of this system,          
                         sharing a primary. It was moved to this more-correct WDS designation            
                         as the AD pair.                                                                 
06332+2517   HJ  392     B is BD+25@1318.                                                                
06332+1719   ARN 103     H 5  71.                                                                MEv2010 
06332+0528   SLE 299     Pair bound. Primary is planet host star. Colors of B component                  
                         consistent with late-K / early-M, mass 0.58 +/- 0.02 Msun               Egn2007 
06332-0724   BRT 379     J 1462.                                                                         
06333+2342   POU1427     GCB 72.                                                                         
06333+1226   GCB  70     J  2023.                                                                Nsn2016 
06333-1213   ALD  30     BRT 2652.                                                                       
06335+4822   UC 1450     AB: CPM candidate does not pass photometry test; likely optical.        Tok2013c
                         AB: A is SB1, P=490.5d. UC_1450 colors do not match.                    Tok2014d
             RAO  80     Another triple where the inner SB with a period of 1.3 yr (D. Latham            
                         2012, private communication) has a tertiary companion discovered with           
                         Robo-AO and seen in an archival 2MASS image. This component is located          
                         above the MS, but its photometry has large errors. Its status remains           
                         indeterminate because the PM(A) is only 0".053/y and we do not have a           
                         sufficiently long time base. A wider pair (AB = UC 1450 at 53") was             
                         identified as a common PM pair (Hartkopf et al. 2013), however, the     UC_2013b
                         colors we find here implies it is optical. Crowding is moderate.                
                         Possibly the preferred motion of background stars accidentally matches          
                         the slow PM of A.                                                       Rbr2015d
06335+2444   POU1431     Aka POU1449.                                                                    
06335+1658   VAS  10     VSK   4.                                                                        
06336-1207   HU   43     Position and BD number corrected by Heintz.                             Hei1987a
06337+1534   BPM 284     [PM2000]  514202 + [PM2000]  513791.                                    Gvr2010 
06341+2207   S   524     AB: B is BD+22@1384.                                                            
                         AB: HJL  78.                                                            HJL1986 
                         AB: SHY 499. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AB: H 5 112.                                                            MEv2010 
06342+2133   J  1094     TDS3932.                                                                        
06343+3805   STT 147     B is BD+38@1524.                                                                
06343-1229   GAL 407     Object #246 in Gallo's original list.                                   Gal1914 
06344+1445   STF 932     A premature orbit has been computed.                                            
06345+5521   BQ Lyn      Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Griffin (2002).                                                         Grf2002c
06345+0420   BAL2672     The measure of Couteau probably has the quadrant reversed. It was       Cou1963a
                         entered as a new pair at Lick.                                          IDS1963A
                         Rectilinear solution by Hartkopf & Mason (2015).                        WSI2015 
06345-1115   HO  235     BRT3196.                                                                Brt1951 
06346+0821   SLE 538     AC: There is apparently a ~20" error in the declination of the C                
                         component in the Soulie (1986) measure.                                 Sle1986b
                         AD appears to be a measure of AB, with a ~40" error in the                      
                         declination of the secondary by Soulie.                                 Sle1986b
06346+0413   LEN   1     AB: [LHR84] RAFGL 961 W/E. Luminous YSO in SW rim of Rosette nebula.    Alv2004 
06347-0836   A   508     Primary is V730 Mon, an eccentric Algol-type eclipsing binary, with             
                         period 1.57232d.                                                        Zas2011 
06348+0819   BRT2120     Also known as J   264.                                                          
06348+0734   STF 938     14 Mon.                                                                         
06348-0610   A   507     AB,C: This connects the pair to BD-06@1616.                                     
06349+0926   SLE 539     Soulie's published coordinates appear to be in error.                   Sle1986b
06350+1520   EVS  12     Primary is the Cepheid W Gem.                                           Evs2016a
06352+0100   BAL1318     J 1961.                                                                         
06353+4746   JNN  54     2MASS J06351837+4745366 is an unconfirmed binary with regards to                
                         common proper motion. Since the brightness and color of the companion           
                         is consistent with expectation, we count it as binary in the                    
                         statistical analysis.                                                   Jnn2012 
06353-0250   BAL  64     J 2609.                                                                         
06354-0403   JNN 271     Estimated age 1000-10000 Myr; masses 0.31 +/- 0.03 and 0.14 +/- 0.01            
                         Msun; a ~2.0 au.                                                        Jnn2014 
06356+1608   BPM 285     [PM2000]  522698 + [PM2000]  523043.                                    Gvr2010 
06356-6238   FIN  74     Finsen and van den Bos both noted 4 possible components on multiple     Fin1928b
                         nights. Their note: "The existence of the components A, B, and C was    B__1928c
                         at this stage regarded as certain, while D was strongly suspected. The          
                         interpretation of the earlier measures of duplicity presents some               
                         difficulties. It is possible that the nova was simply double at that            
                         time and that the triple or quadruple chacter developed later. An               
                         alternate explanation is that the observers were able to see more               
                         detail as they grew more accustomed to the densely nebulous region."            
                         A steady increase in the AB and AC distances were noted between 1928    B__1931a
                         and 1931.                                                               Fin1931 
                         Markedly nebulous in 1932; B and C well outside it but very faint. In           
                         1933 nebulous character of A almost unnoticeable; B very faint but              
                         still measurable; C almost a glimpse objects and measures hardly                
                         better than a guess.                                                    B__1933d
                         Nova Pictoris, RR Pic. Observations of the ejecta similar to those              
                         made by Kuiper for Nova Herculis (1934).                                Kui1935b
                         Not a double star.                                                              
06357-4129   I  9001     Previously known as I  1154 1/2.                                                
06358-1212   GAL 408     Object #249 in Gallo's original list.                                   Gal1914 
06359+0519   STF 939     B is BD+05@1317. Spectrum of A: B0.5III-IV.                                     
06359-3605   SHY 185     AB: HIP  31509 + HIP  31547.                                                    
             RST4816     Ba,Bb: Hipparcos parallax 25.39 +/- 0.43 mas; dynamical parallax 25.5           
                         mas, masses 1.08 and 0.80 Msun. The new orbit with 14 yr period is              
                         radically different from the 28.5 yr orbit of Cvetkovic (2008), but     Cve2008b
                         closer to the three solutions proposed by Branham (2009). A large part  Bnh2009 
                         of the orbit remains unobserved.                                                
06360+0359   BAL2674     BAL2675. It appears that Baillaud's 1910.16 theta value of 152 deg      Bal1944 
                         was erroneous and should have been 360-152 = 208 deg.                           
06360-2237   BRT1390     CD-22@3251.                                                                     
06361+1541   BPMA 28     [PM2000]  525436 + [PM2000]  526168.                                    Gvr2010 
06361-2407   ARG  15     B is CD-24@4208.                                                                
06364+2717   STT 149     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.71 +/- 0.49, 1.96, and 1.00 Msun, respectively.             Mlk2012 
06364-1840   SHJ  73     nu 1 CMa = 6 CMa. H IV 81. Composite spectrum; G8III+F3IV-V.                    
                         B is BD-18@1478.                                                                
                         H 4  81.                                                                MEv2010 
06365+3827   BLL  17     A is the semiregular variable UU Aur.                                           
06365+0743   SHY 501     AC: HIP  31577 + HIP  30362. C component = A component of 06232+0854.           
06366+1755   BPM 288     [PM2000]  527780 + [PM2000]  527789.                                    Gvr2010 
06366+1628   BPM 286     [PM2000]  527469 + [PM2000]  527178.                                    Gvr2010 
06366+1439   BPM 287     [PM2000]  527745 + [PM2000]  527371.                                    Gvr2010 
06367-2237   H 2  60     H II 60.                                                                        
                         Primary is HD 47247, an Algol-type eclipsing binary, P = 1.98571d.      Zas2012 
06368+4108   STF 933     H N  60.                                                                MEv2010 
06368+3654   ES  177     BC: Aka ALI 332.                                                                
06370-1919   FEN   7     Neither component seen on POSS plate; may be flaws on AC Hyderabad              
                         plate.                                                                          
06371+2444   POU1650     Position corrected.                                                             
06371+2421   POU1649     Position corrected.                                                             
06371+0304   EVS   6     Classical Cepheid CV Mon.                                                       
06372+0452   BRT2121     BAL 2677.                                                                       
06374+1618   BPM 289     [PM2000]  531542 + [PM2000]  531909.                                    Gvr2010 
06374+0608   SNA   3     Aa,Ab: The primary is the spectroscopic binary V640 Mon, aka                    
                         Plaskett's star. Period ~14.4d (Linder et al. 2008, A&A 489, 713). It           
                         is the only O-type binary known with a magnetic star.                   Sna2014 
                         The classification is from Bagnuolo & Barry (1996).                     Bgn1992 
                         We took the mass ratio from Bagnuolo et al. (1992)                      Msn1998a
06375+1520   BPM 290     [PM2000]  532258 + [PM2000]  532613.                                    Gvr2010 
06375+0134   J  2610     BC: Also known as J  2746.                                                      
06375-2303   BRT1391     ARA1656.                                                                        
06376+1211   S   529     AB: B is BD+12@1221.                                                            
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
06377+6129   STT 563     AB: 8 Lyn.                                                                      
06377+1624   BUP  90     gam Gem = 24 Cen = Alhena. H V 71. Elements P, T, e, and the longitude  Bey1967 
                         of periastron are from a spectroscopic orbit. Beardsley's data are              
                         inconsistent; the values of a, i, and the node given here approximate           
                         his ABFG most closely.                                                          
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
             gam Gem     Aa,Ab: Combined astrometric/spectroscopic solution. Fekel & Tomkin      Kpr1987b
                         (1993) derive a spectroscopic period of 4614.0 +/- 0.7 days, as well    Fek1993 
                         as an approximate magnitude difference of 6.0 +/- 0.5 mag in V.                 
                         An additional spectroscopic solution by Scholz et al. (1997) yielded a  Slz1997 
                         period of 4614.51 +/- 0.47; Lehmann et al. (2002) found a similar       Leh2002 
                         period and also looked for short-period variations.                             
             OCC 9011    Aa,Ab: Drummond (2014) resolves the Aa,Ab pair, previously detected             
                         only by occultation. Setting scale of the astrometric/spectroscopic             
                         orbit, and combining with the van Leeuwen (2007) Hipparcos parallax,            
                         he derives component masses 3.4 +/- 0.8 and 1.4 +/- 0.3 Msun.           Dru2014 
                         Intensity Interferometer Limb-darkened diameter 1.39 +/- 0.09 mas.      HBr1974 
06377+0903   SLE 553     SLE 764.                                                                        
06377-4942   RST 205     Formerly at 06380-4941 with the unrelated DAM 422.                              
06378-7056   TOK 112     HIP 31692. NOMAD lists 5 components, but none fits the 2MASS PSC                
                         source at 15" which is optical anyway.                                  Tok2011a
06380-4941   DAM 422     The former AB, RST 205 is unrelated and now at 06377-4942.                      
06380-6132   I     5     AB: A = AK Pic (BY-Dra type). AB Dor moving group.                      Tok2014d
             SHY  35     AC: HIP  31711 + HIP  31878. C component = C component of 05287-6527            
                         and 06225-6013.                                                                 
                         AC: C is X-ray source.                                                  Tok2014d
                         AD: HIP  31711 + HIP  30314. D component = A component of 06225-6013.           
06381+5927   STF 923     STF 937.                                                                        
06381+2220   GIC  64     G104-050/G109-016.                                                              
                         NLTT 16769/16768                                                        Chm2004 
06381+1752   BPM 291     [PM2000]  534960 + [PM2000]  535514.                                    Gvr2010 
06383+1828   CBL 128     TOK 260.                                                                        
06383-0526   DAM1167     BRT 538.                                                                Brt1931 
06384+4848   LDS3714     G101-047. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
06384+2859   MCA  27     53 Aur. An occultation and interferometric binary.                              
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.19 +/- 1.06, 4.40, and 2.57 Msun, respectively.             Mlk2012 
06384+1730   BPMA 29     [PM2000]  536898 + [PM2000]  535918.                                    Gvr2010 
06386+4020   FRK   6     AB and AC: Rectilinear solution by Hurowitz et al. (2013).              USN2013a
06386+0137   HD  47432   The star is a member of Mon OB2, according to Hill et al. (1986 PASP            
                         98, 1186).                                                              Msn1998a
06386-4813   DUN  31     B is CD-48@2416. A is variable.                                                 
06387+4135   STF 941     AB: H 1  84.                                                            MEv2010 
06387-4504   HJ 3882     AC: Jacob also measured the distance to 06389-4503HJ 3883 (1847.10,     Jc_1849 
                         71.12 deg, 60" est. mags 8,10), but they are not physically related so          
                         are not merged.                                                                 
06388-2255   BRT1392     CD-22@3315.                                                                     
06388-4133   SWR  14     CPM pair                                                                Skf2004 
06393+4229   BUP  92     psi 3 Aur = 52 Aur                                                              
06393+4200   STT 150     Often too close to measure. Rapid binary.                                       
                         At limit of 26inch; measure uncertain.                                  Wor1967b
06393+3135   S   528     A is an Algol-type system, AK Aur.                                              
06394-1401   GAL 409     Object #252 in Gallo's original list.                                   Gal1914 
06395+2436   TOK  19     Primary is 5.7d SB2.                                                    Tok2006 
06395-3240   BRT1597     Aka JSP 112.                                                                    
06396+2816   STT 152     54 Aur. A is a spectroscopic binary.                                            
                         Primary is eclipsing binary of Algol-type, period 1.8797 d.             Zas2012 
06396-2342   FIN 321     Few measures, which leave the nature of the motion uncertain.                   
06399-4305   HRG   4     Aka SKF1935.                                                                    
06401-3919   HD  48149   The classification given in Mason et al. (1998) is from Conti &         Msn1998a
                         Alschuler (1971).                                                       Cti1971 
06402+1335   J  1365     J 1827.                                                                         
06404+1602   BPM 292     [PM2000]  546196 + [PM2000]  546701.                                    Gvr2010 
06405+1629   BPM 293     [PM2000]  547001 + [PM2000]  547404.                                    Gvr2010 
06405-0331   FAB   6     The astrometry catalogues are partly confused because the position for          
                         the star east has been linked with the star NE to produce a spurious            
                         large proper motion in Tycho-2. Curiously, AC2000 misses the star NE,           
                         which has caused the problem.                                                   
06405-3912   LDS 170     UC 1467.                                                                UC_2013b
06406+0947   STF 951     V684 Mon.                                                                       
                         The A component is an eccentric Algol-type binary, period 1.85142 day.          
                         (see 2009A&A...502..239Z). The B component is also an eclipsing                 
                         binary, period unknown.                                                 Zas2011 
06406+0217   J  1967     BAL 1704.                                                                       
06408-0040   J  2006     BAL 702.                                                                        
06409+1547   BPM 294     [PM2000]  548668 + [PM2000]  548515.                                    Gvr2010 
06409+1344   BPM 295     [PM2000]  548798 + [PM2000]  549055.                                    Gvr2010 
06410+0954   STF 950     A is an irregular variable, S Mon.                                              
                         While not as complex as STF 484/485, a similar method clarified                 
                         numerous ambiguities. CHR 168Aa,Ab; STF 950AB; AC; AD; AE; AF; AK; FG;          
                         and D    11Ea,Eb are all unchanged.                                             
                                                                                                         
                         STF 950AS   ---> STF 950AO                                                      
                         D    11Eb   ---> D    11EH                                                      
                         JRN  31Ec   ---> JRN  31EI                                                      
                         JRN  31Ed   ---> JRN  31EJ                                                      
                         STF 950FS   ---> STF 950FO                                                      
                         STF 950GS   ---> STF 950GO                                                      
                         STF 950     ---> STF 950AH (formerly STF 950A to D    11b)                      
                         STF 950     ---> STF 950AM (formerly STF 950A to STF 952A)                      
                         STF 952AB   ---> STF 952MN                                                      
                         DOB   7AC   ---> STF 950MK                                                      
                         DOB   7BC   ---> STF 950NK                                                      
                         JRN  30CD   ---> STF 950KD                                                      
                         JRN  30CE   ---> JRN  30KL                                                      
                         Note that the WDS coordinate for STF 952 (as well as other                      
                         associated pairs) has been changed to that of STF 950.                          
             CHR 168     A component is an irregular variable, S Mon. See Gies (1993) for        Gie1993 
                         classification of the speckle companion. The spectroscopic orbit and            
                         current periastron passage of Aa are discussed by Gies (1997).          Gie1997 
                         The B component was observed and appeared to be single.                         
                         Classifications of the B, C, D,and E components are from Hoffleit &     Hof1991 
                         Warren (1991), who list the E component as a close pair.                Msn1998a
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 3.58 +/- 1.59, 17.32, 38.90 Msun, respectively.    Mlk2012 
                         Distance to NGC 2264 is 719(+22-21) pc, yielding a mass sum of          MzA2019b
                         45.1(+3.6-3.3) \msun.                                                           
             STF 950     AC: H 3  46.                                                            MEv2010 
             JRN  31     AJ: Also known as SMR   9AR.                                                    
             JRN  31     AI: Also known as SMR   9AS.                                                    
             JRN  31     JI: Also known as SMR   9RS.                                                    
             JRN  30     AL: Also known as SMR   9AQ.                                                    
06410+0215   J   596     J 2007.                                                                         
06411+2348   POU1855     Algol-type eclipsing binary, period 4.88450 d.                          Zas2019 
06411+0111   HJ 2335     BAL 1323.                                                                       
06412+1601   BPM 296     [PM2000]  550102 + [PM2000]  549799.                                    Gvr2010 
06412+0928   STF 954     Spectrum of B: B9V.                                                             
                         AB: H N 103.                                                            MEv2010 
             HER  15     GH: Primary of 06411+0928 found to be G component of 06412+0928;                
                         systems merged.  Additional notes may be found in Herbig (1962).        Her1962 
06412+0926   HER  16     Additional notes may be found in Herbig (1962).                         Her1962 
06412+0859   STF 953     H 3 114.                                                                MEv2010 
06412-0759   PRT9001     Previously known as PRT   1.                                                    
06413+2812   HJ  397     25 Gem.                                                                         
06414+2336   POU1883     This is the same as FOX  11.                                                    
06414+0944   STF3117     Primary is an EA type eclipsing binary, period unknown (see                     
                         2009A&A...502..239Z).                                                   Zas2011 
06415+2436   POU1891     Also known as J  1968.                                                          
06415+0950   STF3118     BDS 3565 probably same star.                                                    
06416+3556   HR 2452     Orbit determined by fitting revised Hipparcos intermediate astrometric          
                         data. Derived component masses 1.28 +/- 0.06 and 1.21 +/- 0.04 Msun.    Ren2010 
06416+1010   CHN  23     Additional notes may be found in Herbig (1962).                         Her1962 
06417+1145   BPM 297     [PM2000]  552581 + [PM2000]  552969.                                    Gvr2010 
06418+3041   A   218     Three possible orbit solutions by Heintz (1997).                        Hei1997 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.63 +/- 3.16, 2.46, and 1.20 Msun, respectively.             Mlk2012 
06419+1558   BPM 298     [PM2000]  553280 + [PM2000]  553142.                                    Gvr2010 
06421+0315   HO  237     Hough notes an additional companion S 13' and following 1m 3s           Ho_1890 
                         (corresponding to theta=130deg, rho=20.4'). This companion is the 6th           
                         magnitude star HD 48348.                                                        
06422+1557   BPM 299     [PM2000]  554962 + [PM2000]  555283.                                    Gvr2010 
06422+1552   BPM 300     [PM2000]  555301 + [PM2000]  555715.                                    Gvr2010 
06422-0035   BAL 708     Aka BAL 710.                                                                    
06423+1444   BPM 301     [PM2000]  555522 + [PM2000]  555397.                                    Gvr2010 
06423+1140   BPM 302     [PM2000]  555934 + [PM2000]  556124.                                    Gvr2010 
06423+0334   GIC  65     G108-021/G108-022 = GJ 3404A+3405B.                                             
06423-0048   J  2024     BAL 707. GAU.                                                                   
06423-2250   BRT1393     CD-22@3396. TDS4047.                                                            
06424+1739   26 Gem      Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
06425+6612   MLR 318     A premature orbit has been calculated.                                          
                         omega corrected from 309.0 to 129.0 by Ruymaekers & Nys (1995)          Ruy1995 
06425+3902   ES 2097     The real ES 2097 is actually the known pair 06437+3911BRT2216.          Dam2015c
06425+2320   FOX 149     Aka POU1924 and POU1931.                                                        
06425-2044   HDO  85     HDO  84                                                                         
06426+6102   LDS2522     LDS5194.                                                                        
06426+3955   HDS 930     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.22 +/- 0.40, 1.79, and 1.05 Msun, respectively.             Mlk2012 
06426+1651   BPMA 30     [PM2000]  557570 + [PM2000]  557964.                                    Gvr2010 
06426-0934   GAL 410     Object #254 in Gallo's original list.                                   Gal1914 
06426-1046   GAL 411     Object #255 in Gallo's original list.                                   Gal1914 
06427-1257   GAL 412     Object #256 in Gallo's original list.                                   Gal1914 
06427-2155   B  2121     CPD-21@1431.                                                                    
06428+1458   BPM 304     [PM2000]  558619 + [PM2000]  558635.                                    Gvr2010 
06428+0953   BPM 303     [PM2000]  558110 + [PM2000]  558560.                                    Gvr2010 
06428-4051   I  9002     Previously known as I  1156 1/2.                                                
06428-5027   HJ 3889     B is CD-50@2356.                                                                
06429+1634   BPM 305     [PM2000]  558826 + [PM2000]  559260.                                    Gvr2010 
06429-5507   I   480     Aka R    68.                                                                    
06431+1618   BPM 306     [PM2000]  560000 + [PM2000]  559460.                                    Gvr2010 
06435+0341   BAL2187     First valid measure is by Heintz. The measure by Baillaud may actually  Dam2016d
                         be 06321+0300BAL2176.                                                           
06437+3911   BRT2216     ALI 1078.                                                                       
                         Aka ES 2097.                                                            Dam2015c
06438+0034   J  1970     BAL 1022.                                                                       
06439+2512   BRT3277     Originally published as BRT 143.                                        Brt1928 
06439+2508   S   533     eps Gem = 27 Gem = Mebsuta. B is BD+25@1407.                                    
                         H 6  73.                                                                MEv2010 
06439-5434   HDS 934     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.33 +/- 0.86, 1.82, and 0.85 Msun, respectively.             Mlk2012 
06439-5435   WFC  41     SWR  15. CPM pair                                                       Skf2004 
06440+1314   LAM   3     30 Gem.                                                                         
06440+0729   J   666     There is a 14th magnitude star 8" np C.                                         
06440-0941   GAL 413     Object #257 in Gallo's original list.                                   Gal1914 
06441+0007   J  1972     BAL 1024.                                                                       
06442+0057   BAL1332     A likely plate flaw.                                                    Grv2021a
06442-5442   DUN  34     B is CPD-54@1096.                                                               
06443+4037   STT 154     B is BD+40@1697.                                                                
06443-0124   BAL 334     Algol-type eclipsing binary, period 1.28758 d.                          Zas2019 
06445-3104   HDO 197     10 CMa. A is the variable FT CMa.                                               
06446-1516   GAL 414     Object #259 in Gallo's original list.                                   Gal1914 
06447-0002   BAL1027     BAL 1029.                                                                       
06448+3249   LDS5681     NLTT 16919/16918                                                        Chm2004 
06448+1215   BPM 307     [PM2000]  569455 + [PM2000]  568924.                                    Gvr2010 
06448+1012   BPM 308     [PM2000]  569484 + [PM2000]  568894.                                    Gvr2010 
06448+0241   BAL1712     J 2752.                                                                         
06448+0019   GAU4234     BAL 1030.                                                                       
06449-0027   BAL 717     No star at primary location - plate flaw or typo in AC catalog.                 
06450+1543   BPM 310     [PM2000]  570597 + [PM2000]  570506.                                    Gvr2010 
06450+1211   BPM 309     [PM2000]  570370 + [PM2000]  570701.                                    Gvr2010 
06450+1107   BPM 312     [PM2000]  570896 + [PM2000]  571332.                                    Gvr2010 
06450+1045   A  2825     Rectilinear solution by Rica & Zirm (2012).                             FMR2012i
06450+1043   BPM 311     [PM2000]  570788 + [PM2000]  571133.                                    Gvr2010 
06450+0243   BAL1714     Appears to be the lost AG  120 with a 1d error in declination.          Dam2013 
06451-1643   AGC   1     AB: Sirius = alp CMa = 9 CMa.                                                   
                         Bessel, in 1834, notes that the proper motion was variable and, in his          
                         letter to Humboldt, stated that "..Procyon and Sirius are genuine               
                         binary systems, each consisting of a visible and an invisible star."            
                         Not quite invisible, this large dm pair consisting of a main sequence           
                         A star and a white dwarf was first resolved by Alvan G. Clark on 31             
                         January 1862 in the process of of testing the 18.5" refractor. See              
                         notes by Burnham and Aitken.                                            Bu_1906 
                         The separation for the 1862.275 measurement by Lassell is reported as   Lsl1862 
                         4.92". This is clearly incorrect and not consistent with measurements           
                         by other observers. WDS catalogers assume an factor of 2 error and              
                         correct separation to 9.84".                                                    
                         Otto Struve lists a measurement of Sirius in 1861.21. However, this     Stt1893a
                         predates the discovery of the companion Sirius B by A. Clark and his            
                         son on 1962 Jan 31 and the first formal measurement by G. P. Bond on            
                         1862 February 7. Comparing the uncorrected PA and separation in                 
                         Struve's table in 1893 with the measurements published by Struve, we    Stt1864 
                         suspect that 1861.21 is a typo and should refer to the observation on           
                         1863-Mar-16.                                                                    
                         Companion almost hidden behind secondary mirror diffraction ray from            
                         Sirius B was never observed at these position angles until the early    Sea1882 
                         20th century. We suspect that this is a clerical error and that the             
                         measurements pertain to another system.                                         
                         For the 1882.988 measurement the PA is listed as 41.6 deg and is        Bu_1883 
                         40.6 in another.                                                        Bu_1883b
                         Many of the recovery observations of Sirius B following the periastron          
                         passage after 1890 are doubtful. The recovery observations made by      See1896d
                         See, Douglass, and Cogshall at Lowell Observatory from 1896.668 to      Dgl1896 
                         1896.695 were taken in the morning shortly before sunrise when Sirius   Cog1896a
                         was low in the sky. See notes that the mean position angle of 220 deg           
                         at 5.10" is about 30 deg behind its predicted location and the sep              
                         sep is larger than expected based on previous orbit fit. Aitken and     A__1896d
                         Schaeberle reported measurements between 1896.814-1897.027 made from    Shb1897a
                         Lick Observatory at a significantly different mean position angle of            
                         189 deg and 3.7". Both Aitken and Schaeberle comment that neither of            
                         them saw a star at the position reported by Dr. See. Following the              
                         contradictory reports, Stimson J. Brown  published observations from    Brs1896 
                         his logbook that were taken earlier in March 1896 at the USNO. The              
                         position angle is similar to the values reported by Aitken, but the             
                         separation is about 1" larger. Brown notes that the observations were           
                         taken under challenging conditions and he did not have much confidence          
                         in their reliability. See later refuted his earlier measurements        See1897e
                         after unsuccessfully searching for the companion while observing from           
                         Mexico and then successfully detecting the companion at a pa of 175 deg         
                         and 4.6" in September 1897 at Lowell. He writes, "The erroneous                 
                         conclusion to which I was led last year seems to have arisen from a             
                         very unusual and entirely unexpected cause, of which we need not                
                         speak here..."  In hindsight, See also reported in that publication,            
                         two observations from April 1895 that he initially did not think were           
                         worthy of announcing. The difficulty in attempting to find Sirius B             
                         using the Lick Observatory 36 inch in February and March of 1896 was            
                         described by William J. Hussey.                                         Hu_1896 
                         See1900d and Brs1900b measures : "All of the observations have been     See1900d
                         thoroughly checked.  A number of errors were discovered in the earlier  Brs1900b
                         reductions and corrected.  These reductions have also been slighty      See1911 
                         changed by the adoption of a later and better determined value of a     Brs1911a
                         revolution of the micrometer screw.  This will account for small                
                         discrepanacies between the results published here and those previously          
                         published in the astronomical periodicals."                                     
                         For the 1904.186 measuremment by T. Lewis, the title of the article,    L__1904 
                         text, and first page of the data table all refer to observations taken          
                         in 1904. Subsequent pages of the data table (including the page that            
                         Sirius is listed on) list an epoch of 1903. However, this is probably a         
                         typo, so date corrected the date to be in 1904.                                 
                         Sirius A.                                                               B__1959a
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Gatewood & Gatewood (1978).                                             Gat1978 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.08 +/- 0.42, 2.46, and 2.19 Msun, respectively.  Mlk2012 
                         BC: Suspected by Fox in 1920, also reported by Innes, van den Bos, and  A__1932a
                         Finsen. Other observers fail to confirm duplicity of B. Single 1945,    B__1929a
                         1946, 1949, 1950. Recovered by Popovic in 1975 at approximately the     Fin1929a
                         the same position as the 1929 resolutions. If these are periodic, the   Pop1977b
                         next approximate time for resolution is 2020. Therefore, since we               
                         believe the detections of C to be real, but likely of a background              
                         optical interloper,  BC carries a "U" code and not an "X" code.                 
                         However, very compelling argument that this is a chance allignment of   Lec2000 
                         a non-physical background star appearing close to Sirius AB is the              
                         1920-30 time period is now assumed.                                             
                         Time displacement residuals over a period of 6.8y are linear ruling     Ldb1973 
                         out a 6.4y perturbation with an amplitude of 0.14". There is no                 
                         evidence of a close companion with this nature associated with Sirius.          
                         Otto Struve corrected his measurements for systematic errors by         Stt1893a
                         measuring artificial double stars. He provided both the original and            
                         corrected measures of the separation and position angle for the                 
                         companion of Sirius. Aitken cautions that the variance of the angles    A__1935f
                         and distances compared with other observers is often larger for                 
                         Struve's corrected values. However in the case of Struve's measurements         
                         of the companion of Sirius, Bond et al. mean residuals in the position  BdH2017 
                         angle improved when using the corrected values, while the residuals in          
                         separation did not change significantly, so the corrected values are            
                         reported here.                                                                  
                         For the photographic observations by Lindenblad, tables are given for   Ldb1970 
                         the raw individual measures, while only the mean measures are corrected Ldb1973 
                         for emulsion contraction. The average time span covered by these mean           
                         measures is ~ 70 nights, so we used Lindenblad's tabulated scale        BdH2017 
                         corrections to compute corrected separations and position angles for            
                         the individual measurements. We then took the mean for plates taken on          
                         the same night, reducing the number of individual measurements from 157         
                         down to 77 measurements on unique dates.                                        
                         X coded van Albada (1962) measures corrected for emulsion contraction.  vAb1971 
                         Jasinta & Hidayat (1999) did not correct these epochs for emulsion      Jas1999b
                         contraction.                                                                    
                         Measure of Anton corrected in a later publication.                      Ant2010 
                                                                                                 Ant2012 
                         Schroeder measure re-reducted and corrected in Bond Table 2.            Shd2000 
                                                                                                 BdH2017 
                         Sirius A mass is 2.063+/-0.023 \msun with an age of 242+/-5 Myr,        BdH2017 
                         a radius of 1.7144+/-0.0090 \rsun, luminosity of 24.74+/-0.70 \lsun,            
                         and Teff of 9845+/-64 K. Sirius B mass is 1.018+/-0.011 \msun,                  
                         an age of 224(+34-19) Myr, a radius of 0.008098+/-0.000046 \rsun,               
                         luminosity of  0.02448+/-0.00033 \lsun and Teff of 25,369+/-46 K.               
                         Intensity Interferometer Limb-darkened diameter 5.89 +/- 0.16 mas.      HBr1974 
                         Mk III Limb-darkened diameter  5.993 +/- 0.108 mas.                     MkT2003 
                         AD: Rectilinear solution by Mason & Hartkopf (2015).                    Msn2015a
             HL    3     AE: Rectilinear solution by Mason & Hartkopf (2015).                    Msn2015a
             BU 1411     AF: Rectilinear solution by Mason & Hartkopf (2015).                    Msn2015a
06451-2047   HDO  87     ARA 870.                                                                        
06452-3512   RST5247     Spectrum: A2/3(m)F0-F2/3.                                                       
06454-3148   EHR   9     All three components appear to be comoving.                             Ehr2010 
06455+1618   BPM 313     [PM2000]  573589 + [PM2000]  572969.                                    Gvr2010 
06455+0424   J  2434     BAL 2700.                                                                       
06455-3057   HJ 3891     This is the variable HP CMa.                                                    
06456+5420   A  1735     Rapid retrograde motion, but few measures.                                      
06456+1332   BPM 314     [PM2000]  574252 + [PM2000]  574343.                                    Gvr2010 
06456-0521   BRT 383     J  3337.                                                                Nsn2016 
06457-2041   HJ 2341     B is BD-20@1548.                                                                
06458+0230   V505 Mon    Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Mayer et al. (2001).                                                    MyP1997 
06458-0225   BAL  75     J 1476.                                                                         
06460+1551   BPM 315     [PM2000]  576489 + [PM2000]  575939.                                    Gvr2010 
06461+3233   LDS6201     HIP 32423. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 16948/16950                                                        Chm2004 
06461+1344   BPM 316     [PM2000]  576771 + [PM2000]  577056.                                    Gvr2010 
06461-0233   BAL  77     J 1477.                                                                         
06462+7934   LOU   1     CPM pair, discovered using data from 2MASS and WISE. Loutrel et al.             
                         (2011) determine a spectral type for the secondary of L9 +/- 1, with            
                         Teff 1360 +50/-80K and mass 0.064 +0.008/-0.019 Msun.                   Lou2011 
06462+5927   STF 948     12 Lyn. A premature orbit has been computed.                                    
                         AB: H 1   6.  AC: H 3  22.                                              MEv2010 
06462+1438   BPM 317     [PM2000]  577722 + [PM2000]  577795.                                    Gvr2010 
06462+1259   J  2592     Same measure was published as J 2594.                                           
06462+0256   BAL2193     2013 measure seems to be of 06463+0311BAL2194.                          Smh2016 
                                                                                                 Dam2016d
06463+0811   J   268     J 2026.                                                                         
06465+3611   HJ 3284     Aka ALI 338.                                                                    
06465+1359   BPM 318     [PM2000]  579367 + [PM2000]  579861.                                    Gvr2010 
06466+1550   BPM 319     [PM2000]  579684 + [PM2000]  579507.                                    Gvr2010 
06466-0231   BAL  78     J 1478.                                                                         
06467+4335   SHJ  75     56 Aur = psi 5 Aur. STTA 78 = H 5 107. B is BD+43@1596.                         
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
06467+1407   BPM 320     [PM2000]  580730 + [PM2000]  581270.                                    Gvr2010 
06468+1300   J  2593     See JO 27, page 5. 1914.09, 150@, 2.5", 9.5-9.7.                                
                         Probably J  2437.                                                       Nsn2016 
06471+1526   BPM 321     [PM2000]  582804 + [PM2000]  583521.                                    Gvr2010 
06473+1027   BPM 322     [PM2000]  583917 + [PM2000]  583681.                                    Gvr2010 
06474+1812   STT 156     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 8.51 +/- 3.94, 5.18, and 2.09 Msun, respectively.             Mlk2012 
06475-2834   RSS   6     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
06475-7651   HJ 3911     B is CPD-76@423.                                                                
06477+1347   BPM 323     [PM2000]  586279 + [PM2000]  585801.                                    Gvr2010 
06477+0827   J  2438     also known as HEI 707.                                                          
06478+1534   BPM 324     [PM2000]  586890 + [PM2000]  587433.                                    Gvr2010 
06478+0020   STT 157     Quadrant noted as definite on first and last night. Yet no change can           
                         have taken place since Rabe's and Baize's measures in 1938 and 1942.    VBs1954 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 14.45 +/- 8.14, 4.44, and 2.09 Msun, respectively.            Mlk2012 
06478-1143   STF 970     B is BD-11@1637.                                                                
06478-2210   HDO  90     Listed as a new double in 1881.20, but no measurement given.            HdO1882a
06479+0225   18 Mon      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin (1984).                                                         Grf1984d
06480-0045   GAU4355     BAL 723.                                                                        
06481-0948   A  1056     A premature orbit has been computed.                                            
06482+5542   STF 958     A has variable proper motion. B is a spectroscopic binary.                      
                         AB: H 2  72.                                                            MEv2010 
06482+1407   BPM 325     [PM2000]  589478 + [PM2000]  589667.                                    Gvr2010 
06482+0927   J  2435     Aka CMR   1.                                                                    
06483+4105   H 2  71     Aka H 2  71 or H II 71. STF 961 rej. Durchmusterung number quoted by    Bu_1906 
                         Burnham (BD+41 1532) was incorrect, resulting in incorrect WDS                  
                         coordinates.                                                                    
06483+1408   BPM 327     [PM2000]  590067 + [PM2000]  590021.                                    Gvr2010 
06483+1154   BPM 326     [PM2000]  589702 + [PM2000]  589729.                                    Gvr2010 
06483-1520   STF 972     BC: Probable rapid motion, but few measures.                                    
                         A,BC: Additional notes may be found in van den Bos (1963).              B__1963b
06484+1600   BPM 328     [PM2000]  590406 + [PM2000]  589973.                                    Gvr2010 
06485+1010   ARG  64     B is BD+10@1277.                                                                
06485-0018   GAU4375     BAL 725. J 2439.                                                                
06487+0737   A  2731     HIP 32650. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         AB: Prieur et al. (2012) derive a dynamical parallax of 17.1 mas and            
                         (using their orbital elements and the revised Hipparcos parallax of             
                         van Leeuwen 2007 A&A 474, 653) a total mass 1.5 +/- 1.6 Msun.           Pru2012 
             LDS5686     age, galactic orbital parameters, etc.                                          
06489+1720   BPM 329     [PM2000]  593319 + [PM2000]  592831.                                    Gvr2010 
06490+1103   BPM 330     [PM2000]  594109 + [PM2000]  594430.                                    Gvr2010 
06490-1509   AC    4     A is a spectroscopic binary.                                                    
06493-0216   FIN 322     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.91 +/- 2.98, 4.84, and 3.31 Msun, respectively.             Mlk2012 
06494+3209   GIC  67     G103-063/G103-064.                                                              
                         NLTT 17022/17023                                                        Chm2004 
06494-0840   A  1058     Aa,Ab: TDS4173. Originally listed as AB pair. Wider pairs had been              
                         erroneously combined and called AB,C; these have been separated.                
06496+5302   STF 960     HJL  79.                                                                HJL1986 
06496+3508   KIR   2     BC: Using data from 2MASS and IRTF. Kirkpatrick et al. (2001) derive    Kir2001b
                         spectral types K5V and M4V, conclude is probably a physical pair with           
                         separation 200 au.                                                              
06497-7433   TOK 389     HIP 32735 has an acceleration detected in HIP2, but no RV data. The             
                         resolved 0".3 pair implies a period of ~80yr. The spectral type K0IV            
                         given in SIMBAD may be inaccurate because the luminosity and color of           
                         the components correspond to main sequence stars with masses of 1.0             
                         and 0.6 Msun.                                                           Tok2015c
06498+1612   J  2028     33 Gem. This is the variable OV Gem.                                            
06499-1651   GAL 415     Object #268 in Gallo's original list.                                   Gal1914 
06499-2806   HDS 947     AB and AC: The 0".2 pair HDS 947 had not been observed since its                
                         discovery by Hipparcos. Here it is revealed as a triple system with             
                         comparable separations between components.                              Tok2015c
06499-5037   tau Pup     Hipparcos astrometric solution adopts some elements from the orbits of  HIP1997d
                         Schroeder & Huensch (1992) and                                          SKP1992 
                         Wilson & Huffer (1918).                                                 WRE1918 
06499-5337   V415 Car    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Jones (1928).                                                           Jon1928a
06500-4527   I   159     Variable.                                                                       
06503+2409   COU 768     1984.9999: The published McAlister et al. (1987) measure contained a    McA1987b
                         10-degree typographical error in theta.                                         
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.23 +/- 1.26, 2.49, and 1.20 Msun, respectively.             Mlk2012 
06503-0134   J  1366     BAL 347.                                                                        
06504-3142   H 5 108     H V 108. B has variable radial velocity.                                        
06505-1215   LDS6202     NLTT 17071/17070                                                        Chm2004 
06506+1242   BPMA 31     [PM2000]  603764 + [PM2000]  602411.                                    Gvr2010 
06506-0134   J  1367     BAL 348.                                                                        
06507+2122   CHB   1     Aka AF Gem.                                                                     
06508+4147   ENG  27     58 Aur = psi 7 Aur                                                              
06508+2927   HDS 949     QW Gem. Primary is eclipsing binary of W UMa type, period 0.35812d.     Zas2014 
06510-5614   HJ 3898     B is CPD-56@1180.                                                               
06514+1840   STF 976     B is BD+18@1372.                                                                
06515+5412   A  1573     Apparently in rapid motion.                                                     
06515+1630   BPM 331     [PM2000]  608920 + [PM2000]  608973.                                    Gvr2010 
06515+0512   J  2011     Variable CG Mon. Red star.                                              J__1962a
06516+2320   J   911     POU2069.                                                                        
06516+2146   BU 1193     36 Gem.                                                                         
06516-0121   BAL 349     Classical Cepheid SZ Mon.                                                       
06516-0658   BNS   3     V743 Mon = MWC 158                                                              
06516-1445   BRT 566     Initially incorrectly designated BRT 556 in WDS.                                
06516-7708   HJ 3926     B is CPD-76@426.                                                                
06517-4418   LDS 173     B is CD-44@2973.                                                                
06518+1349   BPM 332     [PM2000]  610994 + [PM2000]  610760.                                    Gvr2010 
06520+0313   BWL  22     AF and AG: Colors and/or astrometry are inconsistent with a late-type           
                         common proper motion companion based on visual inspection of the field          
                         from 2MASS, SDSS, DSS1, and/or DSS2. Primary is G 108-36.               Bwl2015 
06521+0026   TDS 294     WDS designation changed from 06522+0024 to match designation for                
                         earlier-discovered BAL1050.                                                     
06522-1448   BRT1854     A likely plate flaw.                                                    Grv2021b
06522-5631   GLI  50     B is CPD-56@1185. B is a Beta Lyrae-type system.                                
06523+1136   BPM 333     [PM2000]  613691 + [PM2000]  613573.                                    Gvr2010 
06526+0227   J  1975     BAL 1734.                                                                       
06527+7812   LDS1639     NLTT 16995/16998                                                        Chm2004 
06528+3358   FOX 150     the Gem = 34 Gem. A is a spectroscopic binary.                                  
06529+1420   BPM 334     [PM2000]  617193 + [PM2000]  617491.                                    Gvr2010 
06530+3852   STF 974     59 Aur. A is a Delta Scuti-type variable, OX Aur.                               
                         AB: H 4 102.                                                            MEv2010 
06530+1441   J  2444     J  2442.                                                                Hei1985a
06530-2657   SEE  71     A is variable.                                                                  
06531+5927   STF 963     14 Lyn. AB: Malkov et al. (2012) derive dynamical, photometric, and             
                         spectroscopic masses 7.70 +/- 3.90, 4.86, and 4.43 Msun, respectively.  Mlk2012 
06532+3826   COU1877     60 Aur.                                                                         
06532-0013   J  1057     1896 measures of 2 additional companions are given in                   Bal1944 
                         Ann. de l'Observatoire de Besancon Vol. III.                                    
06533-3147   BRT1599     A likely plate flaw.                                                    Grv2021b
06534+0132   BAL1355     J 2760.                                                                         
06534-5708   SWR  17     CPM pair                                                                Skf2004 
06535+5139   ES 2620     B is BD+51@1248.                                                                
06535+3951   A  3039     Not seen since discovery, possibly due to an incorrect right ascension          
06536-2049   BRT 306     CPD-20@1733.                                                                    
06537+2333   DOO  37     This star is not HJ 401. See HJ 401 at 06540+2319 (Doolittle).          Doo1915b
06537+1412   BPM 335     [PM2000]  622295 + [PM2000]  622273.                                    Gvr2010 
06537-0232   BAL  90     BAL  89.                                                                        
06537-1051   J  2447     RST3473.                                                                        
06538-1401   GAL 416     Object #272 in Gallo's original list.                                   Gal1914 
06539+0144   J   354     BAL1356.                                                                        
06539-0424   STF 985     B is BD-04@1713.                                                                
06540+2319   HJ  401     See star at 06537+2333, BD+23@1527. Doolittle identifies both stars.    Doo1915b
06540-1002   STF 988     B is BD-09@1714.                                                                
06541+6052   HEI 334     L1815-5 aka G250-029. Long-period astrometric binary now resolved. Very         
                         sparse visual data. Fixed e, i, omega, Omega from Heintz (1990). Needs  Hei1990c
                         combined astrometric/visual/Hipparcos solution.                                 
                         Malkov et al. (2012) derive dynamical and photometric masses of                 
                         0.51 +/- 0.28 and 0.65 Msun, respectively.                              Mlk2012 
06541+0641   STTA 79     B is BD+06@1428.                                                                
                         Pair appears in an appendix list, not part of the discoverer's regular          
                         numbering sequence.                                                             
06541-1208   GAL 417     Object #273 in Gallo's original list.                                   Gal1914 
06542+6650   MLB1068     A faint star almost exactly between A and B.                                    
06543+1238   BPM 336     [PM2000]  625524 + [PM2000]  625517.                                    Gvr2010 
06544-0139   FIL  16     BAL 356.                                                                        
06545-2734   B   706     Parabolic orbit by Newburg (1966).                                      Nbg1966e
                         sigma = areal constant in the true orbit = 0.00318 arcsec^2/yr                  
                         q = periastron distance in the true orbit = 0".1522                             
06546+1311   STF 982     38 Gem = e Gem. A is a Delta Scuti-type variable. A premature orbit             
                         has been computed for AB.                                                       
                         Omega and omega in Hopmann's (1974) orbit have been flipped in orbit    Hop1974 
                         catalog to better match observations.                                           
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: H 3  47.                                                            MEv2010 
06546+0114   J  1976     BAL 1359.                                                                       
06548-7417   HJ 3927     B is CPD-74@423.                                                                
06550+1608   BPM 337     [PM2000]  629899 + [PM2000]  629855.                                    Gvr2010 
06550-0147   BAL 359     Secondary appears to be either a plate flaw or typo in the AC catalog.          
06550-2024   H 5  65     H V 65. 17 CMa. B is BD-20@1625.                                                
06551+3208   BUP  94     Nova Gem. No. 2, DN Gem.                                                        
06551+1350   BPM 338     [PM2000]  630584 + [PM2000]  630414.                                    Gvr2010 
06552+0816   J  2034     Identification uncertain; may be same star as J 274.                            
06552+0056   J  2448     BAL 1361.                                                                       
06553+3146   A   220     TDS 4292.                                                                       
06553+0816   J   274     J 2033.                                                                         
06554+3511   BRT3246     ALI 99.                                                                         
06554-1217   GAL 274     06564-1218OL  116 (incorrectly precessed from Olivier's 1920            Ol_1927 
                         coordinates)                                                                    
06555+3204   COU2705     or may be BD+24 1417 at 06503+2409.                                     Cou1979b
06555+3010   STF 981     Hopmann orbit rejected from Fourth Orbit Catalog                        Hop1971 
                         ("period over 4000 years")                                              Wor1983 
06555-0051   GAU4762     BAL 740.                                                                        
06556+3510   HJ  407     Aka HU  833.                                                                    
06556+0624   J  2001     Variable CL Mon. Red star.                                              J__1962a
06556-0929   STF 992     V880 Mon, W Uma (EW) type eclipsing binary, P = 0.372457 d.             Zas2011 
                         CPM.                                                                    B__1963b
06556-1013   GAL 275     Primary is V879 Mon, Algol-type eclipsing binary, period 2.18691d.      Zas2013 
06556-2008   H N 123     pi CMa = 19 CMa. Possibly variable.                                             
06558-1152   STF 993     B is BD-11@1695.                                                                
06559+3644   ES  174     BRT2589.                                                                Brt1942 
06559+0612   BRT2126     J 3247.                                                                         
06559-3147   JSP 125     A is a spectroscopic binary.                                                    
06560-5536   HJ 3906     AB,C = SWR  19. CPM pair                                                Skf2004 
06561-1403   STF 997     mu CMa = 18 CMa                                                                 
06562+4032   RBR  28     Primary has a slow PM of 0".037/y. The Riddle et al. (2015) companion   RAO2015 
                         at 5".6 is located below the MS and could be optical, despite moderate          
                         crowding. We discovered another similarly faint star at 1".9 which was          
                         not spotted in the Robo-AO i'-band image. Little can be said about its          
                         status. The main target itself is a close spectroscopic binary (D.              
                         Latham 2012, private communication) and an X-ray source.                Rbr2015d
06563-0115   HJ  745     BAL 363.                                                                        
06564-3035   TDS4308     SWR  18. CPM pair                                                       Skf2004 
06565+4004   KUI  27     AB: NLTT 17176/17175                                                    Chm2004 
             SIN  24     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
06565+0628   J    41     BRT2127.                                                                Brt1938 
                         On the second night B was noted to be brighter than A, for the first            
                         time in 46 years of observations. Companion was always one magnitude            
                         fainter.                                                                J__1955 
06566+4632   STF 979     Primary is V462 Aur, a Beta Lyr type eclipsing binary, P = 1.75680d.    Zas2012 
06566+1113   BPM 339     [PM2000]  638741 + [PM2000]  639261.                                    Gvr2010 
06566-2239   S   541     B is BD-22@1610.                                                                
06567+1008   BPM 340     [PM2000]  639606 + [PM2000]  639278.                                    Gvr2010 
06567+0317   BAL2216     J 1978.                                                                         
06567+0315   J  1978     BAL 2216.                                                                       
06567-0901   XMI  31     STF 999.                                                                        
06567-6041   RED  21     M3.5 star is ~14" from K dwarf LTT 2697 = HIP 33392 = 2MASS                     
                         J06564360-6041128. Comparison of Digitized Sky Survey UKST and 2MASS            
                         images suggest similar proper motions. Proper motion for LTT 2697 =             
                         +002-274, for companion +214-228 (but may be affected by proximity to           
                         brighter star). Spectroscopic distance ~58pc.                           Red2007a
06569+0413   BAL2715     J 1980.                                                                         
06570+2457   STF 991     CD : Also known as POU2154.                                                     
06571-7202   HJ 3929     Aka LDS6203.                                                                    
06572-3030   TOB   3     SWR  20.                                                                Skf2004 
06573+5825   STT 159     15 Lyn. G5III-IV spectrum. Period poorly determined from old vis obs.           
                         Spectral types and masses of components assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
                         AB: Malkov et al. (2012) derive dynamical and spectroscopic masses              
                         4.01 +/- 2.17 and 3.73 Msun, respectively.                              Mlk2012 
06573-3530   I    65     1997.1172: Despite nearly a century of visual observations and a grade          
                         1 orbit in the orbit catalog of Worley & Heintz (1983), this is         Wor1983 
                         apparently the first speckle measure of this system.                    Hor1997 
                         A few more speckle observations will strengthen orbit considerably.             
                         Martin et al. (1998) derive component masses 1.614 +/- 0.211 and                
                         1.256 +/- 0.195 Msun.                                                   Mig1998 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.53 +/- 0.16, 2.11, and 1.19 Msun, respectively.             Mlk2012 
06573-4929   RST5253     A premature orbit has been computed.                                            
06575-1253   BRT2656     RST 3476.                                                                       
06575-1949   HDO  93     CPD-19@1581+2.                                                                  
06576+0630   J  1981     Not found by Heintz.                                                    Hei1995 
06577+1722   BPM 341     [PM2000]  644902 + [PM2000]  644517.                                    Gvr2010 
06577-4118   I  1160     Primary is V358 Pup, an Algol-type eclipsing binary, P = 6.79393d.      Zas2012 
06579+6220   HEN   2     Delta-M is in K band.                                                           
                         LSPM J0657+6219 = GJ 3417. Law et al (2008) derive a distance of        Law2008 
                         11.4 +/-0.3 pc and a projected separation of 17.5 +0.5/-0.5 au.                 
                         Estimated spectral types are M4.5 and M6.5.                                     
                         GJ 3417 = LHS 1885. If taken at face value, the body of astrometric             
                         points that exists for this target does not make sense. Three epochs            
                         of astrometry exists: One from Henry et al. (1997) taken in 1996 (rho   Hen1997 
                         = 2.0" and theta = 220deg), one from Law et al. (2008) taken in 2005    Law2008 
                         (rho = 1.5" and theta = 320deg), and our data point taken in 2012 (rho          
                         = 1.4" and theta = 240deg). Given that background objects can be                
                         firmly excluded, this would imply an enormously fast orbital motion             
                         since the binary would move from 220deg to 320deg and then back to              
                         240deg within 16 years, which is impossible for such a low-mass binary          
                         with a ∼17 au semi-major axis. However, the astometry becomes entirely  .     
                         sensible in an orbital motion framework if we impose a 90deg phase              
                         shift on the Law et al. (2008) position angle such that it is 230deg            
                         instead, giving a continous motion of 20deg in 16 years. In Janson et           
                         al. (2012), we suggested an equal phase shift for similar reasons for   Jnn2012 
                         the Law et al (2008) data point in the 15553178+3512028 binary system.  Jnn2014 
                         Estimated age 60-300 Myr; masses 0.30 +/- 0.14 and 0.15 +/- 0.08 Msun;          
                         a ~16.5 au.                                                             Jnn2014 
06579+1430   BPM 342     [PM2000]  646412 + [PM2000]  646286.                                    Gvr2010 
06579+0545   J  2618     Also known as J  2615.                                                          
06579-4417   LPM 248     Proper motion -1129 -119.                                                       
06580+0218   CHR  25     Algol-type eclipsing binary, P = 6.7664 d.                              Zas2011 
06581+1207   BPM 343     [PM2000]  647422 + [PM2000]  647050.                                    Gvr2010 
06581+1120   BPM 344     [PM2000]  647426 + [PM2000]  648090.                                    Gvr2010 
06583+1341   J  1058     TDS4336.                                                                        
06584+1334   BPM 345     [PM2000]  649175 + [PM2000]  648571.                                    Gvr2010 
06584-0234   BAL 101     BRT 388.                                                                        
06584-0438   A   326     Primary is V860 Mon, Algol-type eclipsing binary, period 2.516367d.     Zas2013 
06584-1038   GAL 418     Object #281 in Gallo's original list.                                   Gal1914 
06585+1740   BPM 346     [PM2000]  649668 + [PM2000]  649720.                                    Gvr2010 
06586+2339   POU2185     J 2767.                                                                         
06586+0641   J   278     ADS gives BD as +06@1463.                                                       
06586-0016   RST5252     Measures formerly attributed to A 1737 apparently belong to this pair   Hei1987a
06586-2525   B   124     A is a spectroscopic binary.                                                    
06586-2858   CPO   7     eps CMa = 21 CMa = Adhara                                                       
                         Intensity Interferometer Limb-darkened diameter 0.80 +/- 0.05 mas.      HBr1974 
06587+1619   BPM 349     [PM2000]  650768 + [PM2000]  651202.                                    Gvr2010 
06587+1423   BPM 347     [PM2000]  650486 + [PM2000]  650701.                                    Gvr2010 
06587+1306   BPM 348     [PM2000]  650756 + [PM2000]  650991.                                    Gvr2010 
06587-2022   BRG  23     Out of the targets that have been classified as "undetermined" with             
                         respect to common proper motion, the 2MASS J06583980-2021526AB pair is          
                         one out of two that have reasonable (or even large) chances of being            
                         chance alignments rather than physical pairs. The fainter C and D               
                         candidates at larger separations reported in Bergfors et al. (2010)     Brg2010 
                         are clearly identified as background contaminants here, given both the          
                         colors and proper motions. However, the B component gives conflicting           
                         information. On the one hand, its brightness and color are fully                
                         consistent with it being an almost equal-mass companion to the                  
                         primary, which would be a very unusual coincidence for a background             
                         object, especially at a separation of only 1.4". On the other hand,             
                         from an astrometric viewpoint, the B component is fully consistent              
                         with the expectation for a background object. The deviation from the            
                         background expectation is 0.4 sigma, and the B component has moved to           
                         a position that is 7.4 times closer to the background expectation than          
                         its first-epoch position, with confidence for the motion of 7.5 sigma.          
                         This is also unlikely to happen by chance, hence the evidence is                
                         divergent. Since the magnitude of motion is not inconsistent with what          
                         could be expected for orbital motion of a real physical pair, we keep           
                         it as binary in our analysis, but we note that further observations             
                         will be necessary in order to resolve this issue satisfactorily.        Jnn2012 
06588+2605   CHR 170     39 Gem.                                                                         
06588+1444   BPM 350     [PM2000]  651364 + [PM2000]  651338.                                    Gvr2010 
06588+1119   BPM 351     [PM2000]  651493 + [PM2000]  651751.                                    Gvr2010 
06590+1519   BPM 352     [PM2000]  652206 + [PM2000]  652515.                                    Gvr2010 
06591+0044   GAU4894     J 1983. BAL 1061.                                                               
06591-3711   HRG   7     Aka WFC  47.                                                                    
06592-1347   GAL 284     LDS6204.                                                                        
06593+4219   BAG  43     Primary is the alpha2 CVn type variable NY Aur.                                 
06593-1610   GAL 419     Object #283 in Gallo's original list.                                   Gal1914 
06594+1421   BPM 353     [PM2000]  654449 + [PM2000]  654775.                                    Gvr2010 
06595+3706   ALI 574     AC: Due to a typographical error in an 1892 measure by Espin (theta             
                         220.9 rather than 120.9), this measure was erroneously identified as            
                         a new pair (ES 2621AH).                                                 Es_1901 
             BOT   6     AJ: Boettger originally assigned this pair to ALI 574AC, and it was             
                         catalogued with rho as 22.3424 rather than 223.424.  However, the               
                         wide pair is obvious.                                                   Bot1962 
06595+2555   MCA  28     40 Gem.                                                                         
06598+0037   GAU4919     J 1984. BAL 1065.                                                               
06599+0701   DOO  41     J 2620. One-degree error in WDS designation.                                    
07001+7938   PRZ   6     AB: WFC  48.                                                                    
07001+1259   BPM 354     [PM2000]  657977 + [PM2000]  658414.                                    Gvr2010 
07002+1505   BPM 355     [PM2000]  658613 + [PM2000]  658800.                                    Gvr2010 
07002-2243   S   543     B is BD-22@1642.                                                                
07002-3109   SHY 187     HIP  33705 + HIP  33691.                                                        
07003+1639   BPM 356     [PM2000]  659139 + [PM2000]  658729.                                    Gvr2010 
07003-0522   HD  52265   GC 9220. Chauvin et al. (2006) note finding at least one faint          Cvn2006 
                         companion candidate within separation/magnitude range listed. However,          
                         further observations are required for verification                              
                         Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from Butler       CPS2000d
                         et al. (2000).                                                          HaI2001 
07003-2207   FIN 334     A variable, FU CMa.                                                             
                         1989.9336: The system has opened slightly since the last speckle                
                         observation in 1989.3; unfortunately it was last observed in 1966 so            
                         it may be difficult to pin down the time of periastron passage.         Hrt1993 
                         Aa,Ab: Docobo & Andrade (2013) derive a dynamical parallax of 2.03 +/-          
                         0.25 mas and component masses 5.51 +/- 2.64 and 5.51 +/- 2.64 Msun              
                         (for spectral type B3V) or 1.01 +/- 0.25 mas, 6.62 +/- 3.28 and 6.62            
                         +/- 3.28 Msun (for B2IV). See paper for extensive notes on system.      Doc2013d
07004+1926   VKI  14     Aka OL  167.                                                                    
07004+1227   BRT2285     Declination corrected by Heintz.                                        Hei1990b
07005-6052   HJ 3924     B is CPD-60@743.                                                                
07006+3157   RED  16     2MASS J07003664+3157266. Spectral types L3.5 and L6:                    Red2006b
07006+1243   STF1007     Also published as BU 99.                                                        
                         CCD Image taken by Florentino Sanchez Bajo, and obtained with the 40cm          
                         reflector of the Observatory of Extremadura University, Badajoz, Spain          
07006-1915   HDO  95     Winlock AB listed at theta=138.8; changed to 180-138.8 = 41.2 based on  Win1882 
                         later observations.                                                             
                         "C about equally distant from A and B, and at about 2 1/2 times the             
                         distance of A and B from each other."                                   Win1882 
07007+4527   ES 1324     AB: BRT  95                                                                     
07007+0012   J  1985     BAL 1068.                                                                       
07008+3156   AG  129     SEI 467.                                                                Nsn2017b
07008+2716   BU 1022     AB: Rectilinear solution by Rica & Zirm (2012).                         FMR2012i
07008-0656   A   516     J 357.                                                                          
07009+7136   LDS1641     NLTT 17216/17217                                                        Chm2004 
07009+5651   KR   29     All measures attributed to AC pair were actually of BC pair.                    
07012+3622   A  1957     TDS4387.                                                                        
07012+1434   BPM 357     [PM2000]  663617 + [PM2000]  663302.                                    Gvr2010 
07012+1146   STT 163     A premature orbit has been calculated.                                  Mlr1950a
07013+5203   HJ 2354     ES 1078. Probably an error in HJ's angle (ADS).                         A__1932b
07013-5242   BRT2024     CD-52@1784.                                                                     
07015+1630   BPM 358     [PM2000]  665473 + [PM2000]  665063.                                    Gvr2010 
07015-0307   A   518     AB. The classification listed in Mason et al. (1998) is from Conti et   Msn1998a
                         al. (1977).                                                             Cti1977 
             A   517     DH: 07014-0308 was found to be D component of 07015-0307; merged.               
07017+1301   BPM 359     [PM2000]  666419 + [PM2000]  665870.                                    Gvr2010 
07017-1100   GAL 287     Object #287 in Gallo's original list. GAL 420. J  2771.                 Gal1914 
07017-2756   B   126     sig CMa = 22 CMa = Unurgunite. An irregular variable.                           
07018-1118   HU  112     Includes GU CMa, a Beta Lyr type eclipsing binary, P = 1.61014d.        Zas2012 
07021+2148   CHR 215     First detected as an occultation binary by Evans & Edwards.             Evn1983a
                         V335 Gem. Primary is eclipsing binary of Algol-type, period 1.76782d.   Zas2014 
07021-0637   J   359     Declination was 15' in error, according to Heintz, which probably       Hei1985a
                         explains unresolved observation of van den Bos.                         B__1960b
07021-0953   GAL 421     Object #290 in Gallo's original list.                                   Gal1914 
07022-4900   HJ 3920     SWR  21.                                                                        
07023+1235   HJ 3288     B is BD+12@1394.                                                                
07024+3639   BRT2590     ALI 340.                                                                        
07025-1443   LDS 850     NLTT 17333/17335                                                        Chm2004 
07026+1558   A  2462     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 0.87 +/- 0.33, 2.24, and 1.05 Msun, respectively.  Mlk2012 
07026+0250   J  1987     BAL 1760.                                                                       
07026-2106   HJ 2358     Probably = HDO 94 = HDO 96.                                                     
07028+0250   J  1988     BAL 1761.                                                                       
07028-0716   RST4331     J 1464.                                                                         
07028-1642   WZ   11     GAL 292.                                                                        
07031+3809   NLTT 17323  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Latham et al. (2002).                                                   Lat2002 
07031-0029   J  2450     BAL 762.                                                                        
07032+3457   GII  82     Aa,Ab: GII  92Aa,Ab                                                             
07032+1016   BPMA 32     [PM2000]  673827 + [PM2000]  674654.                                    Gvr2010 
07033+1227   GIC  68     G110-031/G110-032.                                                              
                         NLTT 17343/17344                                                        Chm2004 
07034-2948   HJ 2361     B is CD-29@3827.                                                                
07036+3941   A  1959     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.22 +/- 1.29, 1.60, and 0.55 Msun, respectively.             Mlk2012 
07037-5757   BRT2534     A likely plate flaw.                                                    Grv2021b
07038+6727   HD 51708    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
07039+5242   BEU   8     LHS 224. Estimated age 1000-10000 Myr; masses 0.18 +/- 0.03 and 0.14            
                         +/- 0.01 Msun; a ~1.2 au.                                               Jnn2014 
07040+1416   BPM 360     [PM2000]  677579 + [PM2000]  677171.                                    Gvr2010 
07040-4337   DUN  38     A is a spectroscopic binary. B is CD-43@2907. AC = LDS 175.                     
                         HIP 34065. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AC: SHY  36. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
             TOK 390     Ca,Cb: HIP 34052 = HD 53680 = HIP 34065C = GJ 264 is a spectroscopic            
                         and astrometric binary for which Sahlmann et al. (2011) give an orbit   SaJ2011 
                         with P=1688d = 4.62yr and an estimated semi-major axis of 0".15. There          
                         is also an astrometric orbit (Makarov et al. 2008) with P=4.11yr that   Mkr2008 
                         predicts theta = 327deg for the moment of our first observation. The            
                         binary is resolved at 0".23, dI = 4.4mag and shows some orbital                 
                         motion. The binary makes a quadruple system together with components A          
                         and B (GJ 264.1 and 264) that form a 20".5 pair at 185" from C. The B           
                         component was also observed here and found unresolved.                  Tok2015c
                         Ca,Cb: Sahlmann (2011): orb. C: P=1688.6d e=0.475 K1=1.24               SaJ2011 
07041+7514   STF 973     AB: HJL  80.                                                            HJL1986 
             LDS1642     AC: Wrong C coordinates in Tokovinin & Lepine (2012).                   Tok2012c
07041+2034   SHJ  77     zet Gem = 43 Gem = Mekbuda. STTA 81 = H 6   9.                                  
                         A is a Cepheid, and an occultation double.                                      
07041+1544   BPM 361     [PM2000]  678170 + [PM2000]  677669.                                    Gvr2010 
07041+1406   BPM 362     [PM2000]  678323 + [PM2000]  678859.                                    Gvr2010 
07041-0038   RST4836     J 2775.                                                                         
07043+0129   STTA 82     B is BD+01@1663.                                                                
07043-0303   A   519     The A component is a spectroscopic binary, P = 5.72d. The RV range in           
                         the blended light is about 30 km/s.                                             
07043-5645   DSG  11     V386 Car.                                                                       
07045-4232   DON 159     CPD-42@1197.                                                                    
07046+2117   BRT2368BC   Aka SMA  71.                                                                    
07049+2807   STF1012     HJL  81.                                                                HJL1986 
07051+1519   GII  93     Aa,Ab: Gili (2016) is uncertain whether the close pair is associated            
                         with the A or B component of HEI  49.                                   Gii2016 
07051+0124   NLTT 17385  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Latham et al. (2002). They derived component masses 1.16 and 0.70 Msun  Lat2002 
                         and an estimated semimajor axis of 22.71 mas.                           Ren2013 
07051-4711   RST 232     CPD-46@1205.                                                                    
07055+2413   POU2411     Aka POU2388 and POU2416.                                                        
07055+0522   J  2778     Aka AHD  36.                                                                    
07056-2613   SKF1989     Equilateral trio found by Robert Douglas, reported via Steve Gottlieb   Skf2014 
                         ('amastro' mailing-list post 2013 Dec 31).                                      
07056-7116   TOK 114     HIP 34212. A is SB without orbit (dRV= 4.3km/s), also astrometric       Nrd2004 
                         binary in Hipparcos.                                                            
                         A is possible SB, unresolved with NICI in Tokovinin (2012). B is not    Tok2012b
                         seen (outside field).                                                   Tok2014d
             HIP  34212  The image seems elongated at 45deg - partially resolved? A large RV             
                         amplitude and large acceleration hint at a short period.                Tok2013b
07057+5245   STF1009     AB: H 1  69.                                                            MEv2010 
07058+8337   LDS1640     NLTT 17187/17126                                                        Chm2004 
07058-1040   D    12     A is a Beta CMa-type variable, V569 Mon.                                        
                         Spectrum; B0.5V+F5III.                                                          
07059-0101   CRJ   1     Primary is NLTT 17405. Crepp et al. (2012) derive spectral types F8V            
                         and K7-M0, masses 1.51 +0.20/-0.27 and 0.65 +/- 0.03 Msun.              CrJ2012 
07060-3039   TOK 952     IL CMa.                                                                         
07061-1257   HU   48     V388 CMa, Algol-type eclipsing binary, P = 2.98260 d.                   Zas2011 
07062+0425   J  2452     J 2608.                                                                         
07065-0134   BAL 399     B of BAL 399 is A of BAL 400.                                                   
             BAL 397     B of BAL 397 is also B of BAL 400.                                              
07067-1118   BU  328     A is the Beta CMa-type variable, FN CMa.                                        
                         1980.905: This observation was incorrectly attributed to ADS 5975 in    Sta1981b
                         Starikova & Tokovinin (1981) (noted in Tokovinin 1982)                  Tok1982b
07069+6233   STF1006     B is BD+62@904.                                                                 
07069-4720   BRT 701     A likely plate flaw.                                                    Grv2021b
07070+0131   HEI 903     AB: This may actually be a measure of CD.                               Sca2022a
07071-5138   SWR  22     CPM pair                                                                Skf2004 
07073+1109   BPM 363     [PM2000]  692875 + [PM2000]  693183.                                    Gvr2010 
07074+2242   BLL  19     A is the Mira-type variable, R Gem.                                             
07074+0428   BRT2130     Aka BAL2733.                                                                    
07075+2722   BRT 148     A likely plate flaw.                                                    Grv2021b
07075-0112   CHE  83     Star place uncertain; no BD star near.                                          
                         Pair not found in GSC.                                                  Bko2009d
07076-2616   BRT2885     CPD-26@1775.                                                                    
07077+0845   J  3231     J  2779.                                                                Nsn2016 
07079+1053   AG  329     GI: Primary of 07078+1052 was found to be G component of 07079+1053;            
                         systems merged.                                                                 
07079-1542   A  3043     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 10.64 +/- 7.74, 5.08, and 2.75 Msun, respectively.            Mlk2012 
07080+1532   ENG  28     AB: NLTT 17446/17443                                                    Chm2004 
                         AB: HJL  82.                                                            HJL1986 
                         AB: SHY 189. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
07080+1337   BPMA 33     [PM2000]  696183 + [PM2000]  694875.                                    Gvr2010 
07080+1109   BPM 364     [PM2000]  696016 + [PM2000]  696219.                                    Gvr2010 
07081-1036   J  2782     V931 Mon. Primary is eclipsing binary of Algol-type, period 1.9015d.    Zas2014 
07081-1155   SKF1303     Near match in radial velocities (+21 and +19 km/sec, resp).             Skf2012 
07082+2416   POU2473     AB: Position corrected by Gellera.                                      Gel1982 
             POU2474     AC: Position corrected by Gellera.                                      Gel1982 
07082+0323   HJ 2362     B is BD+03@1561.                                                                
07082-0958   EGN   6     Single epoch, so bound/unbound nature of pair unknown.                  Egn2007 
07083+2426   POU2475     Position corrected by Gellera.                                          Gel1982 
07083+1622   BPM 365     [PM2000]  697547 + [PM2000]  697498.                                    Gvr2010 
07084+1650   BPM 366     [PM2000]  697615 + [PM2000]  697946.                                    Gvr2010 
07084+1556   STT 165     45 Gem. B and C are optical.                                                    
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
07084-2624   BU 1412     del CMa = 25 CMa = Wezen                                                        
07085+2459   STF1023     B is BD+25@1585.                                                                
07085+2159   OCC 337     AGK3 +22 834. The cross-identification was misread as BD+22 834, so             
                         the Argue et al. (1984) measure was erroneously added to the WDS as             
                         05083+2214 ARU   2.                                                     Aru1984 
07085-2010   HDO  98     Aka ARA 890.                                                                    
07086+1230   BPM 367     [PM2000]  698852 + [PM2000]  698881.                                    Gvr2010 
07087+1044   BPMA 34     [PM2000]  698923 + [PM2000]  698438.                                    Gvr2010 
07087-7030   DUN  42     A: gam 2 Vol.                                                                   
                         B: gam 1 Vol. B is a spectroscopic binary and is variable.                      
07091-2655   B   710     CPD-26@1815.                                                                    
07092+1903   CHR 216     First detected as an occultation binary by Africano.                    Afr1975 
07092-5622   DUN  40     B is CPD-56@1262.                                                               
                         Identified as optical and linear solution also published.               LRR2022c
07093+0326   BAL2250     Baillaud suspected A to be double.                                      Bal1944 
07093-1021   SNA   5     We resolved the long-period SB2 unveiled by Boyajian et al. (2007, ApJ          
                         664, 1121)                                                              Sna2014 
07093-1347   KRV   1     Classical Cepheid TV CMa.                                                       
07093-4959   HJ 3935     B is CD-49@2647.                                                                
07094+1243   BPM 368     [PM2000]  701909 + [PM2000]  701957.                                    Gvr2010 
07095-0140   BKO 492     Anon. 1.                                                                Bko2009d
07095-2012   HDO 101     Aka ARA 894.                                                                    
07096+2544   HO  519     A is a spectroscopic binary, P = 32.81d.                                        
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
07097+0029   J  2454     BAL 1083.                                                                       
07097-0236   BKO 493     Anon. 2.                                                                Bko2009d
07097-2514   B  2136     A spectroscopic binary. One component variable?                                 
07098-0231   BKO 494     Anon. 3.                                                                Bko2009d
07100+3832   GJ 268      Barry et al. (2012) combine ELODIE radial velocity data with IOTA               
                         interferometric measurements to derive a combined solution for this             
                         nearby pair. An orbital parallax of 0".15888 +/- 0".00072 is derived,           
                         yielding masses 0.22599 +/- 0.00065 and 0.19248 +/- 0.00056 Msun. The           
                         H-band flux ratio is 1.163 +/- 0.021 (or dH = 0.16).                    Sgr2012 
07100+2442   POU2513     BRT3280. BRT 149.                                                               
07100+1008   BRT1223     Probably J  3339.                                                       Nsn2016 
07100-0044   VAS  11     VSK   5.                                                                        
07100-0201   BKO 495     Anon. 4.                                                                Bko2009d
07100-0236   BKO 496     Anon. 5.                                                                Bko2009d
07100-3639   JSP 140     Primary is V652 Pup, eclipsing binary of W UMa-type, period 0.371829d.  Zas2013 
07101+2115   GC 9462     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Beavers & Salzer (1985).                                                Bvr1985 
07101+0454   BAL3006     J 2455.                                                                         
07102-0414   BUP  97     20 Mon.                                                                         
07102-1841   RST2456     HR 2705.                                                                        
07103+3739   GIC  69     G087-028/G087-029 = GJ 3430A/3431B.                                             
07103-0052   VAS  12     VSK   6.                                                                        
07104+3431   LDS3726     Luyten (1978) lists a position angle of 355deg. However, the only       Luy1978 
                         likely pair in the vicinity shows an angle of ~274deg. His value was            
                         changed to 275 with an N code, under the assumption there was a                 
                         typographical error 1n his paper (perhaps he wrote 175 rather than              
                         275, then gave a quadrant flip?)                                                
07104+2421   OSO  19     G088-010. Not a common proper motion pair, based on color and                   
                         comparison with POSS2 red plates.                                       Oso2004 
07104+0535   J  2787     Not found by Heintz.                                                    Hei1995 
07104-5536   RMK   5     Spectrum: G8/K0III+G/K.                                                         
                         SWR  23. CPM pair                                                       Skf2004 
                         Rectilinear solution by Letchford et al. (2018).                        LRR2018a
07105-0306   BAL 143     The C component appears to have been either a plate flaw or a                   
                         typographical error in the catalog used by Baillaud.                    Bal1944 
                         AC: Pair not found in GSC.                                              Bko2009d
                         BC: Pair not found in GSC.                                              Bko2009d
             BKO 497     Anon. 6.                                                                Bko2009d
07106+1543   J   703     Rectilinear solution by Cvetkovic et al. (2015).                        Cve2015 
                         Rectilinear solution by Dugan et al. (2019).                            SHS2019b
                         Gaia parallax and proper motion indicate the pair is optical and the    Dbr2019c
                         orbit in ORB6 appears to be erroneous.                                  Cve2008d
07107+1051   BPM 369     [PM2000]  706894 + [PM2000]  706864.                                    Gvr2010 
07107-4116   RST2458     V362 Pup, Algol-type eclipsing binary, P = 9.26581 d.                   Zas2011 
07108+3642   BRT2591     ALI 344.                                                                        
07108-0130   BKO 498     Anon. 7.                                                                Bko2009d
07108-0230   BKO 499     Anon. 8.                                                                Bko2009d
07108-0234   BKO 500     Anon. 9.                                                                Bko2009d
07109-0134   BKO 501     Anon. 10.                                                               Bko2009d
07109-0251   A   521     Aka TDS4555.                                                                    
07110-0230   BKO 502     Anon. 11. Not BAL 146, as suggested by Berko.                           Bko2009d
07111+3015   BU 1009     tau Gem = 46 Gem. A is an irregular variable.                                   
                         NPOI Limb-darkened diameter    2.346 +/- 0.069 mas,                             
                         R =   30.27 (+1.08- 1.09)  \rsun,  Teff = 4583 +/-  70 K,                       
                         L =  364.7 +/-  14.4 \lsun.                                             NOI2023 
07111-0205   BKO 503     New pair mistaken for BAL 434 by Berko.                                 Bko2009d
07112+4330   MTG   1     AB: LSPM J0711+4329 = NLTT 17488. Law et al (2008) derive a distance    Law2008 
                         of 12.3 +5.6/-2.0 pc and a projected separation of 2.3 +1.1/-0.4 au.            
                         Estimated spectral types are M4.5 and M6.                                       
                         Dupuy et al. (2010) determine system mass 0.194 +0.025/-0.021 Msun;             
                         spectral types are M6.5 +1.0/-0.5 and M6.5 +1.0/-0.5.                   LiM2010 
                         AC: Estimated age 1000-10000 Myr; masses 0.15 +/- 0.03 and 0.09 +/-             
                         0.01 Msun; a ~4.5 au.                                                   Jnn2014 
07112-0206   BKO 504     Anon. 12.                                                               Bko2009d
07112-0304   BAL 151     BRT 397.                                                                        
07113+3307   SHY 190     HIP  34714 + HIP  34700.                                                        
07113-0205   BKO 505     Anon. 13.                                                               Bko2009d
07113-0208   BAL 436     Anon. 14.                                                               Bko2009d
07113-0247   BAL 152     No star at primary location - plate flaw or typo in AC catalog.                 
07114+5851   STI 637     STI2177                                                                         
07114-0025   A  1961     One component is a Delta Scuti-type variable.                                   
07114-0130   BAL 437     The brighter component (even in the blue) is the red variable BW Mon.   Skf2010 
                         It was classified as spectral type M1 in the early Dearborn survey,             
                         but M5: by Jack MacConnell. The strong variability and very bright              
                         2MASS magnitudes suggest the latter is more nearly correct.                     
07114-0138   BKO 506     Anon. 15.                                                               Bko2009d
07114-3906   FIN 377     Hipparcos suspected non-single.                                                 
07115-0006   BKO 507     Anon. 16.                                                               Bko2009d
07115-0244   BKO 508     Anon. 18.                                                               Bko2009d
07117-0006   BKO 509     Anon. 19.                                                               Bko2009d
07117-0219   BKO 510     Anon. 20.                                                               Bko2009d
07117-0224   BKO 511     Anon. 17. Identification corrected by author (private comm.)            Bko2009d
07118+3517   BRT3247     ALI 104.                                                                        
07118-0130   BKO 322     Anon. 21.                                                               Bko2009d
07119-0030   J    58     del Mon = 22 Mon                                                                
07119-0132   BKO 323     Anon. 22.                                                               Bko2009d
07119-0135   BKO 512     Anon. 23.                                                               Bko2009d
07120+2217   STF1035     HJL  83.                                                                HJL1986 
07120-3510   WSI 126     The two components of 2MASS J07115917-3510157 have nearly equal                 
                         brightnesses and colors, hence it is very likely that they form a               
                         physical pair. They have yet to be demonstrated to share a common               
                         proper motion.                                                          Jnn2012 
07123+1211   BPM 370     [PM2000]  712648 + [PM2000]  712876.                                    Gvr2010 
07123-0526   BU  196     Primary is eclipsing binary of Algol-type, period 1.211458 day.         Zas2013 
07124-0139   BKO 324     Anon. 24.                                                               Bko2009d
07124-0307   BKO 513     Anon. 25.                                                               Bko2009d
07124-2158   BRT1399     CPD-21@1867.                                                                    
07124-3633   BU  757     B may be variable.                                                              
07125-0146   BKO 514     Anon. 26.                                                               Bko2009d
07125-0228   BKO 515     Anon. 27.                                                               Bko2009d
07126-0041   STF1043     J 61.                                                                           
07128+2713   STF1037     Variable? See Baize & Petit catalog of doubles with variable component. Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.77 +/- 0.77, 2.42, and 1.10 Msun, respectively.  Mlk2012 
             STT 166     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
07128+2121   STT 168     AB: H N  94.                                                            MEv2010 
07131-0256   BKO 516     Anon. 28.                                                               Bko2009d
07132-3058   HJ 3940     This is the variable HO CMa.                                                    
07133-0150   BAL 452     Pair not found in GSC.                                                  Bko2009d
                         A likely plate flaw.                                                    Grv2021a
07134+1610   H 6  74     AB: H VI 74. 51 Gem. A is the semiregular variable variable BQ Gem.             
07135-4438   HJ 3943     A is a long-period variable.                                                    
07137-2005   FOX9001     Previously known as FOX  12a.                                                   
07138-0502   BRT 400     J 2626.                                                                         
07138-2254   HJ 3938     B is BD-22@1760.                                                                
07139-0645   BRT 401     Not found in Heintz at IDS position.                                    Hei1990b
07140-2610   BRT2886     A likely plate flaw.                                                    Grv2021b
07141+1304   BPM 371     [PM2000]  718812 + [PM2000]  718706.                                    Gvr2010 
07143-2621   FIN 323     27 CMa. B is an irregular variable, EW CMa.                                     
07144+2443   VAS  13     VSK   7.                                                                        
07146-0212   J  2792     BAL 163.                                                                        
07146-1018   STF1052     B is BD-10@1935.                                                                
07147+2453   HO  343     52 Gem.                                                                         
07148+5233   STF1033     AB: H 1  76.                                                            MEv2010 
07148-1529   BU  575     AB. A premature orbit has been computed.                                        
                         1997.1226: The magnitude difference of the system is listed in the WDS          
                         as 0.1. Our reduction does not give the same quadrant as the latest             
                         measure in the WDS.                                                     Hor1997 
07148-2101   HO  344     Includes MP CMa, an Algol-type eclipsing binary, P = 1.96326d.          Zas2012 
07150+0956   J  2457     J  2794.                                                                J__1962a
07151+5717   LDS2529     A is SB1, P=34.034d. RoboAO resolves AC at 0.24", 9d, dI=1.17. Still            
                         to be confirmed before accepting.                                       Tok2014d
07151+2553   BU 1023     BDS 3919; L 8 same star.                                                        
07153+2036   GIC  70     LDS 898. G088-017/G088-018.                                                     
07153+1849   CHR 217     First detected as an occultation binary by Africano.                    Afr1975 
07153-0010   BU 1268     24 Mon.  STT 169.                                                               
07154+1507   BPM 372     [PM2000]  722963 + [PM2000]  723173.                                    Gvr2010 
07154+1444   BPM 373     [PM2000]  723049 + [PM2000]  723124.                                    Gvr2010 
07156+0504   J  3101     BK CMi. No measure published by Jonckheere; coarse 1995 measure from            
                         GSC2.3 (Aladin).                                                                
07156+0503   DOM   2     Mistakenly observed for J  3101. Error reported by John Nanson (2016,           
                         private comm.)                                                                  
07155-1106   J  2459     J  2800.                                                                        
07156-6311   R    72     B is CPD-62@805.                                                                
07157+1537   BPM 374     AB: [PM2000]  724039 + [PM2000]  723705.                                Gvr2010 
             BPM 375     AC: [PM2000]  724039 + [PM2000]  724305.                                Gvr2010 
             BPM 376     CD: [PM2000]  724305 + [PM2000]  724546.                                Gvr2010 
07158-0048   XMI  54     ARN 104.                                                                        
07160-2930   HJ 2370     B is CD-29@4143.                                                                
07161-0138   J  2802     BAL 459.                                                                        
07162+1603   BPM 377     [PM2000]  725546 + [PM2000]  725765.                                    Gvr2010 
07163+2709   GJ 268.3    combined solution of astrometric orbits and DSBs. Paper includes        Are2000 
                         masses and distances.                                                           
07163-0635   CHE  84     Also known as AG  333.                                                          
07164+4738   STF1044     Also known as ARN  68.                                                          
07165-1559   ROE  28     BRT 567.                                                                Brt1932b
07166-2319   HJ 3945     B is CD-23@5192.                                                                
             SHY 508     BC: HIP  35213 + HIP  35578.                                                    
07166-5100   HJ 3951     A is a semi-regular variable.                                                   
07167+1623   BPM 378     [PM2000]  727247 + [PM2000]  726886.                                    Gvr2010 
07167+1502   BPM 379     [PM2000]  727304 + [PM2000]  727556.                                    Gvr2010 
07167+0312   BAL2261AC   Optical/physical nature ascertained from Gaia DR2.                      FMR2019b
07168+1331   BPM 380     [PM2000]  727457 + [PM2000]  727700.                                    Gvr2010 
07168+0059   A  2855     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.08 +/- 0.35, 1.91, and 0.85 Msun, respectively.             Mlk2012 
07170-3054   BSO   2     B is CD-30@4233.                                                                
07171+2641   CHR 218     First detected as an occultation binary by Schmidtke et al.             Smk1989 
07171-1202   A  2123     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 4.05 +/- 1.61, 2.32, and 1.20 Msun, respectively.  Mlk2012 
07171-1202   STF1064     C is a close 22.5-d spectroscopic pair.                                 Tok2019a
07171-3706   DUN  43     pi Pup. B is CD-36@3487.                                                        
07172+3306   TOK 379     AB: The CPM nature of B is not certain (PM diff. with A), but accepted  Tok2014d
07172-2351   I   773     ADS 5960a.                                                                      
07175+1646   BPM 381     [PM2000]  730232 + [PM2000]  730294.                                    Gvr2010 
07175+0048   SLE 301     The Soulie (1985) measure is possibly incorrect due to a 20" error in           
                         the measured declination of the secondary.                              Sle1985 
07175-4659   I     7     The 94-yr orbit by Heintz (1995) plus the HIP parallax gives            Hei1995 
                         impossibly small mass-sum. Probably both a and P are much larger (no            
                         orbit for another century), but motion should be followed.                      
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 0.43 +/- 0.23, 1.54, and 0.76 Msun, respectively.             Mlk2012 
07176+0918   STT 170     A premature orbit has been computed. Speckle would be useful as the             
                         pair closes in.                                                                 
07176-0221   BAL 167     J 2806.                                                                         
07177+1327   BPM 382     [PM2000]  730634 + [PM2000]  730973.                                    Gvr2010 
07178+1553   BPM 383     [PM2000]  730919 + [PM2000]  730654.                                    Gvr2010 
07178+1131   BPM 384     [PM2000]  731123 + [PM2000]  731057.                                    Gvr2010 
07179-0221   BAL 168     J 2808.                                                                         
07180+4548   LDS3731     NLTT 17633 + 17637. Secondary is white dwarf WD 0714+458.               Far2005b
07181+1632   STF1061     lam Gem = 54 Gem. A is a spectroscopic and occultation binary, and may          
                         be variable.                                                                    
                         CHARA Array Limb-darkened diameter  0.835 +/- 0.013 mas,                CIA2012e
                         R =  2.777 +/- 0.047 \rsun, L = 28.306 +/-0.648 \lsun,                          
                         Teff = 8007 +/-  77 K, M = 2.111 +/- 0.010 \msun,                               
                         Age =  0.8 +/- 0.0 Gyr.                                                         
07181+0421   STF1063     J 1992. BAL 2753. BAZ   3.                                                      
                         BAZ   3 was misplaced in the WDS. The Tobal (2010) measures are of      Tob2012c
                         some unknown pair near the original location of BAZ   3 = 04181+0448.           
07181-1342   STF1069     B is BD-13@1925.                                                                
07182+4006   ES 1634     BRT  96                                                                         
07183-0317   RST4347     J 2463.                                                                         
07183-3644   JC   10     A is the variable NV Pup. Spectrum composite; B2V+B3IVne. B is NW Pup.          
07185-5721   RST 244     AB: B moves away from PM(A) at 17mas/yr for 34yr. Optical?              Tok2014d
             TOK 116     HIP 35374. Quadruple. Both A and B are close visual pairs.              Tok2011a
07187-2434   29 CMa      UW CMa.  The classification is from the UV tomographic analysis of      Bgn1994 
                         Bagnuolo et al. (1994).                                                 Msn1998a
07187-2457   FIN 313     A: 30 CMa = tau CMa. A is Beta Lyrae-type system, probably variable.            
                         See discussion of the system by Sana et al. 2014).                      Sna2014 
             HJ 3948     van Leewen & van Genderen (1997 A&A 327, 1070) and Stickland et al.     Stc1999 
                         (1999) argue that the brighter Aa component of the visual Aa,Ab binary          
                         is a triple system consisting of a close 1.28-day eclipsing system              
                         orbiting a distant O star (the spectroscopic binary with a period of            
                         154.9 d).  The visual Aa,Ab pair has slowly decreased in separation             
                         from 0".19 to 0".15 between 1977 and 1994.                              Msn1998a
                         Classification of the D component is from Hoffleit & Warren (1991).     Hof1991 
                         1996.155: Date from J. Christou (private communication).                        
07188+0054   J  2465     BAL 1397.                                                                       
07188-2003   ARA 575     HDO 103                                                                         
07188-2449   BRT2893     CPD-24@2221.                                                                    
07190+1314   BRT1230     J 2466.                                                                         
07190-4934   SWR  24     CPM pair                                                                Skf2004 
07192+1548   BPM 385     [PM2000]  735557 + [PM2000]  735932.                                    Gvr2010 
07192-2457   B   133     Variable radial velocity.                                                       
07193-2453   B   134     CPD-24@2250.                                                                    
07194+1540   BPM 386     [PM2000]  736350 + [PM2000]  736218.                                    Gvr2010 
07195+3226   ES  341     SEI 477.                                                                Nsn2017b
07200-0847   BUG  17     WISE J072003.20-084651.2 is old, active M9.5 dwarf, distance 6.0 +/-            
                         1.0pc. Companion ~T5, rapidly rotating and magnetically active.         Bug2015 
                         Burgasser et al. (2015) derive spectral types M9.5 +/- 0.5 and                  
                         T5.5 +/- 0.5. A best-fit orbit based onastrometry and spectroscopy              
                         yields estimated component masses of 0.081 +0.0029/-0.0016 and                  
                         0.062 +0.009/-0.011 Msun. T0 was not provided and was determined by     Bug2015b
                         trial and error with comparison to their Figure 8.                              
                         Mass : A = 99 +/- 6 \MJup, B = 66 +/- 4 \MJup.                          Dup2019 
                         Teff : A = 2407 +/- 15 K, B = 1250 +/- 40 K.                                    
07201+2159   STF1066     del Gem = 55 Gem = Wasat. CHE  85.                                              
                         Star A is an occultation double and SB1, P = 6.129 yr.                          
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Abt (1965).                                                             AbH1965 
                         H 2  27.                                                                MEv2010 
07201-1435   BRT1871     A likely plate flaw.                                                    Grv2021b
07201-2153   I   391     D is CPD-21@2035.                                                               
07202+1539   BPM 387     [PM2000]  738931 + [PM2000]  738864.                                    Gvr2010 
07202-4411   WFC  53     SWR  25. CPM pair                                                       Skf2004 
07204-5219   RMK   6     Spectrum of B G0V:e.                                                            
                         B is X-ray source, chrom. active.  Ba is SB1, P=122.69d. Ba1 is SB1,            
                         P=10d (Saar et al. 1990 A&A 235, 291).                                  Tok2014d
                         AB: Rectilinear solution by Letchford et al. (2018).                    LRR2018a
07204-5618   VIG  10     The B, C, and D components all appear to be faint background stars.     Vig2012 
07207-5212   HJ 3958     B is CD-51@2444.                                                                
                         Measure of 1938.1 made by a transit interferometer.                     CpP1938c
07207-6205   JSP 158     Spectral type G0?                                                               
07208+6526   CHM   4     AB. NLTT 17675 + 17679.                                                         
             LDS1207     AC. HIP 35599. See Allen et al. (2000) for information on metallicity,  AlC2000 
                         age, galactic orbital parameters, etc.                                          
07208+3128   S   546     B is BD+31@1541.                                                                
07209-2658   SEE  76     A is a variable, HQ CMa.                                                        
07209-4831   HJ 3956     V366 Pup, Algol-type eclipsing binary, P = 2.484026 d.                  Zas2011 
07210-2157   BRT 315     CPD-21@2062.                                                                    
07211+6740   RED  22     M3 star is ~21" from K0 dwarf HD 56168 = HIP 35628 = 2MASS                      
                         J07210672+6739425. The Hipparcos distance for the M dwarf 27pc, the             
                         very different proper motions suggest the stars appear unrelated.       Red2007a
             JNN  55     BC: In addition to the close binarity discovered in the AstraLux data,          
                         there is a star at 21" separation (HIP 35628), but due to its very              
                         different proper motion, it is likely physically unrelated to the       Red2007a
                         2MASS J07210894+6739590 system (Reid et al. 2007).                      Jnn2012 
07213+1602   BPM 388     [PM2000]  742163 + [PM2000]  742430.                                    Gvr2010 
07214+0305   J  1994     BAL 2270.                                                                       
07214-4832   DUN  45     B is CD-48@2891.                                                                
07216-5521   R    75     AB = SWR  26. Eastern pair in 25" CPM trio                              Skf2004 
07217+7300   MLR 476     Also known as TDS4734.                                                          
07217-6157   BSO  16     A is the variable V389 Car. B is CPD-61@813.                                    
07219+4614   ES 2624     B is BD+46@1254.                                                                
07219+2027   BU 1413     56 Gem. A is a suspected variable.                                              
07220+3646   BU  901     65 Aur.                                                                         
07220-0859   HD  57682   Additional radial velocity measurements by Penny et al (1993) confirm   Pny1993 
                         the lack of variability.                                                Msn1998a
07222-2412   HJ 9002     Previously known as HJ 5451a.                                                   
07223+5954   STF1055     47 Cam.                                                                         
07223+5009   STF1065     20 Lyn. Spectroscopic binary.                                                   
                         H N  61.                                                                MEv2010 
07223-3555   HJ 3957     A 4.6d spectroscopic solution for the A component has been found        Tok2018d
                         making this a triple system.                                                    
07224+0854   GIC  72     AB = G089-013/G089-014.                                                         
             LDS2735     G089-014. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         BC : Also known as ALC   2.                                                     
07225-0215   ROE  29     BAL 170.                                                                        
07227-2109   HO  521     aka HO  627                                                                     
07229+5517   STF1062     19 Lyn. Both components appear to be spectroscopic binaries.                    
                         AB: H 3  83.                                                            MEv2010 
07229+3413   HJ  757     Aka POP 207.                                                                    
07230+4500   SHY 510     BC: HIP  35799 + HIP  35341. C component = 64 Aur.                              
07230-2546   B   719     VY CMa. This multiple "star" is involved in nebulosity, shaped like             
                         the tail of a comet. All companions may be knots in the nebulosity,             
                         and all may seem variable.                                                      
                         Adaptive optics imaging by Shenoy et al. (2013) in Ks, L', and M bands          
                         suggest the brightness of the "Southwest Clump" (~1.5" from central             
                         star) is almost entirely due to scattering from silicate dust grains.           
                         Lower mass limit for this feature is 5 x 10^-3 to 2.5 x 10^-2 Msun,             
                         depending on assumed gas-to-dust ratio. Presence of clump with no               
                         apparent counterpart on other side of star suggests ejection event.     SDP2013 
07231+7259   GIC  73     LDS5195. G251-032/G251-033.                                                     
                         NLTT 17701/17707                                                        Chm2004 
07231-2532   RSS   7     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
07234+1237   BPM 389     [PM2000]  749038 + [PM2000]  748794.                                    Gvr2010 
07235-1318   BRT1874     Hipparcos suspected non-single.                                                 
07237+2025   MET  50     Heinze et al. (2010) determine that both the B and C companions are             
                         background objects.                                                     Hze2010 
07240-0359   STF1084     H 4  95.                                                                MEv2010 
07241-2918   SMY   2     eta CMa = 31 CMa = Aludra. B is CD-29@4321.                                     
07242+1428   J   396     J 2628.                                                                         
07242-0859   J  2815     J 2425.                                                                         
07242-2637   RST1345     CPD-26@2080.                                                                    
07245+2330   POU2745     LDS 899. G088-026/G088-025 = NLTT 17816/17814                           Chm2004 
07245+0042   RST5262     Aka TDS4775.                                                                    
07246+3749   STF1079     C of STF 1079 is A of BU 1414 (07244+3746).                                     
07246+0841   SLE 567     There is an error in the published declination of Soulie's secondary.   Sle1986b
07247+1230   BPMA 35     [PM2000]  753090 + [PM2000]  753453.                                    Gvr2010 
07247-3149   DAW 129     A is a suspected variable.                                                      
07250-2101   HJ 3964     Maybe cpm or maybe both components are just members of NGC 2384.        Dam2018d
07250-3821   LDS 180     B is CD-38@3367.                                                                
07251+0638   GIC  74     G089-017/G089-018.                                                              
07251-0050   BAL 807     J 2629.                                                                         
07251-2110   DAM1372AD   Maybe cpm but like 07250-2101 = HJ 3964, maybe these are other members  Dam2018d
                         of NGC 2384.                                                                    
07252-0544   SCJ   5     B is BD-05@2105.                                                                
07253+5507   STI2187AB   Appears to be the same as HJ 2373.                                      Dam2016d
07253+0311   J  2474     BAL 2278.                                                                       
07256+2030   STF1083     H 3  48.                                                                MEv2010 
07257+2748   OCC 132     NPOI Limb-darkened diameter  2.390 +/- 0.024 mas, Sp = G8III,           NOI2018 
                         R = 9.48 +/- 0.12 \rsun, Teff = 5072 +/- 68 K, L = 53.7 +/- 2.8 \lsun,          
                         M = 2.09 +/- 0.10 \msun, Age = 0.96 +/- 0.15 Gyr.                               
07257+0022   BAL1095     J 2630.                                                                         
07260+2205   AG  140     HO 628.                                                                         
07260+1406   STF1088     Same as STF1078. Herschel reports a closer (4") pair. Unconfirmed.      HJ_1836 
07260-0215   TOK 117     HIP 36071. The position measurement in the V-band is of low accuracy.           
                         The status of the B-companion remains uncertain.                        Tok2011a
                         A has small PM, crowded field, B can be optical.                        Tok2014d
07261-2515   EVS   3     Classical Cepheid SS CMa.                                                       
07262+3749   ALI 834     Two recent observations show this object to be single.                          
                         Hipparcos suspected non-single.                                                 
07264+6929   STF1059     AB = LDS1650.                                                                   
07265+0923   J  1064     J  2631.                                                                        
07267+7144   MLR 408     Also known as HDS1044.                                                          
07269+2015   CHR  26     61 Gem. An occultation and spectroscopic binary, now resolved.                  
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.90 +/- 1.65, 5.20, and 1.35 Msun, respectively.             Mlk2012 
07269-0932   RST4362     J 2819.                                                                         
07270+7901   MLR 495     Also known as HDS1046.                                                          
07270-3419   HJ 3969     LDS 182. B is CD-34@3610.                                                       
                         See Allen et al. (2000) for information on metallicity, age, galactic   AlC2000 
                         orbital parameters, etc.                                                        
                         HIP 36165. B = HIP 36160.                                                       
                         A and B both show variable RV, and are possible SBs, but Aa,Ab is not   Tok2010d
                         resolved with NICI. A,B are below MS.                                   Tok2014d
07272+0817   BUP 101     bet CMi = 3 CMi = Gomeisa. A is a spectroscopic binary. Variable?               
             DAL  32FH   Identified as DAL  41 by author, but 06149-0617, too. Redesignated      Dal2008c
                         by author.                                                              Dal2014b
07273+1138   BPM 390     [PM2000]  760960 + [PM2000]  760940.                                    Gvr2010 
07273-1130   HJ  759     AC: 07273-1130 and 07276-1129 were found to share primaries. Systems            
                         were moved, using the more correct WDS designation.                             
07273-2355   ARA2050     Open (galactic) cluster Trumpler 7.                                             
             I   770     OW: Primary of 07274-2356 found to be O component of 07273-2355.                
             ARA2052     PX: Primary of 07274-2357 found to be P component of 07273-2355.                
07274+1519   STF1094     H N 108.                                                                MEv2010 
07275-2047   ARG  17     B is BD-20@1949.                                                                
07276-1830   S   550     B is BD-18@1847. Spectral type B8I.                                             
07277+2208   S   548     AC: H 5  66.                                                            MEv2010 
07277+2127   MCA  30     Aa,Ab: 63 Gem. A is an SB and occultation triple, with the wider pair,          
                         presumably, now resolved.                                                       
                         First detected as an occultation binary by Eitter & Beavers             Bvr1977 
                         Mason et al. (1997) orbit gives good fit to speckle/Hipparcos, but      Msn1997a
                         implausibly large masses even for a multiple system.                            
                         HIP solution spurious. Fekel (1986 private communication) detected              
                         this system as a third component in the spectrum and made a                     
                         preliminary estimate of the period of 760 days. A combined                      
                         spectroscopic/speckle orbit was later undertaken in collaboration               
                         with Fekel. This solution includes a mass determination.                        
                         Aa,Ab: Combined spectroscopic/astrometric solution, yielding masses             
                         2.583 +.- 0.059 and 1.030+/- 0.038 Msun for Aa and Ab, respectively,            
                         and a parallax of 30.22 +/- 0.26 mas.                                   Mut2010d
             63 Gem      Aa1,Aa2: Spectroscopic binary detected as submotion in orbit of Aa,Ab           
                         pair. Derived masses are 1.402 +/- 0.032 and 1.181 +/- 0.027 Msun       Mut2010d
             SHJ 368     AB: Aa component of this multiple system is a 1.9d SB2; estimated               
                         period of the AB pair is 26,000y; period of the AD pair ~760y.          Tok2006 
                         AB: H 5  53.                                                            MEv2010 
             HDS1050     AD not seen in the 2MASS K-band image, not confirmed with RoboAO.       Tok2014d
07279-1133   BU  332     Spectrum: G8Ib-II+B+B8V. Variable?                                              
07279-1853   RST2477     TDS4830.                                                                        
07280+0657   BU   21     eta CMi = 5 CMi                                                                 
07282+0856   LAM   4     gam CMi = 4 CMi. A is a spectroscopic binary.                                   
07282+0035   BAL1098     J 1997.                                                                         
07282-2011   BHA   5     CPD-19@2220.                                                                    
07283+1750   BPM 391     [PM2000]  763796 + [PM2000]  763844.                                    Gvr2010 
07286-2627   B  2628     Also known as WFC  55.                                                          
07287+2439   STTA 85     B is BD+24@1666.                                                                
07287+2151   OCC1064     Aka OCC9029.                                                                    
07287-1349   STF1101     Aka ITF  79.                                                                    
07288-4432   DON 186     CPD-44@1586.                                                                    
07289+4811   KUI  30     A may be a long-period spectroscopic binary.                                    
07289-3015   HDS1054     GJ 2060 = V372 Pup.  Daemgen et al. (2007) derive a distance of 15.8    Dae2007 
                         +/- 2.3 pc, a separation of 2.8 +/- 0.4 au, and a predicted orbital             
                         period of 6 +/- 1 y. Spectral types are M0.5 +/- 0.5 and M1.5 +/- 1.0;          
                         masses are 0.59 +/- 0.05 and 0.52 +/- 0.08 Msun.                                
07291+3147   A  2124     62 Gem = rho Gem. A is a spectroscopic binary.                                  
                         G090-001. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         CHARA Array Limb-darkened diameter  0.853 +/- 0.014 mas,                CIA2012e
                         R =  1.655 +/- 0.028 \rsun, L =  5.542 +/-0.089 \lsun,                          
                         Teff = 6899 +/-  63 K, M = 1.355 +/- 0.013 \msun,                               
                         Age =  2.1 +/- 0.2 Gyr.                                                         
             ALC   3     age, galactic orbital parameters, etc.                                          
                         AE: NLTT 17908/17907                                                    Chm2004 
                         AE: HJL1047.                                                            HJL1986 
                         AE: SHY  41. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
07292+1424   BPM 392     [PM2000]  766616 + [PM2000]  766809.                                    Gvr2010 
07292+1421   STTA 86     B is BD+14@1676.                                                                
07292-4318   DUN  51     sig Pup. LDS 186. A is a spectroscopic binary.                                  
             sig Pup     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Wilson (1917).                                                          WRE1917 
07294-1500   STF1104     A premature orbit has been computed for AB.                                     
                         AD: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             TOK 391     Ca,Cb: This is another nearby multiple system. The main component HIP           
                         36395 is a visual binary with a known 728yr orbit, also measured here.          
                         The C component (NLTT 17952) at 20".4 is physical, and yet another CPM          
                         component F is found at 1072" (Tokovinin & Lepine 2012), while the WDS  Tok2012c
                         components D and E are optical. We observed C and resolved it at                
                         0".09. The orbital period of Ca,Cb is on the order of 6yr, estimated            
                         masses are 0.6 and 0.4 Msun. We also targeted F and did not resolve             
                         it. The magnitudes and colors of C and F are quite similar.             Tok2015c
             STF1104     AD: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
07294-7503   HJ 3991     B is CPD-74@444.                                                                
07295+3448   STT 172     BDS 4152, HJ 3295 same star.                                                    
07295-3807   RSS 132     HIP 36414. A is an SB without orbit, dRV= 1.2*.                         Nrd2004 
07295-7323   RSS   8     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
07297-0242   BAL 173     BAL 172 is a close pair. B of BAL 173.                                          
07298+2755   MCA  31     65 Gem. A is a spectroscopic binary, now resolved by speckle                    
                         interferometry.                                                                 
                         1988.2520: The measurement resulting from the original analysis of              
                         this observation was rejected prior to publication.  Our reanalysis of          
                         the observation by new techniques yielded a quite good result however.  Hrt1992b
07299+4940   ENG  31     22 Lyn.                                                                         
07300-0446   J  1490     J 2827.                                                                         
07301-4509   CPO 159     CPD-44@1605.                                                                    
07303-5657   FIN 105     Ma,Mb = 1.35  +/- 0.13 , 1.33  +/- 0.13  \msun.                         GmJ2022 
07304+1352   STF1102     AB: HJL  84.                                                            HJL1986 
                         AD: HJL1048.                                                            HJL1986 
                         AD: SHY 191. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AD: Halbwachs et al. (2012): SB1 orbit of D, P=2708.2d, e=0.716,        HJL2012b
                         K1=4.93, V0=-2.38 => M2min=0.27.  D co-moving with HIP 33818 at 6.0pc.  Tok2014d
                         BD: HJL1049.                                                            HJL1986 
             TOK 392     Da,Db: This is a quadruple system. The 7".7 AB pair (STF 1102) is               
                         HIP 36485, the CPM component D = HIP 36497 = HD 59450 is located at             
                         112" from it, while the WDS components C and E are optical. The                 
                         physical nature of AD is established by common PM, distance, and RV.            
                         D is a known SB1 with P=2708d=7.4yr (Halbwachs et al. 2012, MNRAS 422,          
                         14) and an estimated semi-major axis of 93mas, also an acceleration             
                         binary. We resolved the Da,Db pair at 0".11, dI=2.6. The minimum mass           
                         of Db derived from its SB orbit is 0.27 Msun, while we estimate the             
                         masses of Da and Db as 1.05 and 0.6 Msun from their luminosity. A               
                         previous non-resolution of D is reported in INT4; it was also           RAO2015 
                         unresolved with Robo-AO (Riddle et al. 2015).                           Tok2015c
07305+0743   A  2869     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.46 +/- 2.07, 4.05, and 1.82 Msun, respectively.             Mlk2012 
07307+4813   GIC  75     G107-069/G107-070 = GJ 275.2AB.                                                 
                         Quadruple. The two close pairs are separated by 103". The G107-070              
                         orbit depends upon elongations of blended photographic images. While            
                         Harrington et al. (1981) do not determine a value for the semimajor     Hrr1981 
                         axis for the close pair, they do determine a period (0.94y), masses of          
                         individual components (0.17 and 0.08 Msun), and distance to the system          
                         (parallax = 0."0896). Application of Kepler's Law yields a = 0."054.            
                         This agrees well with the statement in Harrington et al. that "The              
                         mean separation of the double would be of order 0.05 arcseconds".               
             WNO  49     Ba,Bb: GL 275.2B.  White dwarf pair = EGGR 52AB.                        Grn1986 
07308+0418   BAL2771     Baillaud thought A had a closer companion. Not found by Heintz.         Hei1995 
07309+3034   DOM   1     C is BD+30@1520.                                                                
07309+2441   HJ  424     AC: POU2819.                                                                    
                         AB: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
07309+0030   J  1998     BAL 1102. RST 5264.                                                             
07312+0210   TOK 393     HIP 36557 = HD 59688. According to observations by D. Latham (2012,             
                         private communication), this is a spectroscopic triple with an inner            
                         period of 70d (double-lined, also detected by GCS, mass ratio 0.7) and          
                         an outer period of 2007d or 5.5yr. The outer system is also detected            
                         by astrometric acceleration (Makarov & Kaplan 2005). We resolve it      Mkr2005 
                         here at 0".057, dI=2.0, dy=2.5 mag, and see the orbital motion. The             
                         estimated mass of Ab is 0.88 Msun. The semi-major axis of the 70-d              
                         inner binary Aa,Ab is 7mas, so accurate measurements of AB can detect           
                         the sub-motion to determine the orientation of the inner orbit.         Tok2015c
07312-1215   BRT2673     Error in transcribing to catalog - WDS designation should be -13 deg.           
07312-2110   BRT 317     CPD-20@2532.                                                                    
07314+3528   HJ 3293     ALI 108.                                                                        
07316+1521   BPM 393     [PM2000]  773583 + [PM2000]  773528.                                    Gvr2010 
07317-3553   JSP 167     A is a spectroscopic binary and ellipsoidal variable, PS Pup.                   
                         BC is CPD-35@1289.                                                              
07318+1705   RBR  16     CHARA Array Limb-darkened diameter  1.106 +/- 0.011 mas,                CIA2008c
                         R = 11.62  +/- 0.34  \rsun.                                                     
07319+3613   LDS6206     Ross 989, VYS 246. Component A is VV Lyn, so designated because of              
                         starspots, later also found to be a flare star. Spectrum of B dM4.5e.           
                         Period is about 16.3d with a amplitude of 0.06 mag. Component B is      Skf2019g
                         BL Lyn, period about 17.6d with an amplitude of 0.06 mag.                       
                         AB: NLTT 17999/17998                                                    Chm2004 
07319+1237   BPM 394     AB: [PM2000]  774510 + [PM2000]  774601.                                Gvr2010 
07319-6142   TOK 364     First resolution; estimated period 85 yr.                               Tok2013b
07320+1816   LDS3746     NLTT 18016/18017                                                        Chm2004 
07320+1720   WOR  27     AB: Vyss 498. Incorrect coordinates in Worley (1962) led to this pair   Wor1962a
                         being also entered in the WDS as 17280+1734WOR  39.                             
07320-0841   STF1111     Spectrum composite; A+G.                                                        
07321-0853   STF1112     H 4  26.                                                                MEv2010 
07321-5615   BRT2535     SWR  29.                                                                        
07322+1446   BPM 395     [PM2000]  775343 + [PM2000]  775307.                                    Gvr2010 
07322+0407   J  2634     BAL2772.                                                                        
07323-0431   J  2831     Not found by Heintz at IDS position.                                    Hei1990b
07325-3858   B  1550     Spectrum: A3/5mA7-F2.                                                           
07326-0250   BAL 176     J 2832.                                                                         
07326-1253   STF1115     B is BD-12@2017.                                                                
07327+1025   HJ   55     BC: incorrectly added as AC.                                                    
07327+0540   ARG  67     B is BD-05@1702.                                                                
07328+2253   STF1108     Spectroscopic binary. Spectrum: K0II-III+F8V.                                   
07328-0230   BAL 177     J 1494.                                                                         
07328-2048   RUC  20     Primary is TY Pup.                                                              
07330-2820   B  2631     The classification is from Garrison et al. (1977 ApJS 35, 111).         Msn1998a
07330-5510   HJ 3984     AC measure of 1938.1 made by a transit interferometer.                  CpP1938c
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
07331-5756   LPO   9     Spectral type A2?                                                               
07332+1246   BPM 396     [PM2000]  777962 + [PM2000]  777988.                                    Gvr2010 
07335+3859   BRT2217     ALI 1083.                                                                       
07335-3056   BRT3281     A likely plate flaw.                                                    Grv2021b
07336+3458   BRT3248     ALI 109.                                                                        
07336+1550   MCA  32     68 Gem.                                                                         
07337-1509   A  3091     RST gives magnitudes as 9.2-9.6.                                                
07340-0142   J  1496     BAL 481.                                                                        
07341-5050   HJ 3986     B is CD-50@2840.                                                                
07342-5045   BRT 713     CPD-50@1299.                                                                    
07343+0322   J  2835     del 3 CMi = 9 CMi.  BAL2296.                                                    
07343-2328   H N  19     A is a spectroscopic binary. Spectrum of B: F5/7V.                              
                         Toyota et al. (2009) monitored the RV of both the A and B components            
                         every 1-2 months between 2003 Mar - 2007 Nov, using a high-dispersion           
                         echelle (precision ~10 m/s). The A star showed large RV variation; the          
                         associated body is expected to be massive; however, orbital period is           
                         longer than their observational span, so orbital elements could not be          
                         determined. The B star exhibits rapid rotation, so RVs could not be             
                         measured to high precision.                                             Toy2009 
07345+1713   BPM 397     [PM2000]  781743 + [PM2000]  781683.                                    Gvr2010 
07345-1352   DOO  42     Slightly variable.                                                              
                         AD: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AD: Rectilinear solution by Hurowitz et al. (2013).                     USN2013a
07345-5258   LTT 2891    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
             TOK 118     HIP 36832. A is SB without orbit, dRV= 6.7.                             Nrd2004 
                         This is a new triple system. The A component is a PMS star in SIMBAD,           
                         chromospherically active, X-ray source. Both components are on the MS,  TrC2006 
                         however. See Torres et al. (2006). A is chromospherically active.       Tok2011a
                         A is SB and astrometric binary, P=0.761y, e=0.257, a=17.54mas =>        HIP1997d
                         M2=0.93) Aa,Ab should be double-lined and resolved by speckle, but              
                         unresolved at SOAR.                                                     Tok2014d
07346+3153   STF1110     alp Gem = 66 Gem = Castor. STFB  4. According to R.G. Aitken, this was  A__1935f
                         discovered in 1719 by Bradley and Pound. Mt. Wilson spectral types      Bdy1832A
                         A2,A2,M1. A and B are both SB1's with P = 9.21 d and 2.93 d.            Pnd1832A
                         Castor A is also reported to exhibit x-ray and radio emission.                  
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Star C (mag. 9.1, M1Ve) is the spectroscopic and detached eclipsing             
                         binary YY Gem (P = 0.81 d), 70" from the center of AB and in slow               
                         retrograde motion (cf., Heintz), so the object is sextuple.             Hei1960a
                         AB: H 2   1.                                                            MEv2010 
                         AB: Additional notes may be found in Fu et al. (1997)                   McA1997 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 5.43 +/- 0.97, 4.27, and 4.28 Msun, respectively.  Mlk2012 
                         Components Aa, Ab, Ba and Bb determined to have masses of 2.74+/-0.11,  Ana2015 
                         0.37+/-0.09, 2.26+/-0.10 and 0.53+/-0.09 \Msun, respectively.                   
                         Aa,Ba MYSTIC uniform disk dia. = 1.271 +/- 0.012, 0.994 +/- 0.014 mas.          
                         Aa,Ba MIRC-X uniform disk dia. = 1.273 +/- 0.003, 1.005 +/- 0.008 mas.          
                         Aa,Ab masses = 2.371 +/- 0.015, 0.3859+/- 0.0018 \msun.                         
                         Ba,Bb masses = 1.789 +/- 0.016, 0.3865+/- 0.0020 \msun.                 CIA2022d
                         Many historic AB measures corrected and missing measures added.         CIA2022d
07348+1643   BPM 398     [PM2000]  782626 + [PM2000]  782652.                                    Gvr2010 
07349-2010   BRT 320     CPD-19@2360.                                                                    
07351+3058   STT 175     AB: Using the Hipparcos parallax, the mass sum is found to be 3.00 +/-          
                         0.98 Msun; mass assumed equally divided between A and B components.     Mut2010d
             HR 2896     Ba,Bb:  Close pair seen as trend in solution of AB pair. Impossible to          
                         tell which component of AB pair contains the astrometric subsystem;             
                         selection of the secondary was arbitrary. Estimated masses are 1.3 and          
                         0.2 Msun. The low-mass companion is likely an M dwarf in either a               
                         nearly planar or anti-planar orbit to the wide binary.                  Mut2010d
07351-2830   GC 10171    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
07354-0559   SCJ   6     B is BD-05@2176.                                                                
07354-2822   SHY 512     AD: HIP  36917 + HIP  36890.                                                    
             HJ 3982     AB and BC: Additional notes may be found in Herschel (1847).            HJ_1847a
07354-7417   HJ 3997     A is a spectroscopic binary.                                                    
07356+5212   MLR 670     Also known as HDS1073.                                                          
07357+4303   MAD   3     Called MA 2 in BDS and ADS. MA 2 is 05214-0653.                                 
07359+2654   BUP 103     ups Gem = 69 Gem. Variable?                                                     
07360+1735   BRT3282     A likely plate flaw.                                                    Grv2021b
07360-0147   BAL 484     J 1499.                                                                         
07361+3650   ES 2157     Van Biesbroeck 1944 measure is of BD+37 1743; he questions Espin's      VBs1954 
                         identification.                                                                 
                         Quadrant uncertain. Espin's measures erroneous.                         B__1962d
07362+3250   UC 1599     CPM candidate confirmed physical by photometry (2MASS and V mags).      Tok2013c
07364+1530   BPM 399     [PM2000]  786846 + [PM2000]  786888.                                    Gvr2010 
07364+0705   HEN   3     Delta-M is in K band.                                                           
                         LSPM J0736+0704 = NLTT 18152. Law et al (2008) derive a distance of     Law2008 
                         7.3 +3.9/-1.3 pc and a projected separation of 6.5 +3.5/-1.1 au.                
                         Estimated spectral types are M4.5 and M5.                                       
                         GJ 3454. Estimated age 1000-10000 Myr; masses 0.18 +/- 0.03 and 0.14            
                         +/- 0.01 Msun; a ~5.8 au.                                               Jnn2014 
07364-6152   RST3538     Includes V455 Car, an Algol-type eclipsing binary, P = 5.13298d.        Zas2012 
07365+8238   LDS1652     NLTT 17909/17910                                                        Chm2004 
07366-1429   STF1121     AB: B is BD-14@2021.                                                            
                         AB: H 2  63.                                                            MEv2010 
07368-1434   RAS  23     Giant silicon star, tpye B8; companion estimated as early-F.            Ras2014 
07368-1555   RST3530     Spectrum: Fm delta Del.                                                         
07370-2016   WHC   5     Aka ARA 969.                                                                    
07371-0254   OL  155     Aka SLE 802.                                                                    
07373-0407   BUP 104     25 Mon. A variable? C is BD-03@1978.                                            
07374+1215   HJ   60     Aka J  2483. Large position error for HJ identification.                        
07374-3458   FIN 324     f Pup. It was resolved as 0.2" binary FIN 324AB in 1954.31 by Finsen            
                         (1956) using double-slit interferometer at the 0.7 m Innes refractor.   Fin1956a
                         The components were comparable in brightness with dm from 0.3 to 0.6.           
                         Finsen published 7 mean positions resulting from 25 nights (the last            
                         one in 1960.26). His measures show considerable scatter; the motion             
                         looks erratic rather than regular. Finsen could not resolve AB since            
                         1960.29, despite repeated attempts. However, on 1963.305 he found               
                         another companion C at 0.52" with dm =0.8. In fact W. van den Bos saw   Fin1964a
                         both companions earlier and measured AB and AC simultaneously in                
                         1956.2 and 1959.7 (van den Bos 1957, 1961). AC was measured later by    B__1957b
                         R.H. Wilson, Hipparcos, and various speckle interferometers. All        B__1961a
                         speckle observations show no trace of the subsystem AB, except the one          
                         on 1989.305 where B looks doubtful and much fainter than C (McAlister   McA1990 
                         1990). No trace of B was seen at SOAR in 2008-2011 (4 speckle runs).            
                         AC follows a Keplerian orbit with 81 yr period (Hartkopf et al. 2012)   Hrt2012a
                         which was slightly corrected here using the latest measure. This                
                         excludes confusion between the companions (i.e. B and C being the same          
                         star). Besides, both were measured concurrently by van den Bos.                 
                         The companion B cannot be real. The closest separation of AC is 0.09"           
                         according to the orbit and excludes any sub-system with comparable              
                         separation because such a triple star would be dynamically unstable.            
                         The fact that the orbit of AC is known does not allow us to explain the         
                         apparent non-hierarchical configuration by projection. If B were real,          
                         its orbital period would be on the order of 10 yr (scaling from the             
                         orbit of AC) and it would have shown up in our speckle data. Like 104           
                         Tau, we have here a binary which actually is not binary, but a ghost.   Tok2012b
                         AB,C: Malkov et al. (2012) derive dynamical, photometric, and                   
                         spectroscopic masses 6.74 +/- 1.03, 4.81, and 3.09 Msun, respectively.  Mlk2012 
07375-0202   HO  244     There are two distant companions: 13 mag star P=195deg, dist 34";               
                         9 mag star P=109deg, distance 69".                                      Ho_1890 
07376-1426   S   557     B is BD-14@2052.                                                                
07378+1409   BPM 400     [PM2000]  790698 + [PM2000]  790531.                                    Gvr2010 
07378-0236   A   534     AB,C: Rectilinear solution by Hartkopf et al.  (2012).                  Hrt2012a
07379+7745   MLR 478     AB: Also known as TDS 388.                                                      
07379+1637   BPM 401     [PM2000]  790950 + [PM2000]  791037.                                    Gvr2010 
07379-6026   HJ 3993     CD-60@1821.                                                                     
07380+1802   BPM 402     [PM2000]  791141 + [PM2000]  790925.                                    Gvr2010 
07380-3208   B  1554     Additional companion seen which may be a ghost. The measures of         B__1956a
                         van den Bos and Finsen of this alleged companion are X coded.           Fin1951a
07382+1752   HJ 2404     A measure of A and BD+18@1692.                                                  
             SLE 433     AE: Soulie (1986) measure in error, apparently due to typo in right             
                         ascension of secondary.                                                 Sle1986a
07383+4745   MET   6     Metchev & Hillenbrand say the pair is probably optical, based on                
                         proximity.                                                              Met2004b
07383-2522   B   731     Duplicity still not certain. Needs speckle.                                     
                         PU Pup, an eclipsing binary of Beta Lyr-type, period 2.57895 day.       Zas2013 
                         Likely a spurious pair. Last measured 1966 and unresolved by SOAR on 5          
                         occasions 2009-2015.                                                    Tok2010 
                                                                                                 Tok2012d
                                                                                                 Tok2012b
                                                                                                 Tok2014a
                                                                                                 Tok2015c
                                                                                                 Tok2016a
07383-2524   I   778     CPD-25@2621.                                                                    
07384+3644   LMP   5     AC: Due to the large proper motion of the primary, a 1964 measure of    Pws1993 
                         the AB pair was incorrectly identified as a new component and labelled          
                         LMP   5AC.                                                                      
07384-4743   HJ 3990     B is CD-47@3192.                                                                
07385+3503   BU  200     70 Gem. AC: H VI 70.                                                            
                         AB: H 6  70.                                                            MEv2010 
07385+2400   POU2850     A 2.4" possible companion to 2MASS J07382951+2400088 is noted in the            
                         WDS, but our AstraLux images show no such companion.                    Jnn2012 
07386-5438   UC 1601     CPM candidate does not pass photometry test; likely optical.            Tok2013c
07387-0127   HO  245     B component spectral type GIII                                          AbH2000 
                         AB: Additional notes may be found in Hough (1890).                      Ho_1890 
07388+4925   LAW  15     LSPM J0738+4925 = NLTT 18181. Law et al (2008) derive a distance of     Law2008 
                         19.5 +8.9/-3.7 pc and a projected separation of 4.9 +2.9/-0.6 au.               
                         Estimated spectral types are M4.5 and M5.                                       
07388-0126   HO   35     Also known as RST4859.                                                  Dam2012 
07388-2648   H 3  27     H III 27. Both components suspected variables.                                  
07389+4229   STTA 87     B is BD+42@1745.                                                                
07389+0421   BAL2781     J 2484.                                                                         
07389-2016   BU  201     Listed in the IDS notes as ARG 47a, but in the ADS as BU  201.                  
07393+0514   SHB   1     alp CMi = 10 CMi = Procyon. Proper motion of A -710 -1023 (FK5).                
                         In 1868.17, Searle suspected seeing two faint companions on two                 
                         nights, "one about 7" n, the other about as far f".                     Sea1882 
                         Strand (1951) orbit utilizes radial velocities.                         Str1951 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Irwin et al. (1992).                                                    Irw1992b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.03 +/- 0.05, 1.44, and 1.27 Msun, respectively.  Mlk2012 
                         Most likely age of system is 1.87+/-0.13 Gyr. Procyon B progenitor mass Lie2013 
                         is 2.59(+0.44)(-0.26) Msun.                                                     
                         AB: Bond et al. (2015) position angles published for J2000 equinox;     BdH2015 
                         theta precessed back to epoch of observation.  Bond et al. derive               
                         masses 1.478 +/- 0.012 and 0.592 +/- 0.006 Msun.                                
                         B: Teff = 7740 +/- 50 K, R = 0.01232 +/- 0.00032 \rsun, M = 0.592 +/-   BdH2017b
                         0.006 \msun. Sp = DQZ.                                                          
                         Intensity Interferometer Limb-darkened diameter of A 5.50 +/- 0.17 mas. HBr1974 
                         Mk III Limb-darkened diameter  6.44  +/- 0.25  mas.                     MkT1988 
                         Mk III Limb-darkened diameter  5.46  +/- 0.08  mas.                     MkT2001 
                         Mk III Limb-darkened diameter  5.446 +/- 0.054 mas.                     MkT2003 
                         NPOI Limb-darkened diameter    5.43  +/- 0.07  mas.                     NOI2001b
                         Spectral type of secondary: DQZ6.5.                                     Hbg2013 
             LAM   6     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             DIC   1     AD: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             D    29     AE: Additional notes may be found in Dembowski (1883).                  D__1883 
                         AE: Rectilinear solution by Mason & Hartkopf (2015).                    Msn2015a
             SLE 439     AF: Rectilinear solution by Mason & Hartkopf (2015).                    Msn2015a
             SMR  11     AG: Rectilinear solution by Mason & Hartkopf (2015).                    Msn2015a
07393-3826   B  1557     CPD-38@1481.                                                                    
07397+1305   CRZ   3     LSPM J0739+1304 + 2MASSI J0739438+130507. Secondary is M8 brown dwarf.  Crz2007 
07397+0117   A  2532     Rapid motion.                                                                   
07397-2250   BRT1426     CD-22@4893.                                                                     
07397-3808   I   160     d 2 Pup                                                                         
07398+0516   BRD   2     The A component is the E of 07393+0514.                                         
07398-3235   HD  61827   LS 640. The classification is from Houk & Cowley (1975, Michigan                
                         Spectral Catalogue, vol. 1).                                            Msn1998a
07399-2231   BRT1428     CD-22@4899.                                                                     
07400-0336   BGH   3     B is BD-03@2002.                                                                
                         NLTT 18257/18260                                                        Chm2004 
07400-2453   I   779     CPD-24@2670.                                                                    
07401+0514   STF1126     One component is a spectroscopic binary.                                        
                         AB: H 1  23.                                                            MEv2010 
07402-1724   VBS  41     AB. LUY 745-46A. Van Biesbroek (1974) gives average of 5 measures       VBs1974 
                         obtained over 4 years, notes "little change". It is assumed he was              
                         observing the A component of the 20" LUY6207 pair.                              
             LDS5693     AC. LUY 745-46A+B. Aka LUY6207.                                         Luy1950b
                         NLTT 18271/18270                                                        Chm2004 
07404-1806   SLE 820     TDS5044 (merged 2008/06/25)                                                     
07405+4136   LDS6208     NLTT 18248/18247                                                        Chm2004 
07406+1213   BPM 403     [PM2000]  797667 + [PM2000]  797678.                                    Gvr2010 
07410+2148   VAS  14     VSK   8.                                                                        
07411+1323   BPM 404     AB: [PM2000]  799003 + [PM2000]  798850.                                Gvr2010 
             BPM 405     AC: [PM2000]  799003 + [PM2000]  799074.                                Gvr2010 
             BPM 406     BC: [PM2000]  798850 + [PM2000]  799074.                                Gvr2010 
07414-8555   HJ 4086     B is CPD-85@138.                                                                
07415-4223   GRV1252     Both A and B have approximately the same radial velocity.               Grv2019b
07417+3726   STT 177     Both the Postmas (1963) and Couteau & Laques (1965) orbits depend       Pma1963 
                         on the isolated measures by van den Bos in 1962.                        Cou1965a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 6.29 +/- 5.43, 3.42, and 1.00 Msun, respectively.             Mlk2012 
07417+0942   STF1130     A premature orbit has been computed. Needs speckle.                             
07417+0319   J   283     Also known as DJU   9.                                                          
07418-7236   DUN  57     zet Vol                                                                         
07419+3709   BRT2218     ALI 582.                                                                        
07419+1703   BPM 407     [PM2000]  800895 + [PM2000]  800833.                                    Gvr2010 
07419+0449   SLE 448     Aka BAL3007a.                                                                   
07420+3655   ES 2158     AB: Also known as COU2072.                                                      
                         BD+37 1757. A found to be double, mags become 11.1 and 11.4. There is           
                         no star in the position given in ADS.                                   VBs1954 
07421+0348   GIC  76     G050-002/G050-003.                                                              
07421-2407   CPD   4     B is CD-23@5971.                                                                
07422-0331   STF1132     B is BD-03@2018.                                                                
                         H 4  96.                                                                MEv2010 
07426-1824   JRN  35     AB and AC: SLE 827.                                                             
07427+3400   CIA  30     Ma,Mb = 1.629 +/- 0.023, 1.443 +/- 0.020 \msun.                                 
                         Ra,Rb = 2.53 +/- 0.10, 1.51 +/- 0.06 \rsun.                                     
                         Teff_a,Teff_b = 6390 +/- 180, 6610 +/- 230 K.                                   
                         La,Lb = 9.6 +/- 1.3, 4.1 +/- 0.5 \lsun. distance = 64.4 +/- 0.3 pc.     CIA2022e
07427+1659   BPM 408     [PM2000]  802827 + [PM2000]  802979.                                    Gvr2010 
07427+0110   DOB   8     BAL 1411.                                                                       
07429+6517   HU  843     Same as HEI 132, misidentified by Hussey                                Hei1985a
07430+5843   HJ 2405     24 Lyn.                                                                         
07430+5110   GIC  66     G193-059/G193-060. LDS6209. Typographical error led to this pair being          
                         originally entered in the WDS as 06432+5113.                                    
07430+2327   BLL  22     A is the Mira-type variable, S Gem.                                             
07430-1704   HU  710     Malkov et al. (2012) derive dynamical and spectroscopic masses                  
                         2.88 +/- 1.72 and 2.46 Msun, respectively.                              Mlk2012 
07430-4511   WSI  99     Provisionally designated WSI9104.                                       Tok2010 
07431+1638   BPM 409     [PM2000]  803873 + [PM2000]  803792.                                    Gvr2010 
07431+0011   B  2526     The bright component is B. Distance 0".12; occasionally the star image          
                         was not quite round, but too close to measure.                          Vou1947b
07433+2853   BLL  23     sig Gem = 75 Gem. A is a spectroscopic binary and variable.                     
                         NPOI Limb-darkened diameter 2.31 +/- 0.05 mas,                          NOI1999 
                         R =  9.3 +/- 0.3 \rsun.                                                         
             CIA   7     Aa,Ab: Roettenbacher et al. (2015) resolve the RS CVn binary sig Gem            
                         and determined a combined spectroscopic/astrometric orbit. The orbital          
                         parallax is 25.8 +/- 0.4 mas (38.8 +/- 0.6pc), flux ratio in H is               
                         270 +/- 70, primary radius is 10.1 +/- 0.4 Rsun, primary luminosity             
                         39 +/- 2 Lsun, the system age 5 +/- 1 Gyr. Derived masses are                   
                         1.28 +/- 0.07 and 0.73 +/- 0.03 Msun.                                   CIA2015b
                         NPOI Limb-darkened diameter    2.260 +/- 0.030 mas,                             
                         R =    8.96 (+/- 0.16   )  \rsun,  Teff = 4267 +/-  31 K,                       
                         L =   33.2 +/-   0.8 \lsun.                                             NOI2023 
07435+0329   TOK 355     Aa,Ab: SB1, P=34.8y.                                                    Tok2014d
             STF1134     AB: HJL  85.                                                            HJL1986 
07435-2825   SEE  85     1 Pup.                                                                          
07437-0004   HJ 2413     G112-043/G112-044. See Allen et al. (2000) for information on           AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
                         NLTT 18347/18346                                                        Chm2004 
07437-3706   JSP 179     CPD-36@1566.                                                                    
07441+1713   BPM 410     [PM2000]  806370 + [PM2000]  806526.                                    Gvr2010 
07441-1656   HU  844     V611 Pup, Algol-type eclipsing binary, P = 6.3177 d.                    Zas2011 
07442-5027   DUN  55     B is CD-50@2948.                                                                
                         SHY 195. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
07443-0040   BAL 825BC   Optical/physical nature ascertained from Gaia DR2.                      FMR2019b
07444+2424   STT 179     kap Gem = 77 Gem                                                                
                         NPOI Limb-darkened diameter  2.378 +/- 0.025 mas, Sp = G8III,           NOI2018 
                         R =11.00 +/- 0.16 \rsun, Teff = 5020 +/- 68 K, L = 69.3 +/- 3.7 \lsun,          
                         M = 2.58 +/- 0.09 \msun, Age = 0.58 +/- 0.08 Gyr.                               
07444+0358   J  1999     aka BAL2783.                                                            Dam2016b
07445-2350   BRT2917     CPD-23@2752.                                                                    
07445-2351   ARA2067     This, and ARA 2068 may be more distant companions of I 780.                     
07446+1707   BPM 411     [PM2000]  807720 + [PM2000]  807817.                                    Gvr2010 
07447+1231   BPM 412     [PM2000]  807903 + [PM2000]  808122.                                    Gvr2010 
07448-3344   STN9001     Previously known as STN  60 1/2.                                                
                         Rectilinear solution by Hartkopf et al.  (2012).                        Hrt2012a
                         Despite the linear solution, proper motion and parallax favor a         Grv2020a
                         physical connection. Long period and/or high eccentricity possible.             
07449+0349   BAL2784     J 2486. J 2000.                                                                 
07451-4248   CPO 169     CPD-42@1599.                                                                    
07453+2802   BU  580     bet Gem = 78 Gem = Pollux                                                       
                         AB, AE, and AG: Optical pairs, based on study of relative motion of             
                         the components using the method of apparent motion parameters.          Kiy2008 
             H 6  42     AC: H VI 42.                                                                    
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             STFB  5     F is BD+28@1465.                                                                
                         AF: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             BU  580     AB, AE, AG: Rectilinear solutions by Hurowitz et al. (2013).            USN2013a
             H 6  42     AC: Rectilinear solution by Friedman et al. (2012).                     USN2012a
07453-3812   BRT1610     Also known as DAW 193.                                                          
07454+1739   BPM 413     [PM2000]  809466 + [PM2000]  809614.                                    Gvr2010 
07454+1657   BPM 414     [PM2000]  809532 + [PM2000]  809629.                                    Gvr2010 
07454+1540   BPM 415     [PM2000]  809579 + [PM2000]  809412.                                    Gvr2010 
07455-1441   STF1138     2 Pup. B is the eclipsing binary PV Pup, and is BD-14@2193.             Fen1929 
                         AB: H 4  91.                                                            MEv2010 
07456-3410   RAG   6     AB: B = GJ 288B, white dwarf, PM(B)=(-246,+1654) (Holberg et al 2002).  Hbg2013 
                         B is binary?                                                            Tok2014d
             TOK 193     Triple system at 15 pc. The inner astrometric pair with large dmu is            
                         resolved with speckle. It is accompanied by the white dwarf NLTT 18414          
                         = GJ 288B at 914".                                                      Tok2012a
                         Astrometric binary; dm 4.0 mag, period ~ 10y? Accelerated pm, SB        Tok2012b
07457-2147   ARA1397     A likely plate flaw.                                                    Grv2021a
07458+7749   STF1100     Schiller measures: 1911.50, 238.6@, 33.54", 8.8-10.5.                   Shr1913 
                         Identification uncertain.                                                       
07459+6509   STF1122     BDS 4203, H V 135 same star.                                                    
                         H 5 135.                                                                MEv2010 
07462-3053   I  1169     Spectrum: Fm Delta Del.                                                         
07462-5949   COO  58     B is CPD-59@898.                                                                
                         SWR  32. CPM pair                                                       Skf2004 
             SHY 194     AC: HIP  37918 + HIP  37563.                                                    
             SHY 194     BC: HIP  37923 + HIP  37563.                                                    
07463+5755   GIC  77     LDS2552. G193-064/G193-063.                                                     
07465-2202   B  2153     CPD-21@2740.                                                                    
07466+1102   OL   78     This pair is 13" preceding and 3' south of ADS 6358. Fainter and                
                         closer, not in the B.D. The only earlier measures are given in the              
                         ADS; all later measures assigned to it are of ADS 6358. No change in            
                         either pair.                                                            B__1963b
07466+0408   STF1137     H 2  39.                                                                MEv2010 
07467+2001   RED   9     2MASSW J0746425+200032                                                          
                         Reid (2001) 2000.287 data from HST WFPC2 . Paper includes mass and age  Red2001 
                         estimates, as well as discussion of L dwarf binary frequency and                
                         semimajor axis distribution.                                                    
                         Bouy et al (2004) derive a combined spectroscopic/astrometric solution  Boy2004 
                         for this binary L dwarf. Quoted errors are as follows:                          
                         P: +2.475/-2.100y, a: +0".030/-0".023, i: +2.5/-3.4deg,                         
                         node: +9.9/-14.2deg, T: +0.14/-0.09y, e: +0.08/-0.09,                           
                         omega: +5.2/-5.9deg. Semi-major axis given as 2.53 +0.37/-0.28 au.              
                         Angular values in orbit catalog are based on the quoted distance of             
                         12.21 +/- 0.05 pc. The total derived mass is 0.146 +0.016/-0.006 Msun.          
                         HST spectra indicate spectral types L0 +/- 0.5 and L1.5 +/- 0.5; Bouy           
                         et al. determine age range 150-500 Myr, conclude secondary is brown             
                         dwarf with mass in range 0.060 - 0.072 Msun.                                    
                         Gizis et al. (2006) believe both stars are probably older (>1 Gyr)              
                         than thought by Bouy et al., with masses about 0.080 and 0.075 Msun.    Giz2006 
                         Assuming a parallactic distance of 12.21 +/- 0.05 pc                    Dah2002 
                         (Dahn et al. 2002), Konopacky et al. (2010) derive a system mass of             
                         0.151 +/- 0.003 Msun.                                                   Kon2010 
                         Astrometric orbit by Harris et al. (2015) yielded the following                 
                         properties: spectral types L0+L1.5, absolute J mags 11.85+12.21,                
                         masses 0.080 +/- 0.002 and 0.074 +/- 0.002 Msun.                        USN2015 
07468+0245   BAL2311     BAL1813.                                                                        
07470+6403   STF1127     BDS 4378; H II 101 is probably same star.                                       
07470+0001   STF1141     B is BD+00@2080.                                                                
07471-1933   DAW 182     CPD-19@2666.                                                                    
07471-4130   DUN  56     Alternate spectral type: B1V. B is CD-41@3385.                                  
07472-5905   R    79     B is CPD-58@993.                                                                
07473-0543   HJ   62     There is a faint star near B about half the distance of A.                      
07475+7012   GJ 285.1    Arenou (2000) combined solution of astrometric orbits and DSBs. Paper   Are2000 
                         includes masses and distances.                                                  
                         Improved SB2 orbit for the unresolved pair.                             Kie2018 
                         A: Teff = 5585 +/- 13 K, B: Teff = 4484 +/- 110.                                
             BAG  48     The Aa,Ab pair may be the 553d spectroscopic binary.                    Grf2017e
07475+3325   STF1135     pi Gem = 80 Gem. Variable?                                                      
                         AB: H 4  53.                                                            MEv2010 
07476+1540   BPM 416     [PM2000]  815002 + [PM2000]  814995.                                    Gvr2010 
07478-1601   KNT   4     B is BD-15@2049.                                                                
07478-4418   BRT 716     CPD-43@1790.                                                                    
07479-1212   STF1146     5 Pup.                                                                          
07479-2411   HJ 4003     ARA074.                                                                         
07480+6018   HU 1247     This system underwent periastron sooner than predicted by the orbit of  Baz1961b
                         Baize (1961).                                                           Hrt1992b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.88 +/- 0.15, 2.08, and 2.14 Msun, respectively.             Mlk2012 
                         SB1, P=7236d? = 19.8y?                                                  Tok2014d
07480+1327   BPM 417     [PM2000]  815774 + [PM2000]  815786.                                    Gvr2010 
07481+5013   NI   17     BVD  68.                                                                        
07481+0525   STF1143     Some error in position. See note in BDS II.                             Bu_1906 
                         This may be STF1134AB with a larger error than is typical for a                 
                         FGW Struve measure.                                                             
                         Alternatively, this may be the same as STF1141.                         StF2022 
07481-4812   SWR  34     CPM pair                                                                Skf2004 
07484+1820   STF1140     H 2  64.                                                                MEv2010 
07484+0434   BRT2135     BAL 2789.                                                                       
07484-1922   OL    5     This is probably the same as OL 156.                                            
07486+2308   WRH  15     82 Gem. 1945.82 : System separated.                                             
                         The equinox-1900 position was incorrectly given as 07526+2323 in        McA1978b
                         McAlister (1978) and McAlister & Fekel (1980)                           McA1980b
07487-0030   HJ   63     BAL 828.                                                                        
07488+2855   H 5  67     H V 67.                                                                         
07489-2458   HIP  38134  This metal-poor astrometric and SB is not resolved here.                Tok2013b
07489-2622   BRT2921     CPD-26@2613.                                                                    
07490+2834   STF1144     AB: H 2  65.                                                            MEv2010 
                         Primary is eclipsing binary of Algol-type, 1.425 d.                     Zas2012 
07490+0040   STTA 88     B is BD+01@1912.                                                                
07490-2455   TOK 194     Astrometric binary; dm 1.7 mag, period ~ 2.4y Orbit (Goldin & Makarov           
                         2007)                                                                   Tok2012b
                         The period matches the astrometric orbit of Goldin & Makarov (2007.     Gln2007 
                         The mass sum in this pair composed of a giant primary and possibly an           
                         A-type secondary is 5.9 Msun. The measure on 2011.93 was ignored as             
                         spurious (it was affected by vibrations).                               Tok2015c
07491-5625   SEE  88     A is a spectroscopic binary.                                                    
07492+3117   HJ  429     SEI 481.                                                                Nsn2017b
07492-4622   JC   11     B is CD-46@3462.                                                                
07492-6017   HJ 4012     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
             SHY 197     AC: HIP  38160 + HIP  37918. C component = A component of 07462-5949.           
             SHY 197     AD: HIP  38160 + HIP  37563. D component = C component of 07462-5949.           
07493+0839   GIC  78     G089-043/G089-042.                                                              
07493-2452   BU 1063     xi Pup = 7 Pup. A is a spectroscopic binary.                                    
07494+1655   BPM 418     [PM2000]  819195 + [PM2000]  819247.                                    Gvr2010 
07494-2902   B  2638     CD-28@4920?                                                                     
07495+4128   LDS 900     AB,C: NLTT 18475/18473                                                  Chm2004 
07497+1204   BPM 419     [PM2000]  819741 + [PM2000]  819782.                                    Gvr2010 
07497+1047   BPM 420     [PM2000]  819895 + [PM2000]  819740.                                    Gvr2010 
07498-2012   SEE  87     Both A and B are above MS. Wrong parallax?  B is optical, observed              
                         motion is opposite to the PM of A. Wrong colors.                        Tok2014d
07500+1203   BPM 421     [PM2000]  820582 + [PM2000]  820603.                                    Gvr2010 
07500+0241   J  2044     BAL 1822.                                                                       
07501+0239   J  2046     BAL 1823.                                                                       
07501-0053   SAN   1     Reported by Sanford & Nicholson in 1940. Star 17 Algiers 184.           San1940 
                         Also known as HDS1112.                                                          
07501-1756   ARA 199     A likely plate flaw.                                                    Grv2021b
07502+1333   GRV1253     Both A and B have approximately the same radial velocity.               Grv2019b
07502+1051   BPM 422     [PM2000]  820874 + [PM2000]  820708.                                    Gvr2010 
07502-0214   GCB  21     J 1502. BAL 491.                                                                
07503+0713   LDS3765     GJ 1102B.   White dwarf pair = WD 0747+07 = EGGR 426/427                Grn1986 
07506-3620   JSP 194     CPD-36@1702.                                                                    
07507+0242   BAL1825     J 2047.                                                                         
07508+0317   A  2880     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.70 +/- 0.37, 4.80, and 2.88 Msun, respectively.             Mlk2012 
07509+4428   JNN  59     There is a companion to 2MASS J07505369+4428181 which has a color and           
                         brightness that is consistent with what should be expected if it was            
                         physcially bound. Common proper motion has not yet been tested for the          
                         system.                                                                 Jnn2012 
07509+1203   BRT3375     Unnumbered pair, following BRT1240 in Barton's list.                    Brt1935a
07509+0446   BRT2136     Aka BAL3007b.                                                                   
07510+4231   LDS 901     NLTT 18504/18506                                                        Chm2004 
07510+3137   STTA 89     Also known as FRK   7. B is BD+31@1677, spectrum A5.                            
                         HJL1050.                                                                HJL1986 
07510-2414   HDO 110     CD: J  1503.                                                            J__1962a
07513+1649   BPM 423     [PM2000]  823572 + [PM2000]  823801.                                    Gvr2010 
07517+1245   BPM 424     [PM2000]  824420 + [PM2000]  824507.                                    Gvr2010 
07517+0301   CUD   3     Component A is the central star of the planetary nebula PN G217.1+14.7  Skf2013 
                         = Abell 24.                                                                     
07518-0252   BAL 189     BRT 413.                                                                Brt1931 
07518-1354   BU  101     9 Pup. Discussion of the RV's by Abt & Levy (1976).                     AbH1976 
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Hipparcos parallax 60.59 +/- 0.59 mas; dynamical parallax 59.8 mas,             
                         masses 1.16 and 0.86 Msun. This is a minor revision of the orbit by             
                         Pourbaix (2000) needed to reduce its large residual from our measure    Pbx2000b
                         in 2009. Radial velocities (RVs) from the above paper were included in          
                         the combined orbital solution, but make little influence on the final           
                         elements, which are primarily constrained by speckle interferometry.            
                         The orbit is now extremely well defined.                                Tok2012b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.90 +/- 0.09, 2.09, and 1.02 Msun, respectively.             Mlk2012 
07519+0001   LDS6210     NLTT 18545/18546                                                        Chm2004 
07519-2630   BRT9001     This pair not assigned a Barton number by him, hence the 9001 here.     Brt1951 
                         His cross-reference star, CPD-26@2690 = CD-26@5106, is single,                  
                         however, the precise position identified pair seems to match Barton's           
                         description.                                                                    
07520-0202   BAL 492     J 2856.                                                                         
07522-4035   TOK 195     Astrometric binary; dm 1.0 mag, period ~ 7.0y Orbit (Jancart et al.     Jnc2005 
                         2005), SB1                                                              Tok2012b
                         The bright star a Pup (HD 64440, HR 3080) is known as a spectroscopic           
                         binary. However, examination of the RV data reveals that the orbit by           
                         Parsons (1983 ApJS 53, 553) is only approximate. The binary is                  
                         difficult to measure, always close to the diffraction limit and with            
                         dm~3. Instead of the spectroscopic period of 6.99yr, our orbit has              
                         P=7.4y and is still preliminary. More RV coverage is obviously needed.  Tok2015c
07523-2626   WSI  54     V402 Pup, ellipsoidal binary, period 1.01896 d.                         Zas2018 
07525+7753   LDS1659     NLTT 18453/18452                                                        Chm2004 
07525-1352   H 3  28     H III 28.  Hipparcos suspected non-single.                                      
07526+1635   BPM 425     [PM2000]  826307 + [PM2000]  826550.                                    Gvr2010 
07526+1201   STF1153     Spectral classes may be F8, F5 (McCormick). B is BD+12@1699.                    
07528+1850   OCC9016     The OCC2010 solution is ambiguous and two are arbitrarily "T" coded             
                         until the true solution is determined.                                          
07528-0526   FIN 325     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.20 +/- 0.23, 2.18, and 1.35 Msun, respectively.             Mlk2012 
07529+6454   STF1136     STT 184.                                                                        
07529-5838   RST4379     Spectral type A5?                                                               
07530+3138   SEI 483     KU, Bonn 3465.                                                                  
07532-1248   J  2489     RST 3554. BRT 2616. BRT2689.                                                    
07533+2528   HJ 5471     Herschel coordinates 07 42 59.2 NPD 64 06 50 (1830). He notes: "this    HJ_1870 
                         one and 5472 are in same field and nearly same parallel".                       
07535+2917   ALP  12     2MASSI J0753321+291711                                                          
                         Physical companionship to this ultracool dwarf is ruled out based on            
                         I-J color, using I-band photometry taken at WIYN.                       AlP2007 
07535+2646   phi Gem     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
07536+3036   BUP 108     Proper motion of A +719 -1832.                                                  
                         We do not confirm it using our data and images from the Digitized Sky           
                         Surveys                                                                 Oso2004 
07537-6339   MUG   8     Based on astrometry, photometry and H- and K-band spectroscopy,                 
                         Mugrauer et al. (2007) conclude that HD 65216 A and B comprise a        Mug2007 
                         physical pair. The projected separation is 253 au. The Ba and Bb                
                         (their B and C) components also appear to be co-moving. From narrow-            
                         band photometry of all components, conclude spectral type of Ba is              
                         M7-M8 and that of Bb is L2-L3; masses are 0.089 +/- 0.001 and 0.078             
                         +/- 0.001 Msun for Ba and Bb, assuming a system age of 5 Gyr. Orbital           
                         period of Ba,Bb estimated at 36y. Theta values estimated from their             
                         Figure 6.                                                                       
                         Primary is planet host star. Two companions Ba and Bb bound to A                
                         component. Spectral types of Ba and Bb are M6.5-L0 and M7.5-L4,                 
                         respectively.                                                           Egn2007 
                         AB: A is exoplanet host, P=613d, 5542d                                  Tok2014d
07538+2444   STF1156     Burnham says STF1156 and STF1163 (BDS 4335 and BDS 4352) are            Bu_1906 
                         the same star, but Weis ("F.G.W. Struve's Double Stars") indicates      StF2002 
                         separate pairs. WDS identification 07560+2440STF1163 changed to                 
                         07538+2444STF1156 and 07560+2440STF1163.                                        
07540+1711   BPM 426     [PM2000]  829481 + [PM2000]  829487.                                    Gvr2010 
07541-2413   ARA2083     ARA2082 and ARA2083 found to share same secondary; quadrant flipped             
                         for ARA2082 and systems merged, with ARA2082 as BC pair.                        
07542+1135   BPM 427     [PM2000]  829865 + [PM2000]  830037.                                    Gvr2010 
07542+0429   J   803     J notes a second component at 100@, 11th magnitude.                             
07542-5834   HJ 4021     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
07544-1748   HJ 4015     B is BD-17@2221.                                                                
07545-0011   BAL1121     J  3284.                                                                Nsn2016 
07547+3806   TOK 665     Tokovinin & Lepine (2012): 3 CPM candidates at 802", 1665", 1612", all          
                         likely optical.                                                         Tok2014d
07548-1730   ARA 203     A likely plate flaw.                                                    Grv2021b
07549+1914   ENG  33     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB and AC: Rectilinear solution by Hurowitz et al. (2013).              USN2013a
07549+1218   BPM 428     [PM2000]  831471 + [PM2000]  831462.                                    Gvr2010 
07549-2920   KUI  32     Also known as LHS1955. Parallax = 74.36 +/- 1.13 mas.                   TSN2010 
07552+1601   BPM 429     [PM2000]  832157 + [PM2000]  831932.                                    Gvr2010 
07554-5337   GLI  77     B is CPD-53@1479.                                                               
07557-0328   HJ   71     See note in BDS II.                                                             
07558+3530   HJ 3303     ALI 115.                                                                        
07560+2440   STF1163     Burnham says STF1156 and STF1163 (BDS 4335 and BDS 4352) are            Bu_1906 
                         the same star, but Weis ("F.G.W. Struve's Double Stars") indicates      StF2002 
                         separate pairs. WDS identification 07560+2440STF1163 changed to                 
                         07538+2444STF1156 and 07560+2440STF1163.                                        
07560+2342   COU 929     Mason et al. (1997) orbit includes mass determination.                  Msn1997a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.82 +/- 0.22, 2.35, and 1.05 Msun, respectively.             Mlk2012 
07560+0448   BAL3008     Not found by Heintz at IDS position.                                    Hei1990b
07560-2313   DON 212     CD-22@5380.                                                                     
07563-2221   SEE  90     CD-22@5387.                                                                     
07568-6049   HJ 4027     In the cluster NGC 2516. Spectra B9IVp(Si) and B9.5IVp(SiII).                   
                         Spectrum of C: A2IV.                                                            
07571+1800   BPM 430     [PM2000]  836184 + [PM2000]  836153.                                    Gvr2010 
07572+2342   HJ  433     Also reported as new by Gauchet and Doolittle.                          Gau1926a
07573+0108   STT 185     Perry (as cited by Gledhill) noted two faint companions with his                
                         18-inch reflector in 1881.16. The first was at ~170deg, separation              
                         25-30", the other at ~270deg, 30-35".                                           
                         Additional notes may be found in Schiaparelli (1888).                   Sp_1888 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.85 +/- 0.37, 2.86, and 1.13 Msun, respectively.             Mlk2012 
07573-0950   A  1578     Rectilinear solution by Rica & Zirm (2012).                             FMR2012i
07573-4407   SEE  92     A is variable.                                                                  
07578-6018   LDS 198     A is a spectroscopic binary.                                                    
             JSP 208     BC: CD-59@1774.                                                                 
07581-2916   BRT2933     CPD-28@2627.                                                                    
07582-4915   HRG 137     A is the Beta Lyrae-type system V Pup.                                          
07583+0213   SHJ  87     14 CMi.                                                                         
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: H 6  84.                                                            MEv2010 
07584-0258   BRT 542     BAL 192.                                                                        
07584-2908   EVS   7     Classical Cepheid AQ Pup.                                                       
07584-4619   CPO 183     One of three Barton pairs he may have intended to label BRT 721.        Brt1933 
07584-6051   HJ 4031     Spectrum: B8.5IIIMnII and B9V.                                                  
07587-4740   CPO 184     CPD-47@1729.                                                                    
                         One of three Barton pairs he may have intended to label BRT 721.        Brt1933 
07590-4940   CPO 185     One of three Barton pairs he may have intended to label BRT 721.        Brt1933 
07590-6338   LDS 199     Separation 1050".                                                               
07591-0420   TOT   1     V769 Mon.                                                                       
07592+3457   BRT3249     ALI 117.                                                                        
07592-4959   DUN  59     B is CD-49@3244.                                                                
07592-5038   SWR  36     CPM pair                                                                Skf2004 
07593+6554   MLB 344     Also known as WFC  60.                                                          
07598-0847   GWP 957     ABL 179.                                                                Tob2012b
07598-1351   HLD  94     The 1985.12 measure by Heintz was listed as HJ   74 at it's             Hei1987a
                         previous incorrect southern declination. When given the correct                 
                         hemisphere this is the closest pair which approximately fits, so the            
                         id on this measure is uncertain.                                                
07598-4718   I  1070     Primary is V410 Pup, a bet Lyr type eclipsing binary, period 0.87616d.  Zas2012 
07599-1030   FOX  63     Aka J  2861.                                                            Dam2012 
07599-1433   GWP 958     ABL 180.                                                                Tob2012b
07599-1448   BRT 571     TDS5429.                                                                        
08001-0937   J  2862     RST 3562.                                                                       
08003+1138   HJ   74     aka ROE  32. Friedrich Damm commented on the declination sign being             
                         wrong for the HJ pair. The 1825 coordinates, precessed to 2000                  
                         match this pair, as does the second measure by John Herschel.                   
08005+2900   OSO  20     G090-036. Common proper motion pair                                     Oso2004 
08005+0955   A  2954     Magnitude underestimated by Aitken; should be ~0.7 mag.                 Baz1951a
08007+1635   BPM 431     [PM2000]  843821 + [PM2000]  843697.                                    Gvr2010 
08008+1719   OCC9068     3 Cnc.                                                                          
08009+4452   ES 1325     aka 08017+4451TDS5455.                                                          
08009-0405   LDS6211     NLTT 18799/18798                                                        Chm2004 
08013-1407   BRT2700     A likely plate flaw.                                                    Grv2021b
08014-5431   DUN  60     One component is variable and a spectroscopic binary.                           
                         dRA = 1.83s.                                                            Dun1829 
08016-3430   JSP 216     CPD-34@1901.                                                                    
08017+6019   MCA  33     53 Cam. A variable of the Alpha CVn type, AX Cam, and a spectroscopic           
                         binary now resolved by interferometry.                                          
                         Value of omega in Baize (1993) orbit incorrectly listed as 113.0, same  Baz1993b
                         as Omega (erratum noted in Inf. Circ. 121, 1994).                       Baz1993d
                         Combined spectroscopic/interferometric orbit by Balega et al. (2004),   Bag2004b
                         yielding mass sum 3.61 +/- 0.38 Msun. Spectral types are estimated as           
                         A2V and F0V.                                                                    
                         Combined spectroscopic/interferometric orbit by Carrier et al. (2002),  CrF2002 
                         yielding a = 275.1 x 10^6 km, parallax 10.2 +/- 1.0 mas and mass sum            
                         1.49 +/- 0.66 Msun. Authors note that Scholz & Lehmann (1988)           Slz1988 
                         attempted to scale their spectroscopic solution using then-available            
                         speckle data, deriving masses for the components of 2.5 and 1.6 Msun,           
                         considerably larger than found here.                                            
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.62 +/- 3.60, 3.94, and 2.09 Msun, respectively.             Mlk2012 
08017+2505   H 6  75     ome 2 Cnc = 4 Cnc.  H VI 75.                                                    
08017+1521   BPM 432     [PM2000]  845760 + [PM2000]  845621.                                    Gvr2010 
08017-0836   A  1580     A is the Algol-type system V635 Mon.                                            
08018-3429   I   187     CD-34 4230, mag 11.7, is 46.5" S and a 13.0 is 20" preceding.           Daw1927a
08021+5437   STF1165     Same as STF1166.                                                                
08021-0049   BAL 845     J 3285.                                                                         
08021-1710   HDS1140     AB + TOK 394AC: This is the high-PM M-dwarf LP 784-12 (HIP 39293) at            
                         30pc. A new distant component C was found at 1".8 in addition to the            
                         known pair HDS 1140 which closed from 0".4 in 1991.25 to 0".33 now. It          
                         is confirmed as physical by its fixed position during one year, the             
                         quadrant of the triple was determined in run 5.                         Tok2015c
08024+0409   STF1175     A premature orbit has been computed. Data appear equally well fit by            
                         rectilinear solution - see linear elements catalog.                             
08024+0320   LDS5160     LDS5196.                                                                        
08025+6305   SHJ  86     STTA 90. B is BD+63@750.                                                        
08025-4440   I     8     QQ Pup.                                                                         
08025-5502   HJ 4044     B is CPD-54@1480.                                                               
08026+2028   DOO  47     Doolittle identifies this as BDS 4392, HJ 437 but it seems to be a      Doo1915b
                         different pair.                                                                 
08026+1309   SLE 320     CD: SLE 456.                                                                    
08027-2632   LDS 200     NLTT 18855/18856                                                        Chm2004 
08027-4119   HJ 4038     A component variable? B is CD-40@3775.                                          
08029+0419   BRT2140     BAL 2801.                                                                       
08030-5720   SWR  38     CD-56@ 2090.                                                                    
08031+1637   BPM 433     [PM2000]  848557 + [PM2000]  848413.                                    Gvr2010 
08031-0625   A  1581     A premature orbit has been computed.                                            
08031-3228   HJ 4035     B is CD-32@4768.                                                                
08032-3812   HJ 4039     V626 Pup, EA per 1.425902 d.                                            Zas2011 
08033+5251   HDS1149     An additional component at a distance of 40 mas from the secondary is           
                         suspected in the system. The magnitude difference is between 1.5 and            
                         2 mag.                                                                  Bag2004 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.42 +/- 0.46, 1.07, and 1.00 Msun, respectively.             Mlk2012 
08035+2748   ES 2628     chi Gem. See Espin.                                                     Es_1908a
08035+1211   HO  350     A=SB?  AB is seen in the 2MASS J,K-band images, but A seems saturated.  Tok2014d
08036-4000   zet Pup     = Naos. The distance estimate is from Reid & Howarth (1996 A&A 311,             
                         616). Van Rensbergen et al. (1996 A&A 305, 825)  discuss the star's             
                         trajectory and possible runaway status.                                 Msn1998a
08037-4634   HJ 4043     B is CD-46@3727.                                                                
08038-1055   J  2492     J 2863.                                                                         
08039-3133   LDS 201     AB: B is CD-31@5466.                                                            
                         AB: SHY 520. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AC: C is CPD-31@2104.                                                           
             B  2164     CD: TDS5491.                                                                    
08040-5822   BRT3117     TDS5496.                                                                        
08041+3302   STT 187     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.79 +/- 1.42, 4.53, and 2.14 Msun, respectively.             Mlk2012 
08044+1217   BU  581     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.96 +/- 0.38, 1.75, and 0.85 Msun, respectively.  Mlk2012 
                         Star C (mag. 10.5, 5") is in slow direct motion about AB.                       
                         AB,C: Additional notes may be found in Burnham (1894).                  Bu_1894 
08047+2831   MLB 565     Faint pair, 32s p, 3' n of ADS 6557.                                    Baz1951a
08047-6250   DUN  62     A is the variable V375 Car.                                                     
                         B is CPD-62@952.                                                                
08049-0223   GWP 968     ABL 181.                                                                Tob2012b
08049-2233   ARA1719     A likely plate flaw.                                                    Grv2021b
08050-3419   B  1579     Despite the linear solution, proper motion and parallax favor a         Grv2020a
                         physical connection. Long period and/or high eccentricity possible.             
08052-4525   JC   12     B is CD-45@3742.                                                                
08053-4626   CPO 192     TDS5515.                                                                        
08055-6952   HJ 4055     SWR  39. CPM pair                                                       Skf2004 
08056+2830   MLB 566     The Barton pair formerly at 08049 is identical                          Hei1985a
08056+2732   STF1177     17 Cnc                                                                          
08056-6617   GLI  81     B is CPD-65@867.                                                                
08057+6823   STF1164     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2014).                         USN2014a
08059-2014   ALD  84     CPD-19@3088.                                                                    
08061-0047   A  1971     A premature orbit has been computed.                                    Cou1953d
08062+0201   J   420     Appears to be in rapid retrograde motion.                                       
                         Despite having an orbit, an optical pair based on parallax.             Mlk2022 
08063-4021   RSS   9     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
08068+3303   AG  147     SEI 487.                                                                Nsn2017b
08068-0900   GWP 972     ABL 182.                                                                Tob2012b
08069-1320   GWP 973     ABL 183.                                                                Tob2012b
08069-2707   DUN  61     B is CD-26@5531.                                                                
08069-6618   LUH   5     Primary is the DQ white dwarf WD 0806-661 = GJ 3483, mass 0.62 +/-              
                         0.03 Msun. Mass of companion estimated at ~7 Mjup, Teff ~300K.          Luh2011 
                         Companion Teff 300-345K, mass 6-9 Mjup, distance 19.2 +/- 0.6 pc.       Luh2012 
08071-2138   B  2168     CPD-21@3163.                                                                    
08072+1615   BPM 434     [PM2000]  856195 + [PM2000]  856322.                                    Gvr2010 
08072+0723   AG  149     HJL  86.                                                                HJL1986 
08075+1318   BPM 435     [PM2000]  856648 + [PM2000]  856681.                                    Gvr2010 
08075-2418   RST5284     rho Pup = 15 Pup = Tureis. A is a Delta Scuti-type variable.                    
08076-0814   GWP 976     ABL 184.                                                                Tob2012b
08079-0215   GWP 977     ABL 185.                                                                Tob2012b
08079-6837   RMK   7     eps Vol. A is a spectroscopic binary.                                           
08081+4916   HJ 2428     Rectilinear solution by Cvetkovic et al. (2018).                        Cve2018 
08081-2415   BRT1448     Aka ARA2099.                                                                    
08082+7155   LDS1667     NLTT 18921/18913                                                        Chm2004 
08082+2106   COU  91     LDS 902.                                                                        
                         NLTT 18979/18980                                                        Chm2004 
08082-2208   BU  334     Despite the linear solution, proper motion and parallax favor a         Grv2020a
                         physical connection. Long period and/or high eccentricity possible.             
08084-0005   GWP 979     ABL 186.                                                                Tob2012b
08085+5130   ES   70     27 Lyn.                                                                         
08086-0259   STF1190     zet Mon = 29 Mon. C is BD-02@2449.                                              
                         AB: H 4  97.                                                            MEv2010 
08087+5750   A  1075     Also known as HDS1161. These two pairs were recognized to be the same           
                         by Brian Skiff.                                                         Skf2004 
08089+2437   NLTT 18995  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Latham et al. (2002). They derived component masses 0.92 and 0.62 Msun  Lat2002 
                         and an estimated semimajor axis of 25.73 mas.                           Ren2013 
08089+1213   J   375     AB: Rectilinear solution by Cvetkovic et al. (2018).                    Cve2018 
08090+3249   BDT   2     Aa,Ab : Combined solution yield Ma = 0.72 +/- 0.04 \msun,               Miz2018 
                         Mb = 0.30 +/- 0.03, distance of 24.83 +/- 0.22 pc, Age = 42 +/- 6/5             
                         Myr, and Teff = 4100 +/- 200/400.                                               
             DYR   1     AB: VYS 250. A is a flare star, and B is a double-lined spectroscopic           
                         binary, P = 6.21d.                                                              
08090-6118   EHR  11     Companion appears to be a background star.                              Ehr2010 
08091-3719   BRT1615     CPD-36@1978.                                                                    
08091-3931   GLI  80     B is CD-39@4038.                                                                
08092+1836   SLE 466     BC: Hipparcos suspected non-single.                                             
08094+3752   STF1184     B is BD+38@1869.                                                                
08095+3213   STF1187     Hopmann orbit rejected from Fourth Orbit Catalog                        Hop1971 
                         ("period over 4000 years")                                              Wor1983 
             CHR 190     Aa,Ab: Four observations 1991-1996, with separation decreasing from             
                         0.15" to 0.06"; next observed in 2004 at 0.16". Two possible orbits             
                         are suggested: a short-period (11.3y) solution predicts a separation            
                         of 0.074", while a long-period (28.8y) solution predicts 0.143".        Hrt2009 
08095-4720   DUN  65     A: gam 2 Vel. Spectrum WC8+O7.5e, probably the nearest Wolf Rayet.              
                         B: gam 1 Vel. CD-46@3846. Variable, spectrum B1IV.                              
                         AB: Both components are spectroscopic binaries.                                 
                         The AB pair was formerly known as DUN  64.                                      
             I  1175     DE: DE is I 1175 (= RST 4878) at 08 09.5 -47 25.                                
                         The Hipparcos distance suggests a position in front of the Vel OB2              
                         association (van der Hucht et al. 1997 NewA 2, 245; Schaerer et al.             
                         1997 ApJ 484, L153) at a distance of 258 +41/-31 pc; however, the               
                         Hipparcos distances for the B stars in Vel OB2 (Brandt et al. 1971 ApJ          
                         1623, L99) yield a comparable distance of 317 +/- 42 pc.  This is also          
                         consistent with the distance from the resolution of the binary by               
                         Hanbury Brown et al. (1970) of 350 +/- 50 pc.  Thus, we have chosen to  HBr1970 
                         keep gam 2 Vel as a member of Vel OB2. Classification is from van der           
                         Hucht et al. (1997).  The B component was also observed and appeared            
                         to be single. Classifications of the B, C, and D components are from    Msn1998a
                         Hoffleit & Warren (1991).                                               Hof1991 
             TOK   2     Aa: The primary is a close WR+O binary. Although the pair is                    
                         unresolved, VLTI/AMBER observations on 2004.984 over baselines of               
                         46-85m and wavelength range 1950-2170 nm are fit by a binary model              
                         giving a separation of 3.65 +/- 0.06 mas, position angle 72.7 +/- 8.7           
                         deg, flux ratio 0.62 +/- 0.04 (dm 0.52 +/- 0.07 mag.                    MiF2007 
                         Intensity Interferometer Limb-darkened diameter 0.44 +/- 0.05 mas.      HBr1974 
08098-1658   A  3101     Spectrum: A3/5II/III.                                                           
08099-1923   ARA 632     A likely plate flaw.                                                    Grv2021a
08099-4911   SYO   3     Aka R    81.                                                                    
08100-4241   CPO 195     CPD-42@2143.                                                                    
08102+5548   SHY 524     AC: HIP  40006 + HIP  40536.                                                    
08102+3527   WSI 100     Provisionally designated WSI9105.                                       Hrt2008 
             HJ 3308     AB: Rectilinear solution by Friedman et al. (2012).                     USN2012a
08102+3347   ANR   1     MLB 1049.                                                                       
08102+2551   BUP 111     B is BD+26@1729.                                                                
08103-0607   GWP 984     ABL 187.                                                                Tob2012b
08104+0020   BAL1133     HJL  87.                                                                HJL1986 
08105+2530   BUP 112     psi Cnc = 14 Cnc.                                                               
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
08106-1842   GWP 987     ABL 188.                                                                Tob2012b
08106-2024   ARA1030     Aka BRT1454.                                                            Dam2016b
08107-1348   LDS 204     18 Pup. NLTT 19073/19072                                                Chm2004 
                         AB: Both A and B possible SBs?                                          Tok2014d
08107-1751   GWP 989     ABL 189.                                                                Tob2012b
08110+7955   LDS1668     AB: NLTT 18931/18924                                                    Chm2004 
             OSO  21     G251-054. AD is not a proper motion companion                           Oso2004 
08113+0117   STF1198     B is BD+01@2018.                                                                
08113-1256   BU 1064     19 Pup. Not seen in 1936, 1939                                          B__1951a
08114-4259   HJ 4057     B is CD-42@3976.                                                                
08116+3227   CRJ   2     Aa,Ab: Primary is GJ 9256. Crepp et al. (2012) derive spectral types            
                         G4V and M5, masses 0.85 +0.04/-0.03 and 0.16 +/- 0.02 Msun.             CrJ2012 
             STT 564     AB and AC: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
08116-0014   GWP 993     ABL 190.                                                                Tob2012b
08116-3722   JSP 236     CPD-37@1984.                                                                    
08117-0636   J  2054     LAC.                                                                            
08117-3209   B  2170     According to Brian Skiff, while the WDS has the correct position, this          
                         is not CD-31 5661 (a B giant), but instead is CPD-31 2177 an F/G pair.          
                         Appears to be an IDS error.                                             Skf2003 
08118-0717   GWP 994     ABL 191.                                                                Tob2012b
08118-3521   J  2301     Nova Puppis = PK 252-00.1 = CP Pup.                                     J__1962a
08121-1540   HJ 4050     B is BD-15@2309, spectrum A9/F0V.                                               
08122+1739   STF1196     zet Cnc = Tegmine. Reductions of measures in position angle                     
                         untrustworthy because of confusion among the eithr position angles of           
                         minimum visibility. Distance too great for interferometer measures.     WRH1941a
                         AB: H 1  24.                                                            MEv2010 
                         AB: Additional notes may be found in Burnham (1894),                    Bu_1894 
                         Simonov (1937), and                                                     Smw1937 
                         Muller (1955).                                                          Mlr1955c
                         AB,C: H 3  19.                                                          MEv2010 
                         AB,C: 2-orbit AB,Cc quadruple solution (AB,C in HIP).                   Sod1999 
                         AC: Additional notes may be found in Vyssotsky (1936),                  Vys1936 
                         Simonov (1937), and                                                     Smw1937 
                         Simonov (1951).                                                          Smw1951
                         AB,D: D is BD+18@1870.                                                          
                         The system Cc has been resolved by infrared speckle interferometry.     Mcy1983 
                         Typographical error in the Mason et al. (2006) published elements:      WSI2006b
                         omega = 330.2 +/- 6.7, not 6.7 +/- 1.2.                                         
             zet 1 Cnc B This object was misidentified as HR 3210 by McAlister (1978).           McA1978c
08122-0150   J   421     The note in ADS says that the 1906 measures by Morgan, attributed to    A__1932a
                         HJ 778, may belong to this pair.                                        Mrg1907 
08124-0059   GWP 995     ABL 192.                                                                Tob2012b
08125-1502   GWP 996     ABL 193.                                                                Tob2012b
08125-4616   CHR 143     Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 27.06 +/- 23.28, 9.94, 4.79 Msun, respectively.    Mlk2012 
08129+1044   BPM 436     [PM2000]  865688 + [PM2000]  865603.                                    Gvr2010 
08129-0733   LDS5175     LDS6213.                                                                        
08130+5026   GRV1004     SLW 226.                                                                        
08130-5402   HJ 4065     B is CPD-53@1569.                                                               
08131-3435   EVS  13     Primary is the Cepheid RS Pup.                                          Evs2016a
08132-1227   J  1510     BRT 2703.                                                                       
08132-1354   HU  115     Present parallax value adopted instead of poor HIP-value.               Sod1999 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.46 +/- 0.62, 1.20, and 0.55 Msun, respectively.             Mlk2012 
08136+1527   CLZ  43     Aka FMR 204.                                                                    
08136-0545   HJ 2435     AB: HDO 117                                                                     
                         AB: H 2  87.                                                            MEv2010 
08136-3144   HDO 201     B is below MS, not CPM (NOMAD, WDS). C is below MS, optical.            Tok2014d
08136-4700   GLI  87     A is variable. B is CD-46@3928.                                                 
08137+0407   ARG  68     A is +04 1934b while B is +04 1934a.                                            
08138-2206   LDS 207     CPD-21@3323.                                                                    
                         NLTT 19163/19166                                                        Chm2004 
08138-3444   I   193     For the 1997.1201 measure a smaller annulus was used in the power               
                         spectrum fit due to the faintness of the source. As a consequence, the          
                         separation and position angle uncertainties may be larger than other            
                         measures.                                                               Hor1997 
08140-3619   DUN  67     Variable, OS Pup. B is CD-35@4360.                                              
                         320 Arg. dRA 1.2s, dDEC 1' 12.3". Four stars forming a parallelogram            
                         (with DUN 68, dRA 3.3s, dDEC 1' 41.0", mags 7,7).                       Dun1829 
08140-4021   HJ 4062     The primary is a long-period spectroscopic binary.                              
             h 2 Pup     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Christie (1936).                                                        Crs1936 
08142+1741   H 6  78     AC: H VI 78.                                                                    
             SKF1627     DE: Primary of 08140+1744 found to be D component of 08142+1741.                
08142-3208   HJ 4059     A is a spectroscopic binary.                                                    
08143-3129   B  1592     Spectrum: A1/2III/IV.                                                           
08147-6616   HJ 4075     SWR  41. CPM pair                                                       Skf2004 
08149-0001   J    72     J  1511.                                                                J__1962a
08149+1058   BPM 437     [PM2000]  868831 + [PM2000]  868623.                                    Gvr2010 
08149-0120   J  2055     +1s, +1.5' from BD-00 1945. Companion variable.                         J__1955 
08153-1126   J  2875     BRT 2704.                                                                       
08153-6255   RMK   8     Rectilinear solution by Letchford et al. (2018).                        LRR2018a
08155+0202   DOB   9     BAL 1840.                                                                       
08155-3722   HJ 4063     B is CD-36@4387.                                                                
08156+1126   LEP  30     NI   18.                                                                        
08157+0738   STF1209     B is BD+08@2015.                                                                
08158+0550   ADM   3     WSP  51. HTP  30. HAT-P-30. Primary is exoplanet host star.             Adm2013 
08159+5047   STF1199     Opik reverses quadrant.                                                         
08159-3056   BU  454     Spectrum composite; G5-8III+G:.                                                 
08159-6252   HJ 4077     B is CPD-62@987.                                                                
08161+5706   ENG  34     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             GIC  79     AD: LDS2568.  AD = G194-017/G194-018.                                           
             ENG  34     AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
08161+1942   LDS3781     G040-014. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 19210/19207                                                        Chm2004 
08161-2847   HLD  95     Spectrum: A2/3III/IV.                                                           
08164-0314   HWE  21     A 29d spectroscopic solution for the A component has been found making  Tok2019g
                         this a triple system.                                                           
08165+7930   STF1169     HJL  88.                                                                HJL1986 
                         AB: A is SB1, P=4.884d                                                  Tok2014d
08165+0911   BU 1065     bet Cnc = 17 Cnc. Burnham measured BD+09@1922 and BD+09@1926 with       A__1932a
                         respect to A. A may be variable.                                                
                         Mk III Limb-darkened diameter  5.20  +/- 0.07  mas                      MkT2001 
                         Mk III Limb-darkened diameter  5.238 +/- 0.069 mas.                     MkT2003 
                         NPOI Limb-darkened diameter    5.03  +/- 0.04  mas,                     NOI1999 
                         R = 48.  +/- 4.  \rsun.                                                         
                         NPOI Limb-darkened diameter    5.13  +/- 0.06  mas.                     NOI2001b
                         NPOI Limb-darkened diameter  5.167 +/- 0.035 mas, Sp = K4III,           NOI2018 
                         R = 51.66 +/- 0.98 \rsun, Teff = 4094 +/- 53 K,                                 
                         L = 676.7 +/-41.4 \lsun, M = 1.75 +/- 0.11 \msun,                               
                         Age = 1.49 +/- 0.22 Gyr.                                                        
08167+3216   ES  293     SEI 489.                                                                Nsn2017b
08167+0113   OL  179     Aka HEI 344.                                                                    
08166-7914   HJ 4105     SWR  42.                                                                        
08169+5503   LDS3780     BC: SLW 231.                                                                    
08169+3331   SEI 490     None of the components seen on POSS plate; may be flaws on AC Potsdam           
                         plate.                                                                          
             SEI 491     AC. See note to SEI 490.                                                        
08169-1457   BRT1901     A likely plate flaw.                                                    Grv2021b
08170+5911   STT 565     B is BD+59@1153.                                                                
08170+0001   CHM   5     NLTT 19241 + 19240.                                                             
08172+3515   BRT3250     ALI 120.                                                                        
08173-0522   A   337     Only elements P and T have been amended from the orbit of               Sta1977a
                         Baize (1959).                                                           Baz1959 
08174-1125   BRT2708     J 1513.                                                                         
08175+3623   GRV 756     HJL  89.                                                                HJL1986 
08178+3738   BRT2219     ALI 587. Heintz describes this as identical to PTT  20.                 Hei1985a
08178-1927   LDS 211     = GWP1002 = ABL 194.                                                    Tob2012b
08178-6128   HRG  14     Aka HDS1179.                                                                    
08179+0628   STF1213     BDS 4546, HJ 87 probably same star.                                             
08179-5910   HJ 4084     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
08180-0022   GAU  11     BAL 850.                                                                        
08182-3722   HJ 4073     A is a spectroscopic binary.                                                    
08183+3859   STF1211     AD: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
08184-0803   GWP1003     AB: ABL 195AB.                                                          Tob2012b
             GWP1004     AC: ABL 195AC.                                                          Tob2012b
08184-2017   HJ 2441     A component is close double of spectral types A5III+G0III,                      
                         C component is also a close double of types A0-2III+K0III               AbH2000 
08185-0616   GWP1006     ABL 196.                                                                Tob2012b
08186-0554   GIC  71     G113-026/G113-027. LDS6214. A 1-hour error in transcribing coordinates          
                         led to an incorrect WDS designation for this system of 07185-0550.              
                         It is assumed that Giclas' original value for theta (28deg) was due to          
                         a math error, so it was corrected to 180-28=152deg.                             
                         NLTT 19298/19299                                                        Chm2004 
08186-4254   CPO 198     CPD-42@2341.                                                                    
08187-2033   RSS 154     CPD-20@3578                                                                     
08187-3407   RST2547     CPD-33@2077.                                                                    
08188+6806   LDS2571     NLTT 19229/19230                                                        Chm2004 
08189-3142   PRO  51     Aka TDS5709.                                                                    
08190+4927   HU 1124     AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
08190-7330   HJ 4095     AC = SWR  44. Brightest two stars in a 1' group.                        Skf2004 
08191+1607   BPM 438     [PM2000]  875251 + [PM2000]  875178.                                    Gvr2010 
08193+6230   OS UMa      Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Carquillat et al. (1983).                                               Crq1983 
08193-0537   TOK 121     HIP 40765. Small PM(A)=(-1,+42). NOMAD: PM(B)=(+66,-16), V(B)=12.83.            
                         B can be optical (crowded field, N*=42).                                Tok2011a
08193-6748   LDS 215     Aka LDS6215.                                                                    
08194-3807   JSP 260     CPD-37@2202.                                                                    
08195+3503   STTA 91     B is BD+35@1801.                                                                
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
08198-7131   BSO  17     A: kap 1 Vol. A is a spectroscopic binary.                                      
                         B: kap 2 Vol                                                                    
08199-2418   B   152     HDO 114.                                                                        
08200-5740   CPO 200     B is CPD-57@1483.                                                               
08201+3834   GIC  80     G111-072/G111-071.                                                              
                         NLTT 19314/19311                                                        Chm2004 
08202-5642   SWR  43     CPM pair                                                                Skf2004 
08206-7729   I   799     the Cha                                                                         
08207-0001   SLW 241     ABL 197. GWP1007.                                                       Tob2012b
08211+6527   SHY 199     HIP  40918 + HIP  40882.                                                        
                         AB: A is SB1, P=17.6y; suspected non-single star in Hipparcos           Tok2014d
08211+4725   STT 190     A,Ca: AB,Ca may be a quadruple system, as the proper motions are in             
                         fair agreement..                                                                
                         AB (mag. 8.6-12.0, 4") is HU 224, 39" distant.                                  
                         AD: D is BD+47@1565.                                                            
             STT 190     AC: HJL  90.                                                            HJL1986 
08211+1552   BPM 439     [PM2000]  878193 + [PM2000]  878305.                                    Gvr2010 
08213+3419   LEP  31     NI   19.                                                                        
             BVD 161     AD: X-ray aRX J0821.3+3418 and 2MASS at 5" from A, is it D?             Tok2014d
08213-0136   STF1216     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 8.24 +/- 5.59, 4.58, and 2.09 Msun, respectively.             Mlk2012 
08214-3545   BRT1623     CPD-35@2261.                                                                    
08214-3629   HJ 4085     A is a spectroscopic binary.                                                    
08217+1717   PAR   1     A is the Mira-type variable V Cnc.                                              
08217+1048   BPM 440     [PM2000]  879031 + [PM2000]  878978.                                    Gvr2010 
08217-5841   LDS 216     LDS5695.                                                                        
08221-7324   HJ 4103     eta Vol                                                                         
08223+1558   BPM 441     [PM2000]  879905 + [PM2000]  879851.                                    Gvr2010 
08223-3458   BRT1625     CPD-34@2328.                                                                    
08225+2638   BUP9115     See note to 08231+2648 BUP 115.                                                 
08225-2942   B  1600     Spectrum: Fm Delta Del.                                                         
08225-4829   I    67     B Vel                                                                           
08225-5931   HDS1190     = eps Car = Avior                                                               
08228-2621   B   767     Many negative or uncertain observations.                                        
08228-5727   BRG  27     Aa,Ab: As noted in Bergfors et al (2010), this is a triple system with  Brg2010 
                         component B outside of 6". Hence, we do not include component B in              
                         Table 4, but we note that at 8.429+/-0.001" separation in 2008.88 and           
                         8.374+/-0.003" in 2010.09, there is statistically significant orbital           
                         motion also for this component.                                         Jnn2012 
08228-7626   HJ 4109     B is CPD-76@515.                                                                
08229-5207   SHY 525     HIP  41081 + HIP  40916.                                                        
08231+2648   BUP 115     The IDS incorrectly associated this pair with BD+28 1598, rather than           
                         +27 1602. As a result, it was initially assumed to be a member of a             
                         quadruple system with two other pairs in the IDS. Eventually all were           
                         assigned the discoverer designation BUP 115 and component designations          
                         AB, AC, and CD. However, the two A components differ in precise                 
                         position by some 12.8 arcminutes. They were later assigned different            
                         WDS designations but discoverer and component designations were not             
                         corrected. The AC and CD pairs have now been assigned the designation           
                         BUP9115, with component designations AB and BC.                                 
08231-4912   DENIS-P...  DENIS-P J082303.1-491201 is an L1.5 dwarf at 20.77 +/- 0.08 pc.                 
                         Observations with FORS2 on the VLT reveal an astrometric companion in           
                         an eccentric orbit with period 246.4 +/- 1.4 days.  Masses of the               
                         primary and secondary are estimated at 78.4 +/- 7.8 and 28.5 +/- 1.9            
                         Mjup for an age of 1 Gyr, or 70.2-82.8 and 26.7-29.4 Mjup for ages              
                         0.6-3 Gyr.                                                              SaJ2013 
                         Sahlmann et al. (2015) refine the orbit of this juvenile binary brown           
                         dwarf, deriving spectral types L1.5 +/- 0.6 and L5.5 +/- 1.1, Teff =            
                         2150 +/- 100 and 1670 +/ 140K, log (Lbol/Lsun) = -3.73 +/- 0.08 and             
                         -4.25 +/- 0.20, masses 0.028-0.063 and 0.018-0.045 Msun (mass ratio             
                         0.64-0.74), delta I = 2.3 +/- 1.2 mag. The distance is 20.7pc, the age          
                         estimated to be in the range 80-500 Myr.                                SaJ2015b
08234-1016   GWP1010     ABL 198.                                                                Tob2012b
08234-1115   J  2878     BRT 2709.                                                                       
08234-2207   BRT1457     CPD-21@3515.                                                                    
08234-2310   BRT1458     CD-22@6089.                                                                     
08234-4248   HJ 4090     B is CD-42@4188.                                                                
08235+1434   LDS1210     NLTT 19425/19426                                                        Chm2004 
08236-1920   GWP1011     ABL 199.                                                                Tob2012b
08237-1150   GWP1012     ABL 200.                                                                Tob2012b
08237-2137   B  2654     J  1517.                                                                Nsn2016 
08237-5519   SHY 526     HIP  41147 + HIP  41579.                                                        
08238+5725   STTA 92     B is BD+57@1136.                                                                
                         AB: HJL  91.                                                            HJL1986 
08239+1038   A  2961     21 Cnc.                                                                         
08240-1548   RST4396     A 25d spectroscopic solution for the A component has been found         Tok2019g
                         making this a triple system.                                                    
08242-0150   GWP1014     ABL 201.                                                                Tob2012b
08243+4457   STF1217     LDS 904. B is BD+45@1575.                                                       
                         NLTT 19431/19428                                                        Chm2004 
                         HJL  92.                                                                HJL1986 
08243-0424   GWP1015     ABL 202.                                                                Tob2012b
08244-0432   GWP1016     AC: ABL 203.                                                            Tob2012b
                         08243-0432 and 08244-0431 found to share primary. Systems merged.               
08244-4601   CPO 204     CPD-45@2479.                                                                    
08245-3039   HJ 2446     B is CD-30@6203.                                                                
08246-0109   B  2527     FIN measures 1951-1959 distance less than 0.1".                                 
                         AB pair bound; change in separation and angle consistent with orbital           
                         motion. B component likely M2-M5 dwarf with mass 0.24 +/- 0.01 Msun.            
                         C and D components likely unrelated.                                    Egn2007 
                         AB: Likely a spurious pair. Last measured 1961 and unresolved by SOAR           
                         on 3 occasions 2010-2013.                                               Tok2012d
                                                                                                 Tok2014a
                                                                                                 Tok2015c
                                                                                                 Tok2016a
                                                                                                 Tok2022f
                         AB: Tentative resolution by Finsen, 1 speckle measure at 0.040" in              
                         2001.08, unresolved by Hipparcos, 3 non-resolutions by SOAR 2010-2013.          
                         AB can be "ghost".                                                      Tok2014d
             EGN  27     AE: E companion was not detected by RoboAO in 2013.05, below limit.     Tok2014d
08246-0345   CHR 172     Aa,Ab. Abt & Biggs (1972) note variable RV.                             AbH1972 
                         Aa,Ab: Likely a spurious pair. Last measured 1988 and unresolved by             
                         SOAR on 3 occasions 2011-2013.                                          Tok2012d
                                                                                                 Tok2014a
                                                                                                 Tok2015c
                                                                                                 Tok2016a
                                                                                                 Tok2022f
             TOK  20     AB: GJ 306. AB has estimated period 23,000y; Close triple?              Tok2006 
                         AB: A is SB, P=1.563d.                                                  Tok2014d
08247+4200   S   565     STTA 93. B is BD+42@1860.                                                       
08247-2849   RST1393     A is an Algol-type system, AW Pup.                                              
08248+2009   STT 191     B is BD+20@2078.                                                                
08248-0236   BRT 419     A likely plate flaw.                                                    Grv2021b
08249+1214   BPM 442     [PM2000]  883581 + [PM2000]  883518.                                    Gvr2010 
08249-4418   DAW 194     Turner (1979 A&A 76, 350) includes this star in the Vel OB1 group at a          
                         distance of 1.8 kpc. Photometric spectral classifications of the B and          
                         C components are from Lindroos (1985), who also finds a                 Lnd1985 
                         distance of 2.7 kpc.                                                    Msn1998a
08250+6725   LDS2574     B is BD+67@541.                                                                 
08250-4246   CHR 226     Ba,Bb: This close companion to RST4888 has been observed on three               
                         occasions, but has shown little movement over a 1.6-year period. The            
                         1989 measurements of the Rossiter pair were originally published by             
                         McAlister et al. (1990) and Hartkopf et al. (1993). Following           McA1990 
                         discovery of the close pair in the 1990 data, these 1989 data were      Hrt1993 
                         rereduced, resulting in "preconfirmation" of the new component.         Hrt1996b
                         V438 Pup, Algol-type eclipsing binary, P = 4.9350 d.                    Zas2011 
                         The new pair was initially given component designations Aa,Ab, but              
                         it was uncertain which component of the Rossiter had been split.                
                         Tokovinin et al. (2015) have determined it was the B component, so the  Tok2015c
                         pair has been changed to Ba,Bb.                                                 
08251+5603   STI2206     A likely plate flaw.                                                    Grv2021b
08251-4910   RST 321     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.60 +/- 0.14, 1.77, and 0.85 Msun, respectively.             Mlk2012 
08252-2403   S   568     A is a spectroscopic binary.                                                    
                         B is a K1III and is CD-23@7280.                                                 
08253+1030   BPM 443     [PM2000]  884065 + [PM2000]  884231.                                    Gvr2010 
08254+7607   MLR 547     Aka TDS5815.                                                                    
08254+3723   HU  856     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 7.12 +/- 4.20, 3.34, and 1.20 Msun, respectively.             Mlk2012 
08255-5144   DUN  69     B is CD-51@3003.                                                                
08256-5332   BRT3286     CD-53@2275.                                                                     
08258-4155   RST2553     TDS5818.                                                                        
08259+0734   H 5 109     H V 109. HJ  785.                                                               
08260-4318   DON 249     CPD-42@2480.                                                                    
08263-3904   HJ 4093     AB: A is the Algol-type system NO Pup.                                          
08264-0849   GWP1018     ABL 204.                                                                Tob2012b
08265+2754   S   566     22 Cnc = phi 1 Cnc                                                              
08265-0359   H 6 118     H VI 118. 2 Hya. Possible Delta Scuti-type variable.                            
                         BDS 4606 is the same star.                                                      
08267+2432   STF1224     24 Cnc =  ups Cnc.                                                              
             STF1224     A,BC: H 2  41.                                                          MEv2010 
             A  1746     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         BC: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.54 +/- 0.80, 2.50, and 1.13 Msun, respectively.  Mlk2012 
08267-1910   FEN  14     B. J 2640.                                                                      
08267-3155   PRO  59     CPD-31@2369.                                                                    
08268+2656   STF1223     phi 2 Cnc. Both components suspected of variability.                            
                         H 2  40.                                                                MEv2010 
08268-2252   LDS 219     B is BD-22@2275.                                                                
                         NLTT 19552/19555                                                        Chm2004 
08268-3725   ARU   6     Typo in WDS designation - originally listed as 08228-3725.                      
08270-5242   B  1606     Hipparcos parallax 18.50 +/- 0.44 mas. Dynamical parallax 17.5 mas,             
                         masses 1.61 and 1.28 Msun. The orbit by Finsen (1963) is revised here   Fin1963c
                         using the three available speckle measures, leading to a more accurate          
                         period and to the reduced orbit size. Systematic over-estimation of             
                         the separation by Finsen's visual interferometry is apparent.           Tok2012b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.96 +/- 0.45, 2.61, and 2.27 Msun, respectively.             Mlk2012 
08271+2844   FAR   6     SKF  26. Primary is white dwarf WD 0824+288.                            Far2005b
08271+0331   RUC  21     Primary is FG Hya.                                                              
08276+6235   HJ 3309     B is BD+63@799.                                                                 
08276-2051   B  2179     An eclipsing binary, VV Pyx. Aka B  1100.                                       
08277-0425   A   550     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.92 +/- 1.07, 2.89, and 1.45 Msun, respectively.             Mlk2012 
08277-0934   GWP1021     ABL 206.                                                                Tob2012b
08280-0312   GWP1022     ABL 207.                                                                Tob2012b
08280-3507   FIN 314     A spectroscopic binary, probably due to motion in the visual pair.              
                         Primary is XY Pyx, a W Uma type eclipsing binary, period 0.92254d.      Zas2012 
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 10.61 +/- 4.80, 10.39, 6.92 Msun, respectively.    Mlk2012 
08281+3332   STT 193     SEI 499. Incorrectly referred to as STF 193 by Scheiner.                Nsn2017b
08282-3643   EGN   7     Single epoch, but the A and B components are likely unrelated. A and            
                         C are unbound.                                                          Egn2007 
08283+3338   SEI 500     Not found by Heintz at IDS position.                                    Hei1987a
08283-1736   GWP1023     ABL 208.                                                                Tob2012b
08283-4430   RSS 162     AC: Also known as HDS3409AC.                                                    
08284+0026   LDS3793     Aka SLW 256.                                                            Dam2018l
08285-0231   A   551     A and B are SB's with P = 2.5 d and 6 d, respectively, and star C               
                         (mag. 10.49, 18") appears physical, so that the system is quintuple.            
                         Primary is eclipsing binary LO Hya (period 2.49956 day).                Zas2010 
                         AB,C = STF 1233.                                                                
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: All speckle measures are discordant with the published orbit of     B__1953b
                         van den Bos (1953).                                                     Hrt1992b
08286+6602   JNN 273     Estimated age 300-1000 Myr; masses 0.15 +/- 0.02 and 0.11 +/- 0.01              
                         Msun; a ~4.9 au.                                                        Jnn2014 
08286+5439   MLR 672     Also known as TDS5857.                                                          
08287+1121   BRT2143     A likely plate flaw.                                                    Grv2021b
08289-4235   HJ 4102     B is CD-42@4287.                                                                
08290+4706   GRV1005     SLW 257.                                                                        
08291+1010   BRT3376     Unnumbered pair, following BRT1250 in Barton's list.                    Brt1935a
                         A likely plate flaw.                                                    Grv2021b
08291-1219   GWP1025     ABL 209.                                                                Tob2012b
08291-3456   BRT1630     CPD-34@2548.                                                                    
08291-4756   FIN 315     One component is a spectroscopic binary.                                        
                         Aa,Ab: Docobo & Andrade (2013) derive a dynamical parallax of 3.88 +/-          
                         0.56 mas and component masses 6.08 +/- 3.43 and 5.45 +/- 3.08 Msun              
                         (for spectral type B1.5V) or 3.85 +/- 0.58 mas, 6.27 +/- 3.63 and 5.53          
                         +/- 3.20 Msun (for B2IV). See paper for extensive notes on system.      Doc2013d
08291-6152   TOK 122     HIP 41620. NOMAD: PM(B)=(-21,-3), V(B)=13.21. B is optical based on             
                         the CMDs. PM(A)=(-41,+14).                                              Tok2011a
08295-4443   DUN  70     One component is a spectroscopic binary.                                        
08296+5203   SIN  39     AC: The companion noted by Sinachopoulos & Seggewiss (1990) at (104deg, Sin1990 
                         229") is not seen on Aladin plates. This star at (102deg, 266") agrees          
                         with their magnitude estimate and appears to be the most likely                 
                         candidate for the C component.                                                  
08296-1704   GWP1026     ABL 210.                                                                Tob2012b
08296-3836   I   394     IRAS 08277-3826 = PDS 31.                                               Gre1992 
08299+3123   STF1231     SEI 502.                                                                Nsn2017b
08299-0030   J  1523     BAL 852.                                                                        
08300+2655   ALP  13     2MASSW J0829570+265510                                                          
                         Physical companionship to this ultracool dwarf ruled out based on i-z           
                         and z-J colors, using photometry from SDSS.                             AlP2007 
08301+0412   LDS5696     LDS6216.                                                                        
08303+6253   LDS2282     LDS5197.                                                                        
08303+6043   BU 1067     1 UMa = omi UMa = Muscida. A is variable.                                       
08303+2214   HRO   1     Primary is K2-34, a relatively metal-rich F star. Companion is a hot            
                         Jupiter, mass 1.773 +/- 0.086 Mjup, radius 1.44 +/- 0.16 Rjup           Hro2016 
08303-2602   B   158     ADS 6847a.                                                                      
                         Despite the linear solution, proper motion and parallax favor a         Grv2020a
                         physical connection. Long period and/or high eccentricity possible.             
08305+2818   HJ  788     B component is of spectral type K1III                                   AbH2000 
08306-4031   DUN  71     B is CD-40@4330.                                                                
08307-1610   GWP1027     ABL 211.                                                                Tob2012b
08307-4309   DON 256     CPD-42@2600.                                                                    
08308+1243   BPMA 36     [PM2000]  891033 + [PM2000]  891175.                                    Gvr2010 
08310+4012   SKF 207     For astrometric analysis of 2MASS J08310177+4012115, we compare our             
                         AstraLux measurement with the data from the original discovery as               
                         listed in the WDS. Since there are no error bars quoted, it is                  
                         difficult to formally establish physical companionship. However, even           
                         if we assume that the errors are +/-0.5" and +/-5deg, which should be           
                         very conservative, the background hypothesis can still be firmly                
                         excluded with ~5 sigma confidence. We therefore count it as a                   
                         confirmed companion.                                                    Jnn2012 
08312-1100   GWP1029     ABL 212.                                                                Tob2012b
08313-0601   LDS 221     NLTT 19692/19697                                                        Chm2004 
08313-1938   J  1524     Aravamudan gives position 08267-1916 (1900).                            Ara1963 
08313-8441   HJ 4158     B is CPD-84@192.                                                                
08314+3156   STF1236     B is BD+32@1747.                                                                
                         Additional notes may be found in Lau (1908).                            Lau1908c
08314-3642   LDS 223     C is CPD-36@2622.                                                               
08314-3904   HJ 4107     A is a spectroscopic binary.                                                    
08315-2541   I   805     AC Pyx, Algol-type eclipsing binary, P = 7.66793 d.                     Zas2011 
08316+3458   HU  716     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.58 +/- 0.23, 1.77, and 0.95 Msun, respectively.             Mlk2012 
08316+1806   HJ 2452     the Cnc = 31 Cnc. Occultation double.                                           
                         AB: H 5  59.                                                            MEv2010 
08317+1924   LDS 905     AB: NLTT 19685/19684                                                    Chm2004 
                         CU Cnc and CV Cnc. This is a known quintuple system, as reported in,            
                         e.g Delfosse et al. (1999) and Beuzit et al. (2004). Four of the        Del1999a
                         components are resolved in two separate pairs (Aa,Ab and Ba,Bb) by      Beu2004 
                         AstraLux. The fifth component is unresolved in the images; this is an           
                         eclipsing binary companion to the Aa component.                         Jnn2014 
             BEU  12     Aa,Ab: Estimated age 30-300 Myr; masses 0.20 +/- 0.09 and 0.04 +/-              
                         0.03 Msun; a ~6.0 au.                                                   Jnn2014 
             DEL   1     Ba,Bb: Estimated age 30-300 Myr; masses 0.24 +/- 0.12 and 0.18 +/-              
                         0.09 Msun; a ~10.6 au.                                                  Jnn2014 
08317-0619   TOK  21     Additional faint companion seen; not detected in J band, so concluded           
                         was probably optical.                                                   Tok2006 
08318-0347   J   416     C was not seen in 1950                                                  VBs1954 
08319+5037   CRJ   3     Primary is NLTT 19673. Crepp et al. (2012) derive spectral types G1V            
                         and M3-M4, masses 1.04 +0.06/-0.05 and 0.31 +/- 0.03 Msun.              CrJ2012 
08319+3309   STF1238     SEI 503.                                                                Nsn2017b
08319-0300   GWP1032     ABL 213.                                                                Tob2012b
08320+1620   BPM 444     [PM2000]  892430 + [PM2000]  892422.                                    Gvr2010 
08322-1750   GWP1034     ABL 214.                                                                Tob2012b
08323+1520   BPM 445     [PM2000]  892771 + [PM2000]  892635.                                    Gvr2010 
08323-7656   TOK 123     HIP 41871. Astrometric binary in Hipparcos.                                     
08324-0056   HJ   96     B is BD-00@2012.                                                                
                         AB: HJL  94.                                                            HJL1986 
                         AB: SHY 527. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AC: Rectilinear solution by Friedman et al. (2012).                     USN2012a
08326+0829   STF3119     Also known as STF3066.                                                          
08326-1502   B  2528     Likely a spurious pair. Last measured 1942 and unresolved by SOAR on 4          
                         occasions 2009-2013.                                                    Tok2010 
                                                                                                 Tok2012d
                                                                                                 Tok2014a
                                                                                                 Tok2015c
08327+2026   ZHN   3     Primary is eta Cas. First known wide pair comprised of an L dwarf and           
                         a giant.                                                                Zhn2010 
08327-5528   HDS1221     Aa = V470 Car, eclipsing binary of Algol-type, period 2.16178 days.     Zas2015
08329-0933   J  2642     RST 4407 = LDS 851.                                                             
08331-2436   BU  205     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.73 +/- 0.84, 2.64, and 1.74 Msun, respectively.  Mlk2012 
08332+3326   STF1240     AB: SEI 504.                                                            Nsn2017b
08333-1204   GWP1039     ABL 215.                                                                Tob2012b
08336-0601   GWP1040     ABL 216.                                                                Tob2012b
08338+1104   BPM 446     [PM2000]  894559 + [PM2000]  894443.                                    Gvr2010 
08339-2842   COO 282     SWR  50.                                                                        
08343-1216   GWP1043     ABL 217.                                                                Tob2012b
08344+1557   BPM 447     [PM2000]  895177 + [PM2000]  895164.                                    Gvr2010 
08344-4430   DON 263     CPD-44@2755.                                                                    
08345-3236   FIN 335     Giant primary according to isochrone fit.                                       
                         Hipparcos parallax 14.86 +/- 0.57 mas. Dynamical parallax 14.6 mas,             
                         masses 1.71 and 1.54 Msun.  We confirm and slightly correct the orbit           
                         by Soderhjelm (1999). The 17.35y period is very well defined now, but   Sod1999 
                         further coverage by speckle is still needed. The system is evolved,             
                         judging from its luminosity, estimated masses, and spectral type G5IV.          
                         The speckle dy is very consistent and preferred to dHp.                 Tok2012b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.24 +/- 0.65, 2.42, and 1.07 Msun, respectively.             Mlk2012 
                         Docobo & Andrade (2013) derive a dynamical parallax of 15.42 +/- 0.28           
                         mas and component masses 1.47 +/- 0.10 and 1.35 +/- 0.09 Msun (for              
                         spectral type G5V) or 16.24 +/- 0.39 mas, 1.26 +/- 0.11 and 1.15 +/-            
                         0.10 Msun (for G5IV). See paper for extensive notes on this system.     Doc2013d
08345-3737   I   195     Variable.                                                                       
08348+1107   BPM 448     [PM2000]  895729 + [PM2000]  895613.                                    Gvr2010 
08354+6746   LDS2283     LDS5198.                                                                        
08354+6616   STF1232     B is BD+66@559.                                                                 
08356+3116   SEI 505     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
08356+1024   BPM 449     [PM2000]  896580 + [PM2000]  896563.                                    Gvr2010 
08356-0648   LDS3800     Aka GWP1046 and ABL 218.                                                Tob2012b
08358+0637   STF1245     GJ 9271. Visual pair has estimated period of 2500y.                     Tok2006 
                         AB: HJL  95.                                                            HJL1986 
                         HIP 42172. B = HIP 42173.                                               Tok2011a
                         AB: H 3  49.                                                            MEv2010 
                         AB: A is SB2, P=14.296d                                                 Tok2014d
08360+2050   BOV  29     Praesepe VL 184 = NGC 2632 BDA 1184                                             
                         SB1, P = 1:23 d                                                         Bov2001 
08360-1027   GWP1048     ABL 219.                                                                Tob2012b
08360-2211   B  2182     CPD-21@3748.                                                                    
08360-5337   LPO  70     Spectrum: G2/5(III)+A.                                                          
08361-0334   LDS6217     A may be a close double, 50 deg., 2", mag. diff. 0.7.                   Luy1979 
                         NLTT 19864/19867                                                        Chm2004 
08362+1347   STTA 94     B is BD+14@1930.                                                                
08362+1344   BPM 450     [PM2000]  897256 + [PM2000]  897210.                                    Gvr2010 
08363+1933   BOV  30     Praesepe KW 533 = NGC 2632 BDA 533                                              
                         SB2, long period                                                        Bov2001 
08364+3703   SEI 506     Duplicity not apparent on POSS plate; one component may be either               
                         variable star or flaw on AC Potsdam plate.                                      
08364-0306   RST4413     J 1528.                                                                         
08366-1540   GWP1049     ABL 220.                                                                Tob2012b
08367+1643   BPM 451     [PM2000]  897859 + [PM2000]  897884.                                    Gvr2010 
08368+7443   STT 192     A is a spectroscopic binary.                                                    
                         Additional notes may be found in Baize (1939).                          Baz1939a
08369-1154   GWP1050     ABL 221.                                                                Tob2012b
08369-3050   I    68     Spectrum: A3mA7-F2/3.                                                           
08369-3135   JSP 285     same as TDS5983 with a quadrant flip.                                   Dam2018k
08369-7857   KOH  79     KOH  80.  EG Cha.  Wide pair is likely a chance alignment.              Bnk2006 
                         AB: Koehler & Petr-Gotzens (2002) calculate two possible orbital        Koh2002 
                         solutions. The short-period solution gives a semi-major axis of 15.5au          
                         and a mass sum of 2.1 Msun; the longer-period solution gives 37.6au             
                         and 2.3 Msun.                                                                   
08372+2017   BOV  31     Praesepe KW 540 = NGC 2632 BDA 540                                              
                         SB1, P = 1149 d                                                         Bov2001 
08372-4147   CPO 218     TDS5986.                                                                        
08374-0400   GWP1051     ABL 222.                                                                Tob2012b
08375-5336   HJ 4123     B is CPD-53@1782.                                                               
08377+1931   HJ  454     A is a Delta Scuti-type variable.                                               
08377+0542   BUP 118     del Hya = 4 Hya. A spectroscopic binary.                                        
08378+1409   HLD  97     Position corrected by Heintz                                            Hei1983a
08379-0648   HJ   99     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
08379-2615   RST2571     eta Pyx                                                                         
             VIG  11     The C, E, and F components all appear to be faint background stars;             
                         the D component appears to be co-moving. The mass of D is estimated at          
                         0.07-0.11 Msun.                                                         Vig2012 
08380-0736   GWP1054     ABL 224.                                                                Tob2012b
08380-1750   GWP1053     ABL 223.                                                                Tob2012b
08380-2739   TOK 124     HIP 42344. The ANDICAM position in the V-band is not accurate. NOMAD:           
                         PM(B)=(0,+28), V=16.70, but B is definitely physical. PM(A)=(-147,+95)  Tok2011a
08381+1959   BOV  34     Praesepe KW 79 = NGC 2632 BDA 79                                                
                         Photometric binary                                                      Bov2001 
08382+1922   BOV  35     Praesepe KW 90 = NGC 2632 BDA 90                                                
                         Photometric binary                                                      Bov2001 
08382+1511   RDN   3     Radigan et al. (2013) determine that A and BC appear to share common            
                         proper motion and conclude all components are physically associated.            
                         Derived distance (spectroscopic parallax) is 49 +/- 12 pc. Derived NIR          
                         spectral types and masses (for ages 3 Gyr and 300 Myr) are:                     
                         A  T3   +/- 1   0.060 +/- 0.009 Msun   0.020+/- 0.005 Msun                      
                         B  T3   +/- 1   0.055 +/- 0.008        0.018+/- 0.005                           
                         C  T4.5 +/- 1   0.050 +/- 0.008        0.016+/- 0.004                   Rdn2013 
08386-0249   GWP1056     ABL 225.                                                                Tob2012b
08386-3505   JSP 286     Also known as RSS 167.                                                          
08388-1315   SHY 201     HIP  42401 + HIP  41662.                                                        
08388-3352   B  1621     1995.1160: Quadrant determined by speckle imaging analysis.             Hor1996 
08388-7221   GLI  99     Aka TRR  12.                                                            Dam2018l
08389-1002   GWP1057     ABL 226.                                                                Tob2012b
08391+2000   HD  73430   Praesepe KW 143 = NGC 2632 BDA 143                                              
                         Praesepe cluster member and occultation binary. Peterson & White        Pts1984 
                         (1984) found a vector separation in April 1982 of 0".044, which should          
                         have been resolvable by us unless the system closed. They find                  
                         magnitude differences (noted as unreliable) of 2.5 mag at 445 nm and            
                         0.35 mag at 750 nm, which if correct would not have prevented us from           
                         seeing the companion.  Incorrectly noted as HD 73460 in text, although          
                         the tabular information is correct.                                     Msn1993b
08391+1418   BPM 452     [PM2000]  900491 + [PM2000]  900455.                                    Gvr2010 
08391-2240   BU  208     CPD-22@3750. Newburg finds little evidence for the perturbation         Nbg1968b
                         suspected by Hirst (1943).                                              Hir1943d
                         AB: A is suspected SB, P=106d? (Abt & Willmarth 2006). Fuhrmann (2011   AbH2006 
                         MNRAS 411, 2311)says Aa,Ab has period few hundred days.                 Tok2014d
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
08391-5557   HU 1443     A,BC is a triple system. We provide the first very tentative orbit for          
                         the outer binary, but note its large residuals from the recent                  
                         measures of AB. Strictly speaking, the orbit should describe the                
                         motion of the center-of-gravity of BC around A, rather than the                 
                         measures of AB. Such refinement was made for the orbit of A 2592 AB             
                         (17156-0949)}, but it is not warranted for this preliminary orbit.      Tok2015c
08391-7023   DON 271     the Vol                                                                         
             HJ 4134     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
08392-0317   GWP1060     ABL 227.                                                                Tob2012b
08392-4025   B  1623     Eggen (1982) assigns this star to a group associated with the cluster   Egg1982 
                         IC 2395 at distance of 0.8 kpc.  The Hipparcos Catalogue contains a     HIP1997a
                         light curve with a period of 1.46 d.                                    Msn1998a
                         Includes NX Vel, an Algol-type eclipsing binary, P = 2.91992d.          Zas2012 
                         NX Vel is a quadruple system formed by the 0.65" pair, that contains            
                         an eclipsing pair (Otero 2003, IBVS 5480, 1; P~2.9d) and an SB (Sota            
                         et al. 2014, ApJS 211, 10; P=20.6d).                                    Sna2014 
08394-0935   RST4415     Algol-type eclipsing binary, P = 92.1711 d.                             Zas2011 
08394-3636   I   314     Only elements P, T, and a of Heintz (1968) were adjusted for            Hei1968a
                         Starikova (1981) solution.                                              Sta1981a
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Heintz (1968).                                                          Hei1968a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.79 +/- 0.50, 2.01, and 1.51 Msun, respectively.             Mlk2012 
08395-2100   RST5506     CPD-20@3936.                                                                    
08397+2005   COU  47     In Praesepe.                                                                    
08397+0546   STF1255     AB: HJL  96.                                                            HJL1986 
                         AB: H 4  54.                                                            MEv2010 
08397-2934   HJ 4120     zet Pyx. B is CD-29@6545.                                                       
08398+1131   ENG  36     AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
08399+1933   BU  584     In Praesepe.                                                                    
                         DC: D is variable. Position (2000): 08 39.8 +19 32. In Praesepe.                
             S   571     STTA 95. C is a spectroscopic binary, and is +20@2153.                          
                         AC: HJL  97.                                                            HJL1986 
             CHR 156     Da: No published evidence of RV variation. Noted as occultation binary          
                         by Peterson & White (1984). Magnitude differences of 3.1 in blue and    Pts1984 
                         Magnitude differences of 3.1 in blue and 3.8 in red reported by                 
                         Peterson et al. (1989) are consistent with our difficulty in detecting  Pts1989 
                         the faint secondary. Praesepe cluster member.                           Msn1993b
08400-5303   HJ 4126     A is a spectroscopic binary, and is variable.                                   
08401+2000   ENG  37     A: 39 Cnc. A variable?                                                          
             CHR  28     B: 40 Cnc. Praesepe cluster member with excess luminosity. The                  
                         1986.8922 measure is from reanalysis of archival data. Frequently               
                         unresolved, due to large delta m.                                       Msn1993b
08401-3518   RST4894     bet Pyx. A is a spectroscopic binary.                                           
08401-7218   GLI 100     Spectrum: G8/K0III+A.                                                           
08402+5147   OPI  16     AC: The C component is the primary of 08404+5145 ES  909AB.                     
08404+5145   ES  909     The primary is also the C component of 08402+5147 OPI  16AC.                    
08403+1947   BOV  41     Praesepe KW 275 = NGC 2632 BDA 275                                              
                         Photometric binary                                                      Bov2001 
08403+1921   CHR 130     Praesepe cluster member with anomalous occultation behavior (Appleby            
                         1980 JBAA, 139, 1139). The 1984.0607 and 1986 measure are from                  
                         reanalysis of archival data. Peterson et al. (1989) measured            Pts1989 
                         magnitude differences of 1.9 in blue and red.                           Msn1993b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 13.18 +/- 7.09, 4.10, and 1.51 Msun, respectively.            Mlk2012 
08403-4358   CPO 222     CPD-43@2853.                                                                    
08404+5145   ES  909     The primary is also the C component of 08402+5147 OPI  16AC.                    
08404+1940   STF1254     Algol-type eclipsing binary,  per 7.2209 d.                             Zas2011 
                         Physical with BD+20@2158. A is a spectroscopic binary.                          
             BOV  42     Ba. Praesepe KW 287 = NGC 2632 BDA 287                                          
                         SB1, P = 7635 d                                                         Bov2001 
08404-0641   GWP1063     ABL 228.                                                                Tob2012b
08404-4223   DUN  72     B is CD-41@4370.                                                                
08405+2019   BOV  45     Praesepe KW 297 = NGC 2632 BDA 297                                              
                         SB1, long period                                                        Bov2001 
08405+1933   CIA  28     Aa,Ab : Mass of Aa determined to be 2.420 +/- 0.008 \msun.                      
                         Aa,Ab : Mass of Ab determined to be 2.226 +/- 0.004 \msun.                      
                         Distance 183.1 +/- 0.35 pc.                                             CIA2022c
             S   574     eps Cnc = 41 Cnc = Meleph, a spectroscopic binary. B is BD+20@2163.             
08405-2255   BRT1466     CD-22@6471.                                                                     
08406-5946   JSP 295     A is a spectroscopic binary and variable, V343 Car.                             
08407+1940   Praesepe... Praesepe KW 322 = NGC 2632 BDA 322                                              
                         SB1, P > 10 000 d                                                       Bov2001 
08408+1940   BOV  47     Praesepe KW 334 = NGC 2632 BDA 334                                              
                         Photometric binary                                                      Bov2001 
08408-1334   BRT1906AB   A likely plate flaw.                                                    Grv2021b
08408-1605   GWP1065     ABL 229.                                                                Tob2012b
08408-4504   SNA   6     The primary is the high-mass X-ray binary LM Vel. This O8.5Ib-II(f)             
                         star presents RV variations (Barba et al. 2006, The Astronomer's                
                         Telegram 819, 1) and is an SB candidate. It has been suggested as the           
                         possible counterpart of the fast X-ray transient IGR J08408-4503                
                         (Masetti et al. 2006, The Astronomer's Telegram 819, 1).                Sna2014 
08409-1619   ALD  38     Aka OSO  22.                                                            Dam2018m
08411+1904   BOV  48     Praesepe KW 365 = NGC 2632 BDA 365                                              
                         Triple, A: SB1O, B: single                                              Bov2001 
08411-0430   GWP1066     ABL 230.                                                                Tob2012b
08412-3005   B  1105     Spectrum: B8/9II/III.                                                           
08413+7614   MLR 548     Also known as TDS6037.                                                          
08413+2029   BU  585     Spectroscopic binary. Praesepe cluster member.                                  
                         1991.3184: Although the peak remains convincing, we  have been unable           
                         to confirm this measure, perhaps due to either a variable secondary or          
                         to the star closing within our resolution limit.                        Msn1993b
08413-1646   GWP1067     ABL 231.                                                                Tob2012b
08413-7858   BNK   3     AB: eta Cha. Likely a chance alignment object.                          Bnk2006 
             SHY 528     AC: HIP  42637 + HIP  42794.                                                    
             BNK   7     CD: The primary of 08432-7904 BNK   7 was found to be the C component           
                         of 08413-7858 SHY 528AC. As the AC pair appears physical, the systems           
                         were merged.                                                                    
                         CD: RS Cha. Likely a chance alignment object.                           Bnk2006 
08414+6426   LDS2288     LDS5199.                                                                        
08414-1927   RSS 169     CPD-19@3721                                                                     
08414-4732   RST 341     CPD-47@2539.                                                                    
08414-5736   JNN  62     The two components of this system have nearly equal colors and                  
                         brightnesses, hence they very likely form a physical pair, although             
                         they have not yet been tested for common proper motion.                 Jnn2012 
08415-2809   SEE 101     Aka B  2666.                                                            Dam2018k
08416-7904   BNK   4     EH Cha. Likely a chance alignment object.                               Bnk2006 
08417-1237   ALD  39     BRT 2711.                                                                       
08417-1557   HJ 4124     9 Hya.                                                                          
08417-2018   J  2645     CPD-19@3728.                                                                    
08418+1952   HD  73974   Praesepe KW 428 = NGC 2632 BDA 428                                              
                         Praesepe K0 giant and occultation binary.  Peterson & White (1984)      Pts1984 
                         found a projected separation in April 1982 of 0".018, which could lead          
                         to a true separation below our resolution limit.                        Msn1993b
08419+3546   SEI 508     Secondary not seen on POSS plate; may be either variable star or flaw           
                         on AC Potsdam plate.                                                            
08421-1552   GWP1068     ABL 232.                                                                Tob2012b
08421-4256   EGN   8     C and D components are both background stars.                           Egn2007 
08421-4543   DON 272     CPD-45@2858.                                                                    
08421-5245   B  1624     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.98 +/- 0.24, 1.96, and 0.98 Msun, respectively.             Mlk2012 
08421-6200   HRG  18     Spectral type F8?                                                               
08423-4806   RST5304     A variable, HX Vel.                                                             
08424-5307   BSO  18     A is a variable, HY Vel. B is CD-52@1605.                                       
             B  1625     BC: Position 08 42.3 -53 06.                                                    
08424-7904   BNK   5     EI Cha. Likely a chance alignment object.                               Bnk2006 
08425-0830   H 6 107     H VI 107. B is BD-08@2463.                                                      
08427+0935   ST    8     KUI.                                                                            
             LUY6218     AB,C: SHY  48. Bayesian analysis by Shaya & Olling (2011) indicates     Shy2011 
                         very high (near 100%) probability pair is physical.                             
08428+3152   RAO 501     KX Cnc.                                                                         
08431+1926   BOV  53     Praesepe KW 495 = NGC 2632 BDA 495                                              
                         Triple, A: single, B: SB2                                               Bov2001 
08431-7905   BNK   6     EM Cha. Likely a chance alignment object.                               Bnk2006 
08433+2128   ENG  38     43 Cnc = gam Cnc = Asellus Borealis. A is a spectroscopic binary.               
                         B is BD+21@1897.                                                                
08433-3908   GC 12009    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
08433-7905   BNK   8     ET Cha. Both companions are likely chance alignment objects.            Bnk2006 
08434-2743   TDS6057     SWR  53. CPM pair                                                       Skf2004 
08437-0031   GWP1070     ABL 233.                                                                Tob2012b
08437-0714   S   579     B is BD-06@2707.                                                                
                         AB: H 6  82.                                                            MEv2010 
08437-2316   BRT1468     CD-22@6539.                                                                     
08438-1923   GWP1071     ABL 234.                                                                Tob2012b
08438-5038   BRT 743     CPD-50@1746.                                                                    
08439+8614   STF1150     Distance uncertain.                                                             
08439+1902   BLL  26     A is an Algol-type system, S Cnc.                                               
08441-0412   A   552     Orbital motion. A difficult pair, < 0.1" in 1953, 1954.                         
08441-1506   GWP1072     ABL 235.                                                                Tob2012b
08442+0414   BAL2823     Measure by Sil1931 was incorrectly identified as 08465+0419STF1267.     Sil1931 
08443-1327   J  2062     BRT 2712.                                                                       
08443-4544   DON 277     CPD-45@2933.                                                                    
08443-7859   BNK   9     EN Cha. Wide companion is likely chance alignment.                      Bnk2006 
08444-5957   HJ 4139     B is CPD-59@1097.                                                               
08445+2827   STF1266     BDS 4792, H IV 118 same star.                                                   
                         H 4 118.                                                                MEv2010 
08445+2012   SLE 339     Algol-type eclipsing binary, period 1.2065 d.                           Zas2019 
08445-6550   EHR  12     Physical/optical nature of AB and AC both undefined.                    Ehr2010 
             TOK 520     AD: D component is the primary of 08465-6605 RST 354.                           
08445-7850   BNK  10     EO Cha. Likely a chance alignment object.                               Bnk2006 
08446-3758   JSP 298     The B component is a likely cataclysmic variable and may be optical.            
08446-4541   DON 279     TDS6073 (merged 2008/06/25)                                                     
08447+1809   TOK   3     Aa,Ab: del Cnc = 47 Cnc = Asellus Australis.                                    
             HJ  457     AB: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
08447-2126   HDS1260     AB + TOK 395: Like WDS 08021-1710, the late-type nearby binary HDS              
                         1260 was discovered by Hipparcos and is expected to move rapidly (HIP           
                         42910, BD-20 2665). It was targeted at SOAR for the first time. To our          
                         surprise, the object turned out to be a resolved triple, with the               
                         secondary being a 0".16 pair of equal stars. Hipparcos failed to                
                         recognize the triple nature of this star. The estimated period of BC            
                         is 15yr. The outer pair AB has closed from 0".8 to 0".5 and moved in            
                         position angle since its discovery. The separations between components          
                         are comparable, so this triple system may be interesting dynamically.   Tok2015c
08447-4117   I   815     CPD-40@2823.                                                                    
08447-4238   CHR 238     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.36 +/- 0.77, 1.84, and 0.85 Msun, respectively.             Mlk2012 
08447-5443   I    10     AB: del Vel = Alsephina.                                                        
                         The close pair of Tango et al. (1979), originally thought to be a new   Tng1979 
                         close pair (and called TNG 1), was determined to be the Innes pair              
                         with a reflection around the E/W axis.  This problem was first noticed          
                         by Mike Kerr in a private communication to B. Mason.                            
                         Quoted errors in P and a are +14/-11y, +0".03/-0".01.                   Ary2002b
                         AB: Kervella et al. (2013) measured separations between the A and B             
                         components, then based on their orbit of AB derived apparent                    
                         displacements of the center of light of the eclipsing Aa,Ab pair.       Krv2013 
             KEL   1     Aa,Ab: Eclipsing binary. Interferometric solution by Kellerer et al.    Kel2007 
                         (2007), using data from the VLTI/VINCI (K-band, 155m baseline) taken            
                         in April/May 2003. Semimajor axis given as (5.4 +/- 0.5) x 10^10 m,             
                         converted to mas using parallax of 40.90 mas. Aa and Ab are thought to          
                         be of spectral types A0V and A1V, but model fit yields stellar                  
                         diameters of 6.0 +/- 0.5 and 3.3 +/- 0.6 Dsun, larger than would be             
                         expected for main-sequence stars. Authors also conclude that C and D            
                         components of the system are much further away than Aa+Ab+B, so are             
                         not physically associated with the close triple.                                
                         Aa,Ab: Properties of components Aa, Ab, and B are as follows:                   
                         Spectral types: A2IV           A4V            F8V                               
                         M/Msun:         2.5  +/- 0.1   2.0  +/- 0.1   1.3  +/- 0.1                      
                         L/Lsun:         59.2 +/- 2.0   20.0 +/- 0.7   3.1  +/- 0.2                      
                         R/Rsun:         3.17 +/- 0.08  2.02 +/- 0.05  1.39 +/- 0.06                     
                         Teff (K):       9000 +/- 400   8600 +/- 350   6350 +/- 350              Krv2009 
                         Aa,Ab: Masses 2.43 +/- 0.02 and 2.27 +/- 0.03 Msun, luminosities                
                         67. +/- 1. and 51. +/- 1. Lsun, parallax 39.8 +/- 0.4 mas                       
                         Mass sum (Aa+Ab+B) = 6.15 +/- 0.23 Msun, assuming derived parallax.     Mrd2011 
             SHY  49     AF: HIP  42913 + HIP  43797.                                                    
08448+5532   PIN   4     Primary is variable star LT UMa.                                                
08448-0110   GWP1075     ABL 236.                                                                Tob2012b
08449-4050   WG  111     BRT 744.                                                                Brt1933 
08449-4621   KRV  22     Classical Cepheid SX Vel.                                                       
08452+4140   STF1263     B is BD+42@1923.                                                                
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
08453-0018   HEI 147     Heintz believes Aitken and van den Bos may have observed this pair              
                         instead of +00@2380.                                                    Hei1983a
08453-0236   STF1270     HJL  98.                                                                HJL1986 
                         HIP 42951. Very small PM(A)=(+1,-9). B is considered physical based on          
                         the CMDs and its brightness.                                            Tok2011a
                         A = MX Hya, Algol-type, depth 0.5mag.  Rucinski (2002 PASP 114,                 
                         1124) gives period of MX Hya 0.7960d. So far, no estimates of the mass          
                         ratio for Aa,Ab, no SB orbit. dHp=0.49mag.                              Tok2014d
08453-0432   GWP1076     ABL 237.                                                                Tob2012b
08454+6001   MLB 163     LDS1218.                                                                        
08459-0032   GWP1078     ABL 238.                                                                Tob2012b
08460+6945   LDS1681     NLTT 20128/20129                                                        Chm2004 
08460+6445   VBS  42     Incorrectly identified as H 4  60 in BDS. Error noted by MacEvoy.       MEv2010 
08461+0748   J   735     B brighter than A in K, redder. A,B both on the MS. B could be SB2.     Tok2014d
08461-0230   ITF  83     Aka ITF  86.                                                                    
08461-4653   CPO 232     CPD-46@2963.                                                                    
08462+1915   STF1269     Chevalier's separation is actually 11".58 rather than 23".68. This      Che1908 
                         pair is identical with STF1269, but the incorrect published value for           
                         led to a match with a nearby pair which roughly agreed with the                 
                         Chevalier measure, and its publication as 08467+1914 CHE 507. Measures          
                         have been merged.                                                       Hrt2012b
08464-0852   GWP1079     ABL 239.                                                                Tob2012b
08464-1333   RST5507     12 Hya. A is a spectroscopic binary.                                            
08464-1413   BRT2713     J 2887.                                                                         
08465+6437   LDS2292     LDS5200.                                                                        
08466-4234   JC   13     Also classed B4V.                                                               
08467+2846   STF1268     iot Cnc. B is BD+29@1823, spectral type A3V.                                    
                         HJL  99.                                                                HJL1986 
                         H 4  52.                                                                MEv2010 
08468+0625   SP    1     eps Hya = 11 Hya. Variable.                                             Dan1952 
                         The elements for AB are combined visual-spectroscopic.                  Hei1963c
                         A secondary radial velocity variation with a period of about 70d                
                         was suspected by Underhill (Pub. DAO Victoria 12, 161, 1963)            Fin1970b
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
             STF1273     C is SB1, P = 9.905 d.                                                          
                         AB,C triple solution ((AB)-C in HIP).                                   Sod1999 
                         Star D is in slow direct motion, hence quintuple.                               
08468-0219   GWP1080     AB: ABL 240AB.                                                          Tob2012b
             GWP1081     AC: ABL 240AC.                                                          Tob2012b
08469+4225   LDS3816     NLTT 20202/20201                                                        Chm2004 
08469+1753   CUD   4     Central star of the planetary Nebula Abell 30.                                  
08469-2641   VSP   4     Aa,Ab  : Ab component identified with M = 25+/-5 \MJup, radius of       VSP2020b
                         2+/-0.5 \Rjup, spectral type M6-L2, and orbital period of 130 +/- 90y.          
             KOU  74     AB : Orbital period estimated as 8000 +/- 300 y.                        VSP2020b
                         Mass of A & B are 1.92 and 0.3 \msun.                                   Kou2005 
08470-3846   B  2186     The nf star of CD-38@4867.                                                      
08471-0747   GWP1082     ABL 241.                                                                Tob2012b
08471-4032   WG  114     CPD-40@2867.                                                                    
                         Possible typo in the AC catalog used to generate the WG measure. The            
                         AC2000 coordinates in Aladin agree with the WG measure, but the                 
                         secondary coordinate and the actual star position are about 20" apart,          
                         due north-south of each other.                                                  
08474-4143   CPO 233     CPD-41@2968.                                                                    
08476+0001   STF1281     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             RST5306     The C component of 08476+0001. WDS designation changed from 08476+0005          
                         and this pair given component designations Ca,Cb.                               
08476-0721   GWP1085     ABL 242.                                                                Tob2012b
08476-1859   LDS 235     NLTT 20261/20260                                                        Chm2004 
08477-4144   MUG   6     Theta approximate ("east"). Based on relative motion between 1999               
                         2MASS data and two measures with NTT in 2002, Mugrauer et al. (2004)    Mug2004b
                         conclude the B component is a CPM companion to the planet host star             
                         HD 75289. Assuming distance of 28.94 +- 0.47pc, this corresponds to a           
                         separation of 621 au. Mass of B ~0.135 +- 0.003 Msun. Additional                
                         photometry and astrometry compiled from 2MASS catalog.                          
                         Exoplanet host, P=3.5d. Large motion (diff. with 2MASS). Optical?               
                         Roell et al. (2012 A&A 542, A92) consider B physical (no PM), as do     Rag2006 
                         Raghavan et al. (2006).                                                 Tok2014d
08479-7855   BNK  11     EQ Cha. Koehler & Petr-Gotzens (2002) suspected duplicity but were      Koh2002 
                         unable to split the pair.                                                       
                         More commonly known as EQ Cha, this star appears single in the                  
                         AstraLux images, but has most likely been partially resolved as close           
                         binary in previous imaging campaigns (Kohler & Petr-Gotzens 2002;       Koh2002 
                         Brandeker et al. 2006). With an angular separation as small as 40 mas   Bnk2006 
                         in 2003, it is fully plausible that the companion exists but was too            
                         close to be resolved by AstraLux in 2010.                               Jnn2012 
08480-3115   SHY 529     AC: HIP  43193 + HIP  43316.                                                    
08481+1757   BPM 453     [PM2000]  909715 + [PM2000]  909682.                                    Gvr2010 
08481-0647   GWP1086     ABL 243.                                                                Tob2012b
08484+0550   AGC   3     rho Hya = 13 Hya. A is a spectroscopic binary, P = 8.2d.                        
08485+1449   BPM 454     [PM2000]  910131 + [PM2000]  910071.                                    Gvr2010 
08486+0237   A  2551     Rapid motion. Quadrant ambiguity, but it appears that at least one              
                         revolution is complete.                                                         
08486-1353   JNN  64     B: LP 726-12.                                                                   
                         Ba,Bb: 2MASS J08483696-1353087 and J08483645-1353083 are separated by           
                         only 7", the former is a close binary (as of yet unconfirmed by common          
                         proper motion) and the latter is single, so this is likely a triple             
                         system in reality.                                                      Jnn2012 
08487+0057   A  2552     Aitken's angles 1913-1935 should all be put in the third quadrant.      B__1963b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.29 +/- 0.91, 2.59, and 1.20 Msun, respectively.             Mlk2012 
08494-6216   HJ 4147     CD-61@2042.                                                                     
08495-2054   J  1532     08496-2055ARA1061.  Hyderabad -21@ 8h 44m, Nos 43175-176.                       
08497-0852   GWP1087     ABL 244.                                                                Tob2012b
08497-4249   RSS  10     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
08499+1450   STF1283     H 4 111.                                                                MEv2010 
08499-1928   GWP1089     ABL 245.                                                                Tob2012b
08500+1752   KU   33     B is an Algol-type eclipsing binary, period 5.22474 d.                  Zas2019 
08500+1155   BPM 455     [PM2000]  911727 + [PM2000]  911657.                                    Gvr2010 
08500-0322   GWP1090     ABL 246.                                                                Tob2012b
08502+1219   HJ 2469     Not found by Heintz at IDS position.                                    Hei1990b
08502-0214   J  2065     BAL 512.                                                                        
08503+1057   SKF 363     Aa,Ab: NLTT 20346. Faherty et al. (2011) derive distance estimates for  Fah2011 
                         Aa and Ab of 28 +/- 5 and 33 +/- 5 pc, respectively, and estimate               
                         spectral types at M5 +/- 0.5 and M6 +/- 0.5.                                    
             FAH   1     AB: Faherty et al. (2011) also determine a distance for RED 10 of 29    Fah2011 
                         +/- 7 pc; similar distance and proper motions indicate SKF 363 and              
                         RED 10 form a likely CPM pair at a distance of 248".                            
             RED  10     Ba,Bb: 2MASSs J0850359+105716                                                   
                         Ba component is an L6V brown dwarf; LRIS spectrum shows that other              
                         component is a background M star.                                       Kir1999 
                         Reid et al (2002) observations from HST and WFPC2. Paper includes mass  Red2001 
                         and age estimates, as well as discussion of L dwarf binary frequency            
                         and semimajor axis distribution.                                                
                         Burgasser et al. (2011) derive spectral types of L7 and L6, masses      Bug2011 
                         0.06 +/- 0.02 and 0.05 +/- 0.02 Msun, effective temperatures                    
                         1770 +/- 200 and 1400 +/- 170K.                                                 
                         Ba,Bb: Assuming a parallactic distance of 38.1 +/- 7.3 pc                       
                         (Vrba et al. 2004), Konopacky et al. (2010) derive a system mass of     Vrb2004 
                         0.2 +/- 0.2 Msun.                                                       Kon2010 
08503+0125   J    74     Pair measured in 1947 is indeed the BD+01 2181 observed previously.             
                         Pair is -42s, +4' from BD+02 2072. movement is perhaps rectilinear.     J__1949a
                         Rectilinear solution by Cvetkovic et al. (2017).                        Cve2017 
08503-0156   J  1350     BAL 513. J 2595.                                                                
08503-4349   CPO 236     CPD-43@3034.                                                                    
08504+1123   HJ 2470     CHE 114. Chevalier pair originally copied to catalog with 10' error in          
                         declination (08504+1133).                                                       
08504-0002   HJ 3314     HJL 100.                                                                HJL1986 
08504-0210   J  1533     BAL 514.                                                                        
08504-0440   GWP1091     ABL 247.                                                                Tob2012b
08504-4205   SNA   7     The object is marginally resolved with rho~0.5mas, although with large          
                         relative uncertainty. Given the distance of 947pc (Sota et al. 2014,            
                         ApJS 211, 10) this pair probably  corresponds to the known SB2                  
                         (P=33.1d, a1+a2 sin i = 0.6au; Thackeray et al. 1966, MNRAS 134, 97).   Sna2014 
                         The classification is from Thackeray (1966 MNRAS 134, 97).  The star    Egg1982 
                         is part of a group associated with the cluster IC 2395 (Eggen 1982)     Msn1998a
08505+2308   AG  157     At some time between 1961 (IDS) and the 1984 version of the WDS, the            
                         two Espin pairs 23505+5023ES  926AC and AD were erroneously also added          
                         to this system as 08505+2308ES 2630AC and AD. The reason is unknown.    Es_1910b
08505-3813   JSP 307     A is variable.                                                                  
08506+1211   CHE 115     Based on a check of coordinates for other objects flagged as                    
                         Durchmusterung stars, Chevalier's coordinates are very accurate for     Che1911 
                         this plate. There are no obvious errors in applying the offset from             
                         the plate center, but there are no pairs at Chevalier’s coordinates,    .     
                         nor at coordinates found by reversing the sign of either or both                
                         offsets.  The pair is likely lost.                                      Hrt2012b
                         Coordinates found to be off in dec by ~9arcmin.                                 
08506-4632   HDO 205     The classification is from Conti et al. (1977).  Part of an eclipse     Cti1977 
                         was observed by Balona & Laing (1986 MNRAS 223, 621); the orbital               
                         ephemeris is discussed by Mayer et al. (1997 A&A 320, 109).             Msn1998a
                         The primary is the variable star KX Vel.                                        
08507+1800   A  2473     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 72.60 +/- 61.48, 7.81, and 0.95 Msun, respectively.           Mlk2012 
08507+0752   VDK   3     A premature orbit has been computed.                                    Cou1953d
08508+1143   BPM 456     [PM2000]  912512 + [PM2000]  912473.                                    Gvr2010 
08509+1152   BPM 457     [PM2000]  912707 + [PM2000]  912762.                                    Gvr2010 
08510+3053   HJ  459     SEI 511.                                                                Nsn2017b
08510+1159   BPM 458     [PM2000]  912736 + [PM2000]  912621.                                    Gvr2010 
08510+1150   BPM 459     [PM2000]  912825 + [PM2000]  912775.                                    Gvr2010 
08510+1148   BPM 460     [PM2000]  912844 + [PM2000]  912913.                                    Gvr2010 
08510-0147   GWP1092     ABL 248.                                                                Tob2012b
08511+1146   BPM 462     [PM2000]  912881 + [PM2000]  912908.                                    Gvr2010 
08511+1145   BPM 463     [PM2000]  912886 + [PM2000]  912785.                                    Gvr2010 
08511-0056   GWP1093     ABL 249.                                                                Tob2012b
08512+1149   BPM 461     BD: [PM2000] 913012  + [PM2000]  912857.                                Gvr2010 
                         Secondary of 08510+1149 BPM 461 found to be secondary of 08512+1149             
                         CHE 118 AB. Systems merged, with quadrant flipped 180deg for BPM 461.           
08512-1448   GWP1094     ABL 250.                                                                Tob2012b
08513+1153   BPM 481     [PM2000]  913301 + [PM2000]  913350.                                    Gvr2010 
08513+1152   BPM 474     [PM2000]  913236 + [PM2000]  913266.                                    Gvr2010 
                         Primary is D component of 08513+1150 BPM 464BD.                                 
08513+1151   BPM 467     BC: [PM2000]  913188 + [PM2000]  913213.                                Gvr2010 
             BPM 468     BD: [PM2000]  913188 + [PM2000]  913337.                                Gvr2010 
08513+1150   BPM 475     AB: [PM2000]  913241 + [PM2000]  913165.                                Gvr2010 
             BPM 476     AC: [PM2000]  913241 + [PM2000]  913284.                                Gvr2010 
             BPM 464     BD: [PM2000]  913165 + [PM2000]  913236.                                Gvr2010 
                         D component is primary of 08513+1152 BPM 474.                                   
08513+1149   BKO  38     AB: B component is H component of 08514+1148 BPM 487BH.                         
             BPM 472     AC: [PM2000]  913227 + [PM2000]  913148.                                Gvr2010 
             BPM 473     AD: [PM2000]  913227 + [PM2000]  913158.                                Gvr2010 
             BPM 483     AE: [PM2000]  913227 + [PM2000]  913343.                                Gvr2010 
             BPM 484     AF: [PM2000]  913227 + [PM2000]  913366.                                Gvr2010 
             BPM 485     EF: [PM2000]  913343 + [PM2000]  913366.                                Gvr2010 
08513+1146   BPM 470     CE: [PM2000]  913215 + [PM2000]  913334.                                Gvr2010 
                         B component is G component of 08514+1146 BPM 466FG.                             
                         E component is C component of 08514+1148 BPM 490AC.                             
08513+1145   BPM 482     [PM2000]  913302 + [PM2000]  913225.                                    Gvr2010 
08513+1144   BPM 465     [PM2000]  913178 + [PM2000]  913328.                                    Gvr2010 
08513+1126   BPM 471     [PM2000]  913217 + [PM2000]  913042.                                    Gvr2010 
08514+1149   BPM 495     [PM2000]  913426 + [PM2000]  913355.                                    Gvr2010 
08514+1148   BPM 489     AB: [PM2000]  913415 + [PM2000]  913379.                                Gvr2010 
             BPM 490     AC: [PM2000]  913415 + [PM2000]  913334.                                Gvr2010 
                         C component is E component of 08513+1146 BPM 470CE.                             
             BPM 491     AD: [PM2000]  913415 + [PM2000]  913345.                                Gvr2010 
             BPM 492     AE: [PM2000]  913415 + [PM2000]  913346.                                Gvr2010 
                         E component is E component of 08515+1151 BPM 505AE.                             
             BPM 493     AF: [PM2000]  913415 + [PM2000]  913566.                                Gvr2010 
             BPM 494     AG: [PM2000]  913415 + [PM2000]  913565.                                Gvr2010 
                         G component is E component of 08515+1149 BPM 515BE.                             
             BPM 487     BH: [PM2000]  913379 + [PM2000]  913251.                                Gvr2010 
                         H component is B component of 08513+1149 BKO  38AB.                             
             BPM 469     HI: [PM2000]  913251 + [PM2000]  913194.                                Gvr2010 
08514+1146   BPM 477     AB: [PM2000]  913292 + [PM2000]  913250.                                Gvr2010 
             BPM 478     AC: [PM2000]  913292 + [PM2000]  913402.                                Gvr2010 
             BPM 479     AD: [PM2000]  913292 + [PM2000]  913277.                                Gvr2010 
             BPM 480     BE: [PM2000]  913250 + [PM2000]  913409.                                Gvr2010 
             BPM 488     CF: [PM2000]  913402 + [PM2000]  913326.                                Gvr2010 
             BPM 466     FG: [PM2000]  913326 + [PM2000]  913184.                                Gvr2010 
08515+1154   CHE 120     B component is H component of 08515+1152 BPM 501CH.                             
08515+1152   BPM 498     CE: [PM2000]  913490 + [PM2000]  913519.                                Gvr2010 
             BPM 499     CF: [PM2000]  913490 + [PM2000]  913553.                                Gvr2010 
             BPM 500     CG: [PM2000]  913490 + [PM2000]  913554.                                Gvr2010 
             BPM 501     CH: [PM2000]  913490 + [PM2000]  913458.                                Gvr2010 
                         H component is B component of 08515+1154 CHE 120.                               
             BPM 513     CI: [PM2000]  913490 + [PM2000]  913570.                                Gvr2010 
                         I component is B component of 08516+1152 CHE 123AB.                             
             BPM 517     EI: [PM2000]  913519 + [PM2000]  913593.                                Gvr2010 
             BPM 518     EJ: [PM2000]  913519 + [PM2000]  913609.                                Gvr2010 
                         J component is C component of 08516+1152 BKO  46AC.                             
             BPM 519     EK: [PM2000]  913519 + [PM2000]  913612.                                Gvr2010 
                         K component is J component of 08516+1152 BPM 520CJ.                             
             BPM 512     FG: [PM2000]  913553 + [PM2000]  913554.                                Gvr2010 
             BPM 514     FI: [PM2000]  913553 + [PM2000]  913570.                                Gvr2010 
             BPM 496     GH: [PM2000]  913554 + [PM2000]  913458.                                Gvr2010 
08515+1151   BPM 502     AB: [PM2000]  913499 + [PM2000]  913468.                                Gvr2010 
                         A component is D component of 08516+1152 BPM 506AD.                             
                         B component is E component of 08516+1152 BPM 521AE.                             
             BPM 503     AC: [PM2000]  913499 + [PM2000]  913471.                                Gvr2010 
             BPM 504     AD: [PM2000]  913499 + [PM2000]  913533.                                Gvr2010 
                         D component is F component of 08516+1152 BPM 522AF.                             
             BPM 505     AE: [PM2000]  913499 + [PM2000]  913346.                                Gvr2010 
                         E component is E component of 08514+1148 BPM 492AE.                             
             BPM 509     BD: [PM2000]  913468 + [PM2000]  913533.                                Gvr2010 
             BPM 486     BE: [PM2000]  913468 + [PM2000]  913346.                                Gvr2010 
             BPM 510     CD: [PM2000]  913471 + [PM2000]  913533.                                Gvr2010 
             BPM 508     DE: [PM2000]  913533 + [PM2000]  913346.                                Gvr2010 
             BPM 526     DF: [PM2000]  913533 + [PM2000]  913681.                                Gvr2010 
                         F component is I component of 08516+1152 CHE 124KI.                             
08515+1149   BPM 515     BE: [PM2000]  913582 + [PM2000]  913565.                                Gvr2010 
             BPM 516     BF: [PM2000]  913582 + [PM2000]  913601.                                Gvr2010 
                         E component is G component of 08514+1148 BPM 494AG.                             
08515+1148   BPM 497     [PM2000]  913486 + [PM2000]  913564.                                    Gvr2010 
08515+1146   BPM 511     [PM2000]  913542 + [PM2000]  913676.                                    Gvr2010 
08515+1135   BPM 507     [PM2000]  913518 + [PM2000]  913560.                                    Gvr2010 
08516+1154   BPM 523     AB: [PM2000]  913647 + [PM2000]  913504.                                Gvr2010 
             BPM 524     AC: [PM2000]  913647 + [PM2000]  913672.                                Gvr2010 
08516+1152   CHE 123     AB: B component is I component of 08515+1152 BPM 513CI.                         
             BKO  46     AC: C component is J component of 08515+1152 BPM 518EJ.                         
             BPM 506     AD: [PM2000]  913614 + [PM2000]  913499.                                Gvr2010 
                         D component is A component of 08515+1151 BPM 502AB.                             
             BPM 521     AE: [PM2000]  913614 + [PM2000]  913468.                                Gvr2010 
                         E component is B component of 08515+1151 BPM 502AB.                             
             BPM 522     AF: [PM2000]  913614 + [PM2000]  913787.                                Gvr2010 
             BPM 531     CH: [PM2000]  913609 + [PM2000]  913690.                                Gvr2010 
             BPM 527     CI: [PM2000]  913609 + [PM2000]  913681.                                Gvr2010 
             BPM 520     CJ: [PM2000]  913609 + [PM2000]  913612.                                Gvr2010 
                         J component is K component of 08515+1152 BPM 519EK.                      .      
             BPM 533     CK: [PM2000]  913609 + [PM2000]  913720.                                Gvr2010 
             BPM 534     CL: [PM2000]  913609 + [PM2000]  913724.                                Gvr2010 
             BPM 537     FG: [PM2000]  913787 + [PM2000]  913894.                                Gvr2010 
             BPM 528     HI: [PM2000]  913690 + [PM2000]  913681.                                Gvr2010 
             BPM 536     HL: [PM2000]  913690 + [PM2000]  913724.                                Gvr2010 
             BPM 535     IL: [PM2000]  913681 + [PM2000]  913724.                                Gvr2010 
             BPM 529     IM: [PM2000]  913681 + [PM2000]  913753.                                Gvr2010 
                         M component is C component of 08516+1147 BPM 532BC.                             
             CHE 124     KI: I component is F component of 08515+1151 BPM 526DF.                         
08516+1147   BPM 525     AB: [PM2000]  913651 + [PM2000]  913713.                                Gvr2010 
             BPM 532     BC: [PM2000]  913713 + [PM2000]  913753.                                Gvr2010 
                         C component is M component of 08516+1152 BPM 529IM.                             
08516+1137   BPM 530     [PM2000]  913687 + [PM2000]  913615.                                    Gvr2010 
08516-0711   BU  587     15 Hya. A is a spectroscopic binary, and one component is variable.             
             H 5 120     AC: H V 120.                                                                    
08517+1144   BPM 538     [PM2000]  913812 + [PM2000]  913815.                                    Gvr2010 
08518+1150   BPM 539     CD: [PM2000]  913923 + [PM2000]  914017.                                Gvr2010 
             BPM 545     DE: [PM2000]  914017 + [PM2000]  913879.                                Gvr2010 
08518+1146   BPM 540     [PM2000]  913948 + [PM2000]  913834.                                    Gvr2010 
08519+6308   KR   32     Also known as LDS2294.                                                          
08519+1205   BPM 542     [PM2000]  913976 + [PM2000]  914014.                                    Gvr2010 
08519+1158   BPM 541     [PM2000]  913972 + [PM2000]  913843.                                    Gvr2010 
08519+1148   BPM 546     [PM2000]  914090 + [PM2000]  914091.                                    Gvr2010 
08519+1141   BPM 544     [PM2000]  914010 + [PM2000]  914054.                                    Gvr2010 
08519+1130   BPM 543     [PM2000]  914004 + [PM2000]  913999.                                    Gvr2010 
08520+2543   STTA 96     B is BD+26@1854.                                                                
08520+1156   BPM 547     [PM2000]  914173 + [PM2000]  914218.                                    Gvr2010 
08521-4751   BRT 754     CPD-47@2847.                                                                    
08522+1144   BPM 548     [PM2000]  914371 + [PM2000]  914387.                                    Gvr2010 
08523+1143   BPM 549     [PM2000]  914522 + [PM2000]  914476.                                    Gvr2010 
08523+0804   TOK  22     Estimated period of visual pair 600y.                                   Tok2006 
                         A is SB1, P=10.25d, Griffin & Fuhrmann 2013 MNRAS, 430, 1390). B is             
                         SB2 (P~10d). Fuhrmann (2005 MNRAS, 361, 803) gave Mass(Aa)=0.96Msun,            
                         age 8.2Gyr, Ab is WD?  However, Griffin & Fuhrman said  P(Aa,Ab)=10d            
                         and tertiary. Ab not a WD. Tok2006: dK=(AB)=4.28 => Mass(Ba)=0.23               
08523-1837   GWP1095     ABL 251.                                                                Tob2012b
08523-1913   GWP1096     ABL 252.                                                                Tob2012b
08525+2816   HJ  460     53 Cnc. A is the variable BO Cnc.                                               
                         C component is A component of 08526+2820 LDS6219.                               
08525+1206   BPM 550     [PM2000]  914773 + [PM2000]  914798.                                    Gvr2010 
08526+3228   HU 1125     sig 1 Cnc = 51 Cnc. A spectroscopic binary.                                     
             S   583     AC: H 6  86.                                                            MEv2010 
08526+2820   LDS6219     55 Cnc = Copernicus.  NLTT 20414/20418                                  Chm2004 
                         CHARA Array Limb-darkened diameter  0.854 +/- 0.024 mas,                CIA2008c
                         R =  1.150 +/- 0.035 \rsun.                                                     
                         A component is C component of 08526+2816 HJ  460AC.                             
             55 Cnc      A: Combined solution, based on reduction of Hipparcos intermediate              
                         astrometric data together with spectroscopic elements from Butler       CPS1997a
                         et al. (1997).                                                          HaI2001 
08526+2527   BRT3289     Originally published as BRT 153.                                        Brt1928 
08526-3633   FIN 296     More than one revolution?                                                       
08527+2231   LDS6220     NLTT 20426/20425                                                        Chm2004 
08530+1625   BPM 551     [PM2000]  915167 + [PM2000]  915161.                                    Gvr2010 
08530-0834   GWP1099     ABL 253.                                                                Tob2012b
08531+5457   A  1584     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.07 +/- 0.60, 2.18, and 1.05 Msun, respectively.             Mlk2012 
08531+1320   BPM 552     [PM2000]  915268 + [PM2000]  915272.                                    Gvr2010 
08531-0437   LDS3828     NLTT 20452/20453                                                        Chm2004 
08531-5639   MWT   2     Mawet et al. (2015) find a companion to HR 3549at ~80au, and determine          
                         that the pair shares common proper motion. The companion has a mass             
                         roughly estimated at 15-80 Mjup.                                        Mwt2015 
08532-0732   GWP1100     ABL 254.                                                                Tob2012b
08533-0356   GWP1101     ABL 255.                                                                Tob2012b
08535-2249   DON 292     J  2066.                                                                J__1962a
08535-4603   CPO 241     CPD-45@3221.                                                                    
08536+1210   GII  38     Ba,Bb: Probably the same as GII  79Ba,Bb. Gili (2016) lists two                 
                         separate pairs of similar separation and position angle, and                    
                         associates both with HEI 480. However, he gives a position and UCAC4            
                         designation for the 2011 measure which correspond to a 16th magnitude           
                         star about 34" east of the Heintz pair.                                 Gii2016 
08536-1722   TOK 666     Resolved with ANDICAM2. A has small PM. AB is considered physical on            
                         photometry only.                                                        Tok2014d
08538-0035   STF1292     BDS 4842, HDO 120.                                                              
                         HJL 101.                                                                HJL1986 
08538-4731   FIN 316     Low incl fixed at 15 deg, Omega=0 for Soderhjelm (1999) orbit.          Sod1999 
                         High mass-sum and q=1.5(0.3) corroborates secondary 9.1d SB2            Wor1983 
                         The primary is SB2, P = 9.07 d. 1912-13 (Lick Obs. Bul. 16, 137,                
                         1928); no later observations.                                                   
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Finsen (1973).                                                          Fin1973a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.25 +/- 0.50, 3.21, and 1.58 Msun, respectively.             Mlk2012 
08539+0149   A  2554     Very difficult object, even in good definition, due to magnitude                
                         difference. All 1936-1941 measures noted as very hard and uncertain.            
                         Aitken has two measures in 1913, a very uncertain one in 1923, and              
                         failed to see the companion in 1935.                                    B__1951a
08539-1308   ST    9     L 820-19 = LPM 299 = LDS3829.                                                   
                         NLTT 20496/20497                                                        Chm2004 
08539-2026   RSS 178     CPD-19@3889                                                                     
08539-6648   EGN   9     Single epoch, so bound/unbound nature of pair unknown. Primary is               
                         planet host star.                                                       Egn2007 
08540-0103   GWP1102     ABL 256.                                                                Tob2012b
08540-4229   FGS  24     The classification is from Garrison et al. (1977 ApJS 35, 111).         Msn1998a
08542+3035   STF1291     Mt. Wilson spectral types G7,K0.                                                
                         AB: H 1  30.                                                            MEv2010 
08542-1629   GWP1104     ABL 257.                                                                Tob2012b
08543-3653   BRT1641     SWR  55.                                                                        
08544-0821   GWP1105     ABL 258.                                                                Tob2012b
08546+1219   CHE 134     A star of appropriate magnitude is seen at Chevalier's coordinates,     Che1911 
                         but with no companion. Reversing the sign of either or both offsets             
                         from the plate center yields no likely pairs, either. Perhaps the               
                         secondary measured by Chevalier was instead a plate flaw or other               
                         spot on the emulsion?                                                   Hrt2012b
08546-1925   GWP1107     ABL 259.                                                                Tob2012b
08548+4335   STF1289     H 1  85.                                                                MEv2010 
08548-1406   GWP1108     AB: ABL 260AB.                                                          Tob2012b
             GWP1109     AC: ABL 260AC.                                                          Tob2012b
08549+2612   A  2131     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.43 +/- 0.47, 2.30, and 1.85 Msun, respectively.  Mlk2012 
             HO  357     AB,C: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB,C: Rectilinear solution by Hurowitz et al. (2014).                   USN2014a
08550-1205   GWP1110     ABL 261.                                                                Tob2012b
08551-4736   SNA   8     Star is a member of the Vela OB1 association; at the distance of that           
                         association the projected separation of the new pair is 2.3au. The              
                         resolved companion may be the reported spectroscopic companion, if              
                         the spectroscopic period is greater than ~6 months.                     Sna2014 
                         LS 1204. Classification is from Garrison et al. (1977 ApJS 35, 111).    Msn1998a
08552+1612   BPM 553     [PM2000]  917386 + [PM2000]  917319.                                    Gvr2010 
08552-1814   S   585     B is BD-17@2692.                                                                
08553-1122   S   584     B is BD-10@2691.                                                                
08554+7048   STF1280     AB: LDS1684. Mt. Wilson spectral types M0, M0. Proper motion of                 
                         A -1334 -362, B -1364 -407. C -008-020                                          
                         H N 144.                                                                Bu_1906 
08554-4653   RST 361     Includes OV Vel, a Beta Lyr type eclipsing binary, P = 2.09051d.        Zas2012 
08555-0758   STF1295     17 Hya. Both components are metallic-line stars.                                
                         H 2  77.                                                                MEv2010 
08555-2741   SEE 107     del Pyx                                                                         
08557-1531   GWP1113     ABL 262.                                                                Tob2012b
08558+6458   ARG  21     A is an Algol-type system, AC UMa.                                              
08559+4632   LDS 908     NLTT 20526/20527                                                        Chm2004 
08560-0724   GWP1115     ABL 263.                                                                Tob2012b
08562-5532   DUN  73     B is CPD-55@1852.                                                               
                         Identified as optical and linear solution also published.               LRR2022c
08563+1239   JNN 274     G 41-8. Estimated age 30-300 Myr; masses 0.13 +/- 0.08 and 0.11 +/-             
                         0.06 Msun; a ~27.0 au.                                                  Jnn2014 
08563-1908   BRT1471     J 2646.                                                                         
08563-5243   R    87     A is a spectroscopic binary.                                                    
08564-0916   GWP1116     ABL 264.                                                                Tob2012b
08565+7058   HZG   7     Also known as LDS1685.                                                          
08565+7232   TDS6202     Aka TOI 1169.                                                                   
08567+1951   BLL  27     A is a semiregular variable, T Cnc.                                             
08568+2235   BOY   2     Aa,Ab: 2MASSI J0856479+223518                                                   
                         Physical companionship to this ultracool dwarf ruled out based on i-z           
                         and z-J colors, using photometry from SDSS.                             AlP2007 
08568-1401   GWP1119     ABL 265.                                                                Tob2012b
08568-1726   ARG  72     AB: Despite the linear solution, proper motion and parallax favor a     Grv2020a
                         physical connection. Long period and/or high eccentricity possible.             
             SHY 533     BC: HIP  43920 + HIP  44657.                                                    
08568-3205   HJ 4154     SWR  58. CPM pair                                                       Skf2004 
08570-0754   GWP1120     ABL 266.                                                                Tob2012b
08570-5914   DUN  74     A variable, V376 Car.                                                           
08571-2951   TOK  63     Aa,Ab: Estimated masses 0.64 and 0.59 Msun; sep 15.9 au, period 60 y.   Tok2010c
                         Ba,Bb: Estimated masses 0.55 and 0.24 Msun; sep 10.9 au, period 40 y.   Tok2010c
08572+1519   SHY 204     HIP  43970 + HIP  44001.                                                        
08573-0948   GWP1121     ABL 267.                                                                Tob2012b
08575-5045   HD  76968   Turner (1979 A&A 76, 350) includes this star in a group with the                
                         Cepheid SW Vel which lies beyond Vel OB1 at a distance of 2.6 kpc.      Msn1998a
08579-4744   SNA   9     Aa,Ab: The separation changed from 1.5 to 4.1 mas over 5.6 months,              
                         indicating clear orbital motion. The system exhibits non-thermal X-ray          
                         emission (Benaglia et al. 2001, A&A 535, A53), possibly due to                  
                         wind-wind collision in the binary system.                               Sna2014 
08580+3014   HO  252     61 Cnc. Rapid binary? Measures scattered and uncertain.                 Mlr1950a
                         The separation of this partially resolved pair for 1986.388 was                 
                         calculated under the assumption of zero or otherwise known magnitude            
                         difference.                                                             Tok1985 
08580+2428   OSO  23     G009-036. Not a common proper motion pair                               Oso2004 
08581+1130   GIC  82     G046-012/G046-013.                                                              
08581-3852   RSS  11     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
08582+1945   LDS3836     LSPM J0858+1945 = EI Cnc. Law et al (2008) derive a distance of         Law2008 
                         5.23 +/-0.07 pc and a projected separation of 7.27 +0.11/-0.11 au.              
                         Estimated spectral types are M5.5 and M6.                                       
                         LHS 2077. Estimated age 1000-10000 Myr; masses 0.13 +/- 0.03 and 0.11           
                         +/- 0.02 Msun; a ~9.6 au.                                               Jnn2014 
08584-1422   LDS3837     NLTT 20663/20660                                                        Chm2004 
08585+3548   COU1897     Semi-major axis value of 0".4 in Couteau (1999) appears to have been    Cou1999b
                         a typo. Changed to 0".14 in orbit catalog.                                      
08585+1151   HJ  110     alp Cnc = 65 Cnc = Acubens. A is an occultation double.                         
08586+2711   ZHN   4     NLTT 20640 + 2MASS J08583693+2710518. Baron et al. (2015) estimate              
                         spectral types M4.0 +/- 0.5 and L0 +/- 1, distances 54 +32/-20 and              
                         48 +3/-14 pc, masses 0.207-0.272 and 0.074-0.081 Msun.                  BFr2015 
08588-5303   VSP  24     V524 Vel.                                                                       
08589+0829   DEL   2     G 41-14.  A triple system with a close spectroscopic pair on a 7.6 day          
                         orbit, and one wider component which is reported at a separation of             
                         620 mas in Delfosse et al. (1999). Subsequently, an orbit has been      Del1999a
                         determined for the wider pair (Hartkopf et al. 2012), with a period of  Hrt2012a
                         5.66 years and a 424 mas angular semi-major axis. Using the estimated           
                         orbital elements to predict the location of the wider component in Jan          
                         2012 when the AstraLux image was taken, the predicted separation is             
                         ∼100 mas. This is in excellent agreement with what is seen in the       .     
                         AstraLux image, where the PSF is substantially extended, but not quite          
                         sufficiently to get a satisfactory binary fit.                          Jnn2014 
08589-4714   HJ 4161     A is a Delta Scuti-type variable, FZ Vel.                                       
08590+0938   LDS3838     SLW 320.                                                                        
08591+3155   TOK 522     AB is accepted as physical because of large PM(A) and low crowding              
08592+4803   HJ 2477     iot UMa = 9 UMa = Talitha. A is a Delta Scuti-type variable and SB1,            
                         P = 11.03y.                                                                     
                         A,BC: STT 196. A premature orbit has been computed. Quadruple.                  
                         A,BC: While the orbit may be good for ephemerides, system is unstable.  PkO2014 
                         2009.822: Observation incorrectly attributed to 11491+1434 in           Rdr2015 
                         Rodriguez et al. 2015 and assigned the discoverer designation                   
                         RDR   3AE. Correction provided by G. Duchene (private comm.).                   
             HU  628     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         2009.822: Observation incorrectly attributed to 11491+1434 in           Rdr2015 
                         Rodriguez et al. 2015 and assigned the discoverer designation                   
                         RDR   3Ea,Eb. Correction provided by G. Duchene (private comm).                 
                         AC measures are X coded so they are omitted when fitting the orbit              
                         of HU  628A,BC but are not incorrect or bad measures                            
08593+2006   BRT2396     COU  48.                                                                        
08594-5905   SHY 205     AC: HIP  44143 + HIP  48133. C component = A component of 09488-5237.           
08595+3225   SHJ 100     sig 3 Cnc = 64 Cnc. B is BD+32@1820.                                            
                         AB: H 6  87.                                                            MEv2010 
08595+2918   LAW  16     LSPM J0859+2918 = NLTT 20681. Law et al (2008) derive a distance of     Law2008 
                         21.5 +10.1/-4.0 pc and a projected separation of 16.1 +8.2/-2.7 au.             
                         Estimated spectral types are M4.5 and M5.                                       
08596+0146   BAL1855     BAL2356a.                                                                       
08597-2749   TOK  23     Estimated period of visual pair 680y.                                   Tok2006 
                         A is SB2E, P=3.199d.  Tokovinin et al. (2006): dK(AB)=6.93,             Tok2006 
                         dJ(AB)=7.29 ==> M(B)=0.08 V(B)~18.5                                     Tok2014d
08599+0143   BAL1856     Previously known as BAL2356b.                                                   
08599-0135   HJ  111     HJL 102.                                                                HJL1986 
09001-1228   HU  225     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.38 +/- 1.07, 2.57, and 1.13 Msun, respectively.  Mlk2012 
             WOR  36     A faint companion (mag. about 14, 5") found by Worley may be                    
                         physical.                                                                       
09002+4258   LDS3840     NLTT 20703/20706                                                        Chm2004 
09003+0332   HJ 2479     The proper motion study was:                                                    
                         A component: mu(RA) = -0.006+-0.002 mu(DEC) = -0.005+-0.001,                    
                         B component: mu(RA) =  0.000+-0.006   mu(DEC) = -0.005+-0.001           FMR1999h
09004-0809   OL  171     Aka BRT2287.                                                            Dam2018n
09005+7526   HJ 1162     Also a spectroscopic binary with P = 1324d which cannot be the visual   Grf2016a
                         pair.                                                                           
09005+3225   HU  718     A premature orbit has been computed.                                            
09005+0617   RAB   1     Rabe identifies this as BDS 4887? Looks like another pair.              Rab1923 
09006+4147   KUI  37     10 UMa. Hyad. Well observed RV variation in agreement with the visual           
                         orbit. Spectral types and masses of components assigned by ten                  
                         Brummelaar et al., based on adaptive optics observations.               TtB2000 
                         Calculated mass sum is 2.44 +/- 0.12 Msun, consistent with spectral             
                         types F5V.                                                              Mut2010b
                         AB: Additional notes may be found in Duruy (1941),                      Dur1941 
                         Duruy (1942), and                                                       Dur1942b
                         Baize (1943).                                                           Baz1943a
                         AB: Martin et al. (1998) derive component masses 1.525 +/- 0.104 and            
                         0.920 +/- 0.080 Msun.                                                   Mig1998 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.37 +/- 0.33, 2.39, and 2.14 Msun, respectively.  Mlk2012 
                         AB: A typographical error in the Muterspaugh et al. (2010) orbit has    Mut2010b
                         been corrected; period is 7961.0d, not 7691.0d. Noticed by Rick Wasson          
                         (2016, private comm.)                                                           
             STT 566     AB,C: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB,C: Rectilinear solution by Hurowitz et al. (2014).                   USN2014a
09008+0516   OSV   2     Ross 686,7.                                                                     
09012+0245   STF1302     AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
09013+1516   STF1300     NLTT 20763/20764                                                        Chm2004 
09013-3855   I  1513     CPD-38@2898.                                                                    
09014+3215   STF1298     66 Cnc.                                                                         
09015+3604   ALI 354     Bogus binary.                                                                   
09018+2754   SHJ 101     67 Cnc. A is a spectroscopic binary. B is BD+28@1673.                           
                         H 6  41.                                                                MEv2010 
09024-6547   WFC  78     SWR  62. CPM pair                                                       Skf2004 
09024-6801   SWR  63     CPM pair                                                                Skf2004 
09026-5956   HJ 4170     SWR  61.                                                                        
09032+4232   LDS3848     SLW 323.                                                                        
09032-1740   S   588     B is BD-17@2726.                                                                
09032-6221   HJ 4175     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
09035+3750   MUG   1     Metchev & Hillenbrand say pair probably physical, based on proximity.   Met2004b
                         Metchev & Hillenbrand (2009) estimate companion mass 0.49 Msun,         Met2009 
                         dK=2.10. Estimated V(B)=11.2, dV=4.0.                                   Tok2014d
09036+4709   A  1585     kap UMa = 12 UMa = Alkaphrah.                                                   
                         Elongations and quadrant doubtful.                                      B__1963b
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         1975.950: This observation was made under very poor conditions and              
                         yielded a poor set of fringes.                                          BLM1978 
                         1981.350: This observation was incorrectly attributed to Fin 347 by     Tok1982a
                         Tokovinin (1982a) (noted in Tokovinin 1982b)                            Tok1982b
                         Calculated mass sum is 6.30 +/- 0.98 Msun, not well-constrained.        Mut2010b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 6.63 +/- 1.41, 9.53, and 2.19 Msun, respectively.             Mlk2012 
09036-2619   HJ 2482     SWR  60. CPM pair                                                       Skf2004 
09037+4531   COU2686     Also known as HDS1312. While the HDS measure predates that of Couteau,  Cou1994 
                         the Couteau publication predates that of Hipparcos.                     HIP1997a
09040+1349   FAR   7     SKF  29. Primary is white dwarf WD 0901+140.                            Far2005b
09040+0259   GRV1017     SLW 327.                                                                        
09040-3204   PRO  80     SWR  64.                                                                        
09042+6446   LDS2301     LDS5201.                                                                        
09042+0301   GRV 775     HJL 103.                                                                HJL1986 
                         SHY 536. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
09045-5740   RST 375     Spectral type G2?                                                               
09048+3759   LDS3851     NLTT 20894/20892                                                        Chm2004 
09050+2250   HDS1318     A is SB2, P=893.5d. B not seen in 2MASS K,J-band images, likely bogus.  Tok2014d
09050+1134   TOK 125     HIP 44579.                                                                      
09050+1058   BPM 554     [PM2000]  925928 + [PM2000]  925978.                                    Gvr2010 
09053+3848   OSO  24     G115-049. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
09055+0020   RST5313     Appears to be 5' error in 1855 declination of BD coordinates.                   
                         Appears to be same as TDS6306; pairs merged.                                    
09055-4919   JNN  65     This star has a probably brown dwarf companion, but since only one              
                         epoch of data exists, this is still unconfirmed.                        Jnn2012 
09056+5018   ES 2631     B is BD+50@1606.                                                                
09056-7433   SWR  66     CPM pair                                                                Skf2004 
09057-0816   FAL  26     A = RX Hya, eclipsing binary of Algol-type, period 2.28165 days.        Zas2015 
09061+3537   WLY   4     The pair ALI 355 is bogus and was a measure of a plate flaw.                    
                         The WLY   4 pair was found while searching for the ALI pair.                    
09063-5904   LTT 3359    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
09066+0249   STF1309     HJL 104.                                                                HJL1986 
09067+2031   OSO  25     G009-047. Common proper motion pair                                     Oso2004 
09067-3334   EGN  10     Pair bound. B component colors consistent with it being an M1-M4 dwarf          
                         with mass 0.30 +/- 0.01 Msun.                                           Egn2007 
09071+3037   AG  162     BDS 4940, H N 30 is the same star.                                              
09074+2259   HO  644     AC: Physical pair according to Daley.                                   Dal2006a
             STF1311     AB: HJL 105.                                                            HJL1986 
                         AB: H 3  92.                                                            MEv2010 
09075-3445   HJ 4179     SWR  65. CPM pair                                                       Skf2004 
09076+0004   TOK 126     HIP 44777. X-ray source 1RXS J090732.0+000352.                                  
09077+1040   CHR 257     kap Cnc = 76 Cnc. Hipparcos suspected non-single.                               
09077-4438   I   492     A Beta Cephei-type variable.                                                    
09079-0708   TOK  64     Aa,Ab: Estimated masses 0.95 and 0.61 Msun; sep 29.3 au, period 130 y.  Tok2010c
             STF1316     HIP 44804. Close triple. Observed with NICI (Tokovinin et al. 2010).    Tok2010c
                         BC: Rectilinear solution by Friedman et al. (2012).                     USN2012a
09080-2552   I   491     kap Pyx                                                                         
09080-4326   SEE 109     lam Vel = Suhail. A is an irregular variable.                                   
09080-5808   RST9001     Previously known as RST3624a.                                                   
09080-6402   HJ 4185     B is CPD-63@1097.                                                               
                         SWR  67. Probably dwarfs, not giants (as per Houk). CPM pair            Skf2004 
09081+4510   HJ 1164     Noted as not having been observed in a long time, but this is an error. WSI2008 
                         That "105" note should have gone with 09147-0212BAL 517.                Dam2011 
09081-2204   HDO 121     Separation for 1870.18 >15"                                             Win1882 
09083+3641   BRT2220     ALI 591.                                                                        
09083-3707   TOK 127     HIP 44851. NOMAD: PM(B)=(+102,+500) V=16.37 (??). B is physical,                
                         despite crowded field with N*=98. PM(A)=(-59,-3). PMS star, X-ray               
                         source RXS J090817.3-370649, variable CY Pyx.                           Tok2011a
09084+2732   STTA 97     B is BD+28@1698.                                                                
                         HJL 106.                                                                HJL1986 
                         SHY 207. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
09085+2141   A  2134     Appears to be same pair as 09085+2142 TDS6348; systems merged.                  
09086-2550   RST2610     Possibly triple: the known companion RST 2610 at 1".7 with estimated            
                         period 500 yr is unlikely to cause the RV variability and dmu.          Tok2012a
                         AB: A is suspected SB, no orbit.                                        Tok2014d
09086-3843   RST1416     CPD-38@3012.                                                                    
09086-4841   LDS 251     B is CD-48@4456.                                                                
09087-0835   KUI  38     19 Hya. A is a spectroscopic binary.                                            
09087-2159   RSS 191     CPD-21@4113                                                                     
09088+2638   STT 567     AB: 75 Cnc. A is a spectroscopic binary. B is BD+27@1716.                       
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             75 Cnc      Combined spectroscopic/astrometric solution, based on high-resolution           
                         echelle spectra plus archival PTI visibility measurements.                      
                         Derived masses 1.173 +/- 0.024 and 1.011 +/- 0.021 Msun,                        
                         distance 31.246 +/- 0.051 pc.                                           Knc2010 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.13 +/- 4.27, 1.98, and 1.07 Msun, respectively.             Mlk2012 
09090+1728   ONL   1     OCC 238.                                                                        
09091-1820   VIG  12     Optical/physical nature of the faint companion is undefined.            Vig2012 
09094+2203   WRH  16     xi Cnc = 77 Cnc. Uncertain binary, unresolved by speckle                        
                         interferometry. A long-period spectroscopic binary.                             
09095+3854   OSO  26     G116-009. Common proper motion pair                                     Oso2004 
09097-4207   CPO  40     LDS 253.                                                                        
09098+1134   CHR 131     Suspected occultation binary.                                                   
09099-3022   H N  96     eps Pyx. A is a spectroscopic binary.                                           
09103+2200   WRH  17     79 Cnc. Less than 0.1" 1954 (Finsen); not resolved by speckle despite   Fin1954c
                         numerous attempts 1976-1983. Binary nature uncertain.                           
09104+6708   STF1306     sig 2 UMa = 13 UMa.                                                             
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: H 3  54.                                                            MEv2010 
09109+6331   H 5  73     H V 73. tau UMa = 14 UMa. A is metallic-line star and long-period SB.           
                         A: Ren & Fu (2013) calculated an astrometric orbit, combining           Ren2013 
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Bretz (1961).                                                           Brz1961 
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
09109-4519   HJ 4186     LDS 255.                                                                        
09110+6331   tau UMa     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Bretz (1961).                                                           Brz1961 
09110-1929   I   824     Spectrum: Fm delta Del.                                                         
                         Ma,Mb = 1.83  +/- 0.16 , 1.79  +/- 0.15  \msun.                         GmJ2022 
09111+1757   BPM 555     [PM2000]  930950 + [PM2000]  930951.                                    Gvr2010 
09112+0128   GIC  83     G046-026/G046-027.                                                              
09115+2801   HJ  805     AB: HJL 107.                                                            HJL1986 
09117-4653   SEE 110     Algol-type eclipsing binary, P = 2.61362 d.                             Zas2011 
09118+1617   BPM 556     [PM2000]  931498 + [PM2000]  931492.                                    Gvr2010 
09119+1803   STT 568     AB: 80 Cnc.                                                                     
             BUP 124     BC: C is +18@2136.                                                              
09122-2555   JNN 150     2MASS J09121259-2555025 has the alternative identifier CD-25 6962B in           
                         SIMBAD, implicitly implying companionship with the G2-type star                 
                         CD-25 6962 at 14" separation. However, given the apparently very                
                         different proper motions of the components (e.g. Roser et al. 2010),    XXX2010 
                         we consider such a companionship questionable.                          Jnn2012 
09123+1500   FIN 347     Aa,Ab: pi 1 Cnc = 81 Cnc.                                                       
                         1981.358: This observation was incorrectly attributed to ADS 7158 by    Tok1982a
                         Tokovinin (1982a) (noted in Tokovinin 1982b)                            Tok1982b
                         1983.9371, 1983.9372: Interferometric observations indicate that        Wor1983 
                         Finsen's 1965 orbit (see Worley & Heintz, 1983) must be revised.        Bnu1984 
                         1990.9166: Residuals (4.0 deg in theta, 0".007 in rho) to the orbit of          
                         Hartkopf (1989) are only fair, due to a combination of large zenith     Hrt1989 
                         distance and close angular separation at the time of this observation.          
                         A combined astrometric/spectroscopic orbital solution is given by               
                         Mason et al (1996).                                                     Msn1996a
                         Reversed Delta m and slightly larger parallax/smaller masses than in    Msn1996a
                         the speckle-spectroscopic study by Mason et al.(1996).                          
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Aa,Ab: Combined solution orbit. Mass_a = 0.983 +- 0.045 Msun,                   
                         Mass_b = 0.903 +- 0.049 Msun, orbital parallax = 48.78 +- 2.36 mas.     Msn2012a
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 1.80 +/- 0.25, 1.86, and 0.91 Msun, respectively.  Mlk2012 
             BUP 125     AB: Due to the high proper motion of the A component, a later                   
                         observation of this pair by Soulie was incorrectly entered as a new     Sle1986a
                         component, SLE 478AD.                                                           
             STT 569     AC: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
             WIL   1     AE: CPM pair. Using data from 2MASS, Wilson et al. (2001) derive a      Wil2001 
                         spectral type of L8V and mass 40-74Mjup for the companion (called               
                         Gl 337C in that paper). They also note that the C and D components for          
                         the system appear to be background objects without CPM to the AB pair.          
             BUG  16     Ea,Eb: Burgasser et al (2005) resolved the E component (called Gl 337C          
                         in the paper) into a 0.53" pair of near-equal magnitude. At a distance          
                         to the system of 20.5 +/- 0.4pc, the close pair has a physical                  
                         separation of 10.9 +/- 0.6 au. Period of the pair is estimated at               
                         140-180y. Primary is L8; secondary is possibly early- or mid-T dwarf.   Bug2005 
09124+2653   A  1977     1921-1922 elongation uncertain. Less than 0.1" in 1956.                         
09124-0707   GAA   7     KW Hya.                                                                         
                         Ma,Mb = 1.975  +/- 0.028 , 1.487  +/- 0.013  \msun,                     GaA2019 
                         orbital parallax = 11.462 +/- 0.074 mas.                                        
09125+4912   MET  54     This cannot be the close 20.0-d spectroscopic binary.                   Grf2013f
09125-4337   FIN 317     Aa,Ab: FIN 317 is a close subsystem in the 2.9" AB pair HJ 4188. After          
                         discovery of Aa,Ab in 1951 at 0.116", Finsen (1951) was unable to       Fin1951b
                         resolve the star again on twelve occasions till 1968, except one other          
                         tentative measure in 1962. Yet the object was resolved by speckle in    Fin1964a
                         1989.94 at 0.144" and in 2006.18 at 0.123". Despite orbital period of           
                         ∼50 yr estimated from projected separation, the sub-system was not            
                         detected in 3 runs at SOAR (2009-2012), while the wider pair AB was             
                         measured. This may be yet another case of erratic measures and                  
                         non-resolutions. Possibly another "ghost" which isn't a real binary,    Tok2012b
                         but not "X" coded yet.                                                          
09126+0915   HEI 483     This is apparently the same pair as HJ  121.                                    
09128+6141   STF1315     B is BD+62@1055.                                                                
                         H N  79.                                                                MEv2010 
09128-4329   HU 1456     Primary is GG Vel, Algol-type eclipsing binary, period 1.475216d.       Zas2013 
09128-6055   HDO 207     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 34.09 +/- 12.51, 5.38, 2.57 Msun, respectively.    Mlk2012 
09131+3633   ES 2106     BRT3251.                                                                Brt1951 
09131-4128   CPO  41     LDS 258. A is CPD-40@3274, B is CPD-40@3273.                                    
09133+0540   WFC  81     HJL 108.                                                                HJL1986 
09136+4659   STF1318     A is SB2, P = 2536d. B is SB?                                           Tok2014d
09138+4313   BAG  45     Primary is the rotationally variable star EI Lyn.                               
09139+0252   H 6 108     B is BD+03 2171.                                                                
09142-5021   HJ 4192     B is CD-49@4232.                                                                
09143+6125   16 UMa      SB2. Combined orbit including RV data and Hipparcos Intermediate                
                         Astrometric data. Semimajor axis derived from photocentric a0 plus              
                         stellar evolutionary model. Derived properties for A and B:                     
                         M/Msun = 1.12 + 0.61, L/Lsun = 2.71 + 0.09, dm = 3.70 mag,                      
                         log age = 9.78.                                                         WaX2015b
                         Fekel et al. (2015) derive an astrometric orbit, with values of P, T,           
                         e, and omega adopted from their spectroscopic solution. The secondary           
                         is thought to be a mid- to late-K dwarf.                                Fek2015 
09143-0817   BU  908     B is BD-07@2762.                                                                
09144+5241   STF1321     Proper motion of A = -2530,-563; PM of B = -2559,-656 (UCAC2).                  
                         B is BD+53@1321. A premature orbit has been computed. Both components           
                         are suspected spectroscopic binaries (Abt & Levy 1973).                 AbH1973 
                         AB: NLTT 21249/21251                                                    Chm2004 
                         CHARA Array Limb-darkened diameter of A,B:                              CIA2012f
                         R =  0.5773 +/- 0.0131, 0.5673 +/- 0.0137 \rsun,                                
                         L =  0.06974 +/- 0.00213, 0.06465 +/- 0.00194 \lsun,                            
                         Teff = 3907 +/- 35, 3867 +/- 37 K, M = 0.622, 0.600 \msun.                      
                         Epoch-2000 coordinates of C component 0914355+524209; current AC                
                         separation ~2'.2 at 64deg. PM of D +035-003.                                    
                         ORB6 inclination = 180deg - inc. to match WDS measures                  Pko2020 
09144+0219   HJ 2489     the Hya = 22 Hya. A is a SB.                                                    
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: H 5  54.                                                            MEv2010 
                         B and C optical. No earlier measures of D.                              B__1963b
09149+0427   HEI 350     A long-period astrometric binary, now resolved.                                 
09150+1253   HJ 2490     BDS 4982, HJ 2487 same star.                                                    
09151-0825   GCB  22     BRT 427. J 3248.                                                                
09152+2323   BUP 127     AB: A is exoplanet host.                                                Tok2014d
             STT 570     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
09152+1643   BPM 557     [PM2000]  934187 + [PM2000]  934230.                                    Gvr2010 
09156+0422   RED  17     2MASS J09153413+0422045. Confirmed as binary by Liu (private comm. to           
                         Reid et al). Spectral types L7 and L7                                   Red2006b
09156-1036   MTG   2     LHS 6167. Estimated age 30-300 Myr; masses 0.15 +/- 0.04 and 0.09 +/-           
                         0.03 Msun; a ~1.0 au.                                                   Jnn2014 
                         Also known as G 161-7 or LHS6167.                                               
                         Parallax = 134.9 +/- 12.1 mas.                                          UR_2016 
                         Parallax = 103.33 +/- 1.00 mas.                                         JLB2017 
09157-0114   STF1329     B is BD-00@2163.                                                                
09158-3725   SEE 111     A is a spectroscopic binary.                                                    
09161-4454   DON 329     Variable.                                                                       
09163+2730   SLE 484     No sign of Soulie (1986) pair. Measured pair is obvious double; error           
                         in Soulie (1986) coordinates?                                           Sle1986a
09167+1955   LDS5162     LDS5202.                                                                        
                         NLTT 21351/21352                                                        Chm2004 
09167-0621   KUI  40     23 Hya. A is a long-period spectroscopic binary.                                
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Jones (1928).                                                           Jon1928c
09167-2448   JNN  67     We resolve this star into a close binary (as yet unconfirmed through            
                         common proper motion). It was recently classified as a classical                
                         Cepheid based on light curve analysis (Christiansen et al. 2008 MNRAS           
                         385, 1749). We assume that this is a mis-classification, given that             
                         the unresolved spectral type is M0.5V.                                  Jnn2012 
09167-5501   BRT3291     CD-54@2689.                                                                     
09168-1237   BRT2717     A likely plate flaw.                                                    Grv2021b
09168-2157   I   493     Too close, position angle uncertain.                                            
09169-0524   OSO  27     G161-009. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates.                                                  Oso2004 
09171+0717   STTA 98     AB: Pair appears in an appendix list, not part of discoverer's regular          
                         numbering sequence.                                                             
09172-2249   J  1543     CD-22@7068.                                                                     
09173-5305   KRV  24     Classical Cepheid DK Vel.                                                       
09173-6841   FIN 363     Speckle observations needed to refine relative orbit.                           
                         AB: Hipparcos parallax 30.64 +/- 0.70 mas. Dynamical parallax 27.2 mas,         
                         masses 1.63 and 1.37 Msun. FIN 363 has an unusually short period of             
                         only 3.44 yr. The Hipparcos photometry is doubtful because of close             
                         0.1" separation.                                                        Tok2012b
                         AB: Martin et al. (1998) derive component masses 3.661 +/- 0.338 and            
                         3.661 +/- 0.338 Msun.                                                   Mig1998 
                         AB: Docobo & Andrade (2013) derive a dynamical parallax of 29.71 +/-            
                         1.33 mas and component masses 1.43 +/- 0.25 and 1.06 +/- 0.20 Msun.             
                         See paper for extensive notes on this system.                           Doc2013d
09175+7715   KUI  39     Proper motion of A -1059 -020.                                                  
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 0.66 +/- 0.23, 1.17, and 0.65 Msun, respectively.             Mlk2012 
09176+3641   ES 1734     OL 109 is the same star, according to Barton.                                   
09179+2834   STF3121     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.39 +/- 0.75, 1.57, and 0.85 Msun, respectively.  Mlk2012 
09179+1130   HJ  128     A is a spectroscopic binary.                                                    
09179-6948   RMK  10     Rectilinear solution by Letchford et al. (2018).                        LRR2018a
09180-5453   JNN  69     2MASS J09180165-5452332 has a close (~0.49") companion to which it is           
                         probably physically bound, although this still needs to be confirmed            
                         through common proper motion.                                           Jnn2012 
09182-0036   HJ  126     STF1337. Pettit refers to his 1915 observation as of HJ  126, but       Ptt1917 
                         gives the cryptic note "Hard to identify with H star 1820. P.A. too             
                         small, distance too great." It appears to be a measure of the HJ pair,          
                         but typographically mangled. Earlier catalogued as PTT  25.                     
09184+3522   STF1333     Aka H 1  31.                                                            Bu_1906 
                         Additional notes may be found in Fatou (1941).                          Fat1941 
09184-2022   S   595     B is BD-19@2673.                                                                
09186+5231   HJ 2492     AB: B is the faint nebula NGC 2800.                                             
09186+2134   ALP  15     2MASSW J0918382+213406                                                          
                         Physical companionship of C component to this ultracool dwarf ruled             
                         out based on i-z and z-J colors, using photometry from SDSS. The B              
                         component was not detected by SDSS; followup observations are needed            
                         to determine its nature.                                                AlP2007 
09186+1953   SKF  31     FAR  55.                                                                        
09188+3648   STF1334     38 Lyn. A is a spectroscopic binary.                                            
             CHR 173     Ba. Abt & Biggs (1972) note variable RV.                                AbH1972 
             STF1334     AB: H 1   9.                                                            MEv2010 
09188+2647   LDS6226     NLTT 21428/21426                                                        Chm2004 
09188-2250   DON1080     J 1544. ARA1764.                                                                
09190+1742   83 Cnc      Gontcharov & Kiyaeva (2002) photocentric (astrometric) orbit is based   Gon2002a
                         on a combination of ground-based catalogs with Hipparcos.                       
09191-4128   CHR 239     Astrometric binary; dm 2.4 mag, period ~ 10y? Accelerated pm            Tok2012b
                         Omega for Tokovinin et al. (2014) orbit flipped by 180deg, at request           
                         of author.                                                              Tok2014a
09192+5824   LDS1226     NLTT 21416/21397                                                        Chm2004 
09193+5230   VBS  15     Identified as BDS 5000, HJ 2492 (Van Biesbroeck). May be another pair.  VBs9999 
09193+3831   GIC  84     G115-068/G115-069 = Melotte 25 EGG 33AB = GJ 1122AB.                            
09194-7739   KOH  83     Aa,Ab: Estimated masses 0.88 and 0.81 Msun; sep 6.8 au, period 14 y.    Tok2010c
                         Orbital parallax 14.90 +/- 0.37 mas.                                    Tok2020c
                         Mass of Aa, Ab = 1.12 +/- 0.04, 1.00 +/- 0.03 /msun.                            
             HJ 4214     Physical B component is also binary with spectroscopic P ~ 0.556d.              
                         HIP 45734. This is a PMS quadruple, both components are                         
                         slightly above the MS.                                                  Tok2011a
                         AB: B is X-ray source, SB2 (Desidera et al 2006 A&A 454,553)            Tok2014d
09196-3513   SWR  70     Giants, not dwarfs                                                      Skf2004 
09197+0444   LDS3876     SLW 348.                                                                        
09198-1158   B  2529     26 Hya. 1936, 1938 position angles 139@-122@. Distance 3.0".                    
                         Invisible 1948                                                          B__1951a
09200+0500   STF1343     HJL 109.                                                                HJL1986 
09200+0103   J  2501     Radio galaxy UGC 4956.                                                  J__1962a
09202+3518   RED  11     2MASSW J0920122+351742                                                          
                         2000.107: HST WFPC2 observations by Reid et al. (2001). Paper includes  Red2001 
                         mass and age estimates, as well as discussion of L dwarf binary                 
                         frequency and semimajor axis distribution.                                      
                         Assuming a spectrophotometric distance of 24.3 +/- 5.0 pc, Konopacky            
                         et al. (2010) derive a system mass of 0.11 +/- 0.11 Msun.               Kon2010 
09203-0817   GCB  24     J 2898.                                                                         
09205+0752   BRT2148     OL 172.                                                                         
09205-0933   SHJ 105     27 Hya. A is a spectroscopic binary. Spectrum composite: G8III-IV+F5V.          
                         AB: SHY 540. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AB: H 6  85.                                                            MEv2010 
                         Toyota et al. (2009) monitored the RV of the A component every 1-2              
                         months between 2003 Mar - 2007 Nov, using a high-dispersion echelle             
                         (precision ~10 m/s). The star exhibits a linear trend in RV, with a             
                         slope -30 m/s/y. Toyota et al. assert that these variations are due to          
                         an unseen companion. Assuming a circular orbit, period is estimated at          
                         3400d; if the mass of A is 2.32 Msun, the minimum mass ~10 Mjup.        Toy2009 
09207+5116   ARN  71     AD: HJL1055.                                                            HJL1986 
                         AD: SHY 208. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
09210+3811   STF1338     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.01 +/- 0.61, 2.59, and 2.58 Msun, respectively.  Mlk2012 
09210+3643   STF1339     H 1  31.                                                                MEv2010 
09210+3223   GIC  81     G047-035/G047-034. Typographical error led to this pair being                   
                         originally entered in the WDS as 08211+3226.                                    
09210-0100   FOX 161     J 1546. Bal 859.                                                                
09211+4155   LDS3878     NLTT 21509/21510                                                        Chm2004 
09213+3426   STT 571     40 Lyn                                                                          
             STF1342     BC: H 4  55 = SHJ 369.                                                  MEv2010 
09214+8123   STF1304     B is BD+81@288.                                                                 
09214+0248   BAL2361     J 2497.                                                                         
09215-4528   HJ 9003     Previously known as HJ 5452a.                                                   
09216-0243   FIL  21     BAL 202.                                                                        
09218+4330   LAW  17     LSPM J0921+4330 = GJ 3554. Law et al (2008) derive a distance of        Law2008 
                         11.8 +5.6/-2.2 pc and a projected separation of 7.1 +3.7/-1.2 au.               
                         Estimated spectral types are M4.5 and M4.5.                                     
                         GJ 3554. Estimated age 300-1000 Myr; masses 0.30 +/- 0.06 and 0.21 +/-          
                         0.04 Msun; a ~14.8 au.                                                  Jnn2014 
09219+1156   BPM 558     [PM2000]  939493 + [PM2000]  939496.                                    Gvr2010 
09223-3209   RSS 199     Primary is 12.9d SB1, Period of AB pair ~4700y.                         Tok2006 
09223-5428   SHY 541     AC: HIP  45952 + HIP  45937.                                                    
             I  1107     AB: Rectilinear solution by Zirm (2013).                                Zir2013d
                         Despite the linear solution, proper motion and parallax favor a         Grv2020a
                         physical connection. Long period and/or high eccentricity possible.             
09223-5558   EVS  14     Primary is the Cepheid V Vel.                                           Evs2016a
09226+6251   MLB 203     HJL 110.                                                                HJL1986 
09228-0950   A  1342     A magnetic and variable star, KU Hya, , 3.41d, 0.05V, is in the system. Mlr1956a
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Combined analysis using speckle, radial velocity, various magnetic              
                         field and polarization measurements.                                    Wad2000 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 5.13 +/- 1.94, 4.25, and 2.00 Msun, respectively.  Mlk2012 
09233+0330   STF1347     HJL 111.                                                                HJL1986 
09234-0503   GIC  85     G161-019/G161-020.                                                              
                         NLTT 21625/21628                                                        Chm2004 
09234-7753   HJ 4217     Agrees with Herschel's place but not his description.                   Daw1922 
                         High proper motion of A accounts for the discrepancy.                           
                         The companion is clearly UCAC4 061-008434 and not UCAC2 497073 (UCAC4   Whi2013 
                         061-008429) as suggested by SIMBAD.                                             
09236-5454   HJ 4207     B is CPD-54@2239.                                                               
09243-1601   LDS6227     NLTT 21682/21683                                                        Chm2004 
09243-3926   FIN 348     Hipparcos detects a magnitude difference, which reverses the quadrant           
                         of the prior measures, and indicates that nearly a revolution has been          
                         completed.                                                                      
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.29 +/- 0.76, 5.18, and 1.66 Msun, respectively.             Mlk2012 
09247+2611   BU  105     kap Leo = 1 Leo                                                                 
                         kap Leo. Engelmann speaks of a 10" star in the direction 65deg. There           
                         is certainly no companion in this place, and no third star near in any          
                         direction.                                                              Bu_1894 
09249+5134   STT 200     A is a spectroscopic binary.                                                    
09251+2933   BU 1423     AC. Burnham's measure, X coded now, was actually a measure from NGC     Dam2013 
                         2893 to BD+30 1873.                                                             
09252+4606   HDS1353     Cvetkovic et al. (2016) estimate spectral types K4 and M1, masses 0.72          
                         and 0.43 Msun. Dynamical parallax is 25.49 +/- 2.78 mas.                Cve2016b
09252+1602   FAR   8     SKF  32. Primary is white dwarf WD 0922+162.                            Far2005b
09253-4816   HJ 4209     B is CD-47@4921.                                                                
09254+1137   BPM 559     [PM2000]  942111 + [PM2000]  942115.                                    Gvr2010 
09255+0009   LDS5703     LDS6228. LHS 2140.                                                              
09256+6329   JNN 275     G 235-25. Estimated age 1000-10000 Myr; masses 0.21 +/- 0.04 and 0.13           
                         +/- 0.02 Msun; a ~2.4 au.                                               Jnn2014 
09256+5401   STF1346     AB: H 2  73.                                                            MEv2010 
09257+4626   LDS3889     NLTT 21701/21699                                                        Chm2004 
09257+3837   ES  298     Four-component system. The question of whether the CDB system is a              
                         hierarchical triple remains open.                                       Kiy2012 
09257-6958   HJ 4216     B is CPD-69@1061.                                                               
09260+2839   A   222     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.59 +/- 0.66, 2.49, and 1.10 Msun, respectively.             Mlk2012 
09260-1535   CLZ  15     GWP1172.                                                                Tob2012b
09261+5344   A  1343     Rectilinear solution by Rica & Zirm (2012).                             FMR2012i
09263+5847   BUG   9     SDSS J092615.38+584720.9                                                        
                         Estimated spectral types are T4: + T4:, effective temperatures ~1330            
                         and ~1330 K. Masses are estimated at 0.029-0.073 and 0.029-0.073 Msun,          
                         and the orbital period (assuming the semi-major axis = 1.26 * rho) is           
                         ~18yr.                                                                  Bug2006a
09265+7826   STF1326     SHY 542. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AB: CfA: A=SB?                                                          Tok2014d
09265-6618   RST 404     CD-65@769.                                                                      
09266-3047   SWR  71     CPM pair                                                                Skf2004 
09272-0913   A  1588     29 Hya.                                                                         
09275+5338   LDS3893     SLW 356.                                                                        
09275+3930   LEP  36     A is also a 8.5d spectroscopic binary.                                  Tok2019b
09275+1054   J   388     STF1354.                                                                        
09275-5806   CHR 240     Astrometric binary; dm 0.3 mag, period ~ 4y? Accelerated pm.            Tok2012b
09276-0840   H 6 111     AB: H VI 111. alp Hya = 30 Hya = Alphard. B is BD-08@2681.                      
                         Mk III Limb-darkened diameter  9.727 +/- 0.097 mas.                     MkT2003 
                         Primary unresolved in H alpha.                                          Bla1977a
09276-3500   B  2215     Last position angle uncertain. Needs speckle.                                   
                         Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
                         Astrometric binary; dm 1.5 mag, period ~ 1.97y                          Tok2012b
09276-4311   SWR  73     A component is 0".6 CPM pair                                            Skf2004 
09278-0604   B  2530     There may have been a quadrant reversal about 1951. The 3-year                  
                         spectroscopic motion does not seem to relate to the visual pair.                
                         Giant primary according to isochrone fit.                               Sod1999 
                         Single line SB, P = 2.5 y, also a known visual binary. Primary is G2V,          
                         so companion should likely be a cooler dwarf; this seems to be                  
                         confirmed from magnitude differences observed at 750, 550, and 450nm.   Bag1984b
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.06 +/- 0.31, 2.44, and 1.00 Msun, respectively.             Mlk2012 
09281+1150   BPM 560     [PM2000]  944081 + [PM2000]  944114.                                    Gvr2010 
09283-7815   HJ 4226     B is CPD-77@520.                                                                
09285+0903   STF1356     ome Leo = 2 Leo.                                                        Mlr1956a
                         Chevalier identified this star as ome Leo, but gave incorrect           Che1911 
                         coordinates, leading to its initial designation as 09283+0903 CHE 137.  Hrt2012b
                         Giant primary according to isochrone fit.                                       
                         1980.019: This observation of omega Leo by Weigelt (1983) was           Wgt1983 
                         incorrectly attributed to 09412+0954 = omi Leo in earlier editions              
                         of both the interferometric catalog and the WDS. As a result, omi Leo           
                         was incorrectly assigned the discoverer designation WGT   1.                    
                         H 1  26.                                                                MEv2010 
                         Combined spectroscopic/astrometric solution of SB1. Calculated masses           
                         1.92 +/- 0.96 and 0.28 +/- 0.92 Msun; values are poorly constrained.    Mut2010b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.67 +/- 0.24, 2.14, and 1.27 Msun, respectively.             Mlk2012 
09285+0811   H 4  47     H IV 47. 3 Leo.                                                                 
09285-2426   B   181     Not seen 1959-1962. May exhibit rapid retrograde motion.                        
09286+1721   BPM 561     [PM2000]  944368 + [PM2000]  944357.                                    Gvr2010 
09287+7834   LDS1696     MLR 524.                                                                        
09287+4536   S   598     41 Lyn = Intercrus. STTA 99. B is BD+46@1510.                                   
09288-0722   GIC  87     G161-033/G161-034.                                                              
                         NLTT 21868/21870                                                        Chm2004 
09291-0246   HJ 1167     tau 1 Hya = 31 Hya. B is BD-02@2902.                                            
                         HJL 112.                                                                HJL1986 
                         H 6  71.                                                                MEv2010 
                         GJ 348. A is an X-ray source; also SB1, P=2815d=7.685y (Halbwachs et    HJL2012b
                         al. 2012)                                                               Tok2014d
09292+0024   BAL1151     J 3292.                                                                         
09293-0409   GIC  88     G161-036/G161-037.                                                              
                         NLTT 21891/21892                                                        Chm2004 
09293-4432   DUN  77     B is CD-43@5332.                                                                
                         AB: SHY 210. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
             EGN  11     Ba,Bb: Single epoch, but likely bound. If so, colors indicate Bb                
                         component is M0-M3 dwarf with mass 0.43 +/- 0.01 Msun.                  Egn2007 
             DUN  77     sp, dDEC 24.65".                                                        Dun1829 
09297+0433   HJ  137     Also known as STF1361.                                                          
09298-6743   BRT1978     A likely plate flaw.                                                    Grv2021b
09299-3629   HDS1364     AB + TOK 440BC: HIP 46572 is called a  "high proper motion star" in             
                         SIMBAD, although its PM and RV are actually quite moderate. The binary          
                         AB has moved little in the 24 years since its resolution by Hipparcos.          
                         We discover the subsystem BC with an estimated period of ~100yr.        Tok2015c
09302+5339   TDS 538     Both A and B are eclipsing binaries.                                    Lhr2015 
09304-5822   RST 408     A is an irregular variable.                                                     
09305+3822   LDS3899     NLTT 21915/21914                                                        Chm2004 
09306+1036   STF1360     AB: HJL 113.                                                            HJL1986 
09307+4502   FLA   1     Also known as ES 2632.                                                          
09307+3339   HJ 1166     7 LMi. STTA100 = H 5  69.                                                       
09307-2724   SWR  75     CPM pair                                                                Skf2004 
09307-4028   COP   1     psi Vel. Identification of ascending node not quite certain.                    
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.70 +/- 0.50, 2.42, and 3.00 Msun, respectively.             Mlk2012 
09308-1623   LDS 272     GWP1189.                                                                Tob2012b
09308-3153   DUN  78     zet 1 Ant                                                                       
09309+4441   STF1358     B is BD+45@1729.                                                                
09309+2658   LDS 909     AB: NLTT 21938/21941                                                    Chm2004 
09312+1407   BPMA 37     [PM2000]  946218 + [PM2000]  946038.                                    Gvr2010 
09313-1329   KUI  41     Ross 440. The primary is probably a flare star.                                 
                         Pair often unresolved, so orbit probably eccentric with P<10y.          Kui1943 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 0.74 +/- 0.21, 0.80, and 0.30 Msun, respectively.             Mlk2012 
09314-0012   BVD  77     GWP1190.                                                                        
09315+6304   STF1351     23 Uma. The primary is a Delta Scuti-type variable.                             
                         AB: H 4  29.                                                            MEv2010 
                         CHARA Array Limb-darkened diameter  1.133 +/- 0.009 mas,                CIA2012e
                         R =  2.902 +/- 0.026 \rsun, L = 15.086 +/-0.330 \lsun,                          
                         Teff = 6693 +/-  45 K, M = 1.824 +/- 0.016 \msun,                               
                         Age =  1.4 +/- 0.1 Gyr.                                                         
09317+3830   AG  168     BD+39@2255a.                                                                    
09320+0943   SHJ 107     6 Leo. STTA101 = H 5  26. A is spectroscopic binary. B is BD+10@2015.           
09320-0111   CHR 174     tau 2 Hya = 32 Hya. A spectroscopic binary, now probably resolved.              
                         Abt & Biggs (1972) note variable RV.                                    AbH1972 
09320-6720   RSS  12     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
09321+3531   KU   97     AB: Same as KU  144.                                                            
09322-6247   FIN 140     A is a Mira-type variable, R Car.                                               
09327+3458   ES  299     Erroneously identified as +35 2017.                                     Dam2013 
                         BC also known as POP  56.                                                       
09327+2659   LDS3903     NLTT 22012/22015                                                        Chm2004 
             LAF  38     Heinze et al. (2010) determine the C component is a background object.  Hze2010 
09327+0152   FIN 349     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.59 +/- 1.32, 3.23, and 1.22 Msun, respectively.             Mlk2012 
                         Omega for Tokovinin et al. (2015) orbit flipped by 180deg, at request           
                         of author.                                                              Tok2015c
09327-2826   I  1616     B is CD-27@6693. B is variable.                                                 
09328+0249   J  2498     Not found by Heintz at IDS position.                                    Hei1985a
09328-5706   SYO   1     Spectral type B6/7II/III.                                                       
09329+5141   BU 1071     the UMa = 25 UMa. A is a spectroscopic binary.                                  
                         CHARA Array Limb-darkened diameter  1.632 +/- 0.005 mas,                CIA2012e
                         R =  2.365 +/- 0.008 \rsun, L =  7.871 +/-0.158 \lsun,                          
                         Teff = 6300 +/-  33 K, M = 1.506 +/- 0.095 \msun,                               
                         Age =  2.4 +/- 0.7 Gyr.                                                         
                         NPOI Limb-darkened diameter  1.662 +/- 0.013 mas, Sp = F7V,             NOI2018 
                         R = 2.41 +/- 0.02 \rsun, Teff = 6256 +/- 82 K, L =  8.0 +/- 0.4 \lsun.          
                         HIP 46853. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
09331-3908   JC   21     B is CD-38@5675.                                                                
09333+0910   A  2756     Aka TOI 5128.                                                                   
09333-3838   GLI 292     Also known as RSS 206. #110 in the original list of Gilliss.                    
09334-0711   CBL 131     A: HR 3805. Ren & Fu (2013) calculated an astrometric orbit, combining  Ren2013 
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Griffin (1981).                                                         Grf1981c
                         A: SB1. Combined orbit including RV data and Hipparcos Intermediate             
                         Astrometric data. Semimajor axis derived from photocentric a0 plus              
                         stellar evolutionary model. Derived properties for A and B:                     
                         M/Msun = 1.51 + 0.50, L/Lsun = 63.57 + 0.04, dm = 8.00 mag,                     
                         log age = 9.45.                                                         WaX2015b
09336-4945   DUN  79     B is CD-49@4504.                                                                
                         Identified as optical and linear solution also published.               LRR2022c
09337-4900   HJ 4220     1995.1024: Quadrant determined by speckle imaging analysis.             Hor1996 
09338-1020   WSI 142     AD: Originally assigned to A   131AC.                                   WSI2010 
                         Correct ID provided by Friedrich Damm.                                  Dam2012 
09339+1530   BPM 562     A is also a 3.1d spectroscopic binary.                                  Tok2019b
                         [PM2000]  948128 + [PM2000]  948150.                                    Gvr2010 
09341+3826   HJ 2499     ALI 845. Schembor measures 1926.28, 290.4@, 31.73".                     Sch1927b
                         1900: 09 28.2 +38 51.                                                           
09343+6648   STF1350     Neither AB, AC or BC are physically associated.                         Kiy2015c
09347-1236   STF1370     B is BD-11@2669.                                                                
09348-1208   GC 13236    Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from the Geneva           
                         Extrasolar Planet Search Programs home page.                            HaI2001 
09348-3716   SWR  76     CPM pair                                                                Skf2004 
09349-6500   SHY 548     AC: HIP  47017 + HIP  47115.                                                    
             SHY 546     AD: HIP  47017 + HIP  47351.                                                    
             SHY 550     AE: HIP  47017 + HIP  47335.                                                    
             SHY 548     CD: HIP  47115 + HIP  47351.                                                    
             SHY 548     CE: HIP  47115 + HIP  47335.                                                    
             SHY 543     CF: HIP  47115 + HIP  46460.                                                    
09350-4339   DON 344     CPD-43@3821.                                                                    
09352+1405   STTA102     B is BD+14@2114.                                                                
09353-1019   LDS6229     NLTT 22125/22121                                                        Chm2004 
                         B is BD-09@2878.                                                                
09354+3958   COU2084     A: DI Lyn. Aa is a 1.7d SB2.                                                    
                         Aa is also eclipsing binary DI Lyn (period 1.68154 day).                Zas2010 
                         A is SB1, P=438d                                                        Tok2014d
             STF1369     AB: B component is 28d SB1. AB pair has an estimated period ~40,000y.   Tok2006 
                         SHY 542. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AB: H 4  30.                                                            MEv2010 
09356+1729   BPM 563     [PM2000]  949349 + [PM2000]  949420.                                    Gvr2010 
09356-1935   S   604     B is BD-18@2729.                                                                
09357+3549   HU 1128     11 LMi = SV LMi. Companion not seen 1941-1958 (82-inch).                VBs9999 
                         A is slightly variable, SV LMi, P = 18d, probably due to starspots.     B__1963b
                         CHARA Array Limb-darkened diameter  0.821 +/- 0.013 mas,                CIA2012e
                         R =  1.003 +/- 0.016 \rsun, L =  0.784 +/-0.007 \lsun,                          
                         Teff = 5434 +/-  45 K, M = 0.910 +/- 0.020 \msun,                               
                         Age = 10.6 +/- 2.2 Gyr.                                                         
09359+1423   H 5  58     H V 58. 7 Leo.                                                                  
                         B is BD+15@2078.                                                                
09361+3733   SKF 254     SHY 211. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         Also known as CAB   2.                                                  Cab2011 
                         B is also a 4.4d spectroscopic binary.                                  Tok2019b
09362+1436   ARN  72     HJL 114.                                                                HJL1986 
09364-4845   R   125     A is the variable IM Vel.                                                       
09365+2820   ES  428     Beta Lyr (EB) type eclipsing binary, P = 0.379496 d.                    Zas2011 
09367-4145   BRT 765     CPD-41@3877.                                                                    
09370-2610   WSI 127     The companion discovered with AstraLux is probably physical given the           
                         rather small separation (~0.39"), but so far only one epoch of imaging          
                         exists.                                                                 Jnn2012 
09371-1350   BRT1909     J 3311.                                                                         
09372-4316   EGN  12     Pair likely unbound.                                                    Egn2007 
09372-5340   SEE 115     1995.1024: The WDS Catalog lists equal magnitudes and nearly equal              
                         spectral types for this object. Our observations do not unambiguously           
                         determine the quadrant in this case, so we adopt the same quadrant as           
                         the most recent observation listed in the WDS.                          Hor1997 
                         1997.1229: The magnitude difference of the system is listed in the WDS          
                         as 0.0.  Our reduction does not give the same quadrant as the latest            
                         measure in the WDS.                                                     Hor1997 
09375-5000   HU 1465     HIP 47225. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AB: A=SB? Jones et al. (2002) do not detect SB sub-system with precise  CPS2002b
                         RV.                                                                     Tok2014d
09376+6013   SHY 549     HIP  47231 + HIP  46170.                                                        
09378-4031   CPO 267     CPD-39@3770.                                                                    
09379+4554   A  1765     Incorrectly listed as A 1785 (Erratum noted in Inf. Circ 98, 1986)      Baz1985d
                         Incorrectly listed as ADS 7547 (Erratum noted in Inf. Circ 98, 1986)    Doc1985d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 5.33 +/- 2.42, 2.12, and 1.49 Msun, respectively.             Mlk2012 
09383+4827   OSO  28     G195-035. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
09384+7242   FAR   9     Primary is white dwarf WD 0933+729.                                     Far2005b
09385-0256   TOK 128     HIP 47312. A is SB without orbit, dRV=18.7.                             Nrd2004 
                         A is SB1, P=33.222 d                                                    Tok2014d
09388+0242   J    78     Aka WAM   2.                                                            Dam2016b
                         Rectilinear solutions by Cvetkovic (2015)                               Cve2015b
                         and Cvetkovic et al. (2016).                                            Cve2016 
09389-2016   B   779     J 1554.                                                                         
09392+3014   LDS3909     SLW 375.                                                                        
09392-0247   CUD   5     Component A is the central star of the planetary nebula PN G238.0+34.8  Skf2013 
                         = Abell 33.                                                                     
09393+1319   TOK 270     Primary is SB2, P=25.614d, and occultation binary.                      Tok2014d
09394-5731   RST 419     Spectral type G8/K0II/III.                                                      
09398-1034   CHR 175     1988.1677  Abt & Biggs (1972) note variable RV.                         AbH1972 
                         OW Hya, Algol-type eclipsing binary, P = 14.39303 d.                    Zas2011 
09398-4104   TDS6725     This star is listed as a Tycho double star in the WDS catalog, with a           
                         separation of 600 mas and equal brightness. However, it appears                 
                         entirely single in our AstraLux data. Although we cannot strictly rule          
                         out that the companion is presently too close to be resolved with               
                         AstraLux (e.g. due to a close to edge-on orbit and unfortunate timing           
                         of the observation), we consider it relevant to regard the possible             
                         companion as unconfirmed at present.                                    Jnn2012 
09398-5008   RST4917     1995.1024: Quadrant determined by speckle imaging analysis.             Hor1996 
                         1997.1229: A smaller annulus was used in the power spectrum fit due to          
                         the faintness of the source. As a consequence, the separation and               
                         position angle uncertainties may be larger than other measures.         Hor1997 
09400+3520   SHY 212     HIP  47436 + HIP  47403.                                                        
                         B = HIP 47403 at 494", same PM and parallax but different RV. Is B SB?  Tok2014d
09400+2222   LDS3912     NLTT 22295/22294                                                        Chm2004 
09400-1710   STN  19     Algol-type eclipsing binary, period 0.55925 d.                          Zas2019 
09404+5915   LDS1230     SLW 379.                                                                        
09405+6832   HIP  47461  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Ginestet et al. (1991). They derived component masses 1.82 and 1.28     Gin1991 
                         Msun and an estimated semimajor axis of 16.44 mas.                      Ren2013 
09407+1500   BPMA 38     [PM2000]  952706 + [PM2000]  952794.                                    Gvr2010 
09407-0417   OSO  29     G161-059. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
09407-5759   B   780     Variable RV. with a range of 40 km/s observed in 1912-13.                       
                         Speckle observations needed to confirm orbit. Sp subsystem in sec?              
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 5.83 +/- 0.53, 3.09, and 2.09 Msun, respectively.             Mlk2012 
09409-4913   R   128     B is CD-48@4895.                                                                
09412+0954   HMM   1     Aa,Ab: 4 Leo = omi Leo = Subra                                                  
                         A 1980 observation of 09285+0903 = ome Leo by Weigelt (1983) was        Wgt1983 
                         incorrectly attributed to this star (= omi Leo) in earlier editions             
                         of the interferometric catalog and the WDS. This star was then                  
                         mistakenly given the discoverer designation WGT   1 as a result.                
                         Hummel et al. (2001) include data from the Mark III, NPOI, and PTI      Hmm2001 
                         interferometers. Dates have been converted from Julian to Besselian;            
                         error ellipses have been converted into quoted rho and theta errors.            
                         The Mark III data were taken with baselines of 28.0 and 31.5 meters,            
                         using 500, 550, and 800nm filters. NPOI data were taken using three             
                         baselines from 19 to 38 meters and in 20 channels from 530 to 850nm.            
                         The paper also includes radial velocity data and a combined                     
                         spectroscopic/astrometric orbital solution, yielding a distance and             
                         component luminosity and mass information as well.                              
                         P = 14.498064 +/- 0.000009 days, T = JD2450629.831 +/- 0.003;                   
                         eccentricity assumed zero.                                                      
                         Aa,Ab: Malkov et al. (2012) derive dynamical and spectroscopic                  
                         masses 3.59 +/- 1.93 and 7.07 Msun, respectively.                       Mlk2012 
             ARI   1     Aa,Ac: Hummel (2003, private communication) says there was no sign of           
                         the ARI component in their Mark III and NPOI observations, which        Ari1999 
                         resolved the closer pair HMM   1Aa,Ab. See Hummel et al. (2001).        Hmm2001 
             H 6  76     AB: H VI 76. Optical pair, based on study of relative motion of the             
                         components using the method of apparent motion parameters.              Kiy2008 
09412-3822   SWR  77     CPM pair                                                                Skf2004 
09412-5349   KRV  23     Classical Cepheid CS Vel.                                                       
09413+0256   HEI 752     TDS 547.                                                                        
09416+1532   LDS3915     The primary is the variable DR Leo.                                             
09422-6655   HJ 4241     B is CPD-66@1039.                                                               
09424-0750   BRT 547     J 3232.                                                                         
09425-6229   JNN  70     The two components of this binary have almost equal brightnesses and            
                         colors, hence they are very likely to form a physical pair. Common              
                         proper motion has not yet been tested.                                  Jnn2012 
09427+7004   OSV   3     Also known as ODE   1 or LDS 911.                                               
                         NLTT 22340/22350                                                        Chm2004 
             LDS1698     BC: The C component is listed in the NLTT catalog as Grw+70:4337.               
                         However, no object is apparent on Aladin fields at the purported                
                         position.                                                                       
09431-8120   R   133     LDS 286. B is CPD-80@388.                                                       
09434+0858   HJ  820     STF3122.                                                                        
09435-5114   B  1658     A is the variable IP Vel.                                                       
09437+1401   BUP 128     psi Leo = 16 Leo                                                                
09438+5557   ES 1825     A is W UMa, prototype of its class.                                             
                         A is SB2E, P=0.334d. M1sin3i = 1.14, M2sin3i = 0.55, V0=-28.40                  
                         (Pribulla 2007 AJ 133, 1977). Both A and B are 1.3mag above MS. Wrong           
                         parallax? Hip: code S, acceleration?                                    Tok2014d
09438+0429   J  2499     BAL 2838.                                                                       
09442-2746   FIN 326     the Ant. Spectrum composite; A8V+F7II-III.                                      
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 6.27 +/- 1.23, 5.74, and 1.13 Msun, respectively.             Mlk2012 
                         Docobo & Andrade (2013) derive a dynamical parallax of 10.08 +/- 0.47           
                         mas and component masses 2.1 +/- 0.5 and 1.8 +/- 0.1 Msun. See paper            
                         for extensive notes on this system.                                     Doc2013d
09445+4830   HJ 2503     B is BD+49@1874.                                                                
09446+6459   CHR 176     Cvetkovic et al. (2016) estimate spectral types A4 and A4, masses 2.10          
                         and 2.10 Msun. Dynamical parallax is 9.61 +/- 0.08 mas.                 Cve2016b
09449-0745   J  3250     BRT 430.                                                                Brt1931 
09450-4929   DUN  80     AB: B is CD-48@4963.                                                            
09450-6719   WFC  88     SWR  78. CPM pair                                                       Skf2004 
09451-4502   CPO 271     Aka R   131.                                                                    
09452+4109   SHY 551     AD: HIP  47851 + HIP  47399.                                                    
09452+2327   LDS5705     LDS6230.                                                                        
                         NLTT 22492.  White dwarf pair = WD 0942+24 = EGGR 533/534               Grn1986 
09452-6230   EVS  15     Primary is the Cepheid l Car.                                           Evs2016a
09453+0853   STF1379     Also known as CHE 141 and CHE 142.                                              
09455+4616   LDS3922     SLW 388.                                                                        
09456+1242   BPM 564     [PM2000]  955909 + [PM2000]  955928.                                    Gvr2010 
09457+4104   A  2138     Aka BAR  37.                                                                    
09459+6339   KUI  43     28 UMa. A is a spectroscopic binary.                                            
09459-2145   RSS 215     CPD-21@4482                                                                     
09460-0306   B  2549     Spectral type F2. Found while measuring RST4440 nearby. As it was               
                         missed in the Lick Survey and also by Rossiter in 1939 and is now               
                         easier than Rossiter's pair, it must have opened out.                   B__1963b
09461-0425   JNN 276     LHS 2186. Estimated age 1000-10000 Myr; masses 0.24 +/- 0.07 and 0.20           
                         +/- 0.06 Msun; a ~18.9 au.                                              Jnn2014 
09461-2301   DON1086     CD-22@7568.                                                                     
09464-4329   SWR  79     CPM pair                                                                Skf2004 
09465-0925   LDS3926     NLTT 22564/22562                                                        Chm2004 
09468+7603   Ross 434    GJ 366 = Ci 20,545                                                              
                         Alden orbit rejected from Fourth Orbit Catalog                          Ald1951 
                         ("not confirmed by subsequent observations")                            Wor1983 
09471-6504   RMK  11     ups Car                                                                         
                         Rectilinear solution by Letchford et al. (2018).                        LRR2018a
09474+1134   MCA  34     19 Leo. First detected as an occultation binary by Eitter & Beavers.    Bvr1974 
                         Mason et al. (1997) orbit includes mass determination.                  Msn1997a
                         1980.1538: Theta was incorrectly given as 206.6 degrees in McAlister            
                         et al. (1983).                                                          McA1983 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.57 +/- 0.49, 3.65, and 1.66 Msun, respectively.             Mlk2012 
09474-3953   WG  128     LDS 283.                                                                        
09476+1126   R Leo       1976.397: Disk resolved (0".030 +/- 0.007 at 770 nm, 0".054 +/- 0.009           
                         at 750 nm, 0".049 +/- 0.009 at 730 nm, 0".032 +/- 0.005 at 540 nm).     Bla1977a
09477-2823   UC 1830     CPM candidate confirmed physical by photometry (2MASS and V mags).      Tok2013c
09477-3736   JSP 348     CPD-37@3758.                                                                    
09478+4252   LDS3928     NLTT 22591/22590                                                        Chm2004 
09478-6507   HJ 4252     B is CPD-64@1087.                                                               
09481-2816   SEE 116     I  1131.                                                                        
09482-1011   LDS 281     NLTT 22642/22643                                                        Chm2004 
09489+0858   TOK 130     HIP 48146.                                                              Tok2011a
09490+3405   STF1382     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
09497-1217   FOX 162     Appears to be the same as the lost OL  212. Merged.                             
09498+2111   KUI  44     20 Leo. B is a Delta Scuti-type variable, DG Leo.                       Cou1955c
                         A is a double-lined spectroscopic binary, P=4.147d.                             
                         Radial velocity is variable, amplitude 30 km/sec (Plaskett). Two                
                         spectra are visible (Shajn & Albitzky)                                  Dan1952 
                         Lampens et al. derive effective temperatures for the Aa, Ab, and B      Lmp2008 
                         components of 7470+/-220, 7390+/-220, and 7590+/-220 K, respectively.           
                         Relative fluxes from these three late-A stars are similar: 32+/-2,              
                         31+/-2, and 37+/-2%.                                                            
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.95 +/- 1.87, 4.29, and 1.82 Msun, respectively.             Mlk2012 
09498+1106   TOK  24     Visual pair has estimated period 130y; primary is 3.4d SB1.             Tok2006 
09500-4544   HJ 4254     B is CD-45@5471.                                                                
09502+0509   LDS3936     G043-007. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
09504-5011   HJ 4257     B is CD-49@4737.                                                                
09505+0421   LEP9001     AB: Primary is 4 Sex and is SB2.  B is accepted as real because of              
                         large PM and low crowding.                                              Tok2014d
09505-6058   BNS   5     V596 Car = Hen 3-331                                                            
09506+3950   UC  142     Secondary appears to be a close pair.                                   Cbl2010c
09508+1151   J   389     21 Leo.                                                                         
09508+0341   A  3081     Less than 0.1" in 1956. Not seen double since 1935.                             
09508+0118   LUH   8     AC: LHS 6176 + ULAS J095047.28+011734.3. Companion is likely physical,          
                         based on CPM. J and H photometry of C from UKIDSS Data Release 8.       Luh2012b
09509+1919   STTA103     AB: Pair appears in an appendix list, not part of discoverer's regular          
                         numbering sequence.                                                             
09509+1045   BPM 565     [PM2000]  959252 + [PM2000]  959285.                                    Gvr2010 
09510+5902   STT 521     ups UMa = 29 UMa. A is a Delta Scuti-type variable.                             
09511+3558   RED  13     Primary is NLTT 22741 = LP 261-75, secondary 2MASS J09510549+3558021.           
                         Distance to system 28.0 +/- 5pc, upper age limit about 2.2 Gyr. It is           
                         uncertain whether the pair is physically bound.                         Sef2005b
                         Reid et al. (2006) combine near-IR imaging with 2MASS data and optical  Red2006c
                         spectroscopy; conclude the stars form a CPM pair, with separation 450           
                         +/- 120au and a distance of 38 +/- 10pc. The primary (LP 261-75) is an          
                         M4.5 dwarf; spectral type of the secondary is L6, with mass perhaps             
                         ~0.02 Msun.                                                                     
09512+3629   HO  369     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.40 +/- 0.92, 2.79, and 1.35 Msun, respectively.  Mlk2012 
09513-4612   GC 13574    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
09515+0830   OCC9038     OCC9150.                                                                        
09516-5917   COO  94     Aka HRG  36.                                                                    
09521+5404   STT 208     phi UMa = 30 UMa.                                                               
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 14.53 +/- 5.60, 8.84, and 2.09 Msun, respectively.            Mlk2012 
09522+3930   MLB 842     BRT 2221. ALI 1087.                                                             
09522+0807   A  2762     Rectilinear solution by Hartkopf & Mason (2013).                        Hrt2013b
09522+0313   BAL2368     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
09524+4454   FAR  34     Primary is white dwarf WD 0949+451.                                     Far2006 
09525-0806   AC    5     gam Sex = 8 Sex.                                                        Mlr1956a
                         AB: Additional notes may be found in Fu et al. (1997)                   McA1997 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 6.37 +/- 2.00, 4.61, and 2.19 Msun, respectively.  Mlk2012 
             HJ 4256     AB,C: H N  49.                                                          MEv2010 
09527-7933   KOH  86     A is an unresolved close pair with a period of ~8y, and the secondary           
                         of this close pair is a yet closer pair ~2.4d. Parameters for the four          
                         four components are : Vmag,Kmag : Aa = 10.37,8.80; Ab = 11.53,9.96;             
                         Ac = 11.53, 9.96; B = 11.70,9.73. Masses : Aa = 1.30; Ab = 1.05;                
                         Ac = 1.05; B = 1.02 (all in \msun).                                     Tok2018f
09528+1821   ZUC   7     Primary is white dwarf PG 0950+185.                                     Zuc1992 
09530+1345   LIE   2     Primary is PG 0950+139, white dwarf central star of planetary nebula            
                         EGB 6.  Companion is M dwarf.                                           Lie2013b
09531-5501   R   137     B is CPD-54@2822.                                                               
09535+1657   CHR 219     First detected as an occultation binary by Evans et al.                 Evn1985 
09541+0457   S   605     9 Sex. B is BD+05@2247.                                                         
09546+4023   KLT   3     KELT-3. Primary hosts a transiting hot Jupiter.                         KLT2013 
09549-1750   FEN  16     J 2654.                                                                         
09551+2438   TOK 272     Primary is SBs, P=1385d                                                 Tok2014d
09551-6911   RMK  12     Rectilinear solution by Letchford et al. (2018).                        LRR2018a
09554+1007   STF1395     HJL 116.                                                                HJL1986 
09554-1335   LDS3943     NLTT 22946/22953                                                        Chm2004 
09564+1040   STF1396     AC. Schiaparelli's value for rho is apparently a typographical error,   Sp_1909 
                         as it is identical (3".778) to his AB measure. His C component may be           
                         a 13th magnitude star located 90 deg, 58" from AB, although the                 
                         magnitude difference would appear to make the necessary quadrant flip           
                         unlikely.                                                                       
09565+6932   LDS2581     NLTT 22918/22922                                                        Chm2004 
09568-5713   BRT2556     BRT3132.                                                                Brt1951 
09569-5434   I   396     phi Vel = phi Arg                                                               
09570+1946   STF1399     B is BD+20@2400.                                                                
                         NLTT 23007/23008                                                        Chm2004 
                         HJL 117.                                                                HJL1986 
09571-0121   A  1766     Primary is eclipsing binary of Algol-type, period 0.98705d.             Zas2014 
09573-2902   WHC  30     B is CD-28@7774.                                                                
09575+1030   BPM 566     [PM2000]  963205 + [PM2000]  963219.                                    Gvr2010 
09577+2010   UC 1852     CPM candidate confirmed physical by photometry (2MASS and V mags).      Tok2013c
09577-4825   HJ 4269     A is a spectroscopic binary.                                                    
09579+0959   GIC  89     G042-027/G042-028.                                                              
09579-6045   FIN 152     Spectrum of B is A/F.                                                           
09581-0303   SLW 414     GWP1259.                                                                Tob2012b
09586+0422   ZUC   8     Primary is white dwarf PG 0956+045.                                     Zuc1992 
09586-2420   TOK 437     HIP 48906 is a double-lined binary according to the GCS, first                  
                         resolved here at 64mas. The period should be ~20yr.                     Tok2015c
09587+1058   H 5  63     AB: H V 63.                                                                     
09588+4309   GIC  90     AB,C = G116-071/G116-070.                                                       
                         AB,C: NLTT 23070/23069                                                  Chm2004 
09589-3553   HJ 4271     eta Ant                                                                         
09590+0000   GRV1041     SLW 421.                                                                        
09590-5358   BRT2044     Aka KPP 207.                                                                    
09591+5316   A  1346     H 1  32.                                                                MEv2010 
09591-2326   BRT1481     CD-22@7789.                                                                     
09593+4350   GIC  91     G116-072/G116-073 = GJ 3577A+3578B.                                             
                         NLTT 23087/23091                                                        Chm2004 
09594+3125   SEI 518     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
09594-2329   BRT1482     CD-22@7794.                                                                     
09594-4457   HJ 4273     Equal double lines in the spectrum of A.                                        
09598-2128   DON 376     CPD-20@4801.                                                                    
09598-5916   HJ 4278     B is CPD-58@1765.                                                               
09599+1610   A  2482     Markowitz must have measured some other pair in 1951.                   Wor1967b
10000+2433   CHR 145     The primary is DH Leo, a RS CVn system, and spectroscopic binary with           
                         a period of 1.07d (Barden, AJ 89, 683, 1984). Barden observed three K           
                         stars in his spectra of this system. Fekel (1989, private comm.) has            
                         observed the third component of this system and finds no velocity               
                         changes in excess of +/- 2 km/sec from 12 spectra obtained since 1984.          
                         This new speckle component is thought to be this third spectroscopic            
                         component.                                                              McA1990 
10001-1521   GWP1267     ABL 271.                                                                Tob2012b
10002+0615   STF1401     HJL 118.                                                                HJL1986 
10004-0154   GWP1268     ABL 268.                                                                Tob2012b
10005-0250   GWP1269     ABL 269.                                                                Tob2012b
10007+3219   OSO  30     G118-030. Neither AD or AE is a common proper motion pair               Oso2004 
                         Proper motion of A = -1010,-661 (UCAC2).                                        
10010+3155   RAG   7     GJ 376. Raghavan et al. (2010) consider B as possible eclipsing binary  Rag2010 
                         based on Gizis et al. (2000)                                            Giz2000 
                         CHARA Array Limb-darkened diameter  0.771 +/- 0.012 mas,                CIA2012e
                         R =  1.247 +/- 0.021 \rsun, L =  1.378 +/-0.027 \lsun,                          
                         Teff = 5612 +/-  52 K, M = 1.034 +/- 0.036 \msun,                               
                         Age =  8.5 +/- 1.8 Gyr.                                                         
10010-0651   GWP1270     ABL 270.                                                                Tob2012b
10011-4154   CPO 279     CPD-41@4230.                                                                    
10012-2309   RSS 221     CD-22@7830                                                                      
10012-5606   HDO 209     B is CPD-55@2795.                                                               
10013+3252   OSO  31     G117-063. Not a common proper motion pair, based on astrometry and              
                         color                                                                   Oso2004 
10015+1807   BPM 567     [PM2000]  965525 + [PM2000]  965511.                                    Gvr2010 
10016+5424   STI2239     MLB 125.                                                                        
10017+1725   RUC   7     Elements from Hipparcos Intermediate Astrometric Data are combined              
                         with a light-travel time analysis of eclipse timings by Bakis et al.    Bks2005 
                         XY Leo. Spectral type of resolved companion estimated at K6V.           Ruc2007 
                         Multiple system including contact binary XY Leo. Pribulla & Rucinski            
                         (2006) estimate the mass of the contact pair at 1.378 Msun and the      Pbl2006 
                         minimum mass of the wider component at 1.00 Msun.                               
10019+1354   BPM 568     [PM2000]  965775 + [PM2000]  965789.                                    Gvr2010 
10019-0045   GWP1272     ABL 272.                                                                Tob2012b
10019-1438   GWP1271     ABL 273.                                                                Tob2012b
10019-2841   HJ 4277     B is CD-28@7839.                                                                
10021-5459   DUN  83     B is CPD-54@3041.                                                               
10022-1946   B   781     Primary is the eclipsing binary OZ Hya, P = 2.04876 day.                Zas2010 
10024-3547   BRT1656     TDS6979.                                                                        
10025+1703   RUC  22     Primary is XZ Leo.                                                              
10025-2814   JNN  71     2MASS J10023100-2814280 has a relatively close (~0.56") companion               
                         which is probably real, although this has yet to be confirmed with a            
                         proper motion test.                                                     Jnn2012 
10027+1635   BPM 569     [PM2000]  966270 + [PM2000]  966274.                                    Gvr2010 
10028+1756   BPM 570     [PM2000]  966320 + [PM2000]  966383.                                    Gvr2010 
10028-0134   GWP1273     ABL 275.                                                                Tob2012b
10028-1248   GWP1274     ABL 279.                                                                Tob2012b
10029+6847   STF1400     Very similar in characteristics to STF 1398. Observers have confused            
                         them.                                                                           
                         Despite the linear solution, proper motion and parallax favor a         Grv2020a
                         physical connection. Long period and/or high eccentricity possible.             
             ODE   7     AC: C is found in 2MASS, matching color, physical?                      Tok2014d
10030+0207   GRV1042     SLW 427.                                                                        
10030-5329   GRV1254     Both A and B have approximately the same radial velocity.               Grv2019b
10031-1837   GWP1276     ABL 281.                                                                Tob2012b
10032-0557   GWP1278     ABL 276.                                                                Tob2012b
10032-0658   GWP1277     ABL 277.                                                                Tob2012b
10032-1420   GWP1279     ABL 280.                                                                Tob2012b
10032-5203   HJ 4282     B is CD-51@4435.                                                                
10034+5732   A  1347     The scattered measures show evidence of rapid motion.                           
10034+0203   HJ 1174     BAL 1866.                                                                       
10036-0852   GWP1280     ABL 278.                                                                Tob2012b
10036-2903   TOK 131     HIP 49285.                                                              Tok2011a
10039+0150   HJ 3320     BAL 1867.                                                                       
10040-1806   SHJ 110     AC: H N  25.                                                            MEv2010 
10041-7604   HJ 4288     B IS CPD-75@634.                                                                
10042-0426   GWP1284     ABL 282.                                                                Tob2012b
10043-0142   STF1404     HJL 119.                                                                HJL1986 
10043-0458   GWP1285     ABL 283.                                                                Tob2012b
10043-2823   I   292     A premature orbit has been computed.                                            
                         The A component has a spectroscopic component with a period of 45d. It  Tok2020h
                         is thought that the B component also has a spectroscopic companion of           
                         unknown period.                                                                 
10044+5023   REB   1     G196-003. Spectral types are M2.5 +/- 0.5 and L, masses 0.40 +/- 0.05           
                         Msun and 25 +25/-10 Mjup, respectively.                                 Reb1998 
                         Jameson et al.(2008) confirm the CPM nature of this pair.               Jms2008 
10044+3611   GRV1183     SLW 429.                                                                        
10045-5840   MIF   1     MWC 198 = V640 Car. Primary is a B2e star with a complex circumstellar          
                         environment. Millour et al. (2009) resolve a close companion, and               
                         estimate the orbital period as 20-50y; polarisation suggests a high             
                         inclination, and there is also evidence suggesting high eccentricity.   MiF2009 
10046-3335   SEF   2     LHS 5166 + 2MASS J10043929-3335189. Distance to system 19.0 +/- 3.0pc,          
                         mass of L4 companion 0.070 +0.005/-0.015 Msun.                          Sef2005b
10050-5119   HU 1594     1995.1024: Quadrant determined by speckle imaging analysis.             Hor1996 
10052-2812   I   293     Rectilinear solution by Zirm (2013).                                    Zir2013d
10056+3105   STF1406     STT 211.                                                                        
10056-8405   HJ 4310     AB + TOK 396Aa,Ab: HIP 49442 = HD 88948 is a nearby dwarf in the 3".9           
                         visual binary HJ 4310 AB. According to GCS, the RV of the main                  
                         component A varies by 3.5km/s. Here it is resolved into a 0".18 Aa,Ab           
                         pair with an estimated orbital period of 25yr. No astrometric                   
                         acceleration was detected, however. The visual secondary B was                  
                         targeted separately and found unresolved.                               Tok2015c
                         AB: A is SB, no orbit.                                                  Tok2014d
10062+4105   TOK 535     A comp is SB2, P=2073d                                                  Tok2014d
10062-3514   SWR  83     CPM pair                                                                Skf2004 
10063+3457   DAM 647     C component identified with galaxy LEDA 2057027, and therefore not      Dam2019b
                         a double star.                                                                  
10063-0626   GWP1289     ABL 286.                                                                Tob2012b
10063-1735   GWP1288     ABL 287.                                                                Tob2012b
10064-0046   GWP1290     ABL 284.                                                                Tob2012b
10066-0519   GWP1293     ABL 285.                                                                Tob2012b
10066-1919   TOK  66     Ba,Bb: Estimated masses 0.92 and 0.26 Msun; sep 12.6 au, period 40 y.   Tok2010c
10066-1926   GWP1292     ABL 288.                                                                Tob2012b
10067+1754   HDS1457     The primary is a bright G-type star, mass 1.12 +/- 0.09 Msun, radius            
                         1.55 +/- 0.02 Rsun, Teff 5770 +/- 80K. Hipparcos gives a parallax of            
                         13.59 +/- 1.58 mas (73.58 +/- 9.68pc). Ma et al. (2016) resolve two     MaB2016 
                         close companions, in addition to the HDS companion, and determine some          
                         orbital elements for all three pairs. The Ab companion is likely a              
                         giant planet or brown dwarf, depending on the inclination angle;                
                         mimimum mass is 12.4 +/- 0.7 Mjup. The Ac companion is likely a brown           
                         dwarf; minimum mass 57.7 +/- 3.7 Mjup. The closest companion appears            
                         to be new, so is given the designation MAB 2Aa,Ab. The Ac component             
                         has a separation similar to the unconfirmed companion measured by               
                         Balega et al. (2006) in 2001, so the BAG 23 designation is retained,    Bag2006b
                         although the component pair is changed to Aa,Ac to match that of Ma.            
10067-1234   GWP1294     ABL 292.                                                                Tob2012b
10067-7045   NZO  15     Not found by Heintz at IDS position. The spectral type of -70@964 is    Hei1987a
                         K1/2III/IV.                                                                     
10068+0537   CHR  30     14 Sex.                                                                         
10069+3539   BRT2593     ALI 358.                                                                        
10070-4026   KTK   1     Central star of the planetary nebula NGC 3132.                                  
10070-7129   TOK 397     HIP 49546 is an astrometric binary of 1.5yr period (Goldin & Makarov            
                         2006) with variable RV. The period corresponds to a semi-major axis of  Gln2006 
                         25mas. The star is resolved here tentatively at 26mas. This resolution          
                         is below the diffraction limit and needs confirmation. The measured             
                         position angle of 346deg is close to 342deg predicted by the                    
                         astrometric orbit.                                                      Tok2015c
10071-1119   GWP1295     ABL 291.                                                                Tob2012b
10072-2220   RST3679     CPD-21@4616.                                                                    
10073+1646   WRH  18     eta Leo = 30 Leo. Occultation binary now confirmed by speckle.                  
                         Additional notes may be found in Wilson (1941).                         WRH1941b
10075-3325   SWR  84     CPM pair                                                                Skf2004 
10075-5904   COO  97     B is CPD-58@1922.                                                               
10077-0644   GWP1297     ABL 289.                                                                Tob2012b
10077-0905   RST3681     TDS7042.                                                                        
10077-0916   GWP1298     ABL 290.                                                                Tob2012b
10078+0715   HEI 755     Also known as TDS7045.                                                          
10079+1000   GAN   5     31 Leo.                                                                         
                         NPOI Limb-darkened diameter 3.33 +/- 0.04 mas,                          NOI1999 
                         R = 30.  +/- 2.  \rsun.                                                         
                         NPOI Limb-darkened diameter    3.476 +/- 0.048 mas,                             
                         R =   33.90 (+0.70- 0.71)  \rsun,  Teff = 4066 +/-  29 K,                       
                         L =  283.3 +/-   9.0 \lsun.                                             NOI2023 
10079-1610   GWP1299     ABL 293.                                                                Tob2012b
10081-6405   RST 471     Aka HRG  48.                                                                    
10083+3136   KUI  48     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.77 +/- 0.22, 2.92, and 1.25 Msun, respectively.  Mlk2012 
                         AB Visual orbit, P=17.765y (Hartkopf et al. 1996). SB period 8.882yr    Hrt1996a
                         (Tremko et al. 2010 CoSka 40, 83)                                       Tok2014d
10084+6620   LDS1235     Primary is NLTT 23425. According to the LSPM, the secondary is                  
                         NLTT 23425; however, no object is visible on Aladin images at its               
                         purported position.                                                             
10084+1158   STFB  6     alp Leo = 32 Leo = Regulus.  LDS 913.                                           
                         Intensity Interferometer Limb-darkened diameter 1.37 +/- 0.06 mas.      HBr1974 
                         CHARA Array major, minor axis diameter : 1.65, 1.25 +/- 0.02 mas,       CIA2005 
                         polar      radius = 3.14 +/- 0.06 \rsun, T = 15400 +/- 1400 K.                  
                         equatorial radius = 4.16 +/- 0.08 \rsun, T = 10314 +/- 1000 K.                  
                         mean T = 12901 +/- 500 K, M = 3.4 +/- 0.2 \msun, L = 347 +/- 36 \lsun.          
                         NPOI Limb-darkened diameter  1.664 +/- 0.037 mas, Sp = B6IV,            NOI2018 
                         R = 4.35 +/- 0.10 \rsun, Teff = 11668 +/-195 K,                                 
                         L = 316.2 +/-16.7 \lsun, M = 3.57 +/- 0.04 \msun,                               
                         Age = 0.16 +/- 0.01 Gyr.                                                        
                         AB: H 6  11.                                                            MEv2010 
10084-1945   BU  911     HIP 49668. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AB  CfA: A=SB?                                                          Tok2014d
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
10085+6826   ENG  41     B is BD+69@557.                                                                 
10085+1712   BPMA 39     [PM2000]  969450 + [PM2000]  969537.                                    Gvr2010 
10086-0014   GWP1300     ABL 294.                                                                Tob2012b
10086-7500   SWR  86     Late-K/M giants, not G8 dwarfs. CPM pair                                Skf2004 
10087-0951   GWP1301     ABL 296.                                                                Tob2012b
10087-6549   HJ 4292     B IS CPD-65@1250.                                                               
10088+1401   BPMA 40     [PM2000]  969633 + [PM2000]  969471.                                    Gvr2010 
10090-0741   GWP1302     ABL 295.                                                                Tob2012b
10091-3448   HJ 4287     SWR  85.                                                                        
10092+3320   GRV 812     HJL 120.                                                                HJL1986 
10093+2020   A  2145     Composite spectrum binary, classified G2III+A2V by Markowitz                    
                         (1969 Dissertation, Ohio State Univ.), who quotes delta m = 1.1.                
                         It is not known which spectrum belongs to the visual primary.                   
                         Only elements P and T have been amended by Starikova (1977) from the    Sta1977a
                         second orbit of Baize (1957).                                           Baz1957a
                         1983.9371, 1983.9372: Interferometric observations are in disaccord     Wor1983 
                         with the 1957 orbital elements of Baize (see Worley & Heintz 1983).     Bnu1984 
                         1984.1861, 1984.2814, 1985.2053: The speckle interferometric                    
                         observations show that Finsen's orbit fails to describe the orbital     Fin1977a
                         motion of this system.                                                  Bnu1986 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 13.28 +/- 8.31, 6.98, and 3.29 Msun, respectively.            Mlk2012 
10095-6841   I    13     AB. 1997.1230: Our reduction does not give the quadrant unambiguously.          
                         We therefore adopt the quadrant consistent with the latest measure in           
                         the WDS.                                                                Hor1997 
10098-0502   GWP1304     ABL 297.                                                                Tob2012b
10098-6001   TDS7075     JAW  13.                                                                        
10099+5420   MLB 126     STI2243.                                                                        
10100+1623   A  2367     AB: HJL 122.                                                            HJL1986 
10100-1901   GWP1305     ABL 298.                                                                Tob2012b
10101-0157   HJ  153     ID uncertain, but appears to be most likely system in region                    
10102-6505   BRT1983     TDS7077.                                                                        
10103+3825   HDS1465     Only one HIP measure, presumably wrong. Component B in 2MASS at                 
                         343.7d, 11.33", likely physical.                                        Tok2014d
10106-1221   BU  593     lam Hya = 41 Hya. A is a spectroscopic binary.                                  
10106-1222   lam Hya     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Jones (1928).                                                           Jon1928f
10110+7508   KUI  47     Not resolved in images.                                                 Oso2004 
                         Poorly determined (long) period, only periastron-part covered.                  
10110-4814   BRT 775     CPD-47@3979.                                                                    
10111-1031   GWP1308     ABL 301.                                                                Tob2012b
10112+7622   HJ 3319     LDS1708.                                                                        
                         HJL 121.                                                                HJL1986 
10113+1001   BU 1425     Early component confusion. The 73" pair was apparently initially                
                         designated AB, but a note in the BDS indicated the pair "is not         Bu_1906 
                         BD+10 2119, but smaller stars 47s f 31 Leo". The pair was redesignated          
                         FG, and as a result the system has no AB pair. The E and F components           
                         are separated by ~34'.                                                          
10113-1949   GWP1309     ABL 302.                                                                Tob2012b
10114+4927   ENG  42     AB: Proper motion of A -1353 -501. Slightly variable.                           
                         Proper motion of B -008-012.                                                    
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             BUP 130     BC: C is BD+50@1723. Proper motion of C is +013-021.                            
10114-0642   GWP1310     ABL 300.                                                                Tob2012b
10114-7428   TOK 132     HIP 49913.                                                              Tok2011a
10116+1321   HU  874     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.39 +/- 0.53, 2.82, and 1.17 Msun, respectively.             Mlk2012 
                         Ma,Mb = 1.682 +/- 0.042, 1.381 +/- 0.032 \msun.                         GmJ2022 
10116-0447   GWP1311     ABL 299.                                                                Tob2012b
10120+2007   HJ  476     STT 212.                                                                        
10120-0612   HO   44     Motion in a highly-inclined orbit.                                              
10120-2836   B   194     Although Hartkopf et al. (1993) predicted a time of periastron          Hrt1993 
                         around 1989.3, we find the time of periastron to be 2006.2. The                 
                         discrepancy may be explained by three measures not published at the             
                         time of the 1993 paper.                                                 USN2002 
                         1990.3407: Periastron passage apparently occurred about the time of or          
                         shortly before our first speckle observation in 1989.3.                 McA1990 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.43 +/- 0.86, 4.91, and 2.19 Msun, respectively.             Mlk2012 
10121+2118   A  2146     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 11.22 +/- 10.32, 3.02, and 1.10 Msun, respectively.           Mlk2012 
10122-4847   I  1196     Hipparcos suspected non-single.                                                 
10126-3225   LDS 297     LDS5708.                                                                        
10132-0848   LDS 296     NLTT 23709/23710. UC 1896.                                              Chm2004 
10134-1847   LDS3965     NLTT 23731/23733                                                        Chm2004 
10134-5054   HJ 4299     B is CD-50@4922.                                                                
10137-0723   TOK 133     HIP 50100. A is X-ray source 1RXS J101344.5-072301.                     Tok2011a
10140-1429   GWP1314     ABL 307.                                                                Tob2012b
10141-0401   GWP1316     ABL 304.                                                                Tob2012b
10142-0920   GWP1318     ABL 305.                                                                Tob2012b
10142-1615   GWP1317     ABL 308.                                                                Tob2012b
10142-7636   KOH  88     Due to an error in transcribing data from Kohler's paper, a measure of  Koh2001 
                         RST1521 was inadvertently attributed to this system and assigned the            
                         AB component designation, with this pair listed as the Aa,Ab pair.              
10143+2104   BWL  25     Makarov & Kaplan (2005) and Frankoswki et al. (2007 A&A 464, 377)       Mkr2005 
                         found evidence for a close astrometric companion based on differences           
                         between Hipparcos and Tycho-2 proper motions. Two epochs at Keck in             
                         Mar 2011 and Feb 2013 show substantial orbital motion. The system was           
                         unresolved by Subaru in Dec 2011, suggesting the secondary had moved            
                         too close to the primary to be resolved. System is a probable member            
                         of the Carina young moving group, with an age ~30 Myr. Primary is               
                         GJ 2079 = DK Leo.                                                       Bwl2015 
                         A is also a 73d spectroscopic binary.                                   Tok2019b
10143-5712   HLN  14     Also known as TDS7133.                                                          
10146-0147   GWP1324     ABL 303.                                                                Tob2012b
10149-0059   GWP1325     ABL 309.                                                                Tob2012b
10149-1328   GWP1327     ABL 313.                                                                Tob2012b
10151-6717   CPO  48     C is probably CPD-66@1208.                                                      
10152+0134   BAL1872     BD +02 2309a.                                                                   
10157-3317   HJ 4300     SWR  87. CPM pair                                                       Skf2004 
10157-5115   HD  89137   The classification is from Garrison et al. (1977 ApJS 35, 111).         Msn1998a
10158-0541   GWP1330     ABL 310.                                                                Tob2012b
10159-0613   GWP1332     ABL 311.                                                                Tob2012b
10160+1200   HJ  156     BC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
10160-0816   GWP1334     ABL 312.                                                                Tob2012b
10161-2837   TOK 199     This is marked as an SB2 in the GCS, while Latham (2012, private                
                         communication) derived an orbital period of 916d, now independently             
                         confirmed by our orbit.                                                 Tok2015c
10161-5954   HU 1597     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.77 +/- 0.39, 3.33, and 1.82 Msun, respectively.             Mlk2012 
10163-2859   I   851     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.34 +/- 1.03, 3.12, and 1.30 Msun, respectively.             Mlk2012 
10165-0521   WSI 115     Aka FAR  10. Primary is white dwarf WD 1013-050.                        Far2005b
             FAR  10     AC: In this previously known system, 2MASS J10162867-0520320 is a               
                         spectroscopic binary of two M dwarf components, which is in turn a              
                         visual companion at 3.2" separation from a white dwarf (WD).                    
                         Furthermore, the WD is itself a spectral binary, making the system              
                         quadruple, with a demonstrated physical companionship of all four               
                         components (Vennes et al. 1999 ApJ 523, 386). The 3.2" pairing is               
                         easily distinguished in the AstraLux image, but the spectroscopic               
                         pairs remain unresolved. Because the system must primordially have had          
                         a pre-WD primary much more massive than J10162867-0520320 (given that           
                         the main sequence lifetime of an M0 star is longer than the Hubble              
                         time), we do not count it as an M-star binary for any of our                    
                         statistical purposes. The binary is listed as having confirmed proper           
                         motion in Table 4, this is based on the result in Vennes et al. and             
                         not our comparison with the astrometric point in the literature; since          
                         no error bars are listed for that point and since we only get rather            
                         marginally significant results if we assume reasonable errors of 0.1"           
                         and 1deg, we do not draw any new conclusions on the basis of such a             
                         comparison.                                                             Jnn2012 
10166+4117   SHY 552     HIP  50325 + HIP  50327.                                                        
10167+5737   HJ 1176     AB: HJL 123.                                                            HJL1986 
10167+2325   STFA 18     zet Leo = 36 Leo = Adhafera. A spectroscopic binary.                            
                         B is BD+24@2207.                                                                
10169+2552   BUP 131     B is BD+26@2062.                                                                
10171+1309   JMS   2     2MASS J10170754+1308398 + 2MASS J10171515+1307419.                      Jms2008 
10171-4241   SWR  88     CPM pair                                                                Skf2004 
10171-6120   B  1673     Variable, V337 Car.                                                             
10172+2306   STT 523     39 Leo. Mt. Wilson spectral types are F1s and dM1.                              
10173-1140   GWP1337     ABL 314.                                                                Tob2012b
10174-5354   CVN  16     TWA 22. Chauvin et al. (2010) derive spectral types M6 +/- 1 for both   Cvn2010 
                         components. The semimajor axis was calculated from their value for a            
                         (1.77 +/- 0.04au) and distance of 17.5pc. Effective temperatures are            
                         2900 +/- 200 and 2900 +200/-100 K. The system mass is 220 +/- 21 Mjup.          
10176+2155   LDS3973     NLTT 23914/23917                                                        Chm2004 
10178+7104   STF1415     AC: HJL 124.                                                            HJL1986 
                         AB: H N 145.                                                            MEv2010 
10180+0721   FAR  11     AC: Primary is white dwarf WD 1015+076.                                 Far2005b
10182-5049   HU 1598     V340 Vel, Algol-type eclipsing binary, P = 3.55953 d.                   Zas2011 
10183-0326   RST4454     Two orbit solutions by Heintz (1997); neither clearly preferable.       Hei1997 
10183-1321   J  2900     BRT 2723.                                                                       
10183-2029   LDS3975     The star is single in the AstraLux images, but has a known wide                 
                         companion at 32" separation (WDS).                                      Jnn2012 
10185-1811   GWP1338     ABL 316.                                                                Tob2012b
10186-3546   UC 1910     CPM candidate confirmed physical by photometry (2MASS and V mags).      Tok2013c
                         Primary is X-ray source, PMS star; also SB2, P=11.410d. Not PMS, just           
                         fast rotator?                                                           Tok2014d
10187-1823   GWP1339     ABL 317.                                                                Tob2012b
10189+4403   ENG  43     B is BD+44@1975.                                                                
10190+1613   BPM 571     [PM2000]  975130 + [PM2000]  975121.                                    Gvr2010 
10191-6441   HJ 4306     1997.0902: The magnitude difference of the system is listed in the WDS          
                         as 0.1.  Our reduction does not give the same quadrant as the latest            
                         measure in the WDS.                                                     Hor1997 
10192-0502   GWP1341     ABL 318.                                                                Tob2012b
10193-0724   GWP1343     ABL 319.                                                                Tob2012b
10196+1952   Ci 20,574   = GJ 388 = AD Leo                                                               
                         Reuyl (1943) orbit rejected from Fourth Orbit Catalog                   Reu1943 
                         ("not confirmed by subsequent observations")                            Wor1983 
10196-5724   FIN 162     A is the Algol-type system HP Car.                                              
10197+1928   WNO  53     GJ 9324 + NLTT 23781. CPM pair.                                         Mkr2008 
                         B = NLTT 23781. Co-moving, not binary.                                  Tok2014d
10198-3036   RST2685     Corrected position and Durchmusterung number                            Hei1987a
10199+1217   FAR  12     Primary is white dwarf WD 1017+125.                                     Far2005b
10200+1950   STF1424     A: gam Leo = 41 Leo = Algieba                                                   
                         Star C is flare star AD Leo = BD +20 2465, 5' distant, and not          Bag1984b
                         related to the pair AB. This companion has been detected only at                
                         7500 Angstroms, and is expected to have a very low mass.                        
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         D is BD+20@2464.                                                                
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             BAG  32     Ca,Cb. 1981.2446: Flare star (M4.5Ve) known as having an unseen                 
                         companion of P ~ 27 yr (Reuyl 1943). Companion has been detected only   Reu1943 
                         at 750 nm.  The companion is expected to have a very low mass.          Bag1984b
             STF1424     AB: H 1  28.                                                            MEv2010 
10201-0327   GWP1346     ABL 320.                                                                Tob2012b
10201-6135   HOA   1     GO Car.                                                                 Plt1934 
10204+6808   HJ 3324     Same as STF1418.                                                                
10205+0626   STF1426     AB,C: H 2  43.                                                          MEv2010 
                         AB,C: Also known as SCA 185.                                            Sca2018b
10206-1128   GWP1349     ABL 321.                                                                Tob2012b
10206-7109   GLI 293     Also known as HDS1486. #144 in the original list of Gilliss.                    
10208-6732   HJ 4314     B is CPD-66@1232, spectrum B9/A0IV/V.                                           
10209-0641   OSO  32     G055-014. Neither is a common proper motion pair, based on astrometry           
                         and color                                                               Oso2004 
10209-1911   GWP1350     ABL 322.                                                                Tob2012b
10209-5603   RMK  13     A has a variable spectrum.                                                      
10210-2844   RSS 233     HIP 50681. No V-band photometry in the WDS.                             Tok2011a
10212-0304   BUG  10     SDSS J102109.69-030420.1                                                        
                         Estimated spectral types are T1 + T5, effective temperatures 1260 +/-           
                         210 and 1130 +/- 190 K.  Masses are estimated at 0.025-0.076 and                
                         0.021-0.074 Msun, and the orbital period (assuming the semi-major axis          
                         = 1.26 * rho) is ~50yr.                                                 Bug2006a
10213+7846   RAS  24     Peculiar SrCuEu star DI Dra.                                            Ras2014 
10215+7647   LDS1711     NLTT 24011/23991                                                        Chm2004 
10215-1621   LDS3984     NLTT 24117/24116                                                        Chm2004 
10215-2948   BRT2978     A likely plate flaw.                                                    Grv2021b
10217-0946   BU   25     A=SB1. CfA: prelim. orb. P=3056d=8.37y?                                 Tok2014d
                         Inner pair unresolved thusfar. Elements driven by spectroscopic orbit.  Tok2020i
10217-6920   RSS  13     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
10218+3555   LDS1240     NLTT 24113/24114                                                        Chm2004 
10218-0023   GWP1352     ABL 323.                                                                Tob2012b
10218-4430   LDS6232     B is CD-43@6191.                                                                
10219+3704   BFR   5     LSPM J1021+3704 + 2MASS J10215386+3704166. Baron et al. (2015)                  
                         estimate spectral types M4.0 +/- 0.5 and L0 +/- 1, distances                    
                         88 +39/-25 and 93 +13/-36 pc, masses 0.207-0.272 and 0.071-0.076 Msun.  BFr2015 
10221+1226   BU 1321     HU 876.                                                                         
10222+4114   WIL   2     Using data from 2MASS, Wilson et al. (2001) conclude AB is probably a   Wil2001 
             MUG   7     physical pair, based on proximity and magnitude (time baseline is               
                         insufficient to confirm). They derive spectral type of L0V and mass             
                         77-80 Mjup for the B component. Mugrauer et al. (2004) conclude that    Mug2004c
                         components C,D,E,F,G (their stars 1-5) are background stars, with E,            
                         F, and G (stars 3,4,5) showing a constant separation. The B component           
                         (star 6) shows common proper motion with planet host star HD 89744,             
                         confirming the Wilson et al. discovery.  The mass of B is estimated at          
                         about 0.074-0.080 Msun, making it either a heavy brown dwarf or very            
                         low-mass stellar companion. Additional information was compiled from            
                         the 2MASS catalog to supplement that in these two papers.                       
             GJ 9326     Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from Korzennik    CPS2000a
                         et al. (2000).                                                          HaI2001 
             WIL   2     No comoving objects found within separation/magnitude range listed.             
                         However, Chauvin et al. (2006) note finding at least one faint          Cvn2006 
                         background object.                                                              
                         AB: Primary is exoplanet host, P=256d. Chauvin et al. (2006) detect     Cvn2006 
                         only optical companions at VLT with coronagraphic mask. Roell et al.            
                         (2012 A&A 542, A92) list the companion B at 62" as physical.            Tok2014d
                         CHARA Array Limb-darkened diameter of A :                               CIA2018b
                         Age = 3.8 +/- 0.9 Gyr,   R = 0.556 +/- 0.032 mas,                               
                         R =  2.36   +/- 0.032  \rsun, L =  6.153   +/- 0.332  \lsun,                    
                         Teff = 5927 +/- 185 K, M = 1.37 +/- 0.10 \msun.                                 
             RBR  17     2002.0166: PA is measured in zenith mode. If data collected in                  
                         equatorial mode, PA =  53.6. Confirmation of the pair should establish          
                         the correct theta value.                                                Rbr2011d
10223+4130   mu UMa      Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Jackson et al. (1957).                                                  JES1957 
10223-1032   BD-09 3055  SB1. Curvature seen in proper motion components from Hipparcos data,            
                         although period was unknown. Combined spectroscopic/astrometric                 
                         solution, based on echelle spectra and Hipparcos intermediate                   
                         data (abscissa residuals).  Torres derives a parallax of 19.5 +/-       Trr2006a
                         1.8 mas (compared to Hipparcos value of 29.4 +/- 2.7 mas). An                   
                         estimated primary mass of 0.73 +/- 0.05 Msunyield a mass of 0.88 +/-            
                         0.05 Msun for the secondary.                                                    
             TOK 398     HIP 50796 is a single-lined and astrometric binary according to                 
                         (Torres 2006), with period 570.98d (1.56yr), K1=20.76 km/s, e=0.611.    Trr2006a
                         The Hipparcos parallax corrected for binary motion is 20.6+/-1.9mas.            
                         The spectroscopic secondary companion is over-massive, most likely a            
                         close pair of M-dwarfs. If so, the new speckle companion at 1".66 with          
                         a period on the order of 500yr makes the system quadruple. The speckle          
                         companion might contribute to the IR excess found by Torres. The                
                         system is an X-ray source, and is possibly young.                       Tok2015c
10223-5945   HD  90087   LS 1518.                                                                        
                         The classification is from Garrison et al. (1977 ApJS 35, 111).         Msn1998a
10224+1209   GIC  92     G043-045/G043-043.                                                              
                         NLTT 24159/24144                                                        Chm2004 
10224-2933   GC 14246    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
10227+1521   STT 216     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
10228-1427   GWP1355     ABL 326.                                                                Tob2012b
10231-1525   GWP1356     ABL 327.                                                                Tob2012b
10232+0542   SHJ 115     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         H 5  64.                                                                MEv2010 
             TOK 200     The 1".1 speckle companion can explain dmu, but not the acceleration.   Tok2012a
10233-0203   GWP1357     ABL 324.                                                                Tob2012b
10233-1603   GWP1358     ABL 328.                                                                Tob2012b
10236-1721   GWP1359     ABL 329.                                                                Tob2012b
10236-4408   HJ 4315     B is CD-43@6220.                                                                
10237+0237   LAM   7     AB: B is BD+03@2357.                                                            
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
10237-0221   GWP1360     ABL 325.                                                                Tob2012b
10238+1239   BPM 572     [PM2000]  977607 + [PM2000]  977554.                                    Gvr2010 
10238-4415   I   208     AB. 1997.1230: A smaller annulus was used in the power spectrum fit             
                         due to the faintness of the source. As a consequence, the separation            
                         and position angle uncertainties may be larger than other measures.     Hor1997 
10239-1934   GWP1361     ABL 330.                                                                Tob2012b
10241+6534   CIA  31     ET UMa.                                                                         
                         Ma,Mb = 2.779 +/- 0.153, 1.708 +/- 0.094 \msun.                                 
                         Ra,Rb = 3.16 +/- 0.11, 1.73 +/- 0.06 \rsun.                                     
                         Teff_a,Teff_b = 10260 +/- 100, 7860 +/- 140 K.                                  
                         La,Lb = 101.0 +/- 8.0, 9.7 +/- 1.0 \lsun. distance = 101.1 +/- 2.0 pc.  CIA2022e
10244+3411   STTA104     B is BD+34@2122.                                                                
                         The primary is a semi-regular variable.                                         
10245+4008   ES 1542     BRT 106                                                                         
10246+0305   CHE 147     SLE 586.                                                                        
10246-1906   HS Hya      Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Torres et al. (1997). They derived component masses 1.39 and 0.61 Msun  Trr1997b
                         and an estimated semimajor axis of 8.48 mas.                            Ren2013 
10247-0612   GWP1362     ABL 332.                                                                Tob2012b
10247-1127   GWP1363     ABL 333.                                                                Tob2012b
10249-3818   GLI 294     Also known as RSS 236 and WFC 104. #145 in the original list of Gilliss.        
10250+2437   STF1429     A premature orbit has been computed.                                            
10251-0059   GWP1364     ABL 331.                                                                Tob2012b
10253-1250   GWP1366     ABL 334.                                                                Tob2012b
10254+1603   BPM 573     [PM2000]  978410 + [PM2000]  978438.                                    Gvr2010 
10254-1034   GWP1370     ABL 336.                                                                Tob2012b
10254-1826   GWP1369     ABL 338.                                                                Tob2012b
10256+0847   STF1431     H 1  29.                                                                MEv2010 
10257-0704   SCA  53     Spectrum: K5:IIIbFe-0.5.                                                        
10258+0312   HJ 1177     BAL 2373.                                                                       
10258-4757   SWR  91     CPM pair                                                                Skf2004 
10260+5237   STF1428     BDS 5386, H I 71 probably same star.                                            
                         H 1  71.                                                                MEv2010 
10262+0356   BU 1280     A is a Delta Scuti-type variable, RX Sex.                                       
10263-5353   HJ 4319     Spectrum M2IabCN0.5, variable in light. B has a B-V color of 0.25;              
                         U-B = -0.67 (Humphreys et al., ApJ 172, 75, 1972)                               
10264+6246   LDS2583     SLW 472.                                                                        
10264+1438   BPM 574     [PM2000]  978935 + [PM2000]  978948.                                    Gvr2010 
10264-0658   GWP1371     ABL 335.                                                                Tob2012b
10266-1728   GWP1373     ABL 337.                                                                Tob2012b
10269+1931   COU 292     1983.9557, 1983.9667: Measurements should be given low confidence.      Bag1985 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.26 +/- 1.05, 2.44, and 1.10 Msun, respectively.             Mlk2012 
10269+1713   STT 217     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.38 +/- 1.55, 2.70, and 1.17 Msun, respectively.             Mlk2012 
10269-0703   GWP1374     ABL 339.                                                                Tob2012b
10270+2638   HIP  51157  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Griffin (1987). They derived component masses 0.86 and 0.30 Msun and    Grf1987b
                         an estimated semimajor axis of 76.15 mas.                               Ren2013 
10271-1756   GWP1375     ABL 340.                                                                Tob2012b
10271-6200   TDS7279     AB,C: SHY 555. Bayesian analysis by Shaya & Olling (2011) indicates     Shy2011 
                         very high (near 100%) probability pair is physical.                             
10276+0946   HJ  832     45 Leo. A is an Alpha CVn-type variable, CX Leo, and an SB.                     
10277-0108   LDS3990     NLTT 24410/24411                                                        Chm2004 
10279+3642   HU  879     bet LMi = 31 LMi. G8III-IV.                                                     
                         Combined visual-spectroscopic orbits by Heintz (1981,1982). Visual      Hei1981f
                         observations cover only a narrow apastron arc.                          Hei1982e
                         Only elements P and T have been amended by Starikova (1977) from the    Sta1977a
                         orbit of Baize (1950).                                                  Baz1950b
                         Gontcharov & Kiyaeva (2002) photocentric (astrometric) orbit is based   Gon2002a
                         on a combination of ground-based catalogs with Hipparcos.                       
                         This object was misidentified as HO 879 in McAlister & Hendry (1982).   McA1982d
                         Malkov et al. (2012) derive dynamical and spectroscopic masses                  
                         3.37 +/- 0.94 and 2.63 Msun, respectively.                              Mlk2012 
                         Combined solution leads to masses of 2.98 +/- 0.10 and 1.92 +/- 0.04    WaX2020 
                         \msun for A and B, respectively. Orbital parallax of 19.6 +/- 0.2 mas           
                         leads to luminosities of 50.7 +/- 1.8 and 9.1 +/- 4.1 \lsun for A and           
                         B, respectively.                                                                
10280+1950   STF1435     HJL 125.                                                                HJL1986 
10282-2548   FIN 308     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.71 +/- 0.53, 2.23, and 0.98 Msun, respectively.  Mlk2012 
                         AB: Omega for Tokovinin et al. (2015) orbit flipped by 180deg, at               
                         request of author.                                                      Tok2015c
10283-0436   GWP1378     ABL 341.                                                                Tob2012b
10284-1517   GWP1380     ABL 343.                                                                Tob2012b
10286-1437   GWP1382     ABL 342.                                                                Tob2012b
10287+4558   A  1993     Derived orbital parallax 0".01274, mass sum 2.01 +/- 0.87 Msun          Lin2004a
10288+6300   OSO  33     G236-030. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
10288-6235   DUN  85     B is CPD-61@1676.                                                               
                         Additional notes may be found in Dunlop (1829).                         Dun1829 
10289+3453   SHY 215     HIP  51312 + HIP  52140.                                                        
10289-0300   FIL  25     BAL 211.                                                                        
10290-1952   GWP1385     ABL 344.                                                                Tob2012b
10292-5737   KRV  30     Classical Cepheid UX Car.                                                       
10294+1211   HDS1507     Cvetkovic et al. (2016) estimate spectral types F0 and F7, masses 1.66          
                         and 1.30 Msun. Dynamical parallax is 10.81 +/- 0.15 mas.                Cve2016b
10294+0346   SLE 494     Error in Soulie (1986) measure apparently due to typo in right                  
                         ascension of primary.                                                   Sle1986a
10294-5034   B  1681     V349 Vel, Algol-type eclipsing binary, P = 3.02447 d.                   Zas2011 
10296+3757   HJ 2532     ALI 848.                                                                        
                         AB: HJL 126.                                                            HJL1986 
10296-3036   H N  50     del Ant                                                                         
10297+8415   GC 14305    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
10297-1327   GWP1387     ABL 347.                                                                Tob2012b
10299+2835   STTA105     B is BD+29@2056.                                                                
10299-0435   GWP1388     ABL 345.                                                                Tob2012b
10300-0413   LDS3994     NLTT 24512/24515                                                        Chm2004 
10301-4721   HJ 4324     SWR  92.                                                                Skf2004 
10302+5100   STT 219     BDS 5471, HJ 2535 probably same star. The Hipparcos secondary                   
                         magnitude of 7.70 is very different than the visual mean of 11.2.               
10303-0818   GWP1389     ABL 346.                                                                Tob2012b
10306+5559   LDS2863     A: 36 UMa                                                                       
                         B: BD+56@1458.                                                                  
                         Components of these systems (AB and AC) all have common proper          Egg1950 
                         motion and common radial velocity.  Vyssotsky & Reuyl also claim that   Vys1942 
                         this system shares a common proper motion with BD+57 1266, an 8th               
                         magnitude star 4041" from A.                                                    
                         CHARA Array Limb-darkened diameter  0.794 +/- 0.014 mas,                CIA2012e
                         R =  1.091 +/- 0.020 \rsun, L =  1.605 +/-0.042 \lsun,                          
                         Teff = 6233 +/-  68 K, M = 1.119 +/- 0.035 \msun,                               
                         Age =  1.5 +/- 1.4 Gyr.                                                         
                         AB: HJL 127.                                                            HJL1986 
                         AB: Raghavan et al. (2010) consider B component possible binary (RV     Rag2010 
                         variable)                                                               Tok2014d
10307-5429   HJ 4327     B is CPD-53@3900.                                                               
10307-6121   DUN  87     B is CPD-60@1944.                                                               
10310-0232   GWP1390     ABL 348.                                                                Tob2012b
10310-0738   STF1441     A is a spectroscopic binary. C is BD-06@3171.                                   
10313-5153   HJ 4328     B is CD-51@4816.                                                                
10314-5343   HJ 4329     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
             LUH   9     AC: GJ 9332 + 2MASS J10313234-5338010.                                          
10315-0605   GWP1391     ABL 350.                                                                Tob2012b
10316+4316   SHY 557     HIP  51536 + HIP  51726.                                                        
10316-0253   GWP1392     ABL 349.                                                                Tob2012b
10316-3956   HJ 4326     B is CD-39@6453.                                                                
10317-4429   B  1161     Measures uncertain, too close. Needs speckle.                                   
10318-6356   HD  91452   The classification is from the LSC; however, Garrison et al. (1977              
                         ApJS 35, 111) assign a type B0 Ia.                                      Msn1998a
10319+3223   HJ  482     33 LMi.                                                                         
10319-8155   HJ 5444     B is CPD-81@448.                                                                
10320+3355   LDS1244     Discrepant Luyten measure appears to be due to a 1' error in dec of     Luy1969 
                         his secondary.                                                                  
10320+2202   STF1442     STT 221.                                                                        
10320-2021   B  2248     J 2655. BHA 13.                                                                 
10320-4504   PZ    3     B is CD-44@6582.                                                                
10320-6019   JSP 906     Aka DAM 529.                                                            Skf2018e
10321+3240   SKF 317     SLW 487.                                                                        
10321-7005   HJ 4335     A 2.2d spectroscopic solution for the A component has been found        Tok2019g
                         making this a triple system.                                                    
10323-1827   GWP1395     ABL 352.                                                                Tob2012b
10325-7226   RSS  14     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
                         SHY 558. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
10328+0918   WRH  19     rho Leo = 47 Leo. Possible spectroscopic binary.                                
                         Additional notes may be found in Wilson (1941).                         WRH1941b
                         A is a blue supergiant with multiple pulsation periods.                 IAU2014e
10329-4700   HJ 4330     AB: B is CD-46@6207.                                                            
             YSJ   1     Aa,Ab: 1995.1025: WDS Catalog lists a companion at 40".3 and position           
                         angle 163deg. The component listed here appears to be a new discovery.          
                         Our two observations of this object were forty minutes apart on                 
                         February 7, 1995 (UT).                                                  Dns1997 
                         1997.1176  This is the first measure of this system since the                   
                         discovery measures in 1995 of Dinescu et al. (1997) The difference in   Dns1997 
                         position angle from their last measure is 2.2 deg and the difference            
                         in separation is 0".020.                                                Hor1997 
10330+3033   LDS1246     NLTT 24638/24639                                                        Chm2004 
10332+4026   HJ 2534     A is a spectroscopic binary.                                                    
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
10332-5830   EVS  16     Primary is the Cepheid Y Car.                                           Evs2016a
10334+3410   LDS 916     NLTT 24653/24654                                                        Chm2004 
10335-4659   HJ 4332     B is CD-46@6218.                                                                
10336+1351   BPM 575     [PM2000]  982666 + [PM2000]  982677.                                    Gvr2010 
10339-1750   S   610     B is BD-17@3179.                                                                
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
10340+1631   BPM 576     [PM2000]  982873 + [PM2000]  982856.                                    Gvr2010 
10340-0423   GWP1397     ABL 353.                                                                Tob2012b
10340-2345   BU 1269     44 Hya.                                                                         
10341+1251   BPM 577     [PM2000]  982909 + [PM2000]  982959.                                    Gvr2010 
10343-1732   GWP1400     ABL 355.                                                                Tob2012b
10344+4041   LDS3998     SLW 495.                                                                        
10345-0641   GWP1401     ABL 354.                                                                Tob2012b
10347-3524   HJ 4334     SWR  94. CPM pair                                                       Skf2004 
10349-0820   GWP1403     ABL 359.                                                                Tob2012b
10350+0839   STF1450     49 Leo. A is the Algol-type system TX Leo.                                      
                         Individual J,H,K magnitudes are calculated from 2MASS combined                  
                         magnitudes and AO-derived magnitude differences                         Rbr2005 
10351-5741   COO 107     Spectrum of B is A.                                                             
10352-4545   SWR  95     CPM pair                                                                Skf2004 
10352-4755   SWR  96     CPM pair                                                                Skf2004 
10353+4321   LDS4001     SLW 497.                                                                        
10354+2616   STF1451     LDS1249.                                                                        
                         AB: NLTT 24760/24757                                                    Chm2004 
10355-0234   GWP1404     ABL 356.                                                                Tob2012b
10356-0415   GWP1406     ABL 357.                                                                Tob2012b
10356-0508   GWP1405     ABL 358.                                                                Tob2012b
10359+6336   STF1444     Primary is GT UMa, an Algol-type eclipsing binary, P = 1.16471d.        Zas2012 
10360+0118   GRV1044     SLW 499.                                                                        
10361+1137   BIG   1     B is BD+12@2234.                                                                
10361-2641   BU  411     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.69 +/- 0.48, 2.42, and 1.17 Msun, respectively.             Mlk2012 
10363-1213   GWP1409     ABL 360.                                                                Tob2012b
10363-1621   BU 1075     phi 2 Hya                                                                       
10363-6101   KRV  31     Classical Cepheid UV Car.                                                       
10364-1223   GWP1410     ABL 361.                                                                Tob2012b
10365-1214   EHR  13     AB: Companion appears to be a background star.                          Ehr2010 
             KUI  51     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: Rectilinear solution by Friedman et al. (2011).                     USN2011a
10366+7849   HJ 5480     Discrepant observation by Pettit originally catalogued at PTT  26,      Ptt1917 
                         although he said it was of HJ 5480.                                             
10366-1246   GWP1411     ABL 362.                                                                Tob2012b
10366-2846   I   857     Rectilinear solution by Zirm (2013).                                    Zir2013d
10366-6448   CTI 389     V546 Car.                                                                       
10367+1522   DAE   3     RBS 887                                                                         
                         Daemgen et al. (2007) derive distance of 19.6 +/- 4.6 pc, separations           
                         of 20.8 +/- 6.0 au (AB) and 3.7 +/- 1.1 au (BC), and predicted orbital          
                         periods of 157 +97/-93 yr (AB) and 16 +10/-9 yr (BC). Spectral types            
                         for the three components are M3.5 +/- 0.5, M4.5 +/- 0.5, and M4.5 +/-           
                         0.5; masses 0.29 +0.11/-0.08, 0.16 +0.05/-0.04, 0.16 +0.05/-0.0 Msun.   Dae2007 
                         2MASS J10364483+1521394 is a triple in the Ursa Major moving group,             
                         consisting of a low-mass M dwarf orbited by 2 less-massive companions.          
                         Calissendorff et al. (2017) derive orbits for the BC pair, as well as           
                         A,BC. The semimajor axis for BC is 161 +/- 2 AU; combined mass for the          
                         pair is 0.482 +/- 0.145 Msun. If the BC dynamical mass is constrained           
                         to this value, an orbital solution for A,BC yields a semimajor axis of          
                         38 +/- 4A U and a system mass of 1.00 +/- 0.03 Msun for the triple.             
                         The mass of A is 0.53 +/- 0.20 Msun, while B and C have similar masses          
                         of 0.24 +/- 0.07 Msun each.                                             Jnn2017b
10370-0850   TOK  44     Aa,Ab: Tokovinin et al. (2015) derive spectral types G0V and K5V for            
                         the Aa and Ab components; masses are 1.46 and 0.64 Msun. Aa is a 170d           
                         SB; Aa2 is possibly of type M3V.                                        Tok2015b
                         Aa,Ab: SB, P=7.603y.                                                    Tok2014d
             A   556     AB: Tokovinin et al. (2015) derives a spectral type K5V for the B               
                         component; mass is 0.64 Msun. Dynamical parallax is 27.4 +/- 0.6 mas.   Tok2015b
10370-1538   BRT 578     A likely plate flaw.                                                    Grv2021b
10372+8603   STF1410     AB: STT 214.                                                                    
10373-4814   SEE 119     One component is SB, P = 10.21 d. (#623 in Batten et al., 1989).        Bte1989 
                         According to Evans (1969), this is the primary. Identification of       Evn1969 
                         the ascending node is based on this assumption.                                 
                         The period adopted for the visual orbit utilizes RV and                 Fin1968b
                         interferometric observations.                                                   
                         See also Evans (1969) for residuals, ephemeris,and full discussion of   Evn1969 
                         this interesting system.                                                Fin1970b
10373-5826   JSP 408     TDS7378.                                                                        
10374+3133   LDS1251     NLTT 24861/24863                                                        Chm2004 
10374-5837   SNA  10     Aa,Ab: It is uncertain whether the 33mas companion corresponds to the           
                         SB reported by Sota et al. (2014, ApJS 211, 10). If it does, the                
                         orbital period is at least 5 years.                                     Sna2014 
             HJ 4338     Herschel says "A very neat double star involved in a nebula." There is          
                         perhaps a nebulouse patch running N and S, 5' x 1', but there is no             
                         nebula surrounding this pair as suggested by h. Many small stars near.  I__1916a
                         But what John Herschel was describing was the large (15' diam) object           
                         NGC 3324; Herschel used the pair as the reference position for the              
                         nebula. Innes was probably viewing at quite high magnification to               
                         measure the double, and so missed the nebula. The pair is in fact the           
                         principle source of fluorescing uv photons for the nebula!              Skf2014 
10375+3015   HJ  487     Aka SKF1845.                                                                    
10376+3001   LDS1253     NLTT 24873/24875                                                        Chm2004 
10376-4556   CPO 296     CPD-45@4802.                                                                    
10376-5744   JSP 410     TDS7381.                                                                        
10377-7335   HJ 4344     Algol-type eclipsing binary, P = 2.45763 d.                             Zas2011 
                         B is CPD-72@998.                                                                
                         SWR  97. CPM pair                                                       Skf2004 
10379+3405   36 LMi      SB1. Combined orbit including RV data and Hipparcos Intermediate                
                         Astrometric data. Semimajor axis derived from photocentric a0 plus              
                         stellar evolutionary model. Derived properties for A and B:                     
                         M/Msun = 4.94 + 1.42, L/Lsun = 1296.36 + 5.89, dm = 5.86 mag,                   
                         log age = 8.10.                                                         WaX2015b
10381+4026   STT 223     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
10382-0620   GWP1414     ABL 363.                                                                Tob2012b
10382-0629   GWP1415     ABL 364.                                                                Tob2012b
10383+6007   STT 222     Primary is 2.8d SB1; AB is physical pair, estimated period 3600y.       Tok2006 
10385-1559   GWP1416     ABL 365.                                                                Tob2012b
10386-1653   phi 3 Hya   Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Christie (1936).                                                        Crs1936 
10386-4558   B  2715     CPD-45@4816.                                                                    
10389+0721   J    79     Aitken incorrect; pair is BD+08 2387, not +08 2388.                     J__1949a
10390-0440   GWP1421     ABL 366.                                                                Tob2012b
10390-5849   GLI 152     B is CPD-58@2475.                                                               
10391+0726   J  1351     BRT 2603.                                                                       
                         J  2656.                                                                J__1962a
10392-2551   TOK 135     HIP 52145. A is SB without orbit, dRV= 1.2.                             Nrd2004 
                         A new triple. There is also a bright companion C in the field.          Tok2011a
10395+3142   STF1458     HJL 128.                                                                HJL1986 
                         SEI 521.                                                                Nsn2017b
10397+0851   STT 224     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.81 +/- 0.74, 2.61, and 1.20 Msun, respectively.  Mlk2012 
10398+4209   OSO  34     G146-056. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
10401+1914   STT 225     AC: HJL 129.                                                            HJL1986 
10402-1622   LDS 311     B is BD-15@3101.                                                                
                         NLTT 25010/25005                                                        Chm2004 
10406-1523   GWP1430     ABL 369.                                                                Tob2012b
10406-5933   COO 110     B is CPD-58@2523.                                                               
10409-3545   B  2001     Spectrum composite; G8-K0III+F-G.                                               
10410-1225   GWP1432     ABL 368.                                                                Tob2012b
10412-0811   GWP1433     ABL 367.                                                                Tob2012b
10412-4403   DON 429     TDS7414.                                                                        
10420+6506   GRV1046     SLW 510.                                                                        
10422+3142   BLL  28     A is the semiregular variable RX LMi.                                           
10422-0357   GWP1435     ABL 371.                                                                Tob2012b
10423-1043   GWP1436     ABL 373.                                                                Tob2012b
10424-0114   GWP1437     ABL 370.                                                                Tob2012b
10424-6110   KRV  33     Classical Cepheid EY Car.                                                       
10425-0358   GWP1438     ABL 372.                                                                Tob2012b
10425-3340   NHR   1     The source at 2.4" separation, first reported in Neuhauser et al.       Nhr2000 
                         (2000), is an already known background star (Lowrance et al. 2005), a   Lwr2005 
                         conclusion which we can confirm at ~28 sigma confidence.                Jnn2012 
10425-6158   HZG9001     FV Car.                                                                 Plt1934 
10426+0335   A  2768     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         This object was misidentified as ADS 7986 in McAlister & Hendry (1982)  McA1982d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.37 +/- 1.09, 2.80, and 1.13 Msun, respectively.             Mlk2012 
10426-1555   GWP1439     ABL 374.                                                                Tob2012b
10427-1826   GWP1440     ABL 377.                                                                Tob2012b
10428-0211   GC 14729    Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from the Geneva           
                         Extrasolar Planet Search Programs home page.                            HaI2001 
10430+2620   BU  913     40 LMi.                                                                         
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
10430-6424   the Car     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
10432+2652   LDS1256     May be the same as the other lost pair 10451+2651 = LDS5717. When one           
                         is found they should be merged.                                                 
10432+0440   A  2769     This pair is the C component of 10433+0445.                                     
10432-1542   GWP1441     ABL 376.                                                                Tob2012b
10432-6110   SIN  55     BD: initially listed incorrectly as AD.                                         
10433+0445   STF1466     35 Sex. A is a spectroscopic binary.                                            
                         Spectrum composite; K3III+K0III.                                                
                         AB: H N  36.                                                            MEv2010 
10434-0352   J    89     Also appears to be the long lost pair HLD  11 = BDS 5534.               Dam2014 
10434-1706   BFR   6     2MASS J10432398-1706024 + 2MASS J10432513-1706065. Baron et al. (2015)          
                         estimate spectral types M4.0 +/- 0.5 and M9.0 +/- 0.5, distances                
                         42 +26/-16 and 75 +6/-23 pc, masses 0.207-0.272 and 0.079-0.085 Msun.   BFr2015 
10435+4612   SMA  75     B is BD+46@1658. B is a spectroscopic binary.                                   
                         AB: NLTT 25147/25160                                                    Chm2004 
                         AB: HJL 130.                                                            HJL1986 
                         AB: SHY 216. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
             MET   7     BE and BF: Primary of 10440+4612 MET   7AB and AC same as B component           
                         of 10435+4612 SMA  75AB; systems merged.                                        
                         Based on proximity, Metchev & Hillenbrand (2004) say the BE pair is     Met2004b
                         probably physical.                                                              
10435-1852   GWP1442     ABL 378.                                                                Tob2012b
10438-0039   GWP1444     ABL 375.                                                                Tob2012b
10438-5933   CP-58 2611  Trumpler 14 FMM 20. This object is designated as Trumpler 14 20 in the          
                         list of Feinstein et al. (1973 A&AS 12, 331)  and as FMM 20 in Penny    Pny1993 
                         et al. (1993).                                                          Msn1998a
10438-5957   HJ 4355     B is CPD-59@2547.                                                               
10440-5932   CP-58 2620  Trumpler 14 FMM 8.  This object is designated as Trumpler 14 8 in the           
                         list of Feinstein et al. (1973 A&AS 12, 331) and as FMM 8 in Penny et   Pny1993 
                         al. (1993).                                                             Msn1998a
10440-5933   NEL   1     See discussion of the system by Sana et al. 2014).                      Sna2014 
             HJ 4356     Both A and B components were observed with the speckle camera and       Pny1993 
                         appeared to be single (Penny et al. 1993).                              Msn1998a
10440-5952   HJ 4357     V661 Car, Algol-type eclipsing binary, P = 23.944 d.                    Zas2011 
             SNA  13     Aa,Ab: Primary is V661 Car, a detached Algol-type eclipsing binary.             
                         The 20mas pair probably does not correspond to the 23.9d eclipsing              
                         binary (Otero 2006, Open European Journal on Variable Stars 45, 1),             
                         given the ~2.6kpc distance to the Cr228/Tr16 complex.                   Sna2014 
10441-1536   GWP1445     ABL 382.                                                                Tob2012b
10441-4005   HJ 4349     SWR  98. CPM pair                                                       Skf2004 
10441-5935   HJ 4360     Trumpler 16 MJ 238. Both A and B components were observed with the              
                         speckle camera and appeared to be single. Levato et al. (1991) derive   Lev1991a
                         a single-lined spectroscopic orbit for HD 93161 but they                        
                         do not indicate which component is the binary.  Howarth et al. (1997            
                         MNRAS 284, 265) and Penny (1996) found large radial velocity changes    Pny1996b
                         in closely spaced IUE spectra, and Howarth et al. argue that both               
                         components are short-period binaries.                                   Msn1998a
                         A comp is SB, types O8V and O9V, period 8.566 +- 0.004d. Spectral type          
                         of B component is O6.5V(f) and presents radial velocity variations.     Naz2005 
                         The position angle has been flipped about the E/W axis for the HST      Nel2004 
                         observation.                                                                    
                         The B component is noted as SB1 by Chini et al. (2012). Both A and B    Cii2012 
                         are bright enough for an interferometric analysis of the SAM data, but          
                         no companion was found.                                                 Sna2014 
             SNA  14     Ca,Cb: The C component was reported as SB1 by Chini et al. (2012).      Cii2012 
                         Further observations are desirable to confirm the reality of the tight          
                         Ca/Cb/Cc triple.                                                        Sna2014 
                         This star (component C of HD 93161) was observed with the speckle               
                         camera and appeared to be single.                                       Msn1998a
10442+6111   LDS2320     Pair at precise coordinates matches Luyten's rho/theta, as well as his  Luy1970 
                         BD+61 1312 cross reference, but apparently there was a typographical            
                         error of 2h in his published coordinates.                                       
10442+2927   SLW 515     CVR 572.                                                                        
10442-0732   GWP1446     ABL 380.                                                                Tob2012b
10442-3931   SWR  99     CPM pair                                                                Skf2004 
10443-1227   GWP1447     ABL 381.                                                                Tob2012b
10443-4515   CPO 301     B is CD-44@6765.                                                                
10443-7052   DUN  99     B is CPD-70@1185, spectrum A6IV.                                                
             CHR 227     Ba. Worley (private communication) noted that the systematic binary             
                         star surveys of Rossiter (1955) and van den Bos missed the              Rst1955 
                         declination band -73 to -70 deg. This probably explains why this                
                         half-arcsecond pair remained undiscovered until now.  CHR 227                   
                         represents a new component to the wide (63") common proper motion pair          
                         HR 4211-12 = DUN 99 AB, discovered by J. Dunlap in 1826 (1829) and      Dun1829 
                         last observed nearly 80 years ago (Dawson 1918). A 10th magnitude C     Daw1918a
                         component also lies some 35" from A, discovered by John Herschel in     HJ_1847a
                         1835, but no closer components are known.                               Hrt1996b
10444-6000   DAW   8     Often classified O9 or 9.5. QZ Car. The bright star consists of two             
             HDS1534     eclipsing pairs, P = 20.73d and 6.00d.                                          
                         The classifications are from Morrison & Conti (1980), who describe      Cti1980 
                         this quadruple that consists of a pair of SB1 systems (the shorter              
                         period system is also eclipsing).  Their expressed hope that speckle            
                         interferometry might resolve the pair was not realized in our work,             
                         but the object remains an important target for high resolution work.    Msn1998a
             SNA  15     The primary is QZ Car, a semi-detached beta Lyr type eclipsing binary.          
                         A complex multiple system, with three visual companions. The central            
                         object is itself a quadruple, composed of a pair of SBs, Aa1,Aa2                
                         (O9.7I+B2V, P=20.7d) and Aa3,Aa4 (O8III+O9V, P=60d and eclipsing).      Sna2014 
10445-5734   HDS1535     Classical Cepheid VY Car.                                                       
10445-5944   SEE 513     Noted by See but never added to WDS, this pair was confirmed by USNO    See1897l
                         UCAC1 astrometry. Discoverer designation and data added 12/09/2002.             
10446-5944   BSO   4     A is a spectroscopic binary. B is CPD-59@2584.                                  
                         Primary is V560 Car, an ellipsoidal variable star and eclipsing SB2.    Sna2014 
10446-5945   HD  93205   Trumpler 16 MJ 340.  The classification is from the UV tomographic              
                         analysis of Penny (1996). The companion star, HD 93204 (BsO 4 B) was    Pny1996a
                         also observed and appeared to be single.                                Msn1998a
10447-6001   HJ 4363     B is CPD-59@2593.                                                               
10448-5934   SNA  18     A long-period binary, discussed in Sana et al. (2011). This pair is     Sna2011b
                         one of the tightest resolved binaries in our sample and a non-thermal           
                         radio emitter.                                                          Sna2014 
10449+3224   LDS1258     NLTT 25213/25215                                                        Chm2004 
10451+2651   LDS5717     May be the same as the other lost pair 10432+2652 = LDS1256. When one           
                         is found they should be merged.                                                 
10451-0207   LDS4012     NLTT 25234/25233                                                        Chm2004 
10451-0735   GWP1450     ABL 379.                                                                Tob2012b
10451-1704   GWP1451     ABL 383.                                                                Tob2012b
10451-5941   B  2256     eta Car = Trumpler 16 MJ 480, an old nova in a nebula with nuclei.              
             I  1092     B and C involved in the nebulosity.                                     B__1951a
             WGT   2     One of these three components found by Weigelt is probably B  2256;     Wgt1986a
             DUN  98     however, it is not clear which one due to the lack of a continuous              
                         series of observations and orbital motion.                                      
                         This famous luminous blue variable is not classified as an O star, but          
                         it is almost certainly a massive object. The inner structure of the             
                         ejecta of this star is described by Davidson et al (1997 AJ 113, 335).          
                         A preliminary set of orbital elements is given by Damineli et al.               
                         (1997 NewA 2, 107), who suggest a 5.5-yr orbit with a maximum angular           
                         separation of 0".004.  The central object appeared single in our                
                         observations. The H component (HDE 303308) was also observed and                
                         appeared to be single.                                                  Msn1998a
                         Powell also measured the distance to 10446-5944BSO   4 (1856.012,       Pwl1857 
                         229.57 deg, 294.77; 1860.297, 229.3 deg, 297.8"), but they are not      Pwl1864 
                         physically related so are not merged.                                           
                         Powell also measured the distance to 10441-5935HJ 4360C (1860.306,      Pwl1864 
                         312.6 deg, 571.1"), but they are not physically related so are not              
                         merged.                                                                         
10453-5945   COO 113     Primary is V731 Car, Algol-type eclipsing binary, period 2.29995d.      Zas2013 
                         B is CPD-59@2633.                                                               
10453-8028   I   294     del 1 Cha                                                                       
10454+7550   HJ 5482     BDS 5530, HJ 3329 same star.                                                    
10454+3831   CHR 191     1983.4277: The AB pair is a new component to the 0".7 pair HO 532.              
             HO  532     This new component was actually first resolved in 1983 (McAlister et            
                         al (1987), but it was believed at the time that the measurement was of  McA1987b
                         the known pair (the wide component laid outside the processor "window"          
                         of our old autocorrelator).  Reprocessing of our archival video data            
                         allowed us to resolve both components in the 1983 and 1984 data sets,           
                         although both early measurements of the AB pair are quite weak.                 
10454-4342   HJ 4362     B is CD-43@6533.                                                                
10456+6250   STI 714     Rectilinear solution by Friedman et al. (2011).                         USN2011a
10457-1907   LDS4013     NLTT 25279/25280                                                        Chm2004 
10457-5924   HD  93403   The classification is from the UV tomographic analysis of               Pny1996a
                         Penny (1996).                                                           Msn1998a
10458-5929   HJ 4369     B is CPD-58@2685. A is an irregular variable, BO Car. B has a B-V               
                         color of 0.16; U-B = -0.21 (Humphreys et al., ApJ 172, 75, 1972)                
10459+3041   S   612     42 LMi. B is BD+31@2181.                                                        
10460-1934   GWP1452     ABL 385.                                                                Tob2012b
10461-5657   HRG 133     B is CPD-56@3776.                                                               
10461-5934   HJ 4370     B is CPD-58@2689.                                                               
10463-1343   GWP1453     ABL 384.                                                                Tob2012b
10463-4128   TOK 137     HIP 52676. A is exoplanet host, P=13.2d, 46.0d                          Tok2014d
10463-6036   RST4463     A is a spectroscopic binary.                                                    
10465-6416   FIN 364     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 7.76 +/- 1.39, 5.61, and 3.71 Msun, respectively.  Mlk2012 
                         AB: Omega for Tokovinin et al. (2015) orbit flipped by 180deg, at               
                         request of author.                                                      Tok2015c
10466-5933   HJ 4371     B is CPD-58@2700.                                                               
10468-4925   R   155     mu Vel. A is a SB.                                                              
10470+1302   STF1472     STTA106.                                                                        
10470-1241   GWP1454     ABL 390.                                                                Tob2012b
10472+7250   BUP9007     NGC 3348. For the record, measures are:                                         
                         10472+7250BUP9007      1888 2000    4  74  72  13.5  13.1 11.2  13.1            
                                           -024-005 +012+005               104710.03+725022.7            
                         10472+7250 1888.38      73.6         13.5                       0.3   1 Enh1906B
                         10472+7250 1910.12      67.8         13.5                       1.0   1 Bu_1913 
                         10472+7250 1999.168     72.8         13.29                      1.3   1 Skf2014b
                         10472+7250 2000.0       71.9         13.13           609  70    0.2   1 Skf2014b
10472+4027   LDS4016     AB: NLTT 25336/25338                                                    Chm2004 
10472-6006   COO 115     B is CPD-59@2700.                                                               
10474-1804   GWP1456     ABL 391.                                                                Tob2012b
10474-6555   R   157     Aka HDS1543.                                                                    
10475-2221   SHY 218     AC: HIP  52787 + HIP  52776.                                                    
10476+2008   LDS4018     NLTT 25362/25363                                                        Chm2004 
10476-0601   GWP1457     ABL 387.                                                                Tob2012b
10476-1516   STF1474     BC: H 2  74.                                                            MEv2010 
10476-1538   STF1473     B is BD-14@3187.                                                                
                         AB: SHY 562. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
10477-0748   GWP1458     ABL 388.                                                                Tob2012b
10478-0337   GWP1459     ABL 386.                                                                Tob2012b
10481-0218   OCC1061     Sign error in published WDS designation.                                OCC2012b
10482-1702   GWP1461     ABL 397.                                                                Tob2012b
10482-3956   NHR   2     DENIS-P J104814-395606                                                          
                         Conclude secondary is background object.                                Nhr2002c
10483+1006   BPMA 41     AB: [PM2000]  990241 + [PM2000]  990072.                                Gvr2010 
             BPMA 42     BC: [PM2000]  990072 + [PM2000]  989991.                                Gvr2010 
10484+3734   HD  93521   The classification is from Hobbs et al. (1982 ApJ 263, 690). Fullerton  Ful1990 
                         (1990) and Howarth & Reid (1993 A&A 279, 148) describe the striking             
                         line profile variations in the spectra apparently due to nonradial              
                         pulsations.                                                             Msn1998a
10484-2014   LDS 315     NLTT 25404/25403                                                        Chm2004 
10485-1537   GWP1462     ABL 396.                                                                Tob2012b
10485-2223   RST2710     CPD-21@4800.                                                                    
10488-0721   GWP1464     ABL 395.                                                                Tob2012b
10489-0102   GWP1465     ABL 393.                                                                Tob2012b
10490-4348   DAW  10     AB = SWR 100. CPM pair                                                  Skf2004 
10491-0058   BVD 147     = GWP1467 = ABL 392.                                                    Tob2012b
10491-0247   GWP1466     ABL 394.                                                                Tob2012b
10492-1823   GWP1468     ABL 398.                                                                Tob2012b
10493-0401   STF1476     40 Sex.                                                                         
10493-4652   BRT 790     CPD-46@4866.                                                                    
10493-5319   LUH  16     WISE J104915.57-531906.1. Nearby (2.0 +/- 0.15pc) high-proper motion            
                         (-2759 +/- 6, +354 +/- 6mas/yr) star resolved as 1.5" (3au) binary by           
                         Gemini Multi-Object Spectrograph. Primary classified as L8 +/- 1,               
                         secondary as late-L/early-T.                                            Luh2013 
                         Based on several spectral indices, Burgasser et al. (2013) determine            
                         spectral types L7.5 and T0.5 +/- 1.                                     Bug2013 
                         Boffin et al. (2014) monitored LUH 16 over 2 months, and detected               
                         perturbation in the relative orbital motion which led them to suspect           
                         a substellar companion around one of the two components.                Bof2014 
                         Kniazev et al. (2013) obtained long-slit spectra and NIR images, and            
                         derive spectral types of L8 +/- 1 and T1.5 +/- 2.                       Kni2013 
                         Bedin et al. (2017) derive masses 32 +/- 11 and 27 +/- 10 Mjup for the          
                         components of this L7.5+T0.5 brown dwarf pair.                          Bdi2017 
                         Garcia et al. (2017) derive component masses 34.2 +/- 1.2 and                   
                         27.9 +/- 1.0 Mjup.                                                      GEV2017 
                         Bedin et al. (2024) derive masses 35.4 +/- 0.2 and 29.4 +/- 0.2 Mjup            
                         for the components of this brown dwarf system. They also set limits for         
                         a third body in the system.                                             Bdi2024 
10494+0439   GIC  93     G044-038/G044-037.                                                              
10496+1256   STF1477     HJL 131.                                                                HJL1986 
10496-3552   JC   22     B is CD-35@6767.                                                                
10498+3533   BEU  14     PM = -640-1018.                                                                 
                         GJ 1138. This pair has been previously reported as a 300 mas binary             
                         (Beuzit et al. 2004). The fact that it looks single in our AstraLux     Beu2004 
                         images despite the excellent quality of those observations implies              
                         that it must have undergone substantial orbital motion, bringing it to          
                         a much smaller (<100 mas) projected separation in June of 2012.         Jnn2014 
10498-0854   J  2076     Pair is -28s, -1' from BD-08 3018                                       J__1949a
10499-0453   GWP1469     ABL 399.                                                                Tob2012b
10500-1225   GWP1470     ABL 401.                                                                Tob2012b
10503-0854   HJ  838     41 Sex. A is a spectroscopic binary. C is BD-08@3019.                           
10503-1625   GWP1471     ABL 402.                                                                Tob2012b
10504-1326   LDS4023     AC: NLTT 25480/25488                                                    Chm2004 
10504-1459   RST3714     FIN 310.                                                                        
10505+5627   OSO  35     G196-047. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
10506-0611   GWP1472     ABL 400.                                                                Tob2012b
10506-4112   CPO 306     Nys calls A CPD-40@4776, and B CPD-40@4775.                                     
10509+0648   RAO 256     EE Leo.                                                                         
10510-5957   HJ 4378     B is CPD-59@2783.                                                               
10513+3607   BWL  26     Bowler et al. (2012) estimate the spectral type of the companion at             
                         M7 +/- 2. Age of the system is estimated as 25-300 Myr, distance                
                         22 +/- 3 pc, projected separation 4.4 +/- 0.6 au.  Masses of the                
                         primary and secondary are 0.25 +/- 0.5 Msun and 46 +/- 16 Mjup.         Bwl2012b
                         A comp is GJ 3629, spectral type M3.0Ve, mass 0.3-0.5 Msun. B is M7.5           
                         +/- 0.5, mass 41-94 Mjup. Orbital period is estimated at ~30 yr.        Bwl2015 
10514-1329   GWP1475     ABL 403.                                                                Tob2012b
10516-2115   BU 1428     A is the variable V Hya.                                                        
10519-5859   SNA  20     This object is the O8.5 Iaf spectroscopic standard. The Sb2 status              
                         reported by Chini et al. (2012) may rather trace intrinsic variability  Cii2012 
                         due to the string winds of this Iaf supergiant.                         Sna2014 
10520+1606   A  2373     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 29.48 +/- 39.87, 5.40, and 1.20 Msun, respectively.           Mlk2012 
10522+4423   DUP   2     Dupuy et al. (2015) resolved this L/T pair and determined it to be a            
                         J-band flux reversal binary. Parallax is 38.4 +/- 0.7 mas (distance             
                         26.1 +/- 0.5pc); spectral types are L6.5 +/- 1.5 and T1.5 +/- 1.0,              
                         masses 49 +/- 3 and 39 +/- 3 Mjup.                                      Dup2015b
10522+0728   STF1482     GIR   5 was incorrected listed as the AC pair at these coordinates.             
10524-1924   GWP1477     ABL 407.                                                                Tob2012b
10525+0730   GIR   5     Incorrected listed as the AC pair at the coordinates of STF1482.                
10526+0500   A  2773     HIP 53165. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
10526-1807   GWP1479     ABL 406.                                                                Tob2012b
10528-0516   GWP1481     ABL 404.                                                                Tob2012b
10529-1717   HDS1556     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.26 +/- 0.96, 2.06, and 0.94 Msun, respectively.             Mlk2012 
10530+5742   A  1352     This cannot be the close 5.508-d spectroscopic binary.                  Grf2009c
                         NU UMa, Algol-type eclipsing binary, P = 5.50762 d.                     Zas2011 
10530+0458   TOK 438     Latham (2012, private communication) identified HIP  5212 = HD 94292            
                         as SB2 with a period of 8.3yr and a highly eccentric orbit. It is               
                         resolved here securely at 50mas.                                        Tok2015c
10531-0311   FIL  27     BAL 214.                                                                        
10531-1439   GWP1484     ABL 405.                                                                Tob2012b
10531-2038   GJ 9336     Triple with inner SB1 of 6.8 days and outer SB system of estimated              
                         3.3 yr period which produces large acceleration. The estimated axis is          
                         40 mas, unresolved with speckle.                                        Tok2012a
10532-0905   LDS4030     NLTT 25623/25624                                                        Chm2004 
10532-1519   LDS4031     SKF   7.                                                                        
10532-3006   SHY 563     HIP  53226 + HIP  53314.                                                        
10533-1506   LDS4032     = GWP1486 = ABL 410.                                                    Tob2012b
10533-4316   CPO  53     BVD  87.                                                                        
10533-6207   WFC 110     JAW  19.                                                                        
10534-0215   S   617     BDS 5610 is probably identical (BDS). B is BD-01@2458.                  Bu_1906 
                         A is a spectroscopic binary.                                                    
             GC 14969    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin (1980).                                                         Grf1980b
             S   617     HJL 132.                                                                HJL1986 
                         H 5  62.                                                                MEv2010 
10535-2008   BU 1429     b 2 Hya. A is a suspected variable star, CV 101166.                             
10535-5851   DUN 102     B is CPD-58@2830.                                                               
10536-1111   GWP1487     ABL 409.                                                                Tob2012b
10540-0747   GWP1489     ABL 408.                                                                Tob2012b
10540-1958   GWP1488     ABL 412.                                                                Tob2012b
10543-3325   PRO  96     SWR 102.                                                                        
10546-1711   GWP1491     ABL 411.                                                                Tob2012b
10546-3845   HJ 4381     B is CD-38@6819.                                                                
10550-4215   SCO   1     KQ Vel.                                                                         
10554-1023   GWP1495     ABL 417.                                                                Tob2012b
10555-0055   GWP1498     ABL 413.                                                                Tob2012b
10555-0813   GWP1497     ABL 414.                                                                Tob2012b
10555-0917   GWP1496     ABL 416.                                                                Tob2012b
10556+2445   STF1487     54 Leo. B is a spectroscopic binary.                                            
                         Measure of 1927.33 made by triangulation of multiple measures.                  
                         H 3  30.                                                                MEv2010 
10556-1246   GWP1499     ABL 418.                                                                Tob2012b
10557+4246   MTR   1     While the proper motion indicates the pair is optical, spectral typing  Mtr2013 
                         and the distance based on colors is consistent with a physical pair.            
                         The optical/physical status of the pair is not certain at this time.            
10557+0044   BU 1076     55 Leo. If T is reasonably accurate, the RV run of the primary in               
                         1919-30 would fit the visual motion with an ascending node in the third         
                         quadrant.                                                                       
10557-4625   CPO 309     CPD-45@5026.                                                                    
10558-0841   GWP1500     ABL 415.                                                                Tob2012b
10559+2339   POU3092     LDS4038 = LDS6234.                                                              
10560-6024   HDS1561     This is the B[e] star GG Car, a supergiant with a rotating disk         IAU2014c
                         structure.                                                                      
10560-7725   REP  15     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = M1.5             Teff = 3630 +- 320        L = 0.50  +- 0.09           
                            Age =  1.6 +2.3/-0.8   M =    0.42 +0.21/-0.12   R = 1.79  +- 0.16           
                         B: SpT = M3               Teff = 3420 +- 250        L = 0.10  +- 0.02           
                            Age =  5.8 +10/-2.5    M =    0.29 +0.13/-0.12   R = 0.91  +- 0.07   Dae2013 
10561-2108   S   618     B is BD-20@3300.                                                                
10562+4802   ES 2636     B is BD+48@1901. One component is variable.                                     
10564-5733   HJ 4387     B is CPD-56@4017.                                                               
10566+2620   BRT3296     Originally published as BRT 156.                                        Brt1928 
10566+1739   STF1490     BDS 5613 same star.                                                             
                         HJL 134.                                                                HJL1986 
                         STF1489.                                                                        
10567-0542   GWP1501     ABL 420.                                                                Tob2012b
10568-3615   SWR 103     CPM pair                                                                Skf2004 
10570-0051   LDS6235     NLTT 25797/25799                                                        Chm2004 
                         HJL 135.                                                                HJL1986 
10570-7121   HJ 4392     B is CPD-70@1261.                                                               
                         SWR 104.                                                                        
10571-0214   GWP1504     ABL 419.                                                                Tob2012b
10571-6840   RMU   1     AB: Companion is a probable giant planet, mass 5 +/- 2 Mjup, located            
                         55.7 +/- 2.5 au from its host star, HD 95086.                           Rmu2013b
                         Galicher et al. (2014) provide a revised L' magnitude difference for            
                         the Rameau et al. (2013b) measure of 1/11/2012, obtained by better      Rmu2013b
                         calibration and derivation of the neutral density filter throughput.    Glc2014 
             KOU   2     AC: C component is a background star.                                   Rmu2013a
10576-1735   GWP1507     ABL 425.                                                                Tob2012b
10576-1955   GWP1506     ABL 428.                                                                Tob2012b
10577+1031   BPM 578     [PM2000]  994707 + [PM2000]  994714.                                    Gvr2010 
10578-0107   GWP1509     ABL 421.                                                                Tob2012b
10578-0555   GWP1510     ABL 423.                                                                Tob2012b
10579-1756   GWP1511     ABL 426.                                                                Tob2012b
10581+0634   GIC  94     G045-024/G045-023.                                                              
10583-7717   GHE  33     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = K1               Teff = 5080 +- 490        L = 1.6   +- 0.4            
                            Age = 10.  +12/-7      M =    1.4  +- 0.2        R = 1.65  +- 0.16           
                         B: SpT = M6               Teff = 2990 +- 320        L = 0.06  +- 0.01           
                            Age =  4.2 +5.8/-4.0   M =    0.10 +0.11/-0.07   R = 0.89  +- 0.09   Dae2013 
10585+1711   A  2375     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.93 +/- 1.76, 2.09, and 0.95 Msun, respectively.             Mlk2012 
10585-1046   LDS4041     NLTT 25870/25869                                                        Chm2004 
                         B is also known as LP 731-76.                                                   
                         Parallax of A component = 12.17 +/- 0.45 mas.                                   
                         Parallax of B component = 73.22 +/- 1.69 mas.                           JLB2017 
10585-1450   GWP1513     ABL 424.                                                                Tob2012b
10585-1816   GWP1512     ABL 427.                                                                Tob2012b
10586+0908   STF1497     ARG  73.                                                                        
10586-0234   GWP1514     ABL 422.                                                                Tob2012b
10590-1555   GWP1515     ABL 429.                                                                Tob2012b
10590-3607   SWR 105     CPM pair                                                                Skf2004 
10594-4308   HJ 4394     B is CD-42@6636.                                                                
10595+4026   47 UMa      = Chalawan. Combined solution, based on reduction of Hipparcos                  
                         intermediate astrometric data together with spectroscopic elements from CPS1996b
                         Butler & Marcy (1996).                                                  HaI2001 
10596+2527   AG  342     NLTT 25925/25926                                                        Chm2004 
10596+1800   HDS1568     Cvetkovic et al. (2016) estimate spectral types K0 and K9, masses 0.90          
                         and 0.48 Msun. Dynamical parallax is 29.33 +/- 3.03 mas.                Cve2016b
10598+5854   STF1495     B is BD+59@1339.                                                                
                         H 5 111.                                                                MEv2010 
10599-4445   CPO 310     LDS 326.                                                                        
11001-5149   VIG  13     The C and D components appear to be faint background stars; the                 
                         optical/physical nature of the E component is undefined.                Vig2012 
11003+4255   KUI  53     A is also a spectroscopic binary with a period of 5244d which is not    Grf2014c
                         either of these visual pairs. With the proper motion similarity of              
                         the A and B components this could be a physical quadruple.                      
                         AB: A is SB1, P=10.812y. CfA: P(Aa,Ab)=5241d = 14.35y                   Tok2014d
             LEP  38     AC: SHY 219. Bayesian analysis by Shaya & Olling (2011) indicates only  Shy2011 
                         ~50% probability pair is physical.                                              
11005+1131   BPMA 43     [PM2000]  995938 + [PM2000]  995834.                                    Gvr2010 
11006+3832   ES  304     ALI 1090 is not present                                                 Hei1983a
11006+0337   CHR  33     58 Leo. Also an occultation binary.                                             
11006-1819   HJ 1181     A is the semiregular variable R Crt. B is BD-17@3279.                           
11007+0606   BU  598     59 Leo.                                                                         
11007-5835   BRT3160     Aka JSP 447.                                                                    
11009-4030   FIN 365     Hipparcos parallax 15.42 +/- 0.42 mas. Dynamical parallax 11.2 mas,             
                         masses 1.75 and 1.65 Msun. The latest measure contradicts the first             
                         orbit published in Hartkopf et al. (2012), which in fact predicts an    Hrt2012a
                         unrealistically small mass sum. We propose here an alternative orbit            
                         with retrograde motion which reproduces the non-resolutions by Finsen   Fin1966a
                         in 1963-1966 and corresponds to a reasonable mass sum. Double lines             
                         were noted by Nordstrom et al. (2004). The star appears to be evolved.  Nrd2004 
                         The Hipparcos parallax could be affected by the orbital motion                  
                         unaccounted for in its data reduction.                                  Tok2012b
11013-7627   BRR   1     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = M1.5 +- 1        Teff = 3630 +- 150        L = 0.20  +- 0.03           
                            Age =  4.4 +5.1/-1.6   M =    0.41 +0.10/-0.06   R = 1.14  +- 0.05           
                         B: SpT = M2               Teff = 3560 +- 180        L = 0.22  +- 0.03           
                            Age =  3.3 +3.5/-1.0   M =    0.37 +0.13/-0.07   R = 1.24  +- 0.06   Dae2013 
11020+1437   STF1502     HJL 136.                                                                HJL1986 
11020-7131   Hen 3-554   Noted as possible binary (separation > 0".020) by Baines et al. (2006)  Bns2006 
11021+1659   BPM 579     [PM2000]  996665 + [PM2000]  996649.                                    Gvr2010 
11021-1542   H 1  77     H I  77.                                                                        
11022+0954   STF1503     A is the W UMa-type system AM Leo.                                              
11022+0945   HJ  172     HJL 137.                                                                HJL1986 
                         A small relative motion is obtained with uniform accuracy. There is no          
                         doubt the pair is physical.                                             Kiy2012 
11022-0335   BRT 548     J 2658.                                                                         
11023-6416   KRV  32     Classical Cepheid XY Car.                                                       
11024-2650   B   208     Too close, with few measures. Needs speckle.                                    
11026-2400   ALP  16     2MASSW J1102337-235945                                                          
                         Further observations are required to determine the physical/optical             
                         nature of this pair.                                                    AlP2007 
11026-7729   BRR   2     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = M3               Teff = 3560 +- 270        L = 0.11  +- 0.03           
                            Age =  7.0 +8.0/-3.5   M =    0.37 +- 0.05       R = 0.90  +- 0.03           
                         B: SpT = M5               Teff = 3130 +- 270        L = 0.018 +- 0.003          
                            Age = 13.  +50/-7      M =    0.13 +0.08/-0.09   R = 0.44  +- 0.04   Dae2013 
11028-0920   LSC 139     AB Crt.                                                                         
11028-5944   JSP 455     The primary is variable.                                                        
11029+3541   HO   47     A,BC: SCH   1.                                                                  
11030-0323   LDS 330     NLTT 26095/26096                                                        Chm2004 
11031+3215   SEI 522     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
11033+3558   Lal 21185   GJ 411 = Ci 20,604                                                              
                         Lippincott (1960) orbit rejected from Fourth Orbit Catalog              Lip1960 
                         ("not confirmed by subsequent observations")                            Wor1983 
                         They investigated the entire 40y plate series on Lalande 21185 and      Hry1982b
                         suggested a companion of, at most, two Jupiter mass and a period of             
                         22 years. They state that the 8y period, seen in data prior to 1960,            
                         was not seen after that.                                                        
11035+5432   A  1590     Heintz (1963) determined an orbit from combined visual, spectroscopic,          
                         and transit observations.                                               Hei1963a
11037+6145   BU 1077     alp UMa = 50 UMa = Dubhe.                                                       
                         Soderhjelm (1999) orbit has low incl. fixed at 180 deg; observations    Sod1999 
                         are lacking near periastron. Pair has a giant primary according to              
                         isochrone fit.                                                                  
                         Faint, distant pair at 385", 7.60V. Possible common proper motion               
                         with the SB HD 95638 at 280".                                                   
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         photocentric (astrometric) orbit based on combination of ground-        Gon2002a
                         based catalogs with Hipparcos.                                                  
                         Companion could not be seen any more the following years.               VBs1954 
                         Mk III Limb-darkened diameter  7.6   +/- 0.4   mas.                     MkT1988 
                         Mk III Limb-darkened diameter  7.11  +/- 0.10  mas.                     MkT2001 
                         Mk III Limb-darkened diameter  6.739 +/- 0.099 mas.                     MkT2003 
                         NPOI Limb-darkened diameter    6.91  +/- 0.08  mas.                     NOI2001b
                         NPOI Limb-darkened diameter  6.419 +/- 0.041 mas, Sp = G9III,           NOI2018 
                         R =17.03 +/- 0.13 \rsun, Teff = 5012 +/- 65 K, L = 165.1 +/- 8.3 \lsun,         
                         M = 3.44 +/- 0.11 \msun, Age = 0.28 +/- 0.03 Gyr.                               
                         AB: Malkov et al. (2012) derive dynamical and spectroscopic masses              
                         5.56 +/- 0.80 and 2.75 Msun, respectively.                              Mlk2012 
                         Spectroscopic orbital elements have been determined.                    XXX2018e
11037+4420   HJ 2554     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
11037+3253   HJ  493     Position by Espin is 1 minute greater in right ascension than John              
                         Herschel's. Used Espin position.                                                
11037-5121   NSN 289     Ellipsoidal Variable LL Vel.                                                    
11040+4321   FMR  14     SLW 561.                                                                        
11042-7627   SDT   1     AB: Companion appears to be co-moving with primary CT Cha. Schmidt et           
                         al. (2008) estimate the spectral type of the secondary at M8-L0.; most  Sdt2008b
                         probable mass is 17 +/- 6 Mjup. C component is a background star.               
                         Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = K7               Teff = 4060 +- 180        L = 0.67  +- 0.15           
                            Age =  3.0 +3.0/-1.5   M =    0.78 +- 0.20       R = 1.66  +- 0.07   Dae2013 
11044-6118   PLT   2     EH Car.                                                                 Plt1934 
11045+3814   HO  377     51 UMa.                                                                         
             HZG   8     AC: HJL1060.                                                            HJL1986 
11047-0413   STF1506     A,BC: Star A (mag 7.64, 11", G5) is physical and in slow direct motion          
             A   676     BC: Incorrectly listed by Docobo (1984) as STF1514 (erratum noted in    Doc1984b
                         Inf. Circ. 93, 1984)                                                            
                         BC. Eggen's (1967) orbit for this pair of 11th magnitude M dwarfs       Egg1967 
                         predicts a separation of 0".20 and a position angle of 86deg at this            
                         epoch.  Our measurement is in poor agreement with this prediction.      Hrt1992b
                         BC: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.36 +/- 0.38, 1.19, and 0.91 Msun, respectively.  Mlk2012 
             LAF  43     Heinze et al. (2010) determine the E component is a background object.  Hze2010 
11049+0634   GIC  95     G045-031/G045-032.                                                              
11049-6103   DUN 105     The classification of the B component is from Lindroos (1985),          Lnd1985 
                         who finds a distance of 3.5 kpc.                                        Msn1998a
11050+0720   KUI  54     chi Leo = 63 Leo                                                                
11052-7711   LAF   3     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = M4               Teff = 3270 +- 110        L = 0.10  +- 0.02           
                            Age =  4.2 +- 1.0      M =    0.22 +0.07/-0.05   R = 1.00  +- 0.03           
                         B: SpT = M3 +- 1          Teff = 3420 +- 150        L = 0.11  +- 0.02           
                            Age =  5.2 +5.0/-0.7   M =    0.30 +- 0.08       R = 0.95  +- 0.04           
                         The primary may be an SB2.                                              Dae2013 
11053+8102   GIC  96     LDS5203 = G253-042/G253-043.                                                    
                         NLTT 26133/26138                                                        Chm2004 
11053-2718   FIN  47     chi 1 Hya.                                                                      
                         Masses and bolometric magnitudes are derived for the two components of  Msn1999a
                         this system by Mason et al. (1999), based on assumed spectral types             
                         and available parallaxes.                                                       
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         van den Bos (1957).                                                     B__1957a
                         A new orbital analysis of this system is in progress, some three                
                         decades after  van den Bos published his solution.                      Hrt1996b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.79 +/- 0.19, 2.70, and 1.41 Msun, respectively.  Mlk2012 
11055+4332   VBS  18     Proper motion -4405 +940. The companion is WX UMa.                              
                         NLTT 26245/26247                                                        Chm2004 
                         CHARA Array Limb-darkened diameter of A :                               CIA2012f
                         R =  0.3982 +/- 0.0091 \rsun, L =  0.02129 +/-0.00026 \lsun,                    
                         Teff = 3497 +/-  39 K, M = 0.403 \msun.                                         
11056-1105   TOK 221     Astrometric binary; dm 5.4 mag, period ~ 30y Orbit (Gontcharov et al.           
                         2000)                                                                   Tok2012b
11057-7727   AHM   1     CHXR 15. Primary spectral type M5.25. Estimated mass ratio 0.64         Ahm2007 
                         Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = M5 +- 1          Teff = 3130 +- 140        L = 0.06  +- 0.01           
                            Age =  4.5 +2.5/-0.9   M =    0.16 +- 0.05       R = 0.87  +- 0.04           
                         B: SpT = M5               Teff = 3130 +- 170        L = 0.04  +- 0.01           
                            Age =  6.0 +6.0/-2.0   M =    0.14 +- 0.06       R = 0.71  +- 0.04   Dae2013 
11058+7440   MLR 423     Also known as TDS 616.                                                          
11059-3411   BRT1668     A likely plate flaw.                                                    Grv2021b
11061+7837   LDS1726     NLTT 26189/26190                                                        Chm2004 
11061+4253   GIC  97     AB: NLTT 26262/26264                                                    Chm2004 
11061+1325   BRT1271     Declination corrected by Heintz.                                        Hei1980a
11061+0702   STF1507     HJL 138.                                                                HJL1986 
                         H 2  78.                                                                MEv2010 
11063+3113   OSO  36     G120-015. AC is not a common proper motion pair, based on comparison            
                         with POSS2 red plates.                                                  Oso2004 
11065-1325   STF1509     B is BD-12@3347.                                                                
11065-5841   HDO 210     A is variable.                                                                  
11065-7738   LUH  17     The primary is the young low-mass star CHXR 73 (mass ~0.35 Msun).               
                         Luhman et al. (2006) conclude that the companion is also a member of            
                         Chamaelon I, and a young pre-main sequence star, spectral type >M9.5,           
                         mass 0.012 +0.008/-0.005 Msun.                                          Luh2006c
                         Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = M2.5             Teff = 3490 +- 180        L = 0.09  +- 0.07           
                            Age =  8.  +70/-5      M =    0.32 +- 0.11       R = 0.83  +- 0.04   Dae2013 
11069+0157   BU  599     65 Leo.                                                                         
11069-4629   BRT 795     A likely plate flaw.                                                    Grv2021b
11072+5711   HJ 2556     Position correction by Heintz.                                          Hei1983a
11072+3204   SEI 523     ID uncertain - no sign of SEI pair, and ALADIN only indicates one               
                         Astrographic Catalog star in vicinity of Scheiner's coordinates.                
11072-5952   SNA  21     The new companion can hardly be the SB1 companion (P=5.5d) from         Stc2001 
                         Stickland & Lloyd (2001).                                               Sna2014 
                         The classification and SB1 orbit are from Garcia (1994 ApJ 436, 705).   Msn1998a
11073+2832   HJ 1185     C is a faint nebula (NGC 3527). Distance 259.4".                                
11073-4238   HJ 4409     The variable V815 Cen.                                                          
11073-7738   REP  17     DI Cha, a quadruple in a star-forming region in Chamaelon. Schmidt et           
                         al. (2013) resolve the primary into a 0.2" G2/M6 pair, with estimated           
                         orbital period of 130y. The B component is a 50mas pair of M5.5 +/-             
                         1.5 dwarfs, with estimated period 65y.                                  Sdt2013 
                         Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = G0               Teff = 6030 +- 290        L = 4.7   +- 1.0            
                            Age =  7.1 +3.0/-0.7   M =    1.7  +- 0.2        R = 2.00  +- 0.10           
                         B: SpT = M5               Teff = 3130 +- 290        L = 0.11  +- 0.02           
                            Age =  3.0 +3.0/-2.8   M =    0.18 +0.06/-0.08   R = 1.13  +- 0.11   Dae2013 
11074-1522   TOK 139     HIP 54366. A is SB1, P=1061d, N04: dRV= 1.6.                            Tok2014d
11074-4815   CPO 316     B is CD-47@6520.                                                                
11075-7651   REP  19     Aa,Ab: VV Cha. Imprecise coordinates led to REP 19 and KSA 42 being             
                         Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         Aa: SpT = M1.5            Teff = 3630 +- 180        L = 0.14  +- 0.03           
                             Age =  7.0 +9.0/-3.0  M =    0.40 +0.14/-0.06   R = 0.96  +- 0.05           
                         Ab: SpT = M3 +- 1         Teff = 3420 +- 150        L = 0.09  +- 0.02           
                             Age =  6.4 +4.7/-2.2  M =    0.29 +- 0.07       R = 0.87  +- 0.04   Dae2013 
             KSA  42     initially catalogued as separate pairs. Although REP 19 was added to            
                         the WDS before KSA 42, its WDS designation was less accurate, so was            
                         changed from 11072-7651.                                                        
11076+2346   BRT3297     Originally published as BRT 159.                                        Brt1928 
11077+5958   PRB   3     Primary is WD 1104+60 = NLTT 26342, secondary is LP 93-311. Possible            
                         CPM pair, according to Probst (1983).                                   Prb1983 
11077-7734   AHM   2     Cha Ha 2. Primary spectral type M5.25. Estimated mass ratio 0.94        Ahm2007 
11079-7727   AGE   3     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = K7               Teff = 4060 +- 290        L = 1.2   +- 0.3            
                            Age =  1.3 +2.5/-0.5   M =    0.75 +- 0.25       R = 2.21  +- 0.16           
                         B: SpT = M2.5             Teff = 3490 +- 110        L = 0.42  +- 0.09           
                            Age =  1.6 +- 0.4      M =    0.36 +- 0.04       R = 1.78  +- 0.06           
                         The B component may be an SB1.                                          Dae2013 
11080+4100   LDS4062     NLTT 26367/26368                                                        Chm2004 
11080-0509   LDS 852     LDS6239.                                                                        
                         G163-51 / G163-50.  Secondary is white dwarf WD 1105-048.               Far2005b
11080-7739   GHE  34     The primary is Sz 22, embedded in a circumstellar disk or reflection            
                         nebula. Schmidt et al. (2014) resolve the A component into a 0.5"               
                         pair; the Ab component is a co-moving M4.5 +/- 1.5 dwarf.               Sdt2013 
             LAF   8     BC: Daemen et al. (2013) derive the following component properties              
                         (units are K,Lsun,Myr,Msun,Rsun):                                               
                         B: SpT = M0.5             Teff = 3780 +- 400        L = 0.50  +- 0.09           
                            Age =  2.0 +8/-1.1     M =    0.52 +0.38/-0.19   R = 0.47  +- 0.05           
                         C: SpT = M0.5             Teff = 3780 +- 400        L = 0.090 +- 0.006          
                            Age > 23.              M =    0.50 +- 0.2        R = 0.70  +- 0.07   Dae2013 
11080-7742   GHE  35     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = K7               Teff = 4060 +- 460        L = 1.6   +- 0.3            
                            Age =  1.0 +3.0/-0.7   M =    0.75 +0.50/-0.35   R = 2.55  +- 0.29           
                         B: SpT = M0 +- 1.5        Teff = 3850 +- 290        L = 0.76  +- 0.10           
                            Age =  1.5 +2.5/-0.6   M =    0.57 +0.28/-0.19   R = 1.97  +- 0.15           
                         The primary may be an SB2.                                              Dae2013 
11083-7734   GHE  27     IRAS 11068-7717 = PDS 47 = Glass I.                                     Gre1992 
                         CHXR 32 is a triple system, consisting of a single G5 star with an              
                         edge-on disk, and a co-moving pair of M1/M3.5 dwarfs.                   Sdt2013 
                         Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT < M3                                                                     
                         B: SpT = M0.5             Teff = 3780 +- 210        L = 0.57  +- 0.13           
                            Age =  1.8 +2.2/-0.7   M =    0.52 +0.18/-0.14   R = 1.77  +- 0.10   Dae2013 
11084+0313   H 5  68     H V 68. B is BD+03@2462.                                                        
11084-7742   NHR   6     Primary is Cha Halpha 5, a close (50mas) pair of M5-M7 dwarfs, with an          
                         estimated orbital period of 46y.                                        Sdt2013 
11085-2939   CVR1742     Aka TOI1027.                                                                    
11087-2805   VSP  28     10 Crt.                                                                         
11087-5037   CPO 318     TDS7696.                                                                        
11088+2610   LDS4064     AB: NLTT 26415/26414                                                    Chm2004 
11088+2440   A   677     67 Leo.                                                                         
11088-7519   KOH  89     PU Car.                                                                         
11092-1851   B  2007     Difficult pair; measures puzzling.                                      B__1963b
11092-3002   WBB   2     This previously known binary (e.g. Webb et al. 1999) is part of the     Wbb1999 
                         TW Hya association, and is also known as TWA 2.                         Jnn2012 
11092-7729   REP  20     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = M2.5 +- 0.5      Teff = 3490 +-  70        L = 0.25  +- 0.05           
                            Age =  2.7 +0.7/-0.5   M =    0.36 +- 0.05       R = 1.37  +- 0.03           
                         B: SpT = M2 +- 0.5        Teff = 3560 +-  70        L = 0.20  +- 0.04           
                            Age =  4.0 +1.3/-1.0   M =    0.38 +- 0.05       R = 1.17  +- 0.02           
                         C: SpT = M2.5 +- 0.5      Teff = 3490 +-  70        L = 0.14  +- 0.03           
                            Age =  4.7 +2.3/-1.2   M =    0.34 +- 0.05       R = 1.04  +- 0.02           
                         The B component is an SB1.                                              Dae2013 
11093-7630   BRR   3     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         Aa: SpT = M2 +- 1         Teff = 3560 +- 150        L = 0.36  +- 0.07           
                             Age =  2.0 +1.0/-0.5  M =    0.38 +0.10/-0.05   R = 1.57  +- 0.07           
                         Ab: SpT = M4              Teff = 3270 +- 110        L = 0.035 +- 0.007          
                             Age = 12.  +8.0/-5.5  M =    0.19 +0.14/-0.04   R = 0.59  +- 0.02   Dae2013 
11095+8306   STF1499     LDS1728.                                                                        
                         HJL 139.                                                                HJL1986 
11095-2559   LDS4067     CPM. B is white dwarf WD1107-257                                        Tok2014d
11097-5850   KRV   2     Classical Cepheid ER Car.                                                       
11098+6320   H 4 106     H IV 106. Also known as STF1513.                                                
11098-7637   GHE  28     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = B9               Teff =10500                                           
                         B: SpT = M3.5 +- 0.5      Teff = 3340 +-  70        L = 0.11  +- 0.08           
                            Age =  4.5 +15/-1.9    M =    0.26 +- 0.07       R = 0.99  +- 0.02   Dae2013 
11098-7731   PSI   3     Perci et al. (2005) found [KG2001] 102 to consist of 4 components,      Psi2005 
                         all within a 2" region. The A component is determined to be                     
                         substellar, with a mass of 33-55 Mjup at a distance of 160 pc. The C            
                         and D components are believed to be physical companions, but the B              
                         component, of spectral type K7V, is probably a background star at a             
                         distance of about 550 pc. Nearby star "Anon1" was also found to be              
                         double.                                                                         
11098-7738   GHE  29     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = M1               Teff = 3710 +- 200        L = 0.81  +- 0.15           
                            Age =  1.1 +0.6/-0.3   M =    0.49 +- 0.12       R = 2.18  +- 0.12           
                         B: SpT = M5               Teff = 3130 +- 210        L = 0.10  +- 0.02           
                            Age =  3.3 +2.7/-2.9   M =    0.18 +0.05/-0.06   R = 1.08  +- 0.07   Dae2013 
11099+1456   BPMA 44     [PM2000] 1000317 + [PM2000] 1000217.                                    Gvr2010 
11099+1107   FYM  37     AB and AC were initially incorrectly assigned to 11091+1105 HJ 176.     FyM2014b
11099-7629   LAF  11     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         Aa: SpT = M3.5            Teff = 3340 +- 290        L = 0.29  +- 0.06           
                             Age =  1.8 +1.2/-1.6  M =    0.30 +0.11/-0.10   R = 1.62  +- 0.13           
                         Ab: SpT = M7              Teff = 2880 +- 360        L = 0.05  +- 0.01           
                             Age =  4.0 +4.0/-3.9  M =    0.08 +0.12/-0.07   R = 0.91  +- 0.11   Dae2013 
11100+1237   LDS6240     NLTT 26471/26477                                                        Chm2004 
11100-7635   GVT   4     WW Cha.                                                                         
11103+3840   HJ 2561     A measure by Schembor (1926.08, 172.6@, 23.24") appears instead to be   Sch1927a
                         an additional measure of 11221+3705 STF1533A,BC.                                
11105-3732   REP  21     IRAS 11080-3715 = PDS 50 = TWA 3.                                       Gre1992 
                         This previously known binary (e.g. Brandeker et al. 2003) is part of    Bnk2003 
                         the TW Hya association, and is also known as TWA 3.                     Jnn2012 
                         Rectilinear solution by Miles & Mason (2016)                            Msn2016b
                         and Mason et al. (2018).                                                Msn2018a
11106-7733   GHE  36     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         Aa: SpT = K5.5            Teff = 4210 +- 390        L = 0.72  +- 0.14           
                             Age =  4.5 +9.5/-3.1  M =    0.95 +0.20/-0.42   R = 1.60  +- 0.15           
                         Ab: SpT = K7              Teff = 4060 +- 210        L = 0.47  +- 0.09           
                             Age =  5.5 +6.5/-3.0  M =    0.80 +0.20/-0.22   R = 1.39  +- 0.07           
                         The pair is also an SB2.                                                Dae2013 
11107+3110   HJ 2562     A premature orbit has been calculated.                                  B__1963b
11107-6023   SNA  22     Aa,Ab: The central object was reported as possible SB1 (Thackeray et            
                         al. 1973, MmRAS 77, 199; Chini et al. 2012) but without more            Cii2012 
                         information on the spectroscopic period                                         
                         one cannot decide whether the spectroscopic and PIONIER companions              
                         are identical. The separation and magnitude difference make this a              
                         plausible option, however.                                              Sna2014 
11109-7646   AHM   3     Hn 13. Primary spectral type M5.75. Estimated mass ratio 0.95           Ahm2007 
11110+0625   OSO  37     G010-004. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
11111+3027   STT 231     Mt. Wilson spectral types M1, M2, G5.                                           
                         AB: NLTT 26534/26531                                                    Chm2004 
                         Pair was listed, but in a "rejected" list, not part of discoverer's             
                         regular numbering sequence.                                                     
                         AB Hyperbolic orbit by Hopmann (1960). e = 575.                         Hop1960b
                         sigma = areal constant in the true orbit = 3.75 arcsec^2/yr                     
                         q = periastron distance in the true orbit = 33".73                              
                         All hyperbolic orbits rejected from Fourth Orbit Catalog                Wor1983 
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
11113+6601   S   621     STTA107.                                                                        
                         AB and AC: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
11114+4325   KUI  55     NLTT 26552/26553                                                        Chm2004 
11115+2518   LDS4071     NLTT 26562/26559                                                        Chm2004 
11115+1520   BPM 580     [PM2000] 1001018 + [PM2000] 1001022.                                    Gvr2010 
11116-1459   LTT 4120    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
11117+3441   KZA  10     No object at precise coordinates of A component down to >20th mag,              
                         although Kazeza's AB and AC measures from that location do point to             
                         stars of appropriate magnitudes. Conclude A component is probably               
                         plate flaw. CB measure calculated from Kazeza's AB and AC measures.     Kza1984 
11118+4250   ENG  45     AB: NLTT 26576/26564                                                    Chm2004 
                         AB: HJL 140.                                                            HJL1986 
                         AB: SHY 221. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AB: A is possibly astrometric binary.                                   Tok2014d
11118-3045   BRT2985     SWR 108.                                                                        
11118-6042   B  1182     The star belongs to a group behind Tr 18 (Vazquez & Feinstein 1990              
                         A&AS 86, 209) at a distance of 2.8 kpc; we designate this as "Tr 18B"           
                         in Table 1.                                                             Msn1998a
11118-7620   LAF  14     B is a background star unrelated to A, a young Cha I object.            Laf2008 
11119-7620   LAF  15     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = M2.5             Teff = 3490 +- 110        L = 0.20  +- 0.04           
                            Age =  3.4 +1.2/-0.8   M =    0.34 +- 0.06       R = 1.22  +- 0.04           
                         B: SpT = M3.5             Teff = 3340 +- 110        L = 0.15  +- 0.03           
                            Age =  3.4 +1.2/-0.6   M =    0.27 +- 0.06       R = 1.15  +- 0.04   Dae2013 
11121-7126   B  2273     A may be variable.                                                              
11124-7637   REP  22     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = K7 +- 3          Teff = 4060 +- 590        L = 0.76  +- 0.17           
                            Age =  2.5 +13/-1.7    M =    0.78 +- 0.40       R = 1.77  +- 0.26           
                         B: SpT = M2.5 +- 1.5      Teff = 3490 +- 220        L = 0.10  +- 0.02           
                            Age =  7.2 +12/-3.4    M =    0.32 +0.12/-0.09   R = 0.85  +- 0.05   Dae2013 
11125+3549   STTA108     AB and AC: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         Primary is MN UMa, variable of BY Dra type.                             Tok2014d
             KIR   3     AE. Data from 2MASS. Kirkpatrick et al. (2001) derive spectral types    Kir2001a
                         G0V and L4.5V, determine is physical pair, separation ~2000 au.                 
             STTA108     BD: Distances are 2083.6" in 1825, 2094.6" in 1910. D is BD+36@2170.            
             BOY   5     Ea,Eb: Originally listed as separate pair WDS 11124+3548, before                
                         association with  WDS 11125+3549 recognized.                                    
                         Dupuy et al. (2014) find a total mass 0.095 +/- 0.003 Msun (99 +/- 3            
                         Mjup), log age 8.87 +/- 0.08. Spectral types are L4.5 and L6.           Dup2014 
11125-1830   BU  220     psi Crt.                                                                        
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 10.78 +/- 6.79, 4.90, and 2.19 Msun, respectively.            Mlk2012 
11125-4905   CPO 319     CPD-48@3801.                                                                    
11127-7722   WOI   1     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = G8 +- 3          Teff = 5507 +- 440        L = 2.0   +- 0.4            
                            Age = 16.  +30/-10     M =    1.3  +- 0.2        R = 1.52  +- 0.12           
                         B: SpT = K7 +- 1.5        Teff = 4060 +- 310        L = 0.35  +- 0.08           
                            Age =  9.0 +16/-6.5    M =    0.80 +0.15/-0.3    R = 1.20  +- 0.09   Dae2013 
             LAF  16     AC: C is a background star unrelated to the close AB pair.              Laf2008 
11128+0453   J  1011     Despite having an orbit, an optical pair based on parallax and proper   Mlk2022 
                         motion.                                                                 Izm2019 
11128-6410   HJ 4415     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
11131+4011   HJ  494     Same as STF1515.                                                                
11135-5526   HJ 4417     B is CPD-54@4398.                                                               
11136+5525   A  1353     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.68 +/- 1.12, 2.70, and 1.20 Msun, respectively.             Mlk2012 
11137+2506   SHY 567     HIP  54845 + HIP  54217.                                                        
11137+2008   STF1517     Alternate spectral types G5III, G7IV. Slightly variable.                        
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Hopmann orbit rejected from Fourth Orbit Catalog                        Hop1970 
                         ("period over 4000 years")                                              Wor1983 
             BU 1431     AB,C: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
11140-1904   LDS4073     NLTT 26694/26692                                                        Chm2004 
11141+2031   STT 573     AB: del Leo = 68 Leo = Zosma. Variable? Smyth's quoted separations for  Smy1844 
                         both AB and AC are differences in RA only.                                      
11144-2245   LDS 341     NLTT 26721/26720                                                        Chm2004 
11144-7733   BRR   4     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = M3.5             Teff = 3340 +- 110        L = 0.11  +- 0.02           
                            Age =  4.5 +2.0/-1.0   M =    0.26 +- 0.05       R = 0.99  +- 0.03           
                         B: SpT = M6.5             Teff = 2940 +- 200        L = 0.030 +- 0.006          
                            Age =  5.5 +4.5/-1.5   M =    0.08 +0.10/-0.05   R = 0.66  +- 0.04   Dae2013 
11145+1823   LDS4074     NLTT 26709/26710                                                        Chm2004 
11145+0516   STF1518     J 1012.                                                                         
11148+2257   POU3098     ELS 3 is identical                                                      Hei1983a
11148-7734   LAF  19     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = M2 +- 1          Teff = 3560 +- 150        L = 0.19  +- 0.04           
                            Age =  4.0 +4.0/-1.3   M =    0.37 +0.10/-0.05   R = 1.15  +- 0.05           
                         B: SpT = M4               Teff = 3270 +- 150        L = 0.05  +- 0.01           
                            Age =  8.0 +7.0/-3.2   M =    0.20 +0.07/-0.05   R = 0.71  +- 0.03   Dae2013 
11150+1607   DEA  75     NLTT 26746 + 2MASS J11150150+1607026. Baron et al. (2015) estimate              
                         spectral types M4.0 +/- 0.5 and L5 +/- 1, distances 36 +22/-14 and              
                         37 +3/-35 pc, masses 0.207-0.272 and 0.056-0.073 Msun.                  BFr2015 
11150-5420   BRT2062     CD-53@3941.                                                                     
11151+3735   CHR 192     1987.2666: CHR 192Aa,Ab is a new component to the 0".6 pair STT 232,            
             STT 232     discovered by Otto Struve in 1843. Reprocessing of archival data                
                         (whose 1987 and 1988 measurements for the wide pair were originally             
                         published in McAlister et al. 1989) has allowed us to confirm this      McA1989 
                         discovery and also to note that the system appears to be accelerating           
                         toward periastron.                                                              
11151-3929   SEE 128     Direct motion.                                                                  
11151-6116   B  1184     AE and AF pairs erroneously designated I  1132.                                 
11152+7329   STF1516     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             STT 539     AC: NLTT 26722/26719                                                    Chm2004 
             HDS1603     BD: BD+74  456a.                                                                
             STT 539     BC: Rectilinear solution by Friedman et al. (2012).                     USN2012a
11153-0132   LDS4076     NLTT 26765/26766                                                        Chm2004 
11154-1807   LDS 342     B is BD-17@3337.                                                                
11154-5249   HD 97961    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
11157+4551   STTA109     B is BD+46@1707.                                                                
11157-1621   SHJ 372     B is BD-15@3226.                                                                
                         H N 104.                                                                MEv2010 
11159+1318   MCA  35     73 Leo. A spectroscopic binary now resolved by speckle interferometry.          
                         1985.1123, 1985.2053: This system has been observed at the limit of             
                         resolution of a 2-m telescope, so delta m is probably < 1.              Bnu1986 
                         Values of P, T, e, and omega for the Ren & Fu (2007) orbit are adopted  RSl2007 
                         from the orbit of Mason et al. (1997). Their derived masses for the     Msn1997b
                         primary and secondary are 1.81 +/- 0.49 and 1.54 +/- 0.42 Msun,                 
                         respectively.  The authors note that these masses are less than the             
                         ones predicted by either the Mason et al. or Mante (2002) solutions,    Mnt2002a
                         but that their secondary mass is in reasonable agreement with the               
                         value expected for an F1 main-sequence star.                                    
                         Martin et al. (1998) derive component masses 2.624 +/- 1.197 and                
                         2.315 +/- 1.075 Msun.                                                   Mig1998 
                         Malkov et al. (2012) derive dynamical and spectroscopic masses                  
                         2.49 +/- 0.65 and 2.40 Msun, respectively.                              Mlk2012 
11159+0205   NLTT 26792  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Carney et al. (2001) They derived component masses 1.18 and 0.60 Msun   Crn2001 
                         and an estimated semimajor axis of 16.36 mas.                           Ren2013 
11161+5246   STF1520     HJL 142.                                                                HJL1986 
                         H N  68.                                                                MEv2010 
                         GJ 421.1                                                                Tok2014d
11165+6913   SHY 569     HIP  55076 + HIP  58483.                                                        
11165+2627   BUP 137     B is BD+27@2000.                                                                
11166-5215   RST9002     Previously known as RST2737a.                                                   
11167-0339   SHJ 121     74 Leo = phi Leo. B is BD-02@3314.                                              
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         H 6  79.                                                                MEv2010 
11170-0708   BU  600     A is an Alpha CVn-type variable, SV Crt., and a spectroscopic binary.           
                         AC: H N  26.                                                            MEv2010 
11172-0153   EPI   1     EPIC 201338508 = K2-5. Primary is host star to two planets; planet              
                         periods 5.73 and 10.93d, radii 1.92 Rearth, a 0.05 and 0.08 au.         Mtt2015b
11173-6749   DON 471     A is variable.                                                                  
11175-5906   R   163     Spectrum B9.5/A0III.                                                            
11177-2705   RST1572     TDS7778.                                                                        
11179-4034   I  1538     Measures uncertain.                                                             
11182+3132   STF1523     xi UMa = 53 UMa = Alula Australis. A is known to have an unseen                 
                         companion, P = 1.83y. B is a spectroscopic binary. The first binary             
                         star orbit was computed by Savary, a "librarian-observer" at Paris      Sav1830 
                         Observatory giving courses in "social arithmetic," i.e., statistics.            
                         Spectral types and masses of components assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
                         Preliminary Keplerian AB 2-orbit model by Soderhjelm (1999) gives       Sod1999 
                         good solution (failure in HIP).                                                 
                         Many-body perturbations observable but not yet studied. Cf. Aa,Bb               
                         analysis in Mason et al. (1995)                                         Msn1995 
                         Both orbits are visual and spectroscopic. The orbit of the visible              
                         AB pair includes the secular perturbations in inclination, node,                
                         longitude of periastron, and K. Star B is also SB1, P = 3.98 d.                 
                         The short-period pair has been resolved by infrared speckle                     
                         interferometry                                                          Mcy1983 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         HR 4375 (A component of STF1523) was misidentified as HR 4374 (B                
                         component) in McAlister (1978).                                         McA1978c
                         An orbital analysis of xi UMa, including the AB pair, the astrometric           
                         companion, and the newly-discovered Bc companion, has been published            
                         by Mason et al. (1995).                                                 Msn1995 
                         AB: H 1   2.                                                            MEv2010 
             CHR 178     Bb. Abt & Biggs (1972) note variable RV.                                AbH1972 
                         Given the typical lack of accuracy associated with astrometric orbits   Tok2010b
                         it is possible that in the doubling of peaks CHR 178 is actually the            
                         known Aa,Ab observing when the faint Ab was flaring. In this                    
                         interpretation, the second elongated observation of CHR 178 is assumed          
                         to be false.                                                                    
             WTE   1     AD: Faint T8.5 brown dwarf companion at separation ~4000au exhibits             
                         common proper motion. IR luminosity and color suggest that mass of              
                         companion 14 and 38 Mjup for system ages 2 and 8 Gyr, respectively.     WtE2013 
11183+0746   HEG   1     This  is evidently a lensed quasar and not a double star, or at the             
                         very least with a Z of 1.7, is not a galactic double star.                      
11184-7622   BRR   5     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                         A: SpT = M0 +- 1          Teff = 3850 +- 180        L = 0.44  +- 0.10           
                            Age =  3.0 +4.0/-1.4   M =    0.58 +0.20/-0.13   R = 1.50  +- 0.07           
                         B: SpT = M1               Teff = 3710 +- 110        L = 0.12  +- 0.02           
                            Age = 12.  +17/-7      M =    0.46 +0.10/-0.18   R = 0.83  +- 0.02   Dae2013 
11185+3306   STF1524     nu UMa = 54 UMa = Alula Borealis                                                
                         Mk III Limd-darkened diameter  4.71  +/- 0.07  mas.                     MkT2001 
                         Mk III Limb-darkened diameter  4.759 +/- 0.048 mas.                     MkT2003 
                         NPOI Limb-darkened diameter    4.76  +/- 0.07  mas.                     NOI2001b
                         NPOI Limb-darkened diameter  4.561 +/- 0.016 mas, Sp = K3III,           NOI2018 
                         R =60.00 +/- 1.27 \rsun, Teff = 4422 +/- 56 K, L = 1242  +/- 81  \lsun,         
                         M = 3.82 +/- 0.23 \msun, Age = 0.20 +/- 0.03 Gyr.                               
                         H N  53.                                                                MEv2010 
11186-0504   BRT 433     A likely plate flaw.                                                    Grv2021b
11187+0250   STF1526     B is BD+03@2482.                                                                
                         Primary is eclipsing binary of Algol-type, period 9.1784 d.             Zas2012 
                         HJL 143.                                                                HJL1986 
11188-4812   RST4941     TDS7782.                                                                        
11190+1416   STF1527     A premature orbit has been computed.                                            
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         H N 142.                                                                MEv2010 
                         Prieur et al. (2012) derive a dynamical parallax of 31.2 mas and                
                         (using their orbital elements and the revised Hipparcos parallax of             
                         van Leeuwen 2007 A&A 474, 653) a total mass 1.7 +/- 1.0 Msun.           Pru2012 
                         Hipparcos parallax 32.52 +/- 1.39 mas. Dynamical parallax 34.2 mas,             
                         masses 0.98 and 0.61 Msun. STF 1527 has a long orbital period of 415y,          
                         but it moved fast through the periastron in 2009-2012, allowing us to           
                         compute a better orbit.                                                 Tok2012b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.04 +/- 1.03, 2.06, and 1.07 Msun, respectively.             Mlk2012 
11191+3811   CHR 133     55 UMA. Primary is 2.6d SB1 (#669 in Batten et al., 1989).              Bte1989 
                         The speckle pair must be different, hence a triple.                             
                         Mass-sum in fair agreement with Liu et al. (1997)                       Liu1997 
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         McAlister et al.                                                                
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 5.89 +/- 0.40, 4.71, and 2.09 Msun, respectively.             Mlk2012 
11192-1950   ARA 683     Primary is RV Crt, Algol-type eclipsing binary, period 1.170509d.       Zas2013 
11194-0139   STF1529     NLTT 26997/26995                                                        Chm2004 
11194-6435   LDS6242     A is CD-63@643.                                                                 
11197-0125   LDS4083     NLTT 27027/27026                                                        Chm2004 
11200+6551   TAM   1     Primary is the nearby flar star Gl 424 = SZ UMa. The companion appears          
                         to be a M4.5 dwarf, with a mass of ~0.18Msun. Estimated orbital period          
                         of the system is about 2.5y.                                            Tam2008b
11204+0117   EPI   2     EPIC 201549860. Primary is candidate planet host star; planet period            
                         5.61d, radius 2.20 Rearth, a 0.06 au.                                   Mtt2015b
11205+0530   HJ 2566     G045-048. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
11206+0230   EPI   3     EPIC 201629650 = K2-13. Primary is planet host star; planet period              
                         39.91d, radius 1.89 Rearth, a 0.21 au.                                  Mtt2015b
11206-2718   BRT2986     CPD-26@4502.                                                                    
11210-5429   I   879     pi Cen.                                                                         
                         The spectral lines are very poor; the RV range of 30km/s is probably            
                         mere scatter. A few more speckle obs needed to constrain eccentricity.          
                         1976.474: This system was observed within a few months of periastron.   BLM1978 
                         Hipparcos parallax 9.12 +/- 0.34 mas. Dynamical parallax 9.1 mas,               
                         masses 6.43 and 3.68 Msun.  The orbit by Mason et al. (1999) had to be  Msn1999a
                         revised using our measures near the periastron. The high eccentricity           
                         e = 0.853 is now well established.                                      Tok2012b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 15.29 +/- 3.02, 8.37, and 4.79 Msun, respectively.            Mlk2012 
11211-3531   I  1539     Position angle uncertain. Needs speckle.                                        
11212+5807   GRV1193     SLW 589.                                                                        
11213-3447   SWR 110     CPM pair                                                                Skf2004 
                         RXJ1121.3-3447 = TWA 13. TW Hya association. Both components are                
                         weak-lined T Tauri stars; spectral types are M1 + M2.                   Stz1999 
11214-2027   STN  22     LDS 348.                                                                        
                         NLTT 27132/27131                                                        Chm2004 
11216+5111   LDS5204     LDS6243.                                                                        
11218+2208   LDS4088     NLTT 27148/27149                                                        Chm2004 
11218-1313   FME   1     Dupuy et al. (2009) derive a system mass of 0.146 +/- 0.014 Msun, and           
                         component spectral types M8 +/- 0.5 and L7 +/- 1.                       Dup2009 
                         LHS 2397a. Assuming a parallactic distance of 14.3 +/- 0.4 pc                   
                         (Monet et al. 1992), Konopacky et al. (2010) derive a system mass of    Dah1992 
                         0.144 +/- 0.013 Msun.                                                   Kon2010 
11219+0343   EPI   4     EPIC 201704541. Primary is eclipsing binary, period 0.411d.             SJR2016 
11221+3705   STF1533     B is BD+37@2177.                                                                
                         A,BC: HJL 144.                                                          HJL1986 
11221+0128   UC 2124     Also known as CBL 556.                                                  Skf2013 
11221-2447   GRE   3     Aa,Ab: IRAS 11195-2430 = PDS 54.                                        Gre1992 
             I   507     Variable TV Crt. Tokovinin (1999) gives three possible orbits which     Tok1999b
                         are consistent with visual and IR speckle observations, as well as              
                         radial velocity difference and Hipparcos parallax for stars of this             
                         type (K5V). Inclination is near 90 degrees, but eccentricity is not             
                         high, as predicted by Torres et al. (1995).                             Trr1995b
                         Star has large IR excess. A component is SB1 (P=262 days), while B              
                         component is SB2 (P=315 days).                                          Tok1999b
                         Torres et al. (1995) report radial velocity data and make some                  
                         constraints on possible astrometric orbits.                             Trr1995b
                         See also HST observations and discussion of all components of this              
                         multiple system by Soderblom et al. (1998).                             Sdb1998 
             SHY 228     AC: HIP  55505 + HIP  58029.                                                    
             BOD   1     Ba,Bb. Masses determined at 0.699+/-0.064 and 0.582+/-0.051 Msun by     Bod2005b
                         Boden et al. (2005).                                                            
11222-6119   VOU  47     Aka HRG  58.                                                                    
11224-2713   LDS 350     NLTT 27188/27182                                                        Chm2004 
11225-1028   WHC   9     J 1574.                                                                         
11225-3054   HJ 4428     Herschel's measure moved to HJ 4430 following suggestion by Dawes.      I__1927a
11225-5322   BNS   6     Hen 3-644                                                                       
11226-5134   LDS 351     B is CD-50@5949.                                                                
11230-3054   HJ 4430     Herschel's measure moved to HJ 4430 following suggestion by Dawes.      I__1927a
11231-1020   OL   12     Not found in 1939. Position may be in error                             B__1950c
11237-2831   ARG  25     B is CD-27@8061.                                                                
11238+4307   LDS4093     NLTT 27234/27231                                                        Chm2004 
11239+1032   STF1536     iot Leo = 78 Leo. Mt. Wilson spectral types F3s and F3s. A is a Delta           
                         Scuti-type variable. A small variation in the early RV's was not                
                         confirmed by fairly numerous subsequent observations. From the visual           
                         separations, Baize suggests a subsystem with P = 16 yr.                 Baz1980a
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.67 +/- 1.45, 2.33, and 1.38 Msun, respectively.  Mlk2012 
11239-2319   RST2746     CD-22@8867.                                                                     
11241+3808   RED  23     M4.5 star is ~7" from M8 dwarf 2MASS J11240487+3808054. Distance                
                         estimates for both ~19pc.                                               Red2007a
                         There is a possible brown dwarf companion to 2MASS J11240434+3808108            
                         at 8" separation noted by Reid et al. (2007), but it is single within   Red2007a
                         the AstraLux field of view.                                             Jnn2012 
11244+0620   HJ 2569     Position correction by Heintz.                                          Hei1983a
11245+6807   LDS1260     LDS 1731.                                                                       
11245+3529   OSO  38     G147-050. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
11246+5651   STI2270     Rectilinear solution by Hurowitz et al. (2014).                         USN2014a
11246+2331   LDS5205     LDS6244.                                                                        
                         NLTT 27298/27299                                                        Chm2004 
11247-4718   WFC 113     SWR 111. CPM pair                                                       Skf2004 
11249-0205   EPI   5     EPIC 201324549. Primary is eclipsing binary candidate, period 2.519d.   SJR2016 
11249-1741   HJ  840     gam Crt = 15 Crt                                                                
11250-3200   CHR 242     Aa,Ab: The 0".1 pair CHR 242 has only 1 observation in the WDS,                 
                         unresolved with speckle. Double lines were noted by the GCS. This star          
                         remains a mystery.                                                      Tok2012a
             UC 2133     AB: CPM candidate does not pass photometry test; likely optical.        Tok2013c
11250-5236   RST9003     Previously known as RST 541a. Also known as TDS7851.                            
11251-6044   KRV  37     Classical Cepheid AY Cen.                                                       
11252+1608   HEI 156     There is a third star at 46 deg, 25"                                    Hei1983a
11253+3512   OSO  39     G147-054. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
11254+7817   LDS 920     LDS1732.                                                                        
                         NLTT 27306/27303                                                        Chm2004 
11256+1627   HJ 4433     81 Leo.                                                                         
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             SHY 224     AC: HIP  55765 + HIP  55262.                                                    
             HJ 4433     H 5  61.                                                                MEv2010 
11257-4314   CPO 324     TDS7855.                                                                        
11258-3852   OSO  40     Neither is a common proper motion pair, based on comparison with POSS2          
                         red plates.                                                             Oso2004 
11258-4410   JNN  75     2MASS J11254754-4410267 has a relatively close (~0.55") companion that          
                         is likely physically bound, but so far there is only a single epoch of          
                         data available.                                                         Jnn2012 
11259+6519   GIC  98     LDS2600. G236-068/G236-069.                                                     
                         NLTT 27350/27352                                                        Chm2004 
11261+0114   EPI   6     EPIC 201546283. Primary is candidate planet host star; planet period            
                         6.77d, radius 5.77 Rearth, a 0.07 au.                                   Mtt2015b
11263+1839   ZUC   9     SKF  36.                                                                        
                         Primary is white dwarf PG 1123+189.                                     Zuc1992 
11264+2047   LDS4098     NLTT 27376/27375                                                        Chm2004 
11268+5923   FOX 171     Position of ADS 8161, referred to BD+60@1328.                                   
11268+0301   STF1540     83 Leo = LDS 921. B is BD+03@2503.                                              
                         Hopmann orbit rejected from Fourth Orbit Catalog                        Hop1960a
                         ("period over 4000 years")                                              Wor1983 
                         The C component (mag. 9.9, 90") is also probably physical.              Fin1970b
                         AB: HJL 145.                                                            HJL1986 
                         AB: H 4  13.                                                            MEv2010 
11268-5310   I   883     Spectrum composite; K0III+A2-3V.                                                
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.12 +/- 1.21, 5.03, and 2.88 Msun, respectively.             Mlk2012 
11270-5451   HJ 4436     B is CPD-54@4542.                                                               
11272-1221   KUI  57     kap Crt = 16 Crt                                                                
11272-1539   HU  462     1997.1231: Our reduction does not give the quadrant unambiguously.  We          
                         therefore adopt the quadrant consistent with the latest measure in the          
                         WDS.                                                                    Hor1997 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.65 +/- 0.25, 1.85, and 0.91 Msun, respectively.             Mlk2012 
11272-1604   LDS4100     AB: NLTT 27425/27430                                                    Chm2004 
11274+2042   OSO  41     G120-050. Not a common proper motion pair, based on astrometry and              
                         color                                                                   Oso2004 
11277+4618   STF1541     HJL 146.                                                                HJL1986 
11279+0251   STFA 19     tau Leo = 84 Leo. STTA110. B is BD+03@2505.                                     
                         AB: H 6  12.                                                            MEv2010 
11280-0155   STF3071     Primary is eclipsing binary of Beta Lyr -type, period 1.0143 d.         Zas2012 
11281-2003   TDS7871     RY Crt.                                                                         
11281-6125   COO 269     A is an Algol-type system, MN Cen.                                              
11282+3313   SEI 524     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
11285+0141   EPI   7     EPIC 201577035 = K2-10. Primary is planet host star; planet period              
                         19.31d, radius 3.92 Rearth, a 0.14 au.                                  Mtt2015b
11286-4240   BSO   6     A is a spectroscopic binary.                                                    
11287+6433   GIC  99     LDS2601. G236-072/G236-073.                                                     
                         NLTT 27479/27490                                                        Chm2004 
11287+3224   COU 781     TDS7880.                                                                        
11291+3920   STF1543     57 UMa. A is a spectroscopic binary.                                            
                         AB: H 3  86.                                                            MEv2010 
11291-5848   COO 125     AC: Hipparcos suspected non-single.                                             
11292-1721   H 4 112     H IV 112. S 627.                                                                
11295+3004   TU UMa      Mass of A,B = 0.6 +/- 0.1. 1.98 +/- 0.33 /msun.                         Krv2019a
11296-2428   JC   16     HDO 129 = HDO 130.                                                              
11296-3133   BRT2987     LDS 853.                                                                        
11301+2958   STTA111     LDS 5730. B is BD+30@2164. The primary is the eclipsing pair AW UMa,            
                         P = 0.44d.                                                                      
                         NLTT 27565/27566                                                        Chm2004 
                         Pribulla & Rucinski (2006) estimate the mass of the contact pair at     Pbl2006 
                         1.933 Msun and the minimum mass of the wider component at 0.11 Msun.            
                         HJL 147.                                                                HJL1986 
11303+8102   STF1539     B is BD+81@370.                                                                 
11304-6349   SNA  24     HD 100099 is a 21.6d SB2 (Sana et al. 2011)                             Sna2011a
                         LS 2364.                                                                        
                         The classification is from Garrison et al. (1977 ApJS 35, 111).         Msn1998a
11308+4117   STT 234     One component is SB P = 7.40 d, and the lines of all three stars                
                         appear in the spectrum. The close pair is very probably the visual              
                         primary; the ascending node is identified on that assumption.                   
11308-1046   LDS4108     GWP1596.                                                                        
11308-5849   FIN 187     Spectrum of B: F.                                                               
11309-2012   B  2280     BHA 14.                                                                         
11313+5942   STF1544     B is a spectroscopic binary.                                                    
                         STF1545.                                                                        
                         H N  70.                                                                MEv2010 
11317+1422   WSI 101     HIP 56242. Provisionally designated WSI9107.                            Hrt2008 
                         Aa,Ab: 88 Leo. Aa,Ab could be a 'ghost' binary. Only 1 speckle res.     Tok2014d
             STF1547     AB: HJL 148.                                                            HJL1986 
                         88 Leo.                                                                         
                         AB: NLTT 27657/27656                                                    Chm2004 
                         AB: H 3  51.                                                            MEv2010 
                         AB: B= LTT 13146, X-ray source                                          Tok2014d
11318-2047   TOK 222     Astrometric binary; dm 4.9 mag, period ~ 200y?                          Tok2012b
11318-5927   HJ 4445     omi 1 Cen. A semiregular variable.                                              
11318-6701   GRV1255     Both A and B have approximately the same radial velocity.               Grv2019b
11319+6237   PTT  22     Also known as STI 730.                                                          
11319-3436   ZUC   1     Aa,Ab: Magnitudes in J,H,K by Konacki et al. (2007) based on 2MASS      Kon2007 
                         combined magnitudes plus their flux ratios.  They determine both                
                         components have spectral type M1.5 +/- 0.5; log (Temp) for both is              
                         3.56 +/- 0.01 K, intermediate between temperatures expected for dwarf           
                         and giant stars, thus appropriate for PMS stars. Log (Luminosity) for           
                         Aa and Ab are -0.80 +/- 0.08 and -0.84 +/- 0.08 Lsun, respectively.             
                         Aa,Ab: Schmidt et al. (2008) analyzed all available astrometry and      Sdt2008c
                         concluded TWA 5 exhibited orbital motion, refuting conjecture that              
                         companion was a background object.                                              
             LWR   2     This system has been identified as a member of the TW Hya association           
                         (Kastner et al. 1997 Science 277, 67) and is known as TWA 5. It                 
                         contains a previously known brown dwarf TWA 5B, first suggested by              
                         Lowrance et al. (1999) and later confirmed by e.g. Brandeker et al.     Lwr1999 
                         (2003). The latter also reported the presence of a close companion      Bnk2003 
                         TWA 5Ab at 54 mas from the primary, independently detected by                   
                         Macintosh et al. (2001). We detect TWA 5B in our AstraLux data, but     MBA2001 
                         not TWA 5Ab, which implies that the projected separation was probably           
                         smaller in 2010 than it was in 2000. The orbit of TWA 5Aa/Ab has been           
                         analyzed in detail by Konopacky et al. (2007). Using the orbital        Kon2007 
                         parameters that they determine, we deduce that at epoch 2010.11, the            
                         projected separation should be only about 18 mas, which is well                 
                         consistent with our non-detection of TWA 5Ab. We use the best-fit               
                         total mass of 0.71Msun for TWA 5Aa/Ab from Konopacky et al.             Jnn2012 
                         Kohler et al. (2013) derive new orbits and masses for the young triple          
                         system TWA 5. System mass for the close pair ZUC 1Aa,Ab is 0.90 +/-             
                         0.1 Msun; system mass for the AB pair is 1.1 +/- 0.1 Msun.              Koh2013 
11320-5227   HJ 4446     B is CD-51@5787.                                                                
                         SWR 112. CPM pair                                                       Skf2004 
11321-6357   HJ 4447     B is CPD-63@1914.                                                               
11322+3615   HU 1134     Malkov et al. (2012) derive dynamical and spectroscopic masses                  
                         8.46 +/- 4.04 and 2.63 Msun, respectively.                              Mlk2012 
11323+6105   STT 235     AB. 1979.0369: This measure was incorrectly attributed to ADS 8249 in           
                         McAlister & Hendry (1982).                                              McA1982d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.05 +/- 1.10, 2.34, and 1.10 Msun, respectively.  Mlk2012 
11323-0025   TOK 142     HIP 56282. NOMAD: PM(B)=(0,500), V(B)=16.83 (??). B is physical,                
                         PM(A)=(+43,-158). A is SB without orbit, dRV= 7.4.                      Nrd2004 
                         This is a new triple system.                                            Tok2011a
11323-2916   H 3  96     H III 96.                                                                       
11323-3020   LPR   1     2MASS J11321831-3019518 + 2MASSJ 11321822-3018316. Primary TW Hydrae            
                         Association member TWA 30, companion is distant (~3400) M dwarf.                
                         Spectral types M5 and M4, distance 42 +/- 2 pc, age ~8 Myr.             Lpr2010 
11324+1212   BGH  35     HJL1064.                                                                HJL1986 
11325+5302   HJ 2574     C is a nebula, NGC 3718.                                                        
11326+2419   STF1549     HJL 149.                                                                HJL1986 
11327+0513   GIC 100     LDS 922. G010-032/G010-031.                                                     
11329+5525   A  1593     Primary is HR UMa, an Algol-type eclipsing binary, P = 0.73708d.        Zas2012 
11329-3613   I  1544     A is SB, no orbit                                                       Tok2014d
11330+1319   LDS4114     NLTT 27734/27737                                                        Chm2004 
11330-2327   HDO 130     This system, originally identified as HDO 130, is apparently not the            
                         system observed by Pei1882 in 1868. That measure was later attributed           
                         to 11296-2428JC   16, as was HDO 129.                                           
11330-3151   WSI 102     Aa,Ab: Provisionally designated WSI9108.                                Tok2010 
             HJ 4449     AB: xi Hya                                                                      
11334+5948   LDS1262     NLTT 27746/27749                                                        Chm2004 
11336-4035   I    78     1997.1177: The magnitude difference is listed in the WDS as 0.0. Our            
                         reduction does not give the same quadrant as the latest measure in the          
                         WDS.                                                                    Hor1997 
11343-1531   TOK 143     HIP 56441. NOMAD: PM(B)=(-164,0), V(B)=15.71 (??).                              
                         PM(A)=(-92,+1).                                                         Tok2011a
11347+1648   STF1552     90 Leo. B is a spectroscopic binary.                                    Mlr1952a
                         AB: H 1  27.                                                            MEv2010 
11352-4722   RST 548     A is the semiregular variable V763 Cen.                                         
                         Sinachopoulos et al. (2007) noted an additional component at 131deg,    Sin2007 
                         9".2, dm 6.6mag, but felt it was probably an optical pair and not               
                         worth including as a new entry in the WDS (Gavras, private comm.).              
11354-3232   LTT 4290    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
11358-6301   RST3746     lam Cen                                                                         
11360+7634   LDS1736     BVD 163.                                                                        
11360+7533   KPP3242     Aka TOI 2072.                                                                   
11360-0231   EPI   8     EPIC 201295312. Primary is candidate planet host star; planet period            
                         5.66d, radius 2.16 Rearth, a 0.06 au.                                   Mtt2015b
11362+4843   FAR  35     Primary is white dwarf WD 1133+489.                                     Far2006 
11363+2747   STF1555     A is a SB. A premature visual orbit has been computed                   Wor1956b
                         Quadrant certain in 1951 and 1953. One star is possibly variable.       Baz1954a
                         Data appear equally well fit by rectilinear solution - see catalog.             
             HJ  503     AB,C: According to Le Beau, this pair is physical.                      LBu1990c
11366+5608   STF1553     LDS1265.                                                                        
                         B is SB2, P=4.627y                                                      Tok2014d
11367+2128   STF1558     AB,C: HJL 150.                                                          HJL1986 
11367-0948   GWP1622     Aka tet Crc = 21 Crt.                                                           
11368-1221   BU  456     Prieur et al. (2012) derive a dynamical parallax of 18.6 mas and                
                         (using their orbital elements and the revised Hipparcos parallax of             
                         van Leeuwen 2007 A&A 474, 653) a total mass 1.1 +/- 0.7 Msun.           Pru2012 
11370-3858   DUN 113     B is CD-38@7231.                                                                
11371+6022   LDS2604     NLTT 27985/27990                                                        Chm2004 
11371-0054   EPI   9     EPIC 201403446. Primary is candidate planet host star; planet period            
                         19.15d, radius 2.04 Rearth, a 0.14 au.                                  Mtt2015b
11373-7554   pi Cha      Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
11374+4728   KU   39     A is a BY Dra-type variable, and also a spectroscopic binary. A                 
                         premature visual orbit has been computed.                                       
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
11378+4150   LDS5735     LDS6246.                                                                        
                         NLTT 28037/28036                                                        Chm2004 
11378-4855   HJ 4459     B is CD-48@6669.                                                                
11378-6319   SNA  26     The primary is V1051 Cen, a detached Algol-type eclipsing binary. A             
                         known O+O SB2 (Gies et al. 2002; P~9.7d). Given the distance to the     Gie2002 
                         IC 2944 cluster, this additional component at 61mas is not the                  
                         spectroscopic companion, thus making HD 101131 a hierarchical triple.   Sna2014 
11379+5037   GC 15947    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin & Griffin (1980).                                               Grf1980d
11380-0016   BAL1160     RST 5356.                                                                       
11380-0136   LDS4125     NLTT 28053/28048                                                        Chm2004 
11383-6321   DBR 284     Aka V870 Cen.                                                                   
11383-6322   I   422     Light and radial velocity variable.                                             
                         Primary is eclipsing variable V871 Cen (period 2.0842 day).             Zas2010 
                         This is another complicated multiple system with three visual pairs at          
                         0.36", 1.7", and 9.6". The AB pair further contains an eclipsing                
                         binary (Otero 2007, Open European Journal on Variable Stars 72, 1;              
                         P=2.08d) and a spectroscopic binary with a period of 2.8d (Sana et al.  Sna2011a
                         2011). This brings the number of stars with 10" to six. It is not               
                         currently possible to determine which component of the AB pair is the           
                         eclipsing one and which is the spectroscopic one.                       Sna2014 
11384+6112   LDS2605     SLW 621.                                                                        
11384-6312   HD 101223   IC2944 Tha 49.  Additional similar radial velocities are reported by    Wes1965 
                         Thackeray & Wesselink (1965) and Humphreys (1973 A&AS 9, 85).           Msn1998a
11386+7511   MLR 425     Also known as TDS7973.                                                          
11387+4507   STF1561     AB: Secondary is 23.5d SB1; AB has estimated period of 2100y.           Tok2006 
                         AB: NLTT 28087/28086                                                    Chm2004 
                         AB: H 3  87.                                                            MEv2010 
                         AB: B is SB2, P=23.541d                                                 Tok2014d
                         AC and AE: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         AE, BC: Rectilinear solutions by Friedman et al. (2011).                USN2011a
                         BE: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
11387-1312   KUI  58     AB: iot Crt = 24 Crt                                                            
             UC 2181     AC: CPM candidate does not pass photometry test; likely optical.        Tok2013c
                         AC: The C CPM component at 93" is not on the MS, too "blue".            Tok2014d
11390+0406   GRV1059     SLW 624.                                                                        
11390-0354   EPI  10     EPIC 201208431 = K2-4. Primary is planet host star; planet period               
                         10.00d, radius 2.37 Rearth, a 0.08 au.                                  Mtt2015b
11391+6630   LIE   1     HS 1136+6646 = WD 1136+667. The A component is a hot young DAO white    Lie2006 
                         dwarf plus K7V in a close detached binary. The wider companion is seen          
                         in SDSS and HST/STIS images, and is estimated to be of spectral type            
                         K4-5V. Similar proper motion of the close pair and the companion                
                         during the 3.84 years between images leads the authors to conclude the          
                         companion is probably physical.                                                 
11391+1051   BPM 581     [PM2000] 1012822 + [PM2000] 1012809.                                    Gvr2010 
11391-6326   RSS 268     IC2944 Tha 53.  Additional similar radial velocities of the primary     Wes1965 
                         are reported by Thackeray & Wesselink (1965).                           Msn1998a
11394-3923   DSG  12     V829 Cen.                                                                       
11395+2518   A   678     Slightly elongated, about 263deg, 0".2?                                 Baz1972 
11395-0014   SLN  21     This is from star "A" to QSO "B" so not a double star.                  Dam2020a
11395-0208   CBL 348     GWP1638.                                                                Tob2012b
11395-6524   B  1705     A spectroscopic binary.                                                         
                         GT Mus is one component of this quadruple. One component of the close           
                         visual pair is an SB, with P~61d, and also an RS CVn-type binary. The    .      
                         other is an EB with period ~2.75d.                                      Zas2009 
11396+3125   SEI 526     Primary not seen on POSS plate; may be either variable star or flaw on          
                         AC Potsdam plate.                                                               
11396+1900   STF1565     B is BD+19@2482.                                                                
                         HJL 151.                                                                HJL1986 
11396-2959   SWR 114     CPM pair                                                                Skf2004 
11398-6329   BSO   7     B is CPD-62@2205.                                                               
                         BSO   7B is the optical companion of HD 101436 (Lindroos 1985).         Lnd1985 
                         Both stars were observed and appeared to be single.                     Msn1998a
                         Additional diverse radial velocities for HD 101413 are reported by      Wes1965 
                         Thackeray & Wesselink (1965) and Conti et al. (1977).                   Cti1977 
             SNA  28     Ba,Bb: HD 101413 is a 3 to 6-month period SB2 (Sana et al. 2011), with  Sna2011a
                         the spectroscopic companion being a likely mid-B star. The 54mas                
                         companion is too far away and too bright to be associated with the              
                         spectroscopic companion.                                                Sna2014 
11399-2045   LDS4129     NLTT 28153/28155                                                        Chm2004 
11401-0326   GAU  13     Gauchet calls this HJ 186, but it seems to be another pair.             Gau1926a
11406-0824   TOK  25     A is SB1, P=4.406d                                                      Tok2014d
11406-6234   SNA  29     Aa,Ab: Given the brightness difference and the fact that the combined           
                         spectrum is an O9.2II star, both Aa And Ab are likely late O stars.     Sna2014 
11407+1745   BPM 582     [PM2000] 1013462 + [PM2000] 1013449.                                    Gvr2010 
11408-2056   LDS4134     NLTT 28216/28215                                                        Chm2004 
11410+0341   EPI  11     EPIC 201702477. Primary is candidate planet host star; planet period            
                         40.74d, radius 7.28 Rearth, a 0.22 au.                                  Mtt2015b
11410-6242   B   799     A is the Cepheid UZ Cen.                                                        
11411+3412   STT 574     61 UMa.                                                                         
                         Rectilinear solution by Hurowitz et al. (2014).                         USN2014a
11412+3920   OSO  42     G176-046. AB is a common proper motion pair                             Oso2004 
             LDS4135     AC: NLTT 28236/28208                                                    Chm2004 
11414+5855   ES 2638     LDS2609. B is BD+59@1396.                                                       
                         NLTT 28243/28242                                                        Chm2004 
                         HJL 152.                                                                HJL1986 
11416+3145   BNU   3     Aa,Ab: 62 UMa. B is BD+32@2178.                                                 
                         This system is known to have a variable radial velocity.                Bnu1986 
                         Aa,Ab: Orbit determined by fitting revised Hipparcos intermediate               
                         astrometric data. Derived component masses are 1.31 +/- 0.16 and                
                         1.22 +/- 0.14 Msun.                                                     Ren2010 
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 2.56 +/- 0.30, 2.91, and 1.25 Msun, respectively.  Mlk2012 
             STT 575     AB: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
11417+0543   LDS5738     Aka LDS6247.                                                                    
11421-2321   MUG  14     Primary is HATS-1. Spectral type of comoving secondary estimated as             
                         M0, mass 0.67 Msun.                                                     Mug2014 
11423+2302   LDS 926     NLTT 28297/28298                                                        Chm2004 
11426+0554   EPI  12     EPIC 201828749. Primary is candidate planet host star; planet period            
                         33.52d, radius 3.83 Rearth, a 0.19 au.                                  Mtt2015b
11428-3549   TOK 846     V752 Cen.                                                                       
11431-3601   I  1546     Position angles uncertain, too close. Needs speckle.                            
11432-0330   BRT 435     J 3233.                                                                         
11434+2245   POU3110     Heintz believes HJ 2581 to be identical.                                Hei1983a
11435-5800   MUG   9     Based on astrometry, photometry and H- and K-band spectroscopy,                 
                         Mugrauer et al. (2007) conclude that HD 101930 A and B comprise a       Mug2007 
                         physical pair. The projected separation is 2229 au, which means the             
                         planetary companion to the A component is well within the long-time             
                         stable region.                                                                  
11436+0634   BU  793     AB: EPIC 201862715. Primary hosts an inflated hot Jupiter (WASP-85Ab),          
                         period 1.4786d.                                                         Mtt2015b
             WSP  85     AC: del Valle & Rica (2016) find the star 2MASS J11434596+0635056,              
                         spectral type M2.5V (based on multi-band photometry), appears to have           
                         distance and proper motion similar to WASP-85, and suggest that it              
                         could be a new physical companion.                                      DVG2016c
11437+1331   HJ 2583     B is BD+14@2427.                                                                
11438+4411   ES  123     B is also a 2.2d spectroscopic binary.                                  Tok2019b
11438+1831   BRT2412     HJL 154.                                                                HJL1986 
11441-5332   LDS 360     Typographical error in Luyten's quadrant ("sp")?                        Luy1941 
11441-0448   RST5524     Obviously in rapid motion, but the measures are insufficient to define          
                         the nature of the motion.                                                       
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.56 +/- 0.88, 2.89, and 1.25 Msun, respectively.             Mlk2012 
11443+4032   OSO  43     G122-043. Not a common proper motion pair, based on color and                   
                         comparison with POSS2 red plates.                                       Oso2004 
11445-4539   BRT 803     A likely plate flaw.                                                    Grv2021b
11446-4925   RST9004     Originally published as RST3558a and previously listed in the WDS               
                         under duplicate designation RST3558.                                            
                         Assuming the revised Hipparcos parallax of 20.6 +/- 2.1 mas, Wollert            
                         et al. (2014) find the system mass is 2.6 +/- 0.8 Msun, the semi-major          
                         axis 14.9 +/- 1.6 au. Spectral types at K0 +/- 1 and K5 +/- 1. Some             
                         evidence is found for an unseen third component.                        Wol2014 
11448+1123   J  3234     HJL 155.                                                                HJL1986 
11452+1821   GIC 101     G057-017/G057-015.                                                              
11453+0816   VIG  14     Primary is xi Vir. The optical/physical nature of the faint companion           
                         is undefined.                                                           Vig2012 
11456-6644   HJ 4471     lam Mus                                                                         
             lam Mus     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
11459+1122   J  1017     The measure in 1910 doubtful. No certain measures since.                        
11460+3149   GIC 102     Primary is white dwarf WD 1143+321 = NLTT 28470.                        Far2005b
                         NLTT 28470/28469                                                        Chm2004 
11460+3015   LDS4143     NLTT 28476/28472                                                        Chm2004 
11465-7055   RSS  15     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al. Also known as RSS 272.                        Rss1996 
11466+2231   KER   2     Aa,Ab: RED  12. 2MASSW J1146345+223053                                          
                         HST WFPC2 observations by Reid et al. (2001). Paper includes mass and   Red2001 
                         age estimates, as well as discussion of L dwarf binary frequency and            
                         semimajor axis distribution.                                                    
             ALP  17     AB: Observed in I-band at WIYN in February 2003, but companion not              
                         detected. Ruled out as brown dwarf companion following further                  
                         IRTF/NSFCam H- and methane-band photometry in April 2004.               AlP2007 
             KER   2     Primary is an L3V brown dwarf; LRIS spectrum shows other component is           
                         a background star of much earlier type.                                 Kir1999 
11467-4029   LDS6248     Proper motion -1545 +385.                                                       
                         HIP 57443. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         A is exoplanet host, P=122d                                             Tok2014d
11475+7702   LDS1739     Primary is SB, P=33.776d                                                Tok2014d
11475+2002   SHJ 130     B is BD+20@2651.                                                                
11477+0016   LDS5207     LDS6249.                                                                        
11478+1254   MET  57     Also known as GQ Leo.                                                           
                         Also a spectroscopic binary with uncertain period.                      Tok2019b
11479+0815   CHR 134     4 Vir.                                                                          
                         Aa,Ab: This pair was observed by CHARA 17 times 1987-1998 and resolved  McA1989 
                         once (1987.26, 0.259", note: "uncertain whether real"). Later resolved  WSI2007a
                         by the USNO 26in (2006.31, 0.40").                                      Hrt2009 
             RBR   2     AD: Individual J,H,K magnitudes are calculated from 2MASS combined              
                         magnitudes and AO-derived magnitude differences                         Rbr2005 
             SHJ 131     AB: H 6 113.                                                            MEv2010 
11480+2013   STFB  7     93 Leo = LDS4146. A is a spectroscopic binary and light variable,               
                         spectrum composite; A7V+G5III-IVe. B is BD+21@2357.                             
                         AB: HJL 156.                                                            HJL1986 
                         AB: H 6  80.                                                            MEv2010 
             MKT   7     Visual orbit by Hummel et al. (1995) based on astrometry from Mark III  MkT1995 
                         interferometer. Additional spectroscopic data yield component masses,           
                         luminosities, radii, effective temperatures, and distance.                      
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Hummel et al. (1995).                                                   MkT1995 
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 3.97 +/- 0.25, 4.97, and 1.66 Msun, respectively.  Mlk2012 
11480-6607   GLI 168     LDS 367.                                                                        
                         A 36d spectroscopic solution for the B component has been found         Tok2019g
                         making this a triple system.                                                    
11484-1019   H 6 115     H VI 115. B is BD-09@3368.                                                      
11486+1417   BU  603     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Individual J,H,K magnitudes are calculated from 2MASS combined                  
                         magnitudes and AO-derived magnitude differences                         Rbr2005 
11487-6134   R  9001     Previously known as R   176a.                                                   
11489+1802   LDS5742     LDS6250.                                                                        
11491+1434   BU  604     bet Leo = 94 Leo = Denebola. Possibly variable.                                 
                         Intensity Interferometer Limb-darkened diameter 1.33 +/- 0.10 mas.      HBr1974 
                         NPOI Limb-darkened diameter    1.482 +/- 0.013 mas,                             
                         R =    1.75 (+/- 0.02   )  \rsun,  Teff = 8262 +/-  36 K,                       
                         L =   12.9 +/-   0.1 \lsun.                                             NOI2023 
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
11495+1246   LDS4148     NLTT 28662/28663                                                        Chm2004 
11495-1937   LDS 368     11495-1936DAM  75AB. Other members of 11495-1936 moved to 11495-1937.           
11496+1641   BPM 583     [PM2000] 1017041 + [PM2000] 1017018.                                    Gvr2010 
11498+0557   LDS5743     LDS6251.                                                                        
11498-3816   SWR 117     CPM pair                                                                Skf2004 
11500+3612   GRV 842     HJL 157.                                                                HJL1986 
11501+5024   LDS5208     LDS6252.                                                                        
11502-4951   SWR 118     CPM pair                                                                Skf2004 
11503+3741   HJ  510     AB,C component = LDS5209.                                                       
11503+2519   LDS 928     Also known as LDS6253. It was determined that these two pairs were the          
                         same. LDS 928 was at 11504+2519. The true position is closer to that            
                         of LDS6253, but it was given the discovery designation of the earlier           
                         Luyten number.                                                                  
11504+2626   LDS 927     NLTT 28702/28701                                                        Chm2004 
11507+0146   STT 576     bet Vir = 5 Vir = Zavijava                                                      
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: Rectilinear solution by Friedman et al. (2011).                     USN2011a
                         NPOI Limb-darkened diameter    1.768 +/- 0.070 mas,                             
                         R =    2.08 (+/- 0.08   )  \rsun,  Teff = 5456 +/- 108 K,                       
                         L =    3.4 +/-   0.0 \lsun.                                             NOI2023 
11509-7411   BRR  15     Erroneously listed as BRR   5, a designation already in use.                    
11510+0707   EPI  13     EPIC 201890494. Primary is eclipsing binary candidate, period 2.536d.   SJR2016 
11510-0520   MCA  36     A spectroscopic binary and suspected occultation binary now resolved            
                         by speckle interferometry.                                                      
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Ginestet et al. (1985).                                                 Gin1985 
                         The pair has been resolved 3 times 1980-1994, but unresolved ~35 times  HIP1997d
                         1980-1998. Published astrometric orbits give a period of ~1.3y and an   Jnc2005 
                         inclination near 90deg.                                                 Hrt2009 
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Imbert & Carquillat (2005).                                             Crq2005 
11512+3322   ARG 101     B is BD+34@2263.                                                                
11513+1255   LDS4150     NLTT 28770/28768                                                        Chm2004 
11515+5412   LDS1272     LDS1273. NLTT 28772/28771                                               Chm2004 
11517-3912   HDS1673     V572 Cen.                                                                       
11518-0335   J  1581     Probably variable                                                       J__1962a
11518-0546   CHR  36     This is the variable TY Vir.                                                    
11519+3307   LEP  46     A spectroscopic binary of indeterminate period.                         Tok2019b
11520+0850   STF1575     B is BD+09@2552.                                                                
                         HJL 158.                                                                HJL1986 
                         SHY 581. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         H 4  49.                                                                MEv2010 
11520-0824   HJ  843     J 1580.                                                                 J__1949a
11520-4357   SEE 137     Actually triple. A is a close spectroscopic binary with a P ~ 892d.     Tok2022e
                         The period of AB is estimated as ~900y.                                         
11521+0936   GWP1692     BC: Initially added to WDS incorrectly as AC.                                   
11523+3827   LDS4151     SLW 664.                                                                        
11526-0306   EPI  14     EPIC 201257461. Primary thought to be a planet host star, with planet           
                         period 50.28d, radius 209.52 Rearth, a 0.30 au. Believed to be a                
                         false positive detection, however.                                      Mtt2015b
11528+1526   SHJ 132     AB: HJL 159.                                                            HJL1986 
                         AB: H 5  60.                                                            MEv2010 
11528-0112   EPI  15     EPIC 201384232 = K2-6. Primary is planet host star; planet period               
                         30.940d, radius 2.50 Rearth, a 0.19 au.                                 Mtt2015b
                         B component is the galaxy GAMA 31057.                                           
11529+3050   STF1576     HJL 160.                                                                HJL1986 
                         Additional notes may be found in Schmeidler (1940).                     Scd1940a
11529-3354   HJ 4478     bet Hya. A is an Alpha CVn-type variable.                                       
11532-0722   LDS4154     NLTT 28863/28864                                                        Chm2004 
11532-1540   A  2579     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 59.26 +/- 59.23, 4.05, and 1.45 Msun, respectively.           Mlk2012 
11533+8311   LDS1743     B is BD+83@342.                                                                 
11534-2434   HJ 4479     LDS1274.                                                                        
11535+0552   EPI  16     EPIC 201826968. Primary is eclipsing binary candidate, period 0.367d.   SJR2016 
11537+7345   BU  794     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.31 +/- 1.25, 2.52, and 1.10 Msun, respectively.  Mlk2012 
11537+5032   JMS   3     2MASS J11533966+5032092 + 2MASS J11535018+5035593.                      Jms2008 
11538+5342   SHY 227     AB: HIP  58001 + HIP  61100. A component = gam UMa = Phecda.                    
                         B component = GJ 1160 = A component of 12313+5507.                              
11541+7155   A    75     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.98 +/- 0.64, 2.60, and 1.25 Msun, respectively.             Mlk2012 
11545+2154   UC 2230     CE: Not a CPM pair. The proper motion of the E component was incorrect          
                         (Skiff, private comm.)                                                          
11545+1925   STTA112     LDS 929. B is BD+20@2659.                                                       
                         NLTT 28915/28923                                                        Chm2004 
                         AB: HJL 161.                                                            HJL1986 
                         AB: SHY 229. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
11547-6622   SHY 230     HIP  58085 + HIP  58121.                                                        
11550-6235   BSO  20     B is CPD-61@2779.                                                               
11551+4629   A  1777     65 UMa. The primary is the eclipsing binary DN UMa,                             
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Discrepant 1995.3159 speckle measure found not due to a typographical   Hrt1997 
                         error in theta, following reexamination of original data by authors.            
                         Presumably there was an identification error while pointing telescope,          
                         although no probable match to known close pairs in the vicinity has             
                         been found.                                                                     
             65 UMa      After subtracting out the effects of the 118y AB pair, Zasche et al.            
                         (2012) find a 640d variation, which they attribute to a closer Aa,Ab            
                         pair. The 1.7d eclipsing pair DN UMa, then, is assumed to be Aa1,Aa2.           
                         Their analysis determines a distance 234 +/- 29 pc to the system                
                         (compared with 212 +/- 30 pc from the revised Hipparcos reduction of            
                         van Leeuwen 2007), a and total mass of 8.25 +/- 1.85 Msun. Derived      vlF2007 
                         spectral types, masses, and radii of the components are as follows:             
                             Aa1   A7   1.74 +/- 0.06 Msun   1.86 +/- 0.08 Rsun                          
                             Aa2   A7   1.71     0.06        1.81     0.08                               
                             Ab    A1   2.4      0.4                                                     
                             B          2.4      2.0                                             Zas2012b
             STF1579     STTA113 = STFA 20.                                                              
                         AB,C: H 1  72.                                                          MEv2010 
                         May be a physical septuple: the 1.7d eclipsing pair (2), the 640d               
                         spectroscopic component (+1), the 118y resolved pair A  1777 (+1)               
                         and the wider cpm pair (+1) STF1579AB,D. STF1579AB,C also has similar           
                         proper motion and may be physical and the D component has been split            
                         interferometrically (BAG  46Da,Db).                                             
11551+0313   HD103501    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
11555+7229   MLR 426     Duplicity uncertain.                                                            
11557+1539   H 6  13     H VI 13. 95 Leo. All stars in the field are much more than 90" away.            
                         A is a spectroscopic binary.                                                    
11558+1115   AG  434     No companion seen in 1893 and 1903.                                     IDS1963A
11560+3520   CHR 258     Hipparcos suspected non-single.                                                 
                         Triple system. Spectroscopic orbits of the inner (23-d) and this        Grf2013f
                         more distant 4988-d pair have been determined. Remarkably close to              
                         the initial 15y estimate.                                               Msn1999b
11560+2159   STF1582     HJL 162.                                                                HJL1986 
11560-7701   TOK 145     HIP 58180. A X-ray source RX J1156.0-7700 with small PM(A)=(-45,+1).            
                         B at 13.4" is physical based on CMDs, but the field is crowded, N*=79.  Tok2011a
11561+4533   STF1581     A is a RR Lyrae-type variable. B also variable?                                 
                         Magnitude underestimated in ADS                                         Baz1943b
11563-4546   LDS 373     B is CD-45@7400.                                                                
                         SWR 119. CPM pair                                                       Skf2004 
11566-0437   STF1584     B is BD-03@3206.                                                                
11567-3216   DUN 116     AB = LDS 374. B is CD-31@9364.                                                  
                         AB = SWR 120. CPM pair                                                  Skf2004 
                         HIP 58240. B = HIP 58241. AB is known CPM pair DUN 116 at 19", 82deg.           
                         BC is a new close pair: 3.6" 116deg, dK=5.8, status unknown.            Tok2011a
11568+0521   CHR 220     First detected as an occultation binary by Evans et al.                 Evn1985 
11572+1351   BPM 584     [PM2000] 1020171 + [PM2000] 1020215.                                    Gvr2010 
11572-7922   HUE   3     Aa,Ab:  The primary is T Cha, a weak-lined T Tauri star (spectral type          
                         G8) surrounded by a cold disk. At a distance of 108 +/- 9pc, the                
                         companion detected by Huelamo et al. (2011) is located 6.7 +/- 1.0 au           
                         from the primary, well within the gap in that star's disk.              Hue2011 
             KST   1     AE: Based on optical and X-ray spectroscopy, Kastner et al. conclude            
                         2MASS J11550485-7919108 is a likely CPM companion to the pre-MS                 
                         star/disk system T Cha, with spectral type M3.                          Kst2012 
11578+4518   A  1778     A may be variable.                                                              
11578-7121   HJ 4483     SWR 122. CPM pair                                                       Skf2004 
11580+6520   LDS2620     NLTT 29095/29094                                                        Chm2004 
11581-2930   LDS 375     NLTT 29109/29108                                                        Chm2004 
11582-1045   J  2084     RST 3765. BRT.                                                                  
11582-1120   LDS4162     GWP1719.                                                                        
11583+3338   LDS5210     LDS6254.                                                                        
11585+3811   LDS5211     LDS6255.                                                                        
11585-2350   RST3767     Ma,Mb = 0.864 +/- 0.031, 0.828 +/- 0.030 \msun.                         GmJ2022 
11585-4155   LDS6256     HIP 58401. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
11589-2555   I   510     Too close. Duplicity doubtful, and/or rapid motion. Needs speckle.              
11594-4219   HJ 4485     A is CPD-41@5660. B is CPD-41@5659.                                             
11596-7813   HJ 4486     eps Cha.                                                                        
                         In eps Cha Association. 12001-7812 is also a member.                            
                         11596-7813C = 12001-7812A.                                                      
11598-0315   CBL 365     GWP1724.                                                                Tob2012b
11599+1144   BPM 585     [PM2000] 1021250 + [PM2000] 1021230.                                    Gvr2010 
12001+7039   STT 242     C is BD+71@595 according to ADS, but A and C may be reversed.                   
12001+4107   LDS5212     LDS6257.                                                                        
12001-7812   FGL   2     DX Cha. Hen 3-741. Noted as possible binary (separation > 0".040) by            
                         Baines et al. (2006)                                                    Bns2006 
                         In eps Cha Association. 11596-7813 is also a member.                            
                         11596-7813C = 12001-7812A.                                                      
                         B, C, D, and E components were resolved by Feigelson et al. (2003)      Fgl2003 
                         using Chandra ACIS-I (Advanced CCD Imaging Spectrometer Imager).                
                         Additional wide components G, H, I, J, and K, as well as closer F               
                         companion were resolved by Grady et al (2004) using data from HST/STIS  Gry2004 
                         and VLT/NACO. Their theta values for AD and AE appear to be in error;           
                         correct values are perhaps 180-71=109deg and 180-74=106deg?                     
                         Grady et al. provided no relative astrometry for the H, I, J, and K             
                         companions. Coarse values were extracted by the cataloguer using                
                         Aladin, based on their Figure 4.                                                
12002+8700   STF1583     STT 238. B is BD+87@100.                                                        
12002+3644   STTA114     B is BD+37@2239.                                                                
12003-3552   SWR 123     CPM pair                                                                Skf2004 
12005-0433   EGN  13     Pair bound. B component is likely an M2.5-M4.5 dwarf with mass 0.23             
                         +/- 0.01 Msun.                                                          Egn2007 
12006+6911   A  1088     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 21.73 +/- 14.44, 4.11, and 1.35 Msun, respectively.           Mlk2012 
12007+2051   BDK   5     G 121-42 + 2MASS J12003292+2048513. Distance 30 +14/-7 pc for primary,          
                         26 +/- 3 pc for secondary. Estimated age of system 4-5 Gyr. Mass of             
                         secondary estimated at 0.085-0.103 Msun.                                Fah2010 
12007-1027   SCP   1     Schnupp et al. (2010) determine spectral types G8-K0IV and M4V, masses          
                         1.01 and 0.21 +0.03/-0.02 Msun for the two components.                  Scp2010 
12009+0637   pi Vir      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Abt (1965).                                                             AbH1965 
12015-0023   STF1591     STTA115. B is BD+00@2877.                                                       
12016+4731   KZA  24     30' error in WDS designation                                                    
12016-6000   WFC 121     JAW  30.                                                                        
12018-3439   I   215     A premature orbit has been computed. The motion is nearly rectilinear,          
                         but the sizable proper motion proves the physical nature.                       
                         The position given by Bespalov is that of HLD 114.                      Bsp1961 
                         The primary is a double-lined SB, now SB3. Tokovinin et al. (2014)              
                         derived a solution (P=148.14d, e=0.430) and estimated the angular               
                         separation at 13 mas, meaning it should be resolvable by speckle on an          
                         8m telescope. They also revised the orbit of the AB pair. Estimated             
                         masses for Aa, Ab, and B are all similar: 1.15, 1.16, and 1.12 Msun.    Tok2015a
12019+0006   STTA116     B is BD+00@2881.                                                                
12019-4617   TDS8181     KZ Cen.                                                                         
12021+4303   FOR   1     67 UMa. A is a Delta Scuti-type variable, DP UMa.                               
                         Position of B (+43@2182): 12 02.5 +43 05.                                       
12023-8538   HJ 4490     B is CPD-84@372.                                                                
12025+2145   HO  535     Despite the linear solution, proper motion and parallax favor a         Grv2020a
                         physical connection. Long period and/or high eccentricity possible.             
12025+1646   OSO  44     LHS2500. Not a common proper motion pair, based on astrometry and               
                         color.                                                                  Oso2004 
12027-1043   SHY 588     AC: HIP  58722 + HIP  58751.                                                    
12028+4205   BFR   7     NLTT 29392 + 2MASS J12025009+4204531. Baron et al. (2015) estimate              
                         spectral types M6.0 +/- 0.5 and L0.0 +/- 0.5, distances 33 +2/-16 and           
                         38 +2/-11 pc, masses 0.102-0.133 and 0.074-0.081 Msun.                  BFr2015 
12028+2450   HDS1693     Suspected non-single.                                                   Hor2002b
12029+0004   GRV1068     Aka GWP1737.                                                                    
12029-1908   B  2536     J 1602.                                                                         
12030-6319   CPO  55     the 1 Cru. A is a spectroscopic binary.                                         
12031+4719   OSO  45     G122-069. Not a common proper motion pair, based on astrometry and              
                         color.                                                                  Oso2004 
12033+2902   LDS1275     AB: NLTT 29413/29414                                                    Chm2004 
12036+7932   LDS1746     CBL 553. The pair was long lost, due to a 1deg error in the published           
                         declination, until its rediscovery by Caballero (2012).                 Cbl2012b
12036-3901   SEE 143     89 Cen.                                                                         
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.31 +/- 1.26, 2.46, and 1.13 Msun, respectively.             Mlk2012 
12038-4407   HJ 4491     LDS 380. B is CD-43@7447.                                                       
                         SHY 589. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
12039+4257   LDS4174     NLTT 29456/29454                                                        Chm2004 
12040+0321   ENG  46     B is BD+04@2568.                                                                
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
12042+2407   A   682     A close approach took place from about 1960-1975.                               
12043+2128   STF1596     2 Com. A spectroscopic binary.                                                  
                         H 2  47.                                                                MEv2010 
12047-0546   RST4492     A is the semiregular variable RX Vir.                                           
12048-4003   RST1641     CPD-39@5381.                                                                    
12048-6200   DUN 117     B is CPD-61@2935.                                                               
12048-6704   DON1095     CD-66@1160.                                                                     
12049+1729   LEP  49     NI   29.                                                                        
12049+0910   STF1597     B is BD+09@2580.                                                                
12051+1933   GIC 103     LDS5748. G121-052/G121-053.                                                     
                         NLTT 29534/29540                                                        Chm2004 
12051-6111   FIN 421     The composite spectrum is unlikely to refer to B.                               
12054-2636   RST2777     Motion direct, companion optical.                                               
                         HIP 58962. See Allen et al. (2000) for information on metallicity,      AlC2000 
             LDS 383     age, galactic orbital parameters, etc.                                          
                         AC: NLTT 29556/29553                                                    Chm2004 
12056+6848   STF1599     Djurkovic measured component Ee: 70@, 0.2", 8-8,                                
                         but van den Bos found this round in 1958.                                       
12056+5659   A  1358     Aka HDS1700.                                                                    
12058+5355   CBL  52     Also known as DAL  43.                                                          
12058-1853   WNO  54     GJ 9387 + NLTT 29580. CPM pair.                                         Mkr2008 
                         A spectroscopic binary of indeterminate period.                         Tok2019b
12058-6934   GS Mus      Harmanec (1987 Bull. Astron. Inst. Czech. 38, 283) gives a preliminary          
                         orbit with P = 1.74 d and K = 12.4 km/sec.  The same period and its             
                         double also appear in photometry (van Genderen et al. 1989 A&A 213,             
                         161), so the radial velocity variations may be related to pulsation             
                         instead of orbital motion.  The radial velocity variations are also             
                         discussed by Walborn et al. (1980 PASP 92, 284) and Levato et al.       Lev1988 
                         (1988).                                                                 Msn1998a
12059-4951   HJ 4494     CPD-49@4827.                                                                    
                         AB = SWR 124. CPM pair.                                                         
                         Third component 24" N, CPD-49 4827, is not CPM                          Skf2004 
12060+6842   STF3123     AB: Additional notes may be found in Fu et al. (1997).                  McA1997 
                         Star C (mag. 15, 3") is probably physical.                                      
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.51 +/- 0.88, 3.36, and 1.17 Msun, respectively.  Mlk2012 
12060+2312   WSI 103     MS Com.                                                                         
12061+7022   A    76     LDS1748. B is BD+71@603.                                                        
                         AB: HJL 163.                                                            HJL1986 
12061-3258   HJ 4495     HIP 59021. Both components A,B are above the MS by 1.5 mag. Wrong       Tok2011a
                         parallax? The photometric parallax would be ~40 mas. See Holmberg et    Nrd2009 
                         al. (2009) for improved distance. Planet host?                          Nid2002 
                         AB: B is SB2, P=148.26d. A is SB and possible astrometric binary,       Tok2010c
                         although not resolved with NICI (Tokovinin et al. 2010)                 Tok2014d
12062-2002   B  1714     A rapid binary, angles and period uncertain.                                    
12063+5243   SKF2827     Superposed on west side of galaxy NGC 4102. Pair first noticed by       Skf2017f
                         Steve Gottlieb.                                                                 
12064-1315   JNN  77     Due to the small separation (~0.42") of the companion detected in the           
                         AstraLux images, it is likely a physical companion, although common             
                         proper motion has not yet been tested.                                  Jnn2012 
                         Bowler et al. (2015) confirm the physical nature and detect orbital             
                         motion. Riaz et al. (2006 AJ 132, 866) identify the pair as                     
                         chromospherically active.                                               Bwl2015 
12064-4858   BRT 805     CPD-48@4508.                                                                    
12064-6543   FIN 367     Composite spectrum; G8-K0III+A3.                                                
                         Aa,Ab: Docobo & Andrade (2013) derive a dynamical parallax of 8.11 +/-          
                         0.42 mas and component masses 2.0 +/- 0.5 and 2.0 +/- 0.1 Msun. See             
                         paper for extensive notes on this system.                               Doc2013d
12066-3752   HJ 4500     B is CD-37@7665.                                                                
12067-6114   JAW  32     Also known as R    187.                                                         
12068+4450   FAR  13     BC: Primary is white dwarf WD 1204+450.                                 Far2005b
12069+7008   SKF 237     Aside from the spatially resolved companion, the primary in the 2MASS           
                         J1206557+700749 system is a known spectroscopic binary with a                   
                         semi-major axis less than 0.03 au. This is well consistent with our             
                         AstraLux data, where the primary is significantly brighter than the             
                         secondary, despite having about equal spectral type. Hence, the system          
                         is a triple in reality.                                                 Jnn2012 
12069-6437   HJ 4501     eta Cru. A is a spectroscopic binary.                                           
12071+6905   STF1602     The A component is a spectroscopic triple, P = 3.87d and 6.5y.                  
12073+4306   HJ 2596     Burnham measured a separation of 224.8" at approximately the same       Bu_1913 
                         position angle (239.3) on 1911.22 to NGC 4111 with the 40".                     
12073-7338   NZO  27     Not found by Heintz at IDS position.                                    Hei1990b
12075+1302   LDS4179     HIP 59126. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 29665/29661                                                        Chm2004 
12076-3933   CVN  12     Relative astrometry from Chauvin et al. (2004) was slightly modified    Cvn2004 
                         by Chauvin et al. (2005).                                               Cvn2005b
             SON   1     AC: C component is a field star.                                        Son2006 
12081+5528   STF1603     LDS1278. B is BD+56@1569.                                                       
                         HJL 164.                                                                HJL1986 
                         H 4 108.                                                                MEv2010 
12082+3227   HJ  844     SEI 528.                                                                Nsn2017b
12084-5043   JC    2     A: del Cen. Both A and B are Be stars.                                          
                         B: CD-49 6813. B is the variable V863 Cen.                                      
             MLD   1     Aa,Ab: A component was resolved in K-band using the A0-K0-G1 and        Mld2008 
                         E0-G0-H0 baselines with VLTI/AMBER. The magnitude difference in K was           
                         2.89 +/- 0.16 mag.                                                              
12088-4023   Anon        EQ 1206-4006                                                                    
                         ID as EQ 1206-4006 uncertain; based on Simbad search using epoch-1950           
                         coordinates 120613-400627 from White et al. (1991).                     Whi1991 
12089+2147   LDS 930     G059-001. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
12091-7847   SHY 592     HIP  59243 + HIP  58490.                                                        
12092+1450   TOK 148     HIP 59250.                                                                      
12093-8459   R   188     Also appears to be R   182.                                                     
12094-3409   RST2782     Spectrum: G5/6III/IV.                                                           
12094-5127   I  1218     AC = SWR 126. CPM pair                                                  Skf2004 
12094-6349   HRG  74     Pretty pair. Three distant companions.                                  I__1917a
12095+3838   MET   8     Metchev & Hillenbrand say the pair is probably optical, based on                
                         proximity.                                                              Met2004b
12095-1151   STF1604     AB: Mt. Wilson spectral types are G2 and K8. A is a spectroscopic               
                         binary, and slightly variable. Large relative proper motion, coupled            
                         with the fact that the C component is brighter than B, has led to some          
                         confusion in identification of components.                                      
                         AB: NLTT 29769/29772                                                    Chm2004 
                         HIP 59272.                                                              Tok2011a
                         BC: Rectilinear solution by Friedman et al. (2012).                     USN2012a
12099-1004   LIM   2     2MASS J12095613-1004008. T dwarf, spectral types estimated by Liu et    LiM2010 
                         el. (2010) at T2.0 +/-  0.5 and T7.5 +/- 0.5. Photometric distance 21           
                         +/- 4 pc. Possible masses and effective temperatures are determined             
                         for a range of age estimates.                                                   
12101+0526   TOK 282     AC: 12100+0527 TOK 282 and 12101+0526 WOR  22 found to share same               
                         primary; systems merged.                                                        
12101-4334   CPO  56     B is CD-42@7455.                                                                
12102+1438   BPM 586     [PM2000] 1025354 + [PM2000] 1025384.                                    Gvr2010 
12103-0627   HJ 1213     LDS 387.                                                                        
12105+1649   CHR 135     3 Com.                                                                          
12108+3953   STF1606     A: Preliminary orbit by van der Wiele (1974) calculated to fit          vdW1974 
                         perturbations seen to long-period orbit.                                        
12110+8143   SHJ 136     BDS 6074, STTA117 = STTA118. B is BD+82@357.                                    
12110+1704   BPM 587     [PM2000] 1025639 + [PM2000] 1025679.                                    Gvr2010 
12111-5302   HU 1604     Ma,Mb = 1.045 +/- 0.042, 0.978 +/- 0.039 \msun.                         GmJ2022 
12113+3316   HJ 2600     LDS 932.                                                                        
12113-1958   LDS 390     NLTT 29876/29879                                                        Chm2004 
12114+4334   LDS4186     B is BD+44@2169.                                                                
                         A, B, and C are NLTT 29895, 29881, and 29896. B and C are below MS in           
                         (K,V-K) and to the left in (J,J-K). Sub-dwarfs?                         Tok2014d
12114-1647   S   634     A 211.6d spectroscopic solution for the A component has been found      Tok2019g
                         making this a triple system.                                                    
12114-6057   RST4493     Spectral type B5?                                                               
12115+5325   STF1608     AB: LDS1284. Mt. Wilson spectral types are K2 and G9.                           
                         HJL 165.                                                                HJL1986 
             SHY 233     AC: HIP  59432 + HIP  60121.                                                    
12118+2400   LDS6258     AB: SAND 26.                                                                    
             LDS5749     AC: Assignment of LDS6258 and 5749 as AB and AC pairs is uncertain.             
12118+2319   GC 16657    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin (1985).  Cluster Melotte 111 #AV442.                            Grf1985a
12119+2552   4 Com       Hipparcos astrometric solution adopts some elements from the orbits of  HIP1997d
                         Harper (1930) and Harper (1930).                                        Hrp1930a
                         Cluster Melotte 111 #AV448.                                             Hrp1930b
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Harper (1930).                                                          Hrp1930a
12120+3850   LDS4188     SLW 693.                                                                        
12121+2459   LAS   4     Lasgoity (2014) determines that the two components of the pair in the           
                         region of the Coma Berenice star cluster share common proper motion.            
                         He derives spectral types of M3.5V for both components, and estimates           
                         distance, mass, and radius for both stars.                              Las2014a
12123+5429   VYS   5     LDS5213.                                                                        
                         NLTT 29950/29949                                                        Chm2004 
12123-0621   LDS4189     NLTT 29948/29967                                                        Chm2004 
12125+2509   LAS   5     Lasgoity (2014) determines that the two components of the pair in the           
                         region of the Coma Berenice star cluster share common proper motion.            
                         He derives spectral types of K0V and K3V for the two components, and            
                         estimates distance, mass, and radius for both stars.                    Las2014a
12125-0305   LPM 416     HIP 59532. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         No companions detected with NACO (Eggenberger et al. 2007).             Egn2007 
12127+1631   BPM 588     [PM2000] 1026292 + [PM2000] 1026283.                                    Gvr2010 
12128-7009   EVS  17     Primary is the Cepheid S Mus.                                           Evs2016a
             GAA  13     Aa,Ab : Cepheid with a period of 9.66d. Distance = 858 +/- 17 pc.       GaA2019b
                         M_Aa, M_Ab = 4.44 +/- 0.91, 3.98 +/- 0.21 /msun.                                
12129-4454   HJ 4507     B is CD-44@7860.                                                                
12130+2146   JNN 277     Estimated age 1000-10000 Myr; masses 0.24 +/- 0.08 and 0.12 +/- 0.03            
                         Msun; a ~4.7 au.                                                        Jnn2014 
12135-4847   CBL 142     AC: Secondary of 12135-4848 CBL 142 found to be primary of 12135-4847           
                         TDS8273; systems merged, with quadrant of CBL 142 flipped 180deg.               
12137-1123   JNN  78     LP 734-84.                                                                      
                         A companion to 2MASS J12134173-1122405 is detected in the AstraLux              
                         images which has not yet been tested for common proper motion, but the          
                         color and brightness is consistent with the expectation for a                   
                         physically bound companion.                                             Jnn2012 
12138+4643   A  1849     Rectilinear solution by Rica & Zirm (2012).                             FMR2012i
12140-4543   RMK  14     A is a spectroscopic binary.                                                    
12141+3247   STF1615     B is a spectroscopic binary.                                                    
                         AB: HJL 166.                                                            HJL1986 
12143+1149   HU 1137     A is a W UMa-type system, AH Vir.                                               
                         Pribulla & Rucinski (2006) estimate the mass of the contact pair at     Pbl2006 
                         1.900 Msun and the minimum mass of the wider component at 0.65 Msun.            
12143-0543   HJ  203     A is the Delta Scuti-type variable FG Vir.                                      
12145+0847   STF1616     The declination differences between A and BD+09@2600 have been                  
                         measured. See ADS.                                                      A__1932a
                         AC: HJL 167.                                                            HJL1986 
                         AB: H 4 114.                                                            MEv2010 
12148-5547   HJ 4508     B is CPD-55@4937.                                                               
             SHY 597     AC: HIP  59716 + HIP  59960.                                                    
             SHY 582     AD: HIP  59716 + HIP  57950.                                                    
12151-0715   STF1619     AB: NLTT 30106/30107                                                    Chm2004 
                         C is BD-06@3533.                                                                
                         A rectilinear solution to AB gives a poor fit, due to slight apparent           
                         curvature suggesting very long-period orbital motion.                           
                         AB: The AB pair is comprised of a K0V and a K1V star, at a distance of          
                         35.19 +/- 0.74pc. The C component is not a physical companion. Rica et          
                         al. (2017) derive a combined spectroscopic/astrometric orbit of AB,             
                         finding a period of 4800 years and a separation of 345au. The orbit is          
                         perturbed by a circumprimary planet of mass 9.6 Mjup, previously                
                         discovered through radial velocity variations (Mayor et al., 2011 A&A           
                         submitted, arXiv:1109.2497M)                                            FMR2017 
12152-1019   BUP 139     Proper motion of A +036 -1016.                                                  
                         A: Hipparcos astrometric solution assumed circular orbit (e = omega     HIP1997d
                         = 0). Spectroscopic solution to this astrometric pair given by Griffin  Grf2013a
                         (2013). Periods match "tolerably well," other common elements less so.          
                         A: Ren & Fu (2013) calculated an astrometric orbit, combining                   
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Carney et al. (2001). They derived component masses 1.09 and 0.48 Msun  Crn2001 
                         and an estimated semimajor axis of 91.99 mas.                           Ren2013 
12154+5702   BLL  29     69 UMa = del UMa = Megrez. Smyth's quoted separation is difference in   Smy1844 
                         RA only.                                                                        
12158-1733   RBR   5     = gam Crv = Gienah                                                              
                         Found to be a common proper motion companion.                           Jnn2011b
                         Intensity Interferometer Limb-darkened diameter 0.75 +/- 0.06 mas.      HBr1974 
12158-2321   BU  920     Bespalov orbit rejected from Fourth Orbit Catalog                       Bsp1961 
                         ("orbit completely faulty and irreparable")                             Wor1983 
                         Rica (2012) derived a dynamical parallax of 15.6 mas (compared with     FMR2012g
                         14.37 +/- 0.71 mas from Hipparcos) and a mass sum (using the Hipparcos          
                         parallax) of 3.60 +/- 0.93 Msun.                                                
12159-4417   SWR 128     CPM pair                                                                Skf2004 
12160+4807   HU  736     Value of Omega inadvertently copied as omega as well by Baize (1993).   Baz1993b
12160+0538   STF1621     Additional notes may be found in Baize (1948) and                       Baz1948b
                         Couteau (1955).                                                         Cou1955a
                         One component probably has variable RV (Wilson 1967, AJ, 72, 905).              
                         Indeterminate (long) period, useable a^3/P^2. Poor Hipparcos parallax.  Sod1999 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
12161+4040   STF1622     2 CVn. A is a spectroscopic binary.                                             
                         H 3  85.                                                                MEv2010 
12162+8008   STF1625     B is BD+80@380.                                                                 
12162+0443   STF1623     HJL 168.                                                                HJL1986 
12163+4057   FMR 103     BC: Primary of 12166+4058 FMR 103 found to be secondary of LDS4198;             
                         systems merged.                                                                 
12165+3304   CHR  37     A Delta Scuti-type variable and long-period (1300d) SB.                         
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin (1984).                                                         Grf1984a
                         A spectroscopic orbit with a period of 1300 days was determined by              
                         Christie (1936 ApJ, 83, 433). The many negative results listed here             
                         may be due to a large or variable magnitude difference.                         
12166+1200   BPM 589     [PM2000] 1027880 + [PM2000] 1027935.                                    Gvr2010 
12166-6312   SHY 595     HIP  59865 + HIP  59913.                                                        
12169+0258   LDS 935     LDS6259.                                                                        
12169-2228   LDS 399     NLTT 30204/30203                                                        Chm2004 
12171-6542   SHY 596     HIP  59898 + HIP  60183.                                                        
12176+3205   LDS1288     Also known as LDS6260.                                                          
                         NLTT 30242/30241                                                        Chm2004 
12176+1427   DEA  48     AB + TOK 399Aa,Ab: HIP 59933 has a variable RV according to GCS. The            
                         32mas separation corresponds to an orbital period of ~2yr. However,             
                         the separations in the y and I filters are somewhat discordant;                 
                         further confirmation is needed.                                         Tok2015c
12177-6410   JNN  79     The two targets 2MASS J12173945-6409418 and J12174012-6409389 are               
                         physically bound, as shown by common proper motion analysis. However,           
                         this means that one of the targets likely has an error in the Riaz et           
                         al. (2006) spectral type determination, since J12174012-6409389 is      Ria2006 
                         classified as M2 but is fainter than J12174012-6409389, which is                
                         classified as M3.5. The fact that J12174012-6409389 is fainter holds            
                         true both in 2MASS and in the AstraLux images. Both components are              
                         resolved as close binaries with AstraLux, so we consider it a strong            
                         candidate for a quadruple system, with J12173945-6409418A as the                
                         primary. Concerning which spectral type determination is incorrect, we          
                         consider that it is more likely that J12174012-6409389 is mis-                  
                         classified, as the flux ratio to the close companion is closer to               
                         unity than in the J12174012-6409389 case. We thus set the spectral              
                         type of J12174012-6409389A to M3+/-1, and determine the other spectral          
                         types on the basis of flux ratios. Component Bb is not visible in the           
                         i' data, but becomes visible in z' thanks to the higher Strehl ratio            
                         and intrinsic brightness of the component. A fifth object is visible            
                         in the field, but its color reveals it to be a likely background star.  Jnn2012 
12179+1627   LIM   4     Liu et al. (2012) derive near-IR spectral types of T9 +/- 0.5 and               
                         Y0 +/- 0.5. At a derived photometric distance of 10.5 +/- 1.7 pc, the           
                         two stars are separated by 8.0 +/- 1.3 au. Various evolutionary models          
                         yield masses of 11.5-14.4 Mjup for the primary, 5.5-8.3 Mjup for the            
                         secondary.                                                              LiM2012 
                         Based on resolved IR spectroscopy (0.9-2.5micron), Leggett et al.               
                         (2014) derive spectral types T8.5 and Y0-Y0.5 for this brown dwarf              
                         pair. Assuming an age range 4-8Gyr, they also estimate:                         
                             Teff   = 550-600          and 450K,                                         
                             mass   = 30+/-5           and 22+/-2 Mjup,                                  
                             radius = 0.091 +/- 0.004  and 0.096 +/- 0.003 Rsun,                         
                             log g  = 5.0 +/- 0.1      and 4.8 +/- 0.1                           Leg2014 
12179-5559   BYV   1     Bailey et al. (2014) derive spectral types F5V and L2.5, and estimate           
                         masses (1.5 +/- 0.10 Msun, 11 +/- 2 Mjup) and luminosities (log L/Lsun          
                         = 0.75 +/- 0.06 and -3.64 +/- 0.08). Distance to the system is 92 +/-           
                         6 pc, age is 13 +/- 2 Myr.                                              ByV2014 
12180-1456   RST3783     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Additional notes may be found in van den Bos (1963).                    B__1963b
                         Rectilinear solution by Hurowitz et al. (2014).                         USN2014a
12182+0515   HJ 2609     C is a nebula, HJ 1178.                                                         
12182-0357   STF1627     B is BD-03@3262.                                                                
                         H N  22.                                                                MEv2010 
12183-6317   HDS1734     SU Cru.                                                                         
12184-6400   HJ 4512     zet Cru                                                                         
12187+1148   STF1628     BDS 6116, HJ 1216 same star.                                                    
12189-2130   LDS 403     NLTT 30297/30298                                                        Chm2004 
12190+0555   GIC 105     G012-032/G012-031.                                                              
                         NLTT 30312/30313                                                        Chm2004 
12190+0005   GRV1075     SLW 709.                                                                        
12190-3318   HJ 4513     B is CD-32@8628.                                                                
12191+1036   BPM 590     [PM2000] 1028960 + [PM2000] 1028910.                                    Gvr2010 
12192-0319   TOK 283     Secondary appears to be a WD, mass estimated at 0.6 Msun.               Mug2014 
                         A is exoplanet host, P=48.05d.                                          Tok2014d
12194+1744   A  2059     Rectilinear solution by Rica & Zirm (2012).                             FMR2012i
12195+6232   BRT3377     A likely plate flaw.                                                    Grv2021b
12195+2809   LEP  53     HJL1068.                                                                HJL1986 
                         B is SB1, RV=+17.97. RV(A)=-9.80.                                       Tok2014d
12196-4642   SWR 130     CPM pair                                                                Skf2004 
12199-0040   MCA  37     eta Vir = 15 Vir = Zaniah. A spectroscopic and occultation binary now           
                         resolved by speckle interferometry.                                             
                         Observed parallax corroborates closely the orbital value given by               
                         Hartkopf et al. (1992). Primary is 72d SB2 (#718 in Batten et al.,      Hrt1992a
                         1989). This is not the SB2 because the observed angular separations     Bte1989 
                         are much larger than the 12 mas maximum predicted by Halbwachs (1981)   HJL1981 
                         from the spectroscopic elements. See discussion in Balega et al.        Bag1984b
                         (1984), who give preliminary orbital elements based entirely on                 
                         speckle observations.                                                           
                         1985.2053, 1985.2491: These measures agree well with the preliminary            
                         orbit of Balega et al. (1984), who adopted a period of 13 years. The            
                         orbit proposed by Tokovinin (1984) with P = 9.8 years fails to fit the  Tok1984 
                         speckle observations.                                                   Bnu1986 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         A new speckle/spectroscopic orbit of the early A type triple system             
                         eta Vir has been determined by Hartkopf et al. (1992).                  Hrt1992a
                         Martin et al. (1998) derive component masses 6.009 +/- 2.164 and                
                         0.673 +/- 0.800 Msun.                                                   Mig1998 
12201+1351   BU   27     A is variable.                                                                  
12201-6132   TOB 148     Also known as JAW  34.                                                          
12202+3754   STF1632     A is a spectroscopic binary.                                                    
                         HJL 169.                                                                HJL1986 
                         H N  52.                                                                MEv2010 
12203+2637   PIN   6     Primary is Melotte 111 AV 1113, a variable star.                                
12203+0319   BUP 141     16 Vir.                                                                         
12206-2213   BU 1245     zet Crv. HDO 132. A is a spectroscopic binary.                                  
             BU  605     CD: Rectilinear solution by Rica & Zirm (2012).                         FMR2012i
12207+2703   STF1633     LDS1294.                                                                        
                         H N  31.                                                                MEv2010 
12207+1748   HO   52     11 Com.                                                                         
                         CHARA Array Limb-darkened diameter 1.651 +/- 0.016 mas,                 CIA2014b
                         R = 15.781  +/- 0.3444 \rsun, T = 4705 +/-  24 K,                               
                         L = 109.51   +/- 4.3256 \lsun.                                                  
12208+2546   HJ  517     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
12211+4927   FAR  36     Primary is white dwarf WD 1218+497.                                     Far2006 
12213-6217   EVS  18     Primary is the Cepheid T Cru.                                           Evs2016a
12214+1223   LDS1295     BC: LDS6261. Erroneously listed as AC pair.                                     
12215+3038   GIC 106     LDS1296. G148-047/G148-048.                                                     
                         NLTT 30450/30451                                                        Chm2004 
12215-2413   HWE  26     HDO 133                                                                         
12216-2716   B   227     Motion direct.                                                                  
12219+2833   LDS1300     LDS5214.                                                                        
12221-6731   HDO 215     zet 2 Mus                                                                       
12222+7315   TOK  26     Visual pair has estimated period 6800y.                                 Tok2006 
                         A is SB2, P=5.415d. AB not confirmed by RoboAO, but B is seen on J and          
                         K frames, seems to be real.                                             Tok2014d
12222+5805   WNC   4     Aka Messier 40. Definitively non-physical.                              Nug2002 
12222-3453   SWR 132     CPM pair                                                                Skf2004 
12223+3644   DEA  78     NLTT 30510 + 2MASS J12221837+3643485. Baron et al. (2015) estimate              
                         spectral types M3 +/- 1 and L0, distances 45 +47/-23 and 70 +/-10 pc,           
                         masses 0.377-0.431 and 0.074-0.081 Msun.                                BFr2015 
12225+2551   SHJ 143     12 Com. A is a spectroscopic binary. Spectrum composite: G0III-IV+A3V           
                         AC: H 5 121.                                                            MEv2010 
             CIA  52     Aa,Ab : Mass of Aa = 2.64 +/- 0.07 /msun, Ab = 2.10 +/- 0.03 /msun.     CIA2023b
             SMR  57     Aka LAS   6. Lasgoity (2014) determines that the two components of the          
                         pair in the region of the Coma Berenice star cluster share common               
                         proper motion. He derives spectral types of F5V and K5V for the two             
                         components, and estimates distance, mass, and radius for both stars.            
                         The primary is the D component of 12225+2551ARN   6AD. These stars show         
                         very different proper motions than any of the components of 12225+2551,         
                         however, suggesting that ARN 6AD just an optical double linking the             
                         two systems.                                                            Las2014a
12225+0518   STF1636     17 Vir. B may be variable.                                                      
                         H 4  50.                                                                MEv2010 
12226-4920   SEE 153     Aka FAL  38.                                                                    
12228-0405   BWL  29     AC: Colors and/or astrometry are inconsistent with a late-type common           
                         proper motion companion based on visual inspection of the field from            
                         2MASS, SDSS, DSS1, and/or DSS2. Primary is G 13-33.                     Bwl2015 
12229+1725   GIC 107     LDS1301. G059-015AB.                                                            
12236-6138   EVS  19     Primary is the Cepheid R Cru.                                           Evs2016a
12240-6206   COO 137     Spectrum A0/2+K1/2III                                                           
12241+3827   KZA  30     RA cos(DEC) was in error by 1 arcmin in Kazeza measures.                KZA1984 
12242+6655   LDS2641     SLW 716.                                                                        
12242+0558   STT 248     FK Vir                                                                          
12243+2606   YSC  97     13 Com = GN Com.                                                                
12244-5250   HJ 4520     B is CPD-52@5564.                                                               
12247+0225   AG  177     AB: HJL 170.                                                            HJL1986 
12248-2827   BRT2993     CPD-27@4502.                                                                    
12249-5807   BSO   8     Spectrum F8/G2IV/V+A.                                                           
12250-0414   TOK 400     HIP 60574 is a spectroscopic triple with periods 14d and 22yr (Latham           
                         2012, private communication), also an acceleration binary. We resolved          
                         the outer pair at 0".22 separation, matching the spectroscopic period.          
                         The lines of the visual secondary Ab could potentially be detected in           
                         the spectrum by cross-correlation, leading eventually to a full 3-D             
                         orbit.                                                                  Tok2015c
12251+6025   GIC 108     LDS1306.  G197-057/G197-058.                                                    
                         NLTT 30676/30680                                                        Chm2004 
12265+3858   LDS4208     NLTT 30746/30750                                                        Chm2004 
12266-6306   DUN 252     alp 1 Cru = Acrux. According to R.G. Aitken, this was discovered by     A__1935f
                         the Jesuit missionary, Father Fontenay, at the Cape of Good Hope, in    Fon1733 
                         1685, although the triple was first measured by Dunlop and called       Dun1829 
                         DUN 123AB and DUN 122AC. Spectroscopic binary. CPM with HR 4729 and             
                         HR 4731, so there are at least five components in the system.                   
                         Hyperbolic orbit by Hopmann (1960).                                     Hop1960b
                         q = periastron distance in the true orbit = 0".916                              
                         Both A and B appear to be spectroscopic binaries with undetermined      Bte1967 
                         periods (see Batten 1967).                                              Fin1970b
12268-0536   A    78     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.95 +/- 0.56, 2.88, and 1.25 Msun, respectively.             Mlk2012 
12269+2816   SMR  58     gam Com.                                                                        
                         NPOI Limb-darkened diameter 2.179 +/- 0.057 mas, Sp = K1III,            NOI2018 
                         R =12.01 +/- 0.34 \rsun, Teff = 4660 +/- 84 K, L = 61.4 +/- 3.3 \lsun,          
                         M = 1.78 +/- 0.25 \msun, Age = 1.69 +/- 0.56 Gyr.                               
12269-3728   HJ 4510     B is CD-36@7850. BC: C is CPD-36@5498.                                          
12270-0332   HJ  210     LDS2880.                                                                        
12272+2701   STF1643     A premature orbit has been computed. Omega and omega in Hopmann (1964)  Hop1964b
                         have been flipped in the orbit catalog to better match observations.            
                         Data appear equally well fit by rectilinear solution - see catalog.             
12272-1958   S   637     B is BD-19@3492.                                                                
12273-2026   I   513     PTT 23.                                                                         
12274+0723   STF1644     Optical pair with large relative motion, noted by Muller in his list            
                         of neglected pairs.                                                     Cou1953d
12274-2843   B   228     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.91 +/- 3.62, 2.73, and 1.51 Msun, respectively.             Mlk2012 
12275-7705   RST1668     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.26 +/- 0.25, 1.14, and 1.05 Msun, respectively.             Mlk2012 
12276+7525   LDS1751     NLTT 30801/30819                                                        Chm2004 
12278-1010   HDS1754     Primary is KP Vir, an Algol-type eclipsing binary, P = 2.27720d.        Zas2012 
12279+3110   LDS1310     LDS5215.                                                                        
12280-5014   RIZ   3     sig Cen.                                                                        
12281+4448   STF1645     Alternative spectra F5+K. (Mt. Wilson F8+G0). Statistically the same            
                         parallax within the errors would indicate the components are physical.          
12281-6002   HJ 4524     B is CPD-59@4236.                                                               
12283-6146   CPO  12     A,BC: A is SB, no orbit. AD can be physical. Moved by 1"in 40y (WDS),           
                         while the PM implied 6" motion.                                         Tok2014d
12284+1223   LDS1311     LIT  23. NLTT 30838/30837.                                              Chm2004 
12286+0433   TMA   1     Incorrectly identified as J  1022. Pairs are close, and have similar            
                         position angles (mod 180deg). However, the Jonckheere pair is closer,           
                         and all published measures indicated a small magnitude difference.              
                         This pair has been resolved by 2MASS, so added under that designation.          
12286+0431   J  1022     See note to TMA   1.                                                            
12287-7129   LDS 410     Proper motion -419 +1091.                                                       
12288-1040   RST3792     LDS4217. NLTT 30870 = Ross 948 = GJ 3727.                               Chm2004 
12289+2555   STFA 21     AB: A is an Alpha CVn-type variable, AI Com.                                    
                         B is a spectroscopic binary.                                                    
             BU 1080     BC: Faint companion was suspected sf on both nights.                    B__1963b
12290+4144   BWL  31     AC: Colors and/or astrometry are inconsistent with a late-type common           
                         proper motion companion based on visual inspection of the field from            
                         2MASS, SDSS, DSS1, and/or DSS2. Primary is GJ 3729.                     Bwl2015 
12290+0826   WSI 113     GJ 469. Initally added to WDS as 12297-0320AST   4 with GJ 469.1.               
12297-0320   TOK  27     GJ 469.1.  Visual pair has estimated period 3400y.                      Tok2006 
                         A is SB1, P=25.939d                                                     Tok2014d
12298-0527   B  2737     LDS5216.                                                                        
                         Also known as LHS2567/8. Parallax = 47.68 +/- 1.29 mas.                 TSN2010 
12299-1631   SHJ 145     7 Crv = del Crv = Algorab. B is BD-15@3481.                                     
                         NLTT 30918/30916                                                        Chm2004 
                         A may be variable.                                                              
                         AB: H 4 105.                                                            MEv2010 
12300+5132   BUP 143     7 CVn = del CVn. C is BD+52@1630.                                               
12301-1324   BU   28     Wilson & Seabroke note seeing a distant (290".8) companion in 1874.26   WS_1877 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.80 +/- 0.97, 1.81, and 1.07 Msun, respectively.  Mlk2012 
12302-5336   RSS  16     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
12303+2157   HJL1069     Spectral type of comoving secondary estimated F6-G4, mass 1.02 Msun.    Mug2014 
12306+0943   STF1647     Hopmann (1964) orbit rejected from Fourth Orbit Catalog                 Hop1964b
                         ("period over 4000 years")                                              Wor1983 
12307+5352   ES  726     AB: Also known as STI2284.                                                      
                         AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
12309+2555   LAS   7     Lasgoity (2014) determines that the two components of the pair in the           
                         region of the Coma Berenice star cluster share common proper motion.            
                         He derives spectral types of M3V for both components, and estimates             
                         distance, mass, and radius for both stars.                              Las2014a
12310-5312   HJ 4526     B is CPD-52@5648.                                                               
             B  2738     CD: Additional notes may be found in van den Bos (1930).                B__1930b
12311+6116   LDS1314     NLTT 30989/30986                                                        Chm2004 
12312+0120   SHJ 146     STTA119. B is BD+02@2551.                                                       
12312-5707   DUN 124     gam Cru = Gacrux. A variable? B is CPD-56@5274, spectrum A3V.                   
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
12313+5507   BAG  50     GJ 1160. Primary is the variable NO UMa.                                Bag2013 
                         Arenou (2000) gives combined solution of astrometric orbits and DSBs.   Are2000 
                         Paper includes masses and distances.                                            
                         Schlieder et al. (2016) derive the following properties for A and B:            
                            spectral types  K2V   +/- 0.5     K6.5V +/- 0.5                              
                            masses (Msun)   0.83  +/- 0.03    0.65  +/- 0.02                             
                            Teff (K)        5020  +/- 50      4150  +/- 30                               
                            log (L/Lsun)    -0.48 +/- 0.03    -0.96 +/- 0.03.                    SJE2016 
                         Improved resolved SB2 orbit for this pair.                              Kie2018 
                         A: Teff = 5105 +/- 21 K, M = 0.834 +/- 0.017 \msun.                             
                         B: Teff = 4175 +/- 35 K, M = 0.640 +/- 0.011 \msun.                             
                         Orbital parallax = 38.82 +/- 0.23 mas.                                          
                         Age = 0.4 Gyr.                                                                  
12314-5659   RST2802     P of AB estimated at 1.4 kyr. A is a close spectroscopic binary with    Tok2022e
                         P ~343d.                                                                        
12316+3201   COU 966     Linear solution first suggested and alternative linear solution in      Cve2022 
12316+1631   BPM 591     [PM2000] 1034110 + [PM2000] 1034136.                                    Gvr2010 
12316-1104   STF1649     B is BD-10@3486. Mt. Wilson spectral types A3, F2.                              
12317+1208   SHY 607     HIP  61135 + HIP  61416.                                                        
12317-5925   GAA  12     Classical Cepheid BG Cru = 35 Cru.                                              
12321+7449   STF1654     H N 118.                                                                MEv2010 
12323+2000   HU  571     Possible quadrant reversal about 1920-1930.                                     
12323+1335   LDS1317     AC: NLTT 31039/31038                                                    Chm2004 
12324+1717   BPM 592     [PM2000] 1034422 + [PM2000] 1034445.                                    Gvr2010 
12324+1211   LDS 937     LDS1316.                                                                        
                         NLTT 31034/31037                                                        Chm2004 
12325+2106   STF1652     Primary is KK Com, a Beta Lyr type eclipsing binary, P = 1.06788d.      Zas2012 
12328+4828   LDS4227     NLTT 31062/31063                                                        Chm2004 
12329+5448   A  1600     Primary is II UMa, a W UMa type eclipsing binary, P = 0.82522d.         Zas2012 
12333-2410   ARA2180     May be HJ 4527 = BDS 6203 with a quadrant flip.                         Dam2014f
12333-6330   KRV   8     Classical Cepheid VW Cru.                                                       
12334+3202   STF1653     STF1655.                                                                        
                         SEI 532.                                                                Nsn2017b
12335+0901   REU   1     Wolf 424 aka GJ 473 or LDS1320. One or both components may be a flare           
                         star.Proper motion -1777, +218.                                                 
                         Two possible orbit solutions by Schultz et al. (1998).                  Scz1998b
                         Masses of 0.143 +/- 0.011 and 0.131 +/- 0.10 Msun derived by Torres et  Trr1999 
                         al. (1999) assuming a trig parallax of 0.233 +/- 0.004 arcsec.                  
                         Heintz (1972) orbit utilizes elongations of blended photographic        Hei1972 
                         images.                                                                         
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         1990.04: Theta and rho values are averages of observations taken in             
                         the J, K, and L bands  (1250/380, 2200/480, and 3400/700 nm).                   
                         Magnitude difference is that at K band.                                 Prr1992 
12336+3837   STF1656     B is BD+39@2534.                                                                
12336+0717   TOK 149     HIP 61298. Not observed, but B at 18.7" is bright and likely physical,          
                         considering that N*=12.                                                 Tok2011a
12337+4121   BNU   4     CHARA Array Limb-darkened diameter  1.238 +/- 0.030 mas,                CIA2012e
                         R =  1.123 +/- 0.028 \rsun, L =  1.151 +/-0.018 \lsun,                          
                         Teff = 5653 +/-  72 K, M = 0.852 +/- 0.023 \msun,                               
                         Age = 14.2 +/- 2.1 Gyr.                                                         
                         NPOI Limb-darkened diameter 1.133 +/- 0.034 mas, Sp = G0V,              NOI2018 
                         R = 1.03 +/- 0.03 \rsun, Teff = 5966 +/-117 K, L =  1.2 +/- 0.1 \lsun.          
12340+3458   LDS1323     NLTT 31128/31127                                                        Chm2004 
12342-3206   HJ 4528     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Friedman et al. (2012).                         USN2012a
12344+1517   OSO  46     G059-024. Neither is a common proper motion pair.                       Oso2004 
12345+1206   BPM 593     [PM2000] 1035249 + [PM2000] 1035290.                                    Gvr2010 
12346+3914   LDS4230     NLTT 31156/31154                                                        Chm2004 
12346-5752   R   202     TOB  92.                                                                        
12347+2549   LAS   8     Lasgoity (2014) determines that the two components of the pair in the           
                         region of the Coma Berenice star cluster share common proper motion.            
                         He derives spectral types of K4V and M0V for the two components, and            
                         estimates distance, mass, and radius for both stars.                    Las2014a
12349+2238   WRH  12     23 Com. A spectroscopic binary.                                                 
                         Additional notes may be found in Wilson (1941).                         WRH1941b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 8.26 +/- 4.61, 3.95, and 2.46 Msun, respectively.             Mlk2012 
12349-4538   ZUC   4AB   2MASS J12345629-4538075 is better known as TWA 16. The presence of a            
                         close companion to this star was noted in Zuckerman et al. (2001)               
                         which seems to be consistent with the companion that we detect.                 
                         However, since no explicit astrometric information is given in                  
                         Zuckerman et al. other than a rough estimation of the separation        Zuc2001b
                         (0.67"), it is not possible to test whether the companion shares a              
                         common proper motion with the primary at this point. The brightness             
                         and color are consistent with a physical companion, hence the system            
                         counts as binary in  the statistics.                                    Jnn2012 
12350-4717   HJ 4530     A,BC: Rectilinear solution by Friedman et al. (2012).                   USN2012a
12351+3104   LDS1325     NLTT 31191/31204                                                        Chm2004 
12351+2547   LAS   9     Lasgoity (2014) determines that the two components of the pair in the           
                         region of the Coma Berenice star cluster share common proper motion.            
                         He derives spectral types of K6V and K8V for the two components, and            
                         estimates distance, mass, and radius for both stars.                    Las2014a
12351+1823   STF1657     24 Com. B is a spectroscopic binary, spectrum A9Vm.                             
                         Measure of 1927.49 made by triangulation of multiple measures.                  
                         H 4  27.                                                                MEv2010 
             CIA  32     Ma,Mb = 1.838 +/- 0.218, 1.541 +/- 0.184 \msun.                                 
                         Ra,Rb = 2.28 +/- 0.06, 1.70 +/- 0.07 \rsun.                                     
                         Teff_a,Teff_b = 7630 +/- 120, 7180 +/- 140 K.                                   
                         La,Lb = 15.6 +/- 1.3, 7.2 +/- 0.9 \lsun. distance = 110.1 +/- 6.1 pc.   CIA2022e
12351+0727   STF1658     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
12353+1318   LAW   1     Spectral types M5-M7 and M6-M7, masses 0.097-0.107 and 0.097-0.106              
                         Msun, distance 24.4 +/- 2.7 pc                                          Law2006 
                         The position angle for this system given in Law et al. (2006) is        Law2006 
                         actually 257.0deg, but since the components are fairly similar in               
                         brightness and there is a fake triplet effect, we assume that there             
                         can be a 180deg phase shift present in the Law et al. data (or                  
                         alternatively in both of our epochs). The angular motion in our two             
                         AstraLux images is 1.8deg in about 0.5 years. If taken at face value,           
                         the Law et al. data point would imply 198.4deg angular motion in 4.5            
                         years, corresponding to 22deg per half-year, which is an order of               
                         magnitude too large. On the other hand, if we subtract 180deg from the          
                         Law et al. position angle to get 77.0deg, then the angular motion is            
                         2.0deg per half-year, which is perfectly consistent with our                    
                         measurements. Hence, we adopt the latter value for our analysis.        Jnn2012 
12357-1650   FIN 368     Aa,Ab: Hipparcos parallax 13.56 +/- 0.76 mas. Dynamical parallax 13.3           
                         mas, masses 1.79 and 1.23 Msun.  Speckle measures of 1989-91 and        McA1990 
                         2009-11 repeat themselves, hinting at a 20 yr period. However, the      Tok2010 
                         measure by Mason et al. in 2006.2 does not fall on the same ellipse     Msn2009 
                         and had to be ignored. It could refer to another star, as FIN 368               
                         should have been unresolved at that time according to our preliminary           
                         orbit, which also matches the speckle non-resolution in 1976.3 and the          
                         non-resolutions in 1964-1966 by Finsen. An alternative orbit with P =   Fin1965a
                         10.13 yr and e = 0.9 can also be fitted to the data. The Hipparcos              
                         measure on 1991.25 contradicts speckle interferometry on 1991.39; it    HIP1997a
                         had to be ignored. Nordstrom et al. (1997) noted double lines           Nrd1997 
                         broadened by fast axial rotation of 100 km/s and 20 km/s. However,              
                         individual RVs measured by these authors during 1987-1991 (near the             
                         apastron) do not show any systematic behavior that could be related to          
                         the orbit. Continued speckle monitoring will be critical for                    
                         confirming the orbit.                                                           
12358-5935   WFC 128     TOB  97.                                                                        
12359-0125   BAL 872     RST4964.                                                                        
12360-3952   HJ 4533     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
12362-4650   RST5526     Motion retrograde.                                                              
12366+3001   BFR   8     LSPM J1236+3000 + 2MASS J12363647+3000315. Baron et al. (2015)                  
                         estimate spectral types M6 +/- 1 and M9.0 +/- 1, distances 112 +6/-52           
                         and 126 +18/-44 pc, masses 0.102-0.133 and 0.079-0.085 Msun.            BFr2015 
12368+2014   AG  180     HDS1769.                                                                        
12369+8922   HJ 3170     Aka SKF 987.                                                                    
12371+1546   LDS1328     SLW 746.                                                                        
12372+2112   STF1663     STT 252.                                                                        
12372-6908   DON 541     alp Mus. Variable.                                                              
12373-1703   LDS 414     NLTT 31307/31301                                                        Chm2004 
12375-0334   TOK 150     HIP 61608. Not observed, the status of B at 5.5" is uncertain, could be         
                         physical (it is close and bright, N*=11).                               Tok2011a
12382+6628   LDS2656     Apparently a 1' error in RA for Luyten's secondary led to incorrect     Luy1972 
                         rho and theta for the 1966 measure.                                             
12383-5807   HJ 4534     TOB 105. B is CPD-57@5606.                                                      
12384-6255   COO 139     TOB 106.                                                                        
12386-0041   FAR  37     Primary is white dwarf WD 1236-004.                                     Far2006 
12387-0422   S   639     B is BD-03@3330.                                                                
                         AB: H 5 129.                                                            MEv2010 
12387-0520   STF1665     LDS 415. NLTT 31380/31381                                               Chm2004 
12388-5113   TOK 151     HIP 61698.                                                              Tok2011a
12389+1348   HDS1772     KM Com.                                                                         
12390+1255   BPM 594     [PM2000] 1037092 + [PM2000] 1037097.                                    Gvr2010 
12391+2104   26 Com      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin (1981).                                                         Grf1981a
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Griffin (1981).                                                         Grf1981a
12391-0133   HJ 1220     LDS2886.                                                                        
12391-5816   R   205     AB: TOB 108. B is CPD-57@5611.                                                  
12392+1420   STF1666     Spectrum of A composite; A3+G.                                                  
12392-0800   ENG  47     26 Vir = chi Vir. B is BD-07@3454.                                              
                         Spectrum of A: K2III-IIIbCN1.                                                   
12392-4022   B  1215     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.35 +/- 0.95, 2.18, and 0.98 Msun, respectively.             Mlk2012 
12394-5338   JNN  80     The two components of 2MASS J12392104-5337579 that were detected in             
                         the AstraLux images have almost equal brightnesses and color, hence             
                         they are very likely physically bound. Common proper motion has not             
                         yet been tested.                                                        Jnn2012 
12396+1956   BGH  40     AB: HJL1073.                                                            HJL1986 
12396-3717   DAW  63     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.33 +/- 0.78, 1.60, and 0.76 Msun, respectively.             Mlk2012 
12398+1754   BPM 595     [PM2000] 1037411 + [PM2000] 1037399.                                    Gvr2010 
12399+7425   HJ 2619     HJ 1221.                                                                        
12399-6631   KOU  13     FH Mus.                                                                         
12401+2049   OSO  47     G059-032. The AB pair is not a common proper motion pair, based on              
                         color, but the AC pair is. Astrometry for the wide pair is determined           
                         from Digital Sky Survey images                                          Oso2004 
12402-1150   LDS4241     NLTT 31463/31461                                                        Chm2004 
12406+1513   TDS8482     Aa,Ab: Initially added as 12405+1517 TDS8482, but was found to                  
                         comprise the primary of 12406+1513 HJ  213. Systems merged.                     
12408+7901   MLR 427     Also known as HDS1776.                                                          
12408+4031   LTT13601    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
                         Spectroscopic solution to these astrometric pairs given by Griffin      Grf2013a
                         (2013). Periods match "tolerably well," other common elements less so.          
12409+2708   COU 596     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.92 +/- 1.30, 3.19, and 1.20 Msun, respectively.             Mlk2012 
12409+0850   STF1668     H N 143.                                                                MEv2010 
12412-0127   BU  607     HDO 134. This is the F component of STF1670.                                    
12413-1301   STF1669     58 Crv. Both A and B are spectroscopic binaries (A is SB1), with                
                         periods of 44.4 and 1.46d. Both may also be variable.                           
                         Period of AB estimated at 4500y, AC at 150,000y.                        Tok2006 
                         AB: H N  38.                                                            MEv2010 
                         The B component of STF1669 is the spectroscopic eclipsing binary VV             
                         Crv.  Fekel et al. (2013) derive an orbit based on light and velocity           
                         curves with P=3.1445d and e=0.0852. Both components are F5 dwarfs; V            
                         magnitudes are 6.099 and 7.536, and masses are 1.978 +/- 0.010 and              
                         1.513 +/- 0.008 Msun.                                                   Fek2013b
12415+2136   LDS4249     NLTT 31550/31551                                                        Chm2004 
12415-4858   HJ 4539     gam Cen. AB: Malkov et al. (2012) derive dynamical, photometric, and            
                         spectroscopic masses 7.30 +/- 3.94, 5.19, and 2.29 Msun, respectively.  Mlk2012 
             SHY 239     AD: HIP  61932 + HIP  61622. D component = tau Cen.                             
12416+4814   LDS4251     NLTT 31574/31576                                                        Chm2004 
12416+4105   LDS5757     LDS6262. NLTT 31567/31578                                               Chm2004 
12416+1026   H 6  81     H VI 81. 27 Vir. A is the Delta Scuti-type variable                             
                         GG Vir, and is also a spectroscopic binary.                                     
             SHY 610     AC: HIP  61937 + HIP  62350.                                                    
12417+5543   SHY  64     AB: HIP  61946 + HIP  61481.                                                    
                         AC: HIP  61946 + HIP  59496.                                                    
                         AD: HIP  61946 + HIP  65327.                                                    
             SHY 236     AE: HIP  61946 + HIP  61100.                                                    
                         BE: HIP  61481 + HIP  61100.                                                    
12417+2614   LDS1331     LDS6263.                                                                        
12417-0127   STF1670     gam Vir = 29 Vir = Porrima. According to R.G. Aitken, this was          A__1935f
                         discovered in 1718 by Bradley and Pound.                                        
                         One component is a suspected variable.                                          
                         Measure of 1720.31 made by triangulation of multiple measures.                  
                         Measure of 1927.31 made by triangulation of multiple measures.                  
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: H 3  18.                                                            MEv2010 
                         AB: Additional notes may be found in van de Kamp (1929).                Kam1929 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.69 +/- 0.06, 2.86, and 2.89 Msun, respectively.  Mlk2012 
                         AC: Additional notes may be found in Burnham (1894).                    Bu_1894 
                         AF: F component is primary of 12412-0127 BU  607. Pair not physical,            
                         so systems not merged.                                                          
12418+5645   BWL  33     AD: Colors and/or astrometry are inconsistent with a late-type common           
                         proper motion companion based on visual inspection of the field from            
                         2MASS, SDSS, DSS1, and/or DSS2.                                         Bwl2015 
12419+1014   VIG  15     Primary is rho Vir. The optical/physical nature of the faint companion          
                         is undefined.                                                           Vig2012 
12420+0648   BU  924     31 Vir.                                                                         
12420-2202   DON 547     CPD-21@5405.                                                                    
12420-4113   CPO 351     CPD-40@5868.                                                                    
12421-6924   EVS  20     Primary is the Cepheid R Mus.                                           Evs2016a
12422+2622   A  1851     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.62 +/- 0.38, 1.55, and 0.71 Msun, respectively.             Mlk2012 
                         Mass-A is 0.64 +/- 0.02 and Mass-B is 0.53 +/- 0.04 \msun.              EEA2021 
12423+7510   LDS1755     ZUC  10. Primary is white dwarf PG 1240+754 = LB 261.                   Zuc1992 
                         NLTT 31644/31647                                                        Chm2004 
12423-6117   TDS8491     TOB 113.                                                                        
12423-6300   HDS1780     Primary is DP Cru, a W UMa type eclipsing binary, P = 1.88468d.         Zas2012 
12424-6258   TOB 112     DE: B component of 12422-6258 TOB 112 was found to be the D component           
                         of 12424-6258 SIN  74AD. Systems merged.                                        
12425+1311   LDS1333     NLTT 31615/31612                                                        Chm2004 
12427+3007   LDS1334     LDS6265.                                                                        
12428+4154   BWL  34     Colors and/or astrometry are inconsistent with a late-type common               
                         proper motion companion based on visual inspection of the field from            
                         2MASS, SDSS, DSS1, and/or DSS2. Primary is LHS 2613.                    Bwl2015 
12429+0516   A  1602     Derived orbital parallax 0".01295, mass sum 2.28 +/- 1.10 Msun          Lin2004a
12429-0215   LDS2888     AC: NLTT 31636/31638                                                    Chm2004 
12430-0713   BRT 439     A likely plate flaw.                                                    Grv2021b
12431+6109   LDS2320     Originally listed as 10442+6111, based on Luyten's 1950 coordinates,    Luy1970 
                         but no pair is found at that location. However, a pair in excellent             
                         agreement with his measure is found at the location of his cross-               
                         reference catalog entry, BD+61 1312.  Apparently there was a 2h error           
                         in Luyten's 1950 coordinates. Given the size of the error, correction           
                         to the WDS designation was deemed appropriate.                                  
12431+2117   LDS5758     LDS6266. G059-036. See Allen et al. (2000) for information on           AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
12433+1734   BPM 596     [PM2000] 1038880 + [PM2000] 1038853.                                    Gvr2010 
12433-3341   I  1558     CPD-33@3294. Spectrum: G8IVCNIII.                                               
                         V1133 Cen, Algol-type eclipsing binary, P = 1.270335 d.                 Zas2011 
12436+6001   LAF  48     Heinze et al. (2010) determine the B component is a background object.  Hze2010 
12436-6116   TOB 115     Also known as JAW  35.                                                          
12438+0733   STF1674     Aka H N 143.                                                            Bu_1906 
12439+3421   GC 17317    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
12440+0356   A  1603     B may be variable.                                                              
12441+3546   HO  256     Spectrum: A7/A8V/F2/3.                                                          
12442+5146   GC 17326    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
12443-5553   R   206     B is CPD-55@5202.                                                               
12445+5841   LDS1335     NLTT 31745/31744                                                        Chm2004 
12445-0119   SKF  38     AB: Secondary is white dwarf PG 1241-010.                               Zuc1992 
12446-5717   FIN  65     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.38 +/- 0.80, 2.86, and 2.34 Msun, respectively.  Mlk2012 
                         AB: Docobo & Andrade (2013) derive a dynamical parallax of 7.51 +/-             
                         0.37 mas and component masses 2.20 +/- 0.42 and 1.69 +/- 0.33 Msun              
                         (for spectral type A0V) or 7.84 +/- 0.40 mas, 1.97 +/- 0.39 and 1.45            
                         +/- 0.29 Msun (for A0IV). See paper for extensive notes on system.      Doc2013d
12448+6203   STI 749     MLB 411 is identical                                                    Hei1983a
12449-5245   HJ 4546     B is CPD-52@5846.                                                               
12452-5721   SHY  65     HIP  62229 + HIP  69570                                                         
12453-0353   STF1677     B is BD-03@3348.                                                                
                         H 3  53.                                                                MEv2010 
12454+1422   STF1678     STTA120 = STFA 22.  B is BD+15@2503.                                            
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
12456-6059   HJ 4547     iot Cru                                                                         
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2014).                         USN2014a
12457-1734   FEN  17     ARA 227. An error in transcribing coordinates into the IDS from the             
                         original source resulted in an incorrect WDS designation of 21462-1634          
                         for this pair, as well as it's "rediscovery" by Aravamudan.             Ara1963 
                         Astrographic Catalogue plate defect.                                    Grv2023b
12461+6320   LDS2658     NLTT 31833/31836                                                        Chm2004 
                         SLW 769.                                                                        
12463-6806   R   207     bet Mus. A has variable radial velocity.                                        
                         Rica (2012) derived a dynamical parallax of 11.3 mas (compared with     FMR2012g
                         10.48 +/- 0.65 mas from Hipparcos) and a mass sum (using the Hipparcos          
                         parallax) of 20.9 +/- 5.9 Msun.                                                 
12464+0932   STT 577     33 Vir. B is BD+10@2467.                                                        
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
12464-5629   HJ 4548     B is CPD-55@5216 and is a suspected variable.                                   
12464-5907   KRV   7     Classical Cepheid X Cru.                                                        
12467-1901   B  2540     Elongation and quadrant doubtful.                                       B__1963b
12470-0748   GC 17364    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
12470-5547   R   208     AB: TOB 122.                                                                    
12471+2237   SHY 612     HIP  62384 + HIP  62805.                                                        
12472+3325   LDS5217     LDS6267.                                                                        
12472+1442   GIC 109     G059-039/G061-017.                                                              
                         NLTT 31888/31890                                                        Chm2004 
12472+1157   BUP 145     34 Vir.                                                                         
12472-4105   WG  155     CPD-40@5908.                                                                    
12477-5941   I   362     bet Cru = Mimosa. A is a Beta CMa-type variable.                                
                         Intensity Interferometer Limb-darkened diameter 0.722 +/- 0.023 mas.    HBr1974 
12478-0836   BRT 440     Aka SKF 226.                                                                    
12481+1325   BPM 597     [PM2000] 1040797 + [PM2000] 1040792.                                    Gvr2010 
                         NLTT 31941/31940                                                        Chm2004 
12483+7714   MLR 428     Also known as TDS8530.                                                          
12485+8134   LDS1758     B is BD+82@376.                                                                 
                         HJL 172.                                                                HJL1986 
12487+6019   SHY  66     AC: HIP  62512 + HIP  64532. C component = A component of 13136+5643.           
             SHY  66     AD: HIP  62512 + HIP  65327.                                                    
12489+1206   LEP  59     AE: M4, spectroscopic distance 24pc. 75" from G5 dwarf HD 111398 =              
                         HIP 62536 = 2MASS J12485242+1205469. Hipparcos pm for the G dwarf is            
                         +235-140, consistent with the USNO-B1 pm for M dwarf of +234-119.       Red2007a
                         E: 2MASS J12485345+1204326 is a wide (76") common proper motion                 
                         companion to HIP 62536 (Lepine & Bongiorno 2007), but is single in the  Lep2007 
                         AstraLux images.                                                        Jnn2012 
12491+4213   ES 2643     B is BD+43@2262.                                                                
12491-5125   RST5368     CPD-50@5488.                                                                    
12492+8325   STF1694     B is +84@289 and is a spectroscopic binary, spectrum A0V+A2V.                   
                         AB: H 4  15.                                                            MEv2010 
12492-0450   LDS5759     NLTT 31990/31992                                                        Chm2004 
12493+2733   CHR 179     30 Com. A is a spectroscopic binary, now probably resolved by speckle           
                         interferometry.                                                                 
                         Abt & Biggs (1972) note variable RV.                                    AbH1972 
12496+2053   LDS5760     LDS6269.                                                                        
12496+1035   BPM 598     [PM2000] 1041409 + [PM2000] 1041436.                                    Gvr2010 
12496+0349   STF1681     HJL 171.                                                                HJL1986 
12497+0111   ENG  50     B is BD+02@2584.                                                                
                         OSO  48AC & AD, formerly associated with this pair were imporperly              
                         assigned. They are at 13283-0222.                                               
12500+4708   GIC 110     LDS5761. G123-064/G198-080.                                                     
                         NLTT 32044/32040                                                        Chm2004 
12501+5506   GJ 3753     GD 319. Infra-red excess indicates a red companion. Probst notes a      Prb1983 
                         private communication by Downes & Margon reporting a close companion,           
                         type dK, probably optical. McAlister et al. examined the relative               
                         proper motions and concurred that the pair is optical.                  McA1996b
                         Magnitude difference is based on images from 1988.1736 and 1993.2054.           
             FAR  14     AC: Primary is white dwarf WD 1247+553.                                 Far2005b
12501-4853   SWR 133     CPM pair                                                                Skf2004 
12505+4021   LDS4281     NLTT 32072/32078                                                        Chm2004 
12508+2926   LDS3063     LDS5218.                                                                        
12509+0757   LDS4282     LIT  25.                                                                        
12509-0428   LDS6270     NLTT 32082/32080                                                        Chm2004 
12512-4652   HJ 4552     B is CD-48@8210.                                                                
12514-1020   STF1682     B is BD-09@3568. One component variable?                                        
12515+2207   LDS 940     LDS4285.                                                                        
12516+2531   HJL1074     SHY 242. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
12517-3328   I  1561     Spectrum: Fm delta Del.                                                         
12518+0005   TOK 671     AB: Resolved with ANDICAM2. AB may be optical, but appear to be                 
                         co-moving.                                                              Tok2014d
12519+3447   HJ  523     HJL 174.                                                                HJL1986 
12519+1910   STF1685     AB: HJL 173.                                                            HJL1986 
                         AB: H 4  58.                                                            MEv2010 
12521-0539   TSN  87     Also known as GWP1870 with a quadrant flip.                                     
12522+2247   GIC 111     LDS5219.  G059-042/G059-041.                                                    
                         NLTT 32153/32146                                                        Chm2004 
12522+1704   STFA 23     32 Com. B is BD+17@2553.                                                        
12525+3155   HJ  524     SEI 534.                                                                Nsn2017b
12527-5216   HDS1806     SWR 134. CPM pair                                                       Skf2004 
12528+3344   TOK 284     AC: The C component is the primary of 12534+3339 LDS1339. The LDS pair          
                         does not appear to be physical, so the systems were not merged.                 
12528+1225   TOK 401     41 Vir.                                                                         
                         HIP 62933 (41 Vir) was observed on request by F. Fekel who studies its          
                         spectroscopic orbit. Apparently it is resolved for the first time.      Tok2015c
12529+7741   LDS1761     NLTT 32240/32174                                                        Chm2004 
12530+1502   STF1686     A 13.9d spectroscopic solution for the B component has been found       Tok2019g
                         making this a 2+2 quadruple system.                                             
12531+1936   TOK 152     HIP 62860. A is a ROSAT X-ray source.                                   Tok2011a
12532-0333   CHR  38     38 Vir.                                                                         
12533+2115   STF1687     35 Com. The trend in the RV's of star A suggests that the ascending             
                         node is in the third quadrant.                                                  
                         AC: Star C (mag 9.75, 29", G3IV-V) is physical according to LeBeau,     LBu1990c
                         and in very slow direct motion.                                                 
                         AC: HJL 175.                                                            HJL1986 
                         AC: H 5 130.                                                            MEv2010 
12533+1310   HU  894     Divide the separation given in the IDS by 10. There is no change since          
                         discovery.                                                              Wor1967b
12533-1831   RST2821     HIP 62882. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
12534+1758   HJ  218     SLE 906.                                                                        
12536-0413   HR 4896     Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Griffin (1983).                                                         Grf1983 
                         SB1. Combined orbit including RV data and Hipparcos Intermediate                
                         Astrometric data. Semimajor axis derived from photocentric a0 plus              
                         stellar evolutionary model. Derived properties for A and B:                     
                         M/Msun = 1.62 + 0.39, L/Lsun = 26.66 + 0.02, dm = 7.81 mag,                     
                         log age = 9.33.                                                         WaX2015b
12537-2724   TOK 153     HIP 62925. B is physical, itself possibly a close binary as hinted by           
                         the residuals of the PSF fit. Small PM(A)=(-33,-40).                            
                         NOMAD: PM(B)=(+194,+500), V(B)=16.74 (??)                               Tok2011a
12539+7440   STF1698     WFC 131.                                                                        
12539-2918   STN  26     HDO 135                                                                         
12540+5558   BLM   2     eps UMa = 77 UMa = Alioth.                                                      
                         An Alpha CVn-type variable and eclipsing system.                                
                         1975.383: Erroneously listed as HD 112815 in Morgan et al. (1978)       BLM1978 
                         notes.                                                                          
                         The Yale Bright Star Catalogue cites this star as a spectroscopic       Hof1982 
                         variable with periods of 4.15 years and 0.95 days; the object is also           
                         a photometric variable with period 5.09 days. This observation                  
                         presumably resolved the longer period system.                           BLM1978 
                         NPOI Limb-darkened diameter    1.644 +/- 0.020 mas,                             
                         R =    4.29 (+0.19- 0.21)  \rsun,  Teff = 8908 +/-  54 K,                       
                         L =  104.4 +/-   9.3 \lsun.                                             NOI2023 
12540-1802   S   643     B is BD-17@3725.                                                                
12541+5500   LDS3067     SLW 792.                                                                        
12542+5250   BEM   2     Position corrected by Heintz.                                           Hei1983a
12543-1059   UC 2427     Also known as GWP1874 with a quadrant flip.                                     
12543-1139   CHR 206     First detected as an occultation binary by Africano.                    Afr1975 
12544-5826   EVS  21     Primary is the Cepheid S Cru.                                           Evs2016a
12546-5711   DUN 126     A: mu 1 Cru                                                                     
                         B: mu 2 Cru. B is variable, spectrum B5Vne.                                     
                         Statistically the same parallax within the errors would indicate the            
                         components are physical.                                                        
12547+2206   MET   9     Metchev & Hillenbrand say the pair is probably physical, based on               
                         proximity.                                                              Met2004b
12550+5810   STF1691     AB: HJL 176.                                                            HJL1986 
12550-8507   RST2819     iot Oct                                                                         
12553+0750   NLTT 32291  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Latham et al. (2002). They derived component masses 0.81 and 0.41 Msun  Lat2002 
                         and an estimated semimajor axis of 37.96 mas.                           Ren2013 
12554+6953   A  1092     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.49 +/- 0.47, 1.92, and 0.95 Msun, respectively.             Mlk2012 
12556+0324   BUP 146     del Vir = 43 Vir = Minelauva.                                                   
                         Smyth's quoted separation is difference in RA only.                     Smy1844 
12557+0620   LDS4295     SLW 796.                                                                        
12559+1653   BPM 599     [PM2000] 1044021 + [PM2000] 1044047.                                    Gvr2010 
12559+0812   HJ  850     LDS 941.                                                                        
12560+3819   STF1692     alp CVn = Cor Caroli. Both components are spectroscopic binaries.               
                         Prototype of the Alpha CVn-type variables. Spectrum F0V.                        
                         NLTT 32338/32336                                                        Chm2004 
                         H 4  17.                                                                MEv2010 
12560+0757   KPP4336     The RS CVn type variable V430 Vir.                                              
12560-1257   SJM   1     Aa,Ab: Stone et al. (2016) resolve the primary of the late M dwarf              
                         VHS J125601.92-125723.9, whose 8" companion was found to be an L-type           
                         brown dwarf. (Gauza et al. 2015). Spectrophotometric distance           Gza2015 
                         estimates implied by the M7.5 spectral type of the primary yield a              
                         distance of 17.1 +/- 2.5 pc. Kinematics are consistent with membership          
                         in the AB Dor moving group. For an age ~300 Myr, the masses of these            
                         two near-equal magnitude M7.5 stars are each 64.6 +0.8/-0.2 Mjup, and           
                         the mass of the distant companion is 11.2 +9.7/-1.8 Msun.               SJM2016 
12560-5650   HDO 221     Classification of the B component is from Lindroos (1985), who finds a  Lnd1985 
                         distance of 2.5 kpc.                                                    Msn1998a
12562+0050   SKF 896     Also known as BAL1453.                                                          
12562-6127   ELP  32     FT Cru.                                                                         
12563+5406   STF1695     A spectroscopic binary, P = 5.13d.                                              
12563+3232   HIP  63144  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Griffin (2004).                                                         Grf2004 
12563-0452   STF1690     H 2  42.                                                                MEv2010 
                         Discordant 3rd exposure gives 148.9deg, 6.9".                           Brt1931 
12564-0057   STT 256     Rectilinear solution by Scardia et al. (2017).                          Sca2017c
12564-3007   HJ 4558     B is CD-29@10020.                                                               
12567+0701   STF1693     HJL 177.                                                                HJL1986 
12567-4741   I    83     1995.1028: Quadrant determined by speckle imaging analysis.             Hor1996 
12570-3330   TDS8609     V1141 Cen.                                                                      
12571+2330   LDS 942     2MASS J12565215+2329501 and J12565272+2329506 constitute a known 8"     Red2007a
                         binary pair in the Reid et al. (2007) sample.                           Jnn2012 
12575+1842   BGH   5     LDS 943. HIP 63239. See Allen et al. (2000) for information on          AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
                         NLTT 32427/32423                                                        Chm2004 
                         HJL 178.                                                                HJL1986 
12576+3514   LDS5764     LDS6271. Spectra dM1.5e and dM3.5e. Starspots exist on A, and it is             
                         also a flare star.                                                              
                         NLTT 32441/32438                                                        Chm2004 
12577+4628   LDS4301     NLTT 32443/32444                                                        Chm2004 
12577-2249   LDS4300     1deg error in IDS led to similar error in WDS designation.                      
12578+3038   LDS1348     NLTT 32449/32447                                                        Chm2004 
12579+4948   HU  641     Apparent rapid motion. A premature orbit has been calculated.                   
12582+4153   LDS5766     NLTT 32463/32464                                                        Chm2004 
12583+0537   LDS4302     Aka GWP1883.                                                                    
12584+5822   HJ 2628     B is BD+59@1476.                                                                
12585+3817   STF1702     B is BD+39@2587.                                                                
                         HJL 179.                                                                HJL1986 
12585-4618   DON 568     CPD-45@6129.                                                                    
12586+4013   RDN   2     2MASS J12583501+4013083 + 2MASS J12583798+4014017. Separation ~6700au,          
                         apparently widest very low mass binary found to date. Found in cross-           
                         match of SDSS and 2MASS catalogs. Distance 105 +/- 13 pc, masses (from          
                         evolutionary models) 0.105 +0.029/-0.017 and 0.091 +0.010/-0.007 Msun.  Rdn2009 
12590-0950   B  2541     HIP 63366. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
12595+4159   LTT13738    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
12595+2814   WSI   1     Hipparcos suspected non-single.                                                 
12595-4832   HJ 4562     B is CD-47@8001.                                                                
                         SWR 136. CPM pair                                                       Skf2004 
12596-1026   GWP1885     Aka GWP1886.                                                                    
12597+1002   BFR   9     LSPM J1259+1001 + 2MASS J12594167+1001380. Baron et al. (2015)                  
                         estimate spectral types M5 +/- 1 and L4.5 +/- 0.5, distances                    
                         42 +44/-21 and 47 +5/-18 pc, masses 0.121-0.167 and 0.057-0.074 Msun.   BFr2015 
12597-0349   CHR  39     Aa,Ab. 44 Vir. Rapid binary.                                                    
                         1991.3921: This interferometric system has now completed nearly 180deg          
                         of revolution since its discovery in 1984.  A preliminary                       
                         determination of orbital elements yields a low-eccentricity orbit with          
                         a period of 15.7 years. Absolute quadrant determinations based on               
                         reanalysis of earlier speckle data have ruled out a possible short-             
                         period high-eccentricity orbit. A more complete orbital analysis is in          
                         progress.                                                                       
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 3.41 +/- 0.75, 3.58, and 2.00 Msun, respectively.  Mlk2012 
             STF1704     AB: H 4  51.                                                            MEv2010 
12598+0431   LDS4304     Primary is white dwarf WD 1257+047 = GD 267.                            Far2005b
12598-5555   DUN 127     B is CPD-55@5317.                                                               
13002-2355   I  1225     Measures uncertain, too close. Needs speckle.                                   
13003+3047   BU 1081     AB. 37 Com.                                                                     
             HDS1823     Aa,Ab. 1996.4274: Very weak detection, possibly an artifact.            Msn1999b
13003-6413   RST5372     Spectrum: F3/6IV/V+A.                                                           
13004+3545   HU 1141     Variability has been reported.                                                  
13005-0604   HJ 1224     Motion of pair represented by relative proper motion 0.104" in                  
                         81.8deg.  Footnote in ADS should be deleted; measure of 1922 is by              
                         Gauchet, from his own plate, but that of 1893 was taken by him from             
                         the San Fernando Astrographic Catalogue.                                B__1951a
13006+5904   FAR  15     GRV1201.  Primary is white dwarf WD 1258+593 = GD 322.                  Far2005b
13006-0322   AGC   5     46 Vir.                                                                         
13007+5622   BU 1082     78 UMa.                                                                 Baz1939b
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.69 +/- 0.73, 2.38, and 1.35 Msun, respectively.             Mlk2012 
13008+1423   STF1705     HJL 180.                                                                HJL1986 
13008+1223   GDM   1     AC: GJ 494 + ULAS J130041.72+122114.7. Primary is flare star DT Vir.            
                         Goldman et al. (2010 derive a spectral type T8.9 +0.2/-0.2 for this             
                         distant companion to Ross 458.                                          Gdm2010 
                         Based on colors and absolute magnitudes, Scholz et al. (2010) derive a          
                         spectral type T7.0 +/- 1.0 for the C component.                         Soz2010b
13014-2722   TOK 154     HIP 63559. A is SB without orbit, N04: dRV=17.0.                        Tok2011a
13015-5808   COO 146     Spectrum: A5/7+A1/2V.                                                           
13018+6337   LDS2662     M3.5 companion, distance just over 2' from F6 dwarf HD 113337 = HIP             
                         63584 = 2MASS J13014695+6336368. The pm for the M dwarf is -151+016,            
                         consistent with the brighter star pm of -171+025.  The spectroscopic            
                         distance for the fainter star is 36pc, compatible with the Hipparcos            
                         distance of 26.72 pc for HD 113337.                                     Red2007a
             JNN  83     Ba,Bb: 13015+6338 JNN  83 was found to be the B component of                    
                         13018+6337 LDS2662AB; systems merged.                                           
13020+4241   JNN  84     The companion to 2MASS J13015919+4241160 is clearly inconsistent with           
                         a background contaminant, but the astrometry is also inconsistent with          
                         a simple orbital motion of B around A - for instance, the separation            
                         decreases from June 2008 to February 2009, but then increases again to          
                         June 2009. This could for instance imply that either A or B is a close          
                         unresolved binary, where the photo-center shifts on a shorter                   
                         timescale than that of the AB orbit.                                    Jnn2012 
13020-0205   OSO  49     G014-024. Not a common proper motion pair, based on color and                   
                         comparison with POSS2 red plates.                                       Oso2004 
13021+0717   STF1708     HJL 181.                                                                HJL1986 
13022+1058   BUP 147     eps Vir = 47 Vir = Vindemiatrix.                                                
13023-7133   del Mus     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
13024-5201   JNN  85     Due to the very compact arrangement of the three components of 2MASS            
                         J13022691-5200507, it is highly probable that this is a physically              
                         bound triple system. Futhermore, the system is conspicuously close to           
                         the close binary J13025257-5201384 both on the sky and in distance (52          
                         versus 59 pc), hence this is a candidate quintuple system. Only one             
                         epoch of imaging exists, so common proper motion has not yet been               
                         demonstrated.                                                           Jnn2012 
13027-0159   HJ 1225     BAL 548.  Angular distance decrease 1.6" per century. Angular position          
                         decrease 1.8 degree per century. Minimal angular distance calculated,           
                         7.6" between 2600-2630 years.                                           FMR1999c
13029-6328   NZO  35     LDS 430.                                                                        
13030+0018   GRV1083     Aka SLW 816.                                                                    
13031+2358   LDS2896     LDS5220.                                                                        
13031-7129   CHR 228     As was the case with CHR 227, this star falls within the declination            
                         band missed in the surveys of Rossiter (1955) and van den Bos (1957).   Rst1955 
                         If physical, this 0".56 pair would presumably have an extremely long    B__1957a
                         period, given the spectral type and large calculated distance of its            
                         primary.  The small change in theta seen over 2.75 years is consistent          
                         with this, implying a period of order 500 - 600 years.                          
                         The star is noted in Abt & Biggs (1972) as having variable radial       AbH1972 
                         velocity; Hoffleit & Warren (1991) also note photometric variability    Hof1991 
                         of amplitude ~0.2 mag, as well as variability in the line width of              
                         H-alpha emission.                                                       Hrt1996b
13033+6749   TDS8668     Aka TOI 1297.                                                                   
13033-5936   COO 147     Spectrum: F5IV/V+A/F.                                                           
13038+2135   LDS2897     NLTT 32753/32754                                                        Chm2004 
13038-0510   GC 17714    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
             EVT   3     Primary is BY Dra type variable PX Vir.                                 EvT2012 
13038-2035   BU  341     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.39 +/- 0.67, 2.41, and 1.10 Msun, respectively.             Mlk2012 
13039-0340   BU  929     48 Vir.                                                                         
13040+2414   ITF  18     Aka ITF  96.                                                                    
13040-1738   BU  798     Closing. Earlier negative resuts are probably due to Burnham's                  
                         misidentification.                                                      B__1963b
13046+3100   LDS1358     Aka SLN  75.                                                                    
13046+1028   OSO  50     G060-060. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
13047+1736   BPM 600     [PM2000] 1047714 + [PM2000] 1047703.                                    Gvr2010 
13050-4634   COO 148     SWR 137. CPM pair                                                       Skf2004 
13054-5735   I   914     Spectrum of secondary: A/F.                                                     
13055+0911   LDS 944     Wolf 472,3.  Also known as GEL   1.                                             
13057+3548   TOK 805     14 CVn.                                                                         
13057-2541   LIM   1     Kelu 1. Estimated orbital period >40 yrs, inclination >81deg.                   
                         Spectral types L2 +/- 1 and L3.5 +/- 1                                  Gno2006 
13058-3111   BRT2997     CD-30@10320?                                                                    
13062+2902   BU 1083     BC: Only two attempts since 1901, in 1958, with negative results.       B__1960b
13064+7618   HJ 2644     B is BD+77@501.                                                                 
13064+2217   WSI 104     aka MP Com.                                                                     
13064+2109   CHR 150     Aa,Ab: 39 Com.                                                                  
             COU  11     AB: Rectilinear solution by Hartkopf et al.  (2012).                    Hrt2012a
13065-6505   HD 113659   LS 2919.  The classification is from Houk & Cowley (1975 Michigan               
                         Spectral Catalogue, vol. 1).                                            Msn1998a
13066+2226   LDS2899     LDS4315.                                                                        
13066-6434   I   916     Includes V948 Cen, an Algol-type eclipsing binary, P = 0.97508d.        Zas2012 
13067-2111   HJ 2637     B is BD-20@3775.                                                                
13069-3407   HIP  64006  Astrometric binary. Elongated? Separation ~0.025", period ~1yr?                 
                         Accelerated pm.                                                         Tok2012b
13069-4954   DUN 128     xi 2 Cen. A is a spectroscopic binary.                                          
13072-5420   FIN  54     Includes V949 Cen, an Algol-type eclipsing binary, P = 3.78697d.        Zas2012 
13073+0035   STF1719     HIP 64030. HIP 63810 at 2551" is CPM, possibly forming a wide triple            
                         system with AB = STF 1719 at 7".                                        Tok2011a
                         AB: A is SB1, P=445.8d                                                  Tok2014d
13074-5952   R   213     Spectrum composite; B9IV+F8-G2.                                                 
13075-6207   HJ 4568     B is CPD-61@3460.                                                               
13076+2629   BUP 148     B is BD+27@2217.                                                                
13077+2401   STT 259     B is BD+24@2540.                                                                
                         HJL 182.                                                                HJL1986 
                         SHY 245. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
13081+2657   STT 260     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.47 +/- 0.91, 2.41, and 1.07 Msun, respectively.             Mlk2012 
13081-6518   RMK  16     the Mus. Wolf-Rayet binary, second brightest in the sky.                        
                         The classification is from Houk & Cowley (1975 Michigan Spectral                
                         Catalogue, vol. 1). Moffat & Seggewiss (1977 A&A 54, 607) found                 
                         evidence of orbital motion in the WR star, but the O star appeared              
                         stationary. We found a possible binary companion at a separation of             
                         0".04 which needs confirmation, but if correct, this suggests that the          
                         system is triple, consisting of a WR SB1 plus a distant O star.  The            
                         visual B component was observed and appeared to be single.              Msn1998a
                         The primary is the WR+O spectroscopic binary theta Mus = WR 48. B is            
                         reported as SB by both Chini et al. (2012) and Sota et al.              Cii2012 
                         (2014, ApJS 211, 10).                                                   Sna2014 
13084+6236   MLB 412     Heintz corrects the declination.                                        Hei1983a
13084+3019   JNN  88     Aside from the binary companion detected in the AstraLux images, the            
                         star has a possible wide companion at 101", as noted in the WDS.        Jnn2012 
13084+1529   STF1722     STF1726.                                                                        
13085+2249   POU3133     LDS2902.                                                                        
13085-0241   S   647     Primary is HY Vir, eclipsing binary of Algol-type, period 2.7323 d.     Zas2012 
13085-8243   HJ 4565     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
13086+1710   BPMA 45     [PM2000] 1049381 + [PM2000] 1049350.                                    Gvr2010 
13089+0512   CRJ   5     White-dwarf companion to G5IV-V star HD 114714 found via Keck NIRC2             
                         imaging and RV monitoring. Multi-epoch observations indicate companion          
                         is physical. Absolute magnitude of companion Mj = 13.97 +/- 0.11 and            
                         colors are consistent with a T3 dwarf, but dynamical considerations             
                         preclude interfpretation of a substellar companion. Minimum mass of             
                         companion 0.260 +/- 0.010 Msun.                                         CrJ2013b
13090+3353   LDS4321     NLTT 33051/33036                                                        Chm2004 
13093+4649   COU2105     Appears to be a 10' error in the original 1855 BD declination -                 
                         nothing  at purported coordinates.                                              
13095-1313   BRT2732     13 04.3 -12 47 (Mason) may be same star.                                        
13097+2900   LDS1365     A: Also known as GJ 1167 A, this star has a wide companion at about             
                         190" according to the WDS.                                              Jnn2012 
13097-2212   TOK  28     Primary is 20d SB1; estimated period of AO pair is 23y. G-solution in           
                         HIPPARCOS.                                                              Tok2006 
                         Triple: the inner SB1 of 20.4 day period has tertiary companion TOK 28          
                         at 0".31 with mass ratio of 0.2 which produces the acceleration and             
                         dmu. This tertiary is too faint to be resolved in the optical.          Tok2012a
13098+6214   STTA121     Pair appears in an appendix list, not part of discoverer's regular              
                         numbering sequence.                                                             
13099+5504   GRV1155     Common proper motion white dwarf pair found in SDSS data.                       
13099+3122   STF1727     HJL 183.                                                                HJL1986 
13099-0532   MCA  38     Aa,Ab: the Vir = 51 Vir. Also a long-period spectroscopic binary.               
                         1976.3669: Epoch incorrectly given as 1976.3699 in McAlister (1982)     McA1982b
                         Spectral types of primary and secondary assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
                         Individual J,H,K magnitudes are calculated from 2MASS combined                  
                         magnitudes and AO-derived magnitude differences                         Rbr2005 
             STF1724     AB: H 3  50.                                                                    
             H 6  43     AC: Incorrectly identified as H 3  50. Error noted by MacEvoy.          MEv2010 
13100+1732   STF1728     42 Com = alp Com = Diadem.                                              Baz1964 
                         AB: Additional notes may be found in Madler (1844).                     Mad1844 
                         AB.  A preliminary orbit for this edge-on pair indicates that one of            
                         the F5 V stars may partially eclipse the other in early 1990.                   
                         Components reversed rel std sol's, e.g. in Hartkopf et al.              Hrt1989 
                         (1989). Their preliminary orbit for this edge-on pair indicated that            
                         one F5V star may have partially eclipsed the other in early 1990.               
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         1997.1179: The magnitude difference of the system is listed in the WDS          
                         as 0.0. Our reduction does not give the quadrant unambiguously, so we           
                         adopt the quadrant that gives a position angle consistent with                  
                         previous measures in the WDS.                                           Hor1997 
                         Spectral types amd masses of components assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
                         Calculated mass sum is 2.45 +/- 0.18 Msun, reasonable for two F5                
                         dwarfs. Closest approach of about 0.32 mas is predicted around 2015             
                         Jan 24 (to within about a week), eclipse duration ~1.5 days.            Mut2010b
                         Muterspaugh et al. (2015) revised their orbit, following discovery of   Mut2015 
                         three old measures whose theta measures had incorrect quadrants, which          
                         had led to an incorrect prediction of the eclipse timing.                       
13101+3830   STFA 24     17 CVn.                                                                         
             BU  608     BC: 15 CVn.                                                                     
13102+7358   STT 262     B is BD+74@524.                                                                 
13103+2423   LDS2904     LDS4322.                                                                        
13103-3447   B  2015     Rapid direct motion.                                                            
13105+6118   LDS1367     Aka SLN  77.                                                                    
13106+3356   ISO 13      RS CVn.                                                                         
13106-3128   RST1706     Hipparcos parallax 19.27 +/- 1.23 mas. Dynamical parallax 19.6 mas,             
                         masses 0.90 and 0.71 Msun. RST 1706 is an example of a neglected                
                         binary, discovered by R.A. Rossiter in 1934 but observed so rarely      Rst1955 
                         that only now, after a nearly full revolution, the first orbit could            
                         be proposed.                                                            Tok2012b
13109+2114   COU  96     This cannot be the close 437.7-d spectroscopic companion.               Grf2018b
13111+1220   OSO  51     G061-036. Neither is a common proper motion pair, based on astrometry           
                         and color                                                               Oso2004 
13112+3050   A  1359     The B component of this multiple is itself a close binary with a very   Grf2017a
                         short period of 3.34d.                                                          
13112-5739   JSP 573     Sinachopoulos (1988) apparently misidentified the Jessup pair; a                
                         nearby pair matching his measure has been given the component                   
                         designations EF.                                                                
13112-4717   COO 151     Beta Lyr (EB) type eclipsing binary, P = 0.88693 d.                     Zas2011 
13114+0938   LDS5771     LDS6272. HIP 64345. See Allen et al. (2000) for information on          AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
13115+2930   LDS1368     NLTT 33193/33185                                                        Chm2004 
13115-3508   HJ 4571     B is CD-34@8707.                                                                
13117-2633   FIN 305     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 6.21 +/- 2.03, 3.60, and 1.82 Msun, respectively.             Mlk2012 
                         Docobo & Andrade (2013) derive a dynamical parallax of 9.71 +/- 0.45            
                         mas and component masses 1.76 +/- 0.32 and 1.67 +/- 0.30 Msun. See              
                         paper for extensive notes on this system.                               Doc2013d
13119+2753   STT 578     bet Com = 43 Com. Possibly a long-period spectroscopic binary.                  
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Friedman et al. (2011).                         USN2011a
                         NPOI Limb-darkened diameter    0.887 +/- 0.171 mas,                             
                         R =    0.87 (+/- 0.17   )  \rsun,  Teff = 6612 +/- 637 K,                       
                         L =    1.3 +/-   0.0 \lsun.                                             NOI2023 
13119+1823   LDS 947     LDS6412, also at this location, has been removed. It had one measure,           
                         which was the same as the 1936 measure of LDS 947 with a quadrant flip          
                         G061-038. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
13119-1816   LDS4324     NLTT 33206/33173                                                        Chm2004 
13119-2038   DON 588     CPD-19@5377.                                                                    
13120+3205   STT 261     Scardia et al. say the quadrant is unambiguous for their 2004 theta     Sca2005a
                         value of 159.2; this does not agree with other determinations of                
                         magnitude difference, however.                                                  
13121+2415   HDS1848     1997.4597  Very weak detection, possibly an artifact.                   Msn1999b
13121-1612   HJ 2645     53 Vir. AC: Not found in 1908.                                          Bu_1913 
13122+3214   JNN  90     Aa,Ab: 2MASS J13120525+3213332 and J13120689+3213179 constitute a               
                         known 26" binary pair in the Reid et al. (2007) sample, and in          Red2007a
                         addition, each of the components are discovered as close binaries in            
                         the AstraLux data. Hence, the system is a very likely quadruple                 
                         system, although the close pair of J13120689+3213179 has yet to be              
                         formally confirmed as physically bound.                                 Jnn2012 
13123+1731   GC 17881    Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from Marcy        CPS1999a
                         et al. (1999).                                                          HaI2001 
             PAT  47     Chauvin et al. (2006) note finding at least one faint companion         Cvn2006 
                         candidate within separation/magnitude range listed. However,                    
                         further observations are required for verification                              
                         A is SB1, P=83.9d. "Exoplanet" with P=84d is actually a late-M dwarf?           
                         No transits.                                                            Tok2014d
13123-5803   JSP 918     Aka TDS8721.                                                            Dam2016b
13123-5955   SEE 170     The RV's of 1916 are quite uncertain. There may be a variation, and             
                         it may be related to the visual motion. The A component is also a               
                         Beta Lyrae-type system.                                                         
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         One component is V831 Cen, a beta Lyr system and also an SB with                
                         orbital period ~0.64d.                                                  Zas2009 
13124-4937   CPO 364     LDS 434. B is CD-48@8008.                                                       
13125-3445   LDS 436     B is CD-34@8719.                                                                
                         SHY 615. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
13126+5827   STF1732     AB: SHY 616. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
13126-3207   SWR 138     CPM pair                                                                Skf2004 
13126-6034   WSI  75     Primary is V1266 Cen, eclipsing binary of Beta Lyr -type, period                
                         10.1572 d.                                                              Zas2012 
13127-1619   ALD  50     RST 3826.                                                                       
13127-3152   MUG   3     AB are CPM. Followup spectroscopy confirmed the B component is a                
                         dwarf; estimated mass is 0.253 +- 0.011 Msun.                           Mug2005 
                         HIP 64459. B at 8" is MUG 3, physical. Confirmed by ANDICAM images.     Tok2011a
                         Exoplanet host, P=1135d                                                 Tok2014d
13129-5949   COO 152     LDS 435.                                                                        
             HDS1850     Aa,Ab: Hipparcos parallax 23.72 +/- 0.60 mas. Dynamical parallax 23.6           
                         mas, masses 1.56 and 0.79 Msun. This is a chromospherically active G0V          
                         dwarf and a ROSAT X-ray source. There are at least four components in           
                         the system: Aa1,Aa2 is a double-lined spectroscopic and eclipsing               
                         binary with 4.2 d period, Aa,Ab is the pair considered here, and the            
                         visual companion B at 25.5" is physical. The orbits of Aa1,Aa2 and              
                         Aa,Ab may be co-planar.                                                 Tok2012b
                         Aa,Ab: GJ 2099. Aa is SB2E, P=4.233d                                    Tok2014d
13130-1223   LDS6274     NLTT 33271/33270                                                        Chm2004 
13131+1801   S   648     B is BD+18@2703.                                                                
                         This cannot be the close 401.5-d spectroscopic binary.                  Grf2014a
13132-0233   STF1731     AB: HJL 184.                                                            HJL1986 
             TOK  69     Aa,Ab: Estimated masses 1.09 and 0.71 Msun; sep 20.6 au, period 70 y.   Tok2010c
13132-0501   TOK 402     HIP 64499 has a variable RV, with a preliminary spectroscopic orbit             
                         of 17yr period (Latham 2012, private communication). It is resolved at          
                         0".1 and shows no motion in one month.                                  Tok2015c
13132-0742   LDS4326     NLTT 33282/33283                                                        Chm2004 
13133+3709   LDS4327     NLTT 33310/33311                                                        Chm2004 
13133+1621   DOC   1     Orbital parallax is 7.63 +/- 0.30 mas. Mass of the primary is                   
                         1.240 +/- 0.224 \msun. Mass of the secondary is 1.134 +/- 0.183 \msun.  Doc2018h
13134-1850   SHJ 161     54 Vir. Both components are spectroscopic binaries. Primary is LM Vir,          
                         a W UMa eclipsing binary (period 0.9876 day). Aka H 2  45.              Zas2011 
                         Erroneously called SHJ 151 in BDS (#6422) and ADS (#8824).              MEv2010 
13134-5042   I  1227     Fairly rapid retrograde motion.                                                 
13135+6717   STFA 25     AB: Spectrum K2III+K2III.                                                       
                         Position of C: 13 13.0 +67 19.                                                  
                         AB: HJL1076.                                                            HJL1986 
13136+5643   SHY 246     AE: HIP  64532 + HIP  65327.  E component = F component of 13239+5456           
                         and A component of 13234+5754.                                                  
             SHY 246     AF: HIP  64532 + HIP  61100.  F component = G component of 13239+5456.          
13137+2949   HO   55     Frequent failure to see the companion is probably due to the large              
                         magnitude difference.                                                           
13139+1125   BPMA 46     [PM2000] 1051722 + [PM2000] 1051735.                                    Gvr2010 
13140+1409   BPM 601     [PM2000] 1051749 + [PM2000] 1051799.                                    Gvr2010 
13141+0619   LDS6275     GIC 104 = G062-019/G062-020. A typographical error led to this pair             
                         being originally entered in the WDS as 12141+0617GIC 104.                       
13142+5841   LDS2672     NLTT 33377/33378                                                        Chm2004 
13143+1320   LAW   2     Distance 9.8 +/- 2.0 pc                                                 Law2006 
                         NLTT 3370. Schlieder et al. (2014) derive the following properties for          
                         the A and B components:                                                         
                            log (L/Lsun)         -2.64 +/- 0.06        -2.68 +/- 0.06                    
                            Teff (K)             3200 +/- 500          3100 +/- 500                      
                            Mass (Mjup)          97 +41/-48            91 +41/-44                SJE2014 
                         Recently, Schlieder et al. (2014) reported NLTT 33370 as a binary. In   SJE2014 
                         NACO images approximately coincident with the AstraLux images, the              
                         projected separation of the binary is ∼75 mas, which is consistent      .     
                         with the fact that the binary is unresolved in the AstraLux images.     Jnn2014 
                         Dupuy et al. (2016) derive an orbit for LSPM J1314+1320AB using                 
                         astrometry from Keck/NIRC2 and the VLBA. Derived parameters for A and           
                         B are as follows:                                                               
                            Mass (Mjup)          92.8  +/- 0.6         91.7  +/- 1.0              .      
                            Age (Myr)            79.9  -2.7/+2.5       81.7  -3.3/+2.9            .      
                            Teff (K)             2954  +/- 3           2947  +/- 4                .      
                            Radius (Rjup)        1.831 +/- 0.018       1.808 +/- 0.018            .      
                            log(g) (cm/s^2)      4.836 +/- 0.010       4.842 +/- 0.011            .      
                            Li/Li_init           0.12  -0.05/+0.03     0.17  +/- 0.07             .      
                            Mbol (mag)           11.290 +/- 0.025      11.328 +/- 0.025           .      
                            log (Lbol/Lsun)      -2.616 +/- 0.010      -2.631 +/- 0.010           .      
                         Parallax is 57.975 +/- 0.045 mas, distance 17.249 +/- 0.013 pc, the             
                         integrated spectral type M7.0 +/- 0.2 (optical), M6 +/- 1 (near-IR).    Dup2016 
13143-5906   FIN 205     Unresolved at SOAR on 2013.13 (but in small field), remains                     
                         unconfirmed.  A is possible SB.                                         Tok2014d
13144+2358   POU3134     LDS2907.                                                                        
13145-2417   FIN 297     Inclination corrected from 65.6 to 66.6 by Ruymaekers & Nys (1995)      Ruy1995 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 0.94 +/- 0.48, 3.32, and 1.45 Msun, respectively.  Mlk2012 
13147-6335   MLO   3     Spectroscopic binary.                                                           
             WSI  58     Aa,Ab: One component of the 0.24" pair is a 13.6d SB1 (Sota et al.              
                         2014, ApJS 211, 10).                                                    Sna2014 
13149-1122   SHJ 162     AB: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
13151+2725   B     1     LDS2908.                                                                        
13151+2621   GIC 112     LDS1373.  G149-062/G149-061.                                                    
13152-6754   DUN 131     eta Mus. The primary is a spectroscopic binary and a possible                   
                         eclipsing system.                                                               
13153-0250   JNN  91     LP 617-21.                                                                      
                         Due to the small separation of companion to 2MASS J13151846-0249516 it          
                         is very likely a physical binary, but common proper motion has not yet          
                         been tested for.                                                        Jnn2012 
13155-2650   BUG  14     Estimated spectral types are L3.5 +/- 2.5 and T7 +/- 0.6.  System age           
                         > 0.8-1.0 Gyr, estimated distance 19 +/- 3 pc.  Effective temperatures          
                         are 1760 +/- 70 and 790 +/- 70 K. For an age of 1 Gyr, masses are               
                         60 +/- 6 and 16 +/- 3 Mjup.                                             Bug2011b
13157+1154   AG  435     Single.                                                                 IDS1963A
13161-6235   HD 115071   V961 Cen. Hipparcos has shown this star to be an eclipsing binary with  HIP1997a
                         a period of 1.37d.  Both Penny (1996) and Howarth et al. (1997 MNRAS    Pny1996b
                         284, 265) found evidence of line-doubling.  Turner (1985 ApJ 292, 148)          
                         shows that this star appears close to and has a similar distance to             
                         the cluster Stock 16.                                                   Msn1998a
13163+1715   STF1733     BDS 6440, H 2  46.                                                              
13164+4202   HJ 1230     HJ observes HJ 1230: 1828 290@ 12" 11-11.                                       
13164+2906   LDS6276     HZ 43.                                                                  McA1996b
                         The 1977.10 observation of this system published by McAlister in 1996           
                         was a re-reduction of archival USNO-NOFS data by V.V. Kallarakal.               
                         Evidently, the 1974.345 and 1975.415 data were also from this source,           
                         and were reduced and added by Worley.                                   Wor9999 
13166+1948   HDS1862     1988.1655: Unresolved upon initial inspection (McAlister 1993), a very  McA1993 
                         weak peak was later found which agreed well with the Hipparcos                  
                         measurement.                                                            Msn1999b
             BGH  46     AB: HJL1077.                                                            HJL1986 
                         AB: SHY 617. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
13168+0925   KUI  62     59 Vir.                                                                         
             GJ  504     Aa,Ab: Kuzuhara et al. (2013) image a cold Jovian exoplanet orbiting            
                         the solar-type star GJ 504. Distance to the system is 17.56 +/- 0.08            
                         pc. They derive masses 1.22 +/- 0.08 Msun and 4.0 +4.5/-1.0 Mjup for            
                         the star and planet. The effective temperatures are 6234 +/- 25 and             
                         510 +30/-20K, spectral types are G0V and late-T/early-Y.                Kuz2013 
13169+1701   BU  800     Hyperbolic orbit by Hopmann (1960).                                     Hop1960b
                         sigma = areal constant in the true orbit = 0.2700 arcsec^2/yr                   
                         q = periastron distance in the true orbit = 5".0334                             
                         All hyperbolic orbits rejected from Fourth Orbit Catalog                Wor1983 
                         HIP 64797. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AB: H 2  46.                                                            MEv2010 
                         AB: Additional notes may be found in Worley (1956).                     Wor1956b
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: Rectilinear solution by Friedman et al. (2011).                     USN2011a
13169-3436   I  1567     Also known as SEE 171.                                                          
                         Hipparcos parallax 23.18 +/- 1.10 mas. Dynamical parallax 22.7 mas,             
                         masses 0.96 and 0.84 Msun.  I 1567 has a well-established orbit by              
                         Heintz (1986) which is corrected here to better match the new speckle   Hei1986a
                         data. Heintz notes that this pair is a "puzzling case" because of some          
                         very discordant historical measures; these deviant points were ignored          
                         in the calculation.                                                     Tok2012b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.20 +/- 0.36, 1.81, and 0.95 Msun, respectively.             Mlk2012 
13170+3949   OSO  52     G164-061. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
13174-2132   BU  222     HDO 136                                                                         
13175-0041   FIN 350     This binary is comprised of a pair of F0V stars of near-zero magnitude          
                         difference, so there is considerable uncertainty as to whether the              
                         orbit is of short-period/high-eccentricity (P~9yr, e~0.6) or long-              
                         period/low-eccentricity (P~18yr, e~0.0). The rms residuals to the               
                         speckle observations are slightly smaller for the long-period orbit,            
                         but mass sums (a^3/P^2) for the two orbits differ by just 2%,                   
                         insufficient to rule out either solution on the basis of plausibility.  Hrt1994 
                         (Later speckle observations near periastron appeared to favor a short-          
                         period solution, but this is still uncertain.)                                  
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.39 +/- 0.31, 3.27, and 1.45 Msun, respectively.             Mlk2012 
13175-4033   I   425     Rectilinear solution by Hartkopf et al.  (2012).                        Hrt2012a
13178+4535   LDS4340     NLTT 33606/33599                                                        Chm2004 
13184-1819   H 6  90     61 Vir. H VI 90. Proper motion of A -1070 -1065.                                
                         B is BD-17@3815, proper motion -037 -010.                                       
                         Smyth's quoted separation is difference in RA only.                     Smy1844 
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
13186-6229   SNA  33     This new pair cannot be the 15.1d binary reported by Sota et al.                
                         (2014, ApJS 211, 10); HD 115455 is therefore at least a hierarchical            
                         triple system.                                                          Sna2014 
13187-5816   GAA  25     V963 Cen                                                                        
13189-2310   SMY   3     gam Hya = 46 Hya                                                                
13190-1514   LDS4343     NLTT 33649/33646                                                        Chm2004 
13193+1759   LDS4345     NLTT 33677/33673                                                        Chm2004 
13196+3507   HJ  529     AB: NLTT 33705/33706                                                    Chm2004 
13196+2422   LDS2913     NLTT 33701/33702                                                        Chm2004 
13198+4747   CHR 193     is also a spectroscopic binary with a P of 447d.                        Tok2019b
             HU  644     Beuzit et al. (2004) AO observations confirm speckle third component    Beu2004 
                         of Hartkopf et al. (1994). Mass sum and mass ratio (Heintz, 1969)       Hrt1994 
                         clearly requires the primary to be a closer binary.                     Hei1969c
                         Masses and bolometric magnitudes are derived for the two components     Msn1999a
                         of this system by Mason et al. (1999), based on assumed spectral types          
                         and available  parallaxes. The Hipparcos parallax appears suspect.              
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
             HU  644     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.76 +/- 0.13, 1.11, and 0.85 Msun, respectively.  Mlk2012 
                         Aa,Ab: 1992.3126: This appears to be a new component to the 1".5 49-yr          
                         period pair of K/M dwarfs HU 644. This is the only one of the current           
                         crop of new interferometric binaries which has not yet been confirmed.          
13199-2748   B   247     Spectrum: Fm delta Del.                                                         
13199-6831   JNN  92     2MASS J13195689-6831142 has companion detected in the AstraLux images.          
                         Since the companion is relatively close (~0.88") and has a brightness           
                         and color that is consistent with expectation, it is probably a                 
                         physical pair. Only one epoch of images exists so far.                  Jnn2012 
13203+1746   A  2166     Elongations doubtful, quadrant indeterminate.                           B__1963b
                         Primary is eclipsing binary KR Com (period 0.40796 day).                Zas2010 
                         Omega corrected from 0.0 to 180.0 by Ruymaekers & Nys (1995)            Ruy1995 
                         Zasche et al. (2010) derived a combined solution orbit, based on        Zas2010b
                         published astrometry plus minima timings of the close-contact                   
                         binary KR Com, which comprises the primary of the Aitken pair.                  
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 7.10 +/- 3.80, 2.75, and 1.10 Msun, respectively.             Mlk2012 
13203-0140   LDS 437     AB: NLTT 33750/33731                                                    Chm2004 
13203-0224   LDS4347     NLTT 33739/33741                                                        Chm2004 
13207+0408   BDK   6     G 62-33 + 2MASS J13204427+0409045. Distance 30.5 +/0 1.0 pc for                 
                         primary, 33 +/- 3 pc for secondary. Estimated age of system 3.3-5.1             
                         Gyr. Mass of secondary estimated at 0.079-0.081 Msun.                   Fah2010 
13208+3158   ES  308     SEI 535.                                                                Nsn2017b
13208+0956   BDK   7     G 63-23 + 2MASS J13204159+0957506. Distance 38.1 +2.6/-2.3 pc for               
                         primary, 36 +/- 3 pc for secondary. Estimated age of system 1.0-3 Gyr.          
                         Mass of secondary estimated at 0.083-0.093 Msun.                        Fah2010 
                         NLTT 33793 + 2MASS J13204159+0957506. Baron et al. (2015) estimate              
                         spectral types K5 and M8, distances 38.1 +2.6/-2.3 and 36 +/-3 pc,              
                         masses 0.724-0.782 and 0.087-0.096 Msun.                                BFr2015 
13209+4359   GC 18063    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
13216-0926   BRT 447     It appears that a possible 0.3s error in the RA of the primary may be           
                         the cause of the incorrect 1895 measure.                                        
13217+1542   FOX 177     HJL 185.                                                                HJL1986 
13218+1746   STF1737     BDS 6463, H IV 57.                                                              
                         H 4  57.                                                                MEv2010 
13218-1845   GC 18075    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
13220+6748   GRV1087     SLW 862.                                                                        
13224+7011   LDS1767     NLTT 33937/33932                                                        Chm2004 
13224+1603   BPM 602     [PM2000] 1055415 + [PM2000] 1055437.                                    Gvr2010 
13225-2257   ARG  26     B is BD-22@3573, spectrum G1/2V.                                                
             SHY 618     AC: HIP  65266 + HIP  64670.                                                    
13226+2607   HO  259     AB: A is astrometric binary.                                            Tok2014d
13226-6059   FIN 208     Too close, measures uncertain. One component is the variable V790 Cen.          
13228+6442   LDS2674     NLTT 33948/33949                                                        Chm2004 
13228+4459   KZA  58     16' error in WDS designation.                                                   
13228-1311   H 4 119     H IV 119. B is BD-12@3801. Also known as STF1736. A is a spectroscopic          
                         binary, called "mild Am" by Bidelman.                                           
13229+8932   HJ 3154     2000 position deduced from 1830: 22 47.4 +89 28.                                
13229-1236   LDS 440     Aka GWP1998.                                                                    
13229-7209   B  1736     Spectroscopic binary.                                                           
13230+3141   LDS1386     NLTT 33927/33931                                                        Chm2004 
13233+0344   HDS1878     This is the pair BAL2857 only noted on a 1910 AC-plate.                 Dam2016c
13234+5754   SHY  67     AB: HIP  65327 + HIP  59496.                                                    
13235+2914   HO  260     Undetermined (long) period in nearby K-dwarf pair.                              
                         Baize (1968) elements are provisory. Third body (P of order 30 yr)              
                         is suspected.                                                           Baz1968 
13235+1401   HJ  226     AB is galaxy NGC 5129.                                                          
13237+0243   STF1740     B is BD+03@2766.                                                                
                         HJL 186.                                                                HJL1986 
13237-0043   A  2489     A premature orbit has been computed.                                            
                         T has been revised to comply with recent quadrant determinations.       Zul1972a
13239+5456   STF1744     A is zet UMa = Mizar. B is 80 UMa = Alcor.                                      
                         Split by Benedetto Castelli. After resolving AD in                      C__1616 
                         1617 he wrote to his friend, Galileo, to observe the pair, "It's one of C__1617 
                         the beautiful things in the sky and I don't believe that in our pursuit         
                         one could desire better." Galileo measured it in early 1617. See the    G__1617 
                         excellent discussion of its discovery in Leos Ondra's July 2004 Sky &           
                         Telescope article, from which Galileo's measure was extracted. It was           
                         independently found double in 1650 by Jean Baptiste Riccioli in         Ric1651 
                         Bologna: "There appears to be one star in the middle of the Great               
                         Bear's tail, where there are actually two, as the telescope reveals."           
                         This was also the first to be observed photographically, by John A.             
                         Whipple with the Harvard 15inch on 27 April 1857. According to Aitken,          
                         this was the first observed photographically (G.P. Bond at Harvard      A__1935f
                         College Observatory in 1857 using an 8 second exposure on a collodion   BdG1858a
                         plate), and the first spectroscopic binary discovered (E.C. Pickering   Pck1890 
                         in 1889). A is a spectroscopic binary, P = 20.54d (first orbit 1901).   Vog1901 
                         B is also a spectroscopic binary (first orbits 1908), P  = 175.6d,      XXX1908a
                         spectrum A1m or A1/A2/A7. Also, common proper motion with 80 UMa        XXX1908b
                         80 UMa (Alcor) and other members of the Ursa Major stream.                      
                         AC: SHY 247. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
             PEA   1     Mistakenly given the discoverer designation 'MKT   8' in the WDS,       Pea1925 
                         but actually first resolved by Pease in 1925, six decades before the            
                         Mark III interferometer measures. This system has completed some 1,350          
                         revolutions since its first resolution, probably a record for any               
                         "visual" binary.                                                                
                         The orbit of Aa,Ab by Russell (1927) is combined interferometric/       Rus1927 
                         spectroscopic (double-lined spectrum). A small magnitude difference             
                         (which would probably place the ascending node in the second quadrant)          
                         is uncertain.                                                                   
                         Star B (mag. 3.96, 15") is physical, and is itself a 175.55d SB1.               
                         Visual orbit by Hummel et al. (1995) is based on astrometry from the    MkT1995 
                         Mark III interferometer. Additional spectroscopic data yield component          
                         masses, luminosities, radii, effective temperatures, and distance.              
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
             SMR  4      AD: This was the first component of Mizar split by Benedetto Castelli   C__1616 
                         in late 1616. It was called "Sidus Ludoviciana" (Ludwig's Star) by      XXX2004 
                         Johann Georg Liebnecht for the Landgrave Ludwig of Hessen-Darmstadt             
                         who thought he has discovered a planet. He was wrong.                           
             SHY 247     AE: HIP  65378 + HIP  64532.  E component = A component of 13136+5643           
                         = C component of 12487+6019.                                                    
             SHY 247     AF: HIP  65378 + HIP  65327.  F component = D component of 12417+5543.          
             SHY 248     CE: HIP  65477 + HIP  64532.                                                    
             SHY 248     CF: HIP  65477 + HIP  65327.                                                    
             SHY 248     CG: HIP  65477 + HIP  61100.  G component = G component of 13136+5643.          
             SHY 248     CH: HIP  65477 + HIP  61481.                                                    
             STF1744     AB: H 3   2.                                                            MEv2010 
13240-2055   BU  610     HDO 137. Spectrum: K1/2III/IV.                                                  
13242-0159   GLP   9     B is BD-01@2813.                                                                
13244-0219   SKF 988     Variable IN Vir.                                                                
13245+1226   GC 18139    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin (1986).                                                         Grf1986c
13245-2837   BRT3000     Not found by Heintz at IDS position.                                    Hei1990b
                         A likely plate flaw.                                                    Grv2021b
13246-0510   66 Vir      Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
13246-5130   I  1231     Too close after 1927. Needs speckle.                                            
13246-5557   JNN 155     Secondary appears to be a brown dwarf; masses are estimated at 1.3              
                         Msun and 65 +35/-30 (based on intrinsic brightness) or 45 +/- 10 Mjup           
                         (based on temperature).                                                 Jnn2012b
13247+1755   BPM 603     [PM2000] 1056418 + [PM2000] 1056405.                                    Gvr2010 
13250+0146   GRV1088     SLW 868.                                                                        
13251+2351   SHY 620     HIP  65466 + HIP  65508.                                                        
13252-1110   BUP 150     alp Vir = 67 Vir = Spica. A is an Alpha CVn-type variable and                   
                         spectroscopic binary, spectrum B1III-IV+B2V. According to R.G. Aitken,  A__1935f
                         this is the fourth binary recognized by spectroscopic methods. It was           
                         identified as such based on photographic spectra obtained by Prof.              
                         H.C. Vogel at Potsdam in early 1890. It has been resolved by intensity          
                         interferometry.                                                                 
                         Intensity Interferometer Limb-darkened diameter 0.87 +/- 0.04 mas.      HBr1974 
                         AC. Smyth's quoted separation is difference in RA only.                 Smy1844 
13252-6429   HJ 4583     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
13253+7559   STT 267     Position angles scattered, mostly near 150@. Quadrant uncertain.                
                         Probably in rapid motion.                                               B__1963b
13253+4028   HJ 1231     This is a measure of A and BD+41@2392.                                          
13254-4300   DBR 179     Not a double star, but the Globular Cluster Sersic 13 in NGC 5128.              
13254-5947   WSI  76     A = V379 Cen, eclipsing binary of Algol-type, period 1.874696 days.     Zas2015 
13258+4430   A  1609     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.47 +/- 0.63, 1.91, and 0.85 Msun, respectively.  Mlk2012 
13258-4815   JNN 156     V966 Cen. Secondary appears to be a brown dwarf; masses are estimated           
                         at 1.3 Msun and 55 +30/-20 (based on intrinsic brightness) or                   
                         70 +35/-15 Mjup (based on temperature).                                 Jnn2012b
13258-7038   67 Mus      Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Dworetsky (1982).                                                       Dwo1982 
13264+2334   LDS5779     NLTT 34105/34116                                                        Chm2004 
13264-4303   HJ 4587     SWR 140. CPM pair                                                       Skf2004 
13265+4233   ES 2645     B is BD+43@2334.                                                                
13267-2418   BGH   6     SHY 249. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
13270-7710   GLI 291AB,C #190 in the original list of Gilliss.                                           
13271+6444   STTA123     LDS2675.                                                                        
                         AB: HJL 188.                                                            HJL1986 
                         AB: SHY 622. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
13271+3840   LDS4364     aka RAO 294.                                                                    
13273-3111   DAE   4     GJ 3786 = LHS 2739                                                              
                         Daemgen et al. (2007) derive a distance of 30.2 +/- 7.7 pc, separation  Dae2007 
                         of 16.4 +/- 4.2 au, and a predicted orbital period of 108 +/- 43 yr.            
                         Spectral types for both stars are M3.5 +/- 0.5; masses are 0.33                 
                         +0.10/-0.09 and 0.30 +0.11/-0.09 Msun.                                          
13274-2138   LDS6278     NLTT 34137/34150                                                        Chm2004 
13274-6152   B  2752     A is an Algol-type system, V380 Cen.                                            
13276+0655   HJ 1232     HJL 187.                                                                HJL1986 
13280-5806   R   217     Despite the linear solution, proper motion and parallax favor a         Grv2020a
                         physical connection. Long period and/or high eccentricity possible.             
13283-0222   B  2753     LDS5781 aka OSO  48AC.                                                          
                         NLTT 34200/34203                                                        Chm2004 
13284+1543   STT 266     Scardia et al. say the quadrant is unambiguous for their 2004 theta     Sca2005a
                         value of 178.1; this does not agree with other determinations of                
                         magnitude difference, however.                                                  
13284+1347   STT 579     AB: 70 Vir. B is BD+14@2622.                                                    
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             RBR  18     2001.0994: PA is measured in zenith mode. If data collected in                  
                         equatorial mode, PA = 241.2. Confirmation of the pair should establish          
                         the correct theta value.                                                Rbr2011d
                         CHARA Array Limb-darkened diameter  1.009 +/- 0.024 mas,                CIA2008c
                         R =  1.968 +/- 0.047 \rsun.                                                     
             70 Vir      A: Combined solution, based on reduction of Hipparcos intermediate              
                         astrometric data together with spectroscopic elements from Marcy &      CPS1996a
                         Butler (1996).                                                          HaI2001 
13285-4829   SWR 141     CPM pair                                                                Skf2004 
13286+4246   BRT 108     A likely plate flaw.                                                    Grv2021b
13288+5956   S   649     CA: HJL1079.                                                            HJL1986 
                         CA: SHY 623. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         CA: H 6  22.                                                            MEv2010 
13289+2131   LDS 948     GIC 113. G149-090/G149-089 = NLTT 34235/34234.                          Chm2004 
13291-6441   GC 18206    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
13291-6604   LDS 444     B is CPD-65@2344.                                                               
                         SHY 624. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
13293+6452   LDS2321     NLTT 34300/34302                                                        Chm2004 
13295+5142   JNN  93     The B component seen in the AstraLux images appears to be a very close          
                         binary itself due to a PSF extension visible in five separate epochs.           
                         However, we count the system as a regular binary here since we do not           
                         get a converging fit for the closer pair.                               Jnn2012 
13297-2317   HO  381     A is a Mira-type variable, R Hya.                                               
                         A has a magnitude range of 3 to 11 with a period of 388.0 days.                 
                         B has a B-V (U-B) color of 1.04 (0.97)                                  Egg1971 
13298+0106   J  2091     A is FO Vir, an eclipsing Beta Lyrae-type binary, period 0.77557d.      Zas2011 
13300-7634   RSS  18     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
13303-0834   LDS 448     Proper motion -1093 -419.                                                       
                         Primary is white dwarf WD 1327-083.                                     Far2005b
13304+4010   LDS5782     LDS6279.                                                                        
                         NLTT 34325/34326                                                        Chm2004 
13304-0628   STF1750     72 Vir. A is a spectroscopic binary.                                            
                         H N  27.                                                                MEv2010 
13304-1256   HJ 2656     Rectilinear solution by Hurowitz et al. (2014).                         USN2014a
13304-7851   HD 116852   The classification is from Morgan et al. (1955 ApJS 2, 41). Sembach &           
                         Savage (1994 ApJ 431, 201) suggest that the star lies at 1.3 kpc from           
                         the Galactic plane, so we have assigned it to the "runaway" category.   Msn1998a
13305+2231   SHY 626     HIP  65899 + HIP  65884.                                                        
13305+0729   A  1789     Ma,Mb = 1.581 +/- 0.040, 1.503 +/- 0.036 \msun.                         GmJ2022 
13305-2339   HO  540     A is an Algol-type system, SS Hya.                                              
13306-4311   CPO 371     Nothing at this position, according to Heintz.                          Hei1987a
                         A likely plate flaw.                                                    Grv2021b
13309+2414   STT 268     AB: A is possible SB, no orbit.                                         Tok2014d
             H 5  70     AC: STTA124.                                                                    
                         AC: H V 70. C is the variable FK Com.                                           
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
13310+3626   HLM   5     Also known as STF1753.                                                          
13310-3924   SEE 179     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical and spectroscopic masses                  
                         15.46 +/- 7.56 and 8.91 Msun, respectively.                             Mlk2012 
13311+1216   UC 2550     TYC 895-616-1, W UMa-type eclipsing binary, period 0.21801 d.           Zas2018 
13316+5857   TOK 290     We count 2MASS J13313493+5857171 as single close in, although its PSF           
                         appears somewhat extended in the 2009.13 epoch. However, it is a                
                         likely companion to the nearby G2-star HD 117845 at 11" separation.             
                         HD 117845 has been included in the AstraLux field and appears to be             
                         itself a close binary with a ~0.5" separation.                          Jnn2012 
                         AB: A is SB, no SB orbit. X-ray source.                                 Tok2014d
13316-6135   HDS1894     Primary is Cepheid V659 Cen.                                                    
                         Masses are 5.2 and 4.4 Msun. Estimated period = 3400y,                          
                         a = 500au = 0.67".                                                      Evs2013 
13317-0219   HDS1895     Horch et al (2012) generate two possible orbits, one based on only      Hor2012a
                         astrometry, the second "constrained" solution fixes P, T, e, and Omega          
                         to values determined in a spectroscopic orbit by Torres et al. (2002).  Trr2002 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.27 +/- 0.49, 1.75, and 0.88 Msun, respectively.             Mlk2012 
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Latham et al. (2002). They derived component masses 0.93 and 0.42 Msun  Lat2002 
                         and an estimated semimajor axis of 95.29 mas.                           Ren2013 
13320+3108   WOR  24     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.37 +/- 0.39, 1.20, and 0.55 Msun, respectively.             Mlk2012 
13320-1844   B  2542     73 Vir.                                                                         
13320-6519   FIN 369     In rapid direct motion.                                                         
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.13 +/- 0.94, 2.57, and 1.70 Msun, respectively.             Mlk2012 
                         Docobo & Andrade (2013) derive a dynamical parallax of 15.87 +/- 1.35           
                         mas and component masses 1.14 +/- 0.37 and 1.08 +/- 0.36 Msun. See              
                         paper for extensive notes on this system.                               Doc2013d
13321-1115   TOK 291     No previous indication of binarity was available for HIP 66018, apart           
                         from the CPM companion B at 84". We discovered another faint component          
                         Ab at 0".89, dI=4.6, likely to be physical (low background density).            
                         The B component  (V=14.8) was targeted, but its speckle signal was              
                         weak and no obvious close companions to B were found.                   Tok2015c
13321-2258   HJ 4593     B is BD-22@3617, spectrum F2IV.                                                 
13321-6303   DUN 137     RMK  17. Rectilinear solution by Letchford et al. (2018).               LRR2018a
13322+0744   LDS3074     SLW 887.                                                                        
13324+3649   STF1755     Spectroscopic binary. Spectral type of B: F5IV.                                 
13324-1240   SHJ 165     B is BD-11@3537.                                                                
                         H 5 128.                                                                MEv2010 
13327+3100   LDS1392     NLTT 34410/34417                                                        Chm2004 
13328+1649   VYS   6     LDS4374. Both components are flare stars, VW Com.                               
13328-1746   HU  469     Includes LV Vir, a W UMa type eclipsing binary, P = 0.40943d.           Zas2012 
13329+4143   LDS4375     NLTT 34434/34433                                                        Chm2004 
13329+3454   STT 269     1986.397: The separation of this partially resolved pair was                    
                         calculated under the assumption of zero or otherwise known magnitude            
                         difference.                                                             Tok1985 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 5.23 +/- 1.58, 3.13, and 2.06 Msun, respectively.  Mlk2012 
13329-1522   HJ 2658     75 Vir.                                                                         
13332-7734   HJ 4590     LDS 447. A is a variable, S Cha. B is CPD-76@769.                               
13333+2301   STF1756     HJL 189.                                                                HJL1986 
                         W UMa-type eclipsing binary, period 0.35253 d.                          Zas2018 
13337+4801   ODE  11     HJL1080.                                                                HJL1986 
13340-6403   KRV  35     Classical Cepheid VW Cen.                                                       
13341+6746   STF1767     LDS1393.                                                                        
                         NLTT 34535/34534                                                        Chm2004 
13343-0019   STF1757     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
13344+3847   HJ 1234     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
13344-5931   TOK 403     HIP 66230 has a variable RV in GCS and an astrometric acceleration. We          
                         resolved it at 0".1, dI=2.5, estimated period ~10yr. The pair moved by          
                         4deg in one month.                                                      Tok2015c
13345-1326   S   650     B is BD-12@3842.                                                                
13346+1726   BPM 604     [PM2000] 1060833 + [PM2000] 1060846.                                    Gvr2010 
13347-0036   HNK   7     zet Vir = GJ 3792. Observations over 4.75 years indicate pair has               
                         common proper motion and shows clear evidence of orbital motion.                
                         Hinkley et al. (2010) constrain elements a > 24.9au, P > 124yr, and     Hnk2010 
                         e >0.16. Mass of the companion is estimated at 0.168 +0.012/-0.016              
                         Msun, suggesting a spectral type of M4V-M7V.                                    
                         CHARA Array Limb-darkened diameter  0.852 +/- 0.009 mas,                CIA2012e
                         R =  2.079 +/- 0.025 \rsun, L = 17.885 +/-0.252 \lsun,                          
                         Teff = 8247 +/-  52 K, M = 1.940 +/- 0.006 \msun,                               
                         Age =  0.7 +/- 0.0 Gyr.                                                         
13347-1313   BU  932     y Vir. Variable?                                                        Mlr1956a
                         Only elements P, T, and a have been amended by Starikova (1980) from    Sta1980a
                         the orbit of Heintz (1969).                                             Hei1969a
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Measures hard to reconcile. There has been practically no change in             
                         the last 10-12 years, yet the present position differs by some 290deg           
                         from Burnham's discovery position in 1879. Some of the measures are             
                         evidently spurious.                                                     VBs1954 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 13.50 +/- 8.22, 5.27, and 2.24 Msun, respectively. Mlk2012 
13347-6320   HDS1907     The classification is from Garrison et al. (1977 ApJS 35, 111).         Msn1998a
13348+3711   BH CVn      Close binary comprised of F2IV primary and K2IV secondary. Orbital              
                         elements are from Eker & Doherty (1987 MNRAS 228, 869) except for the           
                         ascending node. The Eker & Doherty inclination was corrected for CW             
                         rotation determined by Abbuhl et al. (2015)                             Abb2015 
13349+7430   LDS1775     B component is NLTT 34606.                                                      
                         Possible common proper motion with BD+75@510, about 1900" distant.              
                         G255-038.  Besides the known companion at 14.275", Gliese & Jahreiss    GJ_1988 
                         list this star as a wide companion to G255-034, separated by 33'.               
                         However, the different Hipparcos distances to G255-038 and G255-034,            
                         and the different measurements of mu_delta, suggest that the two stars          
                         are not related.                                                        Oso2004 
             PRB   4     C, D, and E components are NLTT 34503, NLTT 33451, and WD 1337+70 =             
                         NLTT 34829, respectively. E is also the primary of 13388+7017 KUI 122.          
                         All are possible CPM pairs, according to Probst (1983).                 Prb1983 
13349+3746   DAE   5     CLS 73 = 2M1334                                                                 
                         Daemgen et al. (2007) derive a distance of 35.8 +/- 9.4 pc, separation  Dae2007 
                         of 2.9 +/- 0.9 au, and predicted orbital period of 8 +/- 4 yr.                  
                         Spectral types for both stars are M3.5 +/- 0.5; masses are 0.34                 
                         +0.11/-0.10 and 0.30 0.10/-0.08 Msun.                                           
                         Although the close binarity of 2MASS J13345147+3746195 was reported in          
                         Daemgen et al (2007) and our AstraLux data have a similar sensitivity,  Dae2007 
                         the star appears single in our images. Since the separation was only            
                         82 mas in 2006, it has presumably moved inward since then.              Jnn2012 
13356+1012   HJ  228     B is BD+10@2566.                                                                
                         HJL 190.                                                                HJL1986 
13358-2807   TDS8890     Galaxy 6dFGS gJ133548.0-280642.                                                 
13360+4829   FAR  38     GJ 2103. SKF 319.  Primary is white dwarf WD 1333+487.                  Far2006 
13360+0112   OSO  54     G062-052. Not a common proper motion pair, based on color and                   
                         comparison with POSS2 red plates.                                       Oso2004 
13363+3514   KZA  71     WDS garbled (dec copied from KZA 70)                                            
13364+2156   LDS4381     NLTT 34611/34612                                                        Chm2004 
13366-6433   HDS1909     KN Cen.                                                                         
13367+3555   KZA  72     15' error in WDS designation                                                    
13368-2630   H N  69     Spectral type of B: A7IV-V.                                                     
13368-3224   I   221     Rectilinear solution by Zirm (2013).                                    Zir2013d
13370+0751   VBS  23     LDS3082 = LDS4382.                                                              
13371-1627   RST3845     Spectrum: F2/3III/IV.                                                           
13372+3005   STF1766     LDS1394.                                                                        
                         HJL 191.                                                                HJL1986 
13372-2337   TOK 852     TV Hya.                                                                         
13372-6142   I   365     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.39 +/- 1.84, 2.57, and 1.17 Msun, respectively.  Mlk2012 
                         A 8.1d spectroscopic solution for the A component has been found        Tok2019g
                         making this a triple system (C component is optical).                           
13372-8427   HJ 4585     B is CPD-83@531.                                                                
13374-1204   LDS4384     NLTT 34648/34647                                                        Chm2004 
13375+3618   STF1768     25 CVn. AB: Malkov et al. (2012) derive dynamical, photometric, and             
                         spectroscopic masses 4.61 +/- 2.52, 3.03, and 1.82 Msun, respectively.  Mlk2012 
13376-0752   STF1763     AB: H 1  80.                                                            MEv2010 
13377+5043   STF1770     Composite spectrum; M2II-III+F3III.                                             
13377+0223   STF1764     C and D components are A and B of STF 1765 rej. WAL  64CD measures              
                         moved, but systems not merged, as optical/physical nature of STF1764AC          
                         and WAL  64AD are unknown.                                                      
13377-2337   RST2856     In rapid motion, but quadrant ambiguity makes interpretation uncertain          
                         Two orbit solutions bu Heintz (1967); neither is clearly preferable.    Hei1997 
13378+2819   HJ 3341     AC: Possible error in original reduction?                                       
13379+4808   ES  608     At least one component is variable.                                             
13379+0221   STF1765     WAL  64CD. Systems not merged, as optical/physical nature of STF1764AC          
                         and WAL  64AD are unknown.                                                      
13381+3910   STF1769     AB: A is SB1, P=11.589d                                                 Tok2014d
                         C is BD+39@2662.                                                                
                         AC: HJL 192.                                                            HJL1986 
                         AC: Additional notes may be found in Baize (1936).                      Baz1936c
             TOK  29     AE is CPM. Primary is 11.6d SB1. C component is known CPM; D component          
                         found in 2MASS, confirmed CPM by POSS (approximate 1950 measure: 9.3",          
                         230deg). A is triple, the whole system is quintuple. Metal-poor, high           
                         proper motion.                                                          Tok2006 
                         AE: A,C are on the MS, E below. E is optical or WD?                     Tok2014d
             STF1769     AB: Rectilinear solution by Hartkopf & Mason (2013).                    Hrt2013b
13382-2341   LDS4385     AB + TOK 404Aa,Ab:  HIP 66530 has a variable RV according to the GCS.           
                         It is resolved at 0".16 in the I band only, estimated period ~20yr.             
                         This is a triple system, considering the CPM companion B at 28".        Tok2015c
             TOK 404     Aa,Ab: SB, no orbit                                                     Tok2014d
13383-6416   HRG  88     Aka WFC 138.                                                                    
13385-1042   J  3001     Galaxy PGC 48213 = MCG-02-35-011.                                               
13387+3823   COU1429     The KZA pairs are probably wider companions.                                    
13388+1913   LDS4386     NLTT 34761/34772                                                        Chm2004 
13389+1807   BPM 605     [PM2000] 1062803 + [PM2000] 1062804.                                    Gvr2010 
13390-1052   LDS6280     Ross 479                                                                        
13392-4900   HJ 4600     B is CD-48@8376.                                                                
13395+5255   VIG  16     Optical/physical nature of the faint companion is undefined.            Vig2012 
13396+1045   BU  612     Masses and bolometric magnitudes are derived for the two components     Msn1999a
                         of this system by Mason et al. (1999), based on assumed spectral types          
                         and available parallaxes.                                                       
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.41 +/- 0.36, 3.27, and 1.40 Msun, respectively.  Mlk2012 
13399-5328   RST5376     eps Cen                                                                         
                         Intensity Interferometer Limb-darkened diameter 0.48 +/- 0.03 mas.      HBr1974 
13400+3759   KZA  76     AC: Error in RA caused resulting incorrect measure by Kazeza.           KZA1984 
13403-5737   KRV  36     Classical Cepheid XX Cen.                                                       
13404+5031   STF1774     GJ 521.2. A is X-ray source. Debris disk? In Duquennoy & Mayor (1991).  Duq1991 
13407+7651   HJ 2682     C is BD+77@518.                                                                 
13407+5944   HJ 2673     B is BD+60@1481.                                                                
13407+1957   STF1772     1 Boo. B is a metallic-line star.                                               
13408-1748   SHY 630     HIP  66749 + HIP  66717.                                                        
13401-6033   TOK 292     HIP 66676 (A) and HD 118735 (B, G6V, V=9.17) at 77" share common PM             
                         (although it is small, 58mas/y) which, together with photometry,                
                         indicates with high probability that it is a  physical pair AB                  
                         (Tokovinin & Lepine 2012). We targeted the secondary component B and    Tok2015c
                         found it to be a resolved triple. The faint star C, at 0".92 from B,            
                         is itself a close 0".16 pair Ca,Cb.  Note that this is a region of the          
                         sky with very high stellar density, raising suspicion that the Ca,Cb            
                         pair might be a random background object. Re-observation of the triple          
                         in 2015  (to be published) shows, however, that it is physical because          
                         the center of C=(Ca,Cb) moves relative to B with a speed of 11mas/y             
                         (or 3km/s), compatible with the expected orbital motion of BC and much          
                         less than the system's PM of 58mas/y. The estimated period of Ca,Cb is          
                         ~30 years, the period of BC is ~300 years.                              Tok2015c
13408-2815   HO  382     AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
13412-3053   BGG   1     2MASS J13411160-30525049. Bardalez Gagliuffi et al. (2015) resolved             
                         this very low -mass binary, and derived spectral types L2.5 +/- 1.0             
                         and T6.0 +/- 1.0. Depending on age, this pair has a projected                   
                         separation of 8.1 +/- 0.5 au and estimated orbital period of 63-85y.            
                         Mass estimates range from 0.052-0.075 Msun for the primary,                     
                         0.022-0.061 for the secondary.                                          BGg2015 
13413+3422   SKF  41     AB: FAR  65.                                                                    
13414-6152   JSP 591     Spectrum composite: K2/3III+B8/A0V.                                             
13417-7507   HJ 4598     Spectrum composite: A0V+G8/K0III.                                               
13422-1600   WSI 114     Also known as LHS2783 or GJ 3800.                                               
                         Parallax = 53.87 +/- 1.14 mas.                                          JLB2017 
                         Rectilinear solution by Miles & Mason (2016) &                          Msn2016b
                         Mason et al. (2018).                                                    Msn2018a
13422+1807   HJ  230     Rectilinear solution by Friedman et al. (2012).                         USN2012a
13427+3459   HR 5161     Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Beavers & Griffin (1979).                                               Bvr1979c
13430-3011   DAW 166     Possibly variable?                                                      B__1931b
13431+0332   STF1777     84 Vir. A is a spectroscopic binary.                                            
                         H 2  44.                                                                MEv2010 
13433-2458   HJ 2671     B is CD-24@11047.                                                               
13434+1341   BPM 606     [PM2000] 1064873 + [PM2000] 1064881.                                    Gvr2010 
13434-0556   LDS6281     NLTT 35007/35006                                                        Chm2004 
13435-0416   STF1775     A is a spectroscopic binary.                                                    
13440-5914   DUN 142     B is CPD-58@5094.                                                               
13441+1701   BPM 607     [PM2000] 1065196 + [PM2000] 1065149.                                    Gvr2010 
13443+6841   HJ 2685     Rectilinear solution by Hartkopf & Mason (2015).                        WSI2015 
13443-5101   VSP  40     V827 Cen.                                                                       
13444+2536   LDS5791     LDS6283.                                                                        
                         AB: NLTT 35070/35071                                                    Chm2004 
13446+5142   KUI  64     Ross 492.                                                                       
13446-1652   LDS6284     NLTT 35064/35065                                                        Chm2004 
13448-1403   BRT2736     A likely plate flaw.                                                    Grv2021b
13450+0206   HDS1935     B is also a 41d spectroscopic binary.                                   Tok2019b
13451+2512   BRT3300     Originally published as BRT 164.                                        Brt1928 
13451+1747   BUP 153     AB: Proper motion of A = +455.7 -1832.9 (Tycho).                                
                         Proper motion of B +012-014.                                                    
                         AC: Bu_1912 measures from 1875-1911 are Delta declination                       
                         (i.e., north-south vector separations).                                         
                         Proper motion of C -001-001.                                                    
13453+0903   BU  115     AB: B=SB? AC optical, shows reflex PM.                                  Tok2014d
13453-1031   S   652     AB: B is BD-09@3768.                                                            
                         Statistically the same parallax within the errors would indicate the            
                         components are physical.                                                        
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: C is BD-09@3766.                                                            
13454-4234   TOK 157     HIP 67121. A is SB without orbit (dRV=14.8).                            Nrd2004 
13456+7614   KPP3904     Aka MFL 100.                                                                    
13456-1546   HJ 2677     85 Vir. A is a spectroscopic binary and occultation triple.                     
13459-1226   BU  935     86 Vir.                                                                         
             STF1780     AC: Additional notes may be found in Burnham (1894).                    Bu_1894 
13461+3131   LDS5222     LDS5792 = LDS6285.                                                              
                         NLTT 35170/35180                                                        Chm2004 
13461+0507   STF1781     One of the stars is probably variable.                                  Baz1972 
                         One component is a W UMa-type eclipsing binary.                         Wor1956b
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         One component is a W UMa-type eclipsing binary. A is the variable HT            
                         Vir. Errors for orbit of Alzner (2007) provided by author (private      Alz2007 
                         comm.) With the Hipparcos parallax of 15.39 +/- 2.72 mas, the Alzner            
                         solution yields a mass sum of 3.98Msun.                                         
13462+3054   PIN   8     Primary is a spectroscopic binary.                                      Pin2006 
13466+2826   KOP   1     Djurkovitz suspected the primary of being a close double. It looked             
                         single to me.                                                           B__1963b
                         Pair is +1m28s, +10' from BD+28 2257. Kopal (1939) believes motion is   Kop1939 
                         orbital, with period ~700y.                                             Cou1956 
13467-3636   POL   8     POL 2 1/2.                                                                      
13467-5126   HDO 225     A is a long-period spectroscopic binary.                                        
             M Cen       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Jones (1928).                                                           Jon1928d
13470+3833   S   654     AB: STTA125. B is BD+39@2679.                                                   
                         HJL 194.                                                                HJL1986 
             SHY 633     AC: HIP  67250 + HIP  67041.                                                    
13470+0621   LDS3101     B is BD+07@2692.                                                                
                         HIP 67246. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         SHY 253. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
13472-4640   HRG  91     Aka SKF 468.                                                                    
13472-6235   COO 157     A semiregular variable, V766 Cen.                                               
             CSU   1     Aa,Ac: Chesneau et al. (2014) imaged a close companion to the                   
                         supergiant V766 Cen, using VLTI/AMBER. Based on visual photometry,              
                         they estimate the orbital period at 1304 +/- 6d.                        Csu2014 
                         Wittkowski et al (2017) used VLTI/PIONIER for followup H-band imaging.          
                         At the 2014 epoch they believe the companion was behind the primary.            
                         They conclude the companion is most likely a cool giant or supergiant           
                         with a mass ~5 Msun.                                                    Wtk2017 
13473+1727   STT 270     tau Boo = 4 Boo. A is a Delta Scuti-type variable.                              
                         CHARA Array Limb-darkened diameter  0.786 +/- 0.016 mas,                CIA2008c
                         R =  1.331 +/- 0.027 \rsun.                                                     
                         NPOI Limb-darkened diameter 0.822 +/- 0.049 mas, Sp = F7IV,             NOI2018 
                         R = 1.38 +/- 0.08 \rsun, Teff = 6556 +/-212 K, L =  3.2 +/- 0.2 \lsun.          
                         AB: Tau Boo. A hosts exolanet, P=3.31d                                  Tok2014d
13477-3226   COO 159     SWR 145. CPM pair                                                       Skf2004 
13478+0639   GIC 115     G065-004/G065-005.  The B component corresponds to the primary of               
                         LDS6286; systems merged, with LDS pair labelled BC pair. However, no            
                         obvious C component is found, so the BC pair is X-coded.                        
13478+0112   BAL1459     RST 5529.                                                                       
13479-6352   COO 158     Includes V979 Cen, a Beta Lyr type eclipsing binary, P = 2.56835d.      Zas2012 
13481-1345   DEA   1     LHS 2803. Deacon et al. (2012) derive Teff 2940 +/- 60 and 1100-120K            
                         for the primary and secondary, respectively. The primary is M4.5 +/-            
                         0.5, the seconary T5.5 +/- 0.5. Distance estimates are consistent with          
                         the pair being physical: 21 +/- 3pc for the primary, 24 +5/-4 pc for            
                         the secondary.                                                          Dea2012 
                         Wide M/T binary. Spectral types M4.5 +/- 0.5 and T5.5 +/- 1, masses             
                         0.18 +/- 0.02 and 0.04 +/- 0.01 Msun, age > 4.0 Gyr. Distances for the          
                         two components are consistent, at 21.5 +/- 2.1 and 20.0 +/- 2.0 pc.     Muz2012 
13481-5812   BRT3301     A likely plate flaw.                                                    Grv2021b
13482+2248   COU 401     Docobo et al. (2010) derive a dynamic parallax of 16.28 +/- 0.20 mas    Doc2010h
                         and a total mass of 1.53 +/- 0.07 Msun.  The dynamical and Hipparcos            
                         parallaxes are discrepant.                                                      
13482-7739   NZO  42     Hipparcos acceleration double solution.                                         
13483-3653   RSS  19     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
13484+2337   LDS4410     GJ 1179A+B = NLTT 35290 + 35281. Secondary is white dwarf WD 1345+238.  Far2005b
13489-3542   HWE  94     HIP 67408. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
13490-2822   BU  413     A is a long-period variable, W Hya. B is CD-27@9430.                            
13490-6417   RST 659     13490-6417RST 659 Also knows as TDS8978. The identity of these two              
                         pairs determined by Skiff.                                              Skf2006 
13491+2659   STF1785     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.43 +/- 0.39, 1.49, and 1.34 Msun, respectively.             Mlk2012 
13492+0746   LDS3107     No companion is seen on Aladin at Luyten's original theta value. It     Luy1975 
                         appears likely that his theta value was due to a trigonometry error,            
                         however, and that the correct value was 270-28 = 242deg rather than             
                         270+28 = 298deg. A star seen at that position angle and Luyten's                
                         separation agrees with his magnitude and has a proper motion in                 
                         reasonable agreement, as well. Theta has been changed accordingly.              
13492-6206   DUN 143     Spectral types B2(II), K2/3II/III.                                              
13493-2135   LDS 459     NLTT 35336/35335                                                        Chm2004 
13493-4031   DUN 146     B is CD-39@8491.                                                                
                         Identified as optical and linear solution also published.               LRR2022c
13495-2621   TOK 405     HIP 67458 is a double-lined chromospherically active binary with                
                         orbital period of 7.2d (Latham, 2012, private communication). We found          
                         a faint tertiary companion at 0".73 with an estimated orbital period            
                         on the order of 100yr. The speckle survey of chromospherically active           
                         stars by Mason et al. (1998) did not detect this tertiary, lacking the  Msn1998b
                         dynamic range of HRCam.                                                 Tok2015c
13496+3459   STF1786     AB: Identical with BDS 6644, HJ 852.                                            
             SHY 634     BC: HIP  67476 + HIP  67446.                                                    
13496+1302   SHY 635     HIP  67470 + HIP  67673.                                                        
13496-4228   HDO 226     mu Cen. A is an irregular variable.                                             
13496-4722   DUN 144     SWR 146. CPM pair                                                       Skf2004 
13496-6818   JNN  95     Due to the compact configuration of the three components resolved by            
                         AstraLux, the probability is very high for this to constitute a                 
                         physical triple system. Common proper motion has not yet been tested.   Jnn2012 
13498+3638   GC 18691    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
13499-2811   RSS  20     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
13501+4749   HIP  67526  Candidate brown dwarf companion found in MARVELS RV survey; period              
                         90.27d. Teff 6004K, minimum mass 65.0 +/- 2.9 Mjup.  Lucky imaging and          
                         AO find no tertiary companion, ruling out any stars with mass greater           
                         than 0.2 Msun at separations larger than 40au.                          Jia2013 
13501-4451   UC 2623     AC: CPM candidate confirmed physical by photometry (2MASS and V mags).  Tok2013c
13503-2742   UC 2624     SKF1493.                                                                        
13504+2117   S   656     STTA126 = H 6  89.  B is BD+21@2579.                                            
                         BDS 6648, H VI 15 probably same star. Called a spectroscopic binary in          
                         the BSC Supplement.                                                             
13505-0447   BRT 449     A likely plate flaw.                                                    Grv2021b
13505-5925   R   225     A variable?                                                                     
13506-0608   BRT 450     A likely plate flaw.                                                    Grv2021b
13507-2140   LDS 461     NLTT 35412/35392                                                        Chm2004 
13510+6819   STTA127     LDS2329.                                                                        
13510+2346   HJ 2688     Rectilinear solution by Friedman et al. (2012).                         USN2012a
13513+2442   HIP  67615  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Griffin (1982).                                                         Grf1982e
13513-2423   WSI  77     The 10.3 yr SB1 orbit by Abt & Willmarth (2006) matches the speckle     AbH2006 
                         pair WSI 77 and explains the large dmu.                                 Tok2012a
                         Astrometric binary. Hipparcos parallax 51.35 +/- 0.45 mas. Dynamical            
                         parallax 50.3 mas, masses 0.99 and 0.63 Msun. WSI 77 is a                       
                         chromospherically active G5 dwarf within 20 pc from the Sun. According          
                         to Abt & Willmarth (2006), it is also a single-lined spectroscopic      AbH2006 
                         binary with 10.3 yr period. We used RVs from that work and the average          
                         RV from Nidever et al. (2002) together with four speckle points for     Nid2002 
                         the combined orbital solution presented. The spectroscopic elements             
                         are K1 = 6.06 +/- 0.25 km/s and V0 = 5.38 +/- 0.10 km/s, the rms                
                         residual in RV is 0.11 km/s. The node listed in Table 3 corresponds to          
                         the primary component, therefore Omega was chosen to describe the               
                         secondary’s relative motion. The pair was "caught" at close separation  .     
                         in 2012.                                                                Tok2012b
                         Omega for Tokovinin et al. (2012) orbit flipped by 180deg, at request           
                         of author.                                                              Tok2012b
13513-2734   LDS 855     NLTT 35441/35442                                                        Chm2004 
13514+6443   HJ 3342     10 Dra. A is an irregular variable, CU Dra.                                     
                         NPOI Limb-darkened diameter 6.799 +/- 0.077 mas, Sp = M3III,            NOI2018 
                         R = 83.22 +/- 2.12 \rsun, Teff = 3584 +/- 35 K, L = 1031 +/- 70  \lsun,         
                         M = 0.93 +/- 0.06 \msun, Age = 10.24 +/- 1.40 Gyr.                              
13514+3441   BU  613     C is BD+35@2495.                                                                
13515-4818   CPO  61     LDS 462. B is CD-47@8664.                                                       
                         SHY 636. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
13516-2945   LDS5797     Assuming the current identification is correct, it appears that the             
                         pair was originally tabulated at the position of the B component, but           
                         with magnitutes switched. Luyten's theta value has been flipped by 180          
                         deg and precise coordinates of the primary have been corrected. The             
                         11th magnitude component appears to be comprised of a ~4" pair.                 
                         (WIH, May 2008)                                                                 
13518+3143   LDS4415     NLTT 35491/35500                                                        Chm2004 
13518-3300   H 3 101     H III 101. 3 Cen.                                                               
13519-0341   TDS9005     AY Vir.                                                                         
13520-4752   HJ 4619     B is CD-47@8669.                                                                
13521-6653   DON 625     TDS9009.                                                                        
13523-3047   SEE 189     V981 Cen.                                                                       
13527-1843   WSI  78     DL Vir, Algol-type eclipsing binary, period 1.31549 d.                  Zas2018 
13529-6243   HD 120678   Hen 3-939.                                                                      
                         The classification is from Garrison et al. (1977 ApJS 35, 111).         Msn1998a
13531+1251   HEI 524     The Durchmusterung identification is uncertain.                                 
13532-3156   H N  51     4 Cen. A is a spectroscopic binary. B is CD-31@10727.                           
13535-3540   I  1618     AD: WDS has 1 measure in 1927. 2MASS: AD at 28.3" 152d. AD optical?     Tok2014d
             H 5 124     AE: H V 124.                                                                    
13538+5210   JNN  96     The secondary detected in the AstraLux images is perhaps itself a               
                         close binary, as it appears extended in epochs 2008.64 and 2009.42.             
                         However, we count it as a single component of the system here.          Jnn2012 
13539+1008   BU  614     Same as STT 271.                                                                
                         Easier to see in 1964 than in 1962. Companion perhaps variable.         Cou1964 
13539-1440   RST3852     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.88 +/- 1.13, 3.17, and 1.40 Msun, respectively.             Mlk2012 
13540-4708   HJ 4624     A is the variable V767 Cen.                                                     
13540-7400   NZO  43     Spectrum composite: A3V+F8/G2III.                                               
13546+2429   BRT3302     Originally published as BRT 165.                                        Brt1928 
13546-3436   SEE 191     Rectilinear solution by Hurowitz et al. (2014).                         USN2014a
13546-5041   BSO   9     B is CD-50@8112.                                                                
                         SWR 148. CPM pair                                                       Skf2004 
13546-6654   DUN 145     B is CPD-66@2371.                                                               
13547+1824   eta Boo     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Bertiau (1957).                                                         BFC1957 
                         Daniel & Burns orbit rejected from Fourth Orbit Catalog                 Dni1939 
                         ("amplitude below noise level")                                         Wor1983 
             SHJ 169     eta Boo = 8 Boo = Muphrid. A is a long-period spectroscopic binary.             
                         B is BD+19@2726.                                                                
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         H 6  95.                                                                MEv2010 
13550+8724   STF1887     Doolittle (1901) 1897 measure corrected by the author for refraction            
                         and precession. Epoch=1900.  Probably rectilinear motion.               Doo1901 
13550-0804   STF1788     AB: A is SB, no orbit. A is X-ray source.                               Tok2014d
                         Hopmann's (1970) B and F are interchanged, and his orientational        Hop1970 
                         elements contain additional computing errors.                                   
             TOK 570     AE: AE can be optical (Pphys=0.24), but accepted because it is bright.  Tok2014d
13550-4235   I   401     Measures rather discordant.                                                     
13557-0925   RAP  19     Aa,Ab: EPIC 212651213. The primary of J 1609 consists of two eclipsing          
                         binaries, resolved at a separation of ~90mas:                                   
                         Aa1,Aa2: P =  5.08d, M = 0.94 +/- 0.06 and 0.89 +/- 0.05 Msun                   
                         Ab1,Ab2: P = 13.19d, M = 1.09 +/- 0.07 and 0.64 +/- 0.03 Msun.                  
                         Resolved pair has estimated period ~65y and separation of ~25au.        Rap2016 
             J  1609     AB: EPIC 212651213 + 212651234. The B component is single.              Rap2016 
13559-0945   TOK 158     HIP 68038.                                                              Tok2011a
13560-2532   H N  59     B is CD-24@11171.                                                               
13562+3627   SHY 641     AC: HIP  68069 + HIP  68576.                                                    
13563+2409   LDS5799     LDS6287.                                                                        
13563+0517   BU 1438     AB,C: The C "component" is the galaxy NGC 5363.                                 
13564+1654   BPM 608     [PM2000] 1071043 + [PM2000] 1071058.                                    Gvr2010 
13569-7349   HJ 4621     B is CPD-73@1217.                                                               
13571-2731   I   234     A premature orbit has been computed.                                            
13573-5602   DUN 151     A is an irregular variable. B is CPD-55@5793.                                   
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Chauvin et al. (2006) note finding at least one faint companion         Cvn2006 
                         candidate within separation/magnitude range listed. However,                    
                         further observations are required for verification                              
                         Additional notes may be found in van den Bos (1926).                    B__1928d
13574-6229   FIN 370     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.48 +/- 0.38, 2.34, and 1.12 Msun, respectively.             Mlk2012 
13575-5743   DUN 150     A is variable.                                                                  
13576-3139   SKF1963     Primary is the RS CVn-type binary V988 Cen.                                     
13577+1744   LDS 951     LDS1400.                                                                        
13577-1717   WHC  12     Wilson's 1882 distance for AC should read 31".42 (+ 1/2 rev.)           B__1950c
13579-5624   R   228     B is CPD-55@5797.                                                               
13583+0213   A  2167     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.24 +/- 1.47, 2.57, and 1.05 Msun, respectively.             Mlk2012 
13583-2756   BRT3005     A likely plate flaw.                                                    Grv2021b
13583-7158   TRR  15     AC: Also known as SIN  84AC.                                                    
13584-0140   RAO 502     BH Vir.                                                                         
13588+3140   JNN  97     LP 324-42.                                                                      
13588+1434   BPM 609     [PM2000] 1072223 + [PM2000] 1072207.                                    Gvr2010 
13593-6228   JSP 603     V1202 Cen, Algol-type eclipsing binary, P = 15.5543 d.                  Zas2011 
13594+2515   LDS6288     NLTT 35918/35919                                                        Chm2004 
13597-5056   SWR 149     CPM pair                                                                Skf2004 
13598+5144   LDS1401     NLTT 35954/35953                                                        Chm2004 
13599+2810   HDS1964     CX CVn, Algol-type eclipsing binary, P = 6.563197 d.                    Zas2011 
13599+2520   BUP 156     Distances 1033.9" and 1035.6". B is BD+26@2517.                                 
                         Secondary of BUP 156 is 14012+2522 A   569.                                     
14000-4714   DAW 207     D: AA Cen                                                                       
             HJ 4638     C: ZZ Cen. Both are variables of unknown type.                                  
14004-2708   LDS4424     NLTT 35939/35937                                                        Chm2004 
14006+4741   LDS5803     AC: NLTT 36000/35991                                                    Chm2004 
14007+2404   BRT3304     POU 3156 is identical, and Barton's angle is corrected by Heintz.       Hei1983a
                         Originally published as BRT 166.                                        Brt1928 
14013+1218   GRV1256     Both A and B have approximately the same radial velocity.               Grv2019b
14013-4240   SWR 150     CPM pair                                                                Skf2004 
14014-3137   TOK 159     Aa,Ab: HIP 68507 is an acceleration binary with a variable RV resolved          
                         here at 0".06.  The period of Aa,Ab is on the order of 5yr. There is a          
                         faint physical companion B at 6".7 found in 2MASS (Tokovinin 2011).     Tok2011a
                         Another visual companion at 14", SEE 195, is optical, as revealed by            
                         its fast relative motion.                                               Tok2015c
                         Aa,Ab: SB, no orbit.                                                    Tok2014d
             SEE 195     AC: Linear configuration. A is SB without orbit (dRV= 5.4) and          Nrd2004 
                         astrometric binary (Hipparcos).                                                 
14016+0133   SHJ 171     tau Vir = 93 Vir. A is a spectroscopic binary.                                  
                         B is BD+02@2760.                                                                
                         AB: H 6  77.                                                            MEv2010 
14018-6119   LPO  44     Spectral type F0?                                                               
14019+1530   ALD 112     Worley measured this as ALD 118, but also identified it as Vys 149      Wor1962b
                         = ALD 112, which it matches. Measure moved here.                                
14021-4001   WG  172     SWR 151.                                                                        
14022+1608   BPM 610     [PM2000] 1073886 + [PM2000] 1073930.                                    Gvr2010 
14022-0448   LDS4427     NLTT 36043/36042                                                        Chm2004 
14023-6652   LDS 468     A component appears double.                                             Dam2010 
14024+4620   SWI   1     LDS1403.                                                                        
                         NLTT 36091/36092                                                        Chm2004 
14024-0311   LDS4429     NLTT 36057/36053                                                        Chm2004 
14029-3511   I  1574     Measures uncertain, too close.                                                  
14031+1154   HJ 2699     BC: Rectilinear solution by Cvetkovic et al. (2015).                    Cve2015 
14035+1047   GJ  538     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Kamper (1987).                                                          Kpr1987a
                         Combined astrometric/spectroscopic solution by Kamper (1987).           Kpr1987a
                         GJ 538. Martin et al. (1998) derive component masses 1.109 +/- 0.057            
                         and 0.548 +/- 0.033 Msun.                                               Mig1998 
14037+1914   LDS5806     LDS6289.                                                                        
14037+0829   BU 1270     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.36 +/- 0.53, 2.49, and 1.20 Msun, respectively.             Mlk2012 
14037+0243   AG  192     One component is variable.                                                      
14038-6022   RBT   1     Aa,Ab: bet Cen = Hadar. Also, historically known as Agena. The IAU              
                         sanctioned official name is Hadar. Measure of 1995.035 made by MAPPIT.  Rbt1999 
                         Interferometric data from SUSI are combined with spectroscopic data to          
                         yield orbital parameters, masses, and distance.                         Dvs2005 
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 29.50 +/- 5.38, 23.82, 12.02 Msun, respectively.   Mlk2012 
             VOU  31     AB: Spectroscopic and interferometric measures indicate a multiple              
                         system.                                                                         
14039-6259   LDS 470     Aka VVV  17.                                                                    
14040+1318   BPM 611     [PM2000] 1074837 + [PM2000] 1074832.                                    Gvr2010 
14040-1502   GWP2201     B is the pulsating ZZ Ceti type variable IU Vir.                                
14044+6423   NOI   4     HR 5291 = 11 alp Dra = Thuban.                                                  
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Elst & Nelles (1983).                                                   Est1983 
                         This pair is also a spectroscopic binary.                               Mug2017b
14046-3539   I   941     Many uncertain measures. It appears nearly a revolution has been                
                         completed.                                                                      
14047+1345   BPM 612     [PM2000] 1075186 + [PM2000] 1075177.                                    Gvr2010 
14048+2549   BGH  50     HJL 196.                                                                HJL1986 
14048-3200   LPR   2     Looper et al. (2010) determine NIR spectral types T1+/-1 and T5+/-1.            
                         Distance is estimated at 23pc, separation ~3.9au, orbital period                
                         28-35y. Total masses, for ages 0.5, 1.0, and 5.0 Gyr, are 50, 70, and           
                         80 Mjup, respectively. Mass ratio is 0.80 +/- 0.9, Teff for A and B =           
                         1390 +/- 90 and 1180 +/- 90K. 2MASS component magnitudes are derived            
                         from their MKO component photometry and spectral type estimates, using          
                         transformations from Stephens & Leggett (2004 PASP 116, 9).             Lpr2008 
14050+0157   LDS5807     LDS6290.                                                                        
14051+4913   BEM   7     T0 converted from negative to positive by subtracting from P.           Kiy2020 
14056-1804   S   659     B is BD-17@4003.                                                                
                         SHY 642. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
14057+1537   BPM 613     [PM2000] 1075685 + [PM2000] 1075674.                                    Gvr2010 
14060-1304   HWE  30     Spectrum of A composite; F2, A3.                                                
14061-7259   GLI 199     Also known as R   240.                                                          
14064-5943   HD 122879   The classification is from the LSC; however, Garrison et al. (1977              
                         ApJS 35, 111) assign a type B0 Ia.                                      Msn1998a
14067-3622   DUN 253     the Cen = 5 Cen = Menkent. DUN 253AB was originally known as DUN 156.           
                         When the Dunlop pair was added to the IDS (after publication of the             
                         printed volume but before its transfer to USNO) an ordinal number               
                         following the last Dunlop listing was added, despite already being              
                         assigned. As it has been in use for almost half a century, it will not          
                         be changed.                                                                     
14068+5946   LDS2700     B is BD+60@1512.                                                                
14069+1547   LAW  21     AB: SLW 965.                                                                    
14071-6327   HJ 4642     AB: Spectrum composite; G0+A3.                                                  
                         AD: Hipparcos suspected non-single.                                             
14072-5153   RST 681     CPD-51@6574.                                                                    
14075-5742   HJ 4645     B is CPD-57@6501.                                                               
14076+5322   LDS2922     SLW 968.                                                                        
14077-5341   DUN 155     B is CPD-53@5880.                                                               
                         Identified as optical and linear solution also published.               LRR2022c
14077-5738   R   238     First distance? B is CPD-57@6504.                                               
14077-6609   RSS  21     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
14081-1256   STF1802     A possible SB, no orbit. CfA has mention of RV variability, however.    Tok2014d
14082-4124   KSA 132     Primary is the T-Tauri type variable V1032 Cen = PDS 70. Companion is           
                         a background star.                                                      KsA2014 
14082-5019   CPO 382     CPD-49@6690.                                                                    
14083+4927   H 6 112     H VI 112. 13 Boo. A is the variable CF Boo.                                     
14083+3708   BFR  10     NLTT 36369 + 2MASS J14081969+3708255. Baron et al. (2015) estimate              
                         spectral types M4.0 +/- 0.5 and M7.5 +/- 0.5, distances 55 +33/-21              
                         and 84 +4/-29 pc, masses 0.207-0.272 and 0.087-0.096 Msun.              BFr2015 
14083+2112   STF1804     H N 115.                                                                MEv2010 
14087+3341   HU  742     A premature orbit has been computed.                                    Cou1956 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
14088+7733   BNU   9     4 UMi. A spectroscopic binary, P = 605.8d, now resolved.                        
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Scarfe (1971).                                                          Scf1971 
                         1984.2791: Halbwachs (1981) predicts an angular separation of about     HJL1981 
                         0".03 and the system appears to be at the limit of resolution of the            
                         6-m telescope.                                                          Bnu1986 
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Scarfe (1971).                                                          Scf1971 
14089+7316   LDS1783     NLTT 36481/36478                                                        Chm2004 
14089-4328   SIN  88     BC: initially listed incorrectly as AC.                                         
14090-1020   CHR  40     96 Vir.                                                                         
14095+3549   HJ  540     HJL 197.                                                                HJL1986 
14096+7250   STF1822     Some measures previously listed under H V 178.                                  
14096-5130   HJ 4651     A is a spectroscopic binary and may be variable. B is CD-50@8297.               
14097-3955   WG  176     SWR 153.                                                                        
14098+0822   A  1098     BRT2157.                                                                Brt1938 
                         Rectilinear solution by Hartkopf & Mason (2015).                        WSI2015 
14102-2524   UC 2694     V353 Hya.                                                                       
14103-4459   LDS 476     HIP 69220. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AB: SHY 257. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
14104+3932   SHY 644     AB: HIP  69227 + HIP  69166.                                                    
             YSC 151     Aa,Ac: YSC 218Aa,Ac.                                                            
14104+2506   12 Boo      d Boo. SB2. Combined spectroscopic/interferometric solution by Boden    Bod2000 
                         et al. (2000), including mass determinations, and other analysis.               
                         P = 9.604565d +- 7.6e-6, T (MJD) = 51237.779. Orbital period was                
                         converted to hours in the orbit catalog to allow full precision in the          
                         available column width.                                                         
                         Combined astrometric/spectroscopic solution by Boden et al. (2005),     Bod2005a
                         including interferometry data from PTI and NPOI. Derive orbital                 
                         parallax of 27.74 +- 0.05 mas, luminosities 7.76 +- 0.35 and 4.69 +-            
                         0.74 Lsun, and masses 1.4160 +-  0.0049 and 1.3740 +- 0.0045 Msun, as           
                         well as effective temperatures, radii, and other physical parameters.           
                         Combined spectroscopic/astrometric solution, based on high-resolution           
                         echelle spectra plus archival PTI visibility measurements.                      
                         Derived masses 1.4109 +/- 0.0028 and 1.3677 +/-0.0028 Msun,                     
                         distance 35.820 +/- 0.057 pc.                                           Knc2010 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.17 +/- 6.34, 3.14, and 1.10 Msun, respectively.             Mlk2012 
             ISO  14     AB is bogus, unresolved (2010.481, dm>5.22 @562nm, dm>5.46 @642nm) by   Hor2011 
                         Horch et al. (2011), also unconfirmed by RoboAO                         Tok2014d
14104+1116   GWP2257     CD: Incorrectly added as AC pair, but not physically associated with            
                         14104+1116 GWP2256AB. WDS designation maintained, but component                 
                         designations updated.                                                           
14105-0240   HLD  17     BAL 230.                                                                        
14107-4746   SKF1135     V759 Cen.                                                                       
14107-6229   SNA  36     The 0.7mas companion marginally resolved by PIONIER may correspond to           
                         the P=60d SB1 reported by Gamen et al. (2008, RevMexAA 33, 54), which,          
                         assuming pi=0.5mas and M=20 Msun (Hohle et al. 2010, AN 331, 349), has          
                         a_app = 0.4mas.                                                         Sna2014 
14109+1513   SKF 343     HIP 69281. Aa,Ab is HDS 1989, 0.6".  It is not seen in the V-band               
                         images, too red and faint. Is this a visual multiple system with four           
                         components or a small cluster?                                          Tok2011a
14109+0653   GIC 116     G065-029/G065-030.                                                              
14110+5015   STF1814     NLTT 36518/36516                                                        Chm2004 
                         HJL 198.                                                                HJL1986 
14110+3152   GC 19140    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
14110-0240   BU  803     BAL 231.                                                                        
14113-0320   STF1807     BAL 232.                                                                        
14122+6137   LDS2704     NLTT 36592/36597                                                        Chm2004 
14122+4411   STT 278     Only elements P and T have been amended by Starikova (1980) from the    Sta1980a
                         orbit of Heintz (1976).                                                 Hei1976 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.87 +/- 1.55, 2.93, and 1.45 Msun, respectively.             Mlk2012 
14123+0225   HJ 3343     A is the Alpha CVn-type variable CU Vir.                                        
14124+2843   STF1812     AB,C: HJL 199.                                                          HJL1986 
14124+1335   HJ  234     LDS 952.                                                                        
14125+1646   LDS1408     Recognized to be the same as LDS6291 by John Greaves.                   Grv2006b
14128-3522   SWR 155     CPM pair                                                                Skf2004 
14131+5520   STF1820     Two possible solutions by Kiyaeva et al. (1998), based on a 26-year     Kiy1998 
                         long series of photographic data from Pulkovo.                                  
                         A component is SB1 (P=2.87 yr, e=0.75). Spectral types and                      
                         magnitudes are estimated for all components of this triple system.              
                         A: Ren & Fu (2013) calculated an astrometric orbit, combining                   
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Kiyaeva et al. (1998). They derived component masses 0.84 and 0.52      Kiy1998 
                         Msun and an estimated semimajor axis of 57.65 mas.                      Ren2013 
14131-1056   HJ  541     Herschel coordinates 14 04+/- NPD 100 08 (1830). He notes: "very                
                         unequal, L. white, S. blueish".                                                 
14133+1430   BPM 614     [PM2000] 1079457 + [PM2000] 1079464.                                    Gvr2010 
14133-0827   CHR 221     First detected as an occultation binary by Blow et al.                  Blw1982a
14134+0524   STF1813     H N  98.                                                                MEv2010 
14134-3043   LDS5811     BC = LDS5812BC.                                                                 
14135+5147   STF1821     kap Boo = 17 Boo. A is a Delta Scuti-type system. B is a long-period            
                         spectroscopic binary with P = 1791.2d.                                          
                         The 6101- and 6675-yr period solutions for the AB pair by Kiyaeva       Kiy2006 
                         (2006) assumed total system masses of 4.2 and 3.6 Msun, respectively.           
                         P and T for the astrometric Ba,Bb solutions were adopted from the               
                         spectroscopic solution of Bakos (1986, AJ 91, 1416), as was the                 
                         value of e (0.53) in the first solution.                                        
                         H 3  11.                                                                MEv2010 
14138+3059   COU 606     Systemic mass is estimated at 1.8 +/- 0.5 Msun, assuming an Hipparcos           
                         parallax of 17.21 +/- 1.63 mas. The dynamical parallax of 18.3 mas              
                         lies within about 1 sigma of the Hipparcos value.                       Doc2008a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.20 +/- 0.71, 1.51, and 0.55 Msun, respectively.             Mlk2012 
14139+4620   RED  24     M2, spectroscopic distance 31pc. 83" from G0 dwarf HD 124694 = HIP              
                         69518 = 2MASS J14135135+4619304. Hipparcos distance of the brighter             
                         star is 26.2pc.                                                         Red2007a
                         2MASS J14134677+4618227 is possibly a wide companion to HIP 69518 at    Red2007a
                         83" (Reid et al 2007), but is single in the AstraLux field of view.     Jnn2012 
14141+1258   CHR  41     14 Boo. A spectroscopic binary with P = 726.6d.                                 
14141-5029   BRT 825     CPD-49@6779.                                                                    
14142+5915   STF1827     HJL 200.                                                                HJL1986 
14142+1805   TOK 723     While the visual pair may be a "ghost," it is also a 6d                 Tok2019b
                         spectroscopic binary.                                                           
14142-5111   CPO 383     CPD-50@6728.                                                                    
14144-1521   LDS 483     AC: NLTT 36649/36641                                                    Chm2004 
14145-3910   HJ 4663     SWR 156. CPM pair                                                       Skf2004 
14146-6148   HDS1999     Primary is V997 Cen, a Beta Lyr type eclipsing binary, P = 2.4282d.     Zas2012 
14146-7605   HLN  32     Also known as R   242.                                                          
14148+1006   KUI  66     15 Boo.                                                                         
                         Duplicity uncertain. The companion, 3 mags fainter, was not seen on two         
                         other good nights.                                                      WRH1954b
14148-1254   CHR 231     First detected as an occultation binary by Africano.                    Afr1978 
14150-0511   FAR  39     SKF  43.  Primary is white dwarf WD 1412-049.                           Far2006 
14150-5705   HDO 228     A is the variable V795 Cen.                                                     
14150-6142   SNA  37     Aa,Ab: The new pair is marginally resolved at 1.5mas, and possibly              
                         corresponds to the newly-reported SB2 system (Sota at al. 2014, ApJS            
                         211, 10).                                                               Sna2014 
14152+2216   LDS 954     NLTT 36716/36714                                                        Chm2004 
14153+5232   SHY 645     HIP  69650 + HIP  69917.                                                        
14153+0308   STF1819     Hopmann (1945) orbit is not seen but is quoted from Baize's             Hop1945 
                         catalog.                                                                Baz1950a
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.92 +/- 1.08, 2.15, and 1.05 Msun, respectively.  Mlk2012 
             SHY 261     AC: HIP  69653 + HIP  70782.                                                    
14154+2413   LDS4446     NLTT 36733/36730                                                        Chm2004 
14157+1911   HDS2003     = alp Boo = Arcturus. Proper motion of B -1093 -1999.                           
                         Duplicity questioned by Griffin and subsequently retracted by           Grf1998 
                         Soderhjelm & Mignard                                                    Sod1998 
                         1975.624: Disk not clearly resolved at 600 nm but resolved (0".018              
                         +/- 0".004) at 450 nm.                                                  Bla1977a
                         1975.634: Disk resolved (0".018 +/- 0".005) at 500 nm.                  Bla1977a
14158+1018   A  1101     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.58 +/- 0.71, 1.74, and 0.85 Msun, respectively.  Mlk2012 
                         AB,C: Also known as SCA 186.                                            Sca2018b
14161+5643   STF1831     D. Arnold noted considerable overlap of measures for the two multiple   Arn2004a
                         systems STF1831 and 14157+5640STF1830, with STF1831CE = STF1830DA and           
                         STF1831EF = STF1830AB. They have therefore been combined into one WDS           
                         system, maintaining the WDS and most of the component designations for          
                         STF1831. Designation changes are as follows:                                    
                            STF1830AB --> STF1830EF                                                      
                            STF1830AC --> STF1830EG                                                      
                            STF1830AD --> STF1830CE (with quadrant flip)                                 
                            STF1831CE --> STF1830CE                                                      
                            STF1831EF --> STF1830EF.                                                     
                         Finally, the single measures of AD and CD were misidentified, so these          
                         measures were reassigned to the proper components.                              
14161+5010   BDK   8     G 200-28 + SDSS J141659.78+500626.4. Distance 45.1 +1.6/-1.5 pc for             
                         primary, 44 +/- 31 pc for secondary. Estimated age of system 7-12 Gyr.          
                         Mass of secondary estimated at 0.077-0.078 Msun.                        Fah2010 
14162+5122   STFA 26     21 Boo = iot Boo. STTA128. A is a spectroscopic binary and a Delta              
                         Scuti-type variable, P = 0.027d. B is BD+52@1785.                               
                         Struve suspected a close companion to A (1836.28, 149.9deg, 0".3)       StF1837 
                         as did Smyth (1838.19, 195.0deg, 0".5) but this supposed pair           Smy1844 
                         has never been confirmed with larger telescopes.                                
                         AB: H 5   9.                                                            MEv2010 
14162+3235   HZG  10     B is BD+33@2434.                                                                
14163+0605   STF1824     H N  99.                                                                MEv2010 
14164+4605   VIG  17     Optical/physical nature of the faint companion is undefined.            Vig2012 
                         lam Boo = 19 Boo = Xuange.                                                      
14164+1348   SOZ   3     BNG   1. Physical separation 75 au at distance ~8pc. CPM pair.          Soz2010 
                         Burgasser et al. (2010) confirmed the companion as a T7.5 dwarf.                
                         Spectral model fits yield Teff = 650 +/- 60K and high surface gravity           
                         and/or subsolar metallicity.                                            Bug2010 
                         Very cool (d/sdL7 + T7.5p) common proper motion pair found by                   
                         cross-matching UKIDSS against SDSS.                                     Bng2010 
14165+3334   HU 1266     Possibly an ambiguous case, although only one solution has been tested.         
14165+2007   STF1825     A is X-ray source. B is possible astrometric pair (Gontcharov &         Gon2002a
                         Kiyaeva 2002)                                                           Tok2014d
14165-5718   BSO  10     AH: H is CPD-56@6216.                                                           
14166-5955   I   366     A is the Mira-type variable R Cen.                                              
14170+3143   DEL   5     LSPM J1417+3142 = NLTT 36838. Law et al (2008) derive a distance of     Law2008 
                         16.1 +3.4/-3.4 pc and a projected separation of 11.2 +2.4/-2.4 au.              
                         Estimated spectral types are M4.5 and M4.5.                                     
                         GJ 3839. Estimated age 300-1000 Myr; masses 0.43 +/- 0.03 and 0.33 +/-          
                         0.03 Msun; a ~7.1 au.                                                   Jnn2014 
14170-3935   WG  179     SWR 157.                                                                        
14171-4810   HJ 4666     B is CD-47@9026.                                                                
14172+6136   STI 763     LDS2709.                                                                        
14174+3245   VYS  13     HDS2009.                                                                        
14174+1330   LDS4452     SLW 989.                                                                        
14178+4845   HJ 2710     C is BD+49@2286.                                                                
14179+1118   GIC 117     G065-042/G065-041.                                                              
14179-6803   RSS 324     DF Cir.                                                                         
14180+3531   A Boo       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Scarfe & Alers (1975).                                                  Scf1975 
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Scarfe & Alers (1975).                                                  Scf1975 
14180-0733   BUP 157     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
14182-2731   HDS3407     AD : This pair missed on initial entry into WDS of HDS stars.                   
                         Added 02/26/01.                                                                 
14182-5130   HD 124979   LS 3219. The classification is from McConnell & Bidelman (1976).        Bid1976 
                         Tobin & Kilkenny (1981 MNRAS 194, 937) place the star at 0.7 kpc from           
                         the Galactic plane, so we have included it in the "runaway" group.              
                         Penny (1996) suggests that the star may be a double-lined binary which  Pny1996b
                         needs confirmation since there are only 2 other knowndouble-lined               
                         binaries among the runaway stars (both B-type systems; see Gies &       Gie1986 
                         Bolton 1986).                                                           Msn1998a
14185+1714   BPMA 47     [PM2000] 1082068 + [PM2000] 1081940.                                    Gvr2010 
14187+6915   LDS1788     NLTT 36996/37003                                                        Chm2004 
14188-6342   RSS  22     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
14189+7314   OSO  55     G239-012. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates.                                                  Oso2004 
14189+5452   CHR 137     Docobo et al. (2010) derive a dynamic parallax of 9.49 +/- 0.20  mas    Doc2010h
                         and a total mass of 3.81 +/- 0.35 Msun.                                         
14189+1812   LDS 956     LDS1415.                                                                        
                         NLTT 36923/36924                                                        Chm2004 
14190+0142   GRV1099     Aka SLW 991.                                                                    
14190-0636   SHY  71     AC: HIP  69962 + HIP  69701.                                                    
                         C component = iota Vir = 99 Vir.                                                
                         NPOI Limb-darkened diameter    1.222 +/- 0.061 mas,                             
                         R =    2.89 (+/- 0.15   )  \rsun,  Teff = 6055 +/- 151 K,                       
                         L =   10.2 +/-   0.1 \lsun.                                             NOI2023 
14190-2549   BU 1246     Too faint, if real                                                      B__1951a
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: Rectilinear solution by Friedman et al. (2011).                     USN2011a
14191-1322   IOT   1     lam Vir = 100 Vir = Khambalia.                                                  
                         Combined spectroscopic/interferometric solution by Zhao et al. (2007),          
                         including data from IOTA array. Derive masses 1.897 +/- 0.016                   
                         and 1.721 +/- 0.023 Msun, luminosities 20.84 +/- 0.25 and 12.58 +/-             
                         0.16 Lsun, and distance 53.16 +/- 0.29 pc (pi = 18.81 +/- 0.10 mas).    Zha2007 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.50 +/- 0.22, 4.20, and 2.19 Msun, respectively.             Mlk2012 
                         aka OCC9018. The OCC2010 solution is ambiguous and one is arbitrarily           
                         "T" coded until the true solution is determined.                                
14192+4223   AG  193     HJL 201.                                                                HJL1986 
14192-3002   BRT3305     A likely plate flaw.                                                    Grv2021b
14193+2421   LDS 957     NLTT 36958/36967                                                        Chm2004 
14193+1300   ENG  51     18 Boo.                                                                         
14195-1343   BU  116     Despite the linear solution, proper motion and parallax favor a         Grv2020a
                         physical connection. Long period and/or high eccentricity possible.             
14195-6838   I   325     B is CPD-68@2106.                                                               
14196-0509   KUI  67     LDS5815.                                                                        
                         BD-04 3665; CPM pair (0.66" in 261deg) with large parallax.             Kui1937a
14197-3651   BU 1110     V1002 Cen.                                                                      
14198+1154   BPM 615     [PM2000] 1082740 + [PM2000] 1082764.                                    Gvr2010 
14199+6747   STF1840     AB: H N  71.                                                            MEv2010 
14201+3026   SHY 647     HIP  70051 + HIP  70609.                                                        
14202-6105   SNA  38     Aa,Ab: Given the lack of information, one cannot decide whether the             
                         40mas companion is also the SB2 system reported by Sota et al. (2014,           
                         ApJS 211, 10).                                                          Sna2014 
             HD 125206   This "field" object may belong to the "CLUST 3" group of Mel'nik &              
                         Efremov (1995 SvAL 21, 10).                                             Msn1998a
14203+4830   STF1834     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.78 +/- 1.56, 2.58, and 1.07 Msun, respectively.             Mlk2012 
14206-3753   GAA   9     Psi Cen.                                                                        
                         Ma,Mb = 3.187  +/- 0.031 , 1.961  +/- 0.015  \msun,                     GaA2019 
                         orbital parallax = 13.049 +/- 0.063 mas.                                        
                         Primary is an Algol-type eclipsing binary, period 38.81252                      
                         days (see 2006A&A...456..651B).                                         Zas2011 
14209-1729   MUG  17     A is exoplanet host, P=4.15d, 502d, 3008d. Roell et al. (2012) list     Rol2012 
                         companion at 90", confirmed by Mugrauer (2009).                         Mug2009 
14211+5725   FAR  40     Primary is white dwarf WD 1419+576.                                     Far2006 
14212+4534   KOI-1408    Some weak evidence for a small-separation (<0".1) companion.            Hor2012b
14217+1334   BPM 616     [PM2000] 1083695 + [PM2000] 1083701.                                    Gvr2010 
14218+0355   BAL2861     A is the Mira-type variable AO Vir.                                             
14218-7634   GLI 201     Also known as TOB 323.                                                          
14225-2518   RST5534     Measures discordant by 90@ in 1951.                                             
14226+1159   FMR   2     BC: Companion of B is the star no. 0975-07459414 of USNO-A2.0 catalog.  FMR1999h
14226-0746   STF1833     AB: A=SB? (Desidera et al. 2006 A&A 454, 553)                           Tok2014d
14226-5828   DUN 159     A is a spectroscopic binary.                                                    
14233+1318   LAW   3     Spectral types M5-M6.5 for both components, masses 0.108-0.122 and              
                         0.099-0.109 Msun, distance 33.1 +/- 3.4 pc                              Law2006 
14233+0114   PIN   2     LHS 2907 + WISE J142320.84+011638.0. Pinfield et al. (2012) discovered          
                         a T dwarf companion to BD+01 2920 through a search of the WISE first            
                         data release. Based on images from VISTA and UKIDSS, they determine             
                         the pair share common proper motion. Spectroscopy yields a spectral             
                         type of T8p for the companion.                                          Pin2012 
                         I-band FastCam lucky imaging of the primary in 2010 by Murray et al.            
                         (MNRAS 414, 575,  2011) shows no evidence of a close companion to the           
                         primary (down to 4-5 maggs at 1").                                              
14234+0827   STF1835     A,BC; Mt. Wilson spectral types A1n and F1s.                                    
                         A,BC triple solution (double A-(BC) in HIP).                            Sod1999 
                         A,BC: H 2  38.                                                          MEv2010 
                         RV may be variable.                                                             
                         BC: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.47 +/- 0.42, 2.74, and 2.79 Msun, respectively.  Mlk2012 
14234-1717   LDS4461     NLTT 37151/37150                                                        Chm2004 
14234-2749   TOK 163     HIP 70330. A is SB without orbit (dRV=7.6).                             Nrd2004 
14237+6156   STF1845     Rectilinear solution by Friedman et al. (2011).                         USN2011a
14237-2622   B  2768     CPD-25 5414. van den Bos notes: "has a faint triple north following".   B__1930a
14238-1646   HJ 2713     LDS 487.                                                                        
14240-1948   HJ 2714     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
14241+1115   STF1838     BDS 6833, H III 20 probably same star.                                          
                         HJL 202.                                                                HJL1986 
                         H 3  20.                                                                MEv2010 
14242+4338   LDS5816     LDS6293.                                                                        
                         NLTT 37241/37240                                                        Chm2004 
14244-3535   UC 2752     Aka SKF1499.                                                                    
14245+6015   LDS2710     NLTT 37282/37283                                                        Chm2004 
14246+4750   STF1843     AB: HJL 203.                                                            HJL1986 
14247+0917   ZUC  12     SKF  44.                                                                        
                         Primary is white dwarf PG 1422+095 = GD 165 = CX Boo.                   Zuc1992 
                         SKF  44.                                                                        
                         Primary is L4V brown dwarf; this is prototype of L-dwarf class.         Kir1999 
14248-0251   OSO  57     G124-035. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
14252+5151   STT 580     the Boo = 23 Boo. A is a Delta Scuti-type variable. A = SB?             Tok2014d
                         CHARA Array Limb-darkened diameter  1.109 +/- 0.007 mas,                CIA2012e
                         R =  1.733 +/- 0.011 \rsun, L =  4.131 +/-0.096 \lsun,                          
                         Teff = 6265 +/-  41 K, M = 1.232 +/- 0.058 \msun,                               
                         Age =  4.2 +/- 0.8 Gyr.                                                         
                         NPOI Limb-darkened diameter    0.902 +/- 0.097 mas,                             
                         R =    1.40 (+/- 0.15   )  \rsun,  Teff = 6885 +/- 370 K,                       
                         L =    4.0 +/-   0.0 \lsun.                                             NOI2023 
14253-1321   HJ  546     BDS 6823 same star.                                                             
14255-1958   BU  225     BC = HDO 138                                                                    
             SHJ 179     AB: H N  80.                                                            MEv2010 
14257+2338   BU 1442     LDS 960. Proper motion of A = +792,-1114; PM of B = +794,-1119 (UCAC2)          
                         AB: SHY  73. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         Epoch-2000 coordinates of F = 1425269+233745, current AF separation             
                         ~3'.9 at 280deg. Proper motion of C -005+000.                                   
                         AC and AF: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         AD and AF are the same pair, so were merged. Abetti (1922) was          Abt1922 
                         apparently confused, due to the very large proper motion of A.                  
14258+2217   HJ 2721     B is BD+22@2700.                                                                
14258-3305   PRO 113     Only one star seen; appears to be either a plate flaw or error in               
                         reduction of Perth source catalog.                                      PrO1913 
14259-2108   BHA  17     CPD-20@5922.                                                                    
14259-3713   RST2904     Spectrum: A8/9II/III.                                                           
14260+4213   COU1757     Elements determined by Mante (1998) were also published by the same     Mnt1998b
                         author in Obs. Trav. SAF 52, 44, 2000.                                          
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.03 +/- 0.76, 2.08, and 0.95 Msun, respectively.             Mlk2012 
14260+3422   GIC 118     AB = G178-026/G178-025.                                                         
14260+0714   STT 282     LDS 959.                                                                        
14261-4513   DUN 160     tau 1 Lup. Variable. B is CD-44@9321.                                           
14262-0950   RST3878     TDS9203.                                                                        
14262-4404   SWR 158     CPM pair                                                                Skf2004 
14262-4523   I   402     tau 2 Lup.                                                                      
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.67 +/- 0.76, 4.55, and 3.11 Msun, respectively.             Mlk2012 
14265+1557   CLO   1     Konopacky et al. (2010) derive a distance of 34 +/- 13 pc and a system          
                         mass of 0.11 +0.08/-0.11 Msun.                                          Kon2010 
14265+1459   LDS5818     LDS6294.                                                                        
                         NLTT 37341/37342                                                        Chm2004 
14265-5034   CPO 388     CPD-50@6917.                                                                    
14266+0208   HJ 1254     LDS5819.                                                                        
                         HJL 204.                                                                HJL1986 
14267+1625   A  2069     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.92 +/- 1.69, 2.50, and 1.10 Msun, respectively.             Mlk2012 
14268-0511   HWD   1     AC: Howard et al. (2010) determined that the extremely metal-rich A             
                         component is orbited by a massive planet (M sin 1 = 0.38 Mjup) in a             
                         3.41y, e=0.41 orbit. The C component is an M dwarf, with estimated              
                         mass 0.32 Msun and a projected separation of 33 AY                      Hwd2010 
                         AC: Ginski et al. estimate the mass of C at 0.307 +/- 0.033 Msun.       Gns2012 
14269-6630   RSS  23     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
14270-0308   LDS4466     LDS6295.                                                                        
14275+7542   HJ 2733     5 UMi.                                                                          
14276+1343   BPM 617     [PM2000] 1086775 + [PM2000] 1086813.                                    Gvr2010 
14277+5347   GIC 119     G200-040/G200-039.                                                              
14278+0007   BAL1172     RST 5386.                                                                       
14278-0140   BAL 555     J 2105.                                                                         
14279+2123   HO  543     HJL 205.                                                                HJL1986 
                         STF3085.                                                                        
14279-0032   GIC 120     G124-043/G124-044.                                                              
14279-1806   FEN  20     J 2662.                                                                         
14280+3546   COU1266     AC: Aka DAM  80.                                                                
14282-0214   STF1846     phi Vir = 105 Vir. A may be a spectroscopic binary.                             
14282-2929   FIN 306     52 Hya.                                                                         
14283+6349   LDS2343     NLTT 37499/37498                                                        Chm2004 
14284-3922   HRG  95     This is the variable star V1005 Cen                                             
14286+2817   STF1850     B is BD+28@2331, and is a spectroscopic binary.                                 
14287-1012   STF1847     B is BD-09@3946.                                                                
                         A measure of A and BD-09@3950: 1907.26, Delta (delta) 190.80".                  
14288+5430   HJ 2725     AB,C: Rectilinear solution by Friedman et al. (2012).                   USN2012a
14291+6917   MLR 170     The scattered measures and quadrant ambiguity make determination of             
                         the direction of motion impossible.                                             
14293+0018   SHY 649     AB: HIP  70845 + HIP  70649.                                                    
14294+8049   GC 19630    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
14295+3612   HU 1268     A premature orbit has been computed.                                            
14295+1225   BPM 618     [PM2000] 1087737 + [PM2000] 1087751.                                    Gvr2010 
14295-3702   SEE 205     AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
14298+3510   ALI 128     No secondary seen. Apparently typo or plate flaw in AC catalog.                 
14298+3445   LDS4470     SLW1001.                                                                        
14300-5608   KOU  29     V853 Cen.                                                                       
14301+4737   COU2387     Also known as HDS2046. This double was first resolved by Couteau, but   Cou1988b
                         placed in the WDS at the wrong coordinate and not matched with HDS2046          
14303-4931   HDO 232     A is a spectroscopic binary, spectrum composite; A1V+B.                         
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
14307+8308   LDS1800     Rectilinear solution by Cvetkovic et al. (2015).                        Cve2015 
14308+0446   BU 1443     See BDS 6932. Burnham could not find star measured by Madler. No star   Bu_1906 
                         in or near Madler place. B is BD+05@2885.                                       
14308-0839   BUP 158     Proper motion -1272 -236.                                                       
                         Rectilinear solution by Josties & Hartkopf (2017).                      Msn2017g
14308-5029   LDS 490     B is CD-49@8796.                                                                
14310+1120   BPM 619     [PM2000] 1088568 + [PM2000] 1088537.                                    Gvr2010 
14310-0548   RST4529     Two orbit solutions by Heintz (1981), but the long-period, circular     Hei1981a
                         orbit is ruled out by speckle observations.                                     
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.89 +/- 0.22, 1.91, and 0.95 Msun, respectively.             Mlk2012 
                         Orbital parallax 23.83 +/- 0.8 mas. Mass-A is 1.01 +/- 0.16 \msun.      ATl2021 
                         Mass-B is 0.90 +/- 0.14 \msun.                                                  
                         Mass-A is 1.12 +/- 0.11 and Mass-B is 1.01 +/- 0.11 \msun.              EEA2021 
14310-3006   RSS 341     Y Cen.                                                                          
14312+3426   HU  904     Van Biesbroeck and Fox identify this pair as BD+35@2575, but Hussey     VBs1936 
                         says it is 5.59s following and 4' 46.4" north of that star.             Fox1925 
                         Aka TDS9227.                                                            Dam2018l
14313-1538   BU  117     AB = HDO 139                                                                    
                         AB: A = SB? No orbit.                                                   Tok2014d
14317+0150   AG  195     Heintz believes HJ 5485 is identical; there is no pair in the place     Hei1983a
                         formerly assigned to Herschel's pair.                                           
14318+3022   HJ 2728     rho Boo = 25 Boo                                                                
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
14321+3818   BLM   3     Aa,Ab: gam Boo = 27 Boo = Seginus. A is a Delta Scuti-type system.              
                         1975.383: Photometric variable star of tentative period 0.29 day;               
                         also a member of a binary system with separation ~33".4 and delta m             
                         ~ 9.27. This observation apparently resolves the brighter primary into          
                         two stars.                                                              BLM1978 
                         NPOI Limb-darkened diameter    1.726 +/- 0.011 mas,                             
                         R =    4.65 (+/- 0.04   )  \rsun,  Teff = 6203 +/-  20 K,                       
                         L =   28.9 +/-   0.4 \lsun.                                             NOI2023 
             BU  616     AB: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
14321-2743   SKF1971     Primary is the eclipsing binary V356 Hya.                               Skf2013 
14323+8020   STTA130     B is BD+80@444.                                                                 
14323+2641   A   570     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Martin et al. (1998) derive component masses 1.892 +/- 0.410 and                
                         1.162 +/- 0.257 Msun.                                                   Mig1998 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.57 +/- 0.72, 3.29, and 1.74 Msun, respectively.             Mlk2012 
14324+3138   STF1855     Same as STF1856.                                                                
                         AB: HJL 206.                                                            HJL1986 
                         AB: SEI 536.                                                            Nsn2017b
14325+3442   HJ  554     AB: HJL 207.                                                            HJL1986 
14326-5027   RIZ  10     Sig Lup.                                                                        
14326-5653   EVS  23     Primary is the Cepheid V Cen.                                           Evs2016a
14327-1246   GLP   3     B is BD-12@4080.                                                                
14329+4126   HJ 1255     B is BD+42@2510.                                                                
14330+0340   HD127742    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
14331+5528   LEP  68     NI   33.                                                                        
14331+2154   WOL   1     WSP  14.                                                                        
14343+2424   STTA129     B is BD+25@2797.                                                                
                         H 6  52.                                                                MEv2010 
14345+0540   J  1122     A measure in 1952: 279.2@, 1.4". The 1957 measure may be inaccurate.            
14345-6317   HJ 4683     Spectrum of B: A8/F0.                                                           
14347+2945   STT 582     sig Boo = 28 Boo. Possibly variable.                                            
                         NPOI Limb-darkened diameter    0.714 +/- 0.205 mas,                             
                         R =    1.21 (+/- 0.35   )  \rsun,  Teff = 6922 +/- 994 K,                       
                         L =    3.0 +/-   0.0 \lsun.                                             NOI2023 
14349+2510   LDS4481     NLTT 37790/37787                                                        Chm2004 
14350+0907   RUC   8     Multiple system including contact binary CK Boo. Pribulla & Rucinski            
                         (2006) estimate the mass of the contact pair at 2.012 Msun and the      Pbl2006 
                         minimum mass of the wider component at 1.50 Msun.                               
                         Spectral type of resolved companion estimated at M1V.                   Ruc2007 
14350-2336   LUH  10     2MASS J14345819-2335572 + 2MASS J14351087-2333025.                      Luh2012b
14351-6101   B  2338     A is the Cepheid TX Cen.                                                        
14351-7619   GLI 206     Also known as R   247.                                                          
14352+2438   RAO 503     AD Boo.                                                                         
14354+2546   RAO 317     pa error = 355 deg.                                                     RAO2020b
14354-2954   LDS 492     NLTT 37783/37782                                                        Chm2004 
14358+0620   MAD   6     Not found by Burnham.                                                   Bu_1906 
                         The pair was later rediscovered by Soulie (2007) and coordinates        Sle2007 
                         verified in 2009 by colleague Florent Losse.                                    
14359-6958   DON 664     CI Cir.                                                                         
14360+0945   HZE   1     GJ 3860 = HN Boo. Heinze et al. (2010) determine that the new companion         
                         is a background object.                                                 Hze2010 
14363-4615   HDO 236     A is variable.                                                                  
14365-0536   GWP2417     QX Vir.                                                                         
14369+4813   A   347     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.19 +/- 1.18, 2.79, and 1.35 Msun, respectively.             Mlk2012 
14370-1218   GC 19695    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
14372+5214   MLR 682     Also known as TDS 755.                                                          
14372-6201   EVS  24     Primary is the Cepheid V737 Cen.                                        Evs2016a
14373-4608   FIN 318     Aa,Ab: Docobo & Andrade (2013) derive a dynamical parallax of 5.32              
                         +/- 0.20 mas (based on their orbital elements and masses expected from          
                         spectral types) or 4.65 +/- 0.12 mas (based on their elements and               
                         masses given by Tokovinin 2008 MNRAS 389, 925). See paper for                   
                         extensive notes on this system.                                         Doc2013d
14374+1102   AG  345     LDS 965.  HIP 71505. See Allen et al. (2000) for information on         AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
14375+4743   TDS9251     Ca-Cb: Initially listed incorrectly as Aa,Ab.                                   
14375+0217   CHR  42     Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 2.28 +/- 0.81, 2.95, and 1.10 Msun, respectively.  Mlk2012 
14375-2941   WNO  19     B is CD-29@11196.                                                               
14376+3652   FAR  41     Primary is white dwarf WD 1435+370.                                     Far2006 
14377+1632   BPM 620     [PM2000] 1092020 + [PM2000] 1091979.                                    Gvr2010 
14378-6756   WFC 153     Rectilinear solution by Mason & Hartkopf (2014).                        Msn2014b
14379-4926   RIZ  11     Rho Lupi.                                                                       
14380-5431   DUN 163     B is CPD-53@6038.                                                               
14382+1402   TOK 406     HIP 71572 is an acceleration binary without RV data. It is found to be          
                         a tight 90-mas pair with a small dm and an estimated period under 10yr          
                         (some motion is seen in one month). Very likely it can be studied as a          
                         double-lined SB.                                                        Tok2015c
14384+3632   ALI 367     Primary is eclipsing binary GK Boo (period 0.47777day).                 Zas2010 
14384-1940   HJ 2734     LDS4484.                                                                        
14390+6417   KON   1     Koenig et al. (2005) calculate combined speckle/spectroscopic orbital   Kng2005 
                         solution and derive masses of 0.9 +/- 0.1 and 0.5 +/- 0.1 Msun for the          
                         primary and secondary, respectively. The primary is the young active            
                         variable EK Dra.                                                                
14395+5154   LDS4487     SLW1014.                                                                        
14395-6812   MLO  58     The primary is slightly variable.                                               
14396-6050   RHD   1     alp Cen = LDS 494 = Rigel Kentaurus. C is Proxima Centauri = V645 Cen.          
                         According to R.G. Aitken, this was discovered by                        A__1935f
                         Father Richaud while observing a comet at Pondicherry, India, in        Rhd1729 
                         December 1689. P= 79.9y, a = 17.52", motion direct. Due to the                  
                         proximity of the pair and the eccentricity of the system, the                   
                         separation ranges from 2 to 22". AB is also known as Rigil Kentaurus.           
                         Henroteau notes that a first attempt to measure the relative positions  HFC1928 
                         of binary components was made by Father Louis Feuillee in 1709, when    Feu1714 
                         he estimated the position angle and distance for alp Cen.                       
                         Proper motion -3642 +699. The distant companion, Proxima Centauri,              
                         distance 9000" was discovered by Innes. It is the flare star V645 Cen,  I__1905 
                         (mag. 10.7, 2.2 degrees distant, M5Ve). See Kamper & Wesselink (1978).  Kpr1978 
                         The secular changes of a, i, node, and longitude of periastron have             
                         been allowed for; quoted elements are for 2000.0.                               
                         The semi-major axis has been revised (Heintz 1982).                     Hei1982a
                         Difficult for Hipparcos with secondary (= HIP 71681) at edge of         Sod1999 
                         the sensitivity profile. Present parallax preferable to HIP value.              
                         Mass-ratio from Kamper & Wesselink.                                             
                         Pourbaix gives two combined solutions for this resolved SB2, each       Pbx2000b
                         yielding orbital parallaxes and component masses.                       Pbx2002 
                         AB: Additional notes may be found in van den Bos (1931).                B__1931b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.98 +/- 0.03, 2.04, and 1.79 Msun, respectively.  Mlk2012 
                         Powell also measured a more distant component (CPD-60 5485) which is    Pwl1864 
                         obviously non-physical (1860.312, 353.7 deg, 161.5").                           
                         VLTI Uniform disk diameter of A,B:                                      LTI2003b
                           =  8.314  +/- 0.016,  5.856  +/- 0.027 mas,                                   
                         VLTI Limb-darkened diameter of A,B:                                             
                           =  8.511  +/- 0.020,  6.001  +/- 0.034 mas,                                   
                         R =  1.224  +/- 0.003,  0.863  +/- 0.005  \rsun.                                
                         VLTI Limb-darkened diameter of Proxima (C) 1.044 +/- 0.08 mas,          LTI2003a
                         M = 0.123 +/- 0.006 \msun, R = 0.145 +/- 0.011 \rsun,                           
                         T = 3042 +/- 117 K.                                                             
                         VLTI uniform disk diameter of C:       0.990 +/- 0.050 mas,             LTI2009 
                         VLTI limb-darkened disk diameter of C: 1.011 +/- 0.052 mas,                     
                         R = 0.141 +/- 0.007 \rsun, Teff = 3098 +/-  56 K,                               
                         M = 0.123 +/- 0.006 \msun.                                                      
                         Teff-A = 5829 +/- 6, Teff-B = 5189 +/- 18 K.                            XXX2018a
                         Based on astroseismology, age is 5.9 to 7.3 Gyr.                        XXX2021a
                         Ma = 1.0788 +/- 0.0029 \msun, Mb = 0.9092 +/- 0.0025 \msun;                     
                         Ra = 1.2175 +/- 0.0055 \rsun, Rb = 0.8591 +/- 0.0036 \rsun.             Ake2021 
             LDS 494     AC: alp Cen + Proxima Cen                                                       
                         The Kervella et al. (2017) orbit is based on the following adopted              
                         physical parameters:                                                            
                         alp Cen A: M = 1.1055 +/- 0.0039 Msun  R = 1.2234 +/- 0.0053 Rsun               
                         alp Cen B:     0.9373     0.0033           0.8632     0.0037                    
                         Proxima  :     0.1221     0.0022           0.1542     0.0045            Krv2017 
             SCZ   1     Ca,Cb: Proxima Centauri. Not a binary!                                  Tok2014d
                         Ca: Based on spectroscopic orbit of Proxima Cen b by Anglada-Escude et          
                         al. (2016 Nature 536, 438), Brown (2017) derives an estimate of 0.25            
                         for the eccentricity of the planetary companion.                        BnR2017 
             alp Cen     Beamin et al. (2017) searched for faint co-moving companions to the             
                         alpha Cen system, examining CCD tiles covering a ~19 deg^2 area and             
                         taken at multiple epochs between 2010.2 and 2015.5. No additional               
                         companions were detected down to limiting magnitudes Y=19.3 and J=19.   VVV2017b
14397+1827   ALP  18     2MASSW J1439409+182637                                                          
                         Physical companionship to this ultracool dwarf ruled out based on i-z           
                         and z-J colors, using photometry from SDSS.                             AlP2007 
14397-2643   BU  805     HIP 71682. Linear configuration, C is between AB.                               
                         AB: A possible astrometric pair (Makarov & Kaplan 2005). No SB orbit.   Mkr2005 
                         AC: SHY 262. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
14400-2435   LDS6297     NLTT 38011/38013                                                        Chm2004 
14403+3027   HJL1088     SHY 655. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
14403-4051   HNK   1     Aa,Ab: Member of Sco-Cen Association. Mass of Aa 3.41 +0.53/-0.75Msun;          
                         mass of Ab estimated at 146 +45/-32 Mjup (for age 10 Myr), or                   
                         217 +67/-47 Mjup (for age 20 Myr).                                      Hnk2015 
14403-4548   SEE 209     The primary is slightly variable.                                               
                         IT Lup.                                                                         
14404+2159   MCA  40     A spectroscopic triple system, with periods 101.6 and 3320 days.                
                         The long-period pair has covered more than half its orbit; the orbit            
                         may be determinable.                                                    Bag1984a
                         Barlow & Scarfe (1991) give combined spectroscopic/speckle              Scf1991 
                         interferometric solution.                                                       
                         1985.5226: This measure was found to give very large residuals to the           
                         orbit of Barlow & Scarfe (1991). Comments in our reduction log note     Scf1991 
                         the measure was marginal, and after reinspection we have determined             
                         this measure was spurious.                                              Hrt1992b
                         Martin et al. (1998) derive component masses 3.344 +/- 1.000 and                
                         3.289 +/- 0.988 Msun.                                                   Mig1998 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 6.55 +/- 1.65, 4.67, and 1.05 Msun, respectively.             Mlk2012 
14405-4240   HJ 4692     A,BC = SWR 159. CPM pair. B component is 0".5 pair                      Skf2004 
14405-5702   LDS 495     HIP 71735. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
14407+1625   STF1864     pi 1 Boo = 29 Boo A. B spectrum A6V.                                            
                         Both components are spectroscopic binaries.                                     
                         Measure of 1927.36 made by triangulation of multiple measures.                  
                         AB: H 3   8.                                                            MEv2010 
14410+5757   STF1872     LDS1417.                                                                        
                         AB: NLTT 38127/38134                                                    Chm2004 
                         AB: HJL 208.                                                            HJL1986 
14411+1344   STF1865     zet Boo = 30 Boo.                                                               
                         Spectral types and masses of components assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Errors for orbit of Alzner (2007) provided by author (private comm.)    Alz2007 
                         Hipparcos parallax yields a mass sum 7.95 Msun, rather high for a pair          
                         of A0V stars. Increasing parallax by 1 sigma (1.24mas) yields a more            
                         reasonable mass sum of 6.51 Msun, however.                                      
                         Calculated mass sum is 122  +/- 275 Msun, unconstrained.                Mut2010b
                         AB: Additional notes may be found in Fu et al. (1997)                   McA1997 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 5.60 +/- 1.66, 5.20, and 4.48 Msun, respectively.  Mlk2012 
             H 6 104     H VI 104.                                                                       
14414+1857   BFR  11     LSPM J1441+1856 + 2MASS J14412565+1856484. Baron et al. (2015)                  
                         estimate spectral types M6 and L1 +/- 1, distances 56 +37/-10 and               
                         99 +10/-34 pc, masses 0.102-0.133 and 0.072-0.079 Msun.                 BFr2015 
14414-3548   TDS9269     V1063 Cen.                                                                      
14415+2957   LDS6298     NLTT 38115/38116                                                        Chm2004 
14416-0946   SEF   1     G 124-62 + DENIS-P J144137.2-094558. CPM with the close L1+L1 pair              
                         MEL   8Ba,Bb. Distance to the system 34+/- 7 pc, age 500-850 Myr.       Sef2005a
                         Jameson et al.(2008) confirm the CPM nature of this pair.               Jms2008 
14417+0932   STF1866     Same as STF1868.                                                                
14417+0523   OL  160     Not found by Heintz.                                                    Hei1995 
14419-4723   HDO 238     alp Lup. Variable.                                                              
14420-3110   BRT3012     A likely plate flaw.                                                    Grv2021b
14421+6116   STF1878     A is the Delta Scuti-type variable DL Dra.                                      
14424+6603   GKI   4     G239-025 = GJ 9492                                                              
                         Primary has spectral type M3.0, secondary late M. At distance of 9.9            
                         +/- 1.2 pc and assuming primary mass of 0.32 +/- 0.15 Msun, the pair            
                         has an estimated orbital period of 370 +/- 100y.                        Gki2004 
14425-6459   DUN 166     alp Cir. Probably variable.                                                     
14426+1929   HU  575     Identification of the ascending node, based on a few Mt. Wilson                 
                         spectra, is uncertain at this small difference in magnitude.            Mlr1952b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 0.99 +/- 0.19, 1.28, and 0.55 Msun, respectively.  Mlk2012 
14427-0558   STF1869     B is BD-05@3935.                                                                
14430+1310   KU   48     AB: HJL 209.                                                            HJL1986 
14431+1803   GIC 121     LDS5223. G135-087/G135-086.                                                     
14432-4110   LDS 500     UC 2829. Identification of LDS pair is uncertain, however.                      
14433+1708   BRT2419     Secondary is brighter than primary                                      Los2005 
14434+5155   SKF1640     A is SB2, P=6.459d                                                      Tok2014d
14435-6258   B  1759     C is variable.                                                                  
14436-0415   JNN 100     The two components resolved by AstraLux have very similar brightnesses          
                         and colors, hence physical companionship is probable, although common           
                         proper motion has not yet been tested for.                              Jnn2012 
14437+6234   STI 773     The 1902 discovery observation is in error, due to an apparent          Vat1926 
                         typographical error in the original AC catalog entry for the                    
                         declination of the B component.                                                 
14439+4743   ES  962     MN Boo. Algol-type eclipsing binary, period 0.38769 d.                  Zas2019 
14441+6106   STF1882     AB: H 3  61.                                                            MEv2010 
14443-2701   B   276     ADS 9359a.                                                                      
14446-2215   LDS4498     NLTT 38244/38248                                                        Chm2004 
14448+0742   STF1873     H 2  82.                                                                MEv2010 
14449-3423   JNN 157     Secondary appears to be a very low mass star just above the hydrogen-           
                         burning limit. Masses are estimated at 1.4 Msun and 95 +64/-40 (based           
                         on intrinsic brightness) or 45 +/- 15 Mjup (based on temperature).      Jnn2012b
14450+2704   STF1877     eps Boo = 36 Boo = Izar. B is a spectroscopic binary.                           
                         Scardia et al. say the quadrant is unambiguous for their 2004 theta     Sca2005a
                         value of 162.9. This may have been a typographical error on their               
                         part, as other observers find the secondary to be in the opposite               
                         quadrant and a large magnitude difference.                                      
                         AB: H 1   1.                                                            MEv2010 
14452-4955   EGN  14     The AB pair bound. Primary is K3, B component probably M2.5-M5.5 with           
                         mass 0.18 +/- 0.03 Msun. The C and E components are background stars,           
                         but with only a single epoch the bound/unbound nature of the AD pair            
                         is unknown. The D component is a close binary                           Egn2007 
14452-5536   DUN 169     The primary is BU Cir, a Beta CMa-type variable. B is CPD-55 6152.              
14453-3609   I   528     Too close, measures uncertain.                                                  
14455+4223   STT 285     A faint star (mag. 12.46, 50") has common proper motion                 Maa1938 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.59 +/- 0.86, 2.70, and 1.17 Msun, respectively.  Mlk2012 
14455-1311   LDS4501     NLTT 38285/38284                                                        Chm2004 
14457+6701   LDS2349     GIC 114. G239-027/G239-028. A typographical error led to the Giclas             
                         pair being originally entered in the WDS as 13463+6658.                         
                         NLTT 38380/38391                                                        Chm2004 
14459+2344   COU 100     Docobo et al. (2010) derive a dynamic parallax of 19.95 +/- 0.30 mas    Doc2010h
                         and a total mass of 1.52 +/- 0.09 Msun.                                         
14460+3329   FAR  42     Primary is white dwarf WD 1443+336.                                     Far2006 
14460-1528   HLD  20     5 Lib.                                                                          
14460-2527   H 3  97     H III 97. 54 Hya.                                                               
14462+0154   JNN   9     109 Vir.                                                                        
14462-2111   FIN 309     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.51 +/- 0.21, 2.38, and 1.02 Msun, respectively.             Mlk2012 
14463+0939   STF1879     Mason et al (1999) period should be 243, not 253 yrs (Alzner,           Msn1999a
                         private comm.)                                                                  
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.73 +/- 0.35, 2.10, and 1.00 Msun, respectively.  Mlk2012 
14464-3346   HDS2082     AB + TOK 407Ba,Bb: HIP 72235B is located at 9" from the primary star            
                         and shares its proper motion (AB = HDS 2082). Pre-discovery                     
                         measurements of this Hipparcos pair were published by Wycoff et al.             
                         (2006 AJ 132, 50). The RV of A may be variable (Latham, 2012, private           
                         communication). The star B turns out to be a 0".4 binary Ba,Bb with             
                         masses of 0.70 and 0.17 Msun estimated from the luminosity. Its period          
                         is on the order of 100yr. The whole system could thus be quadruple.     Tok2015c
                         AB: Primary is SB?                                                      Tok2014d
14464-7847   HJ 4689     B is CPD-78@889.                                                                
14467-6128   EVS  25     Primary is the Cepheid BP Cir.                                          Evs2016a
14471-7329   HJ 4693     B is CPD-72@1571.                                                               
14473-5256   BRT2078     A likely plate flaw.                                                    Grv2021b
14475-0017   HD 130322   No comoving objects found within separation/magnitude range listed.             
                         However, Chauvin et al. (2006) note finding at least one faint          Cvn2006 
                         background object.                                                              
14477+2406   HO  263     Suspected double by Hough, but unconfirmed by many other observers;     Ho_1890 
                         duplicity still in doubt.                                                       
14478+1037   BPM 621     [PM2000] 1097755 + [PM2000] 1097751.                                    Gvr2010 
14479-3325   HJ 2744     SWR 160.                                                                        
14482-3647   HJ 4701     LDS 505.                                                                        
14485+2445   COU 304     Primary is EM Boo, Algol-type eclipsing binary, period 2.446228d.       Zas2013 
14485-1720   BU  346     Primary is SB and astrometric binary, P=1724d                           Tok2014d
14489+0557   STF1883     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.86 +/- 1.15, 2.41, and 1.17 Msun, respectively.             Mlk2012 
14492+1013   A  2983     Two orbit solutions by Eggen (1967). Long-period solution later ruled   Egg1967 
                         out by speckle observations.                                                    
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.58 +/- 0.89, 1.74, and 0.79 Msun, respectively.             Mlk2012 
                         Double lined spectroscopic binary whose orbit generates masses of       Grf2015c
                         0.308 +/- 0.012 and 0.306 +/- 0.011 Msun * sin^3 i.                             
                         Orbital parallax 21.81 +/- 0.8 mas. Total Mass is 1.61+/-0.26 \msun.    ATl2021 
14492-5924   FIN 298     Motion direct.                                                                  
14493-1409   BU  106     mu Lib = 7 Lib                                                                  
                         AC and AD: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         AE: There are two other faint stars in the directions of 74.7 and 56.5          
                         deg, respectively, a little farther than E.                             Bu_1894 
14493-2415   H 6 117     H VI 117.                                                                       
14495+5122   STF1889     Both components are spectroscopic binaries.                                     
                         A spectroscopic binary of indeterminate period.                         Tok2019b
                         AB: H N 116.                                                            MEv2010 
14496+2356   JMS   4     2MASS J14493784+2355378 + 2MASS J14493550+2357118.                      Jms2008 
14497+4843   STF1890     39 Boo. B is a spectroscopic binary. Spectral types F6V+F5V.                    
                         H 2  79.                                                                MEv2010 
                         While a linear solution is possible, common parallax and proper motion          
                         argue for an orbital solution.                                          Izm2019 
14497-2605   LDS 508     NLTT 38457/38454                                                        Chm2004 
14497-4300   CPO 402     B is CD-42@9693.                                                                
14503+8231   HZE   2     GJ 3876. Heinze et al. (2010) determine that the A and B components             
                         definitely comprise a CPM pair.                                         Hze2010 
14503+2355   POT   1     GJ 564. Both B and C components are determined to be young contracting          
                         brown dwarfs, spectral type dL2, with masses <0.075 and <0.065 Msun,            
                         respectively.                                                           Pot2002 
                         CHARA Array Limb-darkened diameter of A :                               CIA2013c
                         R =  1.1119 +/- 0.0229 \rsun, L =   1.2437 +/-0.0174 \lsun,                     
                         Teff = 5787 +/-  57 K, M = 0.989 \msun, Age = 7.5 Gyr.                          
                         BC: Assuming an Hipparcos distance of 18.18 +/- 0.08 pc, Konopacky et           
                         al. (2010) derive a system mass of 0.109 +/- 0.002 Msun.                Kon2010 
                         BC: Dupuy & Liu (2011) derive a mass sum of 0.1095 +/- 0.0022 Msun,             
                         and a mass ratio of 0.948 +/- 0.005.                                    LiM2011 
                         BC: Malkov et al. (2012) derive dynamical and photometric spectroscopic         
                         masses 0.11 +/- 0.01 and 0.38 Msun, respectively.                       Mlk2012 
                         BC: Dupuy et al. (2009) derive orbital parameters for the BC pair,              
                         which is comprised of a pair of L4 dwarfs. They determine a mass sum            
                         for the pair of 0.109 +/- 0.003 Msun.                                   Dup2009c
14504-6625   FIN 426     Spectrum: G8/K1(IV)+A/F.                                                        
14505-6730   RSS 349     Classical Cepheid AV Cir.                                                       
14505-7032   HJ 4697     B is CPD-70@1824.                                                               
14506-0001   STF1885     H 1  78.                                                                MEv2010 
14507+7409   BUP 159     bet UMi = 7 UMi = Kochab                                                        
14509-0810   BRT 551     J 1612.                                                                         
14509-1603   SHJ 186     alp 2 Lib = 9 Lib = Zubenelgenubi. B is BD-15@3965. A is a                      
                         spectroscopic binary.                                                           
             CAB   1     AD: HIP  72622 + HIP  71743.                                            Cab2010 
14510+6718   LDS2351     NLTT 38643/38642                                                        Chm2004 
14510+0943   STF1886     BDS 7052; MAD same star.                                                        
14511+0557   WSP  40     HTP  27.                                                                        
14511-3706   I   529     A premature orbit has been computed.                                            
14511-6153   JSP 640     CD-61@4558                                                                      
14512+3107   BWL  39     AE: Colors and/or astrometry are inconsistent with a late-type common           
                         proper motion companion based on visual inspection of the field from            
                         2MASS, SDSS, DSS1, and/or DSS2. Primary is G 166-49.                    Bwl2015 
14513-1700   HU 1270     BC: North and fainter of a 30" pair; ADS is not clear on this point.    B__1949c
14514+1906   STF1888     xi Boo = 37 Boo = EO Boo.                                                       
                         Three orbit solutions by Wielen (1962), only orbit #3 is now in the     Wln1962 
                         orbit catalog. The RV difference is small and renders identification            
                         of the ascending node uncertain.                                                
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         CHARA Array Limb-darkened diameter  1.196 +/- 0.014 mas,                CIA2012e
                         R =  0.863 +/- 0.011 \rsun, L =  0.645 +/-0.015 \lsun,                          
                         Teff = 5580 +/-  46 K.                                                          
                         AB: H 2  18.                                                            MEv2010 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.59 +/- 0.21, 1.60, and 1.56 Msun, respectively.  Mlk2012 
                         AD: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
                         AD: Rectilinear solution by Friedman et al. (2011).                     USN2011a
14516-4335   FIN 319     omi Lup                                                                         
14517-3053   H N  48     B is CD-30@11767.                                                               
14517-7328   GLI 210     SWR 161. CPM pair                                                       Skf2004 
14519+5147   LDS4513     NLTT 38649/38650                                                        Chm2004 
14522+1638   FAR  16     Primary is white dwarf WD 1449+168.                                     Far2005b
14523-4455   DON 689     CPD-44@7016.                                                                    
14524+1757   A  2071     EQ Boo, Algol-type eclipsing binary, P = 5.43536 d.                     Zas2011 
14525+1844   BU   31     HIP 72764.                                                                      
                         AB: A or B are SB? Trapezium (2" and 8")?                               Tok2014d
14525+0007   GIC 122     G066-035/G066-036.                                                              
14526-1151   LDS 511     B is BD-11@3820.                                                                
14526-6349   HDS 2100    Primary is the Cepheid AX Cir. The wide HDS pair has a spectroscopic            
                         orbit, P=6532d, e=0.19 (Evans 2000 AJ 119, 3050).  Gallenne et al.              
                         resolved the primary into a 20mas pair, and find a minimum mass for             
                         Aa+Ab > 9.7 +/- 0.6 Msun.                                               GaA2014 
                         Masses are 5.2 and 5.0 Msun. Estimated period = 17.9y,                          
                         a = 14.8au = 0.03".                                                     Evs2013 
14527+0746   HLD 120     AB. Schlimmer (2008) published linear elements rather similar to those  Smr2008 
                         in the Rectilinear Elements Catalog: x = -1.1407, y  = -0.9315,                 
                         To = 2229.42  +/- 1.74, sep=    1.473 +/- 0.2, PA =  309.24  +/- 0.5            
14533-5220   CPO 403     CPD-51@8545.                                                                    
14534+1909   GC 20037    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Beavers & Salzer (1983).                                                Bvr1983 
14534+1542   STT 288     CfA: A or B have variable RV?                                           Tok2014d
14535-4637   B  2774     A: S Lup                                                                        
                         B: X Lup                                                                        
14537+2321   COU 101     Rectilinear solution by Mason & Hartkopf (2016).                        Msn2016a
14540+2335   REU   2     Additional notes may be found in Wilson (1954) and Wilson (1955).       WRH1955 
14540-6333   RST9005     Previously known as RST 730a.                                                   
14543+0312   BAL2401     May be the same as HJ 5491.                                             Dam2010 
14543-3737   CD-37 9777  Listed as possibly resolved by White et al. (1991), but no separation   Whi1991 
                         or position angle given.                                                        
14544-3409   I   226     Wagner et al. (2016) imaged a Jovian exoplanet orbiting the primary at          
                         a distance of ~80au. They also resolved the Innes B component into a            
                         70mas pair, which they designate as B and C. However, the C component           
                         designation is already in use for Innes' 30" companion. Also, their B           
                         designation redefines B from the photocenter of the previously                  
                         unresolved close stellar pair to one component of that pair. We have            
                         therefore designated the two stars as Ba and Bb, in keeping with our            
                         usual hierarchical designation scheme.                                          
                         Wagner et al. derive the following parameters for system components:            
                                            Aa        Ab             Ba         Bb                       
                            --------------------------------------------------------                     
                            Spectral type   A1V       T2–T4          G          K                .     
                            Mass (Msun)     1.82      4+/-1 Mjup     0.96       0.6                      
                            Teff (K)        9300      850 +/- 50     5700       4400             WgK2016 
14545+1606   FRT   1     AB: The companion is of spectral type dM8.5.e. The measure was made in          
                         the infrared.                                                                   
             MEL   2     GJ 569 Ba,Bb. Lane et al. (2001) paper also includes spectroscopic      Lne2001 
                         information and discussion of spectral type, masses, evolutionary               
                         state, etc.                                                                     
                         Zapatero Osorio et al. (2004) give combined spectroscopic/astrometric   Oso2004b
                         solution, yielding masses 0.071 +/- 0.011 and 0.054 +/- 0.011 Msun.             
                         Total system mass is 0.125 +/- 0.007 Msun.                              Smn2006 
                         Incorrectly listed as MEL   1.                                                  
                         Ba,Bb: GJ 569. Assuming an Hipparcos distance of 9.81 +/- 0.16 pc,              
                         Konopacky et al. (2010) derive a system mass of 0.126 +/- 0.007 Msun.   Kon2010 
                         Dupuy et al. (2010) determine system mass 0.140 +0.009/-0.008 Msun;             
                         spectral types are  M8.5 +/- 0.5 and M9.0 +/- 0.5.                      Dup2010b
14546-3318   BU  347     CPD-32@3746.                                                                    
14550+4301   OSO  60     G178-056. Not a common proper motion pair, based on astrometry and              
                         color                                                                   Oso2004 
14551-0906   TOK 164     HIP 72998.                                                              Tok2011a
14557-3351   HO  390     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2014).                         USN2014a
14558+3939   A  1627     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.37 +/- 0.49, 2.64, and 1.45 Msun, respectively.             Mlk2012 
14562+1745   HDS2108     AB: Cvetkovic et al. (2016) estimate spectral types K5 and K6, masses           
                         0.65 and 0.60 Msun. Dynamical parallax is 16.63 +/- 1.12 mas.           Cve2016b
             GII  61     AC: GII  85AC.                                                                  
14565+5923   SHY 661     AC: HIP  73105 + HIP  73730.                                                    
             SHY 661     CD: HIP  73730 + HIP  72389.                                                    
14565+1755   LDS4516     Also known as LHS3001/2. Parallax = 56.41 +/- 0.95 mas.                 TSN2010 
14565-3438   B  2778     AB,C: Star C (approx. mag. 14, 6") is probably physical.                        
             SEE 215     AB,D: CPD-34@6262.                                                              
14565-4753   HJ 4715     The primary is a spectroscopic binary.                                          
14566-1406   HJ  561     B is BD-13@4022.                                                                
14567-6247   FIN 372     the Cir. One component is variable.                                             
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 39.70 +/- 16.09, 22.40, and 5.75 Msun, respectively.          Mlk2012 
14568+7454   S   666     8 UMi. B is BD+75@549.                                                          
14568+5235   LDS4517     Assuming the current identification is correct, it appears Luyten's             
                         separation should have been 230" rather than his published 330". The            
                         distance value has been adjusted accordingly. (WIH, May 2008)                   
14568-7029   R   253     Also known as WFC 158.                                                          
14571+3529   HJ  243     Same as STT 290.                                                                
14574+8529   BU  353     AB: TDS9351.                                                                    
             MLR 342     AC: 14574+8530PKO  12. LDS1808.                                                 
                         AC: The discovery measure by Muller was corrected in one of his later   Mlr1973a
                         papers. Originally 15028+8532 MLR 342 until association with                    
                         14574+8529 noticed.                                                     Mlr1978b
14575+3124   HDS2112     Proper motion of B -695 -1160.                                                  
14575-2125   H N  28     AB: LDS 514. B is BD-20@4123.                                                   
                         AB: NLTT 38872/38871                                                    Chm2004 
                         Proper motion of A +1034.13 -1725.45, B +987.02 -1666.69.                       
                         VLTI uniform disk diameter of A:       1.147 +/- 0.029 mas,             LTI2009 
                         VLTI limb-darkened disk diameter of A: 1.177 +/- 0.030 mas,                     
                         R = 0.739 +/- 0.019 \rsun, Teff = 4597 +/- 101 K,                               
                         M = 0.802 +/- 0.040 \msun.                                                      
                         B is a spectroscopic binary, P = 308d.                                          
                         Statistically different parallax for the components indicates they are          
                         non-physical.                                                                   
                         Hipparcos triple solution together with A (= HIP 73184). P,T,e,         Duq1988 
                         omega, and q fixed from Duquennoy & Mayor (1988), cf orbit in           Prr1990 
                         Mariotti et al. (1990).  Poor Hipparcos solution.                       Sod1999 
                         Strand (1943) suspects a perturbation with P = 2.2y, a = 0".020,        Str1943 
                         and Omega = 30 deg.                                                             
                         Hyperbolic orbit by Hopmann (1967).                                     Hop1967 
                         sigma = areal constant in the true orbit = 2.540 arcsec^2/yr                    
                         q = periastron distance in the true orbit = 20".388                             
                         All hyperbolic orbits rejected from Fourth Orbit Catalog                Wor1983 
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         AF: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         Ba,Bb: Erroneously entered as BC, although C component is a very wide           
                         companion.                                                                      
                         Ba,Bb: Combined solution (spectroscopic/visual/parallax) by Forveille   Frv1999 
                         at al. (1999) for this low-mass interferometric SB2. P = 308.884 +/-            
                         0.004 days, T0 = JD2450270.220 +/- 0.011. Accurate masses are                   
                         determined for these  M dwarfs, as well as J, H, K, and L magnitudes.           
                         1987.455, 1987.756, 1988.312, 1988.499: Vector separations from the 1D          
                         data are combined to give 2D theta and rho values for these 4 dates.    Mar1990 
                         AC, AD, AE: Rectilinear solutions by Mason & Hartkopf (2016).           Msn2016a
                         AF: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
14575-2914   UC 2880     Spurious pair - primary has zero motion, and secondary is irresolved    Skf2013 
                         pair also with zero motion.                                                     
14575-4515   BRT 836     A likely plate flaw.                                                    Grv2021b
14576+6556   RR UMi      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Batten & Fletcher (1986).                                               Bte1986 
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by Batten &           
                         Fletcher (1986).                                                        Bte1986 
14576-0010   H 6  51     1 Ser. H VI 51. Erroneously called 2 Ser.                               Bu_1875 
14579+2953   LDS5827     LDS6299.                                                                        
                         NLTT 38930/38926                                                        Chm2004 
14580-6333   HJ 4714     B is CPD-63@3460, spectrum B8/A0III/IV.                                         
14581-4852   WSI  80     The 14.9 yr SB1 orbit is mentioned by Raghavan et al. (2010).           Rag2010 
                                                                                                 Tok2012a
14581-6317   LDS 856     The same as LDS6300. Determined by Richard Jaworski.                            
14582-3142   LDS5826     LDS6301.                                                                        
14583+1702   BPM 622     [PM2000] 1103818 + [PM2000] 1103757.                                    Gvr2010 
14584+4403   STF1896     AB: Radial velocity variations, based on 10 years of monitoring,                
                         indicate the presence of a giant planet orbiting the B component, with          
                         P = 1544 +/- 34d, a = 2.62 +/- 0.04 au. M sin i = 1.49 +/- 0.09 Mjup.           
                         The primary is an SB in an eccentric orbit with period 25-30 y; mass            
                         of Ab 0.5-0.6 Msun. No companions were detected by AO imaging.          Des2011 
14585+1024   LIM   5     Liu et al. (2011) use IR imaging to determine the components are                
                         likely physical, and determine the distance to the system at 23.1 +/-           
                         2.4pc. The orbital period is estimated at 20-35y. Spectral type of the          
                         primary is T9.5, that of the secondary is >T10, and possibly the first          
                         member of spectral type Y. Mass estimates are strongly dependent on             
                         age: for ages < 0.5Gyr the masses are <9 and <4 Mjup; for ages >2 Gyr           
                         these increase to >20 and >10 Mjup.                                     LiM2011 
                         Liu et al. (2012) derive near-IR spectral types of T9 +/- 0.5 and Y0            
                         +/- 0.5. At a derived photometric distance of 31.9 +/- 2.5 pc, the              
                         two stars are separated by 3.5 +/- 0.3 au.                              LiM2012 
14585-2843   TOK  30     Visual pair has estimated period 175,000y; primary is 14d SB1.          Tok2006 
14585-4726   CPO  62     B is CD-46@9704.                                                                
14587-2739   BU  239     59 Hya. Alternative spectra:; A4V+A6V.                                          
                         1976.474: The observed separation is much larger than that derived              
                         from the elements given by Mourao (1965), which gives a period of       Mro1965b
                         339.3 yr. These elements yield a total mass of 13.65 Msun, which seems          
                         too large for a pair of A5 stars.                                       BLM1978 
14588+3551   COU1136     Docobo et al. (2010) derive a dynamic parallax of 8.68 +/- 0.50 mas     Doc2010h
                         and a total mass of 1.96 +/- 1.04 Msun.                                         
14589+2238   HU  906     TDS9356.                                                                        
14589-1109   STF1894     18 Lib.                                                                         
                         AB: H 4  56.                                                            MEv2010 
14592+0649   HJ 1263     AC = LDS 971.                                                                   
14592-4206   I  1260     kap Cen. A spectroscopic binary and variable star.                              
14592-4206   HDS2116     MAa,MAb=8.38  +/- 0.27 , 4.41  +/- 0.36  \msun.                         GmJ2022 
14593+4649   COU1760     One component is ET Boo, a beta Lyr eclipsing binary.                   Zas2009 
14594+1530   BPM 623     [PM2000] 1104464 + [PM2000] 1104440.                                    Gvr2010 
14595+4528   DAM  30     SHY 264. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
14595+0851   DAY   2     LSPM J1459+0851 + ULAS J1459+0857. Primary is a cool hydrogen-rich              
                         white dwarf, mass 0.585 Msun. Secondary is a T dwarf (T4.5 +/- 0.5),            
                         distance 43-69pc, mass 0.060-0.075 Msun, depending on model.            Day2011 
14596+5352   SHJ 191     STTA132 = H N  63. B is BD+54@1724.                                             
14597+3506   HJ  562     Also known as STF1900.                                                          
14597-3718   BRT1691     A likely plate flaw.                                                    Grv2021b
14597-7831   HJ 4703     Primary is astrometric binary?                                          Tok2014d
14598-2201   Ci 18,1988  Alden (1938) orbit rejected from Fourth Orbit Catalog                   Ald1938b
                         ("not confirmed by subsequent observations")                            Wor1983 
14599+5352   LDS1419     Aka ARY 130.                                                                    
15001-7332   CP-73 1409  HD 131664. Combined astrometric/spectroscopic solution, using                   
                         spectroscopic elements (P,T,e,omega) from Minniti et al. (2009 ApJ              
                         693, 1424).                                                             SaJ2011 
15002-5856   HJ 4719     B is CPD-58@5778.                                                               
15003+0500   LDS5831     LDS6303.                                                                        
15005+7146   9 UMi       Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by Latham et          
                         al. (2002). They derived component masses 1.17 and 0.14 Msun and an     Lat2002 
                         estimated semimajor axis of 38.27 mas.                                  Ren2013 
15006+4717   STT 291     STTA133. A is the Alpha CVn-type variable BX Boo.                               
                         H 5 122.                                                                MEv2010 
15006+0836   YSC   8     Orbital parallax 25.794 +/- 0.085 mas. Mass-A is 0.897 +/- 0.027 \msun. Mdz2021 
                         Mass-B is 0.857 +/- 0.026 \msun.                                                
15008+3508   TY Boo      Multiple system including contact binary. Pribulla & Rucinski (2006)    Pbl2006 
                         estimate the mass of the contact pair at 1.759 Msun and the minimum             
                         mass of the wider component at 0.47 Msun.                                       
15008+2306   LDS4521     SLW1052.                                                                        
15010+7303   TOK 806     TV UMi.                                                                         
15010+3123   STF1901     Burnham gives Delta(delta) from BD+31@2685. 1871.3, 112.3".             Bu_1913 
                         1907.2, 109.9". SEI 538.                                                        
15010-0831   J  1586     del Lib = 19 Lib. A is an Algol-type system.                                    
                         CD: Additional notes may be found in Jonckheere (1952).                 J__1952 
15010-3145   PRO 119     SWR 164.                                                                        
15010-4300   B  1256     Includes IU Lup, an Algol-type eclipsing binary, P = 1.61907d.          Zas2012 
15011+2250   TVLM...     TVLM 513-46546. M8.5 dwarf, observed at 9 epochs between 2010 Mar 17            
                         and 2011 Aug 3 using NRAO VLBA. Pattern to residual motion is close to          
                         noise limit, and gives upper limits to any companion. Data exclude a            
                         phase space of companion masses and orbital periods ranging from                
                         3.8 Mjup (orbital radius ~0.05au, period 16 days) to 0.3 Mjup (orbital          
                         radius ~0.7au, period 710 days).                                        Frb2013 
15012-0406   A    14     Primary suspected of being elongated at ~140deg in 1946 (3 nights).     Baz1948c
15014+6012   GC 20233    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
15016-4223   I  1263     Spectrum K0/2III+A3/5                                                           
15017-0707   GIC 123     G151-019/G151-021.                                                              
15019-0135   ART   2     Artigau et al. (2011) derive spectral types L4.5 +/- 0.5 and L5.5 +/-           
                         1.0. Distance for A is estimated at 31 +/- 5 or 44 +/- 7 pc, depending          
                         on whether it's a single object or an equal-luminosity binary.                  
                         Distance for B is estimated at 56 +/- 8 pc. Total mass <0.12 Msun if            
                         double, <0.18 Msun if triple.                                           Art2011 
15022+3612   LDS4522     NLTT 39119/39117                                                        Chm2004 
15024-0708   BRT 552     SMH  23. Appears to have been a 1m error in Barton's published RA.              
15024-4723   BRT 843     CPD-46@7153.                                                                    
15025+4745   H 6  53     This star was measured for H VI 53, which could not be identified.              
15027+1809   GIC 124     G136-051/G136-053.                                                              
15032+0740   HJ 1267     HJL 211.                                                                HJL1986 
15035-4035   I  1262     Ruymaekers & Nys (1995) noted discrepancies in the orbit of Erceg &     Ruy1995 
                         Olevic (1986), and calculated elements from the Thiele-Innes            Erc1986b
                         elements originally given.                                                      
15036-2751   HJ 4727     SWR 165. CPM pair                                                       Skf2004 
                         HIP 73674. No new data for the 2MASS PSC companion C at 11.2", it is            
                         likely optical (crowded field, N*=38).                                  Tok2011a
15038+4739   STF1909     44 Boo.                                                                         
                         Spectral types and masses of components assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
                         A is SB1, P=75240d (Abt2006).                                           Tok2014d
                         B is a W UMa-type eclipsing binary.                                             
                         Star B is W UMa-type eclipsing SB2; P = 0.2678 d (Popper 1943;          Ppp1943 
                         Binnendijk 1955, AJ 60, 355). The RV of pair B differs by +30 km/s              
                         from that of star A, much more than the visual motion can effect, and           
                         thus does not represent the true mass-center velocity of B. The                 
                         eclipsing period undergoes intrinsic changes considerably larger than           
                         a lighttime effect in the orbit AB. Attempts to identify the ascending          
                         node are thus unreliable: Time shifts of light minima suggest the               
                         first quadrant (Plaut), the RV difference the third quadrant (Heintz).          
                         The close approach in the visual orbit in recent years has prevented            
                         continued study of the eclipsing system.                                        
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         1975.383: The visual binary has been observed here.                     BLM1978 
                         H 1  15.                                                                MEv2010 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.19 +/- 0.15, 2.02, and 1.83 Msun, respectively.             Mlk2012 
                         The B component is the W UMa type eclipsing binary i Boo.               Zas2009 
15041+1641   BPM 624     [PM2000] 1107378 + [PM2000] 1107320.                                    Gvr2010 
15041+0530   STF1904     H N  37.                                                                MEv2010 
15041-0653   HO  391     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
15041-2517   UC 2911     sig Lib = 20 Lib = Brachium                                                     
15042-5120   B  1258     Spectrum A5/7III/IV                                                             
15043+2905   BU 1445     This may be HJ 564                                                      Bu_1906 
15044-4945   HJ 4726     Spectrum A3/5II/III                                                             
15045+3447   FAR  43     Primary is white dwarf WD 1502+349.                                     Far2006 
15045-1754   S   665     B is BD-17@4247.                                                                
                         Spectrum of A: K2IIICNIb/II, of B: K0III.                                       
15047+6222   LDS1421     NLTT 39299/39301                                                        Chm2004 
15048+3443   CRB 107     BC: Originally 15048+3444 CRB 107, but found to share secondary with            
                         15048+3443 LDS4528. Systems merged, with quadrant flip.                         
15049-1835   LTT 6010    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
15051-4703   HJ 4728     pi Lup. Both components are spectroscopic binaries.                             
15053-1936   RST3907     Spectrum Fm Delta Del.                                                          
15055-0701   TOK 587     AD: D component is the primary of 15041-0653 HO  391.                           
15058+6403   MCT   7     AB: A is G5V, UI Dra (RS CVn type), GJ 577.                             Tok2014d
             LWR  12     Ba,Bb: This pair was initially incorrectly listed as Aa,Ab.                     
15063+5805   LDS2336     The previous WDS coordinate for this pair, 14063+5805, was in error.            
15068-1629   BUP 160     22 Lib.                                                                         
15072-2930   HNK   2     Member of Sco-Cen Association. Primary mass 1.72 +0.08/-0.11 Msun;              
                         secondary mass estimated for B and C at 21 +30/-5 and 22 +38/-6 Mjup            
                         (for age 10 Myr), or 50 +31/-33 and 54 +40/-30 Mjup (for age 20 Myr).   Hnk2015 
15073+2452   ENG  52     45 Boo.                                                                         
                         AB and AC: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
15073+1827   A  2385     1986.384: Separation for this partially resolved pair was calculated            
                         under the assumption of zero or otherwise known magnitude difference.   Tok1985 
                         A "ghost" binary like A  3010.                                          Msn2023a
15074-7036   MLO  63     A likely plate flaw.                                                    Grv2021b
15076+5056   ES  774     Also known as BEM  15, although the astrographic data used to generate          
                         his 1930 measure (as well as the later WFC re-reduction) were in poor           
                         agreement with other measures of this pair.                                     
15078+6307   STF1918     Primary is 2.4d eclipsing SB1; visual pair has estimated period of              
                         35,000y.                                                                Tok2006 
15078-7350   B  2028     Spectrum of B: A/F.                                                             
15079+8545   VVO   1     Also known as LDS1814.                                                          
15079+7612   MET  10     Aa,Ab: Metchev & Hillenbrand (2004) say the pair is probably physical,  Met2004b
                         based on proximity.                                                             
15080-4827   BRT 848     CPD-47@6912.                                                                    
15080-4845   CPO 414     CPD-48@7127. Heintz was unable to find this pair.                       Hei1987a
15082+3958   RUC  23     Multiple system including contact binary TZ Boo.                        Pbl2006 
15083-5957   RSS  24     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
15084-5842   RSS  25     This previously uncataloged double star was a Hipparcos double entry            
                         system. The first measure is determined from the individual positions           
                         listed by Rousseau et al.                                               Rss1996 
15086+0052   J  1027     CD: J  1028.                                                                    
15086-4819   HJ 4732     SWR 167.                                                                        
15087-5140   BRT 849     CPD-51@7573.                                                                    
15088-4517   SEE 219     AB: lam Lup.                                                                    
                         Probably a spectroscopic subsystem, as the RV of the combined light             
                         shows a range of 50 km/s.                                                       
                         1976.471: The observed separation is significantly different from the   B__1962c
                         value derived from van den Bos' (1962) preliminary elements.            BLM1978 
                         AB: Hipparcos parallax 4.20 +/- 0.66  mas. Dynamical parallax 6.3  mas,         
                         masses 8.14 and 5.84 Msun.  lam Lup is a B3V binary belonging to the            
                         Sco-Cen association. A minor revision of the orbit by Docobo & Ling     Doc2007d
                         (2007) proposed here turns it into a definitive one, with both sides            
                         of the ellipse now covered by speckle measures and one full revolution          
                         observed. The Hipparcos parallax corresponds to an uncomfortably large          
                         mass sum. The true parallax should be around 6 mas, matching the                
                         distance to the association.                                            Tok2012b
15090-2144   HJ 2764     Statistically the same parallax within the errors would indicate the            
                         components are physical.                                                        
15091+5904   SKF 365     2MASS J15090696+5904282 and J15090808+5904258 are separated by only 9"          
                         and have similar estimated spectroscopic distances (30 and 39 pc,               
                         respectively) in Riaz et al. (2006), hence it is likely that they form  Ria2006 
                         a physical pair.                                                        Jnn2012 
15092+3304   HJ  566     Also known as STF1913.                                                          
15096-6843   DON 714     T TrA. Uncertainly variable.                                                    
15098-0445   OSO  61     G015-010. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
             LDS 518     HIP 74199. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
15099+3859   STF1916     B is SB1, P=16.191d                                                     Tok2014d
15100+2807   A   690     Aka TDS 768.                                                                    
15103-1616   BUP 161     LDS 519. A : Proper motion -1016 -3571, B: -016-018, D: -024-013                
                         HIP 74235. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AC: LFT 1177/1178.                                                      Bgh1958 
                         AC: NLTT 39456/39457                                                    Chm2004 
                         Proper motion of C -1033 -3526.                                                 
                         AC: SHY 268. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
15103-4954   EGN  15     Aa,Ab: Single epoch, real?                                                      
                         AB: Pair likely bound; colors of B consistent with M2.5-M5.5 dwarf      Egn2007 
15104-2827   HJ 4740     Herschel remarks "Excessively close, if double."                        WHC1890 
15106+3923   NI   34     Rectilinear solution by Hurowitz et al. (2014).                         USN2014a
15107-4344   CPO 415     B is CPD-43@9678, spectrum K0IV-V.                                              
                         SHY 269. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
15108+4651   STF1920     HJL 212.                                                                HJL1986 
                         SHY 664. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
15111+4424   SKF  10     Rectilinear solution by Friedman et al. (2011).                         USN2011a
15112+0608   BGG   2     SDSS J151114.66+060742.9. Bardalez Gagliuffi et al. (2015) resolved             
                         this very low-mass binary, and derived spectral types L5.5 +/- 1.0 and          
                         T5.0 +/- 0.5. Depending on age, this pair has a projected separation            
                         of 2.9 +/- 0.3 au and an estimated orbital period of 17-25y. Mass               
                         estimates range from 0.041-0.072 Msun for the primary, 0.026-0.065 for          
                         the secondary.                                                          BGg2015 
15112-5924   HRG 105     B is CPD-58@5840, spectrum A5V.                                                 
15115-5443   RST2942     Composite-like spectrum: G8/K0III+F/G.                                          
15116-3208   HJ 2765     B is CD-31@11773.                                                               
15116-4517   DUN 178     AC : Identified as optical and linear solution also published.          LRR2022c
15117+1623   BPM 625     [PM2000] 1112160 + [PM2000] 1112208.                                    Gvr2010 
15117-0529   STF1914     B is BD-04@3827.                                                                
15118+6151   STF1927     A and B are both W UMa systems, BV and BW Dra, periods 0.29 and 0.35d.          
                         Spectra F9V, F8V and G3V and G0V.                                               
                         NLTT 39621/39620                                                        Chm2004 
                         AB: HJL 215.                                                            HJL1986 
15118+1013   DJU   3     Pair is -3s, +1' from BD+10 2804.                                       Cou1970c
15119-4844   DUN 177     A: kap 1 Lup                                                                    
                         B: kap 2 Lup. B is CD-48@9705.                                                  
15120+3840   STF1921     B is BD+39@2844.                                                                
15121+3419   ES 2417     Same as POP 209, which was co-discovered by Olevic.                     Ole1970b
15121+1859   COU 189     The variable FL Ser.                                                            
15122-1948   B  2351     iot 1 Lib = 24 Lib. Alternate spectrum of Aa: ApSi.                             
                         Double-lined spectrum, frequently blended. The second spectrum may              
                         belong, not to the visual companion, but to a third star, since the             
                         RV variation - if real - is faster and larger than the visual orbit             
                         with its low inclination could cause.                                           
                         This system has crude Delta m estimates from lunar occultation of               
                         about 1.3 magnitudes in both red and blue.                              Bvr1979b
                         Masses and bolometric magnitudes are derived for the two components             
                         of this system, based on assumed spectral types and available                   
                         parallaxes.                                                             Msn1999a
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Aa,Ab: Orbits of this system have been published by Heintz (1982)       Hei1982c
                         and later by Mason (1994, 1995); further analysis is in                 Msn1994 
                         progress.                                                               Msn1995b
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 6.20 +/- 0.56, 5.14, and 2.82 Msun, respectively.  Mlk2012 
             H 6  44     AB: H VI 44.                                                                    
15123-5206   DUN 176     zet Lup. B is CD-51@8827.                                                       
15125-3555   RSS 367     AB: A is possible astrometric and spectroscopic binary                  Tok2014d
             UC 2956     AC: CPM candidate confirmed physical by photometry (2MASS and V mags).  Tok2013c
15126+4544   MCT   8     GJ 3898. Estimated age 300-1000 Myr; masses 0.30 +/- 0.06 and 0.15 +/-          
                         0.03 Msun; a ~9.9 au.                                                   Jnn2014 
15127+1917   STF1919     LDS 973. STTA134.                                                               
                         NLTT 39601/39603                                                        Chm2004 
                         HJL 213.                                                                HJL1986 
                         H N  62.                                                                MEv2010 
15127-4758   CPO  64     B is CD-47@9781.                                                                
15128+2756   H 5 125     H V 125. STTA135. B is BD+28@2411.                                              
                         HJL 214.                                                                HJL1986 
                         SHY 668. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
15129+3145   HJ  569     Erroneously designated as HJ  469 in BDS.                               Bu_1906 
15134+1959   COU  27     COU  27 and COU 102 are the same.                                               
15135-2519   23 Lib      Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from Vogt et al.  CPS2000c
                         (2000).                                                                 HaI2001 
15135-7753   SWR 169     CPM pair                                                                Skf2004 
15136+3453   HO   60     Misidentified as HO 50 by Baize (1933) (erratum in Inf Circ 121, 1994)  Baz1993b
15138-0121   A   691     Close, rapidly moving, quadrant uncertain.                                      
                         Proper motion of A -1266 -504.                                                  
                         HIP 74537. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
15140+0651   HJ 1270     STF1922.                                                                        
15140-4128   HJ 4748     B is CD-40@9410.                                                                
                         HIP 74549. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
15141+3147   STT 292     B is BD+32@2562.                                                                
15142-2559   SWR 170     CPM pair                                                                Skf2004 
15143-3613   GLP  10     B is CD-35@10137.                                                               
15143-4242   B  1273     CPD-42@6958.                                                                    
15144+3301   OSO  62     G179-022. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
15145-1826   SHJ 195     B is BD-17@4284.                                                                
                         H 5 131.                                                                MEv2010 
15148-0439   A    15     WHC 13.                                                                         
15152+0456   HDS2143     The composite spectrum of this pair is given in the SIMBAD database as          
                         a K0III, and we derive a magnitude difference of approximately 2.5,             
                         which is slightly higher at bluer wavelengths. This suggests that               
                         while the primary is evolved, the secondary is still near the main              
                         sequence, and so a study could be done along the lines of Davidson et   Hor2009b
                         al. (2009) to determine the age and individual masses of the two stars          
                         from the photometry through isochrone fitting. Also, the orbit we               
                         calculate has very high eccentricity, which helps explain why there             
                         were no successful observations of the pair in the late 1990s:                  
                         periastron passage was in 1997, with predicted separation of 6 mas.     Hor2015b
15154-5544   HJ 4747     B is CPD-55@6450.                                                               
15155+3319   STFA 27     49 Boo = del Boo. STTA136. A is a spectroscopic binary.                         
                         Mk III Limb-darkened diameter  2.75  +/- 0.04  mas.                     MkT2001 
                         Mk III Limb-darkened diameter  2.764 +/- 0.030 mas.                     MkT2003 
                         NPOI Limb-darkened diameter    2.74  +/- 0.03  mas,                     NOI1999 
                         R = 10.5 +/- 0.2 \rsun.                                                         
                         NPOI Limb-darkened diameter    2.76  +/- 0.03  mas.                     NOI2001b
                         B is BD+33@2562.                                                                
                         HJL 216.                                                                HJL1986 
                         SHY 270. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         H 6  16.                                                                MEv2010 
                         Toyota et al. (2009) monitored the RV of the A component every 1-2              
                         months between 2003 Mar - 2007 Nov, using a high-dispersion echelle             
                         (precision ~10 m/s). Standard deviation of radial velocities <40 m/s            
                         and velocities show no periodic variation. This result rejects the              
                         association of a planet of mass > 1.8 Mjup                              Toy2009 
15156+5527   WZ   13     STI 2320.                                                                       
15157+3642   ALI 601     BRT2594.                                                                Brt1942 
15157-2736   BU  350     Ma,Mb = 1.98  +/- 0.11 , 1.39  +/- 0.01  \msun.                         GmJ2022 
15158+5056   STTA137     B is BD+51@1992.                                                                
15158-5701   HRG 108     Aka HDS2145.                                                                    
15160+0048   AMM   6     V379 Ser, a BY Dra type variable star.                                          
15160-0454   STF3091     One component is probably variable; position angles have been                   
                         reversed repeatedly.                                                            
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.96 +/- 2.41, 2.43, and 1.10 Msun, respectively.  Mlk2012 
                         The former AB,C and AB,D are now 15177-0430HL 9003.                     Dam2014 
15169-6057   HDO 245     del Cir. A variable and spectroscopic binary.                                   
                         Primary is eclipsing binary of Algol-type, period 3.90247d.             Zas2014 
                         This "field" object may belong to the "Pis 20" group of Mel'nik &               
                         Efremov (1995 SvAL 21, 10). The secondary classification is an                  
                         estimate from Stickland et al. (1993).                                  Stc1993 
                         The Hipparcos Catalogue contains an eclipsing light curve.              HIP1997a
                         Classification of the B component of the optical pair is from Lindroos  Lnd1985 
                         (1985). Lindroos also finds a distance of 750 pc to this system.        Msn1998a
             SNA  39     Aab,c: The primary is del Cir, an ellipsoidal variable star. Penny et           
                         al. (2001) performed a tomographic decomposition and found del Cir to   Pny2001 
                         be a triple system, with an eclipsing inner Aa,Ab pair (3.9d, a sin i           
                         = 11.44 Rsun) and a RV-stable Ac component. Mayer et al. (2014)         MyP2014 
                         established the hierarchical nature of the system, obtaining a 1644d            
                         period for the outer system. PIONIER clearly resolved the outer system          
                         as a 3.78mas pair. We did not detect the dV=7.8 B companion of Mason    Msn1998a
                         et al. (1998), but it may be just below our detection limit.            Sna2014 
15171-5948   I  9003     Previously known as I  1074 1/2.                                                
15173+7113   H 5  86     H V 86.                                                                         
15175-5848   SML   1     bet Cir. Smith et al. (2015) find a distant common proper motion                
                         companion in the VISTA Variables in the Via Lactea survey. Spectral             
                         type of the companion (= VVV J151721.49-585131.5) is estimated at               
                         L1.0 +/- 0.5, mass at 0.056 +/- 0.007 Msun.                             SmL2015 
15177-0430   HL 9003     Formerly 15160-0454STF3091AB,C and AB,D.                                Dam2014 
15179-2323   I  1268     CD-22@10926.                                                                    
15179-3029   HNK   3     Member of Sco-Cen Association. Primary mass 1.42 +0.04/-0.06 Msun;              
                         secondary mass estimated at 28 +37/-10 Mjup (for age 10 Myr), or                
                         65 +36/-25 Mjup (for age 20 Myr).                                       Hnk2015 
15179-7435   I   330     Composite-like spectrum: G8/K0(III)+A.                                          
15182+3139   U CrB       1983.3123: Lippincott's (1983) recent improved parallax of 0".0041      Lip1983b
                         practically rules out direct observation of the companion that is               
                         perturbing the orbital motion of this SB.                               Bag1984a
15183+2650   STF1932     There is evidence of light-variability in the system.                           
                         A subsystem of 30 to 50 yr period, formerly suspected from visual               
                         data, is not supported by the more recent observations.                         
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Spectral types and masses of components assigned by ten Brummelaar et   TtB2000 
                         al., based on adaptive optics observations.                                     
                         AB: Check astrometric orbit of Ba,Bb. Interferometric observations do           
                         not support 30-y or 50-y astrometric subsystem.                         Tok2014d
15183+1851   TOK 167     HIP 74888. The companion B is barely seen in the 30-s V-band image, it          
                         is physical. No references in SIMBAD.                                   Tok2011a
15184+2034   HR 5692     Combined solution of this red giant / white dwarf system, based on              
                         spectroscopy plus intermediate astrometric data from Hipparcos.                 
                         Stefanik et al. (2011) derive a mass of 1.84 +/- 0.04 Msun for the red  Trr2011 
                         giant and 0.59 +/- 0.12 Msun for the WD (compared with 0.79 +/- 0.09            
                         Msun derived from IUE spectrum analysis). Effective temperatures are            
                         4960 +/- 100 and 30400 +/- 780 K.                                               
15185-4753   HJ 4753     mu Lup                                                                          
15187+1026   STF1931     C is slightly variable.                                                         
                         AB: HJL 218.                                                            HJL1986 
                         HIP 74930. B = HIP 74931.                                               Tok2011a
15187-0531   A    16AB,C Also known as PNC   1.                                                  Pnc2018 
15188-6030   I   370     This "field" object may belong to the "Pis 20" group of Mel'nik &               
             45 Cir      Efremov (1995 SvAL 21, 10). Classifications of the B and C components           
                         are from Lindroos (1985); the C component classification is             Lnd1985 
                         photometric.  Lindroos finds a distance of 1.0 kpc.                     Msn1998a
15189-6841   WFC 164     = gam TrA.                                                                      
15190+2541   LDS6304     A is SB, no orbit.                                                      Tok2014d
15190+1537   BPMA 48     [PM2000] 1116755 + [PM2000] 1116759.                                    Gvr2010 
15192+1424   BPM 626     [PM2000] 1116852 + [PM2000] 1116817.                                    Gvr2010 
15193+0146   STF1930     5 Ser. AB: Mt. Wilson spectral types F5s, M0.                           Bu_1906 
                         CHARA Array Limb-darkened diameter  2.371 +/- 0.044 mas,                CIA2008c
                         R =  0.708 +/- 0.085 \rsun.                                                     
                         CHARA Array Limb-darkened diameter of A :                               CIA2013c
                         R =  2.1427 +/- 0.0670 \rsun, L =   4.2283 +/-0.0624 \lsun,                     
                         Teff = 5661 +/-  87 K, M = 1.217 \msun, Age = 5.3 Gyr.                          
                         CHARA Array Limb-darkened diameter 0.459 +/- 0.017 mas,                 CIA2014b
                         R =  0.8668 +/- 0.0324 \rsun, T = 5518 +/- 102 K,                               
                         L =   0.6256 +/- 0.0077 \lsun, M = 0.91 \msun.                                  
                         AD: See BDS and ADS for rectangular measures.                           A__1932a
                         AB: H 3 106.                                                            MEv2010 
15194+4550   BU 1446     C component is galaxy NGC 5918.                                                 
15194+4536   GIC 125     G179-026/G201-046.                                                              
15198-6630   KRV  52     Classical Cepheid R TrA.                                                        
15199-7520   TOK 591     = NY Aps.                                                                       
15200+3614   MUG  15     Primary is HAT-P-4. Spectral type of comoving secondary estimated as            
                         G2, confirmed by follow-up spectroscopy. Mass of secondary 1.08 Msun.   Mug2014 
15200-4423   BUG  12     Burgasser et al. used two epochs of 2MASS data, as well as data from    Bug2007 
                         SERC, ESO, AAO plates to derive proper motion, etc. Component J,H,Ks            
                         magnitudes are calculated from composite 2MASS photometry, plus images          
                         obtained at the IRTF. Spectral types are estimated at L1.4 and L4.5,            
                         distance  at 19 +/- 2 pc, and total mass 0.14-0.14 Msun.                        
15201+2937   ENG  53     1 CrB = omi CrB                                                                 
15202+7708   LDS1819     NLTT 40118/40114                                                        Chm2004 
15204+0015   GIC 126     LDS5836. G015-017/G015-018.                                                     
                         HIP 75069. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
15206+5520   HJ 2779     STT 542.                                                                        
15206+1523   HU 1160     A premature orbit has been computed.                                            
15208+3129   LEP  74     SHY 271. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         B is AX CrB (BY-Dra type). Estimated period of AB is 12Myr. Too wide            
                         to be a binary?                                                         Tok2014d
15210+1721   BPM 627     AB: [PM2000] 1118031 + [PM2000] 1117980.                                Gvr2010 
             BPM 628     AC: [PM2000] 1118031 + [PM2000] 1117956.                                Gvr2010 
15210+0043   BU   32     6 Ser. Possibly variable.                                               Fat1941 
15210-1533   BU 1447     omi Lib = 29 Lib                                                                
15211+2534   GRV 903     SHY 272. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
15212+2745   LDS4544     SLW1084.                                                                        
15214+5312   GRV1209     SLW1085.                                                                        
15218+1255   BPM 629     [PM2000] 1118561 + [PM2000] 1118459.                                    Gvr2010 
15218-0201   STF3092     HJL 219.                                                                HJL1986 
15218-1510   BU 1448     Based on MacEvoy's (2010) conclusion that BU 1448 and H 5 132 are the   MEv2010 
                         same pair, the 1783 measure of 15220-1505 H 5 132 was merged into this          
                         much more well-observed pair.                                                   
15218-3616   SEE 229     phi 1 Lup                                                                       
15219+2807   GIC 127     AB = G167-040/G167-039. The A component is Ross 1053.                           
15220-1505   H 5 132     H V 132. This is either BDS 7219 or 7223.                                       
15222+4508   ES 2649     B is BD+45@2281.                                                                
                         HJL 220.                                                                HJL1986 
15226-4755   SLR  20     Motion retrograde.                                                              
15226-5910   COO 186     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2014).                         USN2014a
15227+1616   GWP2518     OU Ser.                                                                         
15227-4441   COP   2     eps Lup. A is a spectroscopic binary.                                           
15228+1016   BRT3378     Unnumbered pair, following BRT1282 in Barton's list.                    Brt1935a
15230-2326   DON 731     OL  188.                                                                        
15232+3017   STF1937     eta CrB = 2 CrB.                                                                
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Masses and bolometric magnitudes are derived for the two components of          
                         this system by Mason et al. (1999), based on assumed spectral types     Msn1999a
                         Spectral types and masses of components assigned by ten Brummelaar et   TtB2000 
                         al., based on adaptive optics observations.                                     
                         and available parallaxes.                                                       
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         Combined spectroscopic/astrometric solution of SB2. Calculated masses           
                         1.243 +/- 0.054 and 1.100 +/- 0.039 Msun, distance 18.50 +/- 0.22 pc.   Mut2010b
                         AB: H 1  16.                                                            MEv2010 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.11 +/- 0.09, 2.24, and 2.14 Msun, respectively.  Mlk2012 
                         AB: SB2, P=41.628y                                                      Tok2014d
             KIR   4     AE. Data from 2MASS. Kirkpatrick et al. (2001) derive spectral types    Kir2001a
                         G1V+G3V and L8V, determine is a physical pair, separation ~3600 au.             
                         Find that WDS C and D components of system are not physical.                    
             STF1937     AB,C: Rectilinear solution by Hurowitz et al. (2014).                   USN2014a
15232-0246   BAL 237     RST 4539.                                                                       
15232-2601   HLD  24     SWR 173. CPM pair                                                       Skf2004 
15232-4445   RIZ  14     phi 2 Lup.                                                                      
15233+3619   A  1367     AB,C: Wide companion appears to be plate flaw or reduction error in             
                         Astrographic Catalog.                                                           
15234-5919   HJ 4757     gam Cir. A premature orbit has been computed.                                   
15236+4021   LDS4547     Typographical error of 3deg in WDS designation. BVD 239.                        
15239+5610   VVO  14     A probable wide companion to this star at approximately 68" separation          
                         is noted in the WDS.                                                    Jnn2012 
15241-3302   HJ 4765     B is probably a Mira-type variable, GN Lup.                                     
15241-7513   HJ 4751     SWR 172.                                                                        
15242-1019   eps Lib     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Jones (1931).                                                           JoR1931 
15243+6033   GC 20737    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
                         Spectroscopic solution to these astrometric pairs given by Griffin      Grf2013a
                         (2013). Periods match "tolerably well," other common elements less so.          
15245+3723   CHR 181     Aa,Ab: mu 1 Boo = 51 Boo A = Alkalurops. SB, P=298.75d.                         
                         More speckle observations are needed to confirm preliminary orbit.              
                         Aa,Ab: Calculated mass sum is 3.24 +/- 0.23 Msun. Absorption lines too          
                         broad and blended for RV measurements.                                  Mut2010b
                         Aa,Ab: Orbital elements provided in Guerrero et al. (2021) match        Gur2021 
                         measures and previous orbits of STF1938Ba,Bb. The orbit is therefore            
                         attributed to STF1938Ba,Bb in ORB6.                                             
             STF1938     Ba,Bb: mu 2 Boo = 51 Boo B.                                                     
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
             STFA 28     AB: HJL 221.                                                            HJL1986 
                         AB: H 6  17.  STF1938Ba,Bb: H 1  17.                                    MEv2010 
                         AB: SHY 275. Bayesian analysis by Shaya & Olling (2011) indicates very          
                         high (near 100%) probability pair is physical.                          Shy2011 
                         AB: Kiyaeva et al. (2014) find probably significant differences in the          
                         elemental abundances of the Aa,Ab and Ba,Bb subsystems, and suggest             
                         this quadruple is instead a close passage of two separate binaries.     Kiy2014 
15248-3943   RST1839     ups Lup                                                                         
15249+5858   BUP 162     iot Dra = 12 Dra = Edasich. B is BD+59@1655.                                    
15249+1359   HJ  252     AB = LDS 975.                                                                   
                         AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
15250-1837   HJ 1271     BDS 7250, HJ 4768 same star.                                                    
15252-4713   RST 766     CPD-46@7410.                                                                    
15253-3844   DUN 183     k Lup.                                                                          
15255+4557   GC 20750    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
15263-4252   DUN 184     B is CD-42@10392.                                                               
                         The AC component is an error as per communication with the author and   Ary2011 
                         has been removed.                                                               
                         Identified as optical and linear solution also published.               LRR2022c
15265+4351   BU 1449     B is BD+44@2468.                                                                
15266-1706   HU  309     Spectrum: F3/5III/IV.                                                           
15266-3713   HRG 118     Aka TDS9516.                                                                    
15267-5254   B  2354     Not found by Heintz at IDS position.                                    Hei1987a
15269+4610   KU   50     The pair L 13 formerly listed at 15280+4612 is identical                Hei1980a
15270+4128   SKF1924     BC: Originally 15273+4130 SKF1924, but primary is B component of                
                         15270+4128 LDS4554.                                                             
15273+1738   A  2074     Only elements P and T have been amended by Starikova (1980) from the    Sta1980b
                         orbit of Baize (1976).                                                  Baz1976 
15273+0942   A  1120     Only elements P, T, and a have been amended by Starikova (1978) from    Sta1978c
                         the orbit of Muller (1955).                                             Mlr1955a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.69 +/- 1.01, 2.56, and 1.05 Msun, respectively.             Mlk2012 
15277+4253   KU  108     LDS5837.                                                                        
                         NLTT 40312/40309                                                        Chm2004 
                         HJL 223.                                                                HJL1986 
                         AB: A is SB1, P=16.55y.  B is SB1, P=17.430d                            Tok2014d
15278+2906   JEF   1     bet CrB = 3 CrB = Nusakan. A spectroscopic binary resolved visually,            
                         and avariable of Alpha CVn-type.                                                
                         1973.22, 1973.45: See discussion and orbital elements by Labeyrie et            
                         al. (1974).                                                             Lab1974 
                         1975.383, 1975.455: The observations presented here are of poor                 
                         quality but the results are consistent with those of Labeyrie et al.            
                         and McAlister.                                                          BLM1978 
                         1980.4682: See preliminary elements and discussion in Balega et al.             
                         (1984).                                                                 Bag1984b
                         1983.3206: A peculiar SB with a 10.5-year period.                       Bag1984a
                         1984.1867 and other observations through 1985.2440: The speckle                 
                         interferometric observations are in good agreement with both Balega et  Bag1984b
                         al. (1984) and Tokovinin (1984) orbits; radial velocity measurements    Tok1984 
                         are strongly needed to improve the spectroscopic orbit of this system.  Bnu1986 
                         Measure of 1988.256 made by MAPPIT.                                     Naj1989 
                         The speckle observations and derived masses leave no room for a                 
                         conjectured third component, cf. Kamper et al. (1990).                  Kpr1990 
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Kamper et al. (1990).                                                           
                         Based on combined observations from VLT/Naco and CHARA/FLOUR, Bruntt            
                         et al. (2010) derive the following parameters for the components of     Bnt2010 
                         bet CrB: radii 2.63 +/- 0.09 and 1.56 +/- 0.07 Rsun, spectral types A5          
                         and F2, luminosities 25.2 +/- 2.9 and 4.5 +/- 0.05 Lsun, Teff 7980 +/-          
                         180 and 6750 +/- 230K, masses 2.09 +/- 0.15 and 1.40 +/- 0.10 Msun.             
                         The age of the systems is estimated at 0.53 +/- 0.10 Gyr.                       
                         Combined spectroscopic/astrometric solution of SB1. Radial velocities           
                         span nearly a century. Calculated masses 1.71 +/- 0.18 and 1.330 +/-            
                         0.074 Msun.                                                             Mut2010b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.08 +/- 0.24, 4.09, and 3.17 Msun, respectively.             Mlk2012 
15280+1442   STF1945     BC: HJL 222.                                                            HJL1986 
15282+0251   A  2175     Couteau assumption of a double occultation in 1936, giving a period     Cou1957b
                         of 34yr, is probably no longer tenable.                                 Fin1970b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 6.02 +/- 6.17, 3.77, and 1.82 Msun, respectively.             Mlk2012 
15282-0921   SHJ 202     LDS 531. BDS 7220, H V 27 same star. The primary is a spectroscopic             
                         binary of very high eccentricity, P = 889.6d.                                   
                         AB: SHY  76. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         C is BD-08@3984, and is optical. A 15.35mag. star at 20' shares common          
                         proper motion.                                                                  
                         AB: H 5  27.                                                            MEv2010 
15282-3722   RST3920     The primary is the variable GO Lupi.                                            
15282-3411   SEE 235     Spectrum: G8/K0III/IV. Aka B  2785.                                             
15283-1643   OCC 953     = zet 1 Lib = 32 Lib.                                                           
15289+5727   GIC 128     LDS2722. D component = G224-069. Giclas says B component is not                 
                         physical but D is CPM companion.                                                
             BU  945     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AD: NLTT 40385/40401                                                    Chm2004 
15289-3747   SWR 174     CPM pair                                                                Skf2004 
15290-2852   HJ 4774     HIP 75790.                                                              Tok2011a
15292+8027   STF1972     LDS1823. A is a spectroscopic binary. Composite spectrum:                       
                         G0IV-V+G8IV-V. B is BD+80@481, and is also a spectroscopic binary.              
                         AB: NLTT 40576/40590                                                    Chm2004 
                         AB: HJL 224.                                                            HJL1986 
                         AB: H 4  90.                                                            MEv2010 
15292-3249   JSP 659     BRT1694.                                                                Brt1936a
15294+6712   STF1958     B is BD+67@899.                                                                 
15294+1722   BPM 630     [PM2000] 1123830 + [PM2000] 1123850.                                    Gvr2010 
15294-2851   DAW 143     Includes IR Lib, a W UMa type eclipsing binary, P = 0.27437d.           Zas2012 
15295+0609   OSO  63     G015-023. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
15296-1726   UC 3014     = 33 Lib = GZ Lib.                                                              
15297+4252   JNN 278     LHS 3075. Estimated age 1000-10000 Myr; masses 0.24 +/- 0.07 and 0.14           
                         +/- 0.04 Msun; a ~11.2 au.                                              Jnn2014 
15299+0552   GAU  14     Observed for HJ 2782, but evidently a different pair.                           
15299-6729   RSS  26     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
15301-0750   G152-031    Astrometric orbit by Harrington & Dahn (1988), but the true relative    Hrr1988 
                         semimajor axis of 0".071 is calculated. Aka GIC 129.                            
15303+2739   STF1951     HO  394.                                                                        
15304+3935   LAW  23     AB: SLW1101.                                                                    
15304-3352   SWR 175     CPM pair                                                                Skf2004 
15307+3810   HU 1163     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 7.08 +/- 5.05, 3.33, and 0.95 Msun, respectively.             Mlk2012 
15307+0824   OSO  64     G015-024. Not a common proper motion pair                               Oso2004 
15307-5246   RSS  27     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
15308-6536   KRV  53     Classical Cepheid LR TrA.                                                       
15309+5609   WNO  23     aka USN   1.                                                                    
15309+1621   BPM 631     [PM2000] 1124936 + [PM2000] 1124883.                                    Gvr2010 
15312-1852   HO  393     Burnham connects A with BD+18@4083.                                             
15313-1259   DOO  59     AE: Fox in 1926 and van den Bos  in 1959 reverse the                    Fox1946 
                         quadrant.                                                               B__1961a
             BU   34     CD: Also known as AOT  62.                                                      
15314+3637   HR 5769     Orbit determined by fitting revised Hipparcos intermediate astrometric          
                         data. Derived component masses 0.91 +/- 0.11 and 0.69 +/- 0.08 Msun.    Ren2010 
15314+1900   JNN 104     LP 442-66.                                                                      
15315-7323   HJ 4764     kap 1 Aps. A is variable.                                                       
15317+3903   KZA  96     15' error in WDS designation                                                    
15317+0053   GC 20867    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
                         Spectroscopic solution to these astrometric pairs given by Griffin      Grf2013a
                         (2013). Periods match "tolerably well," other common elements less so.          
15317-2010   S   672     A is a spectroscopic binary.                                                    
15318+4704   GIC 130     LDS5840. G201-051/G201-050. A component is the variable star FN Boo.            
                         NLTT 40502/40494                                                        Chm2004 
15318+4054   A  1634     nu 2 Boo = 53 Boo. An example of adequate resolution provided only by           
                         speckle.                                                                        
                         1921.400: This observation is highly uncertain.                         Mrr1922 
                         Omega for Baize (1985) solution corrected from 47.5 to 227.5            Baz1985b
                         degrees.                                                                Ruy1995 
                         1985.2002, 1985.2494: These two measurements are not precise because            
                         this interferometric binary is only marginally resolved with a 2-m              
                         telescope.  Estimates of rho and theta are deduced from the elongation          
                         of the central peak in the autocorrelation.                             Bnu1986 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 4.82 +/- 1.34, 6.07, and 1.82 Msun, respectively.  Mlk2012 
15318-0204   SHY 677     HIP  76046 + HIP  75923.                                                        
15319+0940   SHY 679     AD: HIP  76051 + HIP  76700.                                                    
15320+1322   LDS4557     NLTT 40483/40484                                                        Chm2004 
15320-1123   OSO  65     G152-035. Not a common proper motion pair                               Oso2004 
15325+0835   STTA140     B is BD+09@3061.                                                                
15325-5252   HJ 4778     B is CPD-52@8474.                                                               
                         V392 Nor, Algol-type eclipsing binary, P = 1.298207 d.                  Zas2011 
15325-7731   HJ 4760     Spectral types: B7(III)+B/A. B is CPD-77@1124.                                  
15326+0832   GIC 131     G137-018/G137-017.                                                              
15328+1945   HU  577     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.25 +/- 0.49, 2.40, and 1.20 Msun, respectively.             Mlk2012 
15329+3122   COU 610     the CrB = 4 CrB. Variable.                                                      
15330-0111   SHY 678     HIP  76133 + HIP  77728. Primary is 11 Ser.                                     
15331-5812   DUN 186     B is CPD-57@7083.                                                               
15332-2429   LAL 123     AB: S 673.                                                                      
             CHR 232     Aa,Ab: Gomez et al. (2016) derive dynamical parallax and  component.            
                         masses: 10.01 +/- 0.15 mas, 1.741 +/- 0.012 Msun, 1.200 +/- 0.008 Msun  Doc2016i
15336-4732   DUN 187     CPD. B is CPD-47@7206.                                                          
15337+1223   BPM 632     [PM2000] 1127072 + [PM2000] 1126956.                                    Gvr2010 
15339+6354   STT 299     A is the Algol-type system TW Dra.                                              
15339-1700   HDS2185     Hipparcos parallax 25.85 +/- 0.94 mas. Dynamical parallax 29.9 mas,             
                         masses 0.90 and 0.72 Msun. HDS 2185 has its first 60 yr orbit                   
                         determined here, with nearly half of it covered. The orbit is still             
                         preliminary. The speckle measure on 2001.56 was given a lower weight.   Tok2012b
15340+2057   LDS 976     NLTT 40568/40569                                                        Chm2004 
15340-2907   SWR 177     CPM pair                                                                Skf2004 
15342-1004   KPP3048     37 Lib.                                                                         
15343+1616   LIM   7     Liu et al. (2006) derive a mass ratio 0.80 +/- 0.05 and luminosity              
                         ratio 0.3 +/- 0.1 dex. Estimated distance is 36 pc, orbital period              
                         22-33y. Total mass (for ages 0.5, 1.0, and 5.0 Gyr) estimated at 60,            
                         85, and 145 Mjup, respectively. Spectral types are estimated as                 
                         T1.5 +/- 0.5 and T5.5 +/- 0.5.                                          LiM2006 
15346+4454   HJ 2788     B is BD+45@2304.                                                                
15347+2655   COU 798     BG CrB.                                                                         
                         Docobo et al. (2010) derive a dynamic parallax of 6.51 +/- 0.40  mas    Doc2010h
                         and a total mass of 2.63 +/- 0.50 Msun.                                         
15347+2643   alp CrB     = Alphecca. Hipparcos astrometric solution adopted some elements from   HIP1997d
                         the orbit of Tomkin & Popper (1986).                                    Tom1986 
15348+2500   STT 297     Optical pair; apparent movement of companion 15"/century along                  
                         position angle 333deg. Minimum separation of 0.8" in 1933.              Cou1958a
15348+1032   STF1954     del Ser = 13 Ser. A premature orbit has been computed.                  Fat1941 
                         The primary is a Delta Scuti-type variable.                                     
                         Measure of 1927.40 made by triangulation of multiple measures.          Sha1929 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         A very faint pair CD (mag. about 14 estimated by Burnham, 4") is 65"            
                         distant and may be physical.                                                    
                         1995.556: Absolute quadrant determined by triple-correlation technique  Pru2002b
                         AB: H 1  42.                                                            MEv2010 
15348-2952   BUG   3     Liu et al (2008) estimate spectral types T5.0 +/- 0.5 and T5.5 +/- 0.5  LiM2008 
                         and effective temperatures 1028 +/- 17 and 978 +/- 17K. Orbital                 
                         elements, determined using a Markov Monte Carlo technique, yield                
                         masses 0.0287 +/- 0.0016 and 0.0269 +/- 0.0016 Msun. Age of the system          
                         is estimated at 0.78 +/- 0.09 Gyr.                                              
                         Assuming a parallactic distance of 13.59 +/- 0.22 pc                            
                         (Tinney et al. 2003), Konopacky et al. (2010) derive a system mass of   Bug2003b
                         0.060 +/- 0.004 Msun.                                                   Kon2010 
15351+0045   HDS2189     OZ Ser.                                                                         
15351-4110   HJ 4786     gam Lup. Variable RV.                                                           
                         Heintz (1956) reports that this orbit is not well known.                Hei1956b
                         1976.471: Heintz (1956) reports that this orbit is not                  Hei1956b
                         well known.                                                             BLM1978 
                         Magnitudes changed to Hipparcos V magnitude on recommendation of Ross   Fab2000a
                         Gould.                                                                  Glr2022 
15354+1743   LDS 977     Ross 513.                                                                       
                         NLTT 40631/40630                                                        Chm2004 
15355-1447   WRH  20     Aa,Ab: Uncertain duplicity.                                                     
                         Aa,Ab Abnormal occultation reported in U.O.C. #95.                      WRH1941b
             GOL   1     AB: gam Lib = 38 Lib = Zubenelhakrabi                                           
15356-7454   HJ 4770     SWR 176.                                                                        
15357-8012   HJ 4759     B is CPD-79@845.                                                                
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
15359+5111   GIC 132     G201-057/G201-056.                                                              
15359-4457   HJ 4788     A is a spectroscopic binary.                                                    
15360+5438   CHR  47     Hipparcos Acceleration Double Solution.                                         
                         This system, first announced by McAlister and recalled in a later       McA1984b
                         McAlister paper after repeated attempts at confirmation, has been       McA1993 
                         restored. While perhaps still spurious, the subsequent confirmation or          
                         suspected duplicity (by another technique) makes the discovery                  
                         measurement somewhat more probable.                                             
15360+3948   STT 298     AB: LDS 978.                                                                    
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.80 +/- 0.97, 1.76, and 0.79 Msun, respectively.  Mlk2012 
                         AB,C: HJL 225.                                                          HJL1986 
                         AB,C: SHY  77. Bayesian analysis by Shaya & Olling (2011) indicates     Shy2011 
                         very high (near 100%) probability pair is physical.                             
                         AB,D: D component is galaxy and possible quasar NGC 5966.                       
                         AB,E: Additional notes may be found in Simonov (1937).                  Smw1937 
15360-4930   RST 780     A is the Mira-type variable R Nor.                                              
15360-5051   B  2359     CPD-50@8274.                                                                    
15362-0623   TOK 301     HIP 76400 is identified by the GCS as an SB2 with a mass ratio q=0.93,          
                         but there is no spectroscopic orbit available. We resolved the 0".19            
                         pair with dI=3.9, indicating a mass ratio of ~0.5 and an orbital                
                         period of ~30yr. Very likely the resolved binary does not match the             
                         spectroscopic double-lined system. Considering the CPM component B at           
                         80" (Tokovinin & Lepine 2012), this system could be a quadruple with a  Tok2012c
                         3-tier "3+1" hierarchy.                                                 Tok2015c
                         Aa1,Aa2 has a period of 368d.                                           Tok2022e
15365+1607   UC 3033     18 Ser = Tau05 Ser.                                                             
15366+0915   STF1960     HJL 226.                                                                HJL1986 
15367-4208   HDS2196     AB, etc: HIP 76435 is a G5V star from the FG-67 sample. Its companion           
                         C (AC = FAL 78) at 13".5 is physical, while the Hipparcos companion B           
                         at 4".3 is not seen in the 2MASS images and has not been confirmed              
                         otherwise. We targeted C and resolved it into a close binary.                   
                         Estimated masses of Ca and Cb are 0.70 and 0.66 Msun, period ~4yr.      Tok2015c
             HRG 119     AC: Aka FAL  78.                                                                
             SHY 277     AD: HIP  76435 + HIP  76650.                                                    
15367-6619   DUN 188     eps TrA. B is CPD-65@3101.                                                      
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
15368+3735   LDS4572     BK CrB.                                                                         
                         NLTT 40716/40719                                                        Chm2004 
15370+6426   HU 1168     Only elements P and T have been amended by Starikova (1980) from the    Sta1980a
                         orbit of Heintz (1976).                                                 Hei1976 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.17 +/- 0.58, 1.81, and 0.95 Msun, respectively.             Mlk2012 
15370-0041   HJ 1276     H 2  23.                                                                MEv2010 
15370-2808   I  1271     ups Lib = 39 Lib                                                                
15371+3748   JNN 105     = BL CrB. The star displays photometric variability at a 1.2 day period         
                         (Norton et al. 2007 A&A 467, 785).                                      Jnn2012 
15371+2646   GII  40     AC: GII  84AC.                                                                  
15372-2339   SEE 241     B 296. Misidentified by See.                                            See1898b
15374+1731   BPM 633     [PM2000] 1129829 + [PM2000] 1129734.                                    Gvr2010 
15375+1258   BPM 634     [PM2000] 1129908 + [PM2000] 1129894.                                    Gvr2010 
15378+0017   LDS4575     SLW1119.                                                                        
15379+3006   STF1963     Mt. Wilson spectral types F5s and G1.                                   Fat1941 
                         AB: H 1  18.                                                            MEv2010 
15381+2929   RAO 506     RT CrB.                                                                         
15381-4234   HDO 250     ome Lup. Variable velocity.                                                     
15382+3615   HU 1167AB   Masses and effective temperatures are determined for these four                 
             STF1964CD   components of ADS 9731, based on dynamical parallax (assuming both              
                         pairs are at the same distance) and derived blackbody curves.           Dru1995 
                         AC: HJL 227.                                                            HJL1986 
                         AC: H 4  61.                                                            MEv2010 
15382-4133   HRG 120     Aka SKF1017.                                                                    
15383-1734   TOK 168     HIP 76572.                                                              Tok2011a
15383-2901   SWR 179     CPM pair                                                                Skf2004 
15385-7055   MLO  67     SWR 178.                                                                        
15386+3826   ALI 862     A likely plate flaw.                                                    Grv2021b
15387-0847   STF1962     178 Lib.  A is a spectroscopic binary. B is BD-08@4031.                         
                         HIP 76603. B = HIP 76602.                                               Tok2011a
                         H N  33.                                                                MEv2010 
                         Toyota et al. (2009) monitored the RV of both the A and B components            
                         every 1-2 months between 2003 Mar - 2007 Nov, using a high-dispersion           
                         echelle (precision ~10 m/s). The A component is a known SB1 (Tokovinin          
                         & Gornya 2001; P=844.74d). Toyota et al. derive orbital elements in     Tok2001 
                         reasonable agreement with the earlier solution. The standard deviation          
                         of radial velocities for the B component <40 m/s and velocities show            
                         no periodic variation. This result rejects the association of a planet          
                         of mass > 1.8 Mjup with this star.                                      Toy2009 
15287-2947   RIZ  16     = tau Lib = 40 Lib.                                                             
15387-7311   B  2787     Also known as R   261.                                                          
15389+5728   STTA141     AB: B is BD+57@1599.                                                            
15390-5742   NLS   2     Aa,Ab: The bet Pic moving group member V343 Nor was resolved by the             
                         Gemini Planet Imager into a close pair. Additional archival NaCo data           
                         and radial velocity measures allowed Nielsen et al. (2016) to derive a          
                         combined astrometric/spectoscopic orbit. Component masses are                   
                         1.10 +/- 0.10 and 0.290 +/- 0.018 Msun.                                 Nls2016 
15390+2545   COU 612     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.82 +/- 1.14, 2.51, and 0.95 Msun, respectively.             Mlk2012 
15391+1452   BPM 635     [PM2000] 1131197 + [PM2000] 1131292.                                    Gvr2010 
15394+3638   STF1965     A: zet 2 CrB = 7 CrB A. A is a spectroscopic triple, with periods of            
                         1.72 and 251d (Gordon & Mullis 1997 PASP 109, 221)                              
                         H 2   8.                                                                MEv2010 
                         B: zet 1 CrB = 7 CrB B. Shares common proper motion with A.                     
15396+7959   STF1989     pi UMi.                                                                 Bu_1894 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 5.87 +/- 3.45, 3.45, and 1.35 Msun, respectively.             Mlk2012 
15398-3001   BRT3023     Not found by Heintz at IDS position.                                    Hei1990b
                         A likely plate flaw.                                                    Grv2021b
15399-1946   BU  122     HDO 140                                                                         
15400+4330   VBS  25     NLTT 40867/40868. Aka LDS5842.                                          Chm2004 
15402+1203   STT 300     A is a spectroscopic binary, spectrum G7.5IIIaCN-Fe0.5.                         
15402-5655   GC 21035    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
15403+4351   GC 21088    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
15404-5056   BRT 861     A likely plate flaw.                                                    Grv2021b
15404-7327   HDO 249     kap 2 Aps                                                                       
15408+3853   LDS4582     NLTT 40899/40897                                                        Chm2004 
15408-3252   SHY 278     HIP  76793 + HIP  75753.                                                        
15409+5253   FAR  17     SKF  47. Secondary is white dwarf PG 1539+530.                          Far2005b
15410-1449   HWE  37     See's 1898 measure is perhaps of ADS 9773, with a 10deg error in his            
                         angle.                                                                  B__1951a
                         P of AB estimated at 32 kyr. B is a spectroscopic binary with P ~ 209d. Tok2022e
15413+0350   BAL2870     Aka HDS2214.                                                            Skf2013 
                         Rectilinear solution by Hurowitz et al. (2014).                         USN2014a
15414+1350   WNO  10     LDS5843.                                                                        
                         NLTT 40901/40902                                                        Chm2004 
15414-2910   RST1855     CPD-28@5170.                                                                    
15415+3225   LDS4584     NLTT 40932/40930                                                        Chm2004 
15416+1940   HU  580     iot Ser = 21 Ser.                                                               
                         The centers of the broad, blended spectral lines of the visual pair             
                         show a fast variation (range about 65 km/s), and a weak redshifted              
                         component has been seen occasionally. The system is thus  triple.               
                         1973.22, 1973.45: These measurements agree with the published           B__1967b
                         orbit of van den Bos (1967)                                             Lab1974 
                         1986.388: Separation for this partially resolved pair was calculated            
                         under the assumption of zero or otherwise known magnitude difference.           
                         It is now possible to make the final choice between two orbits of van           
                         den Bos (1964) in favor of the circular orbit and to perform small but  B__1964b
                         necessary corrections to the orbit.                                     Tok1985 
                         AB: Martin et al. (1998) derive component masses 1.999 +/- 0.346 and            
                         1.984 +/- 0.344 Msun.                                                   Mig1998 
                         Calculated mass sum is 3.73 +/- 0.53 Msun, a bit low for a pair of              
                         early A stars.                                                          Mut2010b
15418-4225   CPO 440     B is CD-42@10665.                                                               
15419-1941   ENG  54     43 Lib = kap Lib. A has variable velocity. B is BD-19@4187.                     
15419-3009   ARG  28     B is CD-29@11878.                                                               
15420+1118   BPM 636     [PM2000] 1133488 + [PM2000] 1133476.                                    Gvr2010 
15420+0027   A  2176     One component is SB1, P = 10.9 d. Only elements P, T, and a have been   Sta1978c
                         amended by Starikova (1978) from the orbit of Couteau (1960).           Cou1960c
                         1986.395: Separation for this partially resolved pair was calculated            
                         under the assumption of zero or otherwise known magnitude difference.   Tok1985 
15420-1108   STF1966     Apparently has wrong Hipparcos parallax, affected by both components.   Tok2014d
15421-6731   DON1114     CD-67@1794.                                                                     
15423-5519   KRV  45     Classical Cepheid U Nor.                                                        
15425-2030   ARA1111     A likely plate flaw.                                                    Grv2021a
15427+2618   STF1967     gam CrB = 8 CrB. A is a Delta Scuti-type variable.  The RV does not             
                         show a variation. A few discordant measurements seem to have been               
                         caused by scatter from the poor lines, and the double lines reported            
                         from three old Yerkes plates were also found probably spurious on               
                         remeasurement. See Baize & Petit catalog of doubles with variable       Baz1989d
                         component. Measure of 1989.388 made by MAPPIT. This measure had an      Han1989 
                         identification error, position error, or misprint in publication, which         
                         has been corrected.                                                             
                         Spectral types and masses of components assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
                         Calculated mass sum is 3.73 +/- 0.37 Msun, a bit low for a pair of              
                         early A stars.                                                          Mut2010b
                         Additional notes may be found in Duner (1876).                          Du_1876 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.18 +/- 0.30, 4.34, and 4.57 Msun, respectively.             Mlk2012 
15427-3443   ISO   1     psi 2 Lup = 4 Lup. The pair is also a double-lined spectroscopic                
                         binary, P = 12.26d.                                                             
15428-1601   BU   35     AB: A=SB?  No SB orbit for Aa,Ab. Assume not SB, small RV variation.    Tok2014d
15430+2617   FLA   2     Also known as LDS4588.                                                          
15430-5807   DUN 190     Spectrum of B: B8/A0(III).                                                      
15432+1340   BU  619     One component is a spectroscopic binary.                                        
                         Rectilinear solution by Zirm & Rica (2014).                             Zir2014b
15433+4024   BVD 244     Aka CBL 494.                                                                    
15435+1505   BPM 637     [PM2000] 1134776 + [PM2000] 1134682.                                    Gvr2010 
15435-5151   HJ 4794     B is CD-51@9412. Noted by Alden as an 8.58-day eclipsing binary.        Ald1935 
                         B is the Algol-type system HH Nor.                                              
15439+1700   BPM 638     [PM2000] 1135094 + [PM2000] 1135040.                                    Gvr2010 
15440+2220   COU 106     PS Ser, Algol-type eclipsing binary, P = 15.8861 d.                     Zas2011 
15440+0231   A  2230     A: 23 Ser = psi Ser. C is BD+02@2988. E is BD+02@2987.                          
                         CHARA Array Limb-darkened diameter of A :                               CIA2013c
                         R =  0.9410 +/- 0.0254 \rsun, L =   0.8340 +/-0.0201 \lsun,                     
                         Teff = 5692 +/-  74 K, M = 1.014 \msun, Age = 2.1 Gyr.                          
15440-3906   SHY 684     AC: HIP  77051 + HIP  77015.                                                    
             SHY 682     CD: HIP  77015 + HIP  76875.                                                    
15441-3311   BRR  12     AB: KOH  47AB.                                                                  
15442-5013   HJ 4797     Hipparcos acceleration double solution.                                         
15443+0626   HJ 1277     alp Ser = 24 Ser = Unukalhai. Variable?                                         
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
15444+4223   GIC 134     G179-050/G179-049.                                                              
15445+4256   GIC 135     G179-051/G179-052.                                                              
                         NLTT 41108/41109                                                        Chm2004 
15447+1716   CHR  49     26 Ser = tau 8 Ser. A spectroscopic binary.                                     
                         This system, first announced by McAlister and recalled in a later       McA1984b
                         McAlister paper after repeated attempts at confirmation, has been       McA1993 
                         restored. While perhaps still spurious, the subsequent confirmation or          
                         suspected duplicity (by another technique) makes the discovery                  
                         measurement somewhat more probable.                                             
15451-2739   LDS4589     Primary is white dwarf WD 1542-275.                                     Far2005b
15451-3506   SEE 248     Hipparcos suspected non-single.                                                 
15452-2239   SWR 181     CPM pair                                                                Skf2004 
15452-3819   LDS 539     Spectrum of B sdF5.                                                             
15453-5841   FIN 234     Spectrum composite: G5/8III+A3/7.                                               
15454-0123   STF1968     HJL 228.                                                                HJL1986 
15455-4702   BRT 868     Aka RST5590.                                                                    
15456+4205   UC  212     V337 Boo.                                                                       
15458-1657   TOK 169     HIP 77203.                                                              Tok2011a
15461+3914   OSO  66     G179-054. Not a common proper motion pair, based on astrometry and              
                         color                                                                   Oso2004 
15461-0148   ISO   2     25 Ser. A spectroscopic binary, P = 38.9d.                                      
15462+1525   STF1970     bet Ser = 28 Ser                                                                
                         AB: H 4  36.                                                            MEv2010 
             SHJ 281     AD: HIP  77233 + HIP  77083.                                                    
                         AD: D component is the primary of 15444+1518 ROE  75.                           
15462-2804   BU  620     The binary companion B discovered by S.W. Burnham in 1878 moved since   Bu_1879 
                         then by +6deg in angle, now at 0.63" separation. Considering this               
                         slow motion, the pair is likely much wider than it seems, being seen            
                         in projection. The sub-system CHR 50 Aa,Ab was discovered by speckle            
                         interferometry in 1983.42 at 0.20" (McAlister et al. 1987). A total of  Mca1987b
                         four measures are listed, the last one in 2006.19. Curiously, the wide  Msn2009 
                         pair AB was measured with speckle at 4-m telescopes several times (in           
                         1985.50, 1989.31, 1991.39) without resolving the sub-system. We         Mca1990 
                         measured the AB and found no trace of CHR 50 in three runs at SOAR in   Hrt1993 
                         2009-2012. The separation of CHR 50 implies an orbital period of 50     Tok2012b
                         yr. Yet the few speckle resolutions show a fast motion or a random              
                         scatter. If the sub-system CHR 50 were real, we would expect it to              
                         cause some wobble in the motion of AB, but no such signal is seen.      Tok2012b
             CHR  50     The measures show a large scatter and there are many observations of    Tok2010b
                         the wider AB without a measure of this close companion. The nature of           
                         the motion or even the reality of this pair is in question. A "ghost".          
15463-4703   BRT 870     Aka RST 798.                                                                    
15464+3627   STF1973     B is BD+36@2644.                                                                
                         HJL 229.                                                                HJL1986 
                         SHY 685. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         H N  32.                                                                MEv2010 
15465+0721   lam Ser     This object was misidentified as HR 5863 in McAlister (1978)            McA1978c
15467-3441   B   847     Measures uncertain; too close.                                                  
15467-4314   I  1276     HIP 77282. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         G5V dwarf at 47 pc. The WDS notes its resolution in 1926 by Innes at    I__1948a
                         0.3" and the last measure in 1935. The separation corresponds to an     B__1947 
                         orbital period of 50 yr. Yet the system was not resolved by Hipparcos           
                         in 1991.25 and by speckle in 2001.56 and on SOAR on 4 occasions from    Tok2010 
                         2008-2016. Tok2010 et al. (2004) found only a marginal variability              
                         of RV during 8 yr. The binarity is thus questionable. Possibly a        Tok2012b
                         "ghost" binary, but not "X" coded yet.                                  Tok2014a
                                                                                                 Tok2018c
15475+0337   JMS   5     2MASS J15472723+0336361 + 2MASS J15470234+0338260.                      Jms2008 
15475-3755   SEE 249     LDS5845.                                                                        
                         AB: GJ 599. B is WD NLTT 41169, mass 0.72 Msun, DA4.7 (Holberg et al.   Hbg2013 
                         2013).                                                                  Tok2014d
15476+8316   STF2002     B is BD+83@455.                                                                 
15476+5523   BU  946     A is a spectroscopic binary.                                                    
15479-6527   RMK  20     AB: Rectilinear solution by Letchford et al. (2018).                    LRR2018a
                         Despite the linear solution, proper motion and parallax favor a         Grv2020a
                         physical connection. Long period and/or high eccentricity possible.             
15481-3516   GHE  31     HN Lup.                                                                         
15482+7425   GJ 3922     Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by Griffin &          
                         Suchkov (2003). They derived component masses 0.72 and 0.51 Msun and    Grf2003 
                         an estimated semimajor axis of 29.83 mas.                               Ren2013 
15482+0134   EIS   1     V382 Ser = GJ 3917. Eisenbeiss et al. (2007) use archival data from     Eis2007 
                         POSS-I (1950) and UK Schmidt red and IR (1981, 1992), plus 2MASS, as            
                         well as followup H-band observation with the Omega-Cass IR camera at            
                         the 3.5m Calar Alto telescope; derive pm of secondary similar to that           
                         of primary. The orbital period is estimated at 7000y. Low-resolution            
                         optical spectroscopy yields spectral type M2.5-3.5V for the secondary;          
                         the derived distance is 24.4 +/- 4.2 pc.                                        
15488+1751   LDS 979     NLTT 41254/41252                                                        Chm2004 
15489-3923   HRG 122     Aka SKF2022.                                                                    
15492-3539   NHR   8     GQ Lup                                                                          
                         Primary is L1, age < 2 Myr. Radius of secondary may be ~2 Rjup and              
                         mass a few Jupiters.                                                    Nhr2005 
                         Mugrauer & Neuhauser (2005) reanalyze all relative astrometry and       Mug2005b
                         conclude that pair is CPM and likely bound.                                     
                         Guenther et al. (2005) determine spectral type of secondary M9V - L4V,  Gue2005 
                         Teff 1600-2500K.                                                                
                         Aa,Ab: Primary is T-Tauri type variable GQ Lup. Kraus et al. (2014)             
                         estimate the mass of the companion at 31 +/- 3 Mjup.                    KsA2014 
15492-6707   DON 758     This is CD-66 1805.                                                             
15493+6032   HU  912     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.30 +/- 0.72, 2.53, and 1.20 Msun, respectively.             Mlk2012 
15494-7937   HJ 4787     SWR 180. CPM pair                                                       Skf2004 
15495+2528   STF1977     Griffin & Duquennoy report that the primary is composed of a SpB1 plus  Grf1993 
                         a more distant companion. Thus the system is quadruple.                         
15496-0326   CHR 259     mu Ser = 32 Ser. Hipparcos acceleration double solution.                        
15496-4958   EGN  16     Single epoch, so optical/physical nature of most of the components              
                         unknown; however, all are likely unbound given location of system in            
                         galactic plane.  Primary is planet host star.                           Egn2007 
15499+1512   BPM 639     [PM2000] 1140168 + [PM2000] 1140100.                                    Gvr2010 
15500-0355   FGL   3     AD: Discovered using Chandra ACIS-I (Advanced CCD Imaging Spectrometer          
                         Imager) by Feigelson et al. (2003). Masses of B, C, and D components            
                         estimated at 0.45, 0.22, and 1 Msun.                                    Fgl2003 
15500-4855   GC 21252    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
15501+1134   BPM 640     [PM2000] 1140338 + [PM2000] 1140337.                                    Gvr2010 
15503+0212   SKF1311     Typographical error in initial WDS designation (15583+0212)                     
                         Aka Ome Ser = 34 Ser.                                                           
15506-2043   RSS 387     CPD-20@6243                                                                     
15511-4224   HJ 4811     SWR 183. CPM pair                                                       Skf2004 
15511-4956   RSS  28     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
15511-5503   DUN 193     A is a spectroscopic binary.                                                    
                         Spectrum of B may be K.                                                         
                         V360 Nor.                                                                       
15512+3539   BUP 163     kap CrB = 11 CrB                                                                
                         CHARA Array Limb-darkened diameter  1.456 +/- 0.020 mas,                CIA2018c
                         R =  4.77 +/- 0.07 \rsun, L = 11.6 +/- 0.3 \lsun,                               
                         Teff = 4870 +/-  47 K.                                                          
15513-0305   CHR  51     36 Ser.                                                                         
                         This peak was overlooked in the original analysis of our speckle data,          
                         but rediscovered during work on our quadrant determination paper.       Hrt1992b
                         Docobo et al. (2010) derive two possible orbits of this pair. The       Doc2010h
                         preferred orbit yields a dynamic parallax of 15.63 +/- 0.40 mas and a           
                         total mass of 3.82 +/- 0.21 Msun.                                               
15517-0559   A    21     AB: Rectilinear solution by Rica & Zirm (2012).                         FMR2012i
15519+1732   BPM 641     [PM2000] 1142011 + [PM2000] 1142098.                                    Gvr2010 
15520+5234   AG  199     B is BD+52@1912.                                                                
15520+4238   BAR  41     Identity of this system is uncertain. The Tycho measure supports        TYC2002 
                         identification of AB with 155200.97+423948.7. Aitken notes "Star C is   A__1932a
                         BD+43 2537 (8.2, G5)", which supports identification of C with                  
                         155156.23+423905.8. However, Barnard gave magnitudes of AB as 15 and    Bar1932A
                         15.5, which appears to agree with an elongated Aladin image at                  
                         155209.22+424127.5 rather than the Tycho pair.  CA would in this case           
                         be 45.4deg, 200.3", which could be explained by a typographical error           
                         in his value for rho. Unfortunately, Barnard's original publication             
                         for this measure is unknown.                                                    
15521+2015   HJ 2794     AB = LDS 980.                                                                   
15521+1052   BAG   7     Combined spectroscopic/astrometric solution by Tokovinin et al. (2000)  Tok2000b
                         Mass = 0.510  +/- 0.029 , 0.508 7 +/- 0.029   \msun for A and B.        HJL2020 
                         orbital parallax = 53.1   +/- 1.3   mas.                                        
15522-2953   HO  397     A variable?                                                                     
15523+3415   LDS5848     LDS6308.                                                                        
                         NLTT 41408/41412                                                        Chm2004 
15523-1826   HD 141937   Chauvin et al. (2006) note finding at least one faint companion         Cvn2006 
                         candidate within separation/magnitude range listed. However,                    
                         further observations are required for verification                              
15527+4227   chi Her     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
15529+1526   MUG  21     Mugrauer & Ginski (2015) note that the B component is itself a close            
                         binary, with projected separation about 4.3 +/- 0.7 au. The orbital             
                         period is estimated as 8.5 +/- 2 yr, assuming a total system mass of            
                         1.12 Msun.                                                              Mug2015 
15531+3445   LDS6309     Ross 806.                                                                       
                         NLTT 41446/41447                                                        Chm2004 
15531+1533   BUG  11     2MASS J15530228+1532369                                                         
                         Estimated spectral types are T6.5 + T7, effective temperatures ~980             
                         and ~890 K.  Masses are estimated at 0.019-0.065 and 0.016-0.061 Msun,          
                         and the orbital period (assuming the semi-major axis = 1.26 * rho) is           
                         ~45yr.                                                                  Bug2006a
15532+1312   STT 583     39 Ser.                                                                         
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         A: Ren & Fu (2013) calculated an astrometric orbit, combining                   
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Beavers & Salzer (1985). They derived component masses 1.00 and 0.14    Bvr1985 
                         Msun and an estimated semimajor axis of 31.31 mas.                      Ren2013 
                         Rectilinear solution by Hurowitz et al. (2014).                         USN2014a
15535-4216   CVN  54     NZ Lup.                                                                         
15536-2520   BU   36     2 Sco.                                                                          
15538-1644   OCC 985     tet Lib = 46 Lib.                                                               
15539+1518   BPM 642     [PM2000] 1143768 + [PM2000] 1143706.                                    Gvr2010 
15541+4427   LDS1428     SLW1146.                                                                        
15542+1659   A  2080     Recent observations render the quadrant reversal assumed by Baize       Baz1956 
                         (1956) very unlikely.                                                           
15542-0945   OCC9008     The OCC2010 solution is ambiguous and two are arbitrarily "T" coded             
                         until the true solution is determined.                                          
15548-5020   DUN 195     B is CD-49@10123.                                                               
15548-5434   RST2984     A is the Cepheid SY Nor.                                                        
15549-6045   SLR  11     Variable?                                                                       
15550+1552   BPM 643     [PM2000] 1144734 + [PM2000] 1144810.                                    Gvr2010 
15550-1923   HU 1274     47 Lib. No duplicity seen 1923.5, 1924.5                                VBs1927a
                         A is a spectroscopic binary.                                                    
15550-7646   NZO  61     SWR 184. CPM pair                                                       Skf2004 
15551+2529   BRT3309     Originally published as BRT 168.                                        Brt1928 
15551-6326   LDS 542     bet TrA                                                                         
15555+3512   MCT   9     GJ 3928 = G180-011 = LSPM J1555+3512.                                           
                         Daemgen et al. (2007) derive a distance of 12.6 +/- 3.6 pc, separation  Dae2007 
                         of 19.8 +/- 5.7 au, and predicted orbital period of 216 +101/-97 yr.            
                         Spectral types are M4.0 +/- 0.5 and M7.0 +/- 2.0; masses are 0.20               
                         +0.09/-0.06 and 0.08 +0.06/-0.03 Msun.                                          
                         Law et al (2008) derive a distance of 10.2 +5.6/-1.7 pc and a           Law2008 
                         projected separation of 15.7 +8.8/-2.5 au. Estimated spectral types             
                         are M4.5 and M6.5.                                                              
                         In addition to the astrometric points listed in Table 4, there is               
                         another data point from 2005 in Law et al. (2008). This point is        Law2008 
                         essentially at equal epoch to the Daemgen et al. (2007) point, but the  Dae2007 
                         position angle differs by 88deg in the two cases. While the Daemgen et          
                         al. data point is fully consistent with all other astrometric points            
                         of the target, the Law et al. point is fully inconsistent in this               
                         regard. The close to 90deg offset could imply some trivial                      
                         trigonometric error in reduction. Here we simply exclude the point              
                         from our analysis.                                                      Jnn2012 
15555-2616   TOK 790     4 Sco.                                                                          
15555-6011   HJ 4813     Composite spectrum; G5II-III+A3.                                                
15557-2645   I   977     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.91 +/- 0.69, 2.57, and 1.13 Msun, respectively.             Mlk2012 
15558+6127   GIC 136     LDS2362. G225-033/G225-034.                                                     
15558+3757   H 6  94     H VI 94. lam CrB = 12 CrB                                                       
15559-0210   STF1985     A premature orbit has been computed.                                            
                         H 2  85.                                                                MEv2010 
15564+1204   BPM 644     [PM2000] 1146035 + [PM2000] 1146115.                                    Gvr2010 
15565+5717   STF1996     AB: HJL 231.                                                            HJL1986 
15565+1540   STT 584     gam Ser = 41 Ser. Proper motion of A +312 -1281.                                
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: Rectilinear solution by Friedman et al. (2012).                     USN2012a
15565+0325   BAL2410     LDS 981.                                                                        
15565-2348   KOH  60     V1144 Sco = ScoPMS 13.  Due to typographic error, WDS designation was           
                         initially listed as 15585-2348.                                                 
15566-1450   VIG  18     Optical/physical nature of the faint companion is undefined.            Vig2012 
15567-1736   LDS4605     NLTT 41560/41561                                                        Chm2004 
15567-3426   COO 189     Spectrum of B may be K.                                                         
15567-4219   BIL   5     Hen 3-1119.  Noted as possible binary (separation > 0".040) by Baines           
                         et al. (2006)                                                           Bns2006 
                         Distance 145 +/- 15 pc, age 5 +8/-3 Myr. Spectral type of primary               
                         F6IIIe; Biller et al (2012) estimate masses at 2.2 +/- 0.3 and 0.1-0.4          
                         Msun. Their HKL magnitudes are derived from photometry by Malfait et            
                         al. (1998 A&A 331, 211), combined with their magnitude differences.     Bil2012 
15568+3530   HJ  577     HJL 230.                                                                HJL1986 
15569+3613   SPN   1     Found while searching for HJ  258. This matches the DM cross-id.                
                         The John Herschel pair is at 15569+3604."                                       
15569+3604   HJ  258     Also known as GRV 916.                                                          
15569-2913   SEE 251     rho Sco = 5 Sco = Iklil                                                         
15569-3358   PZ    4     A: xi 1 Lup                                                                     
                         B: xi 2 Lup                                                                     
                         AB: SWR 188. CPM pair                                                   Skf2004 
15571-1602   HJ 1281     The primary is variable.                                                        
                         Additional notes may be found in Burnham (1894).                        Bu_1894 
15572+0509   WLF   2     Wolf 781-782. UCAC2 proper motion of A +062,-1389; PM of B +052,-1389           
15572+0324   STF1987     H 3 103.                                                                MEv2010 
15575+3434   LDS 983     A is also a 322d spectroscopic binary.                                  Tok2019b
                         AB: NLTT 41631/41622                                                    Chm2004 
15576+2653   AGC   7     eps CrB = 13 CrB                                                                
                         NPOI Limb-darkened diameter 2.997 +/- 0.128 mas, Sp = K2III,            NOI2018 
                         R = 21.87 +/- 0.99 \rsun, Teff = 4408 +/-109 K,                                 
                         L = 162.9 +/- 9.4 \lsun, M = 1.37 +/- 0.24 \msun,                               
                         Age = 3.24 +/- 1.81 Gyr.                                                        
15578+5916   PIN  10     Secondary is M9V, pm -0.30 +/- 0.02, 0.21 +/- 0.01 arcsec/yr, distance          
                         34 +/- 2pc. Given the van Leeuwen (2007) proper motion (-0.296 +/-      VlF2007 
                         0.001, 0.203 +/- 0.002 arcsec/yr) and distance (31 +/- 1pc) for the             
                         primary, the pair is likely a true CPM system.  At a projected                  
                         separation of 3800 au, the gravitational binding energy makes this one          
                         of the most fragile binaries known.                                     Thn2013 
15578-3612   SWR 189     CPM pair                                                                Skf2004 
15579-3158   HJ 4821     B is CD-31@12424.                                                               
                         SWR 190. CPM pair                                                       Skf2004 
15580-3144   HNK   4     Member of Sco-Cen Association. Primary mass 2.46 +0.31/-0.59 Msun;              
                         secondary mass estimated at 98 +42/-12 Mjup (for age 10 Myr), or                
                         152 +56/-28 Mjup (for age 20 Myr).                                      Hnk2015 
15583-0913   TSN  93     Same as GWP2566 with a quad flip.                                               
15585+5723   GIC 138     G225-039/G225-038.                                                              
15585-2124   HNK   5     Aa,Ab: Member of Sco-Cen Association. Mass of Aa 1.67 +0.07/-0.12Msun;          
                         mass of Ab estimated at 86 +12/-21 Mjup (for age 10 Myr), or                    
                         124 +27/-24 Mjup (for age 20 Myr).                                      Hnk2015 
15586-4024   BRT 872     A likely plate flaw.                                                    Grv2021b
15587-3910   HJ 4822     SWR 191. CPM pair                                                       Skf2004 
15587-5404   I   553     Spectrum composite: G9/K0III+A2V.                                               
15588+5042   LDS1431     Matched with LDS5852 by BD number.                                              
15589+6132   FAR  44     Primary is white dwarf WD 1558+616.                                     Far2006 
15589+2147   STF1990     B is BD+22@2906.                                                                
                         BC: H 1  81.                                                            MEv2010 
15589-2607   BU  622     pi Sco = 6 Sco = Fang. A is a spectroscopic, occultation, and                   
                         eclipsing binary, period 1.57d.                                         Zas2011 
15590+1820   SHY 691     HIP  78283 + HIP  78067.                                                        
15590+1606   BPM 645     [PM2000] 1148315 + [PM2000] 1148233.                                    Gvr2010 
15591+3736   BFR  12     NLTT 41701 + 2MASS J15590740+3735275. Baron et al. (2015) estimate              
                         spectral types K2 and M8.0 +/- 0.5, distances 61 +61/-27 and                    
                         89 +6/-29 pc, masses 0.872-0.941 and 0.084-0.090 Msun.                  BFr2015 
15591+0036   RAO 507     V335 Ser.                                                                       
15591-1956   SHJ 213     B is BD-19@4274. B spectrum A8/9.                                               
15593+2752   TDS9712     AR CrB.                                                                         
15595+2555   JEF   2     The observation is doubtful. Others of same year do not suggest                 
                         duplicity. This is the recurrent nova T CrB, with composite spectrum;           
                         sdBe+gM3+Q.                                                                     
15598+4404   JNN 106     The primary is an M2.0 star exhibiting Halpha emission and saturated            
                         X-ray emission (Riaz et al. 2006, AJ 132, 866). B component is M8.0             
                         +/- 0.5, mass 43 +/- 9 Mjup.  Age of the system is perhaps 50-200 Myr.  Bwl2015 
15598+1723   STF1994     These are the CD components of STF1993 at 15598+1723.                           
             STF1993     AB: H 5 126.                                                            MEv2010 
16000-2025   HLD 125     AC = LDS 547 = LDS4617.                                                         
16000-2221   KSA 122     V1150 Sco.                                                                      
16001+1317   GRV 919     HJL 232.                                                                HJL1986 
16001-3824   RMK  21     eta Lup                                                                         
16001-5355   LPO  54     TDS9722.                                                                        
16003+1346   BPM 646     [PM2000] 1149477 + [PM2000] 1149501.                                    Gvr2010 
16003-1632   ENG  55     49 Lib. A is a long-period spectroscopic binary.                                
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
16003-2237   LAB   3     del Sco = 7 Sco = Dschubba. A spectroscopic triple and occultation              
                         quadruple.                                                                      
                         Intensity Interferometer Limb-darkened diameter 0.46 +/- 0.04 mas.      HBr1974 
                         1973.22, 1973.45: The new component here appears to have a much longer          
                         period than the 20-day single-line SB reported by van Hoof et al.               
                         (1963 ApJ, 137, 824).                                                   Lab1974 
                         1981.4767 and other observations through 1981.4929: Companion           HBr1974 
                         discovered by intensity interferometry (Hanbury Brown et al. 1974).             
                         Delta m in the visible is about 2.                                      Bag1984b
                         1993.415: observations with MAPPIT on 3.9m AAT; maximum separation of           
                         apertures was 3.3m. Paper gives orbit.                                  Bed1993 
                         Miroshnichenko et al. (2001) give a combined spectroscopic/             Mko2001 
                         interferometric orbit, adopting P and e from Hartkopf et al. (1996).    Hrt1996a
                         Combined spectroscopic/astrometric solution. Tango et al. (2009)        Tng2009 
                         derive masses 15 +/- 7 and 8.0 +/- 2.6 Msun, based on their mass                
                         function and brightness ratio, together with the ZAMS model grid of             
                         Tout et al. (1996 MNRAS 281, 257). The resulting dynamical parallax of          
                         7.03 +/- 0.15 mas agrees well with the revised Hipparcos parallax of            
                         6.65 +/- 0.89 (van Leeuwen 2007, ASSL vol. 350).                                
                         Tycner et al. (2011) give a combined spectroscopic/astrometric          NOI2011b
                         solution, based on spectroscopicdata of Miroshnichenko et al. (2001),   Mko2001 
                         published astrometry, 2 measures obtained with the NPOI array in 2000,          
                         and 94 additional NPOI measures obtained over the years 2005-2010. The          
                         timing of periastron passage has been revised to UT 2011 Jul 6 +/- 2d.          
                         Expected minimum separation at closest approach is predicted to be              
                         6.14 +/- 0.07 mas (14 stellar radii).                                           
                         Malkov et al. (2012) derive dynamical and photometric masses of                 
                         28.41 +/- 11.43 and 20.39 Msun, respectively.                           Mlk2012 
                         Che et al. (2012) derive an orbit of del Sco based on data from NPOI            
                         and CHARA Array. Total mass 28 +/- 11 Msun, with the large error bar            
                         resulting from uncertainty in parallax estimate. Individual masses              
                         estimated at 13.9 (from  photometry and spectroscopy) and ~6 Msun               
                         (based on mass ratio from RV measurements during periastron).           CIA2012c
                         The disk dissipates near apastron and then begins reforming as the      XXX2020d
                         companion approaches periastron. The V magnitude is variable over the           
                         orbit but it is unclear if this is due to the secondary or interaction          
                         between the primary and the disk.                                               
16004+1437   STF1995     Coordinate confusion between this pair and 16005+1439 LAU   2, perhaps          
                         due to switching of BD numbers. Although WDS designations suggest that          
                         STF1995 is the southern of the two pairs, it is actually the northern.          
16005+1439   LAU   2     See note for 16004+1437 STF1995.                                                
16005-3605   HWE  81     SWR 192. CPM pair                                                       Skf2004 
16008+3008   UC 3226     Algol-type eclipsing binary, period 0.29655 d.                          Zas2019 
16008+1602   BPM 647     [PM2000] 1149934 + [PM2000] 1149952.                                    Gvr2010 
16010+3318   S   676     rho CrB = 15 CrB                                                                
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
             rho CrB     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
                         Astrometric orbit by Gatewood et al. (2001) determined be combining     Gat2001a
                         Hipparcos and Multichannel Astrometric Photometer data with the                 
                         spectroscopic elements of Noyes et al. (1997 ApJ 483, L111). It is an           
                         alternate solution for this proposed planetary system.                          
             S   676     H 6  93.                                                                MEv2010 
16010+0147   LDS4619     The primary is Wolf 622.                                                        
16011+2808   AG  349     Spectrum is A7 (Yale) or K (McCormick).                                         
16011+2610   H 5  75     H V 75.                                                                         
16011-2228   KOH  65     V1151 Sco.                                                                      
16012-6347   EVS  26     Primary is the Cepheid S TrA.                                           Evs2016a
16013+0523   LDS4620     G016-025. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
16014+1307   BPM 648     [PM2000] 1150371 + [PM2000] 1150442.                                    Gvr2010 
16014-2241   MET  67     ScoPMS 21 = V1152 Sco.                                                  Msr2005 
16018+2519   WIS 300C    V505 Ser.                                                                       
16019-2159   KOU  44     Followup imaging by Lafreniere et al. (2011) indicates that components          
                         share common proper motion. Spectral types are B9V and M8 +/- 1; mass           
                         of the secondary is estimated from models at 0.022 +/- 0.004 Msun.      Laf2011 
                         Lachapelle et al. (2015) derive the following properties:                       
                           spectral types            | B9V            | M7    +/- 0.5                    
                           Teff(K)                   | ~10,500        | 2700  +/- 100                    
                           log(L/Lsun)               |                | -2.53 +/- 0.09                   
                           Mass (Msun) (5 Myr)       | ~2.5           | 0.022 +/- 0.001                  
                           Mass (Msun) (10 Myr)      | ~2.5           | 0.023 +/- 0.002                  
                           Distance (pc)             | 156.7 +/- 13.0 |                                  
                           Projected separation (AU) | 740   +/- 60   |                          Lch2015 
16019-2822   SEE 260     Primary is V1041 Sco, an Algol-type eclipsing binary, P = 2.18691d.     Zas2012 
16020-3732   KOU  45     LL Lup.                                                                         
16021-2943   HJ 4826     SWR 193.                                                                        
16022-2240   GHE  18     V1154 Sco.                                                                      
16024+0937   KU  109     B is BD+10@2944.                                                                
16029+1548   BPM 649     [PM2000] 1151707 + [PM2000] 1151680.                                    Gvr2010 
16029-2501   BU   38     HDO 141                                                                         
16032+4215   OSO  67     G180-024. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
16033+3638   BAG  52     1983.3070: A dF9 + A0 SB with a 108d period.  A visual companion with           
                         delta m ~ 2 mag is suspected, but further confirmation is required.     Bag1984a
                         1984.2792: Halbwachs (1981) predicts angular separation of about 0".02  HJL1981 
                         Analysis of the interferometric measurements combined with the                  
                         spectroscopic orbit shows that the interferometric binary is probably           
                         not the spectroscopic system.                                           Bnu1986 
16034-3829   I   555     AC = SWR 194. CPM pair. A component is 1" CPM pair                      Skf2004 
16035-5747   SEE 258     AB: iot 1 Nor.                                                                  
                         1976.474: Visual observations of this system extend over more than two          
                         periods, but this separation is significantly different from that       B__1961b
                         derived from van den Bos' (1961) elements.                              BLM1978 
                         This star was misidentified as ADS 9870 = HD 143456 in the first                
                         speckle catalogue.                                                      McA1984b
                         1994.5216: Our measure is plotted with orbital data from the WDS                
                         catalogue in Figure 2.                                                  Hor1996 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.77 +/- 0.55, 2.71, and 1.82 Msun, respectively.  Mlk2012 
                         Ary2014b measure of new pair in the field of SEE 258 has been rejected  Ary2014b
                         by author in private communication on July 2, 2014.                             
                         AB,C triple solution (AB in HIP).                                       Sod1999 
16037-6030   RSS  29     This previously uncataloged double star was a Hipparcos double entry            
                         system. The first measure is determined from the individual positions           
                         listed by Rousseau et al.                                               Rss1996 
16038+0459   KUI  69     43 Ser.                                                                         
16040-2156   LDS 548     NLTT 41839/41840                                                        Chm2004 
                         V1044 Sco, Algol-type eclipsing binary, P = 0.914833 d.                 Zas2011 
16044-1122   STF1998     51 Lib = xi Sco. Quintuple.                                                     
                         AB: Mt. Wilson spectral type F3s.                                               
                         Masses and bolometric magnitudes are derived for the two components             
                         of this system by Mason et al. (1999), based on assumed spectral types  Msn1999a
                         and available parallaxes.                                                       
                         AB: H 1  33.  AC: H 2  20.                                              MEv2010 
                         AB,C triple solution by Soderhjelm (1999). (Failed HIP solution due to  Sod1999 
                         bad pointing with C comp at IFOV edge).                                         
                         Star C (mag. 7.30, 7", G1V) is in retrograde motion, and ADS 9910               
                         (mags. 7.4-8.0, 11", dG6) is 281" distant and shares proper motion.             
                         Appears to be a common proper motion pair associated with RST3949       Tok2010b
                         (16278-0822).                                                                   
                         AC: Additional notes may be found in Fatou (1941).                      Fat1941 
                         Mass = 1.53, 1.53, 1.00 \msun for A, B, C, respectively.                Tok2020d
                         Teff = 6532, 6532, 5705 K for A, B, C, respectively.                            
                         Physical quintuple with 16044-1127STF1999AB with P ~ 300 kyr.                   
16044-1127   STF1999     AB: B is BD-11@4058.                                                            
                         AB: H 2  21.                                                            MEv2010 
                         HIP 78738. B = HIP 78739.                                               Tok2011a
                         Mass = 0.97, 0.91 \msun A, B, respectively.                             Tok2020d
                         Teff = 5622, 5330 K for A, B, respectively.                                     
                         Physical quintuple with 16044-1122STF1998ABC with P ~ 300 kyr.                  
                         The period of AB is suggested to be ~4.5 kyr.                                   
                         AD: D is AB of STF1998. AD also known as 16044-1122ABT  12AB,E.                 
                         AD: D is SB1, P=44.699d                                                 Tok2014d
16044-5343   DUN 198     QY Nor.                                                                         
16045+3226   HJ  581     Also known as GYL  14.                                                          
16046-3752   HDO 253     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
16048+7016   STTA143     B is BD+70@864.                                                                 
16048+6003   STTA142     B is BD+60@1652.                                                                
16048+3910   WNO  47     NLTT 41938/41931                                                        Chm2004 
                         NI   35.                                                                        
16049+4045   A  1641     Aka COU1275.                                                                    
                         2014.513 non-detection at star previously identified as A  1641.        Gii2022 
16052-5355   KRV  12     Classical Cepheid RS Nor.                                                       
16053-4931   CPO 454     V384 Nor, Algol-type eclipsing binary, P = 3.97413 d.                   Zas2011 
16054-1948   BU  947     A: bet 1 Sco = 8 Sco A = Acrab. Common proper motion with bet 2 Sco.            
                         Companion suspected sf on two nights.                                   B__1963b
             H 3   7     H III 7. C is bet 2 Sco and was found as a double in summer 1627 by     C__1627 
                         Benedetto Castelli. It also has a close interferometeric pair found by          
                         McAlister.                                                              McA1978b
             MCA  42     C: bet 2 Sco = 8 Sco C                                                          
                         Orbits for two component pairs AB and CE of this complex star system            
                         were calculated independently of one another by Seymour et al. (2002).  USN2002 
             bet Sco     Combined spectroscopic/astrometric solution for bet Sco by Holmgren et  Hol1997 
                         al. (1997) using lunar occultation data; they derive masses, radii,             
                         distance. There is a typographical error in their Table 4: the value            
                         of a" is 1.42 mas, not 1.42 arcsec.                                             
                         A complex, multi-body solution was not attempted.                               
16055+2955   GRV1217     SLW1162.                                                                        
16055-6610   NZO  73     SWR 195.                                                                        
16057+1332   BPM 650     [PM2000] 1154370 + [PM2000] 1154364.                                    Gvr2010 
16057-0617   FIN 384     Aa,Ab: A spectroscopic binary resolved by interferometry.                       
                         1990.3494: Residuals from orbit of Baize (1992) are (-4.5deg, 0".003).  Baz1992c
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 9.73 +/- 3.12, 3.38, and 1.30 Msun, respectively.  Mlk2012 
             BU  948     AB: Additional notes may be found in Couteau (1956).                    Cou1956 
             SHY 696     AE: HIP  78849 + HIP  78822.                                                    
             FIN 384     Aa,Ab: Docobo & Andrade (2013) derive a dynamical parallax of 10.43             
                         +/- 0.81 mas and component masses 1.74 +/- 0.53 and 1.74 +/- 0.53 Msun          
                         (for spectral type F3V) or 10.98 +/- 0.88 mas, 1.50 +/- 0.47 and 1.50           
                         +/- 0.47 Msun (for F2IV). See paper for extensive notes on system.      Doc2013d
16057-2027   GJ 610      Arenou (2000) gives combined solution of astrometric orbits and DSBs.   Are2000 
                         Paper includes masses and distances.                                            
16057-3252   SEE 264     Spectrum of C may be M.                                                         
16059+1041   HDS2273     Aa,Ab: 1991.3273: This observation confirms the Hipparcos solution at           
                         a similar epoch (1991.25). An elongated secondary peak yielded an               
                         inaccurate value for rho, however.                                      Msn1999b
                         1996.3240: Elongated secondary peak yielded inaccurate value for rho.   Msn1999b
16059-1819   BEJ   1     Bejar et al. (2008) discovered a companion to the Upper Sco brown               
                         dwarf UScoCTIO 108. Spectral types are M7 and M9.5, masses 60 +/- 20            
                         and 14 +2/-8 Mjup; the companion is near the deuterium-burning mass             
                         limit.                                                                  Bej2008 
16060+1319   STF2007     AB: B is BD+13@3063.                                                            
                         Statistically the same parallax within the errors would indicate the            
                         components are physical.                                                        
16061-2336   RAS  25     Main component is He-weak B8V star from Upper Scorpius Association.             
                         Secondary is likely type F.                                             Ras2014 
16062-1935   KSA   1     Kraus et al. (2007) derive spectral types M5, M5.2, and M5 (all +/-     KsA2007b
                         0.5) for the Aa, Ab, and B components, respectively. Masses are 0.14,           
                         0.12, and 0.14 (all +/- 0.02) Msun. Projected separation of Aa,Ab is            
                         7.7 +/- 1.2 au, that of AB 1600 +/- 200 au. Conclude that Aa,Ab is a            
                         close binary with B a young, comoving member of the Upper Scorpius              
                         association.                                                                    
16066-3648   the Lup     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
16068-3357   SWR 197     CPM pair                                                                Skf2004 
16070-2743   RST1877     Carmona et al. (2007) reanalyzed the data obtained by Perez et al.      Crm2007 
                         (2004), resulting in a change in his position angle from 353 to 4deg.   Pez2004 
                         Muller et al. (2011) resolved the B component into a close pair, which  MuA2011 
                         they referred to as BC. However, the C component is a long-known                
                         distant member of the system, so the close pair has been renamed        Glp1892f
                         MUA 1 Ba,Bb.  They derive the following parameters for the close                
                         members of the system:                                                          
                         component:   A               Ba                 Bb                              
                         spec:       F0IIIe           K7V                M1V                             
                         L (Lsun)    12.7 +6.4/-3.7   0.50 +0.24/-0.20   0.41 +0.19/-0.16                
                         Teff (K)    7220 +/- 115     4000 +/- 250       3750 +/- 250                    
                         M (Msun)    1.8 +0.2/-0.1    0.8 +/- 0.2        0.5 +/- 0.2                     
                         R (Rsun)    2.3 +/- 0.5      1.5 +/- 0.7        1.5 +/- 0.7                     
                         age (Myr)   9 +/- 2          4 +5/-2            3 +2/-1                         
16070-3902   REP  29     = HO Lup.                                                                       
16072-1424   LDS4631     NLTT 42002/42006                                                        Chm2004 
16072-1927   LAF 112     AC: Incorrectly added as 16072-1927 LAF 112AC.                                  
16072-6008   HJ 4829     One component is probably variable. Spectrum A5/7V+(M1/2).                      
16073-6255   EVS  27     Primary is the Cepheid U TrA.                                           Evs2016a
16076+2900   STF2011     Called Am by Bidelman.                                                          
16076-0239   STF2008     HJL 233.                                                                HJL1986 
16076-1245   BU   39     11 Sco.                                                                         
16079+1425   A  1798     1983.7151: This autocorrelogram was remeasured; the new results are             
                         listed here.                                                                    
16080+4523   BU  355     Measures of a wider component by Lewis and Bowyer were incorrectly      L__1898a
                         attributed to this system and assigned the designation L   38AD. These  Bow1898 
                         measures were actually of 16089+4521STF2015AC.                                  
16080-2738   GLP   6     B is CD-27@10794.                                                               
16081+1703   STF2010     kap Her = Marsic. B is BD+17@2965. Mt. Wilson spectral types G4 and K1.         
                         AB: H 5   8.                                                            MEv2010 
16081+0049   OL  161     BAL 1469.                                                                       
16081-1815   TOK 171     HIP 79048. The 2MASS companion at 10.3", 356deg is likely an artifact,          
                         in which case another companion at 7.6" in ANDICAM images is measured.  Tok2011a
16084-1308   GIC 139     G153-028AB.                                                                     
                         NLTT 42059/42058                                                        Chm2004 
16085-1006   BU  949     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.30 +/- 1.51, 2.70, and 1.13 Msun, respectively.             Mlk2012 
16086+4003   STF2014     AB: G. Struve's measures of separation in 1929, given as 1.5", need             
                         addition of half a revolution of screw. Corrected result is 8.21".      B__1963b
16086-3906   SEE 265     AB: A is the semiregular variable V856 Sco. There are indications of a          
                         14d spectroscopic companion. There is an extended circumstellar                 
                         atmosphere, and C shares common proper motion and radial velocity.              
16088+4456   NOI   2     phi Her. Hipparcos astrometric solution adopts some elements from the   HIP1997d
                         orbit of Aikman (1976).                                                 Aik1976 
                         Combined spectroscopic/interferometric solution by Torres et al.        Trr2007 
                         (2007) , including NPOI observations from 1997-2005. Derive masses              
                         3.05 +/- 0.24 and 1.614 +/- 0.066 Msun, parallax 14.34 +/- 0.35 mas.            
                         Combined spectroscopic/interferometric solution by Zavala et al.        Zav2007 
                         (2007) , including NPOI observations from 1997-2005. Derive mass sum            
                         4.7 +/- 0.6 Msun, effective temperatures 11525 +/- 150 and 8000 +/-             
                         150 K for A and B, respectively.                                                
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.38 +/- 0.29, 4.98, and 2.57 Msun, respectively.             Mlk2012 
16089+4521   STF2015     AC: Two measures of this pair by Lewis and Bowyer were incorrectly      L__1898a
                         attributed to WDS 16080+4523 and assigned the designation L   38AD.     Bow1898 
                         AB: H 1  37.                                                            MEv2010 
16089+1738   BPM 651     [PM2000] 1157437 + [PM2000] 1157419.                                    Gvr2010 
16090+5756   ES 2651     A is a spectroscopic binary.                                                    
16090+3629   BU 1087     tau CrB = 16 CrB. A is a spectroscopic binary.                                  
16090-1900   HNK   6     Aa,Ab: Member of Sco-Cen Association. Mass of Aa 2.48 +0.32/-0.58Msun;          
                         mass of Ab estimated at 135 +38/-33 Mjup (for age 10 Myr), or                   
                         201 +56/-44 Mjup (for age 20 Myr).                                      Hnk2015 
16092-5603   RST1878     Spectrum composite; K0+A2.                                                      
16092-7104   TOK 172     HIP 79143.                                                              Tok2011a
16093-2008   BIL   6     Biller et al. (2011) derive spectral types for the two components of            
                         M7 +/- 0.5 and M6 +/- 1.0; Teff = 2990 +/- 60 and 2850 +/- 170K.                
                         Assuming an age of 5 Myr, masses are 79 +/- 17 and 55 +/- 25 Mjup. If           
                         the system age is 10 Myr, these increase to 84 +/- 15 and 60 +/- 25             
                         Mjup. Component JHK magnitudes are derived from 2MASS magnitudes,               
                         combined with NIRC2 magnitude differences.                              Bil2011 
16095+2403   BRT3310     Originally published as BRT 169.                                        Brt1928 
16095+1513   BPM 652     [PM2000] 1157993 + [PM2000] 1158079.                                    Gvr2010 
16095-1711   TOK 173     HIP 79169. Another companion B at 5.42" 337deg, dK=5.41 is seen in the          
                         ANDICAM K- and V-band images. Crowded field, N*=40.                     Tok2011a
16095-2105   LAF 76      Aa,Ab: Lafreniere et al. (2008) obtained AO imaging and spectroscopy    Laf2008b
                         of the young star 1RXS J160929.1-210524 and its planetary-mass                  
                         candidate companion. Spectral types of the primary and companion are            
                         K7V +/- 1 andf L4 +1/-2, masses are 0.85 +0.20/-0.10 Msun and 8 +4/-2           
                         Mjup. Projected separation is ~330 au, assuming a distance of 150pc.            
                         Aa,Ab: Primary is the pre-main sequence star 1RXS J160929.1-210524.             
                         Kraus et al. (2014) estimate mass of the companion at 10 +/- 2 Mjup.    KsA2014 
                         AB: Wu et al. (2015) estimate the B component has spectral type                 
                         L2 +/- 1, Teff 2000 +/- 100K, and mass 0.012-0.015 Msun.                WuY2015b
16096-5210   RST 813     CPD-51@8974.                                                                    
16097+6550   LDS2369     NLTT 42208/42209                                                        Chm2004 
16097-2754   GLP   4     B is CD-27@10816.                                                               
16100-6610   I   982     Includes EQ TrA, an Algol-type eclipsing binary, P = 2.70909d.          Zas2012 
16102-4008   I  1082     Measures uncertain, too close.                                                  
16102-8414   HJ 4798     LDS 543.                                                                        
16103+5945   LDS2370     BD+60@1658a.                                                                    
16104+4349   14 Her      Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from the Geneva           
                         Extrasolar Planet Search Programs home page.                            HaI2001 
16104+1720   ROE 140AB   = JRN  3 with quadrant flipped.                                         Dam2010 
16104+1530   BPM 653     [PM2000] 1158838 + [PM2000] 1158883.                                    Gvr2010 
16104-1904   KSA 133     Primary is the T-Tauri type variable ScoPMS 42b. Kraus et al. (2014)            
                         find the D, E, and F components to be background stars.                 KsA2014 
16105-0041   LSR 1610... LSR 1610-0400.  Dahn et al. (2008) derive an absolute parallax of       Dah2008 
                         31.02 +/- 0.26 mas and a proper motion of 1446.5 +/- 0.2 mas/yr in the          
                         direction 213.3+/- 0.1 deg. The absolute magnitude of the system is             
                         16.56 +/- 0.03 mag. LSR 1610-0040 (sd?M6pec) appears to be only mildly          
                         metal-poor; the companion must be a low-mass substellar brown dwarf.            
                         Koren et al. (2016) derive a parallax pf 30.73 +/- 0.34 mas; proper             
                         motion is -795.42 +/- 0.07 mas/yr in RA, -1208.40 +/- 0.9 mas/yr in             
                         DEC.  The systematic radial velocity is -98.3 +/- 0.3 km/sec.           Dah2016 
16105-1913   KSA  93     Primary is the pre-main sequence star [PBB2002] USco 161031.9-191305.           
                         Kraus et al. (2014) estimate mass of the companion at 70 +/- 10 Mjup.   KsA2014 
                         Lachapelle et al. (2015) derive the following properties for Aa,Ab,B:           
                           Spectral type        | K7         | ~M4            | M9    +/- 0.5            
                           Teff (K)             | ~4000      | 3200  +/- 300  | 2500  +/- 200            
                           log(L/Lsun)          | ...        | -1.48 +/- 0.11 | -2.13 +/- 0.12           
                           Mass (Msun) (5 Myr)  | ~0.77      | 0.12  +/- 0.02 | 0.032 +/- 0.004          
                           Mass (Msun) (10 Myr) | ~0.77      | 0.16  +/- 0.02 | 0.058 +/- 0.011          
                           Distance (pc)        | 145 +/- 14 | ...            | ...                      
                           Proj. sep. (AU)      | ...        | 26    +/- 3    | 885   +/- 85     Lch2015 
16107-2252   BRT1496     CD-22@11390.                                                                    
16109+1144   ZUC  13     SKF  50.                                                                        
                         Primary is white dwarf PG 1608+118.                                     Zuc1992 
16111-0814   MTL   1     Mitchell ascribed to STF 2012 rej. B is BD-07@4220.                     Mtl1876 
16111-1905   MSR   7     HBC 630 = V1000 Sco.                                                    Msr2005 
16113-5421   KRV  14     = QZ Nor.                                                                       
16115+1507   A  1799     Rectilinear solution by Scardia et al. (2017).                          Sca2017c
16115+0943   FIN 354     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.09 +/- 1.87, 3.48, and 1.58 Msun, respectively.             Mlk2012 
                         Docobo & Andrade (2013) derive a dynamical parallax of  5.45 +/- 0.28           
                         mas and component masses 2.31 +/- 0.46 and 2.15 +/- 0.43 Msun (for              
                         spectral type A7V) or 5.64 +/- 0.32 mas, 2.09 +/- 0.45 and 1.93 +/-             
                         0.43 Msun (for F0IV). See paper for extensive notes on this system.     Doc2013d
16116-1839   HER  25     Formerly known as CHN  25 and GHE  19.                                          
16118+4222   STF2024     H IV 115. Composite spectrum; K4II+F6-8V.                                       
                         H 4 115.                                                                        
16118+3626   WRH  21     A long-period spectroscopic binary.                                             
                         1983.3098: Very poor atmospheric conditions.                            Bag1984a
                         Torres (2007) incorporates Hipparcos intermediate data with             Trr2007b
                         spectroscopic results to derive orbit. P, e, omega, and T are adopted           
                         from the spectroscopic solution of Scarfe et al. (2007). Resulting      Scf2007 
                         masses are 1.38 +0.09/-0.03 and 1.36 +0.07/-0.02 Msun.                          
16120-1907   KOH  78     HBC 633 = V1001 Sco.                                                    Msr2005 
16120-1928   CHR 146     nu Sco = Jabbah. A is a spectroscopic and occultation binary.                   
             H 5   6     H V 6. Shows two spectra, B8V+B9VpSi; the system is at least quintuple          
16121+1433   STF2017     B is BD+14@3011.                                                                
16121+1155   STF2016     H 2  86.                                                                MEv2010 
16122+0908   A  2782     CD: WAK  17.                                                                    
16123-2825   HJ 4839     12 Sco.                                                                         
16124-4339   HJ 4837     B is CD-43@10607.                                                               
16128+3922   STF2028     Pair was listed, but in a "rejected" list, not part of discoverer's             
                         regular numbering sequence.                                                     
16133+1332   STF2021     49 Ser                                                                          
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Hopmann (1964) orbit rejected from Fourth Orbit Catalog                 Hop1964b
                         ("period over 4000 years")                                              Wor1983 
                         AB: NLTT 42273/42272                                                    Chm2004 
                         AC: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB: H 1  82.                                                            MEv2010 
16133-5414   HJ 4835     AB: V340 Nor.                                                                   
16134+2431   POU3216     Rectilinear solution by Friedman et al. (2011).                         USN2011a
16134-1806   CHR 233     First detected as an occultation binary by Africano.                    Afr1978 
16135-5438   HDO 254     kap Nor                                                                         
16137+4638   A  1642     Pair suspected of variability. The quadrant reversal assumed in         Dom1970 
                         Dommanget orbit did not take place.                                             
16138-5209   RST5594     CPD-51@9079.                                                                    
16142-5047   TOK 409     HIP 79576 has a variable RV (GCS). The 79mas separation implies an              
                         orbital period of ~5yr. This is the high-PM star LTT 6467 with a low            
                         metallicity [Fe/H]=-0.78. Ivanov et al. (2013 A&A 560, 21) found no             
                         CPM companions.                                                         Tok2015c
16143-0342   BUP 164     del Oph = 1 Oph = Yed Prior                                                     
                         NPOI Limb-darkened diameter   10.161 +/- 0.020 mas,                             
                         R =   53.50 (+1.38-1.46 )  \rsun,  Teff = 3735 +/-   5 K,                       
                         L =  501.6 +/-  26.6 \lsun.                                             NOI2023 
16143-5005   HJ 4838     B is CD-49@10426.                                                               
16146-1832   HD 145997   A measure on 1980.7255 was incorrectly attributed to HR 6053 by                 
                         McAlister et al. (1983); that measure, with a factor of two correction  McA1983 
                         in the separation, actually belongs to HR 6560.                                 
16147+3352   STF2032     sig CrB = 17 CrB.                                                               
                         A is a Delta Scuti-type variable, TZ CrB, and double-lined                      
                         spectroscopic binary, P = 1.14d. It exhibits atmospheric and coronal            
                         activity, and radio flares.                                                     
                         Aa,Ab: Raghavan et al. orbit based on based on RV data plus long-       Rag2009 
                         baseline interferometry from CHARA Array. Adopted e=omega=0.0. Derive           
                         masses 1.137 +/- 0.037 and 1.090 +/- 0.036 Msun, radii 1.244 +/- 0.050          
                         and 1.244 +/- 0.050 Rsun.                                                       
                         AB: H 1   3.                                                            MEv2010 
                         AB: Parabolic orbit.  sigma = areal constant in the true orbit =        Zag1936 
                         0.1226 arcsec^2/yr. q = periastron distance in the true orbit = 2".221          
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AC: STT 538.                                                                    
                         AD and BD: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         AD : the lost STT 305AD is also this pair.                              Dam2016b
                         AE: A distant star (L 1490-24, mag. about 12.5, 13') has common proper          
                         motion                                                                  Kam1939b
             YSC 152     Ea,Eb: astrom. orb. Hei1990d P=52yr e=0.36 a=111mas => q=0.26           Tok2014d
16148-2114   J  1590     SWR 198. CPM pair                                                       Skf2004 
16150+6040   LDS1434     NLTT 42399/42396                                                        Chm2004 
16150+1203   BPM 654     [PM2000] 1163547 + [PM2000] 1163484.                                    Gvr2010 
16151+1343   LDS4654     NLTT 42339/42341                                                        Chm2004 
16151-5622   EGN  17     Single epoch, but galactic coordinates (b=-4.0deg) suggest B, C, and D          
                         are all background stars. E and F are unbound.                          Egn2007 
16152-0046   HJ 1290     BAL3017.                                                                        
                         Rectilinear solution by Friedman et al. (2012).                         USN2012a
16153+1435   BPM 655     [PM2000] 1163786 + [PM2000] 1163790.                                    Gvr2010 
16154-4916   BRT 882     CPD-48@8267.                                                                    
16154-6341   R   274     del TrA. Innes doesn't see close pair, suggests Russell measure         I__1902b
                         should be ~140deg, ~30"                                                 R__1871 
16156-0822   BUP 165     18 Sco.                                                                         
16156-2243   GRE   4     IRAS 16126-2235 = PDS 82 = VV Sco.                                      Gre1992 
16156-5059   CPO 461     CPD-50@9115.                                                                    
16156-6321   RST 822     Aka ALD  89.                                                            Dam2014 
16158+1348   BPM 656     [PM2000] 1164308 + [PM2000] 1164264.                                    Gvr2010 
16160+1126   ENG  56     15 Her                                                                          
16160+0721   STF2026     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.22 +/- 0.24, 1.39, and 0.65 Msun, respectively.  Mlk2012 
16165-0659   RST3939     A is the Algol-type system SW Oph.                                              
16167+6714   ENG  57     B component is variable EW Dra.                                                 
                         aka LDS2372 = SHY  80.                                                          
                         Bayesian analysis by Shaya & Olling (2011) indicates very               Shy2011 
                         high (near 100%) probability pair is physical.                                  
16167+2909   SHJ 223     ups CrB = 18 CrB. Possible spectroscopic binary.                                
                         AB: H 5  37.                                                            MEv2010 
                         CD: Additional notes may be found in van den Bos (1963).                B__1963a
16171+5516   BLA   3     Also known as CR Dra.                                                           
                         Gl 616.2 = CR Dra. Tamazian et al. (2008) orbit yields a dynamical      Tam2008 
                         parallax for this flare star of 58.43 +/0 0.7 mas, as well as a system          
                         mass 1.76 +/- 0.13 Msun.                                                        
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.72 +/- 0.13, 1.09, and 0.47 Msun, respectively.             Mlk2012 
16172+3111   LDS6311     NLTT 42438/42437                                                        Chm2004 
16173-2437   WAJ   1     A is a spectroscopic binary with a period of 17.94d. B is an eclipsing  WaJ2018 
                         binary with a period of 4.54d. The catalog dm values are out of eclipse         
                         values. Those during eclipse are 0.44+/-0.04 (J band) and 0.58+/-0.01           
                         Kp band.                                                                        
16174-3449   HJ 4840     SWR 199. CPM pair                                                       Skf2004 
16175+7545   LDS1844     eta UMi = 21 UMi                                                                
16179-0724   A    23     STF3102.                                                                        
16183-0442   BU 1452     eps Oph = 2 Oph = Yed Posterior                                                 
16186-2518   LUH   2     DENIS-P J161833.2-251750                                                        
                         Based on probability arguments, Luhman (2005) concludes this pair in    Luh2005 
                         the Upper Scorpius OB association is likely a physical binary system,           
                         with spectral types about M5 and masses ~0.15 Msun for each component.          
16188+6147   LDS2376     NLTT 42554/42555                                                        Chm2004 
16189+1803   BPM 657     [PM2000] 1167560 + [PM2000] 1167503.                                    Gvr2010 
16189-5754   EVS   1     Primary is Cepheid S Nor.                                                       
                         Masses are 6.3 and 2.4 Msun. Estimated period = 8660y,                          
                         a = 790au = 0.87".                                                      Evs2013 
16193-4240   SEE 271     lam Nor. Direct motion. Half a revolution.                                      
                         Primary not round.                                                      Hln1966 
16195+0314   ART   3     Artigau et al. (2011) derive spectral types T2.5 +/- 0.5 and T4.0 +/-           
                         0.5. Distance is estimated at 22 +/- 3 pc. Total mass <0.12 Msun.       Art2011 
16195-3054   BSO  12     AB + TOK 410Ba,Bb: HIP 79980 and HIP 79979 form a 23" CPM pair AB               
                         where the F6III primary is slightly evolved, while the G1/G2 secondary          
                         is closer to the main sequence, but still above it. The Hipparcos               
                         parallax of B, -4.7mas, is obviously wrong, so we assume the parallax           
                         of the primary, 20.7mas. The RV(B) is variable (GCS), and we resolve            
                         it into a 40mas pair with an estimated period on the order of 1yr. The          
                         pair moved by 10deg in a month. Binary motion is the likely cause of            
                         the incorrect Hipparcos parallax.                                       Tok2015c
16195-4004   OCC9213     Additional solutions of 131.6 deg, 7.2 mas & 259.3 deg, 7.2 mas.        OCC2020a
16197+4619   BU 1198     tau Her = 22 Her. A is a Beta CMa-type variable.                        Bu_1894 
16197-2146   BOY  23     DENIS-P J161939.8-214535                                                        
16195-3054   TOK 410     Ba,Bb: SB?                                                              Tok2014d
16198+2647   A   225     Systemic mass is estimated at 2.6 +/- 1.3 Msun, assuming an Hipparcos           
                         parallax of 7.65 +/- 1.26 mas. According to Heintz (1982), the          Hei1982c
                         computed dynamical mass suggests an evolved pair.                       Doc2008a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.47 +/- 1.14, 2.36, and 0.95 Msun, respectively.             Mlk2012 
16198-5009   HJ 4841     gam 2 Nor                                                                       
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2014).                         USN2014a
16199+2238   OSO  68     G168-042. Neither is a common proper motion pair, based on color and            
                         comparison with POSS2 red plates                                        Oso2004 
16201-2003   SHJ 225     H V 134. B is BD-19@4358.                                                       
                         H 5 134.                                                                MEv2010 
16201-6958   DON 788     NO TrA, Algol-type eclipsing binary, P = 5.66215 d.                     Zas2011 
16202-3734   LDS6312     RSS 401. LDS 555                                                                
16203+3659   HIP  80042  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Carquillat & Ginestet (1996).                                           Crq1996 
16203+5111   OSO  69     G202-043. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates.                                                  Oso2004 
16203-7842   BSO  22     del 1 Aps. An irregular variable. B is CPD-78@1093, spectrum K3III              
16204+5223   FAR  45     Primary is white dwarf WD 1619+525.                                     Far2006 
16204-0416   WIL   3     Gl 618.1                                                                        
                         CPM pair; data from 2MASS. Wilson et al. (2001) derive spectral type    Wil2001 
                         of L2.5V and mass 60-70 Mjup for the companion.                                 
16205-2007   B  1808     AB: Mt. Wilson spectral types B9,A0n.                                           
             SHJ 226     AB,C: H 4 124.                                                          MEv2010 
16206+4535   HDS2309     Cvetkovic et al. (2014) derive spectral types F2 and  K0, masses 1.56           
                         and 0.90 Msun. Dynamical parallax is 11.58 +/- 0.95 mas.                Cve2014 
16211+1131   BPM 658     [PM2000] 1169724 + [PM2000] 1169722.                                    Gvr2010 
16212+4118   FAR  46     Primary is white dwarf WD 1619+414.                                     Far2006 
16212+2259   HU  481     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.03 +/- 0.64, 2.12, and 1.10 Msun, respectively.             Mlk2012 
16212-2536   BLM   4     A: sig Sco = 20 Sco = Alniyat. This system is comprised of a 33d SB             
                         components Aa1 and Aa2), with a third component (Ab) at 0.4" from the           
                         spectroscopic pair and a fourth component at about 20".  The primary            
                         is a beta Cep variable.                                                         
                         North et al. derive masses of 18.4 +/- 5.4 and 11.9 +/- 3.1 Msun for    Nor2007 
                         the two spectroscopic components; spectral types for the primary and            
                         secondary appear to be B1III and B1V, and the age is about 10Myr.               
                         1976.471: These measurements cannot be that of the SB system observed           
                         by Struve et al. (1961 ApJ, 133, 509) but probably relates to the more          
                         distant companion observed by Nather et al (1974) at a lunar            Chu1974 
                         occultation.  The system is also a photometric variable.                BLM1978 
             sig Sco     Aa1,Aa2: Malkov et al. (2012) derive dynamical, photometric, and                
                         spectroscopic masses 56.66 +/- 21.97, 15.64, 16.98 Msun, respectively.  Mlk2012 
             H 4 121     H IV 121.                                                                       
16215-5306   RSS  30     This previously uncataloged double star was a Hipparcos double entry            
                         system. The first measure is determined from the individual positions           
                         listed by Rousseau et al.                                               Rss1996 
16216+1339   BPM 659     [PM2000] 1170287 + [PM2000] 1170334.                                    Gvr2010 
16218+0113   STF2041     STT 308.                                                                        
16219+1909   SHJ 227     gam Her = 20 Her. A is a spectroscopic binary. B is BD+19@2085.                 
                         STTA144 = H 5  19.                                                              
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
16219+1327   GC 22009    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin (1978).                                                         Grf1978c
16219-2043   IRE  14     Primary is a T-Tauri type variable. Kraus et al. (2014) estimate the            
                         mass of the companion at 16 +/- 1 Mjup .                                KsA2014 
                         Lachapelle et al. (2015) derive the following properties:                       
                           Spectral type             | K7    +/- 0.5  | M9    +/- 0.5                    
                           Teff (K)                  | 4200  +/- 150  | 2300  +/- 100                    
                           log(L/Lsun)               | -0.42 +/- 0.08 | -3.01 +/- 0.09                   
                           Mass (Msun) (5 Myr)       | 0.9   +/- 0.1  | 0.015 +/- 0.001                  
                           Mass (Msun) (10 Myr)      | 0.9   +/- 0.1  | 0.016 +/- 0.001                  
                           Distance (pc)             | 145   +/- 14   | ...                              
                           Projected separation (AU) |                | 320   +/- 30             Lch2015 
16221+3054   CHR  53     xi CrB = 19 CrB                                                                 
16221+1214   FAR  18     B = white dwarf WD1619+123, DA2.9, mass 0.55 Msun. Mass(A)=1.05         Hbg2013 
                         (Holberg et al. 2013)                                                   Tok2014d
16221+0102   LUH  11     GJ 3952 + 2MASS J16220644+0101156.                                              
16224+3348   STFA 29     A: nu 1 CrB = 20 CrB                                                            
                         B: nu 2 CrB = 21 CrB                                                            
             H 6  18     BD: H VI 18. Confusion in early component identification led to the BD  Nsn2015 
                         pair being mislabeled as BE.                                                    
16224-2405   CLO   8     Oph 16222-2405                                                                  
                         Spectral types M9 +/- 0.5 and M9.5 +/- 0.5, luminosities -2.77 +/-              
                         0.10 and -2.96 +/- 0.10 log Lsun, masses 17 +4/-5 and 14 +6/-5 Mjup,            
                         age 5 +/- 2 Myr. Conclude that form CPM pair and are currently bound,           
                         although may become unbound in the future.                              Clo2007 
                         From optical and near-IR spectroscopy derive spectral types  M7.25 +/-          
                         0.25 and M8.75 +/- 0.25, and estimate masses of 0.055 and 0.019 Msun.           
                         Conclude are not a planetary-mass binary.                               Luh2007b
16225-0415   BU 1453     B is BD-03@3930. Measured in connection with STF 3103rej.                       
16225-4355   DUN 200     B is CD-43@10723.                                                               
                         Identified as optical and linear solution also published.               LRR2022c
16226+3819   PKO  15     Also known as COU1280.                                                          
16226+2624   BRT3311     Originally published as BRT 170.                                        Brt1928 
16229+3815   KU   53     HJL 235.                                                                HJL1986 
16229+3803   COU1281     Docobo et al. (2010) derive a dynamic parallax of 20.67 +/- 0.40 mas    Doc2010h
                         and a total mass of 1.60 +/- 0.10 Msun.                                         
16229+3220   H 5  38     H V 38. STTA145.                                                                
16229-1701   CHR  54     First detected as an occultation binary by Rad1982c.                            
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.81 +/- 2.27, 3.07, and 1.45 Msun, respectively.             Mlk2012 
16231+3650   LDS4662     NLTT 42674/42677                                                        Chm2004 
16231+1350   STF2040     H 2  88.                                                                MEv2010 
16234+3844   LDS4664     NLTT 42686/42680                                                        Chm2004 
                         SLW1175.                                                                        
16235-1309   HO  402     1m error in IDS led to similar error in WDS designation.                        
16236-2402   CLO   9     Oph 16233-2402                                                                  
                         Spectral types M5 +/- 3 and M5.5 +/- 3, luminosities -1.18 +/- 0.10             
                         and -1.47 +/- 0.10 log Lsun, masses ~100 and 73 Mjup, age ~1 Myr.               
                         Conclude they are member of the Ophiuchus cloud and form a CPM pair.    Clo2007 
16238+6142   CHR 138     The 3rd component cannot be associated with A for certain at this time          
16239-4637   RST 843     CPD-46@7946.                                                                    
16240+6131   STT 312     eta Dra = 14 Dra = Athebyne. Both A and B are variable suspects.                
                         Mk III Limb-darkened diameter  3.68  +/- 0.05  mas.                     MkT2001 
                         Mk III Limb-darkened diameter  3.722 +/- 0.071 mas.                     MkT2003 
                         NPOI Limb-darkened diameter    3.34  +/- 0.07  mas.                     NOI2001b
                         NPOI Limb-darkened diameter 3.470 +/- 0.010 mas, Sp = G8III,            NOI2018 
                         R = 10.53 +/- 0.04 \rsun, Teff = 5060 +/- 64 K, L = 65.6 +/- 3.3 \lsun,         
                         M = 2.45 +/- 0.10 \msun, Age = 0.65 +/- 0.10 Gyr.                               
16240+4822   BUP 168     Distance 1128.4".                                                               
             HEN   1     Discovery designation is per Todd Henry 03/02/98.                               
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Marcy & Moore (1989).                                                   Mrc1989 
                         GJ 623. Martinache et al. derive dynamical masses of 0.371 +/- 0.015    Llo2007 
                         and 0.115 +/- 0.0023 Msun. Based on IR colors and velocities, they              
                         conclude that the pair is of low metallicity and probably old disk              
                         population. Models do not fit all the dtaa adequately, however.                 
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 0.50 +/- 0.02, 0.58, and 0.40 Msun, respectively.  Mlk2012 
16240-3912   RAG   8     Also known as WGN   1.                                                          
                         GJ 620.1. Secondary is white dwarf WD 1620-391.                         Far2005b
                         A is exoplanet host, P=528d                                             Tok2014d
                         SHY  81. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
16241+5835   STI2339     LDS2379.                                                                        
16243-5921   SHY 284     AB: HIP  80365 + HIP  79958.                                                    
16244+2140   OSO  70     G169-004. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
16245-3734   B   868     Measures uncertain, too close.                                                  
                         1991.3926: This system may have made a very close periastron passage            
                         between the times of our 1989.3 observation (rho = 0".039) and this             
                         one, although unfortunately the system was not observed in 1990.                
16247-2942   H N  39     A is possible SB and astrometric binary. Jones et al. (2002) do not     CPS2002b
                         detect SB with precise RV.                                              Tok2014d
16248+3925   HU 1276     Magnitude 13.0, assigned to companion in ADS, is much too faint.        B__1963b
16248+3217   FAR  47     Primary is white dwarf WD 1622+323.                                     Far2006 
16249+5218   LDS4670     NLTT 42778/42776                                                        Chm2004 
16249-3755   HJ 4852     Spectrum: A3/5II/III.                                                           
16249-5205   BRT 891     CPD-51@9487.                                                                    
16250-2456   REP  35     Barsony et al. (2003) note additional 2MASS source at 10" separation.   Bny2003 
16252+1437   LDS4668     NLTT 42740/42738                                                        Chm2004 
16253-4909   CVN  27     Ba,Bb : Many early measures attributed to TOK  50Aa,Ab. Corrected               
                         here.                                                                   Tok2018h
16254+3724   CHR  55     25 Her. A component is a shell star. Strong a/e-correlation, more               
                         speckle observations are needed.                                                
                         Docobo et al. (2010) derive a dynamic parallax of 12.63 +/- 0.30 mas    Doc2010h
                         and a total mass of 3.87 +/- 0.71 Msun.                                         
16254+1402   BU  625     ome Her = 24 Her = Cujam. A is variable.                                        
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: Additional notes may be found in van den Bos (1958).                B__1958 
                         AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
16255+7123   TOK 676     A is SB2, P=149.958d                                                    Tok2014d
16256-2327   H 2  19     H II 19. rho Oph = 5 Oph. Spectrum of D: B3/4V. Based on the long term          
                         double star measures, the Tycho-2 proper motion is not correct. The     VlF2007 
                         proper motion from the new Hipparcos reduction is given here.                   
16257+2657   GIC 140     NLTT 42766/42773                                                        Chm2004 
16258+0542   STF2042     Rectilinear solution by Friedman et al. (2011).                         USN2011a
16260+1322   BRT1283     BRT1942.                                                                Brt1936b
16261-3459   HWE  83     HO  404.                                                                        
16263+0211   LDS5851     AB: LDS6313.                                                                    
             BAL1915     AC: Baillaud suspected both A and C to be closer pairs.                         
16264+5047   BEM9021     Rectilinear solution by Hartkopf & Mason (2015).                        WSI2015 
16264-2421   ZNN   1     Confusion between IR sources HBC 638 = DoAr 24 and HBC 639 = DoAr24E            
                         led to some of these measures being given the discoverer designation            
                         16253-2420GHE  22.  All measures have now been assigned to ZNN   1,             
                         however.                                                                        
16265-2527   RAT   6     Primary is emission-line star ROXs 12 = WSB 32. Kraus et al. (2014)             
                         estimate mass of the companion at 16 +/- 4 Mjup.                        KsA2014 
16266-5158   RST 845     CPD-51@9530.                                                                    
16267-2421   REP  40     Barsony et al. (2003) note additional 2MASS source at 9".3 separation.  Bny2003 
16268+1203   A  1859     Too close 1935 to 1945. Apparently a change of quadrant at this time.           
16268-1423   GIC 141     G153-051/G153-052.                                                              
16268-4803   I    93     Includes V374 Nor, a W UMa type eclipsing binary, P = 2.72950d.         Zas2012 
16269-2421   YLW   1     IR sources in rho Oph cloud. A component = GY 143,                              
                         B = GY 157 = VSSG 7, C = GY 171.                                                
             DCH  73     BD: Originally 16269-2420 DCH  73, but primary found to be B component          
                         of 16269-2421 YLW   1AB.                                                        
             DCH  75     CE: Originally 16270-2422 DCH  75, but primary found to be C component          
                         of 16269-2421 YLW   1AC.                                                        
16270-2436   YLW   4     IR sources in rho Oph cloud. A component = WL 14 = GY 172,                      
                         B = WL 21 = GY 164, C = WL 22 = GY 174.                                         
16270-2446   HER  17     IR sources in rho Oph cloud. AB = HBC 262 = YLW   3AB.                  Her1962 
                         A component = GY 168 = SR 24N, B = GY 167 = SR 24S.                             
                         1949.: Noted as double, apparently seen on plate from Ross "Atlas of            
                         the Milky Way"                                                                  
16270-5412   LDS 559     LDS5850.                                                                        
16271+4255   BU  815     See ADS for rectangular measures.                                       A__1932a
16271-2426   YLW  10     AB: IR sources in rho Oph cloud. A component = GY 203.                          
             ALO   5     Ba,Bb: Originally 16273-2427ALO   5AB, but primary found to be B                
                         component of 16271-2426 YLW  10AB.                                              
                         BD: Originally 16273-2427ALO   5AB,C.                                           
16272-4733   HJ 4853     eps Nor. The primary is a spectroscopic binary. B is CD-47@10764.               
16272-6722   WFC 176     SWR 200. CPM pair                                                       Skf2004 
16273-2429   YLW  12     AB pair a.k.a. ALO   6.                                                         
16273-2439   YLW  11     AB: IR sources in rho Oph cloud. WL 20.                                         
                         WL 20E, WL 20W, and WL 20S are the A, B, and C components,                      
             RES   1     respectively. Astrometry based on average of data taken through three           
             RIE   1     BC: filters: 7900+/-760, 10300+/-1010, 12500+/-1160nm. See Ressler et   Res2001 
                         al. (2001) for fluxes of all components at various wavelengths, as              
                         well as extensive discussion of system. Duplicity of WL 20 was                  
                         discovered by Rieke et al (1989), although no astrometric measurements  Rie1989 
                         are listed in their paper.                                                      
16273-2442   CST   8     AB: IR sources in rho Oph cloud.                                                
                         A component = V2247 Oph = SR 12 = HBC 263 = ROX 21.                             
                         1986.4: 0.45 - 0.18  flux ratio in J band, 1.00 - 0.35 in H band        Smn1987 
             ALO   7     AC: Kuzuhara et al. (2011) confirm that the C component is a member of  Kuz2011 
                         the rho Oph star-forming region and is physically associated with the           
                         AB pair. The mass of C is estimated at 14 +7/-8 Mjup.                           
16274-3729   B   872     Primary is eclipsing binary V1055 Sco (period 0.36367 day).             Zas2010 
16275-2427   YLW  17     IR sources in rho Oph cloud. A component = GY 273 = VSSG 18,                    
                         B component = GY 279 = VSSG 17.                                                 
16275-2431   DCH  77     Primary is young stellar object VSSG 25 = WL 13. The B component is a           
                         young brown dwarf, mass ~30 Mjup.                                       ShC2011 
16275-2427   SHC   1     AC: Primary is the young stellar object VSSG 18 = ISO-Oph 44. The               
                         companion shows IR excess, and is identified as a young low-mass                
                         companion candidate.                                                    ShC2011 
16275-2440   TER   2     Aa,Ab: IRAS 16244-2432. A.k.a. ALO  11.                                         
16277-6857   SWR 201     CPM pair                                                                Skf2004 
16278-0104   GIC 142     AB = G017-016/G017-015.                                                         
                         HIP 80630. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
16278-0822   RST3949     Aa,Ab: ups Oph = 3 Oph. A is a spectroscopic binary, P = 27.2d.                 
                         Appears to be a common proper motion pair associated with STF1998       Tok2010b
                         (16044-1122).                                                                   
             SHY 287     AB: HIP  80628 + HIP  78983.                                                    
16280+1533   JNN 279     G 138-33. Estimated age 1000-10000 Myr; masses 0.45 +/- 0.13 and 0.23           
                         +/- 0.06 Msun; a ~13.6 au.                                              Jnn2014 
16280-6403   DUN 201     iot TrA. A is a spectroscopic binary.                                           
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
16281+1326   BPM 660     [PM2000] 1177313 + [PM2000] 1177384.                                    Gvr2010 
16283+4441   OSO  71     G180-058. Not a common proper motion pair                               Oso2004 
16283-1613   RST3950     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.25 +/- 1.10, 2.60, and 1.20 Msun, respectively.             Mlk2012 
16284-6108   B  1812     Alternative spectra: F5+A2.                                                     
16286+4153   bet Her     = Kornephoros. Malkov et al. (2012) derive dynamical, photometric, and          
                         spectroscopic masses of 14.65 +/- 4.09, 5.90, and 2.57 Msun,            Mlk2012 
                         respectively.                                                                   
16288-0808   STF2048     B is a spectroscopic binary.                                                    
16289+5636   ARG 102     B is BD+56@1894.                                                                
16289+1825   STF2052     AB: NLTT 42901/42900                                                    Chm2004 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.63 +/- 0.88, 1.67, and 0.79 Msun, respectively.  Mlk2012 
16291+0015   GRV 929     B component is +00 3532.                                                        
16292+7805   FAR  48     Primary is white dwarf WD 1631+781.                                     Far2006 
                         Like 2MASS J10162867-0520320, this is a previously known system with a          
                         white dwarf component (Farihi et al. 2010). Hence, we do not include    Far2010 
                         this system in the binary fraction statistics.                          Jnn2012 
16292+3114   BRT3313     BRT2618. BD+31 2857.  DM number erroneously entered as BD+31 2837.      Brt1942 
16293-5133   SEE 279     SIN  92AB                                                                       
             SIN  92     Corrected from 16254-5125 07/10/2002.                                           
16294+1036   STF2051     H 3 102.                                                                MEv2010 
16294-2626   GNT   1     alp Sco = 21 Sco = Antares. The primary is variable: irregular or               
                         semiregular with a trace of a 5.8 yr period.                            B__1953a
                         Mk III Limb-darkened diameter 39.759 +/- 0.399 mas.                     MkT2003 
                         Duplicity of Antares discovered by a lunar occultation observed at              
                         Vienna by Johann Tobias Burg 13 April 1819.                             Dnh2015 
                         Composite spectrum; M1.5Iab-Ib+B4Ve.                                            
                         Parabolic orbit by Hopmann (1957).                                      Hop1957b
                         sigma = areal constant in the true orbit = 0.04448 arcsec^2/yr                  
                         q = periastron distance in the true orbit = 2".2055                             
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
16295-7142   SWR 202     CPM pair                                                                Skf2004 
16299+1107   BPM 661     [PM2000] 1179186 + [PM2000] 1179077.                                    Gvr2010 
16301+3353   HU 1173     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.77 +/- 1.59, 3.32, and 0.95 Msun, respectively.             Mlk2012 
16302+2129   BLA   4     Aa,Ab: bet Her = 27 Her = Kornephoros. A is a long-period spectroscopic         
                         binary, resolved by speckle interferometry.                                     
                         A measure on 1980.4820 was incorrectly attributed to HR 6148 by                 
                         1975.6273: SB, companion is red.                                        Bla1977a
                         McAlister et al. (1983); it actually belongs to HD 163640.              McA1983 
                         1983.3043: Only the asymmetry of the ACF peak indicate that the star            
                         is double.  The system has been resolved in the red (Blazit et al.      Bla1977a
                         1977) with the 200-inch telescope.                                      Bag1984a
                         Mk III Limb-darkened diameter  3.51  +/- 0.05  mas.                     MkT2001 
                         Mk III Limb-darkened diameter  3.462 +/- 0.035 mas.                     MkT2003 
                         NPOI Limb-darkened diameter    3.53  +/- 0.08  mas.                     NOI2001b
                         NPOI Limb-darkened diameter 3.472 +/- 0.008 mas, Sp = G5III,            NOI2018 
                         R = 15.92 +/- 0.40 \rsun, Teff = 5092 +/- 64 K,                                 
                         L = 153.7 +/-10.8 \lsun, M = 2.91 +/- 0.11 \msun,                               
                         Age = 0.42 +/- 0.06 Gyr.                                                        
                         Single line SB; all positive observations have been made in the red             
                         spectral range (wavelength > 6000 Angstroms) so delta m probably is >3          
                         in the visible.                                                         Bnu1986 
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Plummer (1908).                                                         Plu1908 
                         P, T, and e adopted from 1908 spectroscopic orbit for Pan et al.        MkT1992e
                         (1992) combined solution.                                                       
16303+1522   GIC 143     G138-035/G138-036. DUN 201                                                      
             RAO 349     pa error = 356 deg.                                                     RAO2020b
16305-1433   STF3104     C component = A component of 16306-1432 LDS4673.                                
16306-1432   LDS4673     A component = C component of 16305-1433 STF3104.                                
16308-2820   HJ 4859     LDS 562.                                                                        
                         SWR 203. CPM pair. Dwarfs, not giants                                   Skf2004 
16309+0159   STF2055     lam Oph = Marfik. RV possibly variable.                                         
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Spectral types and masses of components assigned by ten Brummelaar et   TtB2000 
                         al. (2000) based on adaptive optics.                                            
                         AB: H 1  83.                                                            MEv2010 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 6.77 +/- 1.92, 4.88, and 4.48 Msun, respectively.  Mlk2012 
16310+2359   SHY 704     HIP  80886 + HIP  81875.                                                        
16310-4629   HJ 4857     Spectrum of C may be M.                                                         
16311-1637   BU  626     phi Oph = 8 Oph                                                                 
16311-2405   REP  41     A: HBC 644 = Haro 1-14c  PMS binary resolved by Keck Interferometer.            
                         The orbit is based on V^2 measurements obtained 2004-2007, plus radial          
                         velocity data from 2001-2007. The best-fit masses and distance from             
                         statistical analysis of the orbital solutions are 0.961 +0.265/-0.083           
                         and 0.326 +0.092/-0.023 Msun; 111 +19/-18 pc. A comparison with                 
                         evolutionary tracks suggests an age of 3-4 Myr.                         Sfr2008 
                         A combined solution yielded masses 0.905 +/- 0.043 and 0.308 +/- 0.011          
                         Msun, plus a distance of 95.55 +/- 9 pc.                                LeB2014 
16312-2434   RAT  18     BC: Initially added as 16313-2433 RAT  18AB, but the primary is also            
                         the B component of 16312-2434 BOV  56.                                          
                         BC: Spectroscopy indicates the C component is a cool substellar object          
                         (M8-L0; Teff = 1800-2600K), not a background dwarf star, with spectral          
                         shape indicative of young, low surface gravity planet-mass companions.          
                         Currie et al. (2014) estimate the mass of the companion at 6-15 Mjup.           
                         They find some evidence of an additional companion at ~0.5" of roughly          
                         equal brightness, although preliminary analysis indicates it is a               
                         background object.                                                      Cre2014 
                         BC: Primary is the T-Tauri type variable ROXs 42B. Kraus et al. (2014)          
                         estimate the mass of the companion at 10 +/- 4 Mjup. The D component            
                         is a background star.                                                   KsA2014 
16313-2430   BRT3030     BOV  57.                                                                        
16313-4757   CPO  68     LDS 561.                                                                        
16314-6513   R   280     Also known as HDS2333.                                                          
16315+7237   HDS2334     CHARA Array Limb-darkened diameter  1.024 +/- 0.029 mas.                CIA2010c
                         R = 15.84 +/- 1.08 \rsun, L = 98.9 +/- 12.2 \lsun,                              
                         Teff = 4572 +/- 158 K.                                                          
16315+0818   SHJ 233     STTA146. B is BD+08@3216.  Also known as FRK   8. The equality of               
                         these two systems was noted by Arnold.                                  Arn2004a
                         HJL 237.                                                                HJL1986 
                         SHY 705. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
16315-2425   REP  42     Barsony et al. (2003) note an additional faint 2MASS source at 7.33"    Bny2003 
                         from the A component.                                                           
                         IRAS 16284-2418 = PDS 85 = DoAr 43.                                     Gre1992 
16315-3901   HDS2335     Aka DSG  19.                                                                    
16316+7056   CBL 159     AC: Originally 16317+7056 CBL 159, but B component was found to be              
                         primary of 16316+7056 TDS 819. Systems merged, with quadrant flip.              
16316+5746   YNG   1     ADS notes that Burnham measured position of Dreyer 6187                 Bu_1906 
                         from AB: 1910.34, 180.2deg, 207".1 (n=3).                               A__1932a
16316+2307   POU3231     Rectilinear solution by Friedman et al. (2011).                         USN2011a
16316+1917   STF2057     C is A of STF 2058.                                                             
                         AB: HJL 238.                                                            HJL1986 
16316+0526   STF2056     H 2  23.                                                                Bu_1906 
16318+4536   STF2063     H 4  62.                                                                MEv2010 
16318-0216   A   693     Only elements P, T, and a have been amended from the orbit of           Sta1978c
                         Heintz (1963).                                                          Hei1963a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.89 +/- 3.44, 2.97, and 1.20 Msun, respectively.             Mlk2012 
16319-2456   HDP   2     HCH   7.                                                                        
16322-2440   BNY   3     A component = ROXs 47A.                                                         
16325-0834   OSO  72     G153-064. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
16326+4007   STT 313     Called G5II comp? by Bidelman.                                                  
16329+0315   GC 22255    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Johnson & Mayor (1986). The use of the orbital elements derived by      Jhn1986 
                         Latham et al. (1992) produces a poorer fit.                             Lat1992 
             DSG   7     Horch et al. (2015) refer to the 280mas pair as AB; however, the B              
                         component has already been assigned to the wide CPM companion of                
                         Lepine (2007).  Since they refer to the 15mas as Aa,Ab the wide DSG     Lep2007 
                         pair is assigned components Aa and Ac.                                          
                         Aa,Ab: For the Horch et al. combined solution, spectroscopic elements   Lat2002 
                         are fixed to those of Latham et al. (2002). Assigned spectral types             
                         for Aa, Ab, and Ac are K1V, K6V, and M5V; derived masses for Aa and Ab          
                         are  0.77 and 0.64 Msun.                                                Hor2015 
                         Teff : A = 5252 K, B = 3400 K, C = 5500 K.                              Cab2018b
                         Mass (\msun) : Aa = 0.77, Ab = 0.64, Ac = 0.15, B = 0.40, C = 0.54.             
16329-4656   CPO 480     A is variable.                                                                  
16331-6054   DUN 203     B is CPD-60@6558.                                                               
16335+4604   GRV1122     BVD 247. WDS designation of GRV pair changed to that of BVD pair, as            
                         it was in better agreement with the precise coordinates.                        
16335+3030   BU  818     A is a spectroscopic binary.                                                    
16339-4807   I  1588     Slightly variable. Central star of planetary nebula.                            
             SNA  40     Aa,Ab: This magnetic O star is resolved by PIONIER as an equal-                 
                         brightness pair with rho=20.3mas. Adopting a parallax of 2.35 +/- 0.78          
                         mas (van Leeuwen 2007), it would correspond to a projected separation   VlF2007 
                         of 40au. While the object is flagged as SB in Simbad, a spectroscopic           
                         study by Naze et al. (2008, 2010) reported no evidence of binarity.     Naz2008 
                         The faint companion detected at 3.3" may correspond to the 2.9" B       Naz2010 
                         companion reported by Mason et al. (1998) if the latter is a high       Msn1998a
                         proper motion (possible foreground) object.                             Sna2014 
16341+4226   LAB   4     sig Her = 35 Her. Double-lined spectrum.                                        
                         1972.28, 1973.45: Two of the three observations yielded fringes in the          
                         Fourier transform which were quite different; this is difficult to              
                         reconcile with the 50-yr period estimated from Kepler's law.            Lab1974 
                         This object was misidentified as tau Her by McAlister (1978). The       McA1978c
                         observation on 1976.2963 which was reported there as yielding a                 
                         negative result does indeed show duplicity, as was correctly reported           
                         by McAlister later that year. The negative result reported in the       McA1978b
                         earlier paper for 1976.2991 is spurious.                                        
                         1977.1781: This is a previously unpublished photographic measure.               
                         1977.3284: Theta incorrectly given as 5.7 deg by McAlister & Hendry     McA1982b
                         (1982); correct value published by McAlister et al. (1989)              McA1989 
                         1983.3098: Very poor atmospheric conditions.                            Bag1984a
                         Measure of 1988.258 made by MAPPIT.                                     Naj1989 
                         Martin et al. (1998) derive component masses 3.036 +/- 0.714 and                
                         1.498 +/- 0.519 Msun.                                                   Mig1998 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 6.05 +/- 1.14, 6.07, and 2.57 Msun, respectively.             Mlk2012 
16341-4403   SNA  41AB   The primary is mu Nor, a pulsating variable star.                       Sna2014 
16345+5709   LDS1436     NLTT 43148/43149                                                        Chm2004 
                         Primary is the eclipsing binary CM Dra, P = 1.26839 day.                Zas2010 
16348+0430   SKF  13     Aka BAL2878.                                                                    
16348-0412   LMP  14     G017-025 = G153-067. We do not confirm the Lampens pair using our data  Pws1993 
                         and images from the Digitized Sky Surveys.  G017-027 is located at              
                         19.616' and PA=36.48 deg. Both G153-067 and G017-027 share a common     GJ_1988 
                         proper motion, according to Gliese & Jahreiss.                          Oso2004 
             GIC 144     AB = G017-025/G017-027 = GJ 629.2AB.                                            
                         A: Ren & Fu (2013) calculated an astrometric orbit, combining           Ren2013 
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Latham et al. (2002).                                                   Lat2002 
16349-6810   HJ 4855     SWR 205. CPM pair                                                       Skf2004 
16352+3721   PAR   2     A is the Mira-type system W Her.                                                
16354+1703   WEB   6     A is a spectroscopic binary. B is BD+17@3054.                                   
16354-5805   HU 1605     Spectrum of B may be M.                                                         
16355+5403   GRV1221     SLW1186.                                                                        
16357+1442   BPM 662     [PM2000] 1185680 + [PM2000] 1185654.                                    Gvr2010 
16360-0025   TOK 175     HIP 81274. NOMAD: PM(B)=(-51,+56), V(B)=14.47. PM(A)=(-29,+49).         Tok2011a
16362+5255   STF2078     A: 17 Dra. Common proper motion with 16 Dra.                                    
                         Aka H 1   4 = SHJ 236.                                                          
             STFA 30     C: 16 Dra                                                                       
                         AC: STTA147.                                                                    
16362+1526   BPM 663     [PM2000] 1186243 + [PM2000] 1186378.                                    Gvr2010 
16364+3057   PRB   5     Primary is NLTT 43194, secondary is WD 1637+33 = NLTT NLTT 43310.               
                         Possible CPM pair, according to Probst (1983).                          Prb1983 
16364-0219   BUP 171     CHARA Array Limb-darkened diameter of A :                               CIA2012f
                         R =  0.7591 +/- 0.0122 \rsun, L =  0.41945 +/-0.00422 \lsun,                    
                         Teff = 5337 +/-  41 K, M = 0.821 \msun.                                         
16364-4252   SNA  42     The primary is V918 Sco, an ellipsoidal variable star. Object is a              
                         9.81d SB2 (Rauw et al. 2001, A&A 368, 212)                              Sna2014 
             HD 149404   The classification is from the UV tomographic analysis of               Pny1996a
                         Penny (1996).                                                           Msn1998a
16366+6948   BU  953     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.79 +/- 1.93, 2.62, and 1.35 Msun, respectively.  Mlk2012 
             BU  953     AB,D: HJL1091. LDS1851.                                                         
             BAZ   7     Da,Db: Also known as HDS2348.                                                   
16367+1225   BPM 664     [PM2000] 1186731 + [PM2000] 1186654.                                    Gvr2010 
16370+1213   BPM 665     [PM2000] 1187143 + [PM2000] 1187170.                                    Gvr2010 
16371+3119   OSO  73     G169-021. Not a common proper motion pair, based on color and                   
                         comparison with POSS2 red plates.                                       Oso2004 
16372-1034   zet Oph     The line profile variations of this nonradial pulsator are most                 
                         recently described in Kambe et al. (1997 ApJ 481, 406). Van Rensbergen          
                         et al. (1996 A&A 305, 825) discuss the runaway trajectory of the star.  Msn1998a
16372-4708   SNA  43     The 2.7" companion is undetected in H-band, indicating a strongly               
                         reddened, possibly background object.                                   Sna2014 
16374-5347   HJ 4863     SWR 208.                                                                        
16374-6133   HJ 4862     B is a spectroscopic binary with P ~ 225d.                              Tok2022e
16375+1341   GIC 145     G138-046/G138-047.                                                              
16376-4053   EGN  18     All 5 companion candidates (B, C, D, E, F) are background stars.        Egn2007 
16378-6339   RST 866     Also known as TDT  11                                                           
16382+2244   POU3235     Rectilinear solution by Hurowitz et al. (2014).                         USN2014a
16384+7020   STF2099     LDS1852.                                                                        
16384+3514   COU 985     A premature orbit has been computed.                                            
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 5.46 +/- 4.84, 2.16, and 0.79 Msun, respectively.             Mlk2012 
16384-2514   HJ 1292     AB: Also a 12.5 at 129deg, 14.5" from B.                                B__1951a
16385+0640   RAO 354     pa error = 354 deg.                                                     RAO2020b
16385-5728   TOK  51     Aa,Ab: A = V841 Ara, var. BY-Dra type.                                  Tok2014d
             RST 869     AB: B is DOZ1, mass 0.65 Msun. Mass(A)=0.85 (Holberg et al. 2013)       Hbg2013 
16386+3820   STF2080     See ADS for rectangular measures.                                               
16387+4856   STF2082     42 Her.                                                                         
                         H 4  63.                                                                MEv2010 
16391+7256   LDS1853     NLTT 43405/43404.                                                               
16391+6042   STF2092     A is the Algol-type system WW Dra, P = 4.63d.                                   
16391-3713   FIN 340     AB. 1991.3926: From its discovery in 1954 through the mid-1960's, this          
                         system closed from 0".14 to 0".10 and increased in theta from 147 deg           
                         to 172 deg.  It is impossible to determine from this single speckle             
                         measure whether the pair has gone through periastron and flipped                
                         quadrant, but this should become obvious within the next couple of              
                         observations.                                                                   
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.37 +/- 0.76, 4.60, and 2.40 Msun, respectively.  Mlk2012 
16391-5815   EGN  19     AB pair unbound. Single epoch, optical/physical nature of AC unknown.   Egn2007 
16394+4642   GIC 133     LDS6315. G202-066/G202-067. NLTT 43322/43323. A typographical error             
                         led to this pair being originally entered in the WDS as 15396+4637.             
16394-0306   BU  820     A 1923 measure by Gauchet was inadvertently attributed to 22390+1850    Gau1925 
                         and listed as new companion GAU 19AC. Error noted by Thorel (2012).     Thr2012 
16397-4921   HJ 4873     BD: Initially entered incorrectly as AD pair.                                   
16397-5700   HJ 4866     A is the Algol-type system R Ara.                                               
16398+4226   LAW  26     AB: SLW1192.                                                                    
16403-2354   HDS2365     Barsony et al. (2003) note additional 2MASS source at 13".1 separation  Bny2003 
             FGL   4     AC: Discovered using Chandra ACIS-I (Advanced CCD Imaging Spectrometer          
                         Imager) by Feigelson et al. (2003).                                     Fgl2003 
16406+0413   CHR  56     Aa,Ab: 37 Her. B is 36 Her, BD+04@3234.                                         
                         This system, first announced by McAlister and recalled in a later       McA1984b
                         McAlister paper after repeated attempts at confirmation, has been       McA1993 
                         restored. While perhaps still spurious, the subsequent confirmation or          
                         suspected duplicity (by another technique) makes the discovery                  
                         measurement somewhat more probable.                                             
             STFA 31     STTA148.                                                                        
                         AB: SHY 707. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AB: H 5  72.                                                            MEv2010 
16407+1044   BPMA 49     [PM2000] 1191425 + [PM2000] 1191452.                                    Gvr2010 
16407-0009   STF2076     AB: HJL 239.                                                            HJL1986 
16409+2157   HO  553     A is SB                                                                 Tok2014d
16409-4550   DON 806     CPD-45@8073.                                                                    
16413+3136   STF2084     zet Her = 40 Her.                                                               
                         Mk III Limb-darkened diameter  2.33  +/- 0.05  mas.                     MkT2001 
                         Mk III Limb-darkened diameter  2.367 +/- 0.051 mas.                     MkT2003 
                         NPOI Limb-darkened diameter    2.49  +/- 0.09  mas.                     NOI2001b
                         Berman (1941) has discussed the RV's.                                   Ber1941 
                         A subsystem with a period of about 12 yr has repeatedly been                    
                         suspected (cf Baize 1976), and the third component has now been         Baz1976 
                         detected by infrared speckle interferometry.                            Mcy1983 
                         No evidence in the speckle or Hipparcos data for the large-amplitude            
                         third-body orbit given by Baize.                                                
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Giant primary according to isochrone fit.                               Sod1999 
                         H 1  36.                                                                MEv2010 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.44 +/- 1.31, 2.12, and 1.26 Msun, respectively.             Mlk2012 
16413-4846   MLO   8     AB: A is a spectroscopic binary.                                                
             SNA   1     Aa,Ab: The system includes the tightly-bound Aa1,Aa2 pair [primary              
                         O3V((f*))-3.5V((f+)), secondary O5.5-6V] with P=2.67d, i=49 +/- 5deg,           
                         e=0. The tertary Ab (spectral type O6.5-7V) orbits the inner pair with          
                         period 3000-5500d.                                                      Sbe2013 
                         Aa,Ab: Component masses are estimated at 62.2 +/- 10.0 Msun for Aa1,            
                         39.5 +/- 6.3 for Aa2, and 33 +/- 12 for Ab.                             Sna2013 
                         Aa,Ab: This is a hierarchical triple system known from spectroscopy             
                         (Mahy et al. 2012, A&A 540, A97). The outer pair (Aa,Ab) was first              
                         resolved in the course of the PIONIER survey (Sana et al. 2013). We     Sna2013 
                         clearly detect the known 1.6" AB pair, but other components of this             
                         system are outside our field of investigation.                          Sna2014 
             DUN 206     AC: C has variable velocity.                                                    
                         The C component was observed and appeared to be single.                 Msn1998a
             SNA   1     Ca,Cb: PIONIER marginally resolved the Aa,Ab pair at 0.95mas. It                
                         probably corresponds to the 183d SB2 reported by Gamen et al. (2008,            
                         RevMexAA 33, 54), assuming pi=0.5mas and M = 20Msun (Hohle et al.               
                         2010, AN 331, 349).                                                     Sna2014 
16415-4359   PRB   6     Primary is GJ 634, secondary is WD 1626-41 = LTT 6576. Possible CPM             
                         pair, according to Probst (1983).                                       Prb1983 
16416+4428   L    14     Another measure: 1911.70, 119.1@, 19.96". Error in one of the                   
                         distances?                                                                      
16416+3053   GC 22471    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
16416+2655   CHR  57     39 Her. A short-period (2.3d) double-lined spectroscopic binary.                
                         Hence a triple.                                                                 
                         This system, first announced by McAlister and recalled in a later       McA1984b
                         McAlister paper after repeated attempts at confirmation, has been       McA1993 
                         restored. While perhaps still spurious, the subsequent confirmation or          
                         suspected duplicity (by another technique) makes the discovery                  
                         measurement somewhat more probable.                                             
16416+1513   USN   2     LHS 3236 = WD1639+153 = NLTT 43383.                                             
                         Harris et al. (2013) derive a distance of 30.86 +/- 0.25pc (parallax            
                         31.67 +/- 0.25mas), which is larger than the spectroscopically-                 
                         determined distance of 21-22pc and yields a nearly normal mass for              
                         this pair. LHS 3236 is a double-degenerate binary, which  eliminates            
                         the possibility of a substellar companion. Temperature of both                  
                         components are 7700 +/- 60K. Astrometric analysis favors a DA+DA pair,          
                         with mass sum 1.84 +/- 0.03 Msun, while spectroscopic analysis                  
                         suggests DA + DC, with a combined mass of 1.68 +/- 0.05 Msun. Age of            
                         the system is about 3.3 Gyr.                                            USN2013b
                         The Harris et al. orbit finds a photocentric semi-major axis of 4.37            
                         +/- 0.25 mas. Matches to 2008 and 2010 Keck AO observations yield               
                         dilution factors of 23.0 and 22.2, respectively. The mean of these two          
                         dilution factors gives the semimajor axis value of 98.76 +/- 5.65 mas           
                         listed in the Sixth Orbit Catalog.                                              
16417+3628   BU 1199     In globular cluster NGC 6205 = M13. Identification of pair uncertain.           
16419+1618   BPM 666     [PM2000] 1192855 + [PM2000] 1192899.                                    Gvr2010 
16419-1955   GC 22453    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
16419-4723   COO 199     B is CD-47@10952.                                                               
16420+7353   MLR 198     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.15 +/- 3.22, 3.47, and 2.09 Msun, respectively.             Mlk2012 
16425-3705   R   283     Premature orbits have been computed.                                            
16427+1336   STF2083     HJL 240.                                                                HJL1986 
                         A typographical error in van den Bergh (1958) resulted in a supposed    Bgh1958 
                         AC pair (103deg, 49") being added to the WDS.                                   
16429+3855   STF2093     eta Her = 44 Her. Aa in direction of C and 2/3 the distance.                    
                         NPOI Limb-darkened diameter 2.42 +/- 0.07 mas,                          NOI1999 
                         R =  8.9 +/- 0.3 \rsun.                                                         
                         Fainter than C.                                                                 
                         Smyth suspected a close companion to A (1842.53, 150deg, 0".3) but      Smy1844 
                         this pair has never been confirmed by larger telescopes.                        
16430-5611   COO 200     SWR 209. CPM pair                                                       Skf2004 
16431-7731   HJ 4858     bet Aps                                                                         
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
16434+1354   BPM 667     [PM2000] 1194757 + [PM2000] 1194704.                                    Gvr2010 
16435+2043   STTA149     B is BD+20@3324.                                                                
                         Pair appears in an appendix list, not part of discoverer's regular              
                         numbering sequence.                                                             
16436+0637   H 5 127     H V 127. B is BD+06@3281.                                                       
16438-5330   FIN 251     Composite-like spectrum: B8/9(IV)+F/G.                                          
                         AB: 1990.3467, 1990.3495, 1991.3926: CHR 147 Aa,Ab, the close third             
                         component to this system discovered in 1989.3, was unfortunately not            
                         confirmed in these observations.                                                
16439+4329   D    15     Errors for orbit of Alzner (2007) provided by author (private comm.)    Alz2007 
                         With the Hipparcos parallax of 36.59 +/- 2.13 mas, the Alzner solution          
                         yields a mass sum of 1.31Msun, which matches well a pair of K5 main             
                         sequence stars.                                                                 
                         Additional notes may be found in Duruy (1944) and                       Dur1944d
                         Worley (1956).                                                          Wor1956b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.27 +/- 0.16, 1.52, and 0.65 Msun, respectively.             Mlk2012 
16439+2638   BRT3315     Originally published as BRT 171.                                        Brt1928 
16439-0032   GLP  12     Proper motion according to Ebell possibly that of A?                    Ebl1895 
             J   448     AB: Additional notes may be found in Jonckheere (1949).                 J__1949b
16439-4107   CPO  70     B is CD-40@10649.                                                               
16440+4459   KZA 110     AC: Error in RA caused resulting incorrect measure by Kazeza.           KZA1984 
16444-4224   DUN 207     B is CD-42@11486.                                                               
16445+2348   AG  205     In BDS. Removed from ADS, reinserted into IDS, removed from WDS.                
                         Re-entered here. A is the planetary nebula NGC 6210.                    Skf2014b
                         For the record, measures are as follows:                                        
                16445+2348       1908.72     271.9     .     123.87                      1.0   6 Bu_1913 
                16445+2348       1992.70     271.6     .     123.52                      1.2   1 Skf2014b
                16445+2348       1998.8     :271.2     .    :123.38                      1.3   1 Skf2014b
                16445+2348       2000.0      271.5     .     123.67           609  70    0.2   1 Skf2014b
                16445+2348       2000.0      271.4     .     123.60           609  70    0.2   1 Skf2014b
                16445+2348       2003.194    271.5     .     123.61                      2.5   1 Skf2014b
                16445+2348       2010.5      271.3     .     123.43                      0.4   1 Skf2014b
16446+7145   MLR 182     Aa,Ab SB1, P=403.9d                                                     Tok2014d
             UC 3219     AB: Candidate on Tokovinin list, now reconfirmed as CPM.                Tok2013c
16447+0220   STF2088     BC: Also known as GRV 936.                                                      
16447-4900   HJ 4882     CPD-48@8773. B is CPD-48@8774.                                                  
16448+6647   AG  206     LDS2398.                                                                        
16448-3912   DAW  71     CPD-38@6519.                                                                    
16450+2928   COU 490     1983.3125: Very poor atmospheric conditions.                            Bag1984a
                         Systemic mass is estimated at 3.1 +/- 0.5 Msun, assuming a dynamical            
                         parallax of 6.94 +/- 0.10 mas. Couteau (1999) gives a spectral type of  Cou1999b
                         F5 for both components. However, 2MASS IR colors suggest a somewhat             
                         earlier spectral type F0-F2V. Adopting an F2V spectral type yields a            
                         rough spectroscopic parallax of 6.92 mas, in good agreement with the            
                         derived dynamical value.                                                Doc2008a
16450+0605   STT 585     41 Her. Alternate spectral type G3IV is more reasonable,                        
                         considering the magnitude difference.                                           
                         B has variable radial velocity.                                                 
                         AB: SHY 289. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: HJL 241.                                                            HJL1986 
                         AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
16451+2821   STF2095     H 1  79.                                                                MEv2010 
16453+5647   MCA  44     A spectroscopic triple with the wider pair, presumably, now resolved            
                         by speckle interferometry.                                                      
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Abt (1965).                                                             AbH1965 
                         1983.3099: Elongated ACF peak suggests that the object may be double            
                         with theta ~ 104 deg, rho ~ 0".024.  HR 6237 is in fact a 1386-day SB.  Bag1984a
16454+5027   ES 2653     Also known as SLE  16.                                                          
16454-7150   B  2392     AB + TOK 411Aa,Ab: HIP 82032 is located in a crowded field, so the              
                         new faint Ab companion found here at 1".3 could be optical. The star            
                         was observed because of its suspected variable RV (GCS), but the newly          
                         found companion, even if physical, is too distant to explain this               
                         variability. Another visual companion B at 11".5 (AB = B 2392) is               
                         optical, as evidenced by its fast relative motion. The star is on the           
                         HARPS exo-planet program.                                               Tok2015c
16457+3000   STF2098     C is BD+30@2872.                                                                
16458+0835   SHJ 239     43 Her.                                                                         
                         AB: H 6 116.                                                            MEv2010 
16458+0103   J  1331     +17s, +2' from BD+01 3298.                                              J__1952 
16458-0046   A  1141     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.86 +/- 1.83, 2.51, and 1.10 Msun, respectively.             Mlk2012 
                         Ma,Mb = 1.138 +/- 0.025, 1.116 +/- 0.024 \msun.                         GmJ2022 
16459-3205   PRO 136     SWR 211.                                                                        
16460+8202   HDO 143     eps UMi = 22 UMi. A is an Algol-type system.                                    
                         Duplicity suspected by Peirce in 1868.11 - this is probably not the     Pei1882 
                         wide pair identified as HDO 143.                                                
16461+5021   SKF 244     HD 234344 + 2MASS J16461148+5019456. Baron et al. (2015) estimate               
                         spectral types K7 and M7.5 +/- 0.5, distances 31.6 +/-0.9 and                   
                         36 +14/-3 pc, masses 0.705-0.751 and 0.087-0.095 Msun.                  BFr2015 
16465+4759   ES 1089     AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
16465+1647   BPM 668     [PM2000] 1198515 + [PM2000] 1198531.                                    Gvr2010 
16466-4137   SNA  44     Aa,Ab: We resolve this SB2 system with rho=1.85mas. The object was              
                         reported by RV variable by Conti et al. (1977) and pre-publication OWN  Cti1977 
                         results indicate a 199d orbital period.                                 Sna2014 
16466-4705   B  1825     AB: Leep (1978 ApJ 225, 165) suggests that this star is a single-lined          
                         binary with a period of approximately 5 d.                              Msn1998a
16467-6707   HDO 257     Variable.                                                                       
16469+0210   BAL1925     J 3295 is identical                                                     Hei1980a
16472+0204   STF2096     19 Oph. A is a spectroscopic binary.                                            
                         AB: H 4 123.                                                            MEv2010 
16472-3301   PRO 138     May be CD-32@12016.                                                             
16475+1329   BPM 669     [PM2000] 1199736 + [PM2000] 1199717.                                    Gvr2010 
16475-1945   LDS 571     NLTT 43547/43553                                                        Chm2004 
16475-4819   DUN 211     B is CD-48@11174.                                                               
16478+0515   BUP 174     45 Her. A is a spectroscopic binary, and is variable.                           
16479-4058   SIN  98     The BC and BD pairs were incorrectly identified as AC and AD.                   
16482-3653   DUN 209     B is CD-36@10973.                                                               
16483-2845   HJ 4887     B is CD-28@12420.                                                               
16484+5903   PRB   7     Primary is GJ 1206 = WD 1647+59 = DN Dra = NLTT 43637, secondary is             
                         NLTT 43992. Possible CPM pair, according to Probst (1983).              Prb1983 
16485+5807   RAO 357     pa error = 356 deg.                                                     RAO2020b
16486+5508   STF2108     NLTT 43634/43633                                                        Chm2004 
16486+1353   BPM 670     [PM2000] 1201056 + [PM2000] 1201085.                                    Gvr2010 
16487-5526   DUN 210     B is CPD-55@7693.                                                               
16487-6902   WFC 179     alp TrA = Atria.                                                                
16489+5930   STT 316     B is BD+59@1762.                                                                
16489+2259   POU3246     Rectilinear solution by Friedman et al. (2011).                         USN2011a
16491+0609   FAR  49     Primary is white dwarf WD 1646+062.                                     Far2006 
16492+4559   BU  627     52 Her. Star A (mag 4.9, A3p) is an Alpha CVn-type variable, V637 Her.  Fat1941 
                         The magnitudes of B and C are quite uncertain.                                  
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
16494-2354   LDS6316     NLTT 43594/43595                                                        Chm2004 
16496+4758   GRV1257     Both A and B have approximately the same radial velocity.               Grv2019b
16496+1316   STF2103     The AC and AD components which were with STF2113 are actually                   
                         associated with this system.                                                    
16498-5902   RST5067     eta Ara                                                                         
16499-6025   B  2393     Spectral type of A may be A.                                                    
16500-4137   HD 151564   NGC 6231 #302. Classification is by Schild et al. (1969 ApJ 156, 609);          
                         however, Garrison et al. (1977 ApJS 35, 111) assign a type B0.5V.       Msn1998a
16501+0443   BUP 175     B is BD+04@3264.                                                                
16501-1526   TOK 176     HIP 82384. Small PM(A)=(-1,+26). NOMAD: PM(B)=(-6,-38). B remains of            
                         uncertain status.                                                       Tok2011a
16502+2219   OSO  74     G169-028. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates.                                                  Oso2004 
16504-0147   OSO  75     G017-037. Not a common proper motion pair, based on astrometry and              
                         color.                                                                  Oso2004 
16506-5003   COO 201     Composite spectrum; A5III+F7III.                                                
16511+4631   LDS4699     NLTT 43702/43703                                                        Chm2004 
16512+3555   JNN 110     LP 276-29.                                                                      
16512+1122   BPM 671     [PM2000] 1204376 + [PM2000] 1204449.                                    Gvr2010 
16514+0113   STT 315     21 Oph. Premature orbits have been calculated.                                  
16518+2840   STF2107     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.70 +/- 1.48, 2.16, and 1.35 Msun, respectively.  Mlk2012 
                         The faint star C (83") may be physical.                                         
16519-2120   RSS 419     CPD-21@6225                                                                     
16519-3803   SHT  72AB   mu 1 Sco = Xamidimura.                                                          
             SKF2608AD   D component is mu 2 Sco.                                                        
16523-3801   RIZ  19     mu 2 Sco = Pipirima                                                             
16528+5048   LDS 4700    Probable match to Luyten's pair gives theta value ~240 deg rather than  Luy1978 
                         than his value of 290. His value has been changed, on the assumption            
                         it was a typographical error.                                                   
16528-4147   HD 152003   NGC 6231 #306. Constant radial velocity is also found by Levato et al.  Lev1988 
                         (1988).                                                                 Msn1998a
16530+4424   STT 317     AC: C is BD+44@2622.                                                            
16530+3142   BU 1454     53 Her.                                                                         
16532-4759   B  2398     Spectral type K?                                                                
16533+4725   CHR  58     CHARA Array Limb-darkened diameter  1.440 +/- 0.004 mas.                CIA2010c
                         R = 31.16 +/- 2.82 \rsun, L = 270.5 +/- 34.4 \lsun,                             
                         Teff = 4193 +/- 142 K.                                                          
                         This frequently unresolved double may be 2119d spectroscopic binary.    Grf2017e
16534-2025   WSI  86     Astrometric binary; dm 2.9 mag, period ~ 10y? Accelerated pm.           Tok2012b
16535-4207   SNA  48     The companion is marginally resolved at 0.77mas, but with large                 
                         uncertainties. The object is reported as SB1 by Williams et al. (2013,          
                         AJ 145, 29), with P=13.8d, but Sota et al. (2014, ApJS 211, 10)                 
                         obtained a different period. We therefore have to wait for                      
                         clarification before one can decide if PIONIER resolved the                     
                         spectroscopic companion or whether HD 152247 is a triple system.        Sna2014 
16535-6049   B  2396     Spectral type M?                                                                
16539-4153   SNA  49     The primary is V1292 Sco, a detached Algol-type eclipsing binary and    Sna2006 
                         SB2, with a period of 4.2d (Sana et al. 2006; Sana 2009). All of the    Sna2009 
                         resolved companions are too wide to be the spectroscopic companion.     Sna2014 
16540+1010   DCH 120     iot Oph = 25 Oph.                                                               
16540-4143   SNA  50     The primary is V1294 Sco, a detached Algol-type eclipsing binary and    Sna2008b
                         SB2, with a period of 5.8d (Sana et al. 2008).                          Sna2014 
             HD 152218   NGC 6231 #2.  The classification is from the UV tomographic analysis    Pny1993 
                         of Penny et al. (1993). A new orbit by Stickland et al. (1997) yields   Stc1997 
                         a period of 5.604 d.                                                    Msn1998a
16540-4148   B  1833     This O star is the F component of a multiple system. The A component            
             SEE 293     is HD 152234 which is a B0.5Ia star (Hoffleit & Warren 1991). The       Hof1991 
             SEE 294     AB system is a 0".5 binary which was observed and resolved 3 times.     Msn1998a
             SNA  51     Aa,Ab: HD 152234 is a 125d SB2 (Sana et al. 2012); the spectroscopic    Sna2012 
                         companion is marginally resolved in PIONIER observations with                   
                         rho=0.9+/-1.9mas and dH=1.37.                                           Sna2014 
             SNA  51     Fa,Fb: We resolve for the first time this long-period SB2 discussed in  Sna2008a
                         Sana et al. (2008a, 2012)                                               Sna2014 
16540-4655   HJ 4890     B is CD-46@11089.                                                               
16541+0826   HEI 857     HDS2391. Erroneously indicated as a new double by Hipparcos.                    
16541-4105   SNA  52     Aa,Ab: This is a 470d hierarchical triple system (Chini et al. 2012)    Cii2012 
                         that PIONIER resolves with a separation of 3mas. A combined                     
                         spectroscopic/interferometric solution is presented in Nasseri et al.           
                         (2014, A&A in press.)                                                   Sna2014 
16541-4151   SEE 295     Aka ARY 122AB.                                                          Dam2017h
16541-4144   SEE 296     Primary is V1294 Sco, Algol-type eclipsing binary, period 5.604d.       Zas2013 
16542-4139   SNA  53     Aa,Ab: We resolve the long-period SB2 discussed in Sana et al. (2012).  Sna2012 
                         Four new faint wide companions are also detected in the NACO FOV.       Sna2014 
16542-4150   SEE 297     Light and velocity variable. Spectroscopic binary, P=5.97d.                     
             CHR 252     Aa,Ab: Classification is from the UV tomographic analysis of Penny      Pny1996a
                         (1996).  The Aa,Ab pair was resolved in 2 of 4 observations.            Msn1998a
16542-4151   SNA  54     Ba,Bb: This is a known SB2 with a period of 5.7d (Sana et al. 2007).    Sna2007 
                         We are lacking PIONIER data on this system, but resolved a third                
                         component at 43mas.                                                     Sna2014 
             HD 152249   NGC 6231 #293. We found a possible binary companion at a separation of          
                         0".06 which needs confirmation.                                         Msn1998a
16543-4149   B  1834     CD: C is a Wolf-Rayet system, spectrum WC7+O5.                                  
                         The classification is from Seggewiss (1974 A&A 31, 211).                Msn1998a
16543-4151   CPO 500     CPD-41@7737.                                                                    
                         Aka ARY 122CD.                                                          Dam2017h
16545-4153   SEE 302     BRT 933.                                                                Brt1933 
16546-4125   HD 152333   NGC 6231 #325. The classification is from Schild et al. (1969 ApJ 156,          
                         609).                                                                   Msn1998a
16549-4031   HD 152405   NGC 6231 #326. Raboud (1996 A&A 315, 384) finds the star to be a                
                         radial velocity variable.                                               Msn1998a
16550+2544   STF2110     56 Her. A is a spectroscopic binary.                                            
16550-4109   I   576     Classification of the B component is by                                 Msn1998a
                         Lindroos (1985).                                                        Lnd1985 
                         The image rotator was in an unknown state, so two possible theta                
                         values are listed for the 2001.4030 observation - one for zenith up             
                         and one for north up.                                                   Trn2008 
16551-4205   HD 152424   Fullerton (1990) finds radial velocity variations that suggest an       Ful1990 
                         orbit with a period greater than a month. Levato et al. (1988) also     Lev1988 
                         find radial velocity  variations.                                       Msn1998a
16551-4459   CHR 253     This Of star is assigned to the field in the LSC, but Turner (1979 A&A          
                         76, 350) argues that it belongs to an anonymous OB association related          
                         to the Cepheid, KQ Sco.                                                 Msn1998a
16554+1826   BU  954     54 Her.                                                                         
16544-4150   SNA  55     Reported as a broad-line fast rotator with line profile variability             
                         (Sana at al. 2008b) and as SB2, we detected two visual companions at    Sna2008b
                         1.1 and 3.4". The 7.3" AB companion reported by Mason et al. (1998)     Msn1998a
                         may lie outside our FOV.  See further discussion by Sana et al. (2014)  Sna2014 
16545-4148   SNA  56     Aa,Ab: We resolve the 3700d SB2 discussed in Sana et al. (2008; 2012),  Sna2008a
                         and detect two additional wide companions in the NACO FOV.              Sna2014 
16549-4031   SNA  57     SB with orbital period 25.5d (Sota et al. 2014, ApJS 211, 10). While            
                         we are lacking PIONIER measurements, NACO/SAM resolved a third                  
                         companion at 54mas.                                                     Sna2014 
16555-0820   KUI  75     Wolf 630.                                                                       
                         A flare star, V1054 Oph. One of the shortest orbital period, for pairs          
                         resolved first by naked eye. The radial velocities indicate a third             
                         component. The intrinsically very faint star VB 8 (mag 17, 220") is             
                         also a member of the system. There is strong evidence that it is an             
                         astrometric binary. The pair is the large proper-motion star Wolf 630           
                         which forms a multiple system with the SB Wolf 629 (mag.11.7, 72",              
                         sdM4) and VBS 8 (mag. about 18, 221"), so  the whole system is probably         
                         a septuple. There is strong evidence that VBS 8 is an astrometric               
                         binary. Eggen suggests that the group is part of a large moving         Egg1965b
                         cluster. He has observed an UV flare on Wolf 630.  According to                 
                         Soderhjelm, the mass ratio and mass sum require the secondary to be a   Sod1999 
                         closer SB. Unuseable HIP solution.                                              
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Combined solution from astrometry, spectroscopy, and parallax.                  
                         Solution yields mass and orbital parallax determination.                Sgr2000 
                         Martin et al. (1998) derive component masses 0.327 +/- 0.045 and                
                         0.558 +/- 0.047 Msun.                                                   Mig1998 
                         KUI  75AB is also known as Gliese 644 (B is an SB1 star), component C           
                         is Gliese 643, also an SB1 star. Component F is VB 8 and is also known          
                         as Gliese 644C.                                                         Och2010 
                         Also known as GJ 644, this is a well-known and much studied triple              
                         system (e.g. Segransan et al. 2000), of which we resolve the wider AB   Sgr2000 
                         pair (the secondary is a spectroscopic binary with a 3 day period). In          
                         addition, there are two much wider components known to share a common           
                         proper motion with GJ 644, making the system a likely quintuple. Since          
                         there are so many existing astrometric points of the AB pair in the             
                         literature, we do not give an extensive list in Table 4, but rather             
                         refer the reader to Segransan et al., where there is a full orbital             
                         analysis of the close triple system.                                    Jnn2012 
                         Using the parallax from van Leeuwen and the mass ratio from Harris,     VlF2007 
                         Strand & Worley individual masses of Ma = 0.487 +/- 0.054 \msun and     Hrs1963 
                         Mb = 0.487 +/- 0.054 \msun are determined for these components.         Msn2023 
             LDS 573     AC: While VB 8 itself is single in the AstraLux sensitivity range, it           
                         is part of a higher-order multiple (at least triple, possibly                   
                         quintuple) as a known 1500 au companion (C component) to GJ 644, which  Jnn2012 
                         was discussed in our Janson et al. (2012) study.                        Jnn2014 
             WNO  55     AF: GJ 644 A+C. CPM pair.                                               Mkr2008 
             SLE 687     AB,E: Rectilinear solution by Mason & Hartkopf (2016).                  Msn2016a
16555-2134   BU  241     Rectilinear solution by Rica & Zirm (2012).                             FMR2012i
16555-3929   SEE 308     CPD-39@7160.                                                                    
16555-4522   I  1111     BRT 936.                                                                Brt1933 
16557+3511   RUC   9     Multiple system including contact binary V829 Her. Pribulla & Rucinski          
                         (2006) estimate the mass of the contact pair at 1.800 Msun and the      Pbl2006 
                         minimum mass of the wider component at 0.30 Msun.                               
                         Spectral type of resolved companion estimated at K1V.                   Ruc2007 
16560+6508   19 Dra      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Abt & Levy (1976).                                                      AbH1976 
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by Abt &              
                         Levy (1976). They derived component masses 1.18 and 0.42 Msun and an    AbH1976 
                         estimated semimajor axis of 21.19 mas.                                  Ren2013 
                         SB1. Combined orbit including RV data and Hipparcos Intermediate                
                         Astrometric data. Semimajor axis derived from photocentric a0 plus              
                         stellar evolutionary model. Derived properties for A and B:                     
                         M/Msun = 1.04 + 0.37, L/Lsun = 2.02 + 0.02, dm = 5.01 mag,                      
                         log age = 9.67.                                                         WaX2015b
16561-1401   LDS4703     NLTT 43811/43813                                                        Chm2004 
16563+7417   A  1144     Possible acceleration. Caused by inner subsystem?                       Tok2014d
16563-4030   HD 152622   NGC 6231 #333. The classification is from Garrison et al. (1977 ApJS            
                         35, 111).                                                               Msn1998a
16563-4040   HDS2394     AB: Fullerton (1990) discovered the short-period spectroscopic          Ful1990 
                         variation, and subsequently Wiemker (1992 MS Thesis, Georgia State              
                         Univ.) showed that the spectral variations are best explained by the            
                         superposition of a stronger stationary component and a moving                   
                         component. Thus, the speckle resolution of this system (aka, CHR 210)           
                         makes clear that this is (at least) a triple consisting of a short-             
                         period SB1 and a distant O star.                                        Msn1998a
             SNA  60     Aa,Ab: Mason et al. (1998, 2009) reported a companion at 23mas, but     Msn1998a
                         with position angles differing by 180deg. Our NACO/SAM data confirm     Msn2009 
                         that the correct theta value is 307deg. A closer Aa,Ab companion is             
                         found in the PIONIER data, with rho=28.24mas; a third AC companion is           
                         detected by NACO at 1.5". The primary is also reported as a 3.9d SB1    Ful1990 
                         by Fullerton (1990).                                                    Sna2014 
             HDS 2394    AB + SNA  60Aa,Ab + SNA 60AC: HIP 82876 is a distant O7V star. The              
                         0".26 AB pair was measured among other neglected binaries. We found             
                         another faint companion C at 1".46. The star has an extensive                   
                         literature, including multiplicity surveys with speckle interferometry          
                         and RV (Chini et al. 2012). Owing to the large distance, no detectable  Cii2012 
                         orbital motion is expected. Indeed, the AB pair was measured with               
                         HRCam in 2008.5 at the same position as it is now. Those observations           
                         in the y band did not detect the companion C owing to a lower                   
                         signal-to-noise ratio.                                                  Tok2015c
16564+6502   STF2118     20 Dra. A premature orbit has been computed.                                    
                         RV not variable. Some observations belonging to the neighboring SB              
                         19 Dra have been published under 20 Dra.                                        
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: H 1  19.                                                            MEv2010 
                         AB: Additional notes may be found in Burnham (1894).                    Bu_1894 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.18 +/- 1.20, 2.50, and 1.45 Msun, respectively.  Mlk2012 
16564-4104   CPO 501     Spectral type K?                                                                
16565+5558   LDS4710     NLTT 43902/43903                                                        Chm2004 
16566+5711   A  1143     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.20 +/- 0.87, 2.16, and 1.05 Msun, respectively.  Mlk2012 
                         CD = BD +57 1717 (0.8") is 97" from AB and not associated with it               
                         as the proper motions differ.                                                   
16566+4505   ES 2655     B is BD+45@2469.                                                                
16568-2309   BU 1117     24 Oph.                                                                         
                         1983.4282: The original McAlister et al. (1987) observation contained   McA1987b
                         a small typo.                                                                   
16568-3906   DAM 350     AC: Aka GAT  20 with a quadrant flip.                                           
16569+2541   LDS 986     NLTT 43869/43868                                                        Chm2004 
16569-4031   CHR 254     Aa,Ab: Fullerton (1990) suggests the A component is a single-lined      Ful1990 
                         spectroscopic binary with a period of about 12 d and a semiamplitude            
                         of approximately 15 km/sec.                                                     
                         Classifications of the B, C, and D components are from Lindroos (1985)  Lnd1985 
                         Lindroos finds a distance of 2.0 kpc.                                   Msn1998a
                         See discussion of system by Sana et al. 2014).                          Sna2014 
16569-6057   COO 203     SWR 212. CPM pair                                                       Skf2004 
16570+1556   ZUC  14     Primary is white dwarf PG 1654+160 = V824 Her.                          Zuc1992 
                         Also known as SKF  53.                                                          
16571+3908   TDT 156     Aa,Ab: WDS designation changed from 16571+3906 after TDT pair was               
                         determined to be primary of HJ 2802.                                            
16573+8651   STT 340     B is BD+86@263. Same as STF2248.                                                
                         AB: HJL 246.                                                            HJL1986 
16575+1508   BPM 672     [PM2000] 1212817 + [PM2000] 1212991.                                    Gvr2010 
16579+4722   A  1874     AB: Kiselev et al. derive a family of possible orbital solutions,       Kis2009b
                         based on a range of mass sums (0.93 to 1.53 Msun) and inclinations of           
                         the pair to the plane of the sky (-32 to +32deg).                               
             STFA 32     AC: HJL 242.                                                            HJL1986 
                         AC: Kiselev et al. derive a family of possible orbital solutions,       Rmn2009 
                         based on a range of inclinations of the pair to the plane of the sky            
                         (-38 to +38deg). The mass of the AB pair is here assumed to be 1.09             
                         Msun and that of the system 1.89 Msun.                                          
                         AC: SHY  84. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
16579-3800   JSP 700     V883 Sco, Algol-type eclipsing binary, period 4.34118 d.                Zas2018 
16580+0547   GRV 942     HJL1092.                                                                HJL1986 
16582-2918   RST1919     CPD-29@4539.                                                                    
16583-3337   I  1304     A is the Cepheid RV Sco. Also a spectrum variable.                              
16584+3943   COU1289     1986.395: The separation of this partially-resolved pair was                    
                         calculated under the assumption of zero or otherwise known magnitude            
                         difference.                                                             Tok1985 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.52 +/- 0.99, 2.95, and 1.05 Msun, respectively.             Mlk2012 
16586+1527   TOK 177     HIP 83083.                                                              Tok2011a
16587+7607   STF2134     Statistically the same parallax within the errors would indicate the            
                         components are physical.                                                        
16589-3737   SEE 315     Also known as B   885. See's observation in 1897 is dubious.                    
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.78 +/- 1.45, 3.70, and 2.00 Msun, respectively.             Mlk2012 
16589-4015   SNA  61     Aa,Ab: The object is a 223d SB1 system. PIONIER observations reveal a           
                         marginal detection (2.5sigma) whose best fit corresponds to dH = 4.3            
                         +/- 1.8, rho~1.5mas. Both the large flux difference and separation are          
                         compatible with the properties of the spectroscopic companion.          Sna2014 
16591-4242   KSS   2     Primary is the Herbig B[e] star V921 Sco.                               Kss2012 
16592+2058   JNN 111     The star displays photometric variability at a 4.1 day period (Norton           
                         et al. 2007 A&A 467, 785).                                              Jnn2012 
16595+0942   BU 1298     AB: Burnham and van Biesbroeck estimate the following star 1.3 mag              
                         fainter; the components appear about equally bright to me. Variable?    B__1951a
15598+4404   JNN 106     SKF1643                                                                         
16599+0121   BAL1481     J 2111.                                                                         
16599-5920   HJ 4900     B is CPD-59@6877. A is slightly variable.                                       
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2014).                         USN2014a
17002-2459   EHR  14     Aa and Ab appear to be comoving, but B component is a background star.  Ehr2010 
                         Primary is 26 Oph.                                                              
17003+3056   ISO   3     eps Her = 58 Her. Spectroscopic binary, P = 4.02d.                              
17003-7612   GLI 232     Spectrum of B: A8/F0.                                                           
17004-4839   SEE 316     Spectrum composite; G8-K0III+G.                                                 
17005+0635   CHR  59     A spectroscopic binary.                                                         
17011+3016   FAR  19     Primary is white dwarf WD 1659+303.                                     Far2005b
17011-0413   ENG  59     30 Oph.                                                                         
17012-3812   SNA  62     A 22.4d SB1, the SB is probably too tight, so not resolved by PIONIER.          
                         Faint companions at 2.0" and 3.4" are deteced in the NACO FOV.          Sna2014 
17013-2808   B   326     Retrograde motion.                                                              
17014+3754   HJ  263     A pair of 12th magnitude stars in field.                                        
17014+3329   BU 1542     Secondary is galaxy IC 4638.                                                    
17016+1457   H 4 122     H IV 122. STF2115. A is the Alpha CVn-type variable V451 Her.                   
17017-2542   HJ 1297     J 1734.                                                                         
17018+1746   BPM 673     [PM2000] 1218945 + [PM2000] 1219146.                                    Gvr2010 
17020+4507   GRV1224     SLW1202.                                                                        
17020+0827   STF2114     A spectroscopic binary.                                                         
17021+0713   STF2113     The AC and AD components which were with this are actually associated           
                         with STF2103.                                                                   
17022-2820   TDT 186     Claimed to be spurious and while the dm is very different, the relative Tok2018c
                         astrometry is close. Measures of TOK 728 were folded in with this pair.         
17024-1154   STF3108     B is BD-11@4281.                                                                
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
17026-5504   HJ 4905     A is the semiregular variable T Ara. B is CPD-54@7976.                          
17031-5314   HDO 263     eps 2 Ara. Duplicity doubtful.                                                  
             SKF 103     Identified as a double but not measured by Wegner.                      Wgn1973 
                         AC: GJ 2125. C is DA3.2, mass 0.65. Mass(A)=1.41 (Holberg et al. 2013)  Hbg2013 
17031-5833   I   997     Composite-like spectrum: A3/5V+K0III.                                           
17033+5935   STF2128     LDS1437. Mt. Wilson spectral types K5 and M0.                                   
                         NLTT 44134/44135                                                        Chm2004 
                         HJL 243.                                                                HJL1986 
17036+6948   A  1146     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.64 +/- 1.51, 2.42, and 1.20 Msun, respectively.             Mlk2012 
17038-3809   PBL   1     V923 Sco.                                                                       
                         Orbital parallax = 16.018 +/- 0.009 mas, a = 63.941 +/- 0.041 \rsun.            
                         Ra = 2.0246 +/- 0.0026 \rsun, Ma =  1.4714 +/- 0.0014 \msun,                    
                         La = 7.67 +/- 0.18 \lsun;                                                       
                         Rb = 1.8496 +/- 0.0019 \rsun, Mb =  1.4186 +/- 0.0013 \msun,                    
                         La = 5.72 +/- 0.14 \lsun.                                               Pbl2018 
17039+3212   DAE   6     NLTT 44114 = LP 331-57                                                          
                         Daemgen et al. (2007) derive a distance of 18.0 +/- 1.2 pc, separation  Dae2007 
                         of 20.3 +/- 1.4 au, and predicted orbital period of 143 yr. Spectral            
                         types are M2.0 +/- 0.5 and M4.0 +/- 0.5; masses are 0.46 +/-0.02 and            
                         0.22 +0.09/-0.06 Msun.                                                          
17039+1941   BU  822     AB: The Brt1939a measure was initially mis-identified with 17047+1936           
                         PRY   2AB - see note for 17047+1936PRY   2 AB.  The A component is a            
                         spectroscopic binary.                                                           
                         AC: See note for 17047+1936FOX 281 AC.                                          
17039-1956   RST3065     CPD-19@6092.                                                                    
17039-3751   V884 Sco    This is a massive X-ray binary with a neutron star companion.  The      HIP1997a
                         ellipsoidal variation is portrayed in a recent Hipparcos light curve.   Msn1998a
17040-5105   DUN 212     B is CD-50@10977.                                                               
17044+1330   BPM 674     [PM2000] 1222616 + [PM2000] 1222740.                                    Gvr2010 
17046+3900   HJ 2804     AB: Rectilinear solutions by Cvetkovic (2015)                           Cve2015b
                         and Cvetkovic et al. (2016).                                            Cve2016 
17046-3800   B   890     CPD-37@6897.                                                                    
17047+1936   PRY   2     AB: The measure was initially mis-identified with the 17039+1941        Fox1925 
                         BU  822AB pair. Due to their similarity in magnitudes, position angle           
                         and separation, there may still be some identification problems in              
                         measures of these two AB systems.                                               
             FOX 281     AC: The Fox, Worley, and Comellas measures were initially               Fox1925 
                         mis-identified with the 17039+1941BU  822AC pair.  This was probably    Wor1967a
                         due to the proximity of these two systems as well as the similarity of  Cll2003 
                         the AB pairs.  The C components of these two systems are also similar           
                         in magnitude and separation, although very different in position angle          
17048+4848   HR 6363     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin (1991).                                                         Grf1991 
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Griffin (1991).                                                         Grf1991 
17048+2805   STF2120     AB: H 3  89.                                                            MEv2010 
17048-3753   HJ 4915     Spectral type K?                                                                
17050-0504   LDS 585     LDS6317. AB: Wolf 531. B is BD-04@4226. Proper motion of A -920,-1138;          
                         PM of B -915,-1130 (UCAC2). Components of this system all have                  
                         common proper motion and common radial velocity                         Egg1950 
                         HIP 83591. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AB: SHY  85. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
17050-5122   RST5596     CPD-51@10149.                                                                   
17053+5428   STF2130     mu Dra = Alrakis.                                                       Fat1941 
                         Small motions with 3 or 6 yr periods in one of the components have              
                         been suspected, but from the positional and RV observations Heintz              
                         finds no evidence for them, and points out that the O-C residuals               
                         would be increased by the hypothetical body.                                    
                         AB: H 2  13.                                                            MEv2010 
                         AB: Additional notes may be found in Simonov (1937).                    Smw1937 
                         AB: Prieur et al. (2012) derive a dynamical parallax of 36.3 mas and            
                         (using their orbital elements and the revised Hipparcos parallax of             
                         van Leeuwen 2007 A&A 474, 653) a total mass 2.8 +/- 0.5 Msun.           Pru2012 
                         AB: Low-grade SB orbit for Ba,Bb (P=2270d, K1=2.8km/s), needs           Pbx2004 
                         confirmation (SB9)                                                      Tok2014d
             BU 1088     AC: Star C (mag 13, 13.4" from the center of AB) is in slow retrograde          
                         motion; Cf. Heintz (1966). Mt. Wilson spectral types F5s.               Hei1966 
17054+1244   H 5 133     H V 133. 60 Her.                                                                
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
17054-3346   WNO   5     Spectral type of B may be M.                                                    
                         AB + TOK 413Aa,Ab: The RV of HIP 83612 varies by 52km/s (GCS). It is            
                         a very close pair with an estimated period of ~1.5yr, and the measure           
                         near the diffraction limit derived from the elongated power spectrum            
                         is tentative. The Hipparcos parallax is likely biased by the binary.            
                         The visual component B = HIP 83609 (AB = WNO 5) at 25" is optical.      Tok2015c
                         AB: Rectilinear solution by Friedman et al. (2012).                     USN2012a
17055+4803   SDK   1     Aka SLN  83.                                                                    
                         White dwarf pair = WD 1704+48 0942+24 = EGGR 576/577                    Grn1986 
17055+1033   BU  357     V2626 Oph, an Algol-type eclipsing binary, period 10.87424.             Zas2011 
17056-4106   HLN  41     CPD.                                                                            
17061+4329   WFC 186     Rectilinear solution by Friedman et al. (2012).                         USN2012a
17061-2635   EVS  29     Primary is the Cepheid BF Oph.                                          Evs2016a
17062+6438   GIC 146     LDS2730. G240-044/G240-045.                                                     
17062+1809   GRV1259     Both A and B have approximately the same radial velocity.               Grv2019b
17064-6829   SWR 214     CPM pair                                                                Skf2004 
17065-0236   STF3110     Also known as BAL 572.                                                          
17065-3527   B   894     This "field" object may belong to the "CLUST 4 " groupof Mel'nik &              
                         Efremov (1995 SvAL 21, 10). An ellipsoidal variation is present in the  HIP1997a
                         Hipparcos data with an unusually long period of 16.11 d.                Msn1998a
             SNA  63     The primary is V1074 Sco, a pulsating variable star and 16.1d EB                
                         (Mason et al. 1998). We do not detect the 2.8" companion at dI=6.3mag,  Msn1998a
                         but do report a 6.7" companion at dKs = 5.9mag.                         Sna2014 
17066+1727   BAR  42     Also known as TDT 215.                                                          
17066+0039   BU  823     AB: Orbits of AB and Ba,Bb may be almost co-planar.                     Tok2014d
17067+0747   RAO 509     WZ Oph.                                                                         
17069+2254   KUI 123     Ross 862. Aka KUI  77.                                                          
17070+0648   STF2123     LDS 988.                                                                        
                         HJL 244.                                                                HJL1986 
17073+6440   ALP  19     2MASSW J1707183+643933                                                          
                         Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
17074-0558   BUG   5     2MASS J17072343-0558249                                                         
                         Noted as binary by Burgasser et al. (2004).                             Bug2004 
                         Spectral types M9 and L3, masses 0.072-0.085 and 0.064-0.077 Msun       McE2006 
17074-3405   V455 Sco    Symbiotic star, spectral type M6.5. Fekel et al. (2008) orbit is a      Fek2008 
                         combined spectroscopic/spectropolarimetric solution. Estimated value            
                         for a" based on their a sin i, i, and estimated distance of 4.3 kpc.            
17075+3810   COU1291     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.39 +/- 0.87, 2.43, and 0.95 Msun, respectively.             Mlk2012 
17075+3557   HJ  264     C component is A component of HU 1176.                                          
17077+0722   YSC  62     GJ 1210. Estimated age 1000-10000 Myr; masses 0.21 +/- 0.06 and 0.13            
                         +/- 0.03 Msun; a ~5.6 au.                                               Jnn2014 
17080+3556   HU 1176     Van de Kamp & Moore point out that Eggen's orbit yields a mass sum      Kam1966 
                         of 52.5, 'an impossible figure'.                                        Egg1945 
                         The speckle observations now resolve the former ambiguity.                      
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Hartkopf et al. (1989).                                                 Hrt1989 
                         Calculated mass sum is 3.32 +/- 0.39 Msun. Spectral types are early A           
                         or F, but spectral class has been reported as either dwarf or giant.            
                         This total mass is more consistent with dwarf stars.                    Mut2010b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.09 +/- 0.14, 3.33, and 1.82 Msun, respectively.  Mlk2012 
17081+3549   BU 1456     This is the same as BU 1455. AC and AD were previously listed as                
                         Aa and Ab, respectively, for that pair. Identical nature noted by               
                         Friedrich Damm.                                                                 
17082-0105   A  1145     The primary is an SB; the observed RV range is 55 km/s.                         
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.23 +/- 1.93, 3.64, and 3.48 Msun, respectively.             Mlk2012 
17082-3500   SNA  64     The object is a 28.6d SB1, but the SB is too tight, so not resolved by          
                         PIONIER.                                                                Sna2014 
             HD 154643   LS 3941. This "field" object may belong to the "CLUST 4 " group of              
                         Mel'nik & Efremov (1995 SvAL 21, 10).                                           
                         The classification is from Garrison et al. (1977 ApJS 35, 111).         Msn1998a
17084+1738   BPM 675     [PM2000] 1228900 + [PM2000] 1228757.                                    Gvr2010 
17085-3639   EGN  20     System is close to galactic plane, so found to have 12 companion                
                         candidates. The B component is physical, colors are compatible with an          
                         M1.5-M4.5 spectral type and mass 0.27 +/- 0.02 Msun.  The C component           
                         is unbound, and the F component is likely unrelated as well. Single             
                         epoch observations, so nature of D, G, H, I, J, K components unknown.           
                         Nature of E and M are also inconclusive.                                Egn2007 
17088+6543   STA   1     zet Dra = 22 Dra = Aldhibah. A premature orbit has been computed.               
                         Martin et al. (1998) derive component masses 5.940 +/- 1.134 and                
                         3.645 +/- 0.770 Msun.                                                   Mig1998 
                         Uniform disk diameter  0.474 +/- 0.026 mas,                                     
                         Limb darkened diameter 0.488 +/- 0.026 mas,                                     
                         Teff = 15000 +/- 800 K based on LDD.                                            
                         Radius is 6.19 +/- 0.49 \rsun.                                          CIA2019a
17088+0911   RAO 510     V2365 Oph.                                                                      
17091-3753   B   896     CPD-37@6976.                                                                    
17093+2244   OSO  76     G170-021. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
17096+4047   MCA  45     The equinox-1900 position was incorrectly given as 17093+4054 by                
                         McAlister et al. (1983).                                                McA1983 
                         A: Ren & Fu (2013) calculated an astrometric orbit, combining           Ren2013 
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Griffin (1978).                                                         Grf1978a
17097+3021   STF2131     B is BD+30@2938.                                                                
17097-5224   R   290     Rectilinear solution by Hurowitz et al. (2014).                         USN2014a
17097-5420   HJ 4917     Rectilinear solution by Friedman et al. (2012).                         USN2012a
17098+6821   LDS1438     NLTT 44344/44348                                                        Chm2004 
17098+0804   OSO  77     G139-016. None of the components share a common proper motion, based            
                         on color and comparison with POSS2 red plates                           Oso2004 
17098-1031   TOK 414     HIP 83962 = HR 6375 has a variable RV according to the GCS, while               
                         Gorynya (2013, private communication) detected double lines. It is              
                         resolved tentatively at 33mas with dy=1.8 mag (the 5-ms exposure makes          
                         it unlikely that the asymmetry is caused by vibrations). The                    
                         separation corresponds to an orbital period on the order of 1yr, which          
                         could bias the Hipparcos parallax.  However, Eggleton & Tokovinin               
                         (2008 MNRAS 389, 869) consider the star as single. The new pair was             
                         not resolved in 2014.3, presumably it became closer.                    Tok2015c
17099-8219   HJ 4884     B is CPD-82@701.                                                                
17102+5430   STF2138     B is BD+54@1862.                                                                
                         HJL 245.                                                                HJL1986 
             SHY  89     AC: HIP  83988 + HIP  86141.                                                    
             SHY  89     BC: HIP  83996 + HIP  86141.                                                    
17104+2107   ALP  20     2MASSW J1710255+210715                                                          
                         Physical companionship to this ultracool dwarf ruled out based on i-z           
                         and z-J colors, using photometry from SDSS.                             AlP2007 
17104-1544   BU 1118     eta Oph = 35 Oph = Sabik.                                                       
                         Smyth notes an additional wide companion (1833.61, 260.5deg, 269")      Smy1844 
                         Measure of 1989.388 made by MAPPIT. This measure had an identification  Han1989 
                         error, position error, or misprint in the publication, which has been           
                         corrected. Measure of 1990.37 also made by MAPPIT.                      Rbt1991 
                         Difficult a/e correlation, needs 20 more years of speckle observations  Sod1999 
                         Spectral types and masses of components assigned by ten Brummelaar      TtB2000 
                         et al.                                                                          
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 7.05 +/- 0.51, 3.61, and 4.58 Msun, respectively.  Mlk2012 
17104-1611   FOX 198     Also known as ARA  86.                                                          
17106-1617   KNP   5     The binary at this position, formerly known as FOX 198, is actually of  Fox1915 
                         a different pair first resolved by Knipe. The FOX 198 pair, also known  Knp1965 
                         as ARA  86, is at 17104-1611.                                                   
17107+1427   BPM 676     [PM2000] 1232570 + [PM2000] 1232441.                                    Gvr2010 
17107-4433   I  1312     Spectrum composite; G8-K0III+G.                                                 
17108-6021   B  1846     Spectrum: G8/K0III+A/F.                                                         
17111+3501   LIM   6     Liu et al. (2012) derive near-IR spectral types of T8 +/- 0.5 and T9.5          
                         +/- 0.5. At a derived photometric distance of 19 +/- 3 pc, the two              
                         stars are separated by 15 +/- 2 au. Various evolutionary models yield           
                         masses of 19-23 Mjup for the primary, 8.1-10.7 Mjup for the secondary.  LiM2012 
17111+2414   SHY 713     HIP  84054 + HIP  84070. Primary is V620 Her.                                   
17111+1739   BPM 677     [PM2000] 1233246 + [PM2000] 1233145.                                    Gvr2010 
17111-2723   REP  45     Inadvertently cataloged with the wrong precise coordinates.                     
17111-2724   REP  46     Inadvertently cataloged with the wrong precise coordinates.                     
17113+1246   JNN 152     2MASS J17111769+1245408 and J17111841+1245080, both from the Riaz et    Ria2006 
                         al. (2006) sample, are separated by only 34" and have comparable                
                         estimated distances (69 and 82 pc), as well as similar proper motions   XXX2010 
                         (e.g. Roser et al. 2010), and thus likely form a physical pair.         Jnn2012 
17113-5641   HD 154857   Chauvin et al. (2006) note finding at least one faint companion         Cvn2006 
                         candidate within separation/magnitude range listed. However,                    
                         further observations are required for verification                              
17115-1630   HU  169     Additional notes may be found in Docobo (1998).                         Doc1998f
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.86 +/- 1.84, 3.07, and 1.91 Msun, respectively.             Mlk2012 
17118+4029   RDN   1     Common proper motion pair G 203-50 + 2MASS J17114559+4028578.                   
                         Spectral types M4.5 + L5, Teff 3114 +/- 115 and 1700 +210/-250 K,               
                         masses 0.146 +- 0.031 and 0.066 +0.008/-0.015 Msun.                             
                         Distance = 21.2 +/- 3.9 pc.                                             Rdn2008 
17118+2232   ALP  21     2MASSI J1711457+223204                                                          
                         Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
17119-0151   LPM 629     Poor Hipparcos solution.                                                Sod1999 
                         Malkov et al. (2012) derive dynamical and photometric masses of                 
                         0.31 +/- 0.14 and 0.74 Msun, respectively.                              Mlk2012 
17120+3158   LOS   2     Discovered while observing GYL   5. A component is GSC 2595 1004,               
                         B = GSC 2595 956. B component magnitude estimated at 13.3.                      
17121+4540   KUI  79     Proper motion of A +257 -1565.                                                  
                         Poor Hipparcos solution.                                                Sod1999 
                         AB: Martin et al. (1998) derive component masses 0.379 +/- 0.035 and            
                         0.369 +/- 0.035 Msun.                                                   Mig1998 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 0.56 +/- 0.05, 0.68, and 0.65 Msun, respectively.  Mlk2012 
                         AB,C: Rectilinear solution by Mason & Hartkopf (2016).                  Msn2016a
17121+2114   STF2135     Despite having an orbit, an optical pair based on parallax and proper   Mlk2022 
                         motion.                                                                 Izm2019 
17125+6918   GC 23290    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
                         Spectroscopic solution to these astrometric pairs given by Griffin      Grf2013a
                         (2013). Periods match "tolerably well," other common elements less so.          
17125+1035   B  2826     37 Oph.                                                                         
17129+4220   BUP 176     Proper motion of A -1015.19 -354.54. B: -004.6 -009.0                           
17129+2317   POU3263     Aka POU3259.                                                                    
17129-0508   SCE   1     GJ 660.1 = GJ 9588.  Schneider et al. (2011) estimate spectral type of          
                         the secondary as M9 +/- 2. Projected separation is 120 +/- 9 au.        Sce2011 
                         Aganze et al (2016) derive spectral types M1 and d/sdM7 and effective           
                         temperatures 3800 and 2550 +80/-90 K.  Masses are 0.57 +/- 0.07 and             
                         0.084-0.091 Msun, radii 0.53 +/- 0.04 and 0.085 +/- 0.014 Rsun. The             
                         authors suggest the possibility that unusual spectral features of the           
                         B component may arise from contamination due to an additional                   
                         unresolved companion.                                                   Bug2016 
17130-5836   HJ 4920     A is a spectroscopic binary, P = 2.88d.                                         
17131-2532   RST3076     Spectrum: B9/9.5IV/V.                                                           
17133-6712   DUN 214     B is CPD-67@3295.                                                               
                         AB: Rectilinear solution by Friedman et al. (2012).                     USN2012a
17133-7243   HJ 4914     Composite-like spectrum: G5III+A4/5V.                                           
17136+1716   A  2087     Ambiguous orbit?                                                                
17137-5425   R   294     SWR 216. CPM pair. B may be variable.                                   Skf2004 
17140+1621   HO  557     A is the W UMa-type system AK Her.                                              
17141+5608   STT 327     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.77 +/- 0.57, 2.53, and 1.35 Msun, respectively.             Mlk2012 
17142+1911   BU 9029     These pairs are not associated with STF2139 as reported by Burnham.     Bu_1906 
17145-0202   BAL 573     J 2905.                                                                         
17145-3946   HJ 4926     A is the variable V915 Sco.                                                     
17146+1423   STF2140     alp Her = Rasalgethi. Star A is an irregular variable, and B is an              
                         SB1, P = 51.58 d. Spectrum composite; G5III+F2V. Radial velocity                
                         measures by Smith (1988 private comm.) for alp Her A since 1984                 
                         have shown an increase in velocity by about 11 km/sec during a                  
                         three-year interval, then an apparent turnover in velocity during               
                         the fourth year. This suggests a component with a period of the                 
                         order of a decade; it now appears that this system may have at least            
                         5 physical components. Measure of 1927.43 made by triangulation of              
                         multiple measures.                                                              
                         The 1779.66 measure by Herschel was corrected.                          H__1804 
                         Mk III Limb-darkened diameter 36.026 +/- 0.439 mas.                     MkT2003 
             CHR 139     Aa,Ab: A premature orbit has been computed.                                     
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Radial velocity measures by Smith (1988 private communication) for alp          
                         Her A since 1984 have shown an increase in velocity by about 11 km/sec          
                         during a three-year interval, then an apparent turnover in velocity             
                         during the fourth year.  This suggests a component with a period of             
                         the order of a decade; it now appears that this system may have at              
                         least five physical components.                                                 
                         Aa,Ab:  Resolved 3 times 1986-1991 at separations 0.16-0.19"                    
                         separations, but unresolved by Balega at the 6-m in 1997 and 10 times   Bag1999a
                         1985-1997 at 4m and 2.5m telescopes                                     Hrt2009 
             STF2140     AB: H 2   2.                                                            MEv2010 
17149-7442   SWR 215     CPM pair                                                                Skf2004 
17150+2450   BNU   5     Aa,Ab: del Her = 65 Her = Sarin. A is a spectroscopic binary.                   
                         1983.3180: Measurements were made with the 20-power objective, hence            
                         the accuracy is low.                                                    Bag1984a
             STF3127     AB: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB: H 5   1.                                                            MEv2010 
17152+3214   COU 805     TDT 292.                                                                        
17153+2423   POU3269     Aka POU3268.                                                                    
17153-2636   SHJ 243     36 Oph = A Oph. AB = HDO 144. Proper motion -480 -1142. A premature             
                         orbit has been computed. A may be a spectroscopic binary.                       
                         Three orbit solutions by Irwin et al. (1996); the shortest-period       Irw1996 
                         orbit is marginally preferable.                                                 
                         VLTI uniform disk diameter of A:       1.253 +/- 0.025 mas,             LTI2009 
                         VLTI limb-darkened disk diameter of A: 1.282 +/- 0.026 mas,                     
                         R = 0.817 +/- 0.016 \rsun, Teff = 4843 +/- 134 K.                               
                         AC: NLTT 44415/44446                                                    Chm2004 
                         AC: SHY  87. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         C component = CD-26 12036 (mag. 6.34, 700", K5V), proper motion                 
                         -481 -1134. C has common proper motion.                                         
                         The original AC and BC components in the BDS and ADS were changed               
                         to AD and BD in the IDS to accommodate the discovery by Luyten          Luy1941 
                         (= LDS 588) assigned AC.  This component assignment has been                    
                         maintained.  However, the BC measures from the BDS were erroneously             
                         assigned to the AD component in the IDS and two AC measures were                
                         assigned to the BD.  This has been corrected, as have errors made               
                         in the IDS in the measures of South and Jacob of the AD and BD          S__1826 
                         components. PM of D +003+026.                                           Jc_1848b
                         AD: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AE: Rectilinear solution by Mason & Hartkopf (2016).                    Msn2016a
                         BD: Rectilinear solution by Friedman et al. (2011).                     USN2011a
17153-3333   SNA  65     Aa,Ab: The primary is the Be star V1075 Sco. The star was reported to           
                         be single in a RV study by Garmany et al. (1980, ApJ 242, 1063) but             
                         reported as SB2 by Chini et al. (2012). Since no period has been        Cii2012 
                         published so far, one cannot decide if the 24.8mas Aa,Ab companion is           
                         the spectroscopic one.                                                  Sna2014 
17155+1052   HDS2440     Cvetkovic et al. (2014) derive spectral types G4 and  G6, masses 1.07           
                         and 1.02 Msun. Dynamical parallax is 15.31 +/- 0.60 mas.                Cve2014 
17156-1018   BU  957     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.37 +/- 1.47, 2.87, and 1.20 Msun, respectively.             Mlk2012 
17156-3836   FIN 355     Rapid motion.                                                                   
                         New orbit based on few observations, mass-sum too small.                Sod1999 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.29 +/- 0.17, 2.22, and 2.12 Msun, respectively.             Mlk2012 
17157-0949   A  2592     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 20.39 +/- 12.95, 4.49, 1.13 Msun, respectively.    Mlk2012 
                         AB + TOK  53Ba,Bb: This is the triple system HIP 84430. We computed             
                         the first orbit of the secondary subsystem Ba,Bb which was discovered           
                         at SOAR in 2009 and has just completed one full revolution since. Its           
                         separation is always close to the diffraction limit. Adopting a mass            
                         sum of 2.6 Msun for Ba,Bb, the resulting dynamical parallax is                  
                         7.6+/-1.5mas, while the HIP2 parallax is 4.9+/-0.9mas. The latest               
                         orbit of the outer pair A 2592 AB published in Tokovinin et al. (2014)  Tok2014a
                         does not account for the fact that the speckle measurements at SOAR             
                         refer to A,Ba and not to AB. Here we give a more accurate solution              
                         that uses the positions of AB computed from the measures of A,Ba under          
                         the assumption that Ba and Bb have equal masses. After this correction          
                         and orbit adjustment, the weighted residuals are 4.3mas in separation           
                         and 1.3deg in angle. Interestingly, there were a considerable number            
                         of speckle-interferometry measures of this pair obtained in the 1980's          
                         and 1990's at 4-m telescopes, but none of them recognized the                   
                         subsystem Ba,Bb, despite its small dm.                                          
                         Ignoring the multiplicity, the spectroscopic survey of Guillout et al.          
                         (2009 A&A 504, 829) determined a moderate axial rotation V sin i =              
                         10.8km/s and detected the lithium line of 52.8mA equivalent width               
                         which, together with the X-ray detection by ROSAT (RasTyc 1715-0948),           
                         normally indicates youth. These authors do not mention this star in             
                         particular, but discuss a group of active lithium-rich giants in their          
                         sample, to which this system apparently belongs. Even with the larger           
                         dynamical parallax (instead of the HIP2 parallax), all three resolved           
                         components of HIP 84430 are located above the main sequence in the              
                         color-magnitude diagram. This multiple system is peculiar and merits            
                         further study.                                                          Tok2015c
17159-6059   R   295     Also appears to be R   292.                                                     
17161+2316   COU 315     Docobo et al. (2010) derive a dynamic parallax of 21.48 +/- 0.50 mas    Doc2010h
                         and a total mass of 1.60 +/- 0.12 Msun.                                         
17161-2556   RST3082     Spectrum: B9.5/A0IV/V.                                                          
17162+0211   CHR  61     This system, first announced by McAlister and recalled in a later       McA1984b
                         McAlister paper after repeated attempts at confirmation, has been       McA1993 
                         restored. While perhaps still spurious, the subsequent confirmation or          
                         suspected duplicity (by another technique) makes the discovery                  
                         measurement somewhat more probable.                                             
17163-4220   I   408     A is variable.                                                                  
17165+0413   LDS 989     Wolf 661-2.                                                                     
17165+0113   HJ  854     A is the Algol-type system U Oph., spectrum composite;                          
                         B5Vnn+B5V.                                                                      
17166+2635   WHC  15     Probable rapid motion in a highly-inclined orbit.                       Ho_1894b
                         CD: Ambiguous wording in the ADS resulted in this pair being                    
                         incorrectly listed as AE or AB,E in the IDS and in earlier versions of          
                         the WDS.                                                                        
17166+0440   LDS4734     A is Wolf 664.                                                                  
17166+0325   SHY 715     AC: HIP  84515 + HIP  85911.                                                    
17166-0027   A  2984     41 Oph. A premature orbit has been computed.                            Vou1951 
17167+1100   BPM 678     [PM2000] 1242397 + [PM2000] 1242317.                                    Gvr2010 
17169+8902   HJ 2985     lam UMi                                                                         
17171+1806   LDS4735     NLTT 44506/44505                                                        Chm2004 
17173+3306   STT 328     68 Her. A is the Beta Lyrae-type system u Her.                                  
                         Composite spectrum, B1.5Vp+B5III.                                               
17173-3010   BU 1119     Spectroscopic binary.                                                           
17173-3533   HD 156134   Bochum 13 #2.                                                           Bid1976 
                         The classification is from McConnell & Bidelman (1976).                 Msn1998a
17173-4140   CPO  73     LDS 589.                                                                        
17173-6016   B  1853     Spectrum: G8/K1III+A.                                                           
17174-6657   LDS 587     Primary is 1.7d eclipsing SB2 V824 Ara; visual pair has estimated               
                         period of 20,000y.                                                      Tok2006 
                         A component is 1.68d SB2, spectral types G5IV+K0IV/V. System is a               
                         member of the bet Pic moving group.                                     Zuc2001b
17175-2746   TRN  24     AB and AC: The image rotator was in an unknown state, so two possible           
                         theta values are listed for the 2001.4959 observation - one for                 
                         zenith up and one for north up.                                         Trn2008 
             HD 156212   Levato et al. (1988) find the radial velocities to be "probably         Lev1988 
                         variable", but since the total range in 11 measurements is 33 km/sec            
                         we assign it to the "C" category.                                       Msn1998a
17177-2638   H 1  35     H I 35.                                                                         
17178+2844   S   686     B is BD+28@2714.                                                                
17179+3229   BU   45     SEI 541.                                                                Nsn2017b
17180-2417   H 3  25     omi Oph. H III 25.                                                              
17183+0459   SLE  19     Aka UC  226.                                                                    
17184+3240   BU  628     A premature orbit has been computed.                                            
17184+0451   SCJ  14     B is BD+05@3367. Aka SLE  18.                                                   
17185+5346   ES  776     Heintz confirms that the Furner measures listed in ADS belong to this   Hei1983a
                         system, so aka FUR   1.                                                         
17186+3229   L    15     Lewis mentions a pair 2' s: 1900.5, 028@, 5.55".                        L__1896a
                         Position of L 15 revised by Heintz.                                     Hei1987a
                         Observations attributed by Popovic & Pavlovic to new pair 17186+3225    Pop2001 
                         PAL   2 have been assigned to this pair. However, there is some                 
                         uncertainty as to whether these two binaries are the same.                      
17186-3223   PRO 154     CPD-32@4467.                                                                    
17187+2146   STTA152     B is BD+21@3090.                                                                
17189-2400   H 6  54     H VI 54.                                                                        
17190-2034   RSS 435     CPD-20@6531                                                                     
17190-3459   MLO   4     Proper motion +1167 -169. Spectral type of C may be M.                          
                         Good double-solution instead of unuseable HIP-data.                     Sod1999 
                         Identification of ascending node is probable.                                   
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.07 +/- 0.61, 1.37, and 1.40 Msun, respectively.  Mlk2012 
                         Using the parallax from van Leeuwen and the mass ratio from Harris,     VlF2007 
                         Strand & Worley individual masses of Ma = 0.65 +/- 0.12 \msun and Mb =  Hrs1963 
                         0.448 +/- 0.085 \msun are determined for these components.              Msn2023 
17191-4638   BSO  13     Proper motion of A +1508,+109; PM of B +1417,+138 (UCAC2). Epoch-2000           
                         coords of C = 1718497-463819, current AC separation ~2'.4 at 265deg.            
                         Epoch-2000 coordinates of D = 1718551-463738, current AD separation             
                         ~1'.6 at 290deg.                                                                
                         41 Apri.                                                                        
                         Four orbit solutions by Wielen (1962); only orbit #4 now in catalog.    Wln1962 
17193-5323   DUN 215     B is CPD-53@8531.                                                               
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
17194-4413   HDO 269     Spectrum composite; B9.5V+A6III.                                                
17195-5004   FIN 356     Composite spectrum, F8III+B9V.                                                  
17197-8520   UC 3324     This pair was included in a list of CPM pairs discovered through data           
                         mining the UCAC4 catalog. However, updated proper motions from UCAC5    UC_2013b
                         give very different values, suggesting the pair is optical.             UC_2015 
17198-3606   SNA  69     Aa,Ab: OWN indicates a 16.4d SB. SAM resolved it as a 185mas pair; a            
                         distant faint companion is also see in the NACO FOV.                    Sna2014 
17199+2629   OSV   5     Ross 867 = LDS 993. Both components are flare stars, V647 and V639 Her          
17200-0801   CHR 151     Aa,Ab: This newly-discovered pair was unresolved in our earlier survey          
                         for duplicity among high-velocity stars (Lu et al. 1987). Abt &         McA1987c
                         Biggs (1972) list a single radial velocity of -89.3 km/s for this       AbH1972 
                         object, published in 1950. Additional observations, both by speckle             
                         and by spectroscopy, are needed for confirmation of its duplicity and           
                         its high velocity.                                                      Hrt1992b
                         B is BD-07@4426.                                                                
17201+2513   BRT3317     Originally published as BRT 173.                                        Brt1928 
17204+2017   LEP  82     NI   37.                                                                        
17207+3228   DOR   1     72 Her. Struve-Dorpat. Proper motion of A +137 -1041.                           
                         Variable. PM of E -016+041, F -052+021                                          
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
17207-0706   A  2593     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 0.93 +/- 0.32, 1.83, and 0.95 Msun, respectively.             Mlk2012 
             TOK 178     HIP 84866. AB is a visual binary A 953 with P=73.5y and a=0.262".               
17207-5625   FIN 255     AB. 1990.3497: This observation finally confirms the discovery of this          
                         system by Finsen, made in 1931!                                                 
17208+0156   LDS6319     Wolf 672. Colors indicate white and red dwarf stars.                            
17208-0902   A    28     aka HO  631                                                                     
17208-1251   SHJ 247     nu Ser = 53 Ser. B is BD-12@4724.                                               
                         H 5  29.                                                                MEv2010 
17208-3932   RST1951     TDT 315.                                                                        
17209+2430   S   687     70 Her. A is a spectroscopic binary.                                            
17209-3604   SNA  70     The 45mas companion was resolved both by PIONIER and NACO/SAM. RV               
                         variability of 7 km/s is reported by Crampton (1972, MNRAS 158, 85)     Cii2012 
                         but not confirmed by Chini et al. (2012).                               Sna2014 
17210-2107   DON 832     xi Oph = 40 Oph                                                                 
17211+0127   STF2150     AB: Rectilinear solution by Hartkopf & Mason (2015).                    WSI2015 
17213-5107   HD156643    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
17214+4552   BRT 343     A likely plate flaw.                                                    Grv2021b
17214+2259   POU3288     Aka WRH   6.                                                                    
17214-3707   BRT1714     CPD-36@7238.                                                                    
17215+2845   CHR 194     Aa,Ab:. 1991.3247: A new close companion to the 0".7 pair KUI 80.               
                         The primary of this system is listed in the preliminary version of the          
                         fifth edition of the Bright Star Catalogue as a G0III SB.               Hof1991 
17215-4154   BRT 960     A likely plate flaw.                                                    Grv2021b
17215-5628   HJ 4939     B is CPD-56@8164.                                                               
17217+3958   MCA  47     Martin et al. (1998) derive component masses 1.150 +/- 0.229 and                
                         2.624 +/- 0.372 Msun.                                                   Mig1998 
             V819 Her    Ba,Bb: Period fixed from spectroscopic orbit by Scarfe et al. (1994).   Scf1994 
                         The visual secondary is a 2.2d eclipsing binary (V819 Her).                     
                         Ba,Bb: Mass-sum in agreement with Scarfe et al. (1994).                 Sod1999 
                         Ba,Bb: Scarfe et al. (1994) give a combined spectroscopic/speckle               
                         solution, yielding distance, masses, etc.                               Scf1994 
                         Ba,Bb: Muterspaugh et al (2008) combine PHASES astrometry with speckle          
                         and radial velocity data to derive orbits for both the AB and Ba,Bb             
                         pairs of this triple. The parallax is determined at 14.57 +/- 0.19 mas          
                         (distance 68.65 +/- 0.87 pc). Masses of the A, Ba, and Bb components            
                         are 1.799 +/- 0.098, 1.469 +/- 0.040, and 1.090 +/- 0.030 Msun.         Mut2008 
                         Ba,Bb: O'Brien et al. (2011) derive an orbit for the B component via a          
                         chi-square fit to interferometric visibility measurements from                  
                         observations of fringe packets at the CHARA Array. The mutual                   
                         inclination compared with the AB orbit is 33.5 +/- 9.3deg. Combined             
                         with spectroscopy by Scarfe et al. (1994), they derive masses for A,    Scf1994 
                         Ba, and Bb of 2.566 +/- 274, 1.488 +/- 0.181, and 1.079 +/- 0.148 Msun,         
                         respectively. Parallax is 14.5 +/- 0.2 mas, yielding a separation               
                         between Ba and Bb of 0.04573 +/- 0.00163 au. The age of the system is           
                         estimated at 1.9 +/- 1.1 Gyr.                                           CIA2011c
                         Zasche et al. (2014) derive a combined solution, including                      
                         interferometry plus times-of-minimia variations in the Algol-type               
                         eclipsing-binary secondary.  They determine a distance of 68.8 +/-              
                         1.8pc and a mass for the secondary of 1.86 +/- 0.30 Msun.               Zas2014b
17221+2310   COU 415     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.99 +/- 1.24, 2.24, and 1.20 Msun, respectively.             Mlk2012 
17221-7007   FIN 373     iot Aps                                                                         
                         Docobo & Andrade (2013) derive a dynamical parallax of 3.89 +/- 0.26            
                         mas and component masses 3.89 +/- 1.02 and 3.45 +/- 0.90 Msun. See              
                         paper for extensive notes on this system.                               Doc2013d
17222+1358   BPM 679     [PM2000] 1252669 + [PM2000] 1252688.                                    Gvr2010 
17222-5902   HJ 4934     B is CPD-58@7077.                                                               
                         SWR 217.                                                                Skf2004 
17224-3012   HO  413     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Friedman et al. (2012).                         USN2012a
17226-3555   GC 23463    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
17228-4537   EVS  30     Primary is the Cepheid V636 Sco.                                        Evs2016a
17232-4937   SWR 218     CPM pair                                                                Skf2004 
17233-4728   HDO 271     iot Ara. A is variable.                                                         
17236+4256   HD157821    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
17237+3709   MCA  48     Aa,Ab: rho Her. Suspected of variable velocity, and resolved by                 
                         speckle interferometry.                                                         
             STF2161     AB: H 2   3.                                                            MEv2010 
17238+0219   BAL1936     J 3297.                                                                         
17239+3300   LDS5854     LDS6320.                                                                        
17239-5154   HJ 4941     SWR 220.                                                                        
17240+3835   HU 1179     1985.741: The residuals of these measurements (as well as those of              
                         McAlister) are irregular and do not permit the correction of an orbit.  Tok1985 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.81 +/- 1.50, 3.55, and 1.70 Msun, respectively.             Mlk2012 
17240-0921   RST3972     High mass-sum, sp duplicity?                                            Sod1999 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.80 +/- 0.64, 2.18, and 1.05 Msun, respectively.             Mlk2012 
                         Aa,Ab: Martin et al. (1998) derive component masses 1.791 +/- 0.499             
                         and 1.749 +/- 0.489 Msun.                                               Mig1998 
             TOK 179     HIP 85141. Aa,Ab = RST3972,                                             Tok2011a
17241-5716   BRT2823     SWR 219.                                                                        
17243-3722   RST3091     Spectrum: B8/9III/IV.                                                           
17244-2248   HJ 4948     AC: HJ 4851.                                                                    
17245-3032   HLD  28     SEE 325.                                                                        
17246+3913   WSI   2     Aa,Ab: Hipparcos suspected non-single.                                          
             S   689     STTA153.                                                                        
                         AB: B is BD+39@3124.                                                            
17246-4709   HJ 4944     B is CD-47@11509.                                                               
17247+3802   HSL   1     Aa,Ab. Masses of 0.887+/-0.030 and 0.788+/-0.021 are determined.        Hor2006d
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 2.37 +/- 0.30, 2.12, and 0.95 Msun, respectively.  Mlk2012 
                         Aa,Ab: For the Horch et al. (2015) combined solution, spectroscopic             
                         elements are fixed to those of Goldberg et al. (2002 AJ 124, 1132).             
                         Assigned spectral types for Aa, Ab, and Ac are G5V, G8V, and K6V;               
                         derived masses for Aa and Ab are 0.92 and 0.84 Msun.                    Hor2015 
17247-3412   HJ 4936     Primary is eclipsing binary of W UMa-type, period 2.359 day.            Zas2013 
             MZA  36     Aa,Ab: Pismis 24-1. Barr Dominguez et al (2013, A&A 557, A13) reported          
                         a 2.36d photometric period, indicating one of the components of this            
                         pair is an eclipsing binary.                                            Sna2014 
17248+3044   BU 1250     Different proper motion. Despite having an orbit,                       Izm2019 
                         an optical pair based on parallax.                                      Mlk2022 
17248-5913   WSI  87     Comparable separations of AB and AD suggest a possibly dynamically      Tok2010b
                         unstable configuration, which is very unlikely. Companion D cannot be           
                         a chance projection: it is too bright and would have been spotted               
                         before.                                                                         
17249+1806   BPMA 50     [PM2000] 1257922 + [PM2000] 1258132.                                    Gvr2010 
17249-4950   CPO 523     CPD-49@9962.                                                                    
17250+0108   RST5431     BAL 1489.                                                                       
17251+3444   HU  922     Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 5.14 +/- 2.29, 1.89, and 1.05 Msun, respectively.  Mlk2012 
             SHY 719     AB: HIP  85238 + HIP  83811.  B component = A component of 17075+3557.          
17252+1355   BPM 680     [PM2000] 1258439 + [PM2000] 1258470.                                    Gvr2010 
17252-5621   BRT3318     A likely plate flaw.                                                    Grv2021b
17254-5233   LPO  62     SWR 221. CPM pair                                                       Skf2004 
17254-5623   HJ 4942     gam Ara                                                                         
17255+5130   HU  672     Includes GQ Dra, a Beta Lyr type eclipsing binary, P = 0.76590d.        Zas2012 
17259+1655   KUI  81     A is the irregular variable V640 Her.                                           
17259-4251   BRT 966     A likely plate flaw.                                                    Grv2021b
17260-0139   TOK 180     HIP 85307. A = HR 6489, F3V, PM(A)=(+61,+52). NOMAD: PM(B)=(-62,+75).           
                         The status of B is uncertain, it is not found in the WDS. A,B are ~1            
                         mag above the MS (true parallax ~25mas?). Nothing on B in SIMBAD.               
                         Crowded field, N*=73.                                                   Tok2011a
17260-0245   OSO  78     G019-025. AB is not a common proper motion pair, based on comparison            
                         with POSS2 red plates.                                                  Oso2004 
17260-5038   HDO 313     kap Ara                                                                         
17261+3550   ES 2228     BOW.                                                                            
17261-3718   RST3096     TDT 349.                                                                        
17262+6311   HO   68     TDT 351.                                                                        
17262+3604   GRV1230     SLW1210.                                                                        
17262+2927   STF2165     Called a Delta Del-type star by Bidelman.                                       
17263+0736   GC 23614    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         McLaughlin (1962).                                                      MLa1962 
17264+2245   RAO 371     pa error = 357 deg.                                                     RAO2020b
17264-4837   SHY 297     HIP  85342 + HIP  85326.                                                        
                         AB + TOK 415Ba,Bb: HIP 85342 and HIP 85326 form a physical pair AB at           
                         127" separation (common PM, RV, and parallax). The B component = HIP            
                         85326 has a variable RV and an astrometric acceleration which could             
                         hardly be produced by the 1" speckle companion Bb found here, owing to          
                         its long estimated period of ~300yr. It seems that B is triple and the          
                         whole system is quadruple. This companion Bb was not detected in the            
                         previous speckle observations because it is red: dI = 2.4, dy = 4mag;           
                         its color matches a dwarf star at the same distance as the system.              
                         However, the field is crowded and the newly found companion could               
                         still be optical.                                                       Tok2015c
                         AB: Tokovinin & Lepine (2012) miss B, but list companion at 1373",      Tok2012c
                         likely optical.                                                         Tok2014d
17266-0505   MKT  14     Aa,Ab: 47 Oph. Preliminary elements determined by Hummel (1997), based          
                         on Mark III interferometric results.                                    MkT1997 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.59 +/- 0.21, 3.02, and 1.30 Msun, respectively.             Mlk2012 
                         Wang et al. (2015) derive a combined interferometric/spectroscopic              
                         orbit, including data from the Mark III and NPOI arrays. Derived                
                         physical parameters for the Aa and Ab components include luminosities           
                         7.80 +/- 0.36 and 3.41 +/- 0.25 Lsun, radii 2.06 +/- 0.07 and                   
                         1.36 +/- 0.06 Rsun.                                                     WaX2015 
17266-3258   TOK 416     HIP 85360 is an acceleration and spectroscopic binary. Its preliminary          
                         spectroscopic period (Latham 2012, private communication) corresponds           
                         to a semi-major axis of 80mas. The star is chromospherically active             
                         and possibly young. The faint companion found here at 1".16 is most             
                         likely optical, as the field is extremely crowded. Re-observation               
                         within a year will resolve its status.                                  Tok2015c
17267+3105   LDS 995     B is BD+31@3025.                                                                
                         NLTT 44816/44814                                                        Chm2004 
                         HJL 247.                                                                HJL1986 
                         SHY 720. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
17268-2620   BU  128     HDO 146                                                                         
17270+5718   ES 2658     STI 2351.                                                                       
17271-3554   BRT1719     A likely plate flaw.                                                    Grv2021b
17272-6105   RSS 441     CD-60@6672                                                                      
17273+1504   BPM 681     [PM2000] 1262856 + [PM2000] 1263009.                                    Gvr2010 
17275+0428   GRV 956     HJL 248.                                                                HJL1986 
17279+1123   STF2166     B is BD+11@3183.                                                                
17279-4702   RST5543     V750 Ara, a light and velocity variable.                                        
17282+4301   OSO  79     G203-068. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
17282+3949   BOY  10     Aa,Ab: 2MASSW J1728114+394859                                                   
                         Aa,Ab: Burgasser et al. (2011) derive spectral types of L5 and L6.5,    Bug2011 
                         masses 0.075 +/- 0.007 and 0.066 +/- 0.008 Msun, and effective                  
                         temperatures 1570 +/- 80 and 1340 +/- 70K.                                      
                         Aa,Ab: Assuming a parallactic distance of 24.1 +/- 2.1 pc                       
                         (Vrba et al. 2004), Konopacky et al. (2010) derive a system mass of     Vrb2004 
                         0.15 +0.25/-0.04 Msun.                                                  Kon2010 
             ALP  22     AB: Physical companionship to this ultracool dwarf ruled out based on           
                         I-J color, using I-band photometry taken at WIYN in August 2002.        AlP2007 
17283-2058   A  2244     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.70 +/- 1.23, 2.64, and 1.20 Msun, respectively.             Mlk2012 
17286+1132   BPM 682     [PM2000] 1265621 + [PM2000] 1265681.                                    Gvr2010 
17287-2304   RST3103     CD-22@12047.                                                                    
17290+5052   STF2180     H 1  66.                                                                MEv2010 
17290-4358   DUN 217     Spectrum of B: A2IV.                                                            
17290-5048   CPO 527     CPD-50@10113.                                                                   
17292-0300   BRT 468     A likely plate flaw.                                                    Grv2021b
17292-3132   SNA  72     The primary is V1081 Sco, a detached Algol-type eclipsing binary                
                         showing apsidal motion (Otero 2005, IBVS 5631, 1), most probably                
                         because of this third component at 26.8mas. The object is reported as           
                         SB3 and we postulate our detection corresponds to the 3rd component.    Sna2014 
             HD 158186   The classification is from Garrison et al. (1977 ApJS 35, 111). An              
                         eclipsing light curve is presented in the Hipparcos Catalogue for a     HIP1997a
                         for a period of 8.77 d.                                                 Msn1998a
17293+2924   A   351     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.06 +/- 0.24, 1.33, and 0.79 Msun, respectively.  Mlk2012 
             KUI  82     AB,C: Baize measures from 1937-1962 were corrected by the author for a  Baz1966b
                         scaling error. In this same paper Baize extracted three measures from           
                         A.C. data and also calculated a rectilinear fit to all measures.                
                         Statistically the same parallax within the errors would indicate the            
                         components are physical.                                                        
                         AB,C: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
17295+3456   STF2178     BDS 8092. H III 40 may be same star?                                            
17297+6351   LDS5227     LDS6321.  Also known as LEP  84.                                                
                         NLTT 44975/44960                                                        Chm2004 
                         HJL1095.                                                                HJL1986 
                         SHY 298. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
17297+1629   BPM 683     [PM2000] 1268087 + [PM2000] 1267932.                                    Gvr2010 
17297-5519   BRT2581     A likely plate flaw.                                                    Grv2021b
17299+3035   SLE  29     SLE 29 and GRV 957 may be the same pair, but there appears to be a              
                         major typographical or reduction error by Soulie (1983).                Sle1983 
17300+3035   GRV 957     SLE 29 and GRV 957 may be the same pair, but there appears to be a              
                         major typographical or reduction error by Soulie (1983).                Sle1983 
17301-3343   HWE  39     A is a spectroscopic binary, P = 38.10d.                                        
17304+5218   BU 1090     bet Dra = 23 dra = Rastaban                                                     
                         Mk III Limb-darkened diameter  3.225 +/- 0.053 mas.                     MkT2003 
17304-0104   STF2173     The eccentricity, inclination, node, and longitude of the node are      Dnc1952 
                         taken from the orbit of Duncombe & Ashbrook (1952) by Wilson (1976).    WRH1976b
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.91 +/- 1.03, 2.05, and 0.95 Msun, respectively.             Mlk2012 
                         High-angular resolution measures only were coupled with radial          Btw1991 
                         velocities from Batten and Duquennoy, Mayor & Halbwachs, to arrive at   Duq1991b
                         a combined solution, resulting in additional orbital elements of K1 =           
                         5.00 +/- 0.11 km/s, K_2 = 5.40 +/- 0.11 km/s, \gamma = -77.197 +/-              
                         0.064 km/s, and individual masses of Ma = 1.018 +/- 0.048 \msun and             
                         Mb = 0.943 +/- 0.046 \msun for these components. In addition,                   
                         an orbital parallax of 59.84 +/- $2.89 mas is determined.               Msn2023 
17306+1731   GC 23718    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
17308+0349   A  2247     In 1923, 183@, 0.1". Quadrant doubtful.                                         
17308-3726   B   912     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.35 +/- 1.71, 3.78, and 2.24 Msun, respectively.             Mlk2012 
17311-6041   EHR  15     Primary is del Ara. Physical/optical nature of AB,AC,AD all undefined.  Ehr2010 
             HJ 4951     AE: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             del Ara     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
17314+0243   A  2386     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Lucke & Mayor (1982).                                                   Luk1982 
                         1978.6174: This epoch was incorrectly given as 1977.6174 by McAlister           
                         & Hendry (1981).                                                        McA1981b
17315-6026   I   600     Ruymaekers & Nys (1995) noted discrepancies in the orbit of Erceg &     Ruy1995 
                         Olevic (1988), and calculated elements from the Thiele-Innes            Erc1988 
                         elements originally given.                                                      
17316+1654   BPM 684     [PM2000] 1272174 + [PM2000] 1271975.                                    Gvr2010 
17316-2616   CHR 229     Possible confirmation of this pair may be found in Hoffleit & Warren    Hof1991 
                         (1991), who note the following: "Duplicity reported from grazing                
                         occultation observations of 1991 Sep 15. Estimated magnitude of                 
                         comparison 8.6, separation several tenths of an arcsecond in position           
                         angle 160 deg (all rough estimates)".                                   Hrt1996b
                         OCC 821.                                                                        
17316-3018   I   105     SEE 330.                                                                        
17316-3041   LDS 602     NLTT 44935/44933                                                        Chm2004 
17317+3019   STF2181     AB and AC: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB, AC: Rectilinear solutions by Hurowitz et al. (2014).                USN2014a
17317+1111   AG  354     HU 179.                                                                         
17318-4953   HJ 4955     alp Ara. A spectroscopic binary.                                                
17320+6808   BU 1458     27 Dra. A is a spectroscopic binary.                                            
17320+0249   STT 331     A: V2373 Oph, a Beta Lyrae eclipsing binary, period 1.08628d.           Zas2010 
             BU 1538     DE: This is a measure of a faint pair 1 minute preceding STT 331.               
17321+3106   LDS4750     NLTT 45001/45000                                                        Chm2004 
17321-2035   LDS5226     NLTT 44964/44965                                                        Chm2004 
17322+8635   DRS  59     del UMi = 23 UMi = Yildun                                                       
17322+5511   STFA 35     A: 25 Dra = nu 2 Dra                                                            
                         B: 24 Dra = nu 1 Dra = BD+55@1944.                                              
                         AB: STTA156. Both components are spectroscopic binaries.                        
                         HJL 249.                                                                HJL1986 
                         SHY 299. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         H 5  11.                                                                MEv2010 
17322+1156   ISO   4     A spectroscopic binary, P = 6.8d.                                               
17324+2848   A   352     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.72 +/- 0.80, 2.79, and 1.35 Msun, respectively.             Mlk2012 
17324-4638   HJ 4957     Nebulous looking star 10' np.                                           I__1909 
17325+1346   BPM 685     [PM2000] 1274391 + [PM2000] 1274440.                                    Gvr2010 
17325+1201   BPM 686     [PM2000] 1274449 + [PM2000] 1274756.                                    Gvr2010 
17326+3445   HU 1181     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.79 +/- 0.33, 2.12, and 1.05 Msun, respectively.             Mlk2012 
17326-0901   LDS 605     Aka GWP2723.                                                                    
17327+7414   29 Dra      Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Fekel et al. (1993).                                                    Fek1993b
17331+0243   BAL1939     TOB 262.                                                                        
17331-3035   CHM   6     NLTT 44988 + 44989.                                                             
17333+4634   ALP  23     2MASSW J1733189+463359                                                          
                         Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
17333+4037   LDS4753     NLTT 45053/45054                                                        Chm2004 
17334+7414   LDS1871     B is BD+74@718.                                                                 
                         HJL 251.                                                                HJL1986 
17335+5734   MLR 571     1980.7255: This measure was incorrectly attributed to HR 6053 in                
                         McAlister et al. (1983), with an additional factor of two error in the          
                         separation.                                                             McA1983 
17335+1553   BPM 687     [PM2000] 1276763 + [PM2000] 1276893.                                    Gvr2010 
17336+1801   BPM 688     [PM2000] 1277005 + [PM2000] 1277076.                                    Gvr2010 
17336-3547   BRT1725     CPD-35@7036.                                                                    
17336-3706   SEE 334     AB: lam Sco = 35 Sco = Shaula. Variable. Spectroscopic binary.                  
             TNG   1     Aa,Ab: The combined solution orbit by Tango et al. (2006) determines    Tng2006 
                         component masses of 10.4 +/- 1.3 Msun and 8.1 +/- 1.0 Msun. There is            
                         also a pre-MS subcomponent to A with a mass of 1.8 +/- 0.2 Msun. The            
                         dynamical parallax is 112 +/- 5 mas, about a factor of two smaller              
                         than the Hipparcos value of 216 +/- 42. The dynamical value is much             
                         more accurate. Two components have calculated effective temperatures            
                         of 25000 +/- 1000 and 21000 +/- 1000 degrees Kelvin, respectively.              
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 77.47 +/- 30.56, 22.63, 10.96 Msun, respectively.  Mlk2012 
17337+1451   WSI   3     Hipparcos suspected non-single.                                                 
17339+1655   LDT  14     V1274 Her.                                                                      
17339+0806   SHY 726     HIP  85940 + HIP  85944.                                                        
17341-0303   TOK 417     HIP 85963 has a variable RV and is an acceleration binary. The 91mas            
                         separation implies an orbital period of ~10yr; the estimated masses             
                         are 1.37 and 0.81 Msun. Despite extensive literature (51 references in          
                         SIMBAD), there is no published spectroscopic orbit, while several               
                         high-resolution spectroscopic studies addressed the abundance.          Tok2015c
17342-1910   B  1863     AB + TOK 418AC: B 1863 is a known close binary which has been                   
                         unexpectedly found to be a triple. The new distant component C is               
                         detectable also in the y filter, but we measured only the inner binary          
                         in y. The star was observed at the Blanco telescope in 2008.5397, and           
                         the pair actually measured then was AC, at 133.8deg, 0".217, dy =3.7.           
                         The inner pair AB with a smaller dm was unresolved in 2008.5, while it          
                         is clearly resolved now. Owing to the large distance from the Sun, we           
                         expect only a slow motion, so even the inner pair observed since 1929           
                         may not yet be ready for computing its first orbit.                     Tok2015c
17342-5454   TOK 419     HIP 85969 has a variable RV according to the GCS and confirmed by               
                         Jones et al. (2002 MNRAS 337, 1170). The 0".55 separation implies a             
                         period on the order of 80yr. The star is on the exo-planet program at           
                         the Anglo-Australian Telescope.                                         Tok2015c
17343-1909   SS 73-90    Symbiotic star, spectral type M6. Fekel et al. (2008) orbit is a        Fek2008 
                         combined spectroscopic/spectropolarimetric solution. Estimated value            
                         for a" based on their a sin i, i, and estimated distance of 4.7 kpc.            
17344+2520   HJ 1300     AB: Rectilinear solution by Hartkopf & Mason (2015).                    WSI2015 
17344+1310   STF2184     AB: H 3  35.                                                            MEv2010 
17345+0335   BAL2443     J 3298.                                                                         
17346+2958   MAB   1     Primary is a slightly evolved subgiant, inferred mass 1.16 +/- 0.11             
                         Msun, and is a 9.009d SB. Minimum mass of close companion is 40.0 +/-           
                         2.5 Mjup. Distance is estimated at 218 +/- 14 pc. A wider possible              
                         companion was discoverd by AO imaging at 643mas, with dm 6.49mag in             
                         K-band. If physically associated, this companions would have an                 
                         estimated mass of 0.13 Msun. Further pm data are needed to determine            
                         its physical or optical association with primary.                       MaB2013 
17346+0935   STFA 34     53 Oph = f Oph. STTA155. B is BD+09@3423.                                       
                         AB: H 5  30.                                                            MEv2010 
17346-5256   CPO 533     B is CPD-52@10710.                                                              
17347-3235   HJ 4962     Central star of cluster NGC 6383, and spectroscopic binary, P = 3.37d           
             ISO   5     Our single observation appears to indicate a single star, so we cannot          
             HDS2480     confirm the reported ISO 5 Aa pair. Nor did we detect the new                   
                         Hipparcos Aa,Ac pair, presumably due to the large magnitude difference          
                         (Delta Hp = 3.2).                                                       Msn1998a
                         Classifications of the Ab and Ac components are from Lindroos (1985).   Lnd1985 
                         Lindroos also notes a wider "X" component (V = 10.8, separation = 25",          
                         photometric classification = B5 IV) which he claims is physical.  This          
                         component is not mentioned in the WDS.  Lindroos finds a distance of            
                         1.8 kpc.                                                                        
             SNA  73     Aa1,2: The primary is V1036 Sco, an ellipsoidal variable star. It is            
                         marginally resolved on two PIONIER observations with minimum                    
                         separation rho>0.9mas on the first epoch and rho=10mas about one month          
                         later.  The known SB2 has an equal mass ration, P=3.36d, and a sin i =          
                         14 Rsun (Stickland et al. 1993; Linder et al. 2007, A&A 474, 193.       Stc1993 
                         Given a probably distance of ~1.5kpc, the expected separation of the            
                         spectroscopic pair is <0.2mas, so we probably detected a 3rd fainter            
                         component. Mason et al. (1998) reported three other companions at       Msn1998a
                         0.27", 0.74", and 5.4". We clearly detect the wider pairs, but not              
                         Aa,Ab. The Ab companion may be a spurious detection (possibly due to            
                         the 10mas Aa1,Aa2 pair), or possibly is too faint for AstraLux and              
                         NACO, implying dm > 5mag.                                               Sna2014 
17348+0601   STF2185     STTA154.                                                                        
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         BC: The 1912 observation was incorrectly attributed to a nonexistent    Dob1927 
                         AD component (apparently the result of an erroneous note in the ADS).   A__1932a
                         Error noted by Burley & Kidd.                                           GSU2002 
                         AB: HJL 250.                                                            HJL1986 
17348-1115   HJ 4964     B is BD-11@4410.                                                                
17349+1234   MCY   4     alp Oph = Rasalhague.                                                           
                         The companion has been detected by infrared speckle interferometry.     Mcy1983 
                         Kamper et al. derive a combined astrometric/spectroscopic solution.     Kpr1989 
                         Gatewood derives a weighted mean parallax of 68.12 +/- 0.75 mas from    Gat2005 
                         MAP and previous results. Masses resulting from solution are 2.842              
                         +/- 0.194 and 0.778 +/- 0.058 Msun; spectral types are A2V and K2V.             
                         This object was incorrectly identified as HD 159571 by Balega et al.    Bag1984b
                         1999: Boccaletti et al. (2001) theta was flipped from 116.3 to 63.7,    Boc2001 
                         as noted by Gatewood (2005).                                            Gat2005 
                         Intensity Interferometer Limb-darkened diameter 1.63 +/- 0.13 mas.      HBr1974 
                         NPOI Limb-darkened diameter 1.855 +/- 0.012 mas, Sp = A4-7III,          NOI2018 
                         R = 2.97 +/- 0.05 \rsun, Teff = 7627 +/- 98 K, L = 26.9 +/- 1.6 \lsun,          
                         M = 1.93 +/- 0.03 \msun, Age = 0.91 +/- 0.03 Gyr.                               
                         Orbital elements by Hinkley et al. (2011) gives a mass ratio of         Hnk2011 
                         2.76 +0.43/-0.27 and individual masses 2.40 +0.23/-0.37 and 0.85                
                         +0.06/-0.04 Msun, assuming a parallax of 69.1 mas.                              
17349-0044   BAL 891     J 2114.                                                                         
17350+6153   BU  962     26 Dra.                                                                         
                         Magnitude of B underestimated by Burnham.                               Baz1954a
                         A distant companion (mag. 9.95, 740") shares the large proper motion            
                         (Upgren 1962).                                                          VVO1962 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.77 +/- 0.95, 1.80, and 1.05 Msun, respectively.  Mlk2012 
                         AB: GJ 684. A is SB1, P=76.1y (Abt & Wilmarth 2006)                     AbH2006 
             LDS2736     AB,C: SHY  88. Bayesian analysis by Shaya & Olling (2011) indicates     Shy2011 
                         very high (near 100%) probability pair is physical.                             
                         AB,C: C is GJ 685.                                                      Tok2014d
             HZE   3     GJ 684. Heinze et al. (2010) determine that the new companion is a              
                         background object.                                                      Hze2010 
17352+2635   LAW   5     Spectral types M7-L3 and M8-L4, masses 0.077-0.086 and 0.066-0.082              
                         Msun, distance 10-12 pc                                                 Law2006 
17354+1322   A  1879     Rectilinear solutions by Rica & Zirm (2012)                             FMR2012i
                         and Scardia et al. (2017).                                              Sca2017c
17355+2311   RAO 511     LV Her.                                                                         
17357-6257   HJ 4956     SWR 225.                                                                        
17358-3542   VOU  72     1.6' n, 1.5m f CPD-35 7046.                                             Vou1947a
17359-6427   SWR 226     Probably giants, not dwarfs                                             Skf2004 
17360+2100   STF2190     A is a spectroscopic binary.                                                    
                         Herschel observed this pair and another nearby pair of similar rho and  HJ_1833c
                         theta and same primary and secondary magnitudes he designated HJ 2807.          
                         Offset from his STF2190 coordinates shows no bright star at location            
                         of HJ 2807, however. Burnham says HJ 2807 is "undoubtedly identical     Bu_1906 
                         with STF2190" (= BDS 8082). Herschel's 1830.47 measure was accordingly          
                         reassigned to STF2190. Gauchet disagrees with Burnham, but his          Gau1925 
                         separation does not agree with Herschel's and his coordinates precess           
                         to location of a 7th magnitude star (BD+20@3531) 1.5m east of                   
                         Herschel's. Separation and magnitudes of this pair, designated                  
                         GAU  21, agree with Gauchet's, although the quadrant is reversed.               
17360-2025   BHA  19     CPD-20@6597.                                                                    
17362+5425   ES  637     B is BD+43@2775.                                                                
17362-3330   B   914     Spectral type may be M.                                                         
17362-5538   HJ 4959     B is CPD-55@8221.                                                               
17363-4357   BRT 983     A likely plate flaw.                                                    Grv2021b
17364+6820   CHR  62     Aa,Ab is also the astrometric binary Ci 18,2354 = GJ 687                        
                         Lippincott orbit rejected from Fourth Orbit Catalog                     Lip1967 
                         ("object still suspected to be binary by some, but no even              Wor1983 
                         approximately reliable or complete elements yet available")                     
             ENG  61     AB: B is BD+68@947. Proper motion of B = -868,-1270 (UCAC2)                     
                         Proper motion of A = +013+084, C -008+005                                       
                         AB: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
17366+4827   COU1922     CHARA Array Limb-darkened diameter  1.515 +/- 0.010 mas.                CIA2010c
                         R = 17.65 +/- 0.42 \rsun, L = 114.4 +/-  9.5 \lsun,                             
                         Teff = 4493 +/-  98 K.                                                          
17366-4825   TDT 431     SWR 227.                                                                        
17368+1147   BPM 689     [PM2000] 1285047 + [PM2000] 1285184.                                    Gvr2010 
17368-2057   HU  751     Direct motion.                                                                  
                         1985.4843: autocorrelogram remeasured; new results listed here.                 
17370+6845   FOX 203     ome Dra = 28 Dra. A is a spectroscopic binary.                                  
             ome Dra     Combined spectroscopic/astrometric solution, based on high-resolution           
                         echelle spectra plus archival PTI visibility measurements.                      
                         Derived masses 1.46 +/- 0.16 and 1.18 +/- 0.13 Msun,                            
                         distance 23.65 +/- 0.15 pc.                                             Knc2010 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.49 +/- 4.97, 2.59, and 1.25 Msun, respectively.             Mlk2012 
17372+2754   KUI  83     LDS 997.                                                                        
                         Masses and bolometric magnitudes are derived for the two components             
                         of this system by Mason et al. (1999), based on assumed spectral types  Msn1999a
                         and available parallaxes.                                                       
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.07 +/- 0.37, 1.37, and 0.55 Msun, respectively.  Mlk2012 
                         AB,C triple solution.                                                   Sod1999 
17373+7105   LDS1872     NLTT 45240/45242                                                        Chm2004 
17373-4300   SEE 510     tet Sco = Sargas                                                                
                         The confirmation by Hipparcos may be due to taking as a first solution          
                         the measure by T.J.J. See. It is possible that a grid-step error is     See1896c
                         involved here and an NDAC solution of PA = 275, sep = 0.51", and                
                         dm = 3.2 seems better. However, this would seem to contradict See's     Jaw2006b
                         original estimate of the magnitude of B at 13. It is entirely possible          
                         that See's pair is spurious. Given the small dm and how obvious the             
                         Sco is, this could not possibly be, as has been suggested, HJ 4963.             
17374-4022   ARY 107     Author listed WDS position as 17373-4027, but corrected in private      Ary2014b
                         communication on July 2, 2014                                                   
17375+2419   CHR  63     79 Her.                                                                         
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 13.76 +/- 1.34, 3.71, and 2.09 Msun, respectively.            Mlk2012 
17375+2036   GAU  21     See note for 17360+2100STF2190.                                                 
17376+1747   BPM 690     [PM2000] 1287091 + [PM2000] 1286976.                                    Gvr2010 
17376+1556   BPM 691     [PM2000] 1287158 + [PM2000] 1287331.                                    Gvr2010 
17376-1524   ISO   6     xi Ser = 55 Ser. Aa,Ab is a spectroscopic binary, P = 2.29d. The Isobe  Iso1990a
                         pair is not the spectroscopic binary.                                           
17376-4049   EVS  31     Primary is the Cepheid V950 Sco.                                        Evs2016a
17379+1836   Ci 18,2347  = GJ 686                                                                        
                         Bieger orbit rejected from Fourth Orbit Catalog                         Bie1964 
                         ("not confirmed by subsequent observations")                            Wor1983 
17379-3752   I   247     A spectroscopic binary.                                                         
17380+5521   GRV1137     SLW1211.                                                                        
17380+3330   JNN 115     The B component of the system appears to be a close binary itself in            
                         several different epochs of AstraLux imaging, but the suspected Ba/Bb           
                         pair is not sufficiently resolved to get a converging binary fit,               
                         hence we treat the AB system as a regular binary in this study.         Jnn2012 
17380-4837   CPO 542     Heintz reverses the quadrant.                                           Hei1987a
17382+0913   OSO  80     GD 211. Not a common proper motion pair, based on comparison with               
                         POSS2 red plates                                                        Oso2004 
17383+4500   ES 1257     Measures are very discordant, and indicate rapid movement.              Baz1940a
17384-0519   BAZ   8     Erroneously identified by me as new pair; it is in reality RST3983.     Baz1952d
17384-5956   HJ 4961     B is CPD-59@7089.                                                               
17385+4013   OSO  81     G204-020. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates.                                                  Oso2004 
17386+7120   WOR   7     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
17386+5546   STF2199     A premature orbit has been calculated.                                  Dur1944d
17387+6114   HOM   1     Aa,Ab : A 3748-d spectroscopic orbit of this pair has been determined.  Grf2013f
17387+1840   SLO   1     Aka TDT 447.                                                                    
17387+1834   OSO  82     G170-056. CD is not a common proper motion pair, based on color and             
                         comparison with POSS2 red plates                                        Oso2004 
17388+1643   BPM 692     [PM2000] 1290109 + [PM2000] 1290424.                                    Gvr2010 
17389+8403   STF2299     LDS1876. B is BD+84@397.                                                        
17390+1320   GC 23923    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
17391+0202   SHJ 251     Spectroscopic binary. Composite spectrum, K0III+F4IV.                           
                         AB: HJL1096.                                                            HJL1986 
17392-5112   HJ 4965     B is CD-51@11033.                                                               
17393+0333   GC 23929    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
17394+0103   GIC 147     Ross 534 = LDS 998. G020-007AB.                                                 
17395+4600   BLA   5     Aa,Ab: iot Her = 85 Her. A is a spectroscopic binary, now resolved by           
                         speckle interferometry.                                                         
17397+7256   H 1  41     H I 41.                                                                         
17398+0225   OSO  83     G020-008. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates.                                                  Oso2004 
17398-0458   STF2191     B is BD-04@4324.                                                                
17400+4046   ES 9003     Previously known as ES 1556a.                                                   
17400-0038   BU  631     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 6.97 +/- 4.66, 4.77, and 2.82 Msun, respectively.             Mlk2012 
17401+2646   BRT3320     Originally published as BRT 176.                                        Brt1928 
17402+0909   STF2228     GRV 964.                                                                        
17404+0544   VVO  16     Aka CBL 162.                                                                    
17404-1319   HU  182     aka HO  633                                                                     
17405-2045   DON 856     CPD-20@6623.                                                                    
17407+3117   STTA157     B is BD+31@3077.                                                                
17407+1237   BPM 693     [PM2000] 1295265 + [PM2000] 1295297.                                    Gvr2010 
17408-3052   BSS   1     Primary is pulsar PSR J1740-3052; companion appears to be a                     
                         main-sequence star.                                                     Bss2011 
17411+7225   GIC 148     LDS5225. G258-016/G258-017.                                                     
                         RoboAO resolved Ba,Bb in 2013 at 0.26", but not accepted as real        Tok2014d
17411+2431   STF2194     Spectroscopic binary. Composite spectrum K0III+F4IV.                            
                         AB: HJL 252.                                                            HJL1986 
                         AB: H 3 104.                                                            MEv2010 
17412+4139   STF2203     BDS 8128, STTA158.                                                              
17417+2831   ROE 119     BRT 177.                                                                        
17417-4604   SWR 228     CPM pair                                                                Skf2004 
17418+0458   BAL3011     Not found by Heintz at IDS position.                                    Hei1990b
                         A likely plate flaw.                                                    Grv2021a
17418-5402   HJ 4969     B is CPD-53@8734.                                                               
17419+7209   STF2241     psi 1 Dra = Dziban. LDS1874. B is BD+72@805.                                    
                         CHARA Array Limb-darkened diameter  0.949 +/- 0.026 mas,                CIA2012e
                         R =  2.329 +/- 0.067 \rsun, L =  6.343 +/-0.153 \lsun,                          
                         Teff = 6014 +/-  90 K, M = 1.311 +/- 0.016 \msun,                               
                         Age =  3.8 +/- 0.1 Gyr.                                                         
                         A premature orbit has been computed.                                            
                         A family of possible orbital solutions are determined by Romanenko      Rmn1994 
                         (1994), with periods  ranging from 5,200 to 120,000 years, using the            
                         method of apparent motion parameters and incorporating parallax and             
                         radial velocity information.                                                    
             STF2241     AB: H 4   7.                                                            MEv2010 
                         31 Dra. Toyota et al. (2009) monitored the RV of both the A and B               
                         components every 1-2 months between 2003 Mar - 2007 Nov, using a                
                         high-dispersion echelle (precision ~10 m/s). The A component exhibits           
                         a linear trend in RV, with a slope +220 m/s/y. Toyota et al. assert             
                         that these variations are due to an unseen companion. Assuming a                
                         circular orbit, period is estimated at 3200d; minimum mass of the               
                         unseen star ~50 Mjup. Standard deviation of radial velocities for the           
                         B component <40 m/s and velocities show no periodic variation. This             
                         result rejects the association of a planet of mass > 1.8 Mjup           Toy2009 
                         AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
17420+2127   STF2197     DRD   1 initially entered incorrectly as AC pair; later moved to new            
                         WDS designation 17421+2127.                                                     
17421+2127   DRD   1     Initially entered incorrectly as AC pair in 17420+2127.                         
17421-5248   HRG 124     SWR 229. CPM pair                                                       Skf2004 
17422+3804   RBR  20     Triple system. The Riddle et al. (2015) companion at 2".2 is confirmed  RAO2015 
                         as physical by its fixed position and its location on the CMD. The              
                         main star is a double-lined spectroscopic binary with P = 6 yr (D.              
                         Latham 2012, private communication) and estimated semimajor axis of             
                         0".1. Our standard algorithm, fitstars, produced subpar results on              
                         this star and instead we used the deconvolution technique used in               
                         Riddle et al. (2015) to analyze this star. It is resolved here at               
                         0".07. The magnitude difference of Aa,Ab (dK = 2.43) matches the                
                         spectroscopic mass ratio of 0.52 and corresponds to the Ab mass of              
                         0.60 Msun. The orbital motion of Aa,Ab can be followed with AO and              
                         speckle interferometry.                                                 Rbr2015d
17422-4838   TDT 468     Primary is D component of 17422-4839 ANT   3AD. AD does not appear to           
                         be a physcial pair, so the systems were not merged.                             
17422-4839   ANT   3     D component = 17422-4838 TDT 468.                                               
17424+6501   ES 1910     STI 828.                                                                        
17425+2434   ENG  62     83 Her.                                                                         
17427-0255   BRT 469     A likely plate flaw.                                                    Grv2021b
17427-5740   RST5544     Spectral type of A may be G5.                                                   
17428+1646   BPMA 51     [PM2000] 1301020 + [PM2000] 1301094.                                    Gvr2010 
17430+1213   BPM 694     [PM2000] 1301421 + [PM2000] 1301372.                                    Gvr2010 
17432+8526   LUH  12     G259-20 + 2MASS J17430860+8526594.                                      Luh2012b
17432-2956   ARG  30     B is CD-29@13894.                                                               
17433+5703   LDS1450     NLTT 45369/45370                                                        Chm2004 
17433+2137   DUQ   1     Aa,Ab: Martin et al. (1998) derive component masses 0.942 +/- 0.166             
                         and 0.337 +/- 0.072 Msun.                                               Mig1998 
17433+1751   BPM 696     [PM2000] 1302167 + [PM2000] 1302018.                                    Gvr2010 
17433+1441   BPM 695     [PM2000] 1302165 + [PM2000] 1302484.                                    Gvr2010 
17433-5743   I   377     A is the semiregular variable V Pav, P = 225d.                                  
17434+3357   HO  560     AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014a
17434+1110   BPM 697     [PM2000] 1302568 + [PM2000] 1302697.                                    Gvr2010 
17436+5844   ALP  24     2MASSI J1743348+584411                                                          
                         Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
17441-5150   HD 160691   No comoving objects found within separation/magnitude range listed.             
                         However, Chauvin et al. (2006) note finding at least one faint          Cvn2006 
                         background object.                                                              
17443+1425   HJ 1303     A is the eclipsing binary V624 Her.                                             
17444+4027   ES 9004     Previously known as ES 1556b.                                                   
17446+0235   STF2202     61 Oph. A is a spectroscopic binary. B is BD+02@3391.                           
                         AB: H 4  32.                                                            MEv2010 
17447-4244   FIN 341     Appears to be in rapid motion.                                                  
17449-1839   A  2250     A is the semiregular variable SZ Sgr.                                           
17450-1646   VOU  42     Spectrum: Fm Delta Del.                                                         
17450-4511   HJ 4973     B is CD-45@11856.                                                               
17451-5408   R   303     SWR 230.                                                                        
17453+1049   BPM 698     [PM2000] 1307466 + [PM2000] 1307473.                                    Gvr2010 
17456-2824   SHY 729     HIP  86919 + HIP  86672.                                                        
17457+1743   STF2205     A premature orbit has been computed.                                            
17457-2900   Sgr A*      Semimajor axis in mpc was converted to arcseconds based on a quoted     Eck2002 
                         distance of 8 kpc.  Errors for Eck2002 orbits are as follows:           Sel2002 
                                                                                                 Ghe2003 
                         Element       Sgr A* - S1       Sgr A* - S2          Sgr A* - S8        Sel2003 
                         ----------------------------------------------------------------------          
                         P (yr)        100. +184/-54     19.4   +7.4/-3.0     57.   +1060/-0             
                         a (mpc)       18.  +18./-8.     5.6    +0.7/-1.1     10.   +48./-0.             
                         a (arcsec)    0.46 +0.46/-0.21  0.14   +0.02/-0.03   0.26  +1.24/-0.00          
                         i (deg)       60.  +/-5.        70.    +6./-17.      0.    +/-70.               
                         Omega (deg)   -14. +7./-12.     23.    +27./-11.     -65.:                      
                         T (by)        2097 +281/-96     2002.6 +6.8/-22.     2043  +1060/-0             
                         e             0.6  +/-0.3       0.8    +0.15/-0.40   0.95  +0./-0.12            
                         omega (deg)   190. +120/-10     190.   +/-10.        -55.  +32/-0               
                         ----------------------------------------------------------------------          
                         Note: This system has grown more complex as additional stars orbiting           
                         the Galactic Center have been observed. With the number of companions           
                         now exceeding 170, it has become increasingly difficult to maintain             
                         the usual WDS designation/component scheme. All WDS pairs were                  
                         therefore copied to the WDSS (WDS supplemental catalog) in July 2017;           
                         henceforth the standard published designations for Sgr A* companions            
                         will be used for all components.                                                
17459+2153   STT 335     B is BD+21@3209.                                                                
17460+3919   STF2224     A is a spectroscopic binary. Composite spectrum, K3III+F7V.                     
                         It is also variable, V826 Her.                                                  
17461+0532   CHR 157     1991.3275  An 18.92d period orbit in Batten et al. (1989) apparently    Bte1989 
                         refers to a closer component.  Membership of this star in the cluster           
                         IC 4665 is in question: Abt et al. (1964) list it as a member,          AbH1964 
                         Sanders & van Altena (1972 A&A, 17, 193) as a non-member.               Msn1993b
17461-3204   LDS 611     B is CD-32@13297.                                                               
17462+1019   AG  356     Rectilinear solution by Friedman et al. (2012).                         USN2012a
17465+2743   TRN   2     Aa,Ab: Astrometric orbit, P=65yr, e=0.32 (Heintz 1994) implies          Hei1994a
                         a=0.265", does not fit the 1.4" companion of Turner (2001).             Trn2001 
                         Roberts et al. derive a spectral type for the secondary of M4V +/- 1.           
                         Using an estimated mass for the primary, they estimate the mass of the          
                         secondary as 0.32 Msun.                                                 Rbr2016a
                         Inclination of this orbit appears to be the same as that of the         XXX2017a
                         rotation axis of the primary.                                                   
                         Mk III Limb-darkened diameter  1.953 +/- 0.039 mas.                     MkT2003 
                         NPOI Limb-darkened diameter 1.880 +/- 0.008 mas, Sp = G5IV,             NOI2018 
                         R = 1.64 +/- 0.01 \rsun, Teff = 5425 +/- 69 K, L =  2.1 +/- 0.1 \lsun,          
                         M = 1.09 +/- 0.01 \msun, Age = 7.68 +/- 0.13 Gyr.                               
             STF2220     A: mu Her = 86 Her is a large-amplitude astrometric binary, P = 65y.            
                         A,BC: LDS1002. HJL 253.                                                 HJL1986 
                         A,BC: H 4  41.                                                          MEv2010 
                         A,BC: Additional notes may be found in Baize (1964).                    Baz1964 
             AC    7     BC: Prieur et al. (2014) derive a dynamical parallax of 123.0 mas and           
                         a total mass of 0.82 +/- 0.07 Msun (based on the revised Hipparcos      VlF2007 
                         parallax of van Leeuwen 2007).                                          Pru2014 
17465-0305   BRT 471     Not found by Heintz at IDS position.                                    Hei1985a
                         A likely plate flaw.                                                    Grv2021b
17468+0534   A  1161     In IC 4665.                                                                     
17469+3555   MLB 936     Not found by Heintz at IDS position.                                    Hei1990b
17471+4737   CHR  64     A spectroscopic binary, P = 2.8d. Hence triple.                                 
17471+1742   STF2215     A spectroscopic binary. A premature visual orbit has been calculated.           
17475-0847   OSO  84     G020-015.                                                                       
17476-2622   J  1732     CPD-26@5975.                                                                    
17476-2750   LIC   1     Classical Cepheid X Sgr = 2 Sgr = 3 Sgr.                                        
17476-4008   SEE 338     iot 1 Sco. A is a spectroscopic binary.                                         
17477+2748   GIC 149     G182-026/G182-027.                                                              
17477-8213   WJG   1     BC: Originally 17464-8212 WJG   1, but primary was found to be B                
                         component of 17477-8213 LDS 603.                                                
17478-2211   B   358     CPD-22@6444.                                                                    
17480-5442   I   612     Primary is V537 Ara, Algol-type eclipsing binary, period 1.874351d.     Zas2013 
17482+1339   BPM 699     [PM2000] 1315705 + [PM2000] 1315640.                                    Gvr2010 
17483+1740   BPM 700     [PM2000] 1315759 + [PM2000] 1315895.                                    Gvr2010 
17483+1547   FOX 209     AC: Also known as J   753AC. Identical nature noted by Friedrich                
                         Damm.                                                                           
17483-3525   JSP 732     CPD-35@7269.                                                                    
17489-2219   BRT1508     CD-22@12253.                                                                    
17490+3704   COU1145     1981.333: This observation was incorrectly attributed to COU 1445 in    Tok1982a
                         Tokovinin (1982).                                                       Tok1982b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.84 +/- 0.14, 2.27, and 1.05 Msun, respectively.             Mlk2012 
17491+5047   CHR  65     Aa,Ab: 30 Dra.  Hipparcos Acceleration Double Solution.                         
                         This system, first announced by McAlister and recalled in a later       McA1984b
                         McAlister paper after repeated attempts at confirmation, has been       McA1993 
                         restored. While perhaps still spurious, the subsequent confirmation or          
                         suspected duplicity (by another technique) makes the discovery                  
                         measurement somewhat more probable.                                             
17491+1151   BPM 701     [PM2000] 1318164 + [PM2000] 1318445.                                    Gvr2010 
17492-3618   JSP 734     CPD-36@7625.                                                                    
17494+2651   BRT3322     Originally published as BRT 178.                                        Brt1928 
17496-2000   HJ 2810     AB: The CPD identifications of A and B are -19@6275 and -19@6274.               
                         AD: D component is planetary nebula NGC 6445.                                   
17497-2100   BRT1509     A likely plate flaw.                                                    Grv2021b
17499-3703   SEE 340     G Sco = Fuyue                                                                   
17499-7505   SWR 231     A component not CD-75 9877: +1m CD RA error, thus = CPD-75 1397         Skf2004 
17500-5428   BRT2096     A likely plate flaw.                                                    Grv2021b
17502+4424   SIG   3     2MASSW J1750129+442404.                                                         
                         Spectral types M7.5, M9.5. Estimated orbital period 36 +10/-9 yrs.      Sig2003 
                         Konopacky et al. (2010) derive a distance of 37.6 +/- 12.3 pc and a             
                         system mass of 0.20 +/- 0.12 Msun.                                      Kon2010 
17502-1339   LDS5856     NLTT 45517/45519                                                        Chm2004 
17502-4005   HDO 279     iot 2 Sco                                                                       
17503+2517   STF2232     H 3  40.                                                                MEv2010 
17503+1737   BPM 702     [PM2000] 1321865 + [PM2000] 1321463.                                    Gvr2010 
17504+5414   OL   89     Aka TDS 888.                                                                    
17504-3652   JSP 737     CPD-36@7660.                                                                    
17505-0603   LAF  59     Due to the large number of components (exceeding the number of upper-           
                         case letters), a non-standard component designation was necessary,              
                         hence the pairings A,Ya; A,Yb; etc. For this pair, as well as LAF  62           
                         and LAF  71, the lower-case designations (such as Ya and Yb) do not             
                         refer to components of a close pair.                                            
17505-4655   CPO 556     SWR 232. CPM pair                                                       Skf2004 
17505-4817   HJ 4982     B is CD-48@12074.                                                               
17505-5337   HJ 4978     A is the Algol-type system V539 Ara.                                            
17506+0714   STT 337     Quadrant uncertain. Star approaching periastron.                        Baz1954a
                         In AJ 63, 68, 1958 I have given a mean of 5 measures of ADS 10828. The  B__1958 
                         first measure is not of this pair, but of the nearby pair ADS 10846.            
                         The result for 10828 should read: 1957.449, 22.7, 0.24, 8.4-8.7, n=3    B__1962a
                         A premature orbit has been computed.                                            
17506-4019   EGN  21     AB pair unbound, but bound/unbound nature of AC pair inconclusive.              
                         Primary is planet host star.                                            Egn2007 
             HD 162020   Chauvin et al. (2006) note finding at least one faint companion         Cvn2006 
                         candidate within separation/magnitude range listed. However, further            
                         observations are required for verification.                                     
17507+0755   STF2230     B is BD+07@3483.                                                                
17507-3444   BRT1741     CPD-34@7161.                                                                    
17509-3342   HDO 280     Classical Cepheid RY Sco.                                                       
17510+5709   STI2360     LDS1455.                                                                        
17515-7748   LDS 609     TSN 104.                                                                        
17518-1336   HU  188     Spectrum: B9.5III/IV.                                                           
17520+1520   STT 338     L    16.                                                                        
                         AB: Prieur et al. (2012) derive a dynamical parallax of  7.9 mas and            
                         (using their orbital elements and the revised Hipparcos parallax of             
                         van Leeuwen 2007 A&A 474, 653) a total mass 12. +/- 11. Msun.           Pru2012 
17520-0114   HR 6659     Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Griffin (1980).                                                         Grf1980a
                         SB1. Combined orbit including RV data and Hipparcos Intermediate                
                         Astrometric data. Semimajor axis derived from photocentric a0 plus              
                         stellar evolutionary model. Derived properties for A and B:                     
                         M/Msun = 1.66 + 0.41, L/Lsun = 42.50 + 0.03, dm = 7.88 mag,                     
                         log age = 9.29.                                                         WaX2015b
17521+0107   S   694     STTA159. B is BD+01@3525.                                                       
17523+4057   A   699     Also unresolved 1960.                                                           
17523+3624   OSO  85     G182-031. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
17524+1733   BPM 703     [PM2000] 1327958 + [PM2000] 1327923.                                    Gvr2010 
17525+1530   WLY  17     AC: Previously known as FOX 209. That pair is actually at 17483+1547            
                         and the pair measured here is new. The correct identification was               
                         ascertained by Friedrich Damm.                                                  
17526+2536   A   234     AB: Rectilinear solution by Rica & Zirm (2012).                         FMR2012i
17526+1154   BPM 704     [PM2000] 1328639 + [PM2000] 1328474.                                    Gvr2010 
17526-0609   EVS  32     Primary is the Cepheid Y Oph.                                           Evs2016a
17527+1459   BPM 705     [PM2000] 1328958 + [PM2000] 1328887.                                    Gvr2010 
17530+8354   STT 349     Heintz (1978) suspects the presence of an unresolved star.              Hei1978d
                         Unless motion takes place in a very short period these measures are             
                         unusually discordant.                                                   VBs1954 
17530+1521   OSO  86     G183-009. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates.                                                  Oso2004 
17530-0755   STF3128     Separation 0.56" of my single night's measure in 1958 (Pub Yerkes Obs   B__1960b
                         IX, pt I, p 77) should read 0.22".                                      B__1963a
                         Semi-major axis incorrectly given as 0.935 by Popovic & Catovic (1989)  Pop1989b
                         should be 0.985 (erratum noted in Inf. Circ. 108, 1989)                         
                         HIP 87533. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
17532+3713   DAE  11     TrES-4.  Daemgen et al. (2009) estimate spectral types F8 and K5.5-M0,          
                         masses 1.18 and 0.59 Msun, and an orbital period of about 21000y.       Dae2009 
                         Bergfors et al. (2013) estimate spectral types F8V and K4.5-M1.5V.      Brg2013 
17533+4000   BU  130     90 Her.                                                                         
17533+2459   A   235     A 2007 measure was inadvertently confused with a measure for BU 435 in          
                         Mason et al. (2011); this measure has been corrected.                   Msn2011d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.88 +/- 0.44, 1.97, and 0.91 Msun, respectively.             Mlk2012 
17533-3444   BU 1123     A premature orbit has been computed.                                            
17533-3547   BRT3324     AB: Not found by Hinetz.                                                Hei1987a
                         A likely plate flaw.                                                    Grv2021b
             BRT3325     CD: CPD-35@7400. Not found by Heintz.                                   Hei1987a
                         A likely plate flaw.                                                    Grv2021b
17534+1058   STTA160     B is BD+10@3314.                                                                
17534-2639   HJ 4991     B is CD-26@12487.                                                               
17534-3454   SEE 342     Spectroscopic binary.                                                           
17535+5652   LDS1457     xi Dra = 32 Dra = Grumium                                                       
17535-0355   TOK  54     Primary is V2610 Oph, eclipsing binary of W UMa -type, period                   
                         0.42651 d.                                                              Zas2012 
17536-1726   HDO 147     BHA  59                                                                         
17536-3445   B   362     CPD-34@7283.                                                                    
17537+1702   BPM 706     [PM2000] 1332137 + [PM2000] 1331879.                                    Gvr2010 
17538+1610   BPM 707     [PM2000] 1332342 + [PM2000] 1332598.                                    Gvr2010 
17539-3445   B  1871     One component is a Beta Lyrae-type system, V906 Sco.                            
17540+0303   OSO  87     G020-019. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
17542+1240   BPM 708     [PM2000] 1333651 + [PM2000] 1333727.                                    Gvr2010 
17542+1108   FIN 381     Primary is 0.80d W UMa ecl. bin (V2388 Oph). Called a SB in the                 
                         Bright Star Catalogue; this may be motion in the visual pair.                   
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.83 +/- 1.03, 3.32, and 1.20 Msun, respectively.             Mlk2012 
                         Docobo & Andrade (2013) derive a dynamical parallax of 13.45 +/- 0.38           
                         mas and component masses 1.76 +/- 0.22 and 1.38 +/- 0.18 Msun (based            
                         on photometry of Yakut et al. 2004 A&A 417, 725) or 13.82 +/- 0.39              
                         mas, 1.72 +/- 0.24 and 1.18 +/- 0.16 Msun (based on photometry of               
                         Rucinski et al. 2002 AJ 124, 1738). See paper for extensive notes on            
                         this system.                                                            Doc2013d
                         Zasche et al. (2014) derive a combined solution, including                      
                         interferometry plus times-of-minimia variations in the primary. They            
                         determine a distance of 70.6 +/- 8.9pc and masses of 1.96 +/- 0.03 and          
                         0.54 +/- 0.06 Msun.                                                     Zas2014b
17547+2016   OSO  88     G183-011. Not a common proper motion pair, based on color and                   
                         comparison with POSS2 red plates.                                       Oso2004 
17551+3745   OSO  89     G182-032. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
17551+3134   AG  215     SEI 551.                                                                        
17555+2250   GRV 970     DAL  25.                                                                        
17555+1322   BPM 709     [PM2000] 1337739 + [PM2000] 1337455.                                    Gvr2010 
17557-1156   HJ 4997     LDS 617.                                                                        
17557-2456   J  2194     May be CD-24@13632.                                                             
17557-3034   I  1011     Spectrum: B9.5II/III.                                                           
17558+3117   SEI 552     ES  342.                                                                        
17559+3326   HO   72     BC: Rectilinear solution by Friedman et al. (2012).                     USN2012a
17559-7032   HJ 4976     B is CPD-70@2439.                                                               
17560-6632   HJ 4983     B is CPD-66@3163.                                                               
17561+2130   STT 339     CfA: A or B is SB?                                                      Tok2014d
17563+6237   STTA163     AB: Pair appears in an appendix list, not part of discoverer's regular          
                         numbering sequence.                                                             
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
17563+0259   A  2189     Systemic mass is estimated at 4.1 +/- 0.5 Msun, assuming a dynamical            
                         parallax of 4.75 +/- 0.15 mas.  The Hipparcos parallax for this pair            
                         is poorly determined (3.67 +/- 1.12 mas)                                Doc2008a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 27.45 +/- 27.60, 6.25, and 2.09 Msun, respectively.           Mlk2012 
17563-1549   HJ 2814     B is BD-15@4723.                                                                
                         A 729d spectroscopic solution for the B component has been found        Tok2019g
                         making this at least a triple system.                                           
17563-3228   JSP 748     A is the eclipsing binary V453 Sco, P = 12.61d.                                 
17564+1820   MCA  49     Aa,Ab: 1980.4820: This measure was incorrectly attributed to HR 6148            
                         by McAlister et al. (1983).                                             McA1983 
17565-3408   JSP 934     CPD-34@7399.                                                                    
17566+5813   ES   20     A is the Mira-type variable T Dra, BD+58@1772a.                                 
17566+5129   BU  633     gam Dra = 33 Dra = Eltanin = Etamin. A is variable.                             
                         Mk III Limb-darkened diameter 10.2   +/- 0.2   mas.                     MkT1989 
                         Mk III Limb-darkened diameter  9.860 +/- 0.128 mas.                     MkT2003 
                         AF. Smyth's quoted separation is difference in RA only.                 Smy1844 
17567-3255   BRT1743     Not found by Heintz at IDS position.                                    Hei1990b
                         A likely plate flaw.                                                    Grv2021b
17568+1736   BPM 710     [PM2000] 1341630 + [PM2000] 1341762.                                    Gvr2010 
17568+0459   V566 Oph    Multiple system including contact binary. Pribulla & Rucinski (2006)    Pbl2006 
                         estimate the mass of the contact pair at 1.828 Msun and the minimum             
                         mass of the wider component at 0.24 Msun.                                       
17568-2036   J  1617     AB: ARA1132.                                                                    
17568-3755   JSP 751     CPD-37@7662.                                                                    
17569+1811   J  1352     Jonckheere notes ADS positions are 1970 and 1920. In his 1952 paper             
                         he uses 1950 ADS position and has a note "two couples?".  There is              
                         indeed a measure that indeed looks different:                                   
                         1951.62, 39.9@, 3.33", 11.3-11.3.                                       J__1952 
                         Observations incompatible. Is there confusion between different pairs,          
                         as thought by Jonckheere (JO 35, p 53)?                                 Cou1952b
17569+0610   HD163642    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
17569-1903   FEN  25     17570-1903ARA 718                                                               
17569-3445   JSP 935     Primary is V907 Sco, Algol-type eclipsing binary, period 3.776277d.     Zas2013 
                         Triple star. The orbital planes of the B9.5V eclipsing binary and the           
                         more distant companion (per= 99.3 d.) are not coplanar so the orbital           
                         plane of the eclipsing binary shows nodal regression with a period of           
                         68 years. For about one-third of this time, the close binary is                 
                         eclipsing, the rest of the time the inclination is too small for                
                         eclipses to occur. The earliest observations of the system in the year          
                         1899 show eclipses; the eclipses stopped about 1918, started again              
                         about 1963, and stopped again in about 1986. Eclipses should start              
                         occurring once again in the year 2030+/-5. (Otero, 1999 AJ 117, 541L).          
17569-3514   BRT1744     CPD-35@7528.                                                                    
17571+0004   STF2244     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 8.83 +/- 5.28, 4.60, and 2.00 Msun, respectively.             Mlk2012 
17572+3541   HO   73     Also known as POP  10. HO   73 was at the location of BD+35 3111, the           
                         DM number to which it was assigned and then POP  10 was rediscovered.           
                         All measures have been assigned to HO   73AB and STF2256AC at the               
                         coordinates of POP  10.                                                         
             STF2256     AC: WAL  86CD. The pair 17574+3540 WAL  86AC is not physical, so the            
                         systems have not been merged.                                                   
17572+2400   MCA  50     A close pair of solar-type stars, astrometric binary                            
                         Balega et al. (1984) derive probable period of 940 days                 Bag1984a
                         Culver et al. (1980 BAAS 12, 250) report this to be a spectroscopic             
                         binary with a period of 2.6 years.                                      Bla1987 
                         Determination of these two old measures resulted from new reduction             
                         techniques developed over the past year; these data were reanalysed             
                         for a joint spectroscopic/speckle analysis of this system.              Hrt1992b
                         All our CCD speckle data for this close system have been reprocessed            
                         and examined. In addition, we have listed 7 negative measures dating            
                         from observations made at the KPNO 2.1-m in the 1970's.                         
                         Hartkopf et al. (1994) derive a combined spectroscopic/interferometric  Hrt1994 
                         solution.                                                                       
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         McAlister et al. (1995).                                                McA1995 
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         Orbit determined by fitting revised Hipparcos intermediate astrometric          
                         data. Derived component masses 1.12 +/- 0.17 and 0.72 +/- 0.11 Msun.    Ren2010 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.29 +/- 0.27, 2.15, and 1.79 Msun, respectively.             Mlk2012 
                         Kiefer et al. (2016) generates a combined spectroscopic/astrometric             
                         orbit, yielding masses 1.132 +/- 0.014 and 0.7421 +/- 0.0073 Msun, and          
                         a parallax 36.35 +/- 0.20 mas.                                          Kie2016 
17573+1238   HD163750    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
17573-5212   HJ 4994     B is CPD-52@10926.                                                              
17574+5111   ES   78     Fox also notes a 1" double (12 mag.) 23" from A in 199@.                Fox1915 
17574-3508   JSP 753     CPD-35@7547.                                                                    
17575+1318   BPM 711     [PM2000] 1344016 + [PM2000] 1344347.                                    Gvr2010 
17575+1058   BU 1299     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 9.51 +/- 8.13, 3.18, and 0.65 Msun, respectively.  Mlk2012 
17575-5740   HJ 4992     SWR 234. CPM pair                                                       Skf2004 
                         Despite the linear solution, proper motion and parallax favor a         Grv2020a
                         physical connection. Long period and/or high eccentricity possible.             
17578+4635   BDK   9     G 204-39 + SDSS J175805.46+463311.9. Distance 13.6 +/- 0.3 pc for               
                         primary, 12 +/- 2 pc for secondary. Estimated age of system 0.5-1.5             
                         Gyr. Mass of secondary estimated at 0.020-0.035 Msun.                   Fah2010 
17578+2751   ALL   2     HJL 254.                                                                HJL1986 
17578+1542   BPM 712     [PM2000] 1344986 + [PM2000] 1345358.                                    Gvr2010 
17578+0442   GJ 699      Ci 20,1069 = Barnard's Star                                                     
                         PTI Limb-darkened diameter = 1.026 +/- 0.04 mas,                        PTI2001 
                         R = 0.201 +/- 0.008 \rsun.                                                      
                         VLTI Limb-darkened diameter  1.004 +/- 0.04 mas,                        LTI2003a
                         M = 0.158 +/- 0.008 \msun, R = 0.196 +/- 0.008 \rsun,                           
                         T = 3163 +/-  65 K.                                                             
                         CHARA Array Limb-darkened diameter of A :                               CIA2012f
                         R =  0.1867 +/- 0.0012 \rsun, L =  0.00338 +/-0.00003 \lsun,                    
                         Teff = 3224 +/-  10 K, M = 0.146 \msun.                                         
                         van de Kamp orbits rejected from Fourth Orbit Catalog                   Kam1969c
                         ("object still suspected to be binary by some, but no even              Wor1983 
                         approximately reliable or complete elements yet available")                     
17579-0223   BRT 472     A likely plate flaw.                                                    Grv2021b
17579-1921   RST5097     CPD-19@6357.                                                                    
17583-3810   I  9004     Previously known as I  1347 1/2.                                                
17584+1812   J  3268     Aka J  3236.                                                                    
17584+0428   KUI  84     In the same field with Barnard's Star.                                          
                         P, T, and e have been taken by Gatewood (1973) from the astrometric     Gat1973 
                         solution. In the same field with Barnard's Star. Two astrometric                
                         mass-ratio determinations showed B to be twice as massive as A. This            
                         has been confirmed by Tokovinin, who finds B to be a SB, P = 34.5d.     Tok1994b
                         A measurement published by McAlister et al. (1987) dating from          McA1987b
                         1985.4872 was misidentified as being of KUI 84; the measurement was             
                         actually of KUI 89 (WDS 18594-1250). In addition, an observation of             
                         KUI 84 dating from 1988.6655 (theta = 270.6 deg, rho = 0".134) was              
                         published by McAlister et al. (1990). The data have been reprocessed,   McA1990 
                         and we now believe the 1988.6655 measurement was spurious.              Hrt1994 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.57 +/- 0.61, 1.41, and 0.58 Msun, respectively.             Mlk2012 
17584-1747   RST3140     TDT 605.                                                                        
17586-1306   HU  190     HIP 88010. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
17587+1530   BPM 713     [PM2000] 1347830 + [PM2000] 1347917.                                    Gvr2010 
17587-0428   BRT 473     A likely plate flaw.                                                    Grv2021b
17587-2232   B   367     CPD-22@6498.                                                                    
                         Additional notes may be found in van den Bos (1928)                     B__1928b
17588+1330   RUC  10     V508 Oph. Spectral type of resolved companion later than M5V.           Ruc2007 
17589-2850   B  2848     CPD-28@6088.                                                                    
17589-3652   DUN 219     B is CD-36@12058.                                                               
                         AB: Rectilinear solution by Friedman et al. (2012).                     USN2012a
17590+3003   STF2259     H 4  42.                                                                MEv2010 
                         T0 converted from negative to positive by subtracting from P.           FMR2021a
17590+0259   BAL2462     J 2119. The close pair suspected by BAL is not confirmed.               Hei1985a
                         In Carte du Ciel, primary is listed as a double of 180deg, 0.9", mags           
                         9.9 and 11.4; but it appears single.                                    Cou1953d
17590+0202   STF2252     C is BD+02@3444.                                                                
17591-3015   PZ    6     A is variable.                                                                  
17591-3559   JSP 758     CPD-35@7594.                                                                    
17592+0304   BAL2464     J 2120.                                                                         
17592-3656   HJ 5000     A is the Algol-type system V1647 Sgr.                                           
17593-0651   STF2250     Same as STF2249.                                                                
17594+1151   BPM 714     [PM2000] 1350087 + [PM2000] 1350363.                                    Gvr2010 
17594-1724   RST3144     A is the Algol-type system WX Sgr.                                              
17595+1753   BPM 715     [PM2000] 1350465 + [PM2000] 1350660.                                    Gvr2010 
17595-3601   TRN  25     The image rotator was in an unknown state, so two possible theta                
                         values are listed for the 2001.4960 observation - one for zenith up             
                         and one for north up.                                                   Trn2008 
             HD 163758   MR 78. Leep (1978 ApJ 225, 165) also finds a constant radial velocity.  Msn1998a
17597+3624   OSO  91     G206-001. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates.                                                  Oso2004 
18001+1517   BPM 716     [PM2000] 1352292 + [PM2000] 1352563.                                    Gvr2010 
18002+8000   STF2308     AB: LDS1882. HJL 257. Statistically the same parallax within the        HJL1986 
                         errors would indicate the components are physical.                              
                         Linear elements fit nicely at present, but this is a physical pair and          
                         an orbit can be computed at some future date.                                   
                         AB: H 4  67.                                                            MEv2010 
                         AB: A,B are 2.6 mag above MS, both evolved, both SB systems. Orbital            
                         parallax 23.0+-2.2mas. Masses 1.39,1.30,1.32,1.20.                      Tok2014d
             BAG   6     A: 41 Dra. Spectroscopic binary, P = 1247.2d, with the highest known            
                         eccentricity to date, e = 0.975.                                                
                         Elements P, T, and e for the Balega et al. (1997) orbit were adopted    Bag1997a
                         from the spectroscopic orbit of Tokovinin (1995).                       Tok1995b
                         Combined spectroscopic/speckle solution by Tokovinin et al. (2003),     Tok2003 
                         deriving masses (1.28 +/- 0.15, 1.20 +/- 0.14 Msun) and orbital                 
                         parallax (23.0 +/- 2.2 mas). Authors note earlier elements and discuss          
                         possibility of orbital evolution.                                               
                         Effective temperatures for the two components are 6370+/-20 and                 
                         6410+/-20K, log g 4.05+/-0.10 and 4.20+/-0.10. Abundances for both              
                         components are very near solar.                                         Bag2005b
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 7.75 +/- 5.22, 3.34, and 2.24 Msun, respectively.  Mlk2012 
                         B: 40 Dra = BD+79@570. B is also a spectroscopic binary, P = 10.53d.            
18002+0851   STTA161     B is BD+08@3556.                                                                
18003+5251   STF2271     AB: B is SB2, P=18.888d                                                 Tok2014d
18003+2154   A  1374     Angle decreasing.                                                               
                         AB: Additional notes may be found in Baize (1945).                      Baz1945b
18003+0038   RAS  26     Peculiar SrCuEu star V2126 Oph, type A3. Companion likely                       
                         late-G/early-K; orbital period perhaps 10y.                             Ras2014 
18005-3742   I   230     CPD-37@7765.                                                                    
18006+2934   LDS6413     NLTT 45789/45791                                                        Chm2004 
18006+0256   BU 1124     67 Oph.                                                                         
             H 6   2     H VI 2. STTA162.                                                                
18007+0627   GRV1260     Both A and B have approximately the same radial velocity.               Grv2019b
18009+2633   STF2263     H 2  90.                                                                MEv2010 
18011+3558   POP 210     Codiscovered by Olevic.                                                 Ole1970b
18015+2136   STF2264     95 Her. B spectrum G8III.                                                       
                         Measure of 1927.47 made by triangulation of multiple measures.                  
                         H 3  26.                                                                MEv2010 
18015+0448   OSO  92     G140-031. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates.                                                  Oso2004 
18015+0006   WTT   1     The primary is of type G5V, with mass 1.10 +/- 0.01 Msun. Based on              
                         isochrone fitting, Wittrock et al. (2016) estimate the mass of the              
                         secondary at 0.42 +/- 0.03 Msun, and type likely an M dwarf.            Wtt2016 
18015-3612   BRT1750     CPD-36@7919.                                                                    
                         A likely plate flaw.                                                    Grv2021b
18015-3732   JSP 763     CPD-37@7798.                                                                    
18017+3714   GCB  29     J 3212.  Also known as BRT2222.                                                 
18018+0118   BU 1125     68 Oph. A spectroscopic binary.                                                 
18019-1906   HD 164438   We found a possible binary companion at a separation of 0".05 which             
                         needs confirmation. The classification is from Garrison et al. (1977            
                         ApJS 35, 111).                                                          Msn1998a
18020-5329   BRT2097     A likely plate flaw.                                                    Grv2021b
18022-3616   BRT1751     CPD-36@7937.                                                                    
18024+1758   BPM 717     [PM2000] 1359934 + [PM2000] 1359490.                                    Gvr2010 
18024-2302   SNA  77     Aa,Ab: HD 164492A is the center of a wide multiple system. We detected          
                         two additional faint companions at 3.1" and 6.5", and further resolved          
                         A into a 25mas pair with a rather faint companion (dH=3.2). The         Cti1977 
                         object was reported as RV variable by Conti et al. (1977) but this is   Cii2012 
                         not confirmed by Chini et al. (2012).                                   Sna2014 
18025+4414   BU 1127     A premature orbit has been computed.                                            
                         L 18 is probably the same star                                          VBs1960 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         L    18.                                                                        
18025+2619   HO  564     Burnham measured BD+26@3146, 26s preceding and 4' south of HO 564:      Bu_1913 
                         1905.8, 185.4@, 23.22", 8.3-11.5.                                               
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
18026+0429   LDS5859     LDS6323.                                                                        
18028+7547   STF2302     STN  45 (with 1h error in RA).                                                  
18028+0137   BU  635     C is BD+01@3566.                                                                
18029+5626   STF2278     STTA166.                                                                        
                         AB: The BD numbers of A and B may be reversed. D is reversed.                   
                         DS: Also known as ES 1745.                                                      
18030-2243   RSS 468     CD-22@12473                                                                     
18031+4828   STF2277     Mt. Wilson spectral type of B is G8.                                            
18031+1654   BPM 718     [PM2000] 1362136 + [PM2000] 1362258.                                    Gvr2010 
18031-0811   STF2262     tau Oph = 69 Oph. A is a SB. RV of the primary may be variable.         Wrz1959 
                         Primary giant according to isochrone fit.                               Sod1999 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: H 1  88.                                                            MEv2010 
18032-0543   HR 6940     Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Scarfe et al. (1983).                                                   Scf1983 
18032+2522   STF2268     AC : 1909.56: Measure unpublished in orbit quotation.                   Dob1927 
                         Statistically the same parallax within the errors would indicate the            
                         components are physical.                                                        
18032+0755   STTA164     B is BD+07@3536.                                                                
18032+0047   BAL1192     J 1371.                                                                         
18033+3921   STF2275     Not the same as L    19, though some measures were misidentified.               
18034+2324   POU3344     LDS1004.                                                                        
18034+0825   GC 24579    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
18035+4032   COU1785     Systemic mass is estimated at 3.0 +/- 0.6 Msun, assuming a dynamical            
                         parallax of 7.32 +/- 0.10 mas.  This is consistent with a pair of F5            
                         dwarfs. There is no Hipparcos parallax for this star.                   Doc2008a
18037-2423   SBE   1     Aa,Ab: Herschel 36 is a young massive system located at 1.3kpc in the           
                         Hourglass high-mass star-forming region in the central part of the M8           
                         nebula. The Ab component is comprised of two stars, spectral types O9V          
                         and B0.5V, in a close orbit with period 1.54d. The Aa component is of           
                         type O9.5V, and is the most luminous star of the system, dominating             
                         its ionizing flux. Aa and Ab are in an orbit with estimated period              
                         500d and projected semi-major axis 3.5mas. The minimum spectrosopic             
                         predicted mass of the Aa+Ab1+Ab2 system is 45,2 Msun. Arias et al.              
                         (2010, ApJ 710, L30) label the components A, B1, and B2 in their                
                         spectroscopic study of the system.                                      SBe2014 
18039+2639   HO  426     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2014).                         USN2014b
18039-2419   SNA  79     The faint but clear companion at 57mas is not the known SB2 system              
                         (P=3.8d, a sin i = 16Rsun), which is separated by 0.07mas assuming a            
                         distance of 1 kpc (Trepl et al. 2012, MNRAS 427, 1014). Moreover, the           
                         SB2 has nearly equal masses, while the resolved pair has dH=3.4,                
                         pointing to quite different masses. The object is also detected in X            
                         rays. Trepl et al. identified a soft X-ray excess and 10sec pulsation           
                         which they interpret as the signature of a neutron star in the system.          
                         Our detection is probably an active later-type object, which may                
                         provide an alternaitve explanation to the X-ray excess.                 Sna2014 
18039-2422   SNA  78     9 Sgr. The primary is an emmission-line star. PIONIER clearly resolves          
                         the long-period SB2 discussed by Rauw et al. (2012, A&A 542, A95) at a          
                         separation of ~5mas.                                                    Sna2014 
18040+3923   L    19     Not found by van den Bos in 1958. Not the same as STF2275, although     B__1960b
                         some measures were misidentified.                                               
18040-2529   HDO 148     EGB   6.                                                                        
18042-2846   BRT3058     J 1644.                                                                         
18043+4206   COU1786     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.80 +/- 1.44, 3.07, and 1.45 Msun, respectively.             Mlk2012 
18043-4019   WG  222     CPD-40@8381.                                                                    
18044-2423   RBR   8     The X ray flux of the closer E and W companions indicate they are M and         
                         K dwarfs, identifying them as young stars that are physical companions          
                         rather than field stars.                                                        
18044+0337   A  2257     Systemic mass is estimated at 2.9 +/- 0.6 Msun, assuming a dynamical            
                         parallax of 4.73 +/- 0.20 mas.                                          Doc2008a
18044+0329   STF2266     AB: HJL 255.                                                            HJL1986 
18044-5953   RST5099     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.92 +/- 2.31, 2.17, and 0.97 Msun, respectively.             Mlk2012 
18046+5053   STF2279     HJL 256.                                                                HJL1986 
18046-1702   HU  194     Spectrum: Fm Delta Del.                                                         
18047-5913   HJ 5006     LDS 622.                                                                        
                         A is SB1, P=108.55d, incl. brown dwarf SB component: Tinney et al.              
                         (2001 ApJ, 551, 507)                                                    Tok2014d
18048+1253   BPM 719     [PM2000] 1368153 + [PM2000] 1368073.                                    Gvr2010 
18049+0311   BAL2471     J  3341.                                                                        
18050-2935   BLM   5     Aa,Ab: gam 1 Sgr. A is the Cepheid W Sgr, spectrum also variable.               
                         It is a long-period spectroscopic binary and speckle/occultation pair           
                         1976.477: This measurement resolves the variable star.                  BLM1978 
                         Masses are 5.8 and 2.2 Msun. Estimated period = 173y, a = 63au = 0.15". Evs2013 
18051-4040   CPO 571     CPD-40@8400.                                                                    
18053+8129   STF2326     B is BD+81@618.                                                                 
                         Additional notes may be found in Dembowski (1883).                      D__1883 
18053+1400   BPM 720     [PM2000] 1369739 + [PM2000] 1369615.                                    Gvr2010 
18054+1527   BPM 721     [PM2000] 1370110 + [PM2000] 1369687.                                    Gvr2010 
18054-2140   TOK 365     The faint red companion at 6".6 is likely optical. This is a very               
                         crowded field in the direction of the Galactic center. We see another           
                         companion at 10".8, but only in the red channel.                        Tok2013b
18055+0230   STF2272     70 Oph = p Oph. A complicated multiple system with high proper motion,          
                         which has led to some confusion in component identification. A 1924             
                         measure by Burton supposedly of AW was not to the same W component as   Btn1929b
                         measured in earlier VW observations. The Burton secondary is now named          
                         Y. Similarly, See supposedly measured the BR pair; this pair is now     See1911 
                         labelled BZ.                                                                    
                         A component is 70 Oph.                                                          
                         CHARA Array Limb-darkened diameter of A,B:                              CIA2012f
                         R =  0.8310 +/- 0.0044, 0.6697 +/- 0.0089 \rsun,                                
                         L =  0.53 +/- 0.02, 0.15 +/- 0.02 \lsun,                                        
                         Teff = 5407 +/- 52, 4393 +/- 149 K, M = 0.846, 0.698 \msun.                     
                         Spectral types K0V,K4V. Proper motions of A and B are (+276,-1092) and          
                         (+442,-1253), respectively. Proper motion of other components follow:           
                            C : -019-012     D : -002+002     R : -007-007                               
                            S : +005-004     T : +001-006     U : -013-010                               
                            V : +002-014     Y : -023-028     Z : -022+007                               
                         The existence of a third body, for which orbits have been computed, is          
                         now generally discounted as the strong photographic coverage fails to           
                         show any such variation. Batten & van Dessel (1976) discuss the radial  Bte1976 
                         velocities.                                                                     
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         1995.559: Absolute quadrant determined by triple-correlation technique  Pru2002b
                         AB: H 2   4.                                                            MEv2010 
                         AB: Additional notes may be found in Simonov (1937) and                 Smw1937 
                         Fatou (1941).                                                           Fat1941 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.60 +/- 0.22, 1.61, and 1.56 Msun, respectively.  Mlk2012 
                         AC, AD, AR, AS, AT, AU, AV: Optical pairs, based on study of relative           
                         motion of components using the method of apparent motion parameters.    Kiy2008 
                         From their combined speckle/spectroscopic solution, Eggenberger et al.  Egn2008 
                         (2008) derive masses 0.89 +/- 0.02 and 0.73 +/- 0.01 Msun and a                 
                         parallax of 194.2 +/- 1.2 mas. Adopting both asteroseismic and                  
                         non-asteroseismic observational constraints with several models, they           
                         derive an age of 6.2 +/- 1.0 Gyr, an initial helium mass fraction Y =           
                         0.266 +/- 0.015, and an initial metallicity (Z/X) = 0.0300 +/- 0.0025.          
                         AS: Additional notes may be found in Burnham (1894).                    Bu_1894 
                         AR, AT, AU, AV, BR: Rectilinear solutions by Hurowitz et al. (2014).    USN2014b
18057+1200   STF2276     A is a spectroscopic binary, and B is a variable of the Beta CrB-type.          
                         AB: H 3  56.                                                            MEv2010 
18057-3437   HJ 5012     B is CD-34@12450.                                                               
18058+2127   STT 341     Triple solution with C (HIP 88639). Primary is 0.88d RS CVn-type                
                         variable or eclipsing binary (V772 Her).                                Sod1999 
                         Combined visual-spectroscopic orbits by Heintz (1982); the lines were   Hei1982b
                         separated at periastron passage. Star A is an eclipsing SB1, P = 0.88d  Hei1982e
                         (Batten et al. 1979).                                                   Bte1979 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.47 +/- 0.51, 2.06, and 2.00 Msun, respectively.  Mlk2012 
                         AB: A is SB1E, P=0.870d. AB is SB2, P=20.081y                           Tok2014d
                         AB,C: C is SB2, P=25.763d                                               Tok2014d
18059-2134   ARA1507     Aka J  1736.                                                                    
18060+0434   STTA165     B is BD+04@3594.                                                                
18060-0807   A  2595     A is SB, no SB orbit.                                                   Tok2014d
18060-1412   HD 165319   The classification and distance are from Crampton & Fisher (1974 Pub            
                         DAO 14, 283).                                                           Msn1998a
18060-2238   BRT1513     J 2099.                                                                         
18060-3018   BRT3059     A likely plate flaw.                                                    Grv2021b
18061+1257   BPM 722     [PM2000] 1372670 + [PM2000] 1372512.                                    Gvr2010 
18061-2412   SNA  81     Aa,Ab: We detect a third companion to this SB2 4.6d eclipsing binary            
                         system (Otero 2007, Open European Journal on Variable Stars 72, 1;      MyP2013 
                         Mayer et al. 2013).                                                     Sna2014 
18062+1427   BPM 723     [PM2000] 1373116 + [PM2000] 1372803.                                    Gvr2010 
18063+6543   LDS1461     NLTT 45993/45994                                                        Chm2004 
18063+3824   HU 1186     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.00 +/- 0.69, 2.28, and 1.10 Msun, respectively.             Mlk2012 
18064-4145   HJ 5011     B is CD-41@12402.                                                               
18065+0920   HZG  12     B is BD+09@3560.                                                                
18066+4616   HD166067    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
18067+1359   AG  358     AB = J    94.                                                                   
18068+0853   BUP 179     Soulie (1984) misidentified Burnham's C component; this pair has been   Sle1984 
                         designated SLE 133AF. There is apparently an error in the declination           
                         of Soulie's D component.                                                        
                         BG: This pair was erroneously identified as BC.                                 
             GC 24683    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
18068-4325   HJ 5014     Quoted errors in P and a for the Argyle et al. (2002) orbit are         Ary2002b
                         +170/-97y, +0".66/-0".41, respectively.                                         
                         Member of the bet Pic moving group.                                     Zuc2001b
18069+1712   BPM 724     [PM2000] 1375827 + [PM2000] 1375834.                                    Gvr2010 
18070+3034   AC   15     99 Her.                                                                         
                         Identification of the ascending node is not very certain.               Hei1972 
                         Kennedy et al. (2012) derive a system mass of 1.4 Msun, using the van           
                         Leeuwen(2008) distance 15.64pc. Using the spectroscopic mass function   VlF2008 
                         of Abt & Willmarth (2006), this yields component masses 0.94 and 0.46   AbH2006 
                         Msun for A and B, respectively.                                         Knd2012 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.73 +/- 0.23, 1.85, and 1.13 Msun, respectively.  Mlk2012 
18071+4943   STT 344     A is a spectroscopic binary.                                                    
18071+3223   HJ 1314     SEI 557.                                                                Nsn2017b
18071-4949   I  1350     I 1350a.                                                                        
18073+0934   STT 342     72 Oph. Spectroscopic binary.                                                   
18074+1817   BPM 725     [PM2000] 1377794 + [PM2000] 1377731.                                    Gvr2010 
18074-3011   B  1350     Spectrum: B9.5/A0IV/V.                                                          
18074-4644   SHY 737     HIP  88782 + HIP  87887.                                                        
18075+4552   KUI  85     Nova Herculis. Not a true visual double star, but the system contains           
                         the eclipsing binary DQ Her.                                                    
18075+2846   STA   2     omi Her = 103 Her. A spectroscopic and interferometric binary.                  
                         1981.373: Result needs further confirmation.                            Tok1980 
18075+1443   BPM 726     [PM2000] 1377872 + [PM2000] 1377790.                                    Gvr2010 
18078+2606   CHR  67     100 Her. One component is variable.                                             
             STF2280     AB: H 3  41.                                                            MEv2010 
18078+1304   H 5  74     H V 74.                                                                         
18079+0153   OSO  93     G020-024. AC, AD, and AE are not common proper motion pairs, based on           
                         color and/or comparison with POSS2 red plates                           Oso2004 
18079-2141   ARA1513     J  2195.                                                                        
18080-1637   RST3996     There was a large change, angle decreasing, during the unobserved               
                         interval 1951-1990.                                                             
18081+3449   POP 211     Aka POP1223.                                                            Dam2016d
                         Codiscovered by Popovic and Olevic.                                     Ole1970b
18081+1232   BPM 727     [PM2000] 1380283 + [PM2000] 1380212.                                    Gvr2010 
18081-2827   WRH  22     Removed from WDS as probably not real.                                          
18082+1059   BPM 728     [PM2000] 1380774 + [PM2000] 1381049.                                    Gvr2010 
18083+2941   LAF  60     Aa,Ab: YSC  65.                                                                 
                         Aa,Ab & Aa,Ac may be the same.                                                  
18088+2049   AGC   8     102 Her. A is a suspected spectroscopic binary.                                 
18089+1802   BPM 729     [PM2000] 1383311 + [PM2000] 1383424.                                    Gvr2010 
18089-2528   WNO  21     One component is a Beta Lyrae-type system, V3792 Sgr.                           
18089-3313   BRT1758     A likely plate flaw.                                                    Grv2021b
18090+2851   BRT  33     A likely plate flaw.                                                    Grv2021b
18090+2409   TOK 318     A is possibly SB, no orbit.                                             Tok2014d
18090+1610   BPM 730     AB: [PM2000] 1383786 + [PM2000] 1384274.                                Gvr2010 
             BPM 731     BC: [PM2000] 1384274 + [PM2000] 1384683.                                Gvr2010 
18090-3617   SHY 738     AB: HIP  88920 + HIP  88351.                                                    
18091+3101   BLL  31     A is the Mira-type system T Her. B is BD+31@3185.                               
18092+1458   BPM 732     [PM2000] 1384749 + [PM2000] 1384733.                                    Gvr2010 
18092-2211   RST3157     Poor fit for visual observations, speckle needed.                               
                         Soderhjelm notes poor Hipparcos solution.                               Sod1999 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.04 +/- 1.19, 1.48, and 0.73 Msun, respectively.             Mlk2012 
18093+1648   BPM 733     [PM2000] 1384997 + [PM2000] 1385231.                                    Gvr2010 
18093+1105   BPM 734     [PM2000] 1385001 + [PM2000] 1384518.                                    Gvr2010 
18093+0909   RUC  24     Primary is V839 Oph.                                                            
18093-2359   VSP  65     V3903 Sgr = 11 Sgr. The classification and orbit are from Niemela &             
                         Morrison (1988 PASP 100, 1436).                                         Msn1998a
18093-2607   B   379     HIP 88937. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
18096+3827   LUH  13     GJ 706 + WISE J180901.07+383805.4. Companion is likely not physical,            
                         based on proper motion.                                                 Luh2012b
18096+1255   BPM 736     [PM2000] 1386179 + [PM2000] 1386086.                                    Gvr2010 
18096+1106   BPM 735     [PM2000] 1386060 + [PM2000] 1386113.                                    Gvr2010 
18096+0400   STF2281     73 Oph. AB: H 1  87.                                                    MEv2010 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.21 +/- 1.75, 3.00, and 1.35 Msun, respectively.  Mlk2012 
18099+2128   LAW   6     Spectral types M5-M6 for both components, masses 0.124-0.109 and                
                         0.101-0.112 Msun, distance 41.8 +/- 4.4 pc                              Law2006 
18099+0307   YSC 132     Aa,Ab: For the Horch et al. (2015) combined solution, spectroscopic             
                         elements are fixed to those of Griffin (1999). Assigned spectral types  Grf1999d
                         for Aa and Ab are F7V and F7.5V; derived masses 1.26 and 1.23 Msun.     Hor2015 
                         Aa,Ab: SB2, P=199.55d                                                   Tok2014d
             BU  637     AB: A is a spectroscopic binary.                                                
                         HIP 89000. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
18100-4852   HJ 5017     B is CD-48@12312.                                                               
18101+1629   STF2289     A premature orbit has been computed.  The positional elements - not             
                         given by Hopmann - were reconstructed from his ephemeris.               Hop1964b
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         1995.553, 1998.657: Absolute quadrant determined by triple-correlation          
                         techniques.                                                             Pru2002b
18101-3044   BU  245     HDO 149                                                                         
18102+3402   STF2291     SEI 558.                                                                Nsn2017b
18102-7859   HJ 4988     SWR 236. CPM pair                                                       Skf2004 
18103+0235   BU  638     BC: No measures since 1929. Probably unchanged. IDS estimates for dm            
                         incorrect.                                                              Wor1967b
18105-2934   BRT3328     A likely plate flaw.                                                    Grv2021b
18106+1155   BPM 737     [PM2000] 1389911 + [PM2000] 1389794.                                    Gvr2010 
18106-1645   S   700     A 4th star "nearly south".                                                      
                         Primary is eclipsing binary of Algol-type, ecc, period 7.8075 d.        Zas2012 
18107-4032   HJ 5025     B is CD-40@12231.                                                               
18111+3241   TOK 615     BC: UC 3529.                                                                    
18112-1723   RST3161     Composite spectrum G5+A0.                                                       
18112-1951   BU  132     Same as SEE 501. A third component is indicated by lunar occultation.           
18112-4557   HDO 286     eps Tel                                                                         
18114+3506   ALI 140     Also known as POP  78.                                                          
18115+1455   OSO  94     G140-044. Not a common proper motion pair, based on color and                   
                         comparison with POSS2 red plates.                                       Oso2004 
18115+1307   BPM 738     [PM2000] 1393525 + [PM2000] 1393886.                                    Gvr2010 
18116+1126   BPM 739     [PM2000] 1394117 + [PM2000] 1393941.                                    Gvr2010 
18116-4035   WG  227     BRT1029.                                                                Brt1933 
18117-2342   HJ 5030     11 Sgr.                                                                         
18118+3327   B  2545     Called a spectroscopic binary. Variation undoubtedly due to motion in           
                         the visual orbit.                                                               
                         1979.360: Theta incorrectly given as 42.4 deg in McAlister & Hendry.    McA1982d
                         1980.4768: Rho incorrectly given as 0".091 in McAlister et al (1983)    McA1983 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 6.14 +/- 2.37, 7.96, and 2.00 Msun, respectively.  Mlk2012 
18118+1147   BPM 740     [PM2000] 1394874 + [PM2000] 1394617.                                    Gvr2010 
18118-1825   HJ 2820     Aka OL  163.                                                                    
18120+4355   ES 1419     Rectilinear solution by Cvetkovic et al. (2019).                        Cve2019b
18120+2640   BRT3329     Originally published as BRT 180.                                        Brt1928 
18121+0207   BAL1957     J 1829.                                                                         
18122+0453   BAL2918     Another yet fainter pair os 1' NW of this.                              Hei1978b
18124+0524   OSO  95     G140-046. Not a common proper motion pair, based on color and                   
                         comparison with POSS2 red plates.                                       Oso2004 
18125+1701   BPMA 52     [PM2000] 1397712 + [PM2000] 1398923.                                    Gvr2010 
18125-1852   VAT   2     J 1737.                                                                         
18126+4033   OSO  96     G204-049. Common proper motion pair.                                    Oso2004 
18126+3836   BU 1091     Prieur et al. (2012) derive a dynamical parallax of  6.0 mas and                
                         (using their orbital elements and the revised Hipparcos parallax of             
                         van Leeuwen 2007 A&A 474, 653) a total mass 2.2 +/- 0.9 Msun.           Pru2012 
18126+1107   BPM 741     [PM2000] 1398075 + [PM2000] 1397943.                                    Gvr2010 
18127+5446   MLR 585     GZ Dra - Algol-type eclipsing binary, P = 2.25335 d.                    Zas2011 
18128+1329   BPM 742     [PM2000] 1398813 + [PM2000] 1398870.                                    Gvr2010 
18128+1151   BPM 743     [PM2000] 1399144 + [PM2000] 1399290.                                    Gvr2010 
18128+0356   J  3270     Heintz equates this with BAL2482.                                       Hei1995 
18128-1618   HJ 2821     Spectrum: B5/7II/III.                                                           
18129-4959   HRG 128     B  2434.                                                                        
18130+4251   ES  473     B is BD+42@3026.                                                                
18130+2815   H 5  93     H V 93. B is BD+28@2956.                                                        
                         HJL 258.                                                                HJL1986 
                         SHY 739. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
18130+1138   BPM 744     [PM2000] 1399708 + [PM2000] 1399455.                                    Gvr2010 
18130-2307   EVS  34     Primary is the Cepheid AP Sgr. 12 Sgr.                                  Evs2016a
18130-2704   J  2199     CPD-27@6260.                                                                    
18131+2602   BWL  48     AD: Colors and/or astrometry are inconsistent with a late-type common           
                         proper motion companion based on visual inspection of the field from            
                         2MASS, SDSS, DSS1, and/or DSS2. Primary is GJ 4044.                     Bwl2015 
18131-2025   ARA1141     Aka J  1621.                                                                    
18133-4410   BRT1031     CPD-44@9008.                                                                    
18133-6513   NZO  89     SWR 238. CPM pair                                                       Skf2004 
18135-4230   BRT1033     A likely plate flaw.                                                    Grv2021b
18136+3249   GIC 150     G206-017/G206-018.                                                              
                         NLTT 46138/46139                                                        Chm2004 
                         NLTT 46138.  White dwarf pair = WD 1811+33 = EGGR 373/330               Grn1986 
18138+6235   ES 1836     LDS2408.  WDS designation for ES 1836 was incorrect, so designation             
                         for LDS pair was adopted.                                                       
18138-1904   ARA 735     The primary is the planetary nebula NGC 6567.                           Skf2013 
18138-2104   H 5   7     H V 7. mu Sgr = 13 Sgr = Polis. A is an Algol-type system and                   
                         occultation binary.                                                             
18139+6424   RDR   7     CHARA Array Limb-darkened diameter of A :                               CIA2013c
                         R =  1.7577 +/- 0.0225 \rsun, L =   4.1486 +/-0.0325 \lsun,                     
                         Teff = 6221 +/-  39 K, M = 1.156 \msun, Age = 5.0 Gyr.                          
18140+2017   HO  268     "Always seen single Flower Obs."                                        Bu_1906 
18140-2052   J  1622     CPD-20@6887. ARA1142.                                                           
18140-5342   BRT2099     A likely plate flaw.                                                    Grv2021b
18141-1912   CHR 234     First detected as an occultation binary by Evans & Edwards              Evn1981 
18141-2201   BRT1520     CD-22@12732.                                                                    
18142+6445   COM   4     B is BD+64@1251.                                                                
18143+1333   BPM 745     [PM2000] 1404868 + [PM2000] 1404985.                                    Gvr2010 
18143-4309   SHY 740     HIP  89373 + HIP  89274.                                                        
18144+2127   HJ 2828     B is BD+21@3356.                                                                
                         HJL 259.                                                                HJL1986 
18145+1752   BPM 746     [PM2000] 1405737 + [PM2000] 1406209.                                    Gvr2010 
18145-6929   GLI 242     Also known as TOB 347.                                                          
18146-4625   CPO 578     SWR 239.                                                                        
18146-4722   HJ 5031     B is CD-47@12140.                                                               
18147+5635   BU 1274     A is a spectroscopic binary.                                                    
18147-1939   J  1623     CPD-19@6670.                                                                    
18148-0441   HJ  856     B is BD-04@4423.                                                                
18148-5350   BRT2100     A likely plate flaw.                                                    Grv2021b
18150+3840   LDS4781     NLTT 46179/46180                                                        Chm2004 
18150+1338   BPM 747     [PM2000] 1407711 + [PM2000] 1408069.                                    Gvr2010 
18150-1955   HJ 2823     B is BD-19@4922.                                                                
18150-5018   I   429     Measures scattered, but probable rapid motion.                                  
18151+1415   BPM 748     [PM2000] 1408129 + [PM2000] 1408042.                                    Gvr2010 
18151-5751   HJ 5029     A=SB? no SB orbit.                                                      Tok2014d
18152+1446   BPM 749     [PM2000] 1408559 + [PM2000] 1408870.                                    Gvr2010 
18152-2023   BU  286     16 Sgr. A is a spectroscopic binary.                                            
             CHR 255     Aa,Ab: Garmany et al. (1980 ApJ 242, 1063) observed a smoothly-varying          
                         velocity indicating that the A component is probably a single-lined             
                         binary with a period of 11 d.                                                   
                         Lindroos (1985) provided the classification of the B component and      Lnd1985 
                         determines a distance of 1.2 kpc.                                       Msn1998a
             SNA  83     16 Sgr. SB. See discussion of system by Sana et al. 2014).              Sna2014 
18152-2044   SNA  82     Aa,Ab: 15 Sgr. The primary is a blue supergiant star. PIONIER resolved          
                         a close pair at ~3mas at three epochs, revealing evidence of orbital            
                         motion. This pair likely corresponds to the 668d SB1 obtained by OWN            
                         (Sota et al. 2014, ApJS 211, 10).                                       Sna2014 
18154+3836   MLB 852     Aka ALI 869.                                                                    
18154-4851   HJ 5033     AD: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
18155+1825   BPM 750     [PM2000] 1409823 + [PM2000] 1409869.                                    Gvr2010 
18155-0220   LDS6324     NLTT 46171/46172                                                        Chm2004 
18155-1840   SEE 349     Component not seen in 1934 with 36-inch.                                Kui1961b
18156+1614   LDS1008     A possible wide companion to 2MASS J18153459+1614253 at 13" is noted            
                         in WDS. The star is however single within the AstraLux field of view.   Jnn2012 
18157-6233   B  1880     AB = SWR 240. CPM pair                                                  Skf2004 
18157-6303   HJ 5024     B is CPD-63@4344.                                                               
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2014).                         USN2014b
18158+4107   ES 1651     A is the Beta Lyrae-type system TZ Lyr, P = 0.52d.                              
18158+1516   BPM 751     [PM2000] 1411272 + [PM2000] 1411318.                                    Gvr2010 
18159-2716   J  2201     CPD-27@6313.                                                                    
18159-4412   GC 24892    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
18160-1006   HU   58     A    38 is identical                                                    Hei1978b
18160-5333   HJ 9004     Previously known as HJ 5453a.                                                   
18162+0434   STTA167     B is BD+04@3677.                                                                
18163-2253   BRT1522     CD-22@12777.                                                                    
18164+2912   OSO  97     G206-020. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
18164+1201   BPM 752     [PM2000] 1413857 + [PM2000] 1414013.                                    Gvr2010 
18164-4638   SWR 241     CPM pair                                                                Skf2004 
18165+2324   BUP 180     BC: Determined to be the same as 18166+2327 POU3376 by Clif Ashcraft.           
18165-1652   HJ 2826     Also known as J  1625 or WHC  16.                                               
18165-2748   RST2043     CPD-27@6328.                                                                    
18166-2033   MCA  51     17 Sgr.                                                                         
18168-1631   SNA  84     We detect three previously unreported distant companions in the NACO            
                         FOV, but lack PIONIER observations to investigate possible closer               
                         companions. The object was reported as SB1? by Abt et al. (1972), a     AbH1972b
                         fact not confirmed by Chini et al. (2012), who prefer a RV stable       Cii2012 
                         classification.                                                         Sna2014 
             HD 167633   LS 4864. Additional radial velocities are reported by Crampton &                
                         Fisher (1974 Pub DAO 14, 283).  The star appears within the boundaries          
                         and at the same distance of Ser OB1 in the LSC.                         Msn1998a
18170-1858   SNA  85     Aa,Ab: Both NACO/SAM and PIONIER resolved the A componnet as a 50mas            
                         pair, which probably corresponds to the 80mas pair detected through     Rad1980 
                         occultation (Radick & Lien 1980). The object may further be an SB1              
                         (Gamen et al. 2008, RevMexAA 33, 54)                                    Sna2014 
             HD 167659   Hilt 730. The 3 speckle observations all indicate a single star, so we          
                         cannot confirm the existence of a companion found by lunar occultation  Msn1998a
                         (Radick & Lien 1980).                                                   Rad1980 
18170-1933   B  2862     J 1626.                                                                         
18171+1706   BPM 753     [PM2000] 1416611 + [PM2000] 1416469.                                    Gvr2010 
18171-1700   WSI 143     AD: Originally assigned to HJ 2826.                                     WSI2010 
                         Correct ID provided by Friedrich Damm.                                  Dam2012 
18172+1517   BPM 754     [PM2000] 1417297 + [PM2000] 1417367.                                    Gvr2010 
18172+0735   J  2514     Pair is BD+07 3619.                                                     J__1948 
18174-1920   B  2863     CPD-19@6748.                                                                    
18174-4929   HDS2586     SHY 743. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
18175+1647   BPM 755     [PM2000] 1418633 + [PM2000] 1418360.                                    Gvr2010 
18175-1638   HJ 2829     Spectrum: B2/3II/III.                                                           
18175-1828   RST3170     The classification of the close spectroscopic pair is from Morrison &   Cti1978 
                         Conti (1978), and that of the B component of the optical pair is from   Lnd1985 
                         Lindroos (1985). Lindroos also gives a distance of 2.0 kpc.             Msn1998a
18176-3406   HJ 5036     A is the Algol-type system RS Sgr.                                              
18176-3646   BU  760     eta Sgr. A is an irregular variable.                                            
18177+4122   LDS4783     NLTT 46260/46265                                                        Chm2004 
18180+3846   GIC 151     G204-058/G204-057 = GJ 4048A/4049B. PM of A -330-1039, B -330-1039              
                         NLTT 46274/46272                                                        Chm2004 
18181+1559   BPM 757     [PM2000] 1421149 + [PM2000] 1421222.                                    Gvr2010 
18181+1454   BPM 756     [PM2000] 1421047 + [PM2000] 1421519.                                    Gvr2010 
18181-1215   TRN  27     MY Ser.                                                                         
             TRN  27     The image rotator was in an unknown state, so two possible theta                
                         values are listed for the 2001.7447 observation - one for zenith up             
                         and one for north up.                                                   Trn2008 
             HD 167971   Leitherer et al. (1987 A&A 185, 121) argue that this is a triple                
                         system consisting of a close eclipsing pair and a brighter, distant O           
                         star; the spectral classification presumably applies to the latter              
                         star.                                                                   Msn1998a
             DBK   1     Aa,Ab: System includes a 3.3d eclipsing binary, unresolved in the VLTI          
                         observations. De Becker et al. (2012) assume the components of the              
                         close pair are both O6.5V, and the wide component is O8I. V=7.35 for            
                         the system yields a distance of about 1.8 kpc, in good agreement with           
                         the 1.7 kpc distance determined by Reipurth (2008 Handbook of Star              
                         Forming Regions, vol 2, 590) for the NGC 6604 open cluster.  The Aa,Ab          
                         orbit is thought to be very eccentric.                                  DBk2012 
18186-1348   DCH  26     The AB pair is visible as SBA in spectroscopy, although no orbital              
                         motion is detected (Sana et al. 2009), inagreement with the large       Sna2009 
                         separation, hence very long period.  Five other faint companions are            
                         detected in the NACO FOV.                                               Sna2014 
18186+1538   BPMA 53     [PM2000] 1423159 + [PM2000] 1423708.                                    Gvr2010 
18187-1206   SNA  90     Aa,Ab: Object is a non-thermal radio emitter (DeBecker et al. 2004).    DBk2004 
                         PIONIER clearly resolved it into a tight pair (3.3mas) with almost              
                         equal brightness (dH=0.17 +/- 0.19).                                    Sna2014 
18187-1837   BU  639     There was a close approach around 1900.                                         
                         Large divergences in estimated distance due to considerable southern            
                         declination.                                                            Vou1951 
                         1994.5191: Quadrant determined by speckle imaging analysis              Hor1996 
18188+4510   WOL   2     WSP  58.                                                                        
18188-3048   BRT3064     A likely plate flaw.                                                    Grv2021b
18189-1348   SNA  91     Aa,Ab: The A component is an O7V+O8V 912d SB (Sana et al. 2012) that    Sna2012 
                         we marginally resove with PIONIER at 6mas separation.                   Sna2014 
18189+3918   MLB1078     ES 2570.                                                                        
18192+2427   105 Her     Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Radford & Griffin (1977).                                               Grf1977b
18192+1116   BPM 758     [PM2000] 1426022 + [PM2000] 1425922.                                    Gvr2010 
18196+3915   MLB 754     Not found by Heintz at IDS position.                                    Hei1985a
18196-1944   WRH  30     SEE 501 is probably BU 132.                                                     
18197+1016   HU  197     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.20 +/- 0.69, 1.95, and 1.05 Msun, respectively.             Mlk2012 
18197-4542   CHR 148     HD 167954 is a SB, with P = 120d (Bopp et al. 1970 MNRAS, 147, 355).            
                         With rho = 0".031, the speckle pair is probably not the SB.             McA1990 
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Bopp et al. (1970).                                                     Evn1970 
18198-0458   SCJ  16     A = QS Ser, false HIP variable (GCVS), artifact of scanning binary.     Tok2014d
18199+1524   BPM 759     [PM2000] 1429486 + [PM2000] 1429612.                                    Gvr2010 
18200+0212   BAL1964     A likely plate flaw.                                                    Grv2021a
18201+2532   STF2309     H 1  86.                                                                MEv2010 
18201-0936   GJ 4052     No comoving objects found within separation/magnitude range listed.             
                         However, Chauvin et al. (2006) note finding at least one faint          Cvn2006 
                         background object.                                                              
                         HD 168443. Combined astrometric/spectroscopic solution, using                   
                         spectroscopic elements (P,T,e,omega) from Wright et al. (2009 ApJ 693,          
                         1084).                                                                  SaJ2011 
18202-3601   BRT1769     CPD-36@8160.                                                                    
18204-1011   HER   2     A post-T Tauri star, FK Ser.                                                    
18205-5107   BRT1043     SWR 242.                                                                        
18205-5344   FIN 264     Spectrum: G0/5III+A7/F0.                                                        
18206+1608   OSO  98     G184-004. Not a common proper motion pair, based on color and                   
                         comparison with POSS2 red plates.                                       Oso2004 
18207+2530   BRT3330     Originally published as BRT 181.                                        Brt1928 
18208+7120   STT 353     phi Dra = 43 Dra. A premature orbit has been computed.                  D__1883 
                         Almost rectilinear relative motion, long period!                        Ole1975b
                         Period of A (SB1) is 127.99d.                                           XXX2016 
                         An Alpha CVn type variable.                                                     
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Also an unresolved 128.165d spectroscopic binary.                       Mug2017b
18208+2732   BU  640     Measure by Van Biesbroeck in 1932 is undoubtedly in error.              Baz1944a
                         CfA: A is SB, P=long. Triple or not? Makarov & Kaplan (2005): dmu=20.4  Mkr2005 
                         (HIP2:20.1), implies triple.                                            Tok2014d
18209+1153   BPM 760     [PM2000] 1434041 + [PM2000] 1433558.                                    Gvr2010 
18209+0323   HJ 5495     74 Oph.                                                                         
18210-0101   WOR  35     This is the nearby star G 21-10 = GJ 1226 = LHS 463 = LP 630-1.                 
18210-1714   J  1627     J  1739.                                                                J__1962a
18210-2842   B  2864BC   A likely plate flaw.                                                    Grv2021b
18210-2950   SEE 350     del Sgr = 19 Sgr = Kaus Media                                                   
18211+7244   LAB   5     Aa,Ab: chi Dra = 44 Dra. Astrometric, interferometric, and                      
                         spectroscopic binary.  See discussion of the RV's by J. Vinter Hansen           
                         (Lick Obs. Bul. 19, 141, 1942).                                                 
                         See discussion and orbital elements by Labeyrie et al. (1974).          Lab1974 
                         P, T, and e for Alden (1936) solution taken from spectroscopic orbit    Ald1936c
                         Speckle and spectroscopic orbit by Tomkin et al. (1987), used P,e       Tom1987 
                         fixed from spectroscopy. Positional elements disagree somewhat with             
                         those of the astrometric orbit (prior to resolution of the companion)           
                         by Breakiron & Gatewood (1974).                                         Brk1974 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Analyses of the spectroscopic/interferometric orbit are given by        McA1980b
                         McAlister (1980) and McA1980c and Tomkin et al. (1987).                 Tom1987 
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Tomkin et al. (1987).                                                   Tom1987 
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         The Farrington et al. (2010) orbit is based on speckle plus K'-band     CIA2010 
                         CHARA Array separated fringe packet observations. An orbital parallax           
                         of 123.4+/-1.9 mas is determined.  Based on the mass ratio                      
                         determination of Nordstrom et al. (2004 A&A 418, 989), derived masses           
                         are 0.96+/-0.03 and 0.75+/-0.03 Msun, well below the expected masses            
                         for an F8IV-V and late-G/early-K dwarf pair. The aperture and method,           
                         8m and speckle, are set to give the resolution capability of this               
                         technique, which is less than classical interferometric methods.                
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 1.71 +/- 0.06, 2.07, and 1.13 Msun, respectively.  Mlk2012 
18211-1339   RST9006     Previously known as RST4585a.                                                   
18212+5917   LDS2411     LDS5235.                                                                        
18213-0254   STFB  8     eta Ser = 58 Ser                                                                
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         H 6  14.                                                                MEv2010 
18214+1259   BPMA 54     [PM2000] 1436289 + [PM2000] 1436037.                                    Gvr2010 
18214-1852   EVS  35     Primary is the Cepheid Y Sgr.                                           Evs2016a
18216+3842   LDS5861     LDS6327.                                                                        
18216-2052   BRT1530     ARA1148.                                                                        
18218+3038   L    21     Appears to be 10deg error in converting Lewis' NPD to Dec for IDS.      L__1900 
18218-1155   EGN  22     AB, AC, and AF pairs unbound; D, E, G, H, and R likely unrelated as             
                         well. Bound/unbound nature of other components is inconclusive.                 
                         Primary is planet host star.                                            Egn2007 
18219+1631   BPM 761     [PM2000] 1438334 + [PM2000] 1437857.                                    Gvr2010 
18220+1621   BPM 762     [PM2000] 1438974 + [PM2000] 1438640.                                    Gvr2010 
18220+1348   BPM 763     [PM2000] 1439257 + [PM2000] 1439185.                                    Gvr2010 
18220-2233   J  2208     CPD-22@6959.                                                                    
18221+5336   BEM  32     ES  649.                                                                        
18222-5534   DUN 220     B is CPD-55@8630.                                                               
                         Primary is QW Tel, a W UMa type eclipsing binary, P = 0.411928d.        Zas2012 
18223+1713   BPMA 55     [PM2000] 1440461 + [PM2000] 1440291.                                    Gvr2010 
18223+1547   BPM 764     [PM2000] 1440458 + [PM2000] 1440241.                                    Gvr2010 
18223-1437   J   519     Additional companion at 222deg, 15", mag 14.5                           J__1946 
18223-2018   BHA  27     J  1628.                                                                Nsn2016 
18224+4545   A   700     Round 1951-1954. Possible quadrant change.                                      
                         Increasing residuals since the orbital solution by Heintz (1998) led    Hei1998 
                         to the determination by Parent et al. (2017) that the relative motion           
                         of the pair was better represented by a rectilinear fit. Thus the pair          
                         appears to be an optical double rather than a physical binary.          CC_2017b
                         Rectilinear solution by Parent et al. (2017).                           CC_2017b
18226+0852   SLE 163     There is apparently a 7s typo in RA of primary by Soulie (1984).        Sle1984 
18228-1727   J  2210     This pair had the wrong coordinate. The correct coordinates were found          
                         by Brian Skiff (Lowell) and the pairs recovered in the 2MASS data.      Skf2004 
18228-1843   CHR 235     First detected as an occultation binary by Africano.                    Afr1978 
18229+1458   HU  581     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.18 +/- 1.48, 2.25, and 1.05 Msun, respectively.             Mlk2012 
18229-1726   J  2209     This pair had the wrong coordinate. The correct coordinates were found          
                         by Brian Skiff (Lowell) and the pairs recovered in the 2MASS data.      Skf2004 
18231+1125   BPM 765     [PM2000] 1444071 + [PM2000] 1444438.                                    Gvr2010 
18231-6235   CPO  79     SWR 244.                                                                        
18232-6130   GLE   2     xi Pav. A is a long-period spectroscopic binary.                                
                         Dynamical elements for Alden's orbit were obtained from a               Ald1946 
                         spectroscopic orbit. Alden's orbit was rejected from the Fourth                 
                         Orbit Catalog ("amplitude below noise level")                           Wor1983 
18236-2610   HO  566     If the quadrants are correct, a revolution has been completed.                  
18237+2146   STT 587     AB: 109 Her.                                                                    
                         Mk III Limb-darkened diameter  4.8   +/- 0.4   mas.                     MkT1989 
18237-2209   BRT1534     J 2126.                                                                         
18237-5841   SWR 246     CD-58@ 7043. CPM pair                                                   Skf2004 
18238+5139   ES  187     AB: B is SB1, P=126.38d                                                 Tok2014d
18238+2808   GRV1261     Both A and B have approximately the same radial velocity.               Grv2019b
18239+5848   STF2323     39 Dra. STTA169 = STFA 36. A is a double-lined spectroscopic binary.            
                         C is a spectroscopic binary, P =2.71d.                                          
                         AC: HJL1098.                                                            HJL1986 
                         AB: H 1   7.                                                            MEv2010 
18240+3844   HO  432AB   This cannot be the close 2347.9-d spectroscopic binary, who postulated  Grf2010d
                         a dm of 6 and a separation of 6 mas.                                            
18240-3516   BRT1773     A likely plate flaw.                                                    Grv2021b
18241-1734   J  2127     Jonckheere gives angle as 40@ in his 1962 catalog.                      J__1962a
18242-3423   SEE 351     eps Sgr = 20 Sgr = Kaus Australis.  Infrared excess and probable                
                         circumstellar disk. Spectral peculiarities lead to classification               
                         problems. Alternative types B9IVp, A0II(shell)                                  
                         Intensity Interferometer Limb-darkened diameter 1.44 +/- 0.06 mas.      HBr1974 
18243-0405   YSC  67     AB + TOK 420Aa,Ab: The neglected pair YSC 67 turned out to be a new             
                         triple. The outer 0".35 binary AB was known previously, now we detect           
                         elongation that implies an inner subsystem Aa,Ab. We compared with              
                         stars in the same area of the sky observed before and after to assure           
                         that the elongation is not of instrumental origin; it is seen in two            
                         filters.                                                                Tok2015c
18243-4407   DUN 221     B is CD-44@12570.                                                               
18244-2932   RSS  31     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
                         Statistically the same parallax within the errors would indicate the            
                         components are physical.                                                        
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
18247-1648   KRV  49     Classical Cepheid XX Sgr.                                                       
18250+2724   STF2315     A is a spectroscopic binary.                                                    
                         AC: 1898 distance probably in error.                                            
18250-0135   AC   11     Spectrum composite; A9III+F6III.                                        Egg1947 
                         Additional notes may be found in Eggen (1947) and Voute (1951).         Vou1951 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 9.58 +/- 9.12, 4.69, and 1.45 Msun, respectively.             Mlk2012 
18251+3016   GIC 152     G206-030/G206-031.                                                              
                         NLTT 46462/46463                                                        Chm2004 
18251+1623   BPM 766     [PM2000] 1454337 + [PM2000] 1454586.                                    Gvr2010 
18251+1152   BPM 767     [PM2000] 1454346 + [PM2000] 1454212.                                    Gvr2010 
18251+0258   BAL1965     J 2579.                                                                         
18252+0720   LDS1011     LDS5236.                                                                        
18253+4846   HU   66     Van Biesbroeck (1954) was unable to resolve this system in 1943,                
                         1944 or 1945 on the 82-inch telescope at the McDonald Observatory.              
                         However, since he resolved the system successfully in 1946 with the             
                         same telescope, and in 1940 with a smaller (40-inch) telescope, the             
                         non-resolution is probably due to bad seeing or ID error.               USN2002 
             STT 351     AC: Additional notes may be found in Muller (1955).                     Mlr1955c
18253+4653   BU  134     Also known as STT 543.                                                          
18253-3701   BRT1776     A likely plate flaw.                                                    Grv2021b
18254+1142   BPM 768     [PM2000] 1455453 + [PM2000] 1455388.                                    Gvr2010 
18254-1631   HU   64     Mt. Wilson spectral classes F5s and G0.                                         
18254-2033   JC    6     21 Sgr.                                                                         
18255-1241   RY Sct      This massive binary and its surrounding gas torus are described by              
                         Gehrz et al. (1995 ApJ 439, 417). A light curve from  Hipparcos is now  HIP1997a
                         available.  The system mass and the nature of the secondary are still           
                         controversial (Skulskii 1992 SvA 36, 411; Skulskii & West 1993 Astron.          
                         Rep. 37, 594; Golovatyi & Skul'skii 1992 SvA 36, 550).  We found a              
                         possible binary companion at a separation of 0".2 which needs                   
                         confirmation.                                                           Msn1998a
18255-6301   ARY 108AC   Author listed the B component as a new component of 18231-6235 CPO 79.  Ary2014b
                         Corrected by USNO.                                                              
18255-6605   HJ 5039     B is CPD-66@3337.                                                               
18256+0802   STT 348     The zeta Aurigae-type binary V2291 Oph. Visual duplicity uncertain.             
18256-3628   OL   19     BRT1777.                                                                Brt1936a
18257+1339   BPM 769     [PM2000] 1457131 + [PM2000] 1456591.                                    Gvr2010 
18259+1458   CHR  70     This system, first announced by McAlister and recalled in a later       McA1984b
                         McAlister paper after repeated attempts at confirmation, has been       McA1993 
                         restored. While perhaps still spurious, the subsequent confirmation or          
                         suspected duplicity (by another technique) makes the discovery                  
                         measurement somewhat more probable.                                             
18259+0541   J  2130     SLE 174.                                                                        
18260+6534   UC 3580     42 Dra = Fafnir                                                                 
                         CHARA Array Limb-darkened diameter  2.041 +/- 0.043 mas.                CIA2010c
                         R = 21.19 +/- 0.60 \rsun, L = 149.7 +/- 15.3 \lsun,                             
                         Teff = 4486 +/- 122 K.                                                          
                         NPOI Limb-darkened diameter 2.048 +/- 0.009 mas, Sp = K1III,            NOI2018 
                         R = 21.25 +/- 0.42 \rsun, Teff = 4714 +/-101 K,                                 
                         L = 201.1 +/- 18.8 \lsun, M = 1.54 +/- 0.24 \msun,                              
                         Age = 1.93 +/- 0.91 Gyr.                                                        
18260+2606   L    22     Appears to be a 10m error in Lewis' epoch-1900 coordinates.             L__1900 
18260-4541   LDS 638     TSN  95.                                                                        
18261+0047   BU 1203     1980.4794  This measure was incorrectly attributed to ADS 11524 by              
                         McAlister et al. (1983).                                                McA1983 
18262+0847   LDS1012     LFT 1415/1416.                                                          Bgh1958 
                         HJL1099.                                                                HJL1986 
                         B is BD+08@3692.                                                                
                         Hipparcos stochastic double solution.                                           
                         A is SB1, P=293.35d (Halbwachs et al. 2012) and astrometric binary,     HJL2012b
                         P=0.827y (Goldin & Makarov 2007).                                       Gln2007 
                         SHY 306. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
18262-1832   CHR 236     First detected as an occultation binary by Africano.                    Afr1978 
18263+1313   BPM 770     [PM2000] 1460131 + [PM2000] 1460594.                                    Gvr2010 
18264+4649   STT 352     B is BD+46@2489.                                                                
18264+1216   BPM 771     [PM2000] 1460407 + [PM2000] 1459847.                                    Gvr2010 
18265-0226   GRV1262     Both A and B have approximately the same radial velocity.               Grv2019b
18266+1147   BPM 772     [PM2000] 1461257 + [PM2000] 1460960.                                    Gvr2010 
18266+0627   GCB  31     BRT2838.                                                                Brt1947 
18267+2627   BU 1326     A is a spectroscopic binary.                                                    
18267-3024   TOK 421     HIP 90397 is an acceleration binary with a variable RV (GCS), resolved          
                         here at 69mas (estimated period ~4yr). The star is targeted by                  
                         exo-planet programs.                                                    Tok2015c
18268+0123   BAL1501     RST 5449.                                                                       
18268-1814   FEN  30     DON 902.                                                                        
18269+2950   HJ 1325     Rectilinear solution by Cvetkovic et al. (2017).                        Cve2017 
18269+1308   BPM 773     [PM2000] 1462688 + [PM2000] 1462619.                                    Gvr2010 
18271+2754   TDS 921     Appears to be the same star as L    23, based on coordinates and                
                         astrometry by Lewis (1911).                                             L__1911 
18272+1543   BPM 774     [PM2000] 1464147 + [PM2000] 1464406.                                    Gvr2010 
18272+1533   BPM 775     [PM2000] 1464561 + [PM2000] 1464426.                                    Gvr2010 
18272+0404   FAR  20     Primary is white dwarf WD 1824+040.                                     Far2005b
18272+0012   STF2316     59 Ser. A is a triple spectroscopic binary, and B may be an SB also.            
                         A is an irregular variable, d Ser.                                              
                         Aa,Ab: Examined for visual duplicity of its components, which are               
                         long-period SBs.                                                        WRH1952 
                         AB: H 1  12.                                                            MEv2010 
18273+0820   J  2911     TDT 882.                                                                        
18273-2503   LDS 639     LDS 640.                                                                        
                         NLTT 46491/46490                                                        Chm2004 
18274+1141   BPM 776     AB: [PM2000] 1465466 + [PM2000] 1465190.                                Gvr2010 
             BPM 777     BC: [PM2000] 1465190 + [PM2000] 1464574.                                Gvr2010 
18275-1522   J  1631     CD is probably AB of 18275-1524 with quadrant reversed.                         
18277-3207   I  1023     Measures uncertain, too close. Duplicity dubious, but needs speckle.            
18278+2442   STF2320     Eclipsing and spectroscopic multiple (periods 1.42001 & 2.08327 days).  Zas2010 
                         An updated orbit predicts that the two close pairs may be resolvable            
                         by interferometry, with predicted separations ~17mas and a magnitude            
                         difference of ~1.4mag.                                                  Zas2016b
18278-2949   GC 25175    Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from the Geneva           
                         Extrasolar Planet Search Programs home page.                            HaI2001 
             RAG   2     Primary is exoplanet host, P=225.6d                                     Tok2014d
18279-1444   J  1651     Aka TDT 892.                                                                    
18280+0612   CHR  71     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 10.53 +/- 3.67, 5.69, and 3.20 Msun, respectively.            Mlk2012 
18280-2525   WFC 208     lam Sgr = Kaus Borealis.                                                        
18281-2048   RSS  32     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determinedfrom the individual positions           
                         listed by Rousseau et al.                                               Rss1996 
18284-1527   FOX  82     May be component of multiple 18275-1524.                                        
18285-1013   HJ 5497     Herschel coordinates 18 19, NPD 100 19 17 (1830). Colors orange and             
                         green. RA is described as "precarious".                                         
18286+0451   STTA168     B is BD+04@3759.                                                                
18287+0016   SHC   2     Primary is young stellar object [HMH2007] 20. The companion shows IR            
                         excess, and is identified as a young low-mass companion candidate.      ShC2011 
18288+0009   LI    1     Due to an error in cross-referencing, this pair was originally                  
                         entered into the WDS as 18288-2715.                                             
18289+0019   SHC   6     Primary is young stellar object [HMH2007] 43. The companion shows IR            
                         excess, and is identified as a young low-mass companion candidate.      ShC2011 
18289+0020   SHC   3     Primary is young stellar object [HMH2007] 36. The companion is a young          
                         brown dwarf, mass ~80 Mjup.                                             ShC2011 
18289+0029   SHC   4     Primary is young stellar object [HMH2007] 37. The companion shows IR            
                         excess, and is identified as a young low-mass companion candidate.      ShC2011 
18289+0030   SHC   5     Primary is young stellar object [HMH2007] 40. The companion shows IR            
                         excess, and is identified as a young low-mass companion candidate.      ShC2011 
18290-2635   WNO   6     Variable? B is CD-26@13205.                                                     
18290+0017   SHC   7     Primary is young stellar object [HMH2007] 48. The companion is a                
                         low-mass YSO.                                                           ShC2011 
18292+1142   TOK 321     Spectral type of comoving secondary estimated as M1, mass 0.52 Msun.    Mug2014 
                         AB: A is exoplanet host P=1145d                                         Tok2014d
                         AC: white dwarf candidate at 167", likely optical.                      Tok2012c
18293+1624   BPM 778     [PM2000] 1474812 + [PM2000] 1474553.                                    Gvr2010 
18293-3431   B  1364     CPD-34@7858.                                                                    
18295-5053   CPO 586AB   A likely plate flaw.                                                    Grv2021b
18296+0034   SHC   8     Primary is young stellar object [HMH2007] 112. The companion shows IR           
                         excess, and is identified as a young low-mass companion candidate.      ShC2011 
18296+1639   BPM 780     [PM2000] 1476424 + [PM2000] 1476961.                                    Gvr2010 
18296+1553   BPM 779     [PM2000] 1476312 + [PM2000] 1476163.                                    Gvr2010 
18297+5740   LDS2414     LDS2743.                                                                        
18298+1201   BPM 781     [PM2000] 1477006 + [PM2000] 1476757.                                    Gvr2010 
18298-4241   BRT1059     A likely plate flaw.                                                    Grv2021b
18299+2639   HD170737    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin (1980).                                                         Grf1980c
18299+1345   BPM 783     [PM2000] 1477579 + [PM2000] 1477791.                                    Gvr2010 
18299+1222   BPM 782     [PM2000] 1477520 + [PM2000] 1477271.                                    Gvr2010 
18300-1257   HU   69     Spectrum: B9.5II/III.                                                           
18301+1127   BPM 784     [PM2000] 1478740 + [PM2000] 1478561.                                    Gvr2010 
18301+0404   CHR  72     Aa,Ab: 1985.8424: This autocorrelogram was remeasured; the new results          
                         are listed here.                                                                
18305+1408   BPM 785     [PM2000] 1480330 + [PM2000] 1479915.                                    Gvr2010 
18306+2805   ES  476     MLB 649 is identical                                                    Hei1983a
18306+1337   BPM 786     [PM2000] 1481254 + [PM2000] 1480624.                                    Gvr2010 
18307+0431   STTA170     B is BD+04@3775.                                                                
                         Pair appears in an appendix list, not part of discoverer's regular              
                         numbering sequence.                                                             
18308+1803   BPMA 56     [PM2000] 1482352 + [PM2000] 1483143.                                    Gvr2010 
18308-1309   BRT2754     Aka J  1652.                                                                    
18309+3840   STF2338     C is the semiregular variable KP Lyr.                                           
18310+0648   SLE 349     AC: The Soulie (1985) C component is not seen; possibly due to a 2s             
                         error in the published RA?                                              Sle1985 
18312+6526   KUI  86     A is a spectroscopic binary.                                                    
18312+1311   STF2330     B is BD+13@3668.                                                                
18313-1306   EVS   8     Classical Cepheid X Sct.                                                        
18313-4821   HJ 5046     SWR 247. CPM pair                                                       Skf2004 
18313-5532   HJ 5044     B is CPD-55@8709.                                                               
18314+0628   STF2329     Same as STF2331.                                                                
18314-1048   STF2325     H N  54.                                                                MEv2010 
18314-4322   CPO  81     AB = LDS 641.                                                                   
18316+1204   BPM 787     [PM2000] 1486217 + [PM2000] 1486275.                                    Gvr2010 
18317+2310   HU  321     Mt. Wilson spectral type of B is G0.                                            
                         AB: Rectilinear solution by Friedman et al. (2012).                     USN2012a
18318+0641   J  1372     Appears to be the same as KRU   6.                                      Dam2010 
18319+0836   OSO  99     G141-015. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
18319-1908   BU  966     Cluster M 25. A is the Cepheid U Sgr.                                           
                         Identifications on Hyd. ph. -19@, 18:28 are as follows:                         
                         A  51273   G  51291   P  51300                                                  
                         B  51272   H  51271   Q  51299                                                  
                         C  51297   J  51270   R  51274                                                  
                         D  51298   K  51267   S  51263                                                  
                         E  51266   L  51268   T  51292                                                  
                         F  51265   M  51269   U  Close comp. to B.                                      
                         The C of the BC pair is not the same as the C of the CD, CG, and CQ             
                         pairs. Therefore, it has been re-designated Ba,Bb. Aa, aB and aC are            
                         now designated AI, IB and IC. Bb is designated BQ (the identity of CQ           
                         and Bb was first noted by Dave Arnold).                                         
18320+2031   LAW  18     LSPM J1832+2030. Law et al (2008) derive a distance of 20.6 +9.6/-3.9   Law2008 
                         pc and a projected separation of 27.0 +14.6/-4.0 au. Estimated                  
                         spectral types are M4.5 and M5.                                                 
18323-1439   CHR  73     1989.3041: Due to typographical error, measurement was incorrectly      McA1990 
                         attributed to 18444+3937 = CHR 77 in McAlister et al. (1990).           Hrt1996b
18326-1542   RBR   9     2001.7364: PA is measured in zenith mode. If data collected in                  
                         equatorial mode, PA = 218.1. Confirmation of the pair should establish          
                         the correct theta value.                                                Rbr2007 
18326-4936   RST9007     Previously known as RST2060a.                                                   
18327+0504   BAL3014     Epoch-1900 coordinates not precessed in creating WDS designation.               
18329+6343   STF2357     Also known as STF2363.                                                          
18329+3850   STTA171     B is BD+38@3211.                                                                
18329+1418   BPM 788     [PM2000] 1492426 + [PM2000] 1492794.                                    Gvr2010 
18330+3136   STF2340     AB: SEI 565.                                                            Nsn2017b
18330+2420   POU3427     J 1886.                                                                         
18331-1042   HDS2632     The motion of AB is reflex of PM(A), crowded field N*=641, optical!     Tok2014d
18331-1918   J  2215     CPD-19@6927.                                                                    
18332+4010   STT 356     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
18333+3203   SLE 201     Nothing at Soulie (1984) published coordinates. A pair 25s east                 
                         appears to be the most likely candidate.                                Sle1984 
18333+1437   BPM 789     [PM2000] 1494752 + [PM2000] 1494587.                                    Gvr2010 
18333+1309   OSO 100     G141-019. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
18334+5842   ES  188     Primary is HI Dra, a W UMa type eclipsing binary, P = 0.59742d.         Zas2012 
18334+3727   ES 2481     Not found by Heintz at IDS position.                                    Hei1985a
18334-3004   I  1370     Variable companion?                                                     Jsp1964 
18334-3844   DUN 222     kap 2 Cra. B is CD-38@12896, kap 1 Cra.                                         
18335+2102   COU 204     Also known as TOR   4.  The similarity of these systems was first               
                         noted by Dave Arnold.                                                           
18335+0726   SCJ  18     B is BD+07@3740.                                                                
18338+7003   STF2370     HJL 260.                                                                HJL1986 
18338+1744   HU  322     Distance less than 0.1" in 1960.                                                
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 10.48 +/- 51.06, 3.98, 1.17 Msun, respectively.    Mlk2012 
18339+5221   A  1377     Mt. Wilson spectral classes A is G5, C is B8n.                                  
                         AB. This appears to be part of a triple system.  The elements given by          
                         Wilson (1950) and by Baize (1958) are different, possibly due to the    WRH1950b
                         long period of the system. This 1975.533 separation is less than that   Baz1958 
                         derived from either ephemeris but it and the position angle are closer          
                         to Baize's values.                                                      BLM1978 
                         2003.6: Differential astrometry by Lane & Muterspaugh (2004) was        Lne2004 
                         originally published as follows, but converted to BY, rho, and theta            
                         by WIH for inclusion in our catalogs:                                           
                                MJD            dRA (arcsec)           dDEC (arcsec)                      
                            52862.30085   0.222109 +/- 0.000143  -0.119309 +/- 0.00000839                
                            52863.28229   0.222233 +/- 0.000143  -0.119302 +/- 0.0000155                 
                            52864.31096   0.222134 +/- 0.000197  -0.119323 +/- 0.0000189                 
                            52865.29921   0.221981 +/- 0.000155  -0.119361 +/- 0.0000148                 
                         AB: Additional notes may be found in Wilson (1955).                     WRH1955 
18339+5144   ZUC  16     TOK  31.                                                                        
                         GJ 719. Primary is 6d SB2; period of wide pair esimated at 3800y. The           
                         114-day astrometric orbit by HIPPARCOS is not supported by RV. This is          
                         a PMS spotted binary BY Dra.                                            Tok2006 
             BY Dra      Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
                         Combined spectroscopic/astrometric (Palomar Testbed Interferometer)             
                         solution by Boden & Lane (2001), including determination of distance,   Bod2001 
                         masses, luminosities, etc.                                                      
                         Low-mass SB2. Helminiak et al. calculate a combined spectroscopic/              
                         astrometric orbit by combining precise RVs with archival astrometric            
                         data from the Palomar Testbed Interferometer. They derive masses 0.792          
                         +/- 0.026 and 0.697 +/- 0.023 Msun, radii 7.400 +/- 0.016 and 8.414             
                         +/- 0.016 Rsun, parallax 60.43 +/- 0.12 mas.  They conclude it is not           
                         a pre-main sequence system, despite its high orbital eccentricity       Hel2012 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 9.00 +/- 32.45, 1.36, and 0.62 Msun, respectively.            Mlk2012 
18342+0341   ABT9001     Previously known as ABT  13.                                                    
18342-1741   ARA 284     A likely plate flaw.                                                    Grv2021b
18343+1841   MET  85     Also known as V889 Her.                                                         
18344+2615   BUP 183     D component = A component of 18352+2616 BUP 184.                                
18346+1739   BPM 791     [PM2000] 1501242 + [PM2000] 1501100.                                    Gvr2010 
18346+1134   BPM 790     [PM2000] 1501189 + [PM2000] 1501042.                                    Gvr2010 
18346-2734   I  1026     AB +  TOK 422Aa,Ab: HIP 91075 was noted as a double-lined binary by             
                         the GCS (one observation only). The separation of 86mas implies a               
                         period of ~10yr, while the double-lined observation matches the                 
                         moderate magnitude difference (estimated masses 1.04 and 0.77 Msun.             
                         The star is an X-ray source, so a future combined orbit could                   
                         determine masses for testing evolutionary models of young stars. The            
                         sky around the object is quite crowded; the 9" companion I 1026 is              
                         optical (it moves too fast).                                            Tok2015c
             I  1027     CD: CPD-27@6461.                                                                
18346-3753   JSP 780     CPD-37@8199.                                                                    
18347-6557   I   634     Spectrum: G3/6III+(A).                                                          
18349-0043   RST5119     Primary is eclipsing binary of Algol-type, period 1.953876 day.         Zas2013 
18349-1442   STF2337     B is BD-14@5117. B spectrum B9/A0II/III.                                        
18349-4801   HJ 5047     B is CD-48@12597.                                                               
18351+0003   RST5120     V413 Ser, Algol-type eclipsing binary, P = 2.25977 d.                   Zas2011 
18352+6342   STF2365     Primary is SB2, P=4.738y                                                Tok2014d
18352+2616   BUP 184     A component = D component of 18344+2615 BUP 183.                                
18352+1812   CHR  74     A well-known speckle binary whose first interferometric observations            
                         date from the CHARA speckle program in the mid-1980's, this object              
                         went unobserved from 1996 until the present work. The new data suggest          
                         that nearly half an orbit has been completed since the first speckle            
                         observation. The primary is probably close to an A0V star, and with a           
                         magnitude difference of perhaps 2-2.5, we estimate that the secondary           
                         is an F2V star. This would suggest a mass sum in the range 4-5 Msun,            
                         which is lower than what is implied by the value of P and a we derive,          
                         together with the Hipparcos parallax of 5.04 +/- 0.39 mas. We expect            
                         that the next decade will provide an opportunity to improve upon the            
                         orbit presented here since the separation will be above 0.1 arcsec and          
                         the position angle is expected to cover about 30deg. We encourage               
                         other observers to put this object back on their observing lists for            
                         the next few years.                                                     Hor2015b
18353+2842   OSO 101     G206-034. None of the components share a common proper motion, based            
                         on color and/or comparison with POSS2 red plates.                       Oso2004 
18354+0649   J   100     Van Biesbroeck calls this Toulouse +7@, 18h 28m                         VBs1954 
                         No. 300. Jonckheere gives BD+06@3866.                                   J__1910d
18354-2118   ARA1544     Aka J  1747.                                                                    
18355+4546   LDS6329     NLTT 46716 + 46720.                                                             
                         Also known as GJ 720 A, this star has a wide companion with a                   
                         demonstrated common proper motion at about 112" according to Lepine &   Lep2007 
                         Bongiorno (2007).                                                       Jnn2012 
18355+2336   STT 359     Spectrum composite; G9III+G7III.                                                
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.80 +/- 1.54, 4.11, and 1.85 Msun, respectively.             Mlk2012 
18355+1005   BRT1945     J 2134; also J 2137. Jonckheere noted BRT1945 = J 2134 and suspected    J__1942d
                         J 2137 at 18356+1007 was probably the same star as well. Identity               
                         concluded after search of region, despite fair amount of discrepancy            
                         in some measures.                                                               
18356+0456   BU  643     A is the Alpha CVn-type variable FR Ser.                                        
18358+2522   HDS2637     Fekel et al. (2013) derive a spectroscopic orbit for the primary, with          
                         P=14.685d and e=0.2495. Estimated masses are 2.5 and 2.35 Msun.         Fek2013a
18359+1659   STT 358     Alternative spectrum: G2V+G2V                                                   
                         Identification of the ascending node is uncertain due to weak data.     Hei1954 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
             RED  25     AB,E:  M3.5, 35" from G0/F8 binary HD 171746 = HIP 91159 = 2MASS                
                         J18355323+1658316. Proper motion for the brighter star +049-071.                
                         From measurements of DSS POSS and 2MASS plates Reid et al. derive a             
                         proper motion of +080-070 for the M dwarf. Trigonometric parallax               
                         for the G dwarf gives a distance ~34pc, significantly larger than               
                         the spectroscopic distance of 21pc for M star. It is uncertain                  
                         whether the stars are associated.                                       Red2007a
                         AE: 2MASS J18355276+1659057 is possibly a wide companion to HIP 91159   Red2007a
                         at 35" separation, as noted in Reid et al. (2007).                      Jnn2012 
18360+2528   BRT3332     Same as BRT 132.                                                        Kpp2022b
18360+1144   STT 357     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 8.78 +/- 7.73, 4.26, and 1.66 Msun, respectively.             Mlk2012 
18360+0452   J  2138     BAL2930.                                                                        
18361+6405   MLB 214     Position corrected by Heintz.                                           Hei1983a
18362+6529   GC 25491    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
18362-1053   EGN  23     System is only 21deg from galactic center, so 12 companion candidates           
                         were detected. The B, C, H, I, J, K, L, and M components are unbound;           
                         D is likely a background star as well. Single epoch, so the nature of           
                         E, F, and G are unknown.                                                Egn2007 
18362-1407   SNA  92     The object was clearly resolved with PIONIER as a 1.5mas pair. The      Cti1977 
                         possible RV variability reported by Conti et al. (1977) was not         Cii2012 
                         confirmed by Chini et al. (2012).                                       Sna2014 
18363+2143   COU 206     Docobo et al. (2010) derive a dynamic parallax of 3.15 +/- 0.30 mas     Doc2010h
                         and a total mass of 3.72 +/- 2.07 Msun. The mass is excessive for the           
                         spectral types.                                                                 
18364-4952   CPO 592     CPD-49@10659.                                                                   
18366+3328   STF2349     A is possibly a spectroscopic binary. Variable.                                 
18367+3841   H 4  59     H IV 59. Also known as STF2354.                                                 
18367+0640   CHR  76     A is a spectroscopic binary, now resolved by speckle.                           
             J    99     AB: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
18367-0811   KRV  21     Classical Cepheid EV Sct.                                                       
18368+1151   L    39     The Sternberg measure evidently does not belong to this pair.           Srb1969 
18369+3846   H 5  39     AB: H V 39. alp Lyr = 3 Lyr = Vega                                              
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
             STFB  9     AE: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             MET  11     Metchev & Hillenbrand say the F, G, H, I, J, and K components are all   Met2003 
                         probably optical companions of Vega. Physicality of the Ia,Ib and               
                         Ka,Kb pairs is unknown.                                                         
             MBA   2     Macintosh et al. (2003) made a K-band search for extrasolar planets in  MBA2003 
                         the dust surrounding Vega, using Keck, NIRC2, and AO. The relative              
                         motions for these 7 objects between 2002 Feb and 2002 Aug were all              
                         well below expected motions for true companions, leading to the                 
                         conclusion that all these faint companions are background stars.                
                         Identities of the objects discovered by Metchev et al. and Macintosh            
                         et al. are as follows:                                                          
                             MET  11AF     = Met2003 object 1 = MBA2003 object 1                         
                             MET  11AG     = Met2003 object 2 = MBA2003 object 2                         
                             MET  11AH     = Met2003 object 3 = MBA2003 object 3                         
                             MET  11A,Ia   = Met2003 object 4                                            
                             MET  11A,Ib   = Met2003 object 5                                            
                             MET  11AJ     = Met2003 object 6 = MBA2003 object 7                         
                             MET  11A,Ka   = Met2003 object 7                                            
                             MET  11A,Kb   = Met2003 object 8                                            
                             MBA   2AL     =                    MBA2003 object 4                         
                             MBA   2AM     =                    MBA2003 object 5                         
                             MBA   2AN     =                    MBA2003 object 6                         
             H 5  39     AB: Rectilinear solution by Friedman et al. (2012).                     USN2012a
             STFB  9     AE: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
18369+1506   BPM 793     [PM2000] 1512466 + [PM2000] 1511835.                                    Gvr2010 
18369+1129   BPM 792     [PM2000] 1512306 + [PM2000] 1512288.                                    Gvr2010 
18370+3452   STF2352     AB: SEI 566.                                                            Nsn2017b
18372-0236   BAL 248     BRT1946.                                                                Brt1936b
18374-4704   HJ 5049     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2014).                         USN2014b
18378+1752   BPM 794     [PM2000] 1516606 + [PM2000] 1517111.                                    Gvr2010 
18379-0648   LDS5239     HIP 91360. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
18379-1111   BRT2755     J 2139.                                                                         
18380+1107   BPM 795     [PM2000] 1517796 + [PM2000] 1518152.                                    Gvr2010 
18380-0648   TOK  32     Allen et al. (2000) list a CPM companion at 37.1", confirmed as CPM     AlC2000 
                         and ptm by 2MASS. Primary is 21d SB1.                                   Tok2006 
18381+1245   BPM 796     [PM2000] 1517997 + [PM2000] 1517765.                                    Gvr2010 
18381+1229   BPM 797     [PM2000] 1518189 + [PM2000] 1518302.                                    Gvr2010 
18381-0822   KRV  51     Classical Cepheid Y Sct.                                                        
18383-0236   BRT3333     Originally published as BRT1947.                                        Brt1936b
18384+6708   STF2384     Unobserved periastron can be covered by speckle in near future.         Sod1999 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.03 +/- 0.58, 2.10, and 0.95 Msun, respectively.  Mlk2012 
18384+0850   HU  198     Variable X Oph; it is the northern component that varies.               Baz1954a
                         The M5e star is the Mira-type variable X Oph, P = 334 d, and at                 
                         minimum often fainter than the K1 star. Motion so far is rectilinear.           
                         Spectrum composite; K1III+M6IIIe.                                               
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         A measure on 1980.4794, incorrectly attributed to ADS 11524 by                  
                         McAlister et al. (1983), actually belongs to ADS 11339.                 McA1983 
18384-0312   A    88     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.42 +/- 0.32, 2.50, and 1.07 Msun, respectively.  Mlk2012 
                         A 4432-d spectroscopic orbit has been determined for this pair.         Grf2013e
18385+1107   BPM 798     [PM2000] 1520282 + [PM2000] 1520283.                                    Gvr2010 
18386+3046   STF2359     Kamper erroneously assigned the wide pairs to 18386+3043 = STF2358.     Kpr1992 
                         The C and D components are A and B of STF2358.                                  
18386+3043   STF2358     The A and B components are also the C and D components of STF2359.              
18386+2422   POU3450     Secondary (from AC catalog) not seen in Aladin - probably plate flaw            
                         or typographic error.                                                           
18386+1632   HO   87     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 4.52 +/- 2.14, 2.99, and 0.95 Msun, respectively.  Mlk2012 
18387+2858   L    53     Aka SLE 100.                                                                    
18387+2847   L    25     L 25a.                                                                          
18387+2439   HJ 1332     B is BD+24@3479.                                                                
18387-4127   HJ 5052     SWR 249. CPM pair                                                       Skf2004 
18389+5221   STF2368     Mt. Wilson spectral classes A1n and G0.                                         
                         AB: H 2  31.                                                            MEv2010 
18389+1715   BPM 799     [PM2000] 1522179 + [PM2000] 1522332.                                    Gvr2010 
18390+0624   SLE 498     Typographical error (1 arcmin error in coordinates of B component) led          
                         to error in rho and theta by Soulie (1986).                             Sle1986a
18394+0111   BAL1503     J 2519.                                                                         
18395+3009   LDS4794     NLTT 46821/46824                                                        Chm2004 
18395+1225   BPM 800     [PM2000] 1524582 + [PM2000] 1524944.                                    Gvr2010 
18396-3207   PRO 208     SWR 250. CPM pair                                                       Skf2004 
18401+4100   SLE  93     There appears to be a ~90" error in the declination of the primary by           
                         Soulie (1983).                                                          Sle1983 
18404+0942   S   704     B is BD+09@3814.                                                                
18405+4906   COU2394     Aka TDT 988.                                                            Dam2018l
18405+1936   OSO 102     G184-017. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates.                                                  Oso2004 
18406+0307   STF2361     B is BD+02@3649.                                                                
18408+1214   HJ 1334     Probably same as J 2142. Jonckheere gives BD as +12@3414; perhaps a     J__1942d
                         misprint for BD+12@3614.                                                        
18409+6633   LDS2419     LDS5242. UC 3635.                                                               
18409+3132   HJ 1337     G206-038. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 46857/46858                                                        Chm2004 
18411+2447   LDS6330     Aka POU3485.                                                                    
                         GJ 1230. Estimated age 30-300 Myr; masses 0.40 +/- 0.18 and 0.12 +/-            
                         0.03 Msun; a ~40.0 au.                                                  Jnn2014 
18411+1035   BPMA 57     [PM2000] 1532102 + [PM2000] 1533512.                                    Gvr2010 
18412+1747   BPM 801     [PM2000] 1532364 + [PM2000] 1531960.                                    Gvr2010 
18412+1128   BPM 802     [PM2000] 1532425 + [PM2000] 1532577.                                    Gvr2010 
18413+3018   STF2367     Bidelman classifies AB as composite gK+A:.                                      
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         Only elements P and T have been amended by Starikova (1977) from the    Sta1977a
                         orbit of Baize (1950).                                                  Baz1950b
18413-0727   J  1748     Aka J  2918.                                                                    
18414+7001   GNO   2     Distance is estimated at about 40.2 +/- 4.9 pc, giving a projected              
                         component separation of 2.8 +/- 0.7 au. Estimated orbital period is             
                         ~11 yr, for an assumed age of 1 Gyr. Masses are ~60Mjup for each of             
                         these T5 components.                                                    Gno2011 
18414+1133   BPM 803     [PM2000] 1533639 + [PM2000] 1533477.                                    Gvr2010 
18417+1029   BPM 804     [PM2000] 1534975 + [PM2000] 1535121.                                    Gvr2010 
18417-5514   SWR 251     Southern component not red?                                             Skf2004 
18418+3314   KU  119     SEI 569.                                                                Nsn2017b
18418+1033   BPM 805     [PM2000] 1535637 + [PM2000] 1535209.                                    Gvr2010 
18421+3445   B  2546     A is called a spectroscopic binary, but the variation is likely caused          
                         by motion in the close visual pair.                                             
                         B is BD+34@3286.                                                                
             STF2372     AB: H 4  94.                                                            MEv2010 
             STF2372     AB: SEI 571.                                                            Nsn2017b
18422-1022   J  2522     J 1655 is probably identical                                            Hei1985a
18423-0903   RST4594     A: del Sct = 2 Sct, prototype of the Delta Scuti variables.                     
             H 5  36     AC: H V 36.                                                                     
18424+7550   LDS1890     NLTT 46982/46986                                                        Chm2004 
18424-0520   KRV  20     Classical Cepheid CM Sct.                                                       
18425+0334   J   464     AB pair not confirmed by Jonckheere (1962).                             J__1962a
18426+5532   ISO   7     46 Dra. A spectroscopic binary, P 9.87d. Abundance peculiarities.               
             H 6  37     H VI 37.                                                                        
18426-0704   GC 25586    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin (1982).                                                         Grf1982b
18426-4740   HJ 5054     B is CD-47@12469.                                                               
18427+1354   JNN 280     There is a point source at 3.7" separation from GJ 4071. The system             
                         has only been observed in one epoch, but based on the colors of the             
                         candidate (dz' = 5.8 +/- 0.1 mag and di' = 5.7 +/- 0.1 mag), it counts          
                         as a probable background contaminant in our analysis.                   Jnn2014 
18428+5938   STF2398     AB: Mt. Wilson spectral classes M4 and M4. Proper motion -1298 +1879.           
                         B is variable. Also known as LDS1466.                                           
                         CHARA Array Limb-darkened diameter of A,B:                              CIA2012f
                         R =  0.3561 +/- 0.0039, 0.3232 +/- 0.0061 \rsun,                                
                         L =  0.01531 +/- 0.00018, 0.00871 +/- 0.00012 \lsun,                            
                         Teff = 3407 +/- 15, 3104 +/- 28 K, M = 0.318, 0.235 \msun.                      
                         Optical pair.                                                           Doo1901 
                         Statistically the same parallax within the errors would indicate the            
                         components are physical.                                                        
                         Parabolic orbit by Wieth-Knudsen (1953).                                Wie1953b
                         sigma = areal constant in the true orbit = 2.207 arcsec^2/yr                    
                         q = periastron distance in the true orbit = 16".603                             
                         A short-period motion in one of the components has been suspected               
                         repeatedly, but photographic measures do not show it. (Heintz 1978)     Hei1978d
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AC: Same as ADS 11632 AB.                                                       
                         BC: Rectilinear solution by Friedman et al. (2012).                     USN2012a
18429+4456   STF2380     B is BD+44@2974.                                                                
18430-7126   HJ 5048     zet Pav                                                                         
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
18431+1318   BPM 806     [PM2000] 1542850 + [PM2000] 1543469.                                    Gvr2010 
18431+0742   LDS1013     B is BD+07@3814.                                                                
18432+1017   BPM 807     [PM2000] 1543666 + [PM2000] 1544209.                                    Gvr2010 
18433+3918   BLL  35     A spectroscopic binary. B is BD+39@3504.                                        
18433+2506   POU3503     COU 509.                                                                        
18434-5252   HJ 5055     SWR 252. CPM pair                                                       Skf2004 
                         Primary is QZ Tel, a W UMa type eclipsing binary, P = 1.03099d.         Zas2012 
18434-5546   HJ 5053     Also known as R   310.                                                          
             B   398     AB: Tokovinin & Lepine (2012) miss AC, but list 2 optical companions    Tok2012c
                         at 697" and 1340".                                                      Tok2014d
                         AB: Gomez et al. (2016) derive dynamical parallax and component masses          
                         for both short- and long-period solutions:                                      
                         short: 16.93 +/- 0.41 mas, 1.126 +/- 0.013 Msun, 0.896 +/- 0.010 Msun.          
                         long:  14.33 +/- 0.47 mas, 1.219 +/- 0.019 Msun, 0.970 +/- 0.015 Msun.  Doc2016i
18435+1247   BPM 808     [PM2000] 1545429 + [PM2000] 1546011.                                    Gvr2010 
18435-0817   J   104     eps Sct                                                                         
18436+4237   ES  478     JKA   1. KIC 7090654/7090649.                                                   
18436+1439   BPM 809     [PM2000] 1545884 + [PM2000] 1545616.                                    Gvr2010 
18436-5138   RST5451     A is variable. Spectral type A2/3III/IV.                                        
18437+3141   A   253     Only elements P, T, and a have been amended by Starikova (1978) from    Sta1978c
                         the orbit of Muller (1956).                                             Mlr1956b
18438+1200   BPM 810     [PM2000] 1546793 + [PM2000] 1546974.                                    Gvr2010 
18438-3819   COO 227     11 Cra. Variable?                                                               
18439+1601   OSO 103     G184-020. None is a common proper motion pair                           Oso2004 
18439-0649   YSC 133     A first orbit for this system was reported recently in Tokovinin et     Tok2015c
                         al. (2015), but those authors assumed a quadrant flip of one data               
                         point taken by Horch et al. (2008). That was not an unreasonable        Hor2008 
                         assumption based on the relatively small magnitude difference, but the          
                         points presented here give support to an "alternate" orbit where no             
                         quadrant flips are needed and the period is about half of that derived          
                         in the earlier calculation. Given the revised Hipparcos parallax of             
                         13.55 +/- 0.43 mas, the new orbit gives a mass sum of 3.5 +/- 1.0Msun,          
                         which is somewhat high for a system of composite spectral type F7, but          
                         with substantial uncertainty at this stage. In contrast, the Tokovinin          
                         orbit gives a mass sum of about 1 Msun, which would seem to be too low          
                         by roughly the same amount.                                             Hor2015b
18440+1820   BPM 811     [PM2000] 1548500 + [PM2000] 1548937.                                    Gvr2010 
18440+0321   A  2388     Rectilinear solution by Rica & Zirm (2012).                             FMR2012i
18442+4321   DEA 409     JKA   2. KIC 7659402/7659417.                                                   
18442+1030   BPM 812     AB: [PM2000] 1549644 + [PM2000] 1550217.                                Gvr2010 
             BPM 813     BC: [PM2000] 1550217 + [PM2000] 1550653.                                Gvr2010 
18443+3940   STF2382     A: eps 1 Lyr = 4 Lyr                                                            
                         AB: A premature orbit has been computed.                                        
             STFA 37     AB,CD: See ADS for notes of components.                                 A__1932a
                         AB and CD form the physical quadruple eps Lyrae, separation                     
                         208". The observed small RV variations in each pair are probably                
                         merely scatter due to the very poor lines.                                      
                         BD: SHY 307. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
             STF2383     C: eps 2 Lyr = 5 Lyr                                                            
             CHR  77     Ca: See note for 18323-1439 = CHR 73.                                   Hrt1996b
                         Ca is an Alpha CVn-type variable.                                               
                         The measures show a large scatter and there are many observations of            
                         the wider pair without a measure of this close companion. The nature            
                         of the motion or even the reality of this pair is in question.          Tok2010b
             STF2383     The longitude of periastron in the orbit of CD has been corrected.      Gzl1956a
             SHJ 277     EF, EG, etc.: A preliminary sketch of the motions of the SHJ group              
                         show the G component may be flying away in position angle ~190          Dal2002a
             STF2382     AB: H 2   5.  STF2383CD: H 2   6.                                       MEv2010 
18444+2003   GRV 238     B component is +19 3770.                                                        
18444-4657   HU 1528     V359 Tel, Algol-type eclipsing binary, P = 19.2449 d.                   Zas2011 
18445+3400   STTA172     B is BD+33@3191.                                                                
18445+1913   J   466     TDT1030.                                                                        
18446+1138   BPM 814     [PM2000] 1552151 + [PM2000] 1551797.                                    Gvr2010 
18448+3736   BU  968     A: zet 1 Lyr = 6 Lyr. A is a spectroscopic binary and variable.                 
             STFA 38     D: zet 2 Lyr = 7 Lyr                                                            
                         AD: STTA173. According to Henroteau, the wide pair zet 1 + zet 2 Lyr    HFC1928 
                         was first by Bianchini in 1737.                                         Bia1737 
                         AD: SHY 308. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AD: H 5   2.                                                            MEv2010 
18448+1036   BPM 815     [PM2000] 1553946 + [PM2000] 1553909.                                    Gvr2010 
18448-3449   BRT1786     CPD-34@8050.                                                                    
18448-5354   HRG 139     SWR 253.                                                                        
18449+1606   HEI 173     A third star at 323 deg, 62"                                            Hei1983a
18450+1255   BPM 816     [PM2000] 1555247 + [PM2000] 1555413.                                    Gvr2010 
18451+4746   ES 1161     KIC 10514430 = KOI 263.                                                         
                         Also known as KOI1614.                                                          
18451+1415   BPM 817     [PM2000] 1556143 + [PM2000] 1556451.                                    Gvr2010 
18452+4227   KOI  10     AB: Adams et al. (2012) theta values corrected to 360-theta             Adm2012 
                         (reported by Dressing et al. (2014).                                    Dre2014 
18452+3819   STF2393     Also known as STF2387.                                                          
                         AB: H 3  81.                                                            MEv2010 
18452+3532   STF2386     B is BD+35@3350.                                                                
18453+1434   BPM 818     [PM2000] 1557759 + [PM2000] 1558675.                                    Gvr2010 
18453-1509   BRT 594     A likely plate flaw.                                                    Grv2021b
18453-2039   EVS  37     Primary is the Cepheid V350 Sgr.                                        Evs2016a
18454-6452   SKF 105     Member of the bet Pic moving group.                                     Zuc2001b
18454-5025   R   313     B is CD-50@12120.                                                               
18455+1024   BPMA 58     [PM2000] 1559344 + [PM2000] 1559289.                                    Gvr2010 
18455+0530   STF2375     This remarkable quadruple system is comprised of two close (0".14)              
                         pairs of similar position angle, discovered by Finsen with his          Fin1953c
                         eyepiece interferometer.  Our 1982 observations (McAlister et al.       McA1987b
                         1987) were made at lower magnification and included all four stars in           
                         the field. The resulting overlapping autocorrelation peaks precluded            
                         measurement of the Aab or Bab pairs directly, but did permit measures           
                         of the AB; Aa,Bb; and Ab,Ba configurations.  In later observations              
                         made at higher magnification we observed the A and B components                 
                         separately, enabling measurement of Aa,Ab and Ba,Bb but not AB.                 
                         Listed in the first speckle catalogue as STF 2375 AB,CD.                McA1984b
             FIN 332     Aa,Ab: Listed in the first speckle catalogue as Fin 332 AB.             McA1984b
             FIN 332     Ba,Bb: Listed in the first speckle catalogue as Fin 332 CD.             McA1984b
18456+1604   BPM 820     [PM2000] 1560170 + [PM2000] 1560342.                                    Gvr2010 
18456+1041   BPM 819     [PM2000] 1559506 + [PM2000] 1559263.                                    Gvr2010 
18457+2033   HJ 2839     110 Her.                                                                        
                         CHARA Array Limb-darkened diameter  1.000 +/- 0.006 mas,                CIA2012e
                         R =  2.064 +/- 0.017 \rsun, L =  6.296 +/-0.136 \lsun,                          
                         Teff = 6376 +/-  39 K, M = 1.422 +/- 0.009 \msun,                               
                         Age =  2.6 +/- 0.1 Gyr.                                                         
                         NPOI Limb-darkened diameter    0.905 +/- 0.022 mas,                             
                         R =    1.88 (+/- 0.05   )  \rsun,  Teff = 6568 +/-  80 K,                       
                         L =    6.0 +/-   0.0 \lsun.                                             NOI2023 
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
18457-1624   J  1656     J 1749.                                                                         
18458+4647   KOI1537     Primary is Kepler exoplanet host star.                                  Adm2013 
18458+3431   STF2390     H 2  67.                                                                MEv2010 
18460+1124   BPM 821     [PM2000] 1562588 + [PM2000] 1562091.                                    Gvr2010 
18460+2422   SLE 508     One degree error In Soulie (1986a) declination.                         Sle1986a
18461+2734   SLE 366     Apparently a typographical error in Soulie's RA for the secondary led   Sle1985 
                         to his discrepant measure.                                                      
18462+1432   BPM 822     [PM2000] 1564514 + [PM2000] 1563801.                                    Gvr2010 
18462+1034   BPM 823     [PM2000] 1564654 + [PM2000] 1564191.                                    Gvr2010 
18462+1001   J  1215     Aka HEI 804.                                                                    
18463+1030   BPM 824     [PM2000] 1565096 + [PM2000] 1565598.                                    Gvr2010 
18463-2224   SEE 360     28 Sgr.                                                                         
18463-7249   HIP  92103  The NICI images are of poor quality resulting in a shallow detection            
                         limit (at 0".2, dK < 3 and dH < 2).                                     Tok2012a
18464+3116   HJ 1345     Recognized to be the same as SLE 121 by Francisco Romero                FMR2006c
18464+1240   BPM 825     [PM2000] 1565889 + [PM2000] 1565812.                                    Gvr2010 
18464-3559   BRT1787     CPD-36@8476.                                                                    
18465-0058   MCA  53     Aa,Ab: 5 Aql. A suspected spectroscopic binary, now resolved by                 
                         speckle interferometry.                                                         
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 12.98 +/- 5.76, 5.05, and 2.09 Msun, respectively. Mlk2012 
             STF2379     AB: H 3  33.                                                            MEv2010 
18466+3821   HU 1191     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.47 +/- 0.12, 1.69, and 0.88 Msun, respectively.             Mlk2012 
18467-0916   JNN 118     The primary star has two candidate companions in the field of view.             
                         The fainter candidate C is most likely a background star, since its             
                         color is entirely inconsistent with a late M-type star. The brighter            
                         candidate B is more uncertain. It's colors are fully consistent with            
                         the brightness contrast to the primary for a physical companion,                
                         implying a spectral type of M5. It is also visible in 2MASS (Skrutskie          
                         et al. 2006 AJ 131, 1163), which enables to perform a rough CPM test.           
                         The test indicates that B is inconsistent with a static background              
                         object, again implying physical companionship. However, the motion is           
                         also poorly consistent with orbitalmotion, with a sky-projected speed           
                         of order 2 au per year - highly unlikely for such a wide and low-mass           
                         binary. This implies either under-estimated uncertainties in the data,          
                         or an unusual astronomical coincidence. With the small separation and           
                         relatively high brightness difference of the candidate companion, it            
                         is just at the detection limit of 2MASS, and is only reliably                   
                         detectable in K-band. Perhaps there is a systematic noise component             
                         beyond the quoted astrometric 2MASS error in this circumstance. If all          
                         the data are taken at face value, another possible interpretation is            
                         an unfortunate chance alignment with a local M-dwarf, which has a               
                         signficant proper motion of its own. In any case, due to all these              
                         uncertainties, we tentatively treat the pair as a candidate binary              
                         here, but emphasize that more data is needed to test physical                   
                         companionship.                                                          Jnn2012 
18467-2930   TOK 366     Triple system. The wider C component is confirmed as CPM by 2MASS.      Tok2013b
                         AB: A is astrometric binary, P=20.828y (Makarov & Kaplan 2005)          Mkr2005 
18468+4224   KOI 2914    This system hosts a 2.0 Rearth planet with a 21.1 day period (Burke et  KOI2014a
                         al. 2014).                                                              Dre2014 
18468-1428   RST4596     Primary is possible SB, no orbit.                                       Tok2014d
18468-3636   NHR  10     AB: KOH 108.                                                                    
18469+1105   BPM 826     [PM2000] 1569882 + [PM2000] 1569114.                                    Gvr2010 
18469-1222   BRT2757     Possibly BD-12@5164. J 2147.                                                    
18470+1811   ENG  64     AB: 111 Her. BC: Hipparcos acceleration double solution.                        
             SMA  80     Also known as ENG  64CD.                                                        
             ABH 103     All ABH pairs were incorrectly identified with the C component rather           
                         than B. In addition, three early measures of BI were actually of the            
                         new pair, now labelled ENG  64DJ.                                               
18471+5523   SIG   5     Konopacky et al. (2010) derive a distance of 29.8 +/- 7.1 pc and a              
                         system mass of 0.18 +0.35/-0.13 Msun.                                   Kon2010 
18471+1328   BPM 827     [PM2000] 1572182 + [PM2000] 1572776.                                    Gvr2010 
18471-2331   LDS4798     NLTT 46980/46981                                                        Chm2004 
18472+1227   BPM 828     [PM2000] 1572338 + [PM2000] 1573212.                                    Gvr2010 
18472-0445   NOI   5     HR 7063 = bet Sct.                                                              
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Young (1927).                                                           YRK1927 
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Young (1926).                                                           YRK1926 
                         NPOI Limb-darkened diameter    2.223 +/- 0.011 mas,                             
                         R =   49.26 (+3.24-3.72 )  \rsun,  Teff = 4951 +/-  25 K,                       
                         L = 1315.  +/- 186.  \lsun.                                             NOI2023 
18473+0323   LDS5866     LDS6331.                                                                        
18474+1122   BPMA 59     [PM2000] 1574643 + [PM2000] 1574494.                                    Gvr2010 
18474-2108   B  1889     Spectrum: B9.5II/III.                                                           
18475+4926   BU  971     The primary is a spectroscopic binary, and is also the semiregular              
                         variable S Sct.                                                                 
                         Algol-type eclipsing binary, P = 4.243 d.                               Zas2011 
18476+4450   KOI  68     AB, AC, AD: Adams et al. (2012) theta values corrected to 360-theta     Adm2012 
                         (reported by Dressing et al. (2014).                                    Dre2014 
18476+2903   DAM 679     Typographic error in initial WDS designation (18376+2903)                       
18476+2335   HJ 2841     POU3552.                                                                        
18476+1234   BPM 829     [PM2000] 1575822 + [PM2000] 1575179.                                    Gvr2010 
18476+1121   BPM 830     [PM2000] 1576469 + [PM2000] 1576881.                                    Gvr2010 
18476-0156   LUQ   1     Primary is the Wolf-Rayet star WR 121a, in the W43 star-forming                 
                         complex; this confirms  earlier spectroscopic suspicion of a companion          
                         star, as well as the colliding wind binary scenerio invoked to                  
                         interpret X-ray emission.                                               Luq2011 
18476-0157   LUQ   2     Primary is an O star in the W43 star-forming complex; it appears to             
                         concide with the peak in non-thermal emission by the cluster.           Luq2011 
18477+3600   ALI 142     A is the RR Lyrae-type variable EZ Lyr.                                         
18477+1539   BPM 831     [PM2000] 1577255 + [PM2000] 1576842.                                    Gvr2010 
18478+1725   BPM 832     [PM2000] 1577924 + [PM2000] 1576931.                                    Gvr2010 
18479+1403   BPM 833     [PM2000] 1579102 + [PM2000] 1579251.                                    Gvr2010 
18479+1110   STTA174     B is BD+10@3660.                                                                
18481+1656   BPM 834     [PM2000] 1580332 + [PM2000] 1581229.                                    Gvr2010 
18481+1557   BPM 835     [PM2000] 1580795 + [PM2000] 1579735.                                    Gvr2010 
18481+1231   BPMA 60     [PM2000] 1580760 + [PM2000] 1582659.                                    Gvr2010 
18482+1039   STT 362     Also known as STT 546.                                                          
18483-1935   B  2461     J 1635, J 1750.                                                                 
18483-2033   DON 924     CPD-20@7194.                                                                    
18483-6856   JAO   8     The fainter source in the STIS UV data is the red dwarf primary; the            
                         brighter blue companion is a faint white dwarf with a mass >0.5Msun.    Jao2014b
                         Primary is SCR 1848-6855, a high-proper motion M5.0V dwarf at 24.6pc.           
                         Astrometric observations spanning 8.5 years reveal large photocentric           
                         perturbation due to an initially unseen companion. The pair was                 
                         subsequently resolved by HST/STIS.                                      Jao2014b
18484+1542   BPMA 61     [PM2000] 1582816 + [PM2000] 1585071.                                    Gvr2010 
18485+4240   DEA 188     JKA   5. KIC 7092930/7092937.                                                   
18485+1045   STF2396     AB, AC, and AD: Optical pairs, based on study of relative motion of             
                         the components using the method of apparent motion parameters.          Kiy2008 
18486+1344   BPM 836     [PM2000] 1584779 + [PM2000] 1584834.                                    Gvr2010 
18487+2053   RAS  27     Main component is poorly-studied silicon star, type A1; companion               
                         late-G/early-K.                                                         Ras2014 
18487+1803   BPM 840     [PM2000] 1585768 + [PM2000] 1586803.                                    Gvr2010 
18487+1426   BPM 838     AB: [PM2000] 1585727 + [PM2000] 1586604.                                Gvr2010 
             BPM 839     BC: [PM2000] 1586604 + [PM2000] 1585866.                                Gvr2010 
18487+1137   BPM 837     [PM2000] 1585336 + [PM2000] 1586244.                                    Gvr2010 
18487-0600   STF2391     AB: H 6  50.                                                            MEv2010 
18487-1702   J  2235     Spectrum: G6/8III/IV.                                                           
18487-4647   CPO  84     Aka TSN 119.                                                                    
18488+3319   HJ 1349     Rectilinear solution by Friedman et al. (2012).                         USN2012a
18488-0120   BAL 585     J 1373.                                                                         
18489+1615   STF2400     AC: Mt. Wilson spectra are F5s for A and A4n for C.                             
                         AD: D not seen in 1901 and 1919.                                                
                         BC: Additional notes may be found in Burnham (1894).                    Bu_1894 
                         AB, AC: Rectilinear solutions by Cvetkovic (2015).                      Cve2015b
                         A,BC: Rectilinear solution by Cvetkovic et al. (2016).                  Cve2016 
18489+1219   BPM 841     [PM2000] 1587296 + [PM2000] 1587585.                                    Gvr2010 
18490-0828   STF2388     C component is of spectral type K0:III                                  AbH2000 
18491+1524   BPM 842     [PM2000] 1589068 + [PM2000] 1588083.                                    Gvr2010 
18492+2503   CHR  79     Hipparcos Suspected non-single.                                                 
                         A spectroscopic binary, P = 13.08d. Hence triple.                               
                         This system, first announced by McAlister and recalled in a later       McA1984b
                         McAlister paper after repeated attempts at confirmation, has been       McA1993 
                         restored. While perhaps still spurious, the subsequent confirmation or          
                         suspected duplicity (by another technique) makes the discovery                  
                         measurement somewhat more probable.                                             
18493+2606   BRT3334     Originally published as BRT 184.                                        Brt1928 
18493+1416   BPM 845     [PM2000] 1590859 + [PM2000] 1591945.                                    Gvr2010 
18493+1214   BPM 844     [PM2000] 1590851 + [PM2000] 1590883.                                    Gvr2010 
18493+1206   BPM 846     [PM2000] 1591164 + [PM2000] 1591513.                                    Gvr2010 
18493+1144   BPM 843     [PM2000] 1590805 + [PM2000] 1590470.                                    Gvr2010 
18494+5811   STI2392     MLB 76.                                                                         
18494+1400   BPM 847     [PM2000] 1591238 + [PM2000] 1591692.                                    Gvr2010 
18494+1252   BPM 848     [PM2000] 1591568 + [PM2000] 1591349.                                    Gvr2010 
18496+1621   BPM 849     [PM2000] 1593370 + [PM2000] 1592493.                                    Gvr2010 
18496+1313   SHY 309     HIP  92388 + HIP  92638.                                                        
18497+1238   BPM 852     [PM2000] 1594564 + [PM2000] 1593619.                                    Gvr2010 
18497+1147   BPM 850     [PM2000] 1594069 + [PM2000] 1594283.                                    Gvr2010 
18497+1038   BPM 851     [PM2000] 1594230 + [PM2000] 1593700.                                    Gvr2010 
18497-0555   H 6  50     H VI 50. C is BD-06@4923.                                                       
                         A is a long-period spectroscopic binary.                                        
18497-2019   SEE 362     29 Sgr. Spectroscopic binary.                                                   
18497-7300   R   314     A is a spectroscopic binary.                                                    
18498+3249   H 5  40     A: nu 1 Lyr = 8 Lyr.  H V 40. A is a Beta Lyrae-type system.                    
18498+1639   BPM 853     [PM2000] 1594694 + [PM2000] 1594986.                                    Gvr2010 
18499+3233   HO  440     A: nu 2 Lyr = 9 Lyr                                                             
18499+2806   OSO 104     G184-032. None is a common proper motion pair                           Oso2004 
                         The 2002 measure by Osorio was mistakenly added as a different pair,    Oso2004 
                         designated AC. Pairs have been merged.                                          
18500+2043   HU  328     A is the Algol-type system AD Her.                                              
18500+1733   BPM 855     [PM2000] 1596993 + [PM2000] 1596377.                                    Gvr2010 
18500+1519   YSC  12     Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Nidever et al. (2002). They derived component masses 1.21 and 0.10      Nid2002 
                         Msun and an estimated semimajor axis of 34.92 mas.                      Ren2013 
                         HD 174457. Combined astrometric/spectroscopic solution, using                   
                         spectroscopic elements (P,T,e,omega) from Nidever et al. (2002 ApJS             
                         141, 503).                                                              SaJ2011 
18500+1420   BPM 854     [PM2000] 1596486 + [PM2000] 1595844.                                    Gvr2010 
18501+3322   STFA 39     STTA175. A is 10 Lyr = Sheliak = bet Lyr, the prototype variable of             
                         its class. B is BD+33@3224.                                                     
                         AB: H 5   3.                                                            MEv2010 
             CIA   3     Aa1,2: bet Lyr. Eclipsing binary (P=12.9d) resolved by CHARA Array              
                         (Zhao et al. 2008). Reductions by two techniques (MACIM and BSMEM) and  CIA2008b
                         a model fit listed in paper; MACIM and BSMEM results given in WDS and           
                         Interferometric Catalog. Three possible orbital solutions also given,           
                         adopting period and Tmin from Ak et al. (2007 A&A 463, 233) and e=0             
                         (Harmanec 2002 ANac 323, 87). These yield distance estimates ranging            
                         from 271 to 313 pc; masses for the gainer and donor are 12.76 +/- 0.27          
                         and 2.83 +/- 0.18 Msun, respectively.                                           
                         Aa1,2: Malkov et al. (2012) derive dynamical and spectroscopic masses           
                         19.84 +/- 11.13 and 15.84 Msun, respectively.                           Mlk2012 
                         In addition to the close pair there is also a hot spot with a size of   IAU2014b
                         22-33 solar radii. What is unknown is where the mass is lost and how            
                         much matter is in the jets.                                                     
18501+2949   HJ 1352     J   109.                                                                        
18501+1230   BPM 856     [PM2000] 1597921 + [PM2000] 1598622.                                    Gvr2010 
18502+1339   BPM 857     [PM2000] 1598720 + [PM2000] 1598294.                                    Gvr2010 
18502-3708   SWR 254     CPM pair                                                                Skf2004 
18503+1626   BPM 859     [PM2000] 1599627 + [PM2000] 1598472.                                    Gvr2010 
18503+1229   BPM 858     [PM2000] 1599448 + [PM2000] 1600027.                                    Gvr2010 
18503-0754   BU  969     S Scuti, variable 9.7-10.9, 148 days.                                           
18503-3736   SWR 255     CPM pair                                                                Skf2004 
18504+1554   BPM 860     [PM2000] 1600232 + [PM2000] 1600303.                                    Gvr2010 
18504+1336   BPM 861     [PM2000] 1600353 + [PM2000] 1599901.                                    Gvr2010 
18504+1241   J  469      Pair is +1m16s, -3" from BD+12 3661. In 1911 Jonckheere noted the               
                         companion was magnitude 10.0, and in 1915 14.0.                         Cou1955a
18504+1210   BPMA 62     [PM2000] 1600642 + [PM2000] 1600936.                                    Gvr2010 
18506+1525   BPM 862     [PM2000] 1601565 + [PM2000] 1600976.                                    Gvr2010 
18506+1458   BPM 863     [PM2000] 1601827 + [PM2000] 1600984.                                    Gvr2010 
18507+1233   BPM 864     [PM2000] 1602976 + [PM2000] 1603469.                                    Gvr2010 
18508+1301   BPM 865     [PM2000] 1603392 + [PM2000] 1602522.                                    Gvr2010 
18508+1059   STF2404     A spectroscopic binary. Composite spectrum, K5III+K3III.                        
18508-2210   BU 1300     30 Sgr.                                                                         
18509+1751   BPM 867     [PM2000] 1604886 + [PM2000] 1604822.                                    Gvr2010 
18509+1109   BRT1312     Also known as COU  16.                                                          
18509+1107   BPM 866     [PM2000] 1604810 + [PM2000] 1605623.                                    Gvr2010 
18510+1505   BPMA 63     [PM2000] 1605089 + [PM2000] 1604284.                                    Gvr2010 
18510+1339   BPM 868     [PM2000] 1605715 + [PM2000] 1605908.                                    Gvr2010 
18510+1041   BPM 869     [PM2000] 1605785 + [PM2000] 1605090.                                    Gvr2010 
18510-2018   PLT   3     A is BB Sgr, B is V 4088 Sgr.                                           Plt1934 
                         Primary is a Cepheid variable.                                          Evs2016a
18511+1421   BPMA 64     [PM2000] 1605963 + [PM2000] 1603708.                                    Gvr2010 
18511-1421   RST4602     J 1659.                                                                         
18511-3142   BRT3077     A likely plate flaw.                                                    Grv2021b
18512+5923   STF2420     omi Dra = 47 Dra. A is a spectroscopic binary and also variable.                
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: H 4  20.                                                            MEv2010 
             omi Dra     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Young (1920).                                                           YRK1920 
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Young (1920).                                                           YRK1920 
             CIA   8     Aa,Ab: Roettenbacher et al. (2015) resolve the RS CVn binary omi Dra            
                         and determined a combined spectroscopic/astrometric orbit. The orbital          
                         parallax is 9.36 +/- 0.10 mas (106.8 +/- 1.1pc), flux ratio in H is             
                         370 +/- 40, the system age 3.0 +/- 0.5 Gyr. Radii are 25.1 +/- 0.3 and          
                         1.0 +/- 0.1 Rsun, luminosities 220 +/- 30 and 1.3 +/- 0.2 Lsun.                 
                         Derived masses are 1.35 +/- 0.05 and 0.99 +/- 0.02 Msun.                CIA2015c
18515+4340   UC 3697     JKA   9. KIC 7871438/7871442.                                                   
18515+1700   BPMA 65     [PM2000] 1609645 + [PM2000] 1607904.                                    Gvr2010 
18515+1507   OL  105     Not found by Heintz at IDS position.                                    Hei1985a
18517+1600   BPM 870     [PM2000] 1611210 + [PM2000] 1610854.                                    Gvr2010 
18518-2141   DON 929     CPD-21@7088.                                                                    
18519-5756   HJ 5065     B is CPD-58@7511.                                                               
18520+5951   STI 866     LDS2752.                                                                        
18520+4243   LEH   1     Lehmann et al. (2016) find that KIC 7177553 is a quadruple system,              
                         consisting of two close binaries of nearly equal magnitude, separated           
                         by about 0.4". They estimate the distance to the quadruple as 406 +/-           
                         10 pc, giving a physical separation of the wide pair 167+/- 5 au and            
                         an orbital period >1000y.  One close pair is an eclipsing binary with           
                         orbital period 18.00d. The other pair is an SB with period 16.5d. All           
                         four stars are of similar mass and spectral type (main-sequence G).     Leh2016 
18520+1047   STF2408     Also known as GAN   6.                                                          
18520-5418   TOK 325     Triple system. The inner astrometric binary is resolved here; the CPM   Tok2012c
                         companion at 146 is found by Tokovinin & Lepine (2012).                 Tok2013b
18521+2431   COU 510     Previously classified as an Algol-type system, JZ Her, Petr Zasche              
                         (personal corres.) reports that Couteau must have confused it with      Cou1972a
                         the nearby HS Her. This pair is non-variable and is often used as a             
                         check star in variability analyses.                                             
18521+1635   BPM 871     [PM2000] 1615013 + [PM2000] 1614900.                                    Gvr2010 
18522+1409   BPM 872     [PM2000] 1615303 + [PM2000] 1616136.                                    Gvr2010 
18522+1203   BPM 873     [PM2000] 1615368 + [PM2000] 1615921.                                    Gvr2010 
18522-6211   HJ 5062     lam Pav. A is a Cepheid.                                                        
18523+3926   WEI  33     B is BD+39@3557.                                                                
18523+2126   ISO   8     112 Her. A spectroscopic binary, P = 6.36d. The interferometric pair            
                         cannot be this object, so the system is triple.                                 
18523+1432   STF2411     B spectrum F7V. It is called a spectroscopic binary.                            
18523+1357   BPM 874     [PM2000] 1616566 + [PM2000] 1617001.                                    Gvr2010 
18524+1445   BPMA 66     [PM2000] 1617269 + [PM2000] 1616881.                                    Gvr2010 
18525+1644   BPM 875     [PM2000] 1618619 + [PM2000] 1618464.                                    Gvr2010 
18526+1414   BPMA 67     [PM2000] 1619286 + [PM2000] 1619792.                                    Gvr2010 
18528+3125   A   257     Also a faint unequal pair about 28" from CD in 226@.                            
18528+1357   BPM 876     [PM2000] 1621241 + [PM2000] 1620626.                                    Gvr2010 
18528+1234   AG  365     B is BD+12@3695.                                                                
18528-1725   HU  257     Spectrum: Fm Delta Del.                                                         
18528-5057   HJ 5067     SWR 256.                                                                        
18529-5708   LUH  14     LHS 3421 + 2MASS J18525777-5708141.                                     Luh2012b
18530+5816   ES 1746     MLR 359.                                                                        
18530-0935   CHR  81     This system, first announced by McAlister and recalled in a later       McA1984b
                         McAlister paper after repeated attempts at confirmation, has been       McA1993 
                         restored. While perhaps still spurious, the subsequent confirmation or          
                         suspected duplicity (by another technique) makes the discovery                  
                         measurement somewhat more probable.                                             
18531+7405   GC 26011    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
18531+1412   BPM 877     [PM2000] 1623188 + [PM2000] 1622811.                                    Gvr2010 
18531-5011   MUG  10     Aa,Ab: PZ Tel. Companion shows common proper motion and detected                
                         orbital motion. Infrared magnitudes are consistent with companion               
                         being a brown dwarf of mass 28 +12/-4 Mjup and Teff = 2500-2700K.       Mug2010 
                         Biller et al. (2010) derive spectral types K0, M7 +/- 2, estimated      Bil2010 
                         masses 1.25 +0.05/-0.20 Msun and 36 +/- 6 Mjup. Age 12 +8/-4 Myr,               
                         distance 51.5 +/- 2.6 pc. Their JHK magnitudes are derived from 2MASS   TMA2003 
                         photometry, combined with their magnitude differences.                          
                         PZ Tel. Member of the bet Pic moving group.                             Zuc2001b
18533+1737   BPM 878     [PM2000] 1624711 + [PM2000] 1625113.                                    Gvr2010 
18533+1557   BPM 879     [PM2000] 1625218 + [PM2000] 1625017.                                    Gvr2010 
18534+2417   RAO 513     DI Her.                                                                         
18534+1851   LDS5867     LDS6332.                                                                        
18535+7547   STF2452     233 Dra. A spectroscopic binary.                                        D__1883 
                         Aka H 2  31 = S   713.                                                  Bu_1906 
18535+0912   ROE 112     J 2930. Roe and Jonckheere measures of AB were earlier erroneously      Roe1918 
                         attributed to BC.                                                       J__1962a
18535-2030   DON 933     CPD-20@7296.                                                                    
18536-1941   RST3203     Spectrum: A2/3II/III.                                                           
18537+4550   DEA 437     JKA  13. KIC 9326053/9326073.                                                   
18537+3658   H 6   3     H VI 3. del 1 Lyr = 11 Lyr. A is a SB. B is BD+36@3308.                         
18537+1353   BPM 880     [PM2000] 1628451 + [PM2000] 1628755.                                    Gvr2010 
18537-0533   A    93     Wilson's value for omega was corrected by Muller.                       WRH1954c
                                                                                                 Mlr1954d
18538+1756   BPM 881     [PM2000] 1628952 + [PM2000] 1628974.                                    Gvr2010 
18540+1516   L    40     Hipparcos acceleration double solution.                                         
                         J  2585.                                                                Nsn2016 
18541+1500   HD175292    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
18541-5131   RST1008     V362 Tel, Algol-type eclipsing binary, P = 1.21125 d.                   Zas2011 
18541-5421   HJ 5068     LDS 656.                                                                        
18542-2245   BU 1033     nu 1 Sgr = 32 Sgr = Ainalrami                                                   
             nu Sgr      Henroteau notes that Ptolemy (Magna compositio. Venetiis 1515, lib      HFC1928 
                         VIII, cap 1) called the 14' pair nu 1 + nu 2 Sgr a double star.                 
                         This is perhaps the earliest description of a double star.                      
18543+4259   OSO 105     G205-042. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
18543+1158   BPM 882     [PM2000] 1633715 + [PM2000] 1634697.                                    Gvr2010 
18545+4823   WOL   4     KOI1725.                                                                        
18545+3654   ES 2028     del 2 Lyr = 12 Lyr. A is an unclassified variable.                              
18545+1149   BPM 883     [PM2000] 1634622 + [PM2000] 1634682.                                    Gvr2010 
18546+2754   BRT3335     ADS 11819a. Originally published as BRT 185.                            Brt1928 
18547+2239   BU  646     113 Her. The G-type component is a long-period spectroscopic binary.            
             MKT   9     Visual orbit by Hummel et al. (1995) based on astrometry from Mark III  MkT1995 
                         interferometer. Additional spectroscopic data yield component masses,           
                         luminosities, radii, effective temperatures, and distance.                      
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Hummel et al. (1995).                                                   MkT1995 
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 1.71 +/- 3.27, 5.64, and 4.08 Msun, respectively.  Mlk2012 
                         Aa,Ab: Ren & Fu (2013) calculated an astrometric orbit, combining       Ren2013 
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Luyten (1936).                                                          Luy1936 
18547-1946   OL   80     DON 934. J 1752.                                                                
18549+4734   DEA 460     JKA  14. KIC 10388283/10388259.                                                 
18549+3358   STT 525     A is a spectroscopic binary. C is BD+33@3256.                                   
18549+1201   BPM 884     [PM2000] 1637865 + [PM2000] 1638783.                                    Gvr2010 
18549-2157   RSS 495     CD-22@13417                                                                     
18550+4822   KOI2754     This system hosts a 0.7 Rearth planet candidate with a 1.3 day period           
                         (Burke et al. 2014). Our ARIES observations revealed a companion 2.11   KOI2014a
                         J mags and 1.65 Ks mags fainter than KOI2754 at a 0".763 separation.            
                         The predicted Kp mag of the companion star is Kp = 15.3 (dKp = 3.0)             
                         if the star is a dwarf and Kp = 15.2 (dKp = 2.9) if the star is a               
                         giant. The companion star was also detected in the WIYN speckle                 
                         imaging acquired with DSSI. The companion is 3.12 mag. fainter than             
                         KOI2754 at 692 nm and 2.56 mags fainter at 880 nm. Assuming that the            
                         planet orbits the target star and that all of the light from the                
                         companion is captured in the Kepler aperture, then the planet radius            
                         should be increased by 3% to account for dilution. KOI2754 does not             
                         exhibit a significant source offset during transit.                     Dre2014 
18550+1136   BPM 886     [PM2000] 1638955 + [PM2000] 1638009.                                    Gvr2010 
18550+1119   BPM 885     [PM2000] 1638777 + [PM2000] 1638092.                                    Gvr2010 
18550-6356   NZO  93     Not found by Heintz at IDS position. Position since corrected.          Hei1990b
18551+4051   HEI  73     KIC 5598639. Primary is Algol-type elipsing binary, period 1.29755d.    Zas2017b
18551+1537   BPM 887     [PM2000] 1639912 + [PM2000] 1640333.                                    Gvr2010 
18551+1522   BPMA 68     [PM2000] 1639841 + [PM2000] 1637903.                                    Gvr2010 
18552+4409   GIC 153     G205-045/G205-044.                                                              
18553+1304   BPMA 69     [PM2000] 1641172 + [PM2000] 1641740.                                    Gvr2010 
18553-2341   B   412     Spectrum: B9.5III/IV.                                                           
18553-2618   BED   1     Aa,Ab: Measure of 1991.566 made by MAPPIT.                              Bed1994 
             SMY   4     AB: sig Sgr = 34 Sgr = Nunki. B is CD-26@13591.                                 
18554+1331   BU  647     Also DU    2, BDS 8899. Identification, position corrected by Heintz.   Hei1983a
18554-4131   BRT1082     A likely plate flaw.                                                    Grv2021b
18555+1413   BPM 888     [PM2000] 1643332 + [PM2000] 1643189.                                    Gvr2010 
18555+0816   J  1191     BRT3336.                                                                        
18556+1413   BPM 889     [PM2000] 1643867 + [PM2000] 1642939.                                    Gvr2010 
18557+1254   COG   1     CD: OL  189.                                                                    
                         J   810.                                                                Nsn2016 
18557+1216   BPM 890     [PM2000] 1644364 + [PM2000] 1643759.                                    Gvr2010 
18558+1243   BPM 891     [PM2000] 1645258 + [PM2000] 1644843.                                    Gvr2010 
18558+0327   A  2192     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.52 +/- 2.27, 3.68, and 1.82 Msun, respectively.             Mlk2012 
18559+2333   MET  87     V775 Her.                                                                       
18559+1258   BPM 892     [PM2000] 1646011 + [PM2000] 1645924.                                    Gvr2010 
18559+0323   A  2193     Quadrants uncertain.                                                            
18560+4414   STT 365     AB: Duplicity doubtful, needs speckle.                                          
             STF3130     Lewis  measures a pair 1m following and 1' south:                       L__1897 
                         1897, 37@, 3.1", 10.0-11.0.                                                     
18560+3347   STF2421     B is BD+33@3264.                                                                
18560+1147   BPM 893     [PM2000] 1646644 + [PM2000] 1647444.                                    Gvr2010 
18560-2503   B   413     A is a close 312-d spectroscopic pair.                                  Tok2019a
18561+1709   BPM 894     [PM2000] 1647451 + [PM2000] 1647696.                                    Gvr2010 
18562+0412   STF2417     A: the 1 Ser = 63 Ser A = Alya                                                  
                         B: the 2 Ser = 63 Ser B = BD+04@3917.                                           
                         AC: C component = A component of 18566+0416 TOK 620.                            
                         BC: This system was analysed in detail by Teague, who determined the    Tea2001 
                         source of the errors in all three historical measures (Labitzke,        Lbz1929 
                         Przbyllok, and Kamper), which actually belong with the AC pair of this  Prz1926 
                         system.                                                                 Kpr1992 
                         BC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: H 4   6.                                                            MEv2010 
18562-5049   RST1011     Spectral type G8/K0 II/III.                                                     
18563+5432   HDS2682     Aa is also a 8d spectroscopic binary (Aa1,Aa2).                         Tok2019b
                         AB = G229-018/G229-019. The B component is GJ 4091B.                            
18563+1435   BPM 896     [PM2000] 1648823 + [PM2000] 1649237.                                    Gvr2010 
18563+1344   BPM 895     [PM2000] 1648725 + [PM2000] 1648525.                                    Gvr2010 
18563-0425   LDS 659     HIP 92960. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
18564+4530   HJ 1356     AB: JKA  17. KIC 9139163/9139151.                                               
                         B is BD+45@2796.                                                                
                         HJL 261.                                                                HJL1986 
18564+1710   BPM 897     [PM2000] 1649308 + [PM2000] 1650135.                                    Gvr2010 
18564-4040   WG  238     CPD-40@8697. SWR 258.                                                           
                         CPM pair. ASAS J185622-4040.6 (spurious variable?)                      Skf2004 
18565-0511   BRT 485     LEO 43.                                                                         
18565-5313   SWR 257     CPM pair                                                                Skf2004 
18566+1545   BPM 898     [PM2000] 1650833 + [PM2000] 1651015.                                    Gvr2010 
18566+0416   TOK 620     A component = C component of 18562+0412 STF2417AC.                              
18567+5014   JNN 153     2MASS J18564143+5014071 and J18564286+5013483 are separated by only             
                         23" and have similar estimated spectroscopic distances (79 and 77 pc,           
                         respectively) in Riaz et al. (2006), as well as very similar proper     Ria2006 
                         motions (e.g. Roser et al. 2010), hence it is likely that they form a   XXX2010 
                         physical pair.                                                          Jnn2012 
18567+1657   BPM 899     [PM2000] 1651939 + [PM2000] 1652523.                                    Gvr2010 
18568+1733   BPM 901     [PM2000] 1652793 + [PM2000] 1653380.                                    Gvr2010 
18568+1505   BPM 900     [PM2000] 1652502 + [PM2000] 1651646.                                    Gvr2010 
18569+4048   KOI1962     Distance is 1101 +/- 629/294 pc. Ma (Mb) = 1.05 (1.02) +/- 0.1 \msun.   Hor2024 
18569+3112   ES 2422     A is the irregular variable OQ Lyr.                                             
18569+1546   L    42     Baize questions BD identification.  Heintz and Worley were unable to    Baz1944a
                         locate this pair. Identical to OL 180?                                  Hei1983a
18569-3320   GLP  15     B is CD-33@13738.                                                               
18570+3254   BU  648     Identification of the ascending node is somewhat uncertain.             Stk1939 
                         AB: Primary is SB1 and exoplanet host, P=1016d, in a 61y binary         Mut2010e
                         (Muterspaugh et al. 2010). Wobble 1016d, 0.24mas - planet? Astrometric          
                         orbit gives mass 1.5 Mjup if planet around B, 3 Mjup if around A.       Tok2014d
                         AB,C: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB,C: Rectilinear solution by Hurowitz et al. (2014).                   USN2014b
18570+1752   BPM 902     [PM2000] 1653997 + [PM2000] 1654609.                                    Gvr2010 
18571+5143   SHY 749     HIP  93029 + HIP  92467.                                                        
18572+3845   COU1611     TDT1145                                                                         
18573+6224   STF2440     Spectrum of A also called composite; G5IV+G8V.                                  
18573+1800   BPMA 70     [PM2000] 1655946 + [PM2000] 1654297.                                    Gvr2010 
18573+1724   BPM 904     [PM2000] 1656031 + [PM2000] 1655503.                                    Gvr2010 
18573+1644   BPM 903     [PM2000] 1655854 + [PM2000] 1656255.                                    Gvr2010 
18574+2129   HU  329     Many negative results, but probably double.                                     
18574+1517   BPM 905     [PM2000] 1657245 + [PM2000] 1657814.                                    Gvr2010 
18575+5814   STF2438     H 1  43.                                                                MEv2010 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.95 +/- 1.38, 3.19, and 2.19 Msun, respectively.             Mlk2012 
18575+1306   BPMA 71     [PM2000] 1657465 + [PM2000] 1659069.                                    Gvr2010 
18576+7250   OSO 106     G260-013. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
18576+1420   BPM 906     AB: [PM2000] 1658704 + [PM2000] 1659034.                                Gvr2010 
             BPM 907     BC: [PM2000] 1659034 + [PM2000] 1658470.                                Gvr2010 
18577+1731   BPM 908     [PM2000] 1658828 + [PM2000] 1659154.                                    Gvr2010 
18577+1509   OL  180     Position and Durchmusterung correction by Heintz.                       Hei1980a
                         OL  191.                                                                        
18577+1312   BPM 909     [PM2000] 1659281 + [PM2000] 1658736.                                    Gvr2010 
18577+0942   HJ 5505     B is BD+09@3942.                                                                
18578-3802   B   414     Spectral type K?                                                                
18579+4424   KOI 122     Adams et al. (2012) theta values corrected to 360-theta                 Adm2012 
                         (reported by Dressing et al. (2014).                                    Dre2014 
18579+4214   COU1795     TDT1149.                                                                        
18579-2524   B  2871     Spectrum: F2/3III/IV.                                                           
18580+6159   ES 1843     Rectilinear solution by Cvetkovic et al. (2018).                        Cve2018 
18580+1543   BPM 910     [PM2000] 1661167 + [PM2000] 1660955.                                    Gvr2010 
18581+4711   AG  366     Astroseismology determines Mass and Radius for A(B) as 0.95+/-0.02      XXX2017b
                         (0.93+/-0.01) \msun and 0.93+/-0.01 (0.89+/-0.01) \rsun and an age of           
                         3.0+/-0.5 Gyrs for both stars.                                                  
18581+3813   STF2427     B is BD+38@3377. BC is also known as ALI 875.                                   
18582+1722   CHR  82     Aa,Ab is the Cepheid FF Aql. The system is also a long-spectroscopic            
                         binary, now resolved by speckle.                                                
18582+1644   BPM 911     [PM2000] 1662278 + [PM2000] 1661343.                                    Gvr2010 
18582-2025   HO  271     A is a double-lined spectroscopic binary.                                       
                         Classification of the B component is from Lindroos (1985), who also     Lnd1985 
                         gives a distance of 1.9 kpc to the system.                              Msn1998a
18583+4857   GII  46     Gili (2016) described this pair as the B component of 18582+4858                
                         KOI 258, but the systems differ in position by over 1'.                 Gii2016 
18583+1705   BPM 912     [PM2000] 1663427 + [PM2000] 1663942.                                    Gvr2010 
18583+1654   BPMA 72     [PM2000] 1662798 + [PM2000] 1664716.                                    Gvr2010 
18584+4750   BD+47 2730  Spectroscopic orbit of 858.1d corresponds to this astrometric pair.     Grf2014d
18584+3625   STF2429     H 1  58.                                                                MEv2010 
18584+1459   BPM 913     [PM2000] 1663987 + [PM2000] 1664237.                                    Gvr2010 
18585+1429   BPM 914     [PM2000] 1664713 + [PM2000] 1664939.                                    Gvr2010 
18586+1703   BPMA 73     [PM2000] 1664953 + [PM2000] 1663498.                                    Gvr2010 
18586+1653   BPM 916     [PM2000] 1664901 + [PM2000] 1664659.                                    Gvr2010 
18586+1514   BPM 915     [PM2000] 1664752 + [PM2000] 1665020.                                    Gvr2010 
18588+4041   STF2431     BDS 8981, H IV 93 is identical. A spectroscopic binary.                         
                         H 4  93.                                                                        
18588-0648   J   111     J 2684.                                                                         
18589+3241   AGC   9     gam Lyr = 14 Lyr = Sulafat. Variable? Also known as STT 544.                    
                         AC. Smyth's quoted separation is difference in RA only.                 Smy1844 
18590+1542   BPM 917     [PM2000] 1667679 + [PM2000] 1667227.                                    Gvr2010 
18591+1338   STF2424     11 Aql.                                                                         
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: H 3  32.                                                            MEv2010 
18591-2609   B   415     J 1733.                                                                         
18594-1250   KUI  89     A light variable.                                                       Baz1954a
                         1985.4872: This measurement was incorrectly attributed to Kui 84                
                         (WDS 17584+0427) by McAlister et al. (1987).                            McA1987b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.80 +/- 1.84, 4.41, and 5.25 Msun, respectively.             Mlk2012 
18595+1631   BPM 918     [PM2000] 1670405 + [PM2000] 1670058.                                    Gvr2010 
18595+1420   BPMA 74     [PM2000] 1670255 + [PM2000] 1671086.                                    Gvr2010 
18596+1504   ENG  65     13 Aql = eps Aql. A is a spectroscopic binary.                                  
                         Spectral type K1IIICN0.5Ba0.2.                                                  
             eps Aql     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin (1982).                                                         Grf1982c
18596+1317   BPM 919     [PM2000] 1670767 + [PM2000] 1670975.                                    Gvr2010 
18597+1345   BPM 920     [PM2000] 1671285 + [PM2000] 1671690.                                    Gvr2010 
18597+1206   BPMA 75     [PM2000] 1671862 + [PM2000] 1670609.                                    Gvr2010 
18599+1937   L    43     Not found by Heintz at IDS position.                                    Hei1985a
                         Position in ADS and later WDS was erroneously given as 18597+1036,              
                         although pair also not seen at "correct" coordinates.                           
18599+1454   STF2428     AB: H 2  93.                                                            MEv2010 
19000+3916   MLB 859     Not found by Heintz at IDS position.                                    Hei1985a
19002+1353   BPM 921     [PM2000] 1674730 + [PM2000] 1675218.                                    Gvr2010 
19003+4835   DEA 191     JKA  19. KIC 11017620/11017626.                                                 
19003+4625   KOI2706     The system hosts a 1.5 Rearth planet candidate with a 3.1 day orbit             
                         (Burke et al. 2014).  The estimated dilution correction for this        KOI2014a
                         system is a 0.2% increase in the radius of the planet candidate.                
                         KOI 2706 exhibits a 0".83 (3.7 sigma) source offset during transit.     Dre2014 
19003-0914   BRT 488     AB: J  2245AB.                                                                  
19004+0552   LDS6333     Pair found using AGK3+5:2636 as starting point to reach the place.              
                         Here is a pair that is barely alike to NLTT data. May be a noticeable           
                         change. Nothing else around the zone.                                   Gel1987 
19005+1657   BPM 922     [PM2000] 1676683 + [PM2000] 1676889.                                    Gvr2010 
19006+4500   KOI2159     This system hosts one candidate planet with a period of 7.6 days and a   .      
                         radius of 1.1 Rearth (Batalha et al. 2013). The NASA Exoplanet Archive  KOI2013a
                         entry for KOI2159 also includes a 1 Rearth false positive at a period           
                         of 2.4 days. The estimated dilution correction due to the extra light           
                         from the companion is a 3% increase to the planet radius. KOI2159 does          
                         not display a significant source offset during transit.                 Dre2014 
19006-0807   STF2425     B is BD-08@4810.                                                                
19007+1431   BPM 923     [PM2000] 1677681 + [PM2000] 1677628.                                    Gvr2010 
19008+1118   BPM 924     [PM2000] 1678452 + [PM2000] 1678224.                                    Gvr2010 
19008-0027   HJ  874     Bloch measures 1923.7, 260@, 16.96", which actually belongs to          Blo1931 
                         19000+1253 STF2426AB.                                                           
19010+1507   BPM 925     [PM2000] 1679533 + [PM2000] 1679239.                                    Gvr2010 
19010-2439   COO 230     ADS 11921.                                                                      
                         J  1599.                                                                Nsn2016 
19010-4455   CPO 605     A likely plate flaw.                                                    Grv2021b
19011-3657   JOY   7     A is the T-Tauri variable S CrA.                                                
19011-3704   BSO  14     B is CD-37@13017. Both components are spectroscopic binaries.                   
                         SWR 259. CPM pair                                                       Skf2004 
19012+1253   J  1279     Not found in 1959 by Van Biesbroeck. He suggests it may be ADS 12017.           
                         Found by Heintz, who notes that the OL pair at 19 02.6 +12 56 is        Hei1987a
                         identical.                                                                      
                         OL  192.                                                                        
19012+0229   GC 26129    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
19013+1758   BPM 926     [PM2000] 1681692 + [PM2000] 1682051.                                    Gvr2010 
19014+4656   HJ 1362     16 Lyr.                                                                         
19014-3548   BRT1794     CPD-35@8339.                                                                    
                         A likely plate flaw.                                                    Grv2021b
19016+1429   BPM 927     [PM2000] 1683796 + [PM2000] 1682902.                                    Gvr2010 
19016-3653   B   957     C is the irregular variable TY CrA, resolved into a 0.3" pair                   
             CVN  13     by Chauvin et al. (2003). The Ca component is also a close                      
                         spectroscopic triple, including one eclipsing pair.                     Cvn2003b
19018+1638   BPM 930     [PM2000] 1685383 + [PM2000] 1686044.                                    Gvr2010 
19018+1554   BPM 928     [PM2000] 1685084 + [PM2000] 1684425.                                    Gvr2010 
19018+1253   BPM 929     [PM2000] 1685237 + [PM2000] 1684483.                                    Gvr2010 
19019+4138   KOI1613     Distance is 492.5 +/- 161.2/97.4 pc. Ma (Mb) = 1.19(0.87)+/-0.1 \msun.  Hor2024 
19019+1910   STF2437     Primary = E component of 19020+1907 ARN  18AE.                                  
19019-2340   ARA2252     Aka WFC 286.                                                                    
19019-3620   B   958     Spectral type M?                                                                
19019-3657   VSP   1     R CrA. HBC 288.                                                                 
19020+1907   ARN  18     AE: E component = primary of 19019+1910 STF2437.                                
             HJ 2851     AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
19020+0846   BU  973     Van Biesbroeck notes that this group is misidentified in both BDS and   VBs1965 
                         ADS as BD+08@3945 rather than the correct BD+08@3948. The latter is     Bu_1906 
                         already identified with ADS 11954, J 533. It seems advisable to keep    A__1932a
                         the ADS number 11947.                                                           
                         Here AB is BU 973, STF 2435 = AC of J 533. AD = AB of J 533.  DC =              
                         Howe 45 is BC of J 533. AB is the C component of 19022+0845STF2436.             
             STF2435     C component = C component of 19022+0845 STF2436AC.                              
19022+1630   BPM 931     [PM2000] 1687652 + [PM2000] 1687123.                                    Gvr2010 
19022+0845   STF2436     B is BD+08@3949.                                                                
                         C component = 19020+0846 STF2435AC.                                             
19024+1535   BPM 932     [PM2000] 1688945 + [PM2000] 1689575.                                    Gvr2010 
19024+1332   BPM 933     [PM2000] 1689380 + [PM2000] 1689255.                                    Gvr2010 
19024-0536   PLT   4     A is FG Aql, B is FH Aql.                                               Plt1934 
19024-3656   REP   4     Erroneously listed as 04385+1611.                                               
19026+5719   STI2407     One deg error in WDS designation.                                               
19026+1611   BPM 934     [PM2000] 1690498 + [PM2000] 1689949.                                    Gvr2010 
19026-0621   A    42     CD same as J  2162.                                                     Dam2010 
19026-2953   HDO 150     zet Sgr = 38 Sgr = Ascella. Spectrum composite; A2III+A4IV.                     
                         Masses and bolometric magnitudes are derived for the two components             
                         of this system by Mason et al. (1999), based on assumed spectral types  Msn1999a
                         and available parallaxes.                                                       
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 5.24 +/- 0.37, 3.45, and 2.46 Msun, respectively.  Mlk2012 
             H 5  78     AB,C: H V 78.                                                                   
19027+4307   YSC  13     Slightly metal-poor F5 primary. Preliminary orbit gives a mass sum 5.8          
                         +/- 2.1 Msun; the magnitude difference suggests an F2 primary and F8            
                         secondary, but this would imply a mass sum ~3 Msun                      Hor2012b
19027+1650   BPM 935     [PM2000] 1691217 + [PM2000] 1691945.                                    Gvr2010 
19027-0027   J   475     This is the planetary nebula NGC 6741.                                          
19027-3606   HJ 5080     SWR 260.                                                                        
19028+3123   STF2441     BDS 9008; H I 60 is probably same star.                                         
                         H 1  60.                                                                        
19028+1417   BPM 936     [PM2000] 1691784 + [PM2000] 1692123.                                    Gvr2010 
19029+2429   POU3668     Also known as J  2935.                                                          
19029-0342   A  3105     14 Aql. Rapidly moving binary, position angles scattered.               WRH1955 
19029-4245   LDS 663     Also known as RSS 504.                                                          
19032+1717   BPM 939     [PM2000] 1694438 + [PM2000] 1693749.                                    Gvr2010 
19033+1702   BPM 940     [PM2000] 1695373 + [PM2000] 1695930.                                    Gvr2010 
19033+1701   BPM 937     AB: [PM2000] 1694906 + [PM2000] 1694269.                                Gvr2010 
             BPM 938     BC: [PM2000] 1694269 + [PM2000] 1693765.                                Gvr2010 
19033+1651   BPM 941     [PM2000] 1695391 + [PM2000] 1695341.                                    Gvr2010 
19034+1608   BPM 942     [PM2000] 1695695 + [PM2000] 1695015.                                    Gvr2010 
19035+2421   GEL   1     Measured due to misidentification with 19035+2422 POU3674.                      
19035+1549   BPM 944     [PM2000] 1696619 + [PM2000] 1696194.                                    Gvr2010 
19035+1500   BPM 943     [PM2000] 1696277 + [PM2000] 1695902.                                    Gvr2010 
19035-6845   FIN 357     Martin et al. (1998) derive component masses 1.892 +/- 0.265 and                
                         1.647 +/- 0.246 Msun.                                                   Mig1998 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.21 +/- 0.54, 2.98, and 1.10 Msun, respectively.             Mlk2012 
                         Docobo & Andrade (2013) derive a dynamical parallax of 18.51 +/- 0.46           
                         mas and component masses 1.49 +/- 0.15 and 1.38 +/- 0.14 Msun                   
                         (for spectral type F8V) or 19.69 +/- 0.52 mas, 1.25 +/- 0.13 and 1.14           
                         +/- 0.12 Msun (for G0IV). See paper for extensive notes on system.      Doc2013d
19036+3812   ES 2672     ALI 879.                                                                        
19037+5727   ARG  33     A is the Algol-type system BH Dra.                                              
19037+3545   STF2448     H 1  59.                                                                MEv2010 
19037-2243   DON 945     A is the semiregular variable SU Sgr.                                           
19038+4941   DEA 453     JKA  21. KIC 11600772/11600744.                                                 
19038+1651   BPM 945     [PM2000] 1698915 + [PM2000] 1699239.                                    Gvr2010 
19038-3451   BRT3338     A likely plate flaw.                                                    Grv2021b
19039+3409   BU 1285     A: Burnham noted "possibly a close pair" in 1892, but Aitken found      Bu_1906 
                         it single in 1899 using the 36-inch.                                            
19039+2642   A  2992     Only elements P, T, and a of the orbit of Dommanget (1978) were         Dom1978 
                         adjusted by Starikova (1981).                                           Sta1981a
19039+1623   BPM 947     [PM2000] 1699191 + [PM2000] 1699396.                                    Gvr2010 
19039+1527   BPM 946     [PM2000] 1699167 + [PM2000] 1698750.                                    Gvr2010 
19040+1813   BPM 948     [PM2000] 1699831 + [PM2000] 1699703.                                    Gvr2010 
19041+1106   AG  371     J 477.                                                                          
19042+3638   ADM   4     TrES-1. Primary is exoplanet host star.                                 Adm2013 
19042+2519   BRT 187     A likely plate flaw.                                                    Grv2021b
19042+1705   BPM 949     AB: [PM2000] 1701291 + [PM2000] 1700687.                                Gvr2010 
             BPM 950     BC: [PM2000] 1700687 + [PM2000] 1700757.                                Gvr2010 
19042-2254   H N 129     HDO 151.                                                                        
19043+1725   BPM 951     [PM2000] 1701823 + [PM2000] 1701868.                                    Gvr2010 
19043-1128   HO   94     J 2251.                                                                         
19044+1328   BPM 952     [PM2000] 1702577 + [PM2000] 1703176.                                    Gvr2010 
19044-1553   UTR   1     A is V 727 Sgr, B is V 728 Sgr.                                         Plt1934 
19045+1809   BPM 953     [PM2000] 1703252 + [PM2000] 1703253.                                    Gvr2010 
19045+1104   BPM 954     [PM2000] 1703414 + [PM2000] 1703632.                                    Gvr2010 
19046+1819   BPMA 76     [PM2000] 1704418 + [PM2000] 1703420.                                    Gvr2010 
19046+1739   BPM 955     [PM2000] 1704325 + [PM2000] 1704815.                                    Gvr2010 
19046-3635   BRT1796     SWR 261. CPM pair. Dwarfs                                               Skf2004 
19047+1734   BPMA 77     [PM2000] 1705092 + [PM2000] 1705774.                                    Gvr2010 
19047+0756   SMA  83     J 2582.                                                                         
19047-2144   SEE 369     omi Sgr = 39 Sgr                                                                
19048+1551   BPM 956     [PM2000] 1705775 + [PM2000] 1705472.                                    Gvr2010 
19049+1552   BPM 957     [PM2000] 1706592 + [PM2000] 1706496.                                    Gvr2010 
19050-0402   SHJ 286     15 Aql. B is BD-04@4683.                                                        
                         H 5  33.                                                                MEv2010 
19050-0709   STF2439     Primary is V1440 Aql, a Beta Lyr type eclipsing binary, P = 1.83672d.   Zas2012 
19051-4508   SKF1152     Initial WDS designation (19051-4935) garbled - dec copied from SKF1151          
19052+4955   ES 2673AB   This cannot be the close 674.7-d spectroscopic binary.                  Grf2009a
19053+2555   GJ 743.2    Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from Vogt et al.  CPS2000c
                         (2000).                                                                 HaI2001 
             EGN  24     AB pair bound.  Primary is planet host star. Colors of B component              
                         consistent with M2-M5 dwarf, mass 0.23 +/- 0.01 Msun. A is a very               
                         evolved K0 subgiant.                                                    Egn2007 
                         CHARA Array Limb-darkened diameter  0.467 +/- 0.058 mas,                CIA2008c
                         R =  2.99  +/- 0.39  \rsun.                                                     
19053+1811   BPM 958     [PM2000] 1709391 + [PM2000] 1709708.                                    Gvr2010 
19054+3803   AG  227     Very different proper motion. Despite having an orbit,                  Izm2019 
                         an optical pair based on parallax.                                      Mlk2022 
19054+1820   BPMA 78     [PM2000] 1710040 + [PM2000] 1708036.                                    Gvr2010 
19054+1352   BU  287     zet Aql = 17 Aql. A is a spectroscopic binary.                                  
                         CHARA Array Limb-darkened diameter  0.895 +/- 0.017 mas,                CIA2012e
                         R =  2.449 +/- 0.046 \rsun, L = 38.492 +/-0.627 \lsun,                          
                         Teff = 9205 +/-  95 K, M = 1.984 +/- 0.006 \msun,                               
                         Age =  0.8 +/- 0.0 Gyr.                                                         
                         AC. Smyth's quoted separation is difference in RA only.                 Smy1844 
19055+3352   HU  940     aka HO  635                                                                     
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.08 +/- 0.94, 2.25, and 1.10 Msun, respectively.             Mlk2012 
19056+1702   BPM 959     [PM2000] 1711312 + [PM2000] 1711110.                                    Gvr2010 
19056+1005   BRT3224     J 2164.                                                                         
19056-5347   HJ 5081     B is CPD-53@9461.                                                               
19057+6502   ES 1914     Position corrected by Heintz, who also notes that the pair J 1353 is    Hei1980a
                         identical.                                                                      
19057+1659   BPM 961     [PM2000] 1711605 + [PM2000] 1711341.                                    Gvr2010 
19057+1136   BPM 960     [PM2000] 1711462 + [PM2000] 1711494.                                    Gvr2010 
19057-1540   HJ 5507     A is a spectroscopic binary. Variable?                                          
19058+5918   MLR 217     AB is STI 873, not in WDS because of questionable duplicity.                    
19058+3831   STF2456     B is BD+38@3428. The 1888 AC measure was earlier erroneously also       StH1906A
                         attributed to BC.                                                               
             STH   5     BE: Incorrectly added as AD, in part due to reversed identifications            
                         of A and B by Struve. Companion designation changed to E, as existing   StH1901 
                         BD pair measured to different star.                                             
19058+0633   STF2446     Mt. Wilson spectral types F3s and G5.                                           
                         AB: HJL 262.                                                            HJL1986 
                         AB: H 3 108.                                                            MEv2010 
19059+4006   DEA 435     JKA  25. KIC 4995565/4995581.                                                   
19059+3004   L    27     Possibly BD+29@3478 (9.3).                                                      
19060+4549   STF2463     AC: In Cin. 5 a faint pair is noted: 1879.5, 300@, 18.4". See BDS       Bu_1906 
                         part II for a discussion of possible identifications.                           
19060+3553   H 5 103     H V 103.                                                                        
19061+1732   BPM 962     [PM2000] 1714383 + [PM2000] 1714837.                                    Gvr2010 
19062+4926   DSG   2     Kepler 296 = KOI-1422. Derived properties for the A and B components            
                         are as follows:                                                                 
                           Teff (K)       3740  +/- 130         3440  +/- 75                             
                           Radius (Rsun)  0.480 +0.066/-0.087   0.322 +0.060/-0.068                      
                           Mass (Msun)    0.498 +0.067/-0.087   0.326 +0.070/-0.079                      
                         Using statistical and analytical arguments, Barclay et al. (2015)               
                         conclude that the five transiting planets associated with this pair             
                         orbit the primary star. The two outer planets (Ae and Af) have radii            
                         of 1.53 +/- 0.26 and 1.80 +/- 0.31 Rearth, respectively, and receive            
                         incident stellar fluxes of 1.40 +/- 0.23 and 0.62 +/- 0.10 times that           
                         received from the Sun by the Earth; this level of irradiation places            
                         both planets within or close to the circumstellar habitable zone of             
                         their parent star.                                                      Bcy2015 
19062+3026   STF2454     A premature orbit has been computed for AB. Component A reported                
                         double by Dommanget, but observation unconfirmed by observers with              
                         larger instruments. However, A is a SB2, P = 27.25d. From the visual            
                         separations of AB, Baize suspects a third body with P = 35 yr.                  
                         A component (suggested as possibly double by Dommanget) perfectly               
                         round on these 3 nights.                                                Baz1954a
                         Only elements P and T from the orbit of Baize (1976) have been          Baz1976 
                         amended by Starikova (1982).                                            Sta1982b
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
19062-0453   EHR  16     Primary is lam Aql. Companion appears to be a background star.          Ehr2010 
             JNN  10     The usual capital letter component designations (e.g., AB, AC, etc.)            
                         are insufficient to accommodate the very large number of companions             
                         discovered by Janson et al. (2011), so upper/lower case combinations    Jnn2011b
                         (A,Ca; A,Cb; etc.) were utilized. Since none of the JNN 10 companions           
                         appear to be physical, the lower case letters here are not meant to             
                         indicate any sort of hierarchical structure within this system.                 
19064+1355   BPM 963     [PM2000] 1716011 + [PM2000] 1716217.                                    Gvr2010 
19064+1153   BRT1315     J 3326.                                                                         
19064+0814   BLL  36     A is the Mira-type variable R Aql.                                              
19064+0709   STF2449     H 3 109.                                                                MEv2010 
19064-1154   RST4028     HIP 93827. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
19064-3704   HJ 5084     gam Cra.                                                                        
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.38 +/- 0.65, 2.38, and 2.19 Msun, respectively.             Mlk2012 
                         Magnitudes changed to Hipparcos V magnitude on recommendation of Ross   Fab2000a
                         Gould.                                                                  Glr2022 
19065+1555   BPM 964     [PM2000] 1716453 + [PM2000] 1715741.                                    Gvr2010 
19066-0121   STF2447     Spectrum of B: A0VpSrCrSi.                                                      
                         AB: H 4 127.                                                            MEv2010 
19067+1727   BPM 965     [PM2000] 1718118 + [PM2000] 1718187.                                    Gvr2010 
19067+1654   BPM 966     [PM2000] 1718155 + [PM2000] 1718163.                                    Gvr2010 
19068+6106   LDS2758     LDS5243.                                                                        
19069+4137   COU2197     Measures scattered and impossible to interpret.                                 
19069+2210   STF2455     Mt. Wilson spectral types F1s and B5.                                           
                         Relative motion is nearly rectilinear.                                  Fat1941 
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
19069+1638   BPM 967     [PM2000] 1719528 + [PM2000] 1719355.                                    Gvr2010 
19069+0847   HJ 2854     FOX 237 is 4s faster and 1' north of HJ 2854.                                   
             FOX 237     CD: FOX 237 is 4s faster and 1' north of HJ 2854.                               
19069-2740   tau Sgr     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
19070+1104   HEI 568     18 Aql. This is the eclipsing and spectroscopic binary Y Aql,                   
                         P = 1.30d. Hence a triple system.                                               
19072+4919   DAE  12     TrES-2 = KOI-1. Daemgen et al. (2009) estimate spectral types G0 and            
                         K4.5-K6, masses 1.05 and 0.67 Msun, and orbital period about 3900y.     Dae2009 
                         Bergfors et al. (2013) estimate spectral types G0V and K0-M0V.          Brg2013 
19072+2053   LDS1017     Ross 730,1.                                                                     
19073+3606   STA   3     iot Lyr = 18 Lyr                                                                
19073+1742   BPM 968     [PM2000] 1722355 + [PM2000] 1722300.                                    Gvr2010 
19074+5905   KPP3335     Aka TOI 1450.                                                                   
19074+3230   STF2461     17 Lyr. Mt. Wilson spectral type A is A9n.                                      
                         A is a spectroscopic binary.                                                    
                         AC: Proper motion of C +1219,+1114. Mt. Wilson spectral type is M3.             
                         Proper motion A : +124+030, E : -004-006, G : -003+007, H : -017-013.           
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             KUI  90     Ca: Combined solution from astrometry, spectroscopy, and parallax by            
                         Segransan et al. (2000). Solution yields mass and orbital parallax      Sgr2000 
                         determination.                                                                  
             STF2461     AB: H 2  68.                                                            MEv2010 
                         AC, CE: Rectilinear solutions by Friedman et al. (2012).                USN2012a
19074+1616   BPM 970     [PM2000] 1722846 + [PM2000] 1722676.                                    Gvr2010 
19074+1351   BPM 969     [PM2000] 1722601 + [PM2000] 1723017.                                    Gvr2010 
19075-1456   J  1646     J 2165.                                                                         
19075-2407   B   426     J  1600.                                                                J__1962a
19075-3622   B   963     C is CPD-36@8723.                                                               
19076+1648   BPM 971     [PM2000] 1724040 + [PM2000] 1723777.                                    Gvr2010 
19077+1538   BPM 972     [PM2000] 1724465 + [PM2000] 1724668.                                    Gvr2010 
19077+1447   BPM 973     [PM2000] 1724637 + [PM2000] 1725353.                                    Gvr2010 
19077-5515   RST1020     Not in Michigan Vol. XI.                                                        
19078+3856   STF2469     A is a spectroscopic binary and Algol-type eclipsing binary, period             
                         1.5403d.                                                                Zas2010 
19079+4652   A   704     KOI  13AB = KIC 9941662.                                                Hor2011c
19079+3043   HLM  16     Originally in WDS as 19079+3039, the Holmes AB pair was determined to           
                         be the same as 19079+3043J  2945AB.                                             
                         19079+3039HLM  16AC renamed 19079+3043HLM  16AG, aka ABH 110AG.                 
                         AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
19080+1745   BPMA 79     [PM2000] 1727055 + [PM2000] 1725133.                                    Gvr2010 
19080+1651   ISO   9     Aa,Ab is a spectroscopic binary, P = 22d. B is +16@3751.                        
19080+1645   BPM 974     [PM2000] 1726469 + [PM2000] 1726319.                                    Gvr2010 
19080+1337   BPM 975     [PM2000] 1726786 + [PM2000] 1727065.                                    Gvr2010 
19081+2142   CHR  83     Discovered in a reanalysis of data for Bagnuolo et al. (1992), this     Bgn1992 
                         measure predates our "discovery" observation by more than one year.     Hrt1992b
19081+1630   BPM 977     [PM2000] 1727548 + [PM2000] 1727293.                                    Gvr2010 
19081+1259   BPM 976     [PM2000] 1727426 + [PM2000] 1727256.                                    Gvr2010 
19081-2650   S   711     B is CD-27@13592.                                                               
19082+1702   BPMA 80     [PM2000] 1728088 + [PM2000] 1727867.                                    Gvr2010 
19082+0118   EVS  39     Primary is the Cepheid TT Aql.                                          Evs2016a
19082-1409   BRT 596     A likely plate flaw.                                                    Grv2021b
19083+5520   D    19     AB: Elongated 1863-1870                                                 D__1906A
19083+2522   HD178593    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
                         Spectroscopic solution to these astrometric pairs given by Griffin      Grf2013a
                         (2013). Periods match "tolerably well," other common elements less so.          
19083-0726   EVS  40     Primary is the Cepheid V496 Aql.                                        Evs2016a
19083-3121   PRO 221     A is the Algol-type system V526 Sgr.                                            
19085+0218   J  1281     Pair is +15s, -2' from BD+02 3791. At -29s, -3' from J 1281 is a faint          
                         pair: 1954.580, 4.1deg, 4.39", mags 12.2, 12.5.                         Cou1955a
19086+3755   STF2473     CD: DEA 107.                                                                    
19087+5630   TDS 970     Aka MLR 577.                                                            Dam2015b
19087+1527   BPM 978     [PM2000] 1731194 + [PM2000] 1731688.                                    Gvr2010 
19087+1244   BPM 979     [PM2000] 1731528 + [PM2000] 1731534.                                    Gvr2010 
19087-0708   DAM  53     B is IO Aql.                                                            Plt1934 
             PLT   5     C is IP Aql.                                                            Plt1934 
19088+3446   STF2470     B is BD+34 3436. A is a spectroscopic binary.                                   
19088+1433   BPM 980     [PM2000] 1731709 + [PM2000] 1731154.                                    Gvr2010 
19088+1304   OL   91     Not found by Heintz at IDS position.                                    Hei1990b
19089+3404   COU1462     More observations needed to define orbit.                                       
                         Elements determined by Mante (1999) were also published by the same     Mnt1999b
                         author in Obs. Trav. SAF 52, 44, 2000.                                          
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.51 +/- 0.20, 1.34, and 0.58 Msun, respectively.             Mlk2012 
19090+0604   LSC 129     19 Aql.                                                                         
19091+4502   ARG  83     AC pair originally listed as BC, but all measures were from A to AC.            
19091+3436   STF2474     B is BD+34 3438.                                                                
                         AB: NLTT 47474/47473                                                    Chm2004 
                         AB: B is exoplanet host, P=71.5d.                                       Tok2014d
             CHR  84     Aa,Ab: 1985.5232: This autocorrelogram was remeasured; the new results          
                         are listed here.                                                                
                         The paper by Tokovinin et al. (2000) also includes a combined           Tok2000a
                         spectroscopic/astrometric solution for orbital elements and masses.             
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 5.43 +/- 2.10, 2.39, and 1.02 Msun, respectively.  Mlk2012 
                         Aa,Ab: SB2, P=3.540y.                                                   Tok2014d
                         Combined solution by Farrington et al. (2014) yields masses 0.802 +/-           
                         0.055 and 0.622 +/- 0.053 Msun, as well as an orbital parallax 28.26            
                         +/- 1.70 mas.                                                           CIA2014a
19091+1325   BPM 981     [PM2000] 1733900 + [PM2000] 1733074.                                    Gvr2010 
19092+4649   DEA 477     JKA  28. KIC 9942242/9942231.                                                   
19092+1301   BPM 982     [PM2000] 1734282 + [PM2000] 1734644.                                    Gvr2010 
19092+0325   STF2462     An incorrect DM designation in the BDS resulted in an imprecise WDS             
                         designation and later "rediscovery" of this system by Soulie (2006).    Sle2006b
                         The 19107+0326 SLE 932 pairs have been merged with the Struve system.   StF1837 
                         The A and B components were switched at some point post-IDS; all                
                         components have been corrected back to their original identifications.          
19093+3912   FMR 144     AB: JKA  29. KIC 4043389/4142913.                                               
19094+1550   BPM 985     [PM2000] 1735847 + [PM2000] 1735578.                                    Gvr2010 
19094+1336   BPM 986     [PM2000] 1735941 + [PM2000] 1735983.                                    Gvr2010 
19094+1305   BPM 984     [PM2000] 1735693 + [PM2000] 1736310.                                    Gvr2010 
19094+1300   BPM 983     [PM2000] 1735609 + [PM2000] 1736033.                                    Gvr2010 
19094-4939   HJ 5088     HJ 5088a.                                                                       
19095+3839   KOI 118     Adams et al. (2012) theta values corrected to 360-theta                 Adm2012 
                         (reported by Dressing et al. (2014).                                    Dre2014 
19095+1925   HO  443     Also known as TDS 969.                                                          
19095+1552   BPM 988     [PM2000] 1736455 + [PM2000] 1736408.                                    Gvr2010 
19095+1511   J   480     BD+14 3806 (the A component) is at 251 deg, 62"                         Hei1983a
                         BC: Additional notes may be found in Jonckheere (1949).                 J__1949b
19095+1403   BPMA 81     [PM2000] 1736413 + [PM2000] 1734918.                                    Gvr2010 
19095+1341   BPM 987     [PM2000] 1736420 + [PM2000] 1735550.                                    Gvr2010 
19095-4934   HJ 9005     Previously known as HJ 5088d.                                                   
19095-4937   HJ 9006     Previously known as HJ 5088b.                                                   
19096+1321   BPM 989     [PM2000] 1736788 + [PM2000] 1736128.                                    Gvr2010 
19096-4940   HJ 9007     Previously known as HJ 5088c.                                                   
19098+3849   ES 2035     The pair MLL 7 is identical                                             Hei1980a
19098+1315   BPM 990     [PM2000] 1738444 + [PM2000] 1738331.                                    Gvr2010 
19098-1948   B   427     A premature orbit has been computed. Voronov orbit rejected from        Vor1934 
                         Fourth Orbit Catalog ("probably not double")                            Wor1983 
                         Additional notes may be found in Wilson (1951).                         WRH1951 
19098-2101   FIN 311     pi Sgr = 41 Sgr = Albaldah                                                      
19099+1610   BPM 991     [PM2000] 1738659 + [PM2000] 1737891.                                    Gvr2010 
19099+1511   BPM 992     [PM2000] 1739136 + [PM2000] 1738753.                                    Gvr2010 
19099+1323   BPMA 82     [PM2000] 1738693 + [PM2000] 1738578.                                    Gvr2010 
19099-6556   DON 948     CD-66@2279.                                                                     
19099-6825   SHY 314     HIP  94150 + HIP  94154.                                                        
19100+1237   BPM 993     [PM2000] 1739198 + [PM2000] 1739344.                                    Gvr2010 
19100+1232   KRV  26     Classical Cepheid V0916 Cyg.                                                    
19101+1755   BPM 994     [PM2000] 1739811 + [PM2000] 1739029.                                    Gvr2010 
19101-2907   I  9005     Previously known as I  1136 1/2.                                                
19102+4657   KOI 959     Distance is 35.662 +/- 0.053 pc. Ma (Mb) = 0.24 (0.22) +/- 0.1 \msun.   Hor2024 
19102+0841   STF2468     HJL 263.                                                                HJL1986 
19104+4210   DEA 364     AC: JKA  31. KIC 6678383/6678367.                                               
19105+4612   DEA 398     JKA  32. KIC 9579208/9579191.                                                   
19105+1556   BPM 995     [PM2000] 1742668 + [PM2000] 1742889.                                    Gvr2010 
19105-3000   UC 3830     CPM candidate confirmed physical by photometry (2MASS and V mags).      Tok2013c
19106+5429   A  1391     Prieur et al. (2014) derive a dynamical parallax of 6.2 mas and a               
                         total mass of 4.1 +/- 2.6 Msun (based on the revised Hipparcos          VlF2007 
                         parallax of van Leeuwen 2007).                                          Pru2014 
19106-4134   DEA   3     Published proper motion indicates all three are CPM, however, the       Dea2005 
                         values from UCAC4 presented here would indicate only BC is.             UC_2013a
19107+6646   TDS 975     Aka TOI 1654.                                                                   
19107+2114   BRT2452     J 3214.                                                                         
19107+1736   BPM 996     [PM2000] 1743664 + [PM2000] 1743756.                                    Gvr2010 
19108+4720   KOI  98     Kepler-14b is a hot Jupiter transiting one component of this close              
                         binary system.  The planet has an orbital period P = 6.7901230 +/-              
                         0.0000043d, a mass M = 8.40 +0.35/-0.34 Mjup, and a radius R = 1.136            
                         +0.073/-0.054 Rjup, yielding a density of 7.1 +/- 1.1 g/cc. It is one           
                         of the most massive transiting exoplanets yet discovered.               Lat2011 
19108+1318   BPM 997     [PM2000] 1744066 + [PM2000] 1743667.                                    Gvr2010 
19109+4414   DEA 313     JKA  33. KIC 8289464/8289460.                                                   
19109+3018   JNN 121     The AstraLux images reveal 3 components in the 2MASS J19105480+3017476          
                         system. Due to their very compact configuration, the triple system is           
                         very likely physically bound. Only one epoch of imaging exists so far.  Jnn2012 
19110-0726   A    95     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 6.01 +/- 4.00, 4.44, and 1.10 Msun, respectively.             Mlk2012 
19111+3847   STF2481     Mt. Wilson spectral type of A is G4.                                            
                         A,BC triple solution.                                                   Sod1999 
                         H 2  68                                                                 Bu_1906 
             SE    2     Mt. Wilson spectral type of BC is K0.                                           
                         SE 2 is the np component of STF 2481 (van den Bos).                     B__1925a
                         The pair BC is 4.5" Nf star A (mag. 8.4, G5) and is in slow             B__1960b
                         retrograde motion about it. The combined light of B and C is                    
                         slightly brighter than that of A; thus the quadrant of A,BC                     
                         (= STF 2481) is sometimes confused.                                             
                         BC: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.04 +/- 0.45, 2.02, and 0.95 Msun, respectively.  Mlk2012 
             TAR   4     DE: 3' south of ADS 12145. Heintz identifies this with HLM  17          Hei1990b
                         (aka ADS 12149).                                                                
19113+1317   BPM 998     [PM2000] 1746728 + [PM2000] 1746950.                                    Gvr2010 
19116-5642   HRG 130     Spectrum: G8/K0III+A/F.                                                         
19118+2615   STF2480     STF2495.                                                                        
19118-5319   FIN  68     Rapid direct motion.                                                            
19120+5057   KOI 153     Adams et al. (2012) theta values corrected to 360-theta                 Adm2012 
                         (reported by Dressing et al. (2014).                                    Dre2014 
19121+4951   STF2486     Mt. Wilson spectral type is G3.                                                 
19121+4619   RAO 514     FL Lyr.                                                                         
19121+0254   AST   1     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
                         Papers by Franz et al. (1998) and Benedict et al. (2001) both include   AST1998 
                         orbital elements and detailed discussions of component masses, etc.     AST2001 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 0.57 +/- 0.31, 0.51, and 0.35 Msun, respectively.             Mlk2012 
19121+0237   BU 1204     Slightly variable. Alternate spectrum: B9eShell.                                
19121+0055   SCJ  19     B is BD+00@4131.                                                                
19124-3304   OL   22     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.03 +/- 1.68, 2.44, and 1.07 Msun, respectively.             Mlk2012 
19124-5148   DUN 225     Spectrum of B: F6IV. B is CPD-52@11382                                          
                         Identified as optical and linear solution also published.               LRR2022c
19125+0306   J  2168     BAL 1978.                                                                       
19125+2422   RAS  28     Includes the alpha2 CVn type variable star QW Vul.  Companion likely            
                         late-G.                                                                 Ras2014 
19125-0525   HIP  94370  Unresolved. Delta-mu and long-period SB, according to CfA.              Tok2013b
19126+6740   BUP 186     del Dra = 57 Dra = Altais                                                       
                         Smyth's quoted separation is difference in RA only.                     Smy1844 
19126+5117   KOI2331     The system hosts a single 1.4 Rearth planet candidate with a 2.8 day    KOI2013a
                         period (Batalha et al. 2013).                                           Dre2014 
19126+1651   BU  139     AB: This object was misidentified as HD 179558 by McAlister et al.      McA1983 
                         V338 Sge, Algol-type eclipsing binary, P = 3.49784 d.                   Zas2011 
             STTA177     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             BU  139     AD/AE: Confusion in component designation, with the "D" component of            
                         the 29" AD pair not the same star as the "D" component of the 137" CD           
                         pair. The ADS identifies the two pairs as "Aa" and "CD", respectively.  A__1932a
                         The IDS changes "Aa" to "AP" (due to the lack of lower-case letters     IDS1963A
                         available on the IDS's computer punch cards). However, some measures            
                         of the pair are also listed erroneously as an additional pair in this           
                         system, identified as "AD". The two pairs were later recognized as              
                         being the same, and were merged under the "AD" designation in the WDS.          
                         The designation for 29" pair has been changed to "AE". Our thanks to            
                         Steve Smith (2014, private comm.) for pointing out the discrepancy.             
19126-2002   B   429     Measures uncertain, too close.                                                  
19127+2435   A   264     Despite having an orbit, an optical pair based on parallax.             Mlk2022 
19127+2435   MAD   7     AC: Despite having an orbit, optical pair, based on study of relative   Izm2019 
                         motion of the components using method of apparent motion parameters.    Kiy2008 
                         AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
19127+0643   OSO 107     G022-019. AD, AE, AH, and AI are not common proper motion pairs, based          
                         on comparison with POSS2 red plates.                                    Oso2004 
19128+2957   BRT  37     19129+2957J  3300                                                               
19129+1528   J  2951     J 3274 is probably identical                                            Hei1983a
19129+1433   BPM 999     [PM2000] 1753880 + [PM2000] 1753476.                                    Gvr2010 
19130+4323   KOI1463     Primary is an eclipsing binary of Algol-type (detached).                        
19130-0333   SCJ  20     B is BD-03@4511.                                                                
19130-3351   SCT   1     Aka ARY  77.                                                                    
19131-7836   HJ 5073     B is CPD-78@1214.                                                               
19132+6312   AG  228     B is BD+62@1696.                                                                
19132+3908   HLM  19     ALI 884.                                                                        
19133+0153   BAL1511     J 2169.                                                                         
19133-0036   OSO 108     G022-020. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates                                                        Oso2004 
19133-0223   HJ  265     Herschel notes star is quadruple. A third companion is seen in the              
                         Carte du Ciel San Fernando results.                                     Gau1926a
19134-0246   J  1378     BAL 251.                                                                        
19134-3215   PRO 223     A likely plate flaw.                                                    Grv2021b
19135+4321   KOI2722     This system contains four confirmed planets with radii of 1.4, 1.4,             
                         1.1, and 1.3 Rearth and one candidate planet with a radius of 1.3       KOI2014a
                         Rearth (Burke et al. 2014).                                             Dre2014 
19135+3902   SHJ 289     B is BD+38@3489.                                                                
                         H 5  42.                                                                MEv2010 
19135-1632   HJ 2856     Also known as J 1667.                                                           
19136+2012   HU  335     Very red; variable? Magnitude noted as 7.3 by Hussey, 8.0 by van                
                         Biesbroeck, 8.6 by van den Bos, 7.7 in 1953, 7.4 in 1954, 7.3 in 1966,          
                         and 8.3 in 1969. Listed as 7.95 in HD catalog.                          Baz1972 
19136-0824   J   535     J 2690.                                                                         
19137+2905   BRT 190     J 2956.                                                                         
19137+0218   HJ  879     21 Aql. A is the Alpha CVn-type variable V1288 Aql. Spectrum of B: F8V          
19138+4548   KOI2298     This system contains a 1 Rearth planet candidate with a 16.7 day orbit          
                         (Batalha et al. 2013). NEXSci also reports a 0.8 Rearth false positive  KOI2013a
                         with a 31.8 day period. We detected a companion 1.3 Ks mags fainter             
                         than KOI2298 at a distance of 1".47. The companion is expected to have          
                         Kp = 15.2 (dKp = 1.4), indicating that contamination may lead to a              
                         significant underestimate of the planet radius.  In the simple                  
                         approximation that all light from the companion star is captured in             
                         the Kepler aperture, the radius estimate for the planet should be               
                         increased by 13% to account for the dilution if indeed the planet               
                         orbits the target star and the companion has Kp = 14.9. However, the            
                         companion may be the same object identified ~1" away from KOI2298 in a          
                         HIRES guider image. The estimated brightness contrast from the HIRES            
                         image is three mags, which implies companion is red enough that the             
                         dilution correction might be only a 3% change to the planet radius      Dre2014 
19138+3909   STF2487     eta Lyr = 20 Lyr = Aladfar. B is BD+38@3491. A is a spectroscopic               
                         binary.                                                                         
                         AB: H 4   2.                                                            MEv2010 
                         AB: SEI 581.                                                            Nsn2017b
19138+0632   BRT2180     J 2955.                                                                         
19139+5742   TOK 328     NPOI Limb-darkened diameter 1.630 +/- 0.028 mas, Sp = K2III,            NOI2018 
                         R = 8.87 +/- 0.17 \rsun, Teff = 4868 +/-124 K, L = 39.9 +/- 3.9 \lsun,          
                         M = 1.65 +/- 0.25 \msun, Age = 1.97 +/- 0.94 Gyr.                               
19139+2252   HJ 2859     AC: C component is primary of 19139+2250 HJ 2858.                               
19139+2250   HJ 2858     Primary is C component of 19139+2252 HJ 2859AC.                                 
19139-4722   HJ 5092     B is CD-47@12795.                                                               
19140+3252   SEI 580     Secondary not seen in ALADIN image - possibly plate flaw                        
19141+6707   HDS2722     Mean motion indicates P ~ 80 yr, rho decreasing.                        Msn1999b
19141+4057   KOI 283     Adams et al. (2012) theta values corrected to 360-theta                 Adm2012 
                         (reported by Dressing et al. (2014).                                    Dre2014 
19142+2308   STF2485     POU 3754.                                                                       
19142+1445   BPM1001     [PM2000] 1758831 + [PM2000] 1758495.                                    Gvr2010 
19142+1418   BPM1000     [PM2000] 1758823 + [PM2000] 1758888.                                    Gvr2010 
19143+6754   STF2508     B is BD+67@1133.                                                                
19143+1904   STF2484     A premature orbit has been computed.                                            
                         The semi-major axis value of 2".041 in Hopmann (1973) is apparently a   Hop1973b
                         typo. The value was changed to 2".841 in the orbit catalog to better            
                         match the observations.                                                         
19143-0843   GC 26500    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
19144+2026   BRT2453     Also known as J 2957.                                                           
19145+3434   STT 367     A,BC  HJL 264.                                                          HJL1986 
             HO  648     AD: Rectilinear solution by Hartkopf & Mason (2013).                    Hrt2013b
19146+6733   MLB 356     NSVS 1209822, W UMa-type eclipsing binary, period 0.43913 d.            Zas2018 
19146+3252   SEI 582     Secondary not seen in ALADIN image - possibly plate flaw                        
19147+1918   LDS1020     Ross 733-4.                                                                     
                         NLTT 47575/47576                                                        Chm2004 
             BWL  49     AC, AL, and AX: Colors and/or astrometry are inconsistent with a late-          
                         type common proper motion companion based on visual inspection of the           
                         field from 2MASS, SDSS, DSS1, and/or DSS2. Primary is GJ 9652.          Bwl2015 
19148+4950   UC 3864     JKA  39. KIC 11707001/11707004.                                                 
19148+0100   J  1036     Aka TDT1315.                                                                    
19149+0209   BAL1514     Ross 651.                                                                       
19150+6354   MOT   1     B is BD+63@1502.                                                                
19150-1559   HWE  46     Primary is eclipsing binary of Beta Lyr -type, period 0.875 d.          Zas2012 
19153+1505   STTA178     B is BD+14@3845.                                                                
19155+2721   BRT3339     Originally published as BRT 191.                                        Brt1928 
19155+1713   BPM1003     [PM2000] 1763918 + [PM2000] 1763786.                                    Gvr2010 
19155+1510   BPM1002     [PM2000] 1763568 + [PM2000] 1763253.                                    Gvr2010 
19155-2515   B   430     psi Sgr = 42 Sgr. B is SB2, P = 10.78 d. Alternative spectra:                   
                         F2:+F7III.                                                                      
                         1982.5056: This autocorrelogram was remeasured; the new results are             
                         listed here.                                                                    
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.47 +/- 0.71, 3.83, and 4.22 Msun, respectively.             Mlk2012 
19156+3748   BRT2224     19157+3748ALI 618                                                               
19156-2411   HD 179949   Chauvin et al. (2006) note finding at least one faint companion         Cvn2006 
                         candidate within separation/magnitude range listed. However,                    
                         further observations are required for verification                              
19158-4107   HIP  94668  Variable RB and large acceleration - close binary?                      Tok2013b
19159+2727   STT 371     A spectroscopic binary.                                                         
19159+2018   J  2959     Jonckheere gives BD as +20@4098, but position and magnitude agree with  J__1945 
                         BD+20@4090.                                                                     
19160+1508   BPM1004     [PM2000] 1765754 + [PM2000] 1765647.                                    Gvr2010 
19160-0238   J  1380     BAL 252.                                                                        
19161-2510   BRT3084AB   Aka J  1841.                                                                    
19162+6333   MOT   2     B is BD+63@1506.                                                                
19162+2123   HJ 2862     1 Vul. A is a spectroscopic binary, P = 249.4d, and possibly variable.          
19162+1612   BPM1005     [PM2000] 1766442 + [PM2000] 1766083.                                    Gvr2010 
19163+4018   COU2280     TDT1335.                                                                        
19164+3808   SHJ 292     the Lyr = 21 Lyr. B is BD+37@3399.                                              
                         AB: H 6  56.                                                            MEv2010 
                         NPOI Limb-darkened diameter    2.357 +/- 0.045 mas,                             
                         R =   60.31 (+1.92-1.99 )  \rsun,  Teff = 4523 +/-  44 K,                       
                         L = 1374.  +/-  73.  \lsun.                                             NOI2023 
19164+1612   BPM1006     [PM2000] 1767230 + [PM2000] 1766880.                                    Gvr2010 
19164-2521   HJ 5101     B is CD-25@13879.                                                               
19165+3910   A   158     SEI 587.                                                                Nsn2017b
19166+1503   BPM1007     [PM2000] 1768050 + [PM2000] 1768125.                                    Gvr2010 
19167+3308   HO  102     STF2493.                                                                        
19167-4553   RST4036     Strange (but useable) reference point for the Transit Data due to               
                         reversed signs for proper motions in the Hipparcos Input Catalog.       Sod1999 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.24 +/- 0.20, 1.14, and 0.60 Msun, respectively.             Mlk2012 
19168+6742   STF2514     D is BD+67@1142. Delta(RA) +104"; delta(DEC) -162".                             
19168+0141   BAL1515     J 2257.                                                                         
19169+1359   BPM1008     [PM2000] 1769464 + [PM2000] 1769180.                                    Gvr2010 
19169+0510   LDS6334     Proper motion of A -603 -1339.                                                  
                         CHARA Array Limb-darkened diameter of A : 0.836 +/- 0.051 mas           CIA2006 
                         R = 0.526 +/- 0.032 \rsun, Teff = 3368 +/- 137 K.                               
19169-1058   BU  140     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
19170+3332   ES  351     ES 2292.                                                                        
19171+0920   STT 370     B is the Algol-type system V342 Aql.                                            
                         A 180.5-d spectroscopic orbit has been found for the A component.       Grf2012 
19172+1403   BPM1009     AB: [PM2000] 1770724 + [PM2000] 1770299.                                Gvr2010 
             BPM1010     BC: [PM2000] 1770299 + [PM2000] 1769858.                                Gvr2010 
19172+0143   B  2875     Nova Aquilae 1936. Undoubtedly of the same character as the other               
                         measures of such objects, and not a true double star.                           
19172-6640   GLE   3     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.89 +/- 1.65, 4.28, and 3.40 Msun, respectively.             Mlk2012 
19173+2702   BRT3340     Originally published as BRT 192.                                        Brt1928 
19173-3331   VOU  14     SWR 262.                                                                        
19174+2416   GCB  37     Position in error and found single                                      Hei1980a
19174+1640   BPM1011     [PM2000] 1771245 + [PM2000] 1770821.                                    Gvr2010 
19174+1253   BPM1012     [PM2000] 1771545 + [PM2000] 1771276.                                    Gvr2010 
19177+2302   BU  248     2 Vul. A is the Beta CMa-type variable ES Vul.                                  
19177+1531   BPM1013     [PM2000] 1772762 + [PM2000] 1772823.                                    Gvr2010 
19177+0847   HJ 5509     Primary is eclipsing binary of W UMa-type, period 0.520681 day.         Zas2013 
19178+2411   GCB  73     Many measures of this pair erroneously assigned to GCB  37.                     
19178-5007   RST1031     CPD-50@11025.                                                                   
19179+2522   BUP 187     B is BD+25@3783.                                                                
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
19180+2012   COU 321     1986.394: Separation of this partially resolved pair was calculated             
                         under the assumption of zero or otherwise known magnitude difference.   Tok1985 
19180+1459   BPM1014     [PM2000] 1774045 + [PM2000] 1774336.                                    Gvr2010 
19181+1718   BPM1015     [PM2000] 1774148 + [PM2000] 1773980.                                    Gvr2010 
19181+0351   HEI 873     Aka BAL2507.                                                            Dam2016d
19181-1557   S   716     Appears to also be STN  46 (formerly at 19267-1557) with an RA error.           
19182+4928   DEA 408     JKA  45. KIC 11503111/11503101.                                                 
19182-1852   H 5  77     H V 77.                                                                         
19182-3823   TOK  33     Confirmed by 2MASS, with consistent position as further evidence of             
                         physical nature. Primary is 2.5d SB. Estimated period of visual pair            
                         6600y.                                                                  Tok2006 
19183+1450   BPM1016     [PM2000] 1774996 + [PM2000] 1774899.                                    Gvr2010 
19185+0105   STF2492     23 Aql.                                                                         
                         AB: H 1  14.                                                            MEv2010 
19187+4042   KOI1677     KOI1677 hosts a 2.2 Rearth planet candidate with a 52.1 day orbit and           
                         a 0.8 Rearth candidate with a 8.5 day orbit (Batalha et al. 2013).      KOI2013a
                         Assuming that all of the flux from the target star and the companion            
                         is captured in the Kepler aperture and that the planet orbits the               
                         target star, the planet radius estimate should be increased by roughly          
                         2% to account for the contamination from the nearby star.               Dre2014 
19188+1937   AG  432     U Sge.                                                                          
19188+1736   HU  337     Not seen for certain after 1960, until 1987.                                    
19188+1629   RAO  67     A is SB2, P=5.480d.                                                     Tok2014d
19188+0020   STFA 40     24 Aql. Alternate spectral type of A:                                           
                         K0IIIa:Ba0.3CH1.                                                                
19189+4952   ES 1095     AB: JKA  47. KIC 11709006/11709022.                                             
19189+1507   BPM1017     [PM2000] 1777397 + [PM2000] 1777772.                                    Gvr2010 
19189+1237   BPM1018     [PM2000] 1777497 + [PM2000] 1777524.                                    Gvr2010 
19190+4138   KOI3158     A,BC: Kepler-444 is a metal-poor triple system that hosts five                  
                         sub-Earth-sized planets. The secondary is an SB2 consisting of two M            
                         dwarfs. Dupuy et al. (2016) determine an eccentric orbit of A,BC and            
                         derive mass ratios (M_B + M_C)/M_A = 0.71 and M_C/M_B = 0.86 +/- 0.03.          
                         Limits are determined for the BC orbit, with a <10mas. System mass is           
                         1.30 +/- 0.06 Msun.                                                     Dup2016b
19190+3916   STF2502     Primary is an eccentric Algol-type eclipsing binary, period 8.64731d.   Zas2010 
                         Also known as KOI3156.                                                          
19190-3317   TOK 624     AC: C component is the primary of 19209-3303 HJ 5107.                           
19192+4333   DEA 302     JKA  48. KIC 7816387/7816381.                                                   
19192+4321   DEA 476     JKA  49. KIC 7676737/7676799.                                                   
19192+2847   DOO  73     Not found by Van Biesbroeck and van den Bos. Object may be 3' south.            
19192+2844   VBS  28     This may be same as DOO 73, ADS 12308. No other pair nearby.                    
19192+1519   BPM1019     [PM2000] 1778568 + [PM2000] 1778992.                                    Gvr2010 
19192+0401   HJ 2864     STF3124.                                                                        
19194+1514   BPM1020     [PM2000] 1779043 + [PM2000] 1779116.                                    Gvr2010 
19196+5125   UC 3884     JKA  50. KIC 12507868/12507882.                                                 
19196+3720   CIA   2     Combined solution yield Ma = 0.941 +/- 0.076 \msun,                     CIA2018d
                         Mb = 0.926 +/- 0.075 & orbital parallax of 41.1 +/- 0.8 mas.                    
19197+1222   S   717     28 Aql. STTA179 = H 5  34.                                                      
                         A is the Delta Scuti-type variable V1208 Aql.                                   
19199+3532   STF2505     Spectrum composite; A0+K.                                                       
19200+2756   EVS  41     Primary is the Cepheid V473 Lyr.                                        Evs2016a
19200+1510   BPM1021     [PM2000] 1781304 + [PM2000] 1781405.                                    Gvr2010 
19200+1439   BPM1022     [PM2000] 1781388 + [PM2000] 1781600.                                    Gvr2010 
19200+0535   STF2497     B is BD+05@4114.                                                                
19201+3752   ES 2489     A is the Mira-type variable U Lyr.                                              
19201+2639   STTA181     B is BD+26@3528.                                                                
                         A: Ren & Fu (2013) calculated an astrometric orbit, combining                   
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Griffin (1982). They derived component masses 1.45 and 1.19 Msun and    Grf1982a
                         an estimated semimajor axis of 12.85 mas.                               Ren2013 
19202+3441   POP 204     AKA WFC 220                                                                     
19202+0403   STF2498AB   A is a close spectrscopic binary (1137.2-d) as is B (90.508-d).         Grf2010c
                         Their respective gamma velocities are consistent with them being                
                         physical but of extreme orbital period.                                         
19203+0056   BAL1202     J  1382.                                                                Nsn2016 
19204-1034   HU   72     A is variable.                                                                  
19205+1519   BPM1023     [PM2000] 1782664 + [PM2000] 1782585.                                    Gvr2010 
19205-0525   ISO  10     Aa,Ab: 26 Aql. Aa,Ab is a spectroscopic binary, P = 266.5d.                     
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Franklin (1952).                                                        Frn1952 
                         The astrometric orbit is relative to the spectroscopic elements, not            
                         the speckle pair, which is not real.                                            
19206+3911   STF3131     SEI 590.                                                                Nsn2017b
19206-0645   HDS2735     AB + TOK 432AC: HIP 95068 is the neglected Hipparcos binary HDS 2735            
                         AB, a distant K-type giant. We did not resolve this 0".1 binary, which          
                         remains unconfirmed, but detected instead another faint star at 1".             
                         The stellar background is crowded, the PM is small, and the status of           
                         the new companion remains uncertain.                                    Tok2015c
19206-0740   LDS 678     A is a white dwarf. B is variable.                                              
                         AB: NLTT 47693/47691                                                    Chm2004 
                         AB: GJ 9653.                                                            Far2005b
19207+1425   STTA180     B is BD+14@3879.                                                                
19209-3303   HJ 5107     AB + TOK 433Aa,Ab: HIP 95106 and 95110 form the 13".7 pair HJ 5107 AB.  Tok2015c
                         The RV variability of A was suspected by the GCS, it is now resolved            
                         as a 0".27 binary with estimated period of ~35yr. The component B was           
                         also observed and found unresolved. It contains a spectroscopic pair,   Tok2018d
                         the whole system is quadruple.                                          Tok2015c
             TOK 433     Aa,Ab: Possible SB, no orbit.                                           Tok2014d
19209-5103   HJ 5104     B is CD-51@12042.                                                               
19212-1250   J  1672     Same as J  2693.                                                                
19213+5543   A  1395     Not seen since 1929.                                                            
19215+4231   JNN 122     The very close companion resolved by AstraLux is probably physically            
                         bound, but this has yet to be tested through proper motion analysis.    Jnn2012 
19215-0807   J  2265     J 2544 is identical.                                                    Hei1983a
19216+5223   BU 1129     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.41 +/- 2.05, 3.61, and 1.89 Msun, respectively.             Mlk2012 
19216+4017   KOI 123     AC: Adams et al. (2012) theta values corrected to 360-theta             Adm2012 
                         (reported by Dressing et al. (2014).                                    Dre2014 
19216-1914   H 6 120     H VI 120.                                                                       
19217+6956   ELD   1     Primary is NSV 11987 = DW Dra. The companion was seen during a visual           
                         check on the variable star by Elias & Locher; the relative astrometry   ElD1986 
                         and secondary magnitude are estimates (+/- 5deg, 0".5, 0.3mag).                 
19217+2534   ES  483     A is the Algol-type system Z Vul.                                               
19217+0912   AG  229     B is BD+08@4056.                                                                
19217-1557   NOI   7     ups Sgr.                                                                        
                         Massive interacting binary. Bonneau et al. (2011) orbit combines the            
                         spectroscopic elements of Koubsky et al. (2006 A&A 459, 849) with               
                         interferometric data by Netolicky et al. (2009 A&A 499, 827) and new            
                         CHARA array data.                                                       Bnu2011 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 10.60 +/- 7.39, 32.14, and 1.35 Msun, respectively.           Mlk2012 
19217-1715   HO  272     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: Nothing in the field appears to match Hough's measure.              Ho_1899a
                         AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
19218+7708   HDS2740     Rectilinear solutions by Cvetkovic (2015)                               Cve2015b
                         and Cvetkovic et al. (2016).                                            Cve2016b
19218+3959   DEA 404     JKA  54. KIC 4831350/4831378.                                                   
19218+1737   BPM1024     [PM2000] 1785926 + [PM2000] 1785678.                                    Gvr2010 
19220+2512   RAS  29     Silicon star, type B9. B component estimated as F0-F2, C component as           
                         type K.                                                                 Ras2014 
19221-0444   STF2501     B is BD-05@4946.                                                                
19221-2931   SHY 753     HIP  95203 + HIP  95164.                                                        
                         AB + TOK 423Aa,Ab: HIP 95203 is another acceleration binary with                
                         variable RV resolved here. The relatively large separation of 0".77             
                         corresponds to a period of ~180yr. The actual period can be as short            
                         as 60yr if the pair is seen now near its maximum separation (it would           
                         then have been closer at the time of the Hipparcos mission). Most               
                         likely, however, the faint visual companion found here and the                  
                         spectroscopic/acceleration pair make a triple system. There is another          
                         companion HIP 95164 at 435". The status of this wide pair (is it a              
                         real binary or just two members of a moving group?) is not clear, but           
                         the association of those stars leaves no doubt (common RV, PM, and              
                         parallax).                                                              Tok2015c
19222+4808   KOI1316     Primary is Kepler exoplanet host star.                                  Adm2013 
19223+6118   MLB 173     FOX 85.                                                                         
19224+1459   J   822     Position corrected by Couteau. See measures of 19240+1507J  2964.       Cou1959a
                         Heintz confirms that these are different pairs.                         Hei1985a
19225+1610   BPM1025     [PM2000] 1787557 + [PM2000] 1787322.                                    Gvr2010 
19226+3709   ALI 389     A likely plate flaw.                                                    Grv2021a
19226-4428   DUN 226     bet 1 Sgr = Arkab Prior. B is CD-44@13278.                                      
19228-3147   PRO 225     Secondary not seen; possibly plate flaw in Perth source catalog.        PrO1913 
19229-5425   LWR   3     eta Tel                                                                         
                         Probably a physical pair; spectral type M7-M8V, mass <50 Mjup,                  
                         age < 30Myr for companion                                               Lwr2000 
                         Based on known proper motion of A component and very small change in            
                         separation between components over two years, conclude are likely               
                         physical pair.                                                          Gue2001 
                         Member of the bet Pic moving group.                                     Zuc2001b
             TOK 331     AC : Also known as CAB   9.                                             Cab2011 
19230+3925   GIC 156     G208-019/G208-020.                                                              
19232+1151   BPM1026     [PM2000] 1789274 + [PM2000] 1789251.                                    Gvr2010 
19234+2034   RAO  68     A is SB1 and asrometric binary (Makarov & Kaplan 2005), P=18.4y.        Mkr2005 
                         High-PM, metal-poor star.                                               Tok2014d
19235+2234   TDT1416     Assumed to be the once lost L    28 = BDS 9264.                         Dam2016d
19235-3432   COO 235     SWR 263. CPM pair                                                       Skf2004 
19235-6924   SHY 755     AC: HIP  95315 + HIP  95718.                                                    
19236+3313   THA   1     Primary is Gl 758, a high-metallicity G9 dwarf atdistance of 15.5pc.            
                         The faint B component is found to share common proper motion. Mass of           
                         B is estimated to fall in range 10.3-34.3 Mjup, temperature 549-637K;           
                         spectral type T9. C component is considered candidate companion.        Tha2009 
                         Based on additional epoch astrometry, the C component appears to be a           
                         background star.                                                        Jnn2011 
                         AB: Nilsson et al. (2017) derive a spectral type for the secondary of           
                         T7.0 +/- 1. Teff = 741 +/- 25K; inferred mass is 40-50 Mjup.            Nln2017 
19238+3942   HJ 2870     AB: SEI 594.                                                            Nsn2017b
19238+3832   COU2201     Primary is an Algol-type eclipsing binary, orbital period 52.58 day.    Zas2011 
19239-2939   HJ 5110     SWR 264.                                                                        
19240+2437   DOO9001     Aka TDS 988.                                                                    
19240+1507   J  2964     J  3342.                                                                        
                         Pair seen by Jonckheere sometimes confused with J 822, found at -1.6m           
                         and -7'. Did not see third companion noted by Jonckheere, which was             
                         apparently a diffuse star -0.5m from BD+14 3902.                        Cou1961a
19240-4557   I   116     Spectral type of C may be K.                                                    
19241+1724   BPM1027     [PM2000] 1791664 + [PM2000] 1791770.                                    Gvr2010 
19243+2032   HDS2752     Mean motion indicates P ~ 80 yr, rho increasing.                        Msn1999b
19243+0305   HJ  885     J 2694. BAL 1983. J 1844.                                                       
19244+1656   STFA 41     2 Sge. A spectroscopic binary.                                                  
                         B is BD+16@3842. B is also a spectroscopic binary.                              
             HDS2753     Aa,Ab: Very weak detection in 1996.5425 (Hipparcos found dm geq 3.8)    Msn1999b
                         Fekel et al. (2013) derive a spectroscopic orbit for the primary, with          
                         P=7.392d and e=0.00613. Estimated masses are 2.08 and 1.67 Msun.        Fek2013a
19244-1400   LEO  44     J 1757. J 1674.                                                                 
19246+5014   CH Cyg      Speckle interferometry can clarify the geometry of this symbiotic               
                         star: adopting a 5750-day period, eccentricity = 0, and distance of             
                         100 pc, and assuming the total mass of the system is small                      
                         (Wallerstein, 1983 PASP, 95, 564), we obtain rho ~ 0".07. Joint                 
                         speckle interferometric observations with Bonneau and Foy on the 6-m            
                         telescope in October 1981 also failed to disclose the companion.        Bag1984a
19248+0231   J  2965     BAL 1986.                                                                       
19249+0150   H 6  47     H VI 47. B is BD+01@3987.                                                       
19250+1157   STT 588     31 Aql.                                                                         
                         AB and AC: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
19251-2919   HJ 5113     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
19253-2431   FIN 327     chi 1 Sgr = 47 Sgr. We apparently view the pair at nearly 90 deg                
                         inclination, and since delta m for the components is near zero there is         
                         considerable ambiguity between a high-eccentricity short-period orbit           
                         and a low-eccentricity long-period one.                                         
                         Orbital analysis included reanalysis of earlier CHARA speckle data in           
                         order to derive absolute quadrants and possibly resolve this period             
                         ambiguity.                                                              Hrt1993 
                         Alternate spectral classification: A3/5IV/V.                                    
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Finsen (1965).                                                          Fin1965b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.62 +/- 1.35, 4.51, and 1.00 Msun, respectively.             Mlk2012 
19254+2455   CHR  86     Aa,Ab: This system, first announced by McAlister and recalled in a      McA1984b
                         later McAlister paper after repeated attempts at confirmation, has      McA1993 
                         been restored. While perhaps still spurious, the subsequent                     
                         confirmation or suspected duplicity (by another technique) makes the            
                         discovery measurement somewhat more probable.                                   
             STT 589     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
19254-6718   MLO  85     Hipparcos suspected non-single.                                                 
19255+6820   LDS2436     LDS5244.                                                                        
19255+1948   HJ 2871     4 Vul.                                                                          
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
19255+0307   BNU   6     Aa,Ab: del Aql = 30 Aql. A is a spectroscopic binary, now resolved by           
                         speckle interferometry.                                                         
                         Hipparcos astrometric solution adopts some elements from the            HIP1997d
                         spectroscopic orbit of Kamper et al. (1989).                            Kpr1989 
                         The spectroscopic binary remains unresolved, BNU 6 is not real          Msn2023a
                         and the speckle measure from Bonneau & Foy 1980 is no good.             Bnu1980b
19256+0907   SOL   1     B is BD+08@4093.                                                                
19258-3006   I  1401     Spectrum: B9/9.5IV/V.                                                           
             WSI  91     Aa,Ab: The close WSI pair was initially given component designation             
                         Ba,Bb. However, Tokovinin et al. (2015) have determined that it was     Tok2015c
                         the A component that was split. Deisgnation has therefore been changed          
                         to Aa,Ab.                                                                       
19260+3555   BU 1286     AB: SEI 600.                                                            Nsn2017b
19260+1533   A  1647     Bidelman classifies A as composite: gK+A.                                       
19264+4928   YSC 134     Metal-poor SB2, spectroscopic orbit published by Tokovinin (1991).      Tok1991 
                         An astrometric orbit was deduced from Hipparcos data by Jancart et al.  Jnc2005 
                         (2005). The period derived for the visual orbit matches both the                
                         spectroscopic and astrometric solutions within the uncertainty, and             
                         other orbital parametrs are in reasonable agreement with the Tokovinin          
                         solution. The updated Hipparcos parallax (39.98 +/- 0.73 mas),                  
                         combined with the orbit, yields a mass sum of 2.0 +/- 0.3 Msun. The             
                         composite spectral type is K3V; a magnitude difference of 0.8 mags              
                         makes the component spectral types roughly K1V + K4V, which suggests            
                         a mass sum of 1.2-1.5 Msun, accounting for the lower metallicity.       Hor2012b
                         For the Horch et al. (2015) combined solution, spectroscopic elements           
                         are fixed to those of Halbwachs et al. (2012).  Assigned spectral       HJL2012 
                         types are K2V and K4.5V; derived masses 0.74 and 0.68 Msun.             Hor2015 
                         Orbital parallax is 42.01 +/- 1.08 mas. Mass of the primary is                  
                         0.695 +/- 0.066 \msun. Mass of the secondary is 0.621 +/- 0.058 \msun.  Doc2018h
19264+0149   H 6  48     H VI 48. B is BD+01@3996.                                                       
19265+1953   STF2521     AB: H N  85.                                                            MEv2010 
19265+0020   BU 1469     nu Aql = 32 Aql. B is BD+00@4204.                                               
19266+3934   SEI 602     J 1157.                                                                         
19266+2719   STF2525     AB: CfA: RV of A or B can be variable                                   Tok2014d
19266+2530   STF2524     AB: H N 100.                                                            MEv2010 
                         AB: Additional notes may be found in Fatou (1941).                      Fat1941 
19268+5009   STTA182     B is BD+49@3011.                                                                
                         AD: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
19268+2110   STF2523     AB: H 3  57.                                                            MEv2010 
             KRU   8     J 2968. Probable light and velocity variations.                                 
19268+1638   BPM1028     [PM2000] 1800161 + [PM2000] 1799927.                                    Gvr2010 
19269-5813   HJ 5108     CD-58@7433.                                                                     
19277+3632   STF2534     H 2  69.                                                                MEv2010 
19277+1229   BPM1029     [PM2000] 1803202 + [PM2000] 1803245.                                    Gvr2010 
19277-1821   TOK 367     First resolution; estimated period 9yr.                                 Tok2013b
19278-5420   HJ 5114     AE. Herschel notes "some doubt".                                                
19279+7316   PAL   1     Aka WFC 221.                                                                    
19282+1400   AG  381     100deg error in first published measure.                                        
19282-1209   SCJ  22     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.88 +/- 0.54, 1.89, and 0.91 Msun, respectively.             Mlk2012 
19284+0821   HD 183263   Chauvin et al. (2006) note finding at least one faint companion         Cvn2006 
                         candidate within separation/magnitude range listed. However,                    
                         further observations are required for verification                              
             GNS   2     Proper motion analysis suggests both companions are background stars.   Gns2012 
19285+4156   KOI3117     This system hosts a 1.5 Rearth planet candidate with a 6.1 day period   KOI2014a
                         (Burke et al. 2014).                                                    Dre2014 
19285-2600   HJ 5119     SWR 266.                                                                        
19286+3808   SEI 604     JKA  61. KIC 2992956/2992960.                                                   
19287+3437   LTT15689    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
                         Spectroscopic solution to these astrometric pairs given by Griffin      Grf2013a
                         (2013). Periods match "tolerably well," other common elements less so.          
19287+2440   STFA 42     8 Vul = alp Vul = Anser. B is BD+24@3761, spectrum K0III.                       
19288+4203   KOI2838     This system hosts a 0.7 Rearth planet candidate with a 4.8 day period.          
                         The Kepler data also revealed a 7.7 day false positive (Burke et al.    KOI2014a
                         2014). We detected a companion 4.04 Ks mags fainter than KOI2838 at a           
                         distance of 1".75. The estimated Kp mag of the companion is Kp = 18.5           
                         (dKp = 5.0) and the approximate dilution correction is a 0.5% increase          
                         to the radius of the planet candidate. KOI 2838 does not display a              
                         significant source offset during transits.                              Dre2014 
19288+2653   BRT3342     Originally published as BRT 194.                                        Brt1928 
19289+3515   POP  34     AB: Rectilinear solution by Cvetkovic et al. (2015).                    Cve2015 
19289-4608   BRT1097     RST5605.                                                                        
19290+4758   NRT   1     Primary is HAT-P-7 = Kepler-2, which hosts the 1.82 Mjup planet                 
                         Hat-P-7b in a 2.2d orbit, with a=0.0386 au. Narita et al (2010)         Nrt2010 
                         estimate the spectral type of the B and C components at M9V-L0V and             
                         M5V-M6V, respectively, assuming they are both physical companions to            
                         HAT-P-7. However, they note that it is unlikely that both companions            
                         are physical, as the system would probably be unstable.                         
                         Narita et al. (2012) estimate spectral type of C component as M5.5V             
                         based on colors, and conclude the star shared common proper motion              
                         with HAT-P-7.                                                           Nrt2012 
19290-4952   SHY 319     HIP  95795 + HIP  96725.                                                        
19291+4259   DEA 316     JKA  62. KIC 7364380/7364389.                                                   
19291+3740   KOI 113     AC, AE: Adams et al. (2012) theta values corrected to 360-theta         Adm2012 
                         (reported by Dressing et al. (2014).                                    Dre2014 
19292+2917   MLB 652     Not found by Heintz at IDS position.                                    Hei1990b
19293+3024   RUC  25     A = V401 Cyg, eclipsing binary of W UMa type, period 0.582722 days.     Zas2015 
19293+2017   CIA  57     7 Vul.                                                                          
19293+0015   H 4  33     H IV 33. See note in BDS Vol II.                                        Bu_1906 
19293-0618   PLT   6     FZ Aql.                                                                 Plt1934 
19293-1742   HJ 5124     J 1384.                                                                         
19294+4740   KOI2961     This system hosts a single planet candidate with radius of 1.2 Rearth           
                         and an orbital period of 3.78 days (Burke et al. 2014). Our ARIES       KOI2014a
                         observations revealed a companion 6.94 Ks mags fainter than KOI2961 at          
                         distance of 1".95. The predicted Kp mag of the companion is Kp = 21.5           
                         (dKp = 8.9) and the estimated dilution correction is only 0.01% due to          
                         the large brightness contrast between KOI2961 and the companion.        Dre2014 
19294+1950   J  3241     Pair is BD+19 4040.                                                     Cou1955a
19294-0703   KUI  91     A is the Cepheid U Aql.                                                         
                         Aa,Ab: ISM   3. Ismailov made three observations of U Aql, but listed   Ism1992 
                         one observation as 19279+0659 and the others as 19279-0659. This                
                         typographical error led to the inclusion of 19279+0659ISM   3 in                
                         the WDS.                                                                        
             TOK   4     Aa,Ab : Cepheid with a period of 7.02d. Distance = 592 +/- 19 pc.       GaA2019b
                         M_Aa, M_Ab = 6.2  +/- 0.8 , 2.2  +/- 0.2  /msun.                                
                         Masses are 5.7 and 2.3 Msun. Estimated period = 5.1y,                           
                         a = 5.9au = 0.01".                                                      Evs2013 
19295+3617   RUC  11     V2082 Cyg. Spectral type of resolved companion estimated at K2V.        Ruc2007 
19295+1241   BPM1030     [PM2000] 1810823 + [PM2000] 1810928.                                    Gvr2010 
19296+1224   A  1653     Prieur et al. (2014) derive a dynamical parallax of 3.3 mas and a               
                         total mass of 3.8 +/- 3.7 Msun (based on the original Hipparcos         HIP1997a
                         parallax) or 26 +/- 41 Msun (based on the revised Hipparcos parallax    VlF2007 
                         of van Leeuwen 2007).                                                   Pru2014 
19296+1200   BPM1031     [PM2000] 1811333 + [PM2000] 1811859.                                    Gvr2010 
19296-1239   HU   75     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
19297+0102   OSO 109     G092-006. AB, AC, AF, and AJ are not common proper motion pairs, based          
                         on astrometry and/or color                                              Oso2004 
19298+1236   BPMA 83     [PM2000] 1812289 + [PM2000] 1811725.                                    Gvr2010 
19298+1103   BPM1032     [PM2000] 1812029 + [PM2000] 1812133.                                    Gvr2010 
19298-6718   HJ 5109     B is CPD-67@3647.                                                               
19299-2659   H N 119     HDO 153.                                                                        
19300+4920   KOI2771     This system was reported to have a 1.7 Rearth planet with a 0.8 day             
                         period, but this signal has been found to be a false positive           KOI2014a
                         (Burke et al. 2014).                                                    Dre2014 
19300+1148   BPM1033     [PM2000] 1813024 + [PM2000] 1812582.                                    Gvr2010 
19301+4743   DEA 475     JKA  64. KIC 10536753/10536761.                                                 
19301+1142   BPM1034     [PM2000] 1813853 + [PM2000] 1813567.                                    Gvr2010 
19301+1117   GCB  41     Also known as J  2974, TOR  14, PAN  11.                                        
19301-1518   J  1847     Spectrum: Fm Delta Del.                                                         
19302+5639   A   712     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 9.74 +/- 6.20, 5.86, and 2.24 Msun, respectively.             Mlk2012 
19302+5525   ARG 104     B is BD+55@2212.                                                                
19302+1657   BPM1035     [PM2000] 1814163 + [PM2000] 1813717.                                    Gvr2010 
19302+1122   BPMA 84     [PM2000] 1814391 + [PM2000] 1812853.                                    Gvr2010 
19302+0254   STF2532     Bu_1932A and Ni_2003a BD measures originally assigned to BC.                    
                         AB: H 5  31.                                                            MEv2010 
19303+1145   BPM1036     [PM2000] 1814746 + [PM2000] 1814383.                                    Gvr2010 
19304+1240   BPM1038     [PM2000] 1815404 + [PM2000] 1815631.                                    Gvr2010 
19304+1111   TOR  13     Formerly known as PAN  10.                                                      
19304+1110   BPM1037     [PM2000] 1815401 + [PM2000] 1815873.                                    Gvr2010 
19305+1135   AG  384     B is BD+11@3864.                                                                
19306+1110   BPM1039     [PM2000] 1816847 + [PM2000] 1816218.                                    Gvr2010 
19307+2758   MCA  55     Aa,Ab: bet 1 Cyg = bet Cyg A = Albireo = 6 Cyg A. Resolved in 1976 by           
                         speckle interferometry and has also been seen visually.                 McA1982b
                         See the discussion of colors and magnitudes of this composite spectrum          
                         system by Bonneau & Foy (1980).                                         Bnu1980a
                         1977.4816: This object was incorrectly attributed to the system ADS             
                         12540 = STF  43 by McAlister (1979).                                    McA1979b
                         McAlister & Hendry (1982) also note a distant companion.                McA1982b
                         1983.4904: The distant companion reported by McAlister & Hendry (1982)  McA1982b
                         would be located beyond our 0".371 ACF window.                          Bag1984a
                         Spectral types of primary and secondary assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
                         1998.657: Absolute quadrant determined by triple-correlation technique  Pru2002b
                         Aa,Ac: Malkov et al. (2012) derive dynamical and spectroscopic masses           
                         50.66 +/- 15.18 and 22.40 Msun, respectively.                           Mlk2012 
                         Mk III Limb-darkened diameter  4.834 +/- 0.048 mas.                     MkT2003 
                         NPOI Limb-darkened diameter    4.904 +/- 0.035 mas,                             
                         R =   58.69 (+2.83-3.12 )  \rsun,  Teff = 4860 +/-  20 K,                       
                         L = 1734.  +/- 174.  \lsun.                                             NOI2023 
             STFA 43     STTA183.                                                                        
                         AB: B is BD+27@3411, spectrum B8V.                                              
                         The physicality of this wide pair has been discussed by Griffin.        Grf1999b
                         1995.559: Absolute quadrant determined by triple-correlation technique  Pru2002b
                         AB: H 5   5.                                                            MEv2010 
                         While A & B may share a common origin, it seems virtually certain that  Bst2018 
                         are not physically associated with each other. The parallax of A is             
                         9.95+/-0.60 mas while B is 8.38+/-0.17 mas.                                     
             RBR  12     Ba,Bb: First resolved in 2002, after multiple non-detections, this is   Rbr2007 
                         now thought to be a measure of the known Aa,Ab pair MCA  55 with a much Rbr2013a
                         larger than expected position angle error.                                      
19307+1237   BPM1041     [PM2000] 1817521 + [PM2000] 1817428.                                    Gvr2010 
19307+1157   BPM1040     [PM2000] 1817495 + [PM2000] 1817123.                                    Gvr2010 
19308+6337   HU  951     A premature orbit has been computed. Needs speckle.                             
19309+1208   BPM1044     [PM2000] 1818892 + [PM2000] 1818372.                                    Gvr2010 
19309+1205   BPM1042     [PM2000] 1818647 + [PM2000] 1818253.                                    Gvr2010 
19309+1201   BPM1043     [PM2000] 1818808 + [PM2000] 1818929.                                    Gvr2010 
19309+1137   OL   64     CD is 2' South.                                                         Hei1985a
19309-0631   HO  578     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
19310+3507   ES 2241     AB and BC: POP 95 AB and BC. WDS designation is considerably off,               
                         compared with precise coordinates.                                              
19310+1140   BPMA 85     [PM2000] 1819508 + [PM2000] 1817952.                                    Gvr2010 
19311+5835   MCA  56     Baize's (1989) value for omega was corrected from 0.0 to 180.0          Baz1989b
                         degrees by Ruymaekers & Nys (1995).                                     Ruy1995 
                         Spurious HIP solution for fast-moving 1.35 y pair. SB2 solution                 
                         (#1162 in in Batten et al. 1989), speckle-spectroscopic orbit           Bte1989 
                         worthwile.                                                              Sod1999 
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         Arenou (2000) gives combined solution of astrometric orbits and DSBs.   Are2000 
                         Paper includes masses and distances.                                            
                         The Farrington et al. (2010) orbit of this K2V + K4V? pair is based on  CIA2010 
                         spectroscopic, speckle, and K'-band CHARA Array separated fringe                
                         packet data. This orbit yields an orbital parallax of 59.2+/-2.04 mas           
                         and component masses of 0.82+/-0.09 and 0.77+/-0.09 Msun. The aperture          
                         and method, 8m and speckle, are set to give the resolution capability           
                         of this technique, which is less than classical interferometric                 
                         methods.                                                                        
                         Martin et al. (1998) derive component masses 1.217 +/- 0.172 and                
                         0.456 +/- 0.167 Msun.                                                   Mig1998 
                         Orbit determined by fitting revised Hipparcos intermediate astrometric          
                         data. Derived component masses 0.86 +/- 0.43 and 0.81 +/- 0.40 Msun.    Ren2010 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.59 +/- 0.07, 1.63, and 0.79 Msun, respectively.             Mlk2012 
                         Improved resolved SB2 orbit for this pair.                              Kie2018 
                         A: Teff = 5114 +/- 11 K, M = 0.833 +/- 0.031 \msun.                             
                         B: Teff = 4705 +/- 101 K, M = 0.812 +/- 0.030 \msun.                            
                         Orbital parallax = 56.10 +/- 0.81mas.                                           
                         Age = 2.2-7.9 Gyr.                                                              
19311+1204   BPM1045     [PM2000] 1819761 + [PM2000] 1819903.                                    Gvr2010 
19311-7348   GLI 295     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al. Also known as RSS  33.                        Rss1996 
19312+6319   STF2549     STTA184.                                                                        
19312+4338   A   595     A is the semiregular variable UV Cyg.                                           
19312+3607   GIC 158     G125-015/G125-014.                                                              
                         NLTT 47904/47903                                                        Chm2004 
                         While no candidates are visible in the AstraLux images, it is actually          
                         a triple system. G 125-15 itself is noted as a very close (<0.01 au)            
                         double-lined spectroscopic binary in Shkolnik et al. (2010 ApJ 716,             
                         1522). Additionally, there is a wide CPM companion at 46".              Jnn2014 
19312+1205   BPM1046     [PM2000] 1821052 + [PM2000] 1821056.                                    Gvr2010 
19313+4729   A   713     Primary is eclipsing binary V2083 Cyg (period 1.86749 day).             Zas2010 
                         Spectral types of the Aa and Ab stars are both about A7-A8. The mass            
                         and spectral type of the B component are uncertain; two reduction               
                         methods give discrepant results. Possible reasons include an incorrect          
                         Hipparcos parallax or duplicity of the companion.                       Zas2012c
19313-0207   D    20     A is the Algol-type system V822 Aql, P = 5.3d.                                  
             STF2535     AC: Additional notes may be found in Burnham (1894).                    Bu_1894 
19314+1135   BPMA 86     [PM2000] 1822192 + [PM2000] 1820076.                                    Gvr2010 
19314+1036   BPM1047     [PM2000] 1822578 + [PM2000] 1823419.                                    Gvr2010 
19315-2053   HJ 2875     HJ 1403. HJ 1412.                                                               
19316+1747   STF2536     A premature orbit has been computed.                                            
19316+1337   BPM1049     [PM2000] 1824037 + [PM2000] 1824881.                                    Gvr2010 
19316+1249   BPM1048     [PM2000] 1823829 + [PM2000] 1824162.                                    Gvr2010 
19316+1204   BPM1050     AB: [PM2000] 1824111 + [PM2000] 1824879.                                Gvr2010 
             BPM1051     BC: [PM2000] 1824879 + [PM2000] 1824544.                                Gvr2010 
19317+5300   STF2542     AB: HLM  25.                                                                    
19317+4836   KOI 124     Adams et al. (2012) theta values corrected to 360-theta                 Adm2012 
                         (reported by Dressing et al. (2014).                                    Dre2014 
19317+4506   BVD 267     JKA  65. KIC 8888543/8888573.                                                   
19317+1300   BPM1052     [PM2000] 1824769 + [PM2000] 1824127.                                    Gvr2010 
19317+1038   BPM1053     [PM2000] 1824822 + [PM2000] 1824619.                                    Gvr2010 
19317+0848   BU 1470     Involved with a very faint nebula, HJ 2043.                                     
19318+1244   BPMA 87     [PM2000] 1824949 + [PM2000] 1826976.                                    Gvr2010 
19318+1209   BPM1055     [PM2000] 1825562 + [PM2000] 1825777.                                    Gvr2010 
19318+1153   BPMA 88     AB: [PM2000] 1825589 + [PM2000] 1826582.                                Gvr2010 
             BPMA 89     AC: [PM2000] 1825589 + [PM2000] 1826993.                                Gvr2010 
             BPMA 90     BD: [PM2000] 1826582 + [PM2000] 1827191.                                Gvr2010 
             BPM1059     BC: [PM2000] 1826582 + [PM2000] 1826993.                                Gvr2010 
             BPMA 91     CD: [PM2000] 1826993 + [PM2000] 1827191.                                Gvr2010 
19318+1150   BPM1054     [PM2000] 1825094 + [PM2000] 1824821.                                    Gvr2010 
19318+1104   BPM1056     [PM2000] 1825566 + [PM2000] 1825101.                                    Gvr2010 
19319+1229   BPM1058     [PM2000] 1825830 + [PM2000] 1826607.                                    Gvr2010 
19319+1113   BPM1057     [PM2000] 1825809 + [PM2000] 1826576.                                    Gvr2010 
19320+1238   BPM1060     AB: [PM2000] 1826953 + [PM2000] 1826793.                                Gvr2010 
             BPM1061     AC: [PM2000] 1826953 + [PM2000] 1826942.                                Gvr2010 
19321+3221   HU  945     AC: SEI 618.                                                            Nsn2017b
19321+2816   STF2539     AC: H 2  99.                                                            MEv2010 
19321+2653   BRT3344     Originally published as BRT 195.                                        Brt1928 
19321+1204   BPM1062     AB: [PM2000] 1827238 + [PM2000] 1827503.                                Gvr2010 
             BPM1063     BC: [PM2000] 1827503 + [PM2000] 1827581.                                Gvr2010 
19321+1136   BPM1064     [PM2000] 1827494 + [PM2000] 1827935.                                    Gvr2010 
19322+1237   BPMA 93     [PM2000] 1828662 + [PM2000] 1829919.                                    Gvr2010 
19322+1202   BPM1065     [PM2000] 1828197 + [PM2000] 1828901.                                    Gvr2010 
19322+1148   BPM1066     [PM2000] 1828595 + [PM2000] 1829480.                                    Gvr2010 
19322+1146   BPMA 92     [PM2000] 1828537 + [PM2000] 1827948.                                    Gvr2010 
19322+0630   BU  650     E is BD+06@4177.                                                                
19323+1212   BRT1319     J 2550.                                                                         
19323+1201   BPM1067     [PM2000] 1828790 + [PM2000] 1829827.                                    Gvr2010 
19323+0132   BAL1521     Incorrectly listed as BD+11 3879 in the WDS, although the source of             
                         that attribution is unknown.                                                    
19324+6940   STT 590     sig Dra = 61 Dra = Alsafi. Proper motion of A: +593-1738. B : -010-014.         
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         CHARA Array Limb-darkened diameter  1.254 +/- 0.012 mas,                CIA2008d
                         R =  0.778 +/- 0.008 \rsun, Teff = 5299 +/- 32,                                 
                         L =  0.428 +/- 0.013 \lsun.                                                     
                         CHARA Array Limb-darkened diameter  1.254 +/- 0.012 mas,                CIA2012e
                         R =  0.776 +/- 0.008 \rsun, L =  0.410 +/-0.006 \lsun,                          
                         Teff = 5255 +/-  31 K.                                                          
19324+1147   BPM1068     AB: [PM2000] 1829523 + [PM2000] 1829115.                                Gvr2010 
             BPM1069     BC: [PM2000] 1829115 + [PM2000] 1829331.                                Gvr2010 
19324+1142   BPMA 94     [PM2000] 1830084 + [PM2000] 1828135.                                    Gvr2010 
19324+1033   BPM1070     [PM2000] 1829721 + [PM2000] 1830060.                                    Gvr2010 
19324+1026   BPM1071     [PM2000] 1829726 + [PM2000] 1829534.                                    Gvr2010 
19324-2244   DON 961     CD-22@14037.                                                                    
19325+4056   KOI 555     Primary is Kepler exoplanet host star.                                  Adm2013 
19325+1146   BPM1074     [PM2000] 1830857 + [PM2000] 1830665.                                    Gvr2010 
19325+1110   TOR  15     Formerly known as PAN  12.                                                      
19325+1036   BPM1072     AB: [PM2000] 1830345 + [PM2000] 1831165.                                Gvr2010 
             BPM1073     BC: [PM2000] 1831165 + [PM2000] 1830121.                                Gvr2010 
19326+1153   BPMA 95     [PM2000] 1831148 + [PM2000] 1833114.                                    Gvr2010 
19326+1143   BPMA 96     [PM2000] 1831455 + [PM2000] 1832847.                                    Gvr2010 
19327+1207   BPM1075     [PM2000] 1831930 + [PM2000] 1832682.                                    Gvr2010 
19327+1159   BPM1078     [PM2000] 1832573 + [PM2000] 1832479.                                    Gvr2010 
19327+1102   BPM1077     [PM2000] 1832501 + [PM2000] 1832358.                                    Gvr2010 
19327+1035   BPM1076     [PM2000] 1832027 + [PM2000] 1832447.                                    Gvr2010 
19328+3001   RAO 515     V885 Cyg.                                                                       
19328+1219   BPM1079     [PM2000] 1832647 + [PM2000] 1832867.                                    Gvr2010 
19328+1138   BPMA 97     [PM2000] 1832820 + [PM2000] 1830918.                                    Gvr2010 
19329+3028   BKO 517     Anon. 29.                                                               Bko2009d
19329+1223   BPM1082     [PM2000] 1834138 + [PM2000] 1834697.                                    Gvr2010 
19329+1201   BPM1080     [PM2000] 1833742 + [PM2000] 1834648.                                    Gvr2010 
19329+1200   BPM1081     [PM2000] 1834124 + [PM2000] 1833975.                                    Gvr2010 
19329+1149   BPMA 98     [PM2000] 1833735 + [PM2000] 1831835.                                    Gvr2010 
19329-1735   FEN  35     A likely plate flaw.                                                    Grv2021b
19330+1307   BPM1084     [PM2000] 1835031 + [PM2000] 1834509.                                    Gvr2010 
19330+1144   BPMA 99     [PM2000] 1835062 + [PM2000] 1836500.                                    Gvr2010 
19330+1104   BPM1083     [PM2000] 1834841 + [PM2000] 1835945.                                    Gvr2010 
19331+1655   BPM1089     [PM2000] 1835632 + [PM2000] 1835981.                                    Gvr2010 
19331+1338   BPM1085     AB: [PM2000] 1835445 + [PM2000] 1836113.                                Gvr2010 
             BPM1086     BC: [PM2000] 1836113 + [PM2000] 1835389.                                Gvr2010 
19331+1155   BPM1088     [PM2000] 1835631 + [PM2000] 1834728.                                    Gvr2010 
19331+1150   BPM1087     [PM2000] 1835624 + [PM2000] 1836609.                                    Gvr2010 
19331+0725   BUP 192     AB: Also known as FOX 244.                                                      
19331-4954   HJ 5125     B is CD-50@12544.                                                               
19332+6010   STFA 44     STTA186. B is BD+59@2059.                                                       
19332+1808   BPM1090     [PM2000] 1836618 + [PM2000] 1836364.                                    Gvr2010 
19332+1241   BPMA100     [PM2000] 1836171 + [PM2000] 1838669.                                    Gvr2010 
19332+1130   BPMA101     [PM2000] 1836746 + [PM2000] 1836809.                                    Gvr2010 
19333+3329   HO  108     No measures 1907-1944, and then uncertain until 1955.                           
19333+3235   RAS  30     SrCuEu star, type A9; companion late K.                                 Ras2014 
19333+1248   BPM1094     [PM2000] 1837489 + [PM2000] 1837396.                                    Gvr2010 
19333+1207   BPM1093     [PM2000] 1837109 + [PM2000] 1837896.                                    Gvr2010 
19333+1039   BPM1091     [PM2000] 1836821 + [PM2000] 1836541.                                    Gvr2010 
19333+1026   BPM1092     [PM2000] 1836932 + [PM2000] 1837920.                                    Gvr2010 
19333-4706   RSS  34     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
19334+2403   POU3907     J  2977.                                                                        
19334+1210   BPMA102     [PM2000] 1838182 + [PM2000] 1840014. 100deg error in theta.             Gvr2010 
19334+1106   BPM1095     [PM2000] 1838434 + [PM2000] 1838063.                                    Gvr2010 
19334+0227   BAL1998     J 1849.                                                                         
19335+4447   KOI1279     This system contains two short-period planet candidates with radii of           
                         1.6 and 0.9 Rearth (Borucki et al. 2011; Batalha et al. 2013). KOI1279  KOI2011 
                         does not exhibit a large source offset during transits, which supports  KOI2013a
                         the interpretation that the planet candidates orbit the target star.    Dre2014 
19335+3610   HJ 1414     The first Sei1908 measure at epoch 1895.5 is of a pair that does not            
                         exist.  The secondary component of this pair is a bogus AC2000.2                
                         position.  Sometimes these positions occur in the AC2000.2 catalog.             
                         SEI 630. SEI 631.                                                       Nsn2017b
19335+1814   HU  341     J 149.                                                                          
19335+1119   BPM1096     [PM2000] 1838656 + [PM2000] 1839614.                                    Gvr2010 
19335+1105   BPM1097     [PM2000] 1839143 + [PM2000] 1839863.                                    Gvr2010 
19336+2414   POU3911     J  2978.                                                                        
19336+1211   BPM1099     [PM2000] 1839909 + [PM2000] 1839636.                                    Gvr2010 
19336+1205   BPMA103     [PM2000] 1839929 + [PM2000] 1840960.                                    Gvr2010 
19336+1028   BPM1098     [PM2000] 1839629 + [PM2000] 1839730.                                    Gvr2010 
19336+0346   TOK 903     V1294 Aql.                                                                      
19336-0411   STF2537     B is BD-04@4842.                                                                
19337+5003   HJ 1418     B is BD+49@3045.                                                                
19337+2936   SLE 630     AC: There is a 10" error in the published declination of Soulie's C             
                         component.                                                              Sle1986b
19337+1441   BPM1101     [PM2000] 1840319 + [PM2000] 1840365.                                    Gvr2010 
19337+1207   BPMA105     AB: [PM2000] 1840506 + [PM2000] 1840587.                                Gvr2010 
             BPMA106     BC: [PM2000] 1840587 + [PM2000] 1839865.                                Gvr2010 
19337+1206   BPM1100     [PM2000] 1840269 + [PM2000] 1839931.                                    Gvr2010 
19337+1202   BPMA104     [PM2000] 1840247 + [PM2000] 1839435.                                    Gvr2010 
19337+1158   BPM1106     [PM2000] 1840429 + [PM2000] 1840623.                                    Gvr2010 
19337+1142   BPM1104     AB: [PM2000] 1840977 + [PM2000] 1840682.                                Gvr2010 
             BPM1105     BC: [PM2000] 1840682 + [PM2000] 1841765.                                Gvr2010 
19337+1137   BPM1107     [PM2000] 1841002 + [PM2000] 1840982.                                    Gvr2010 
19337+1108   BPM1102     AB: [PM2000] 1840414 + [PM2000] 1841400.                                Gvr2010 
             BPM1103     BC: [PM2000] 1841400 + [PM2000] 1841112.                                Gvr2010 
19338+3250   HJ 1413     SEI 634.                                                                Nsn2017b
19338+1247   BPM1109     [PM2000] 1841854 + [PM2000] 1841933.                                    Gvr2010 
19338+1244   BPMA107     [PM2000] 1841822 + [PM2000] 1841040.                                    Gvr2010 
19338+1207   BPMA108     [PM2000] 1842011 + [PM2000] 1842770.                                    Gvr2010 
19338+1157   BPM1108     [PM2000] 1841789 + [PM2000] 1842145.                                    Gvr2010 
19338-2024   HJ 2879     Measures uncertain.                                                             
19338-2703   HJ 2877     B is CD-27@14070.                                                               
19339+1205   BPM1110     [PM2000] 1842146 + [PM2000] 1841798.                                    Gvr2010 
19340+6017   STF2554     B is BD+59@2064.                                                                
19340+1030   BPM1111     [PM2000] 1843391 + [PM2000] 1843871.                                    Gvr2010 
19341+1736   BPM1115     [PM2000] 1844231 + [PM2000] 1845308.                                    Gvr2010 
19341+1635   BPM1112     [PM2000] 1843902 + [PM2000] 1843719.                                    Gvr2010 
19341+1205   BPM1114     [PM2000] 1844104 + [PM2000] 1843757.                                    Gvr2010 
19341+1201   BPM1113     [PM2000] 1844089 + [PM2000] 1844639.                                    Gvr2010 
19341+1136   BPMA109     AB: [PM2000] 1844452 + [PM2000] 1844989.                                Gvr2010 
             BPMA110     BC: [PM2000] 1844989 + [PM2000] 1842347.                                Gvr2010 
19341+0723   BU  653     38 Aql = mu Aql                                                                 
                         NPOI Limb-darkened diameter    2.032 +/- 0.040 mas,                             
                         R =    7.43 (+/- 0.15   )  \rsun,  Teff = 4746 +/-  47 K,                       
                         L =   25.2 +/-   0.2 \lsun.                                             NOI2023 
                         AB and AC: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
19342+1231   BPM1116     [PM2000] 1845174 + [PM2000] 1845605.                                    Gvr2010 
19343+1720   BPM1117     [PM2000] 1846155 + [PM2000] 1845891.                                    Gvr2010 
19343+1257   BPMA111     [PM2000] 1846402 + [PM2000] 1848092.                                    Gvr2010 
19344+1332   BPM1118     [PM2000] 1846826 + [PM2000] 1845740.                                    Gvr2010 
19344+1129   BPM1119     [PM2000] 1847284 + [PM2000] 1847037.                                    Gvr2010 
19345+1552   BPM1124     [PM2000] 1848073 + [PM2000] 1847123.                                    Gvr2010 
19345+1218   BPM1121     [PM2000] 1847559 + [PM2000] 1847323.                                    Gvr2010 
19345+1138   BPM1123     [PM2000] 1847774 + [PM2000] 1848407.                                    Gvr2010 
19345+1133   BPM1120     [PM2000] 1847460 + [PM2000] 1848250.                                    Gvr2010 
19345+1107   BPM1122     [PM2000] 1847649 + [PM2000] 1848467.                                    Gvr2010 
19345+0037   BAL1206     J 2552.                                                                         
19346+5039   DAL  20     AB: NI   39.                                                                    
19346+3518   AG  232     SEI 639.                                                                Nsn2017b
19346+1946   BU 1130     9 Vul. Alternate spectrum: A0V+F8III.                                           
19346+1808   STT 375     Characterized as a constant velocity star with an orbital period of     Grf2010b
                         more than a thousand years.                                                     
19346+1419   BPM1128     [PM2000] 1848400 + [PM2000] 1848826.                                    Gvr2010 
19346+1225   BPM1125     AB: [PM2000] 1848732 + [PM2000] 1848240.                                Gvr2010 
             BPM1126     BC: [PM2000] 1848240 + [PM2000] 1847422.                                Gvr2010 
19346+1110   BPM1127     [PM2000] 1848489 + [PM2000] 1848004.                                    Gvr2010 
19347+1259   BPM1131     [PM2000] 1849760 + [PM2000] 1850280.                                    Gvr2010 
19347+1243   BPM1132     [PM2000] 1849787 + [PM2000] 1850201.                                    Gvr2010 
19347+1134   BPM1129     [PM2000] 1849305 + [PM2000] 1849959.                                    Gvr2010 
19347+1118   BPM1130     [PM2000] 1849745 + [PM2000] 1849553.                                    Gvr2010 
19347+1115   BPMA112     [PM2000] 1849963 + [PM2000] 1848857.                                    Gvr2010 
19348+2928   WRH  32     9 Cyg. A long-period spectroscopic binary resolved by interferometry.           
                         Balega et al (2007) discuss orbital evolution of this pair to explain   Bag2007d
                         apparent mixing of the primary during its main-sequence evolution.              
                         Additional notes may be found in Wilson (1951) and                      WRH1951 
                         Wilson (1952).                                                          WRH1952 
                         Martin et al. (1998) derive component masses 3.344 +/- 1.165 and                
                         1.586 +/- 0.612 Msun.                                                   Mig1998 
19348+1629   BPMA115     [PM2000] 1850748 + [PM2000] 1851533.                                    Gvr2010 
19348+1549   BPM1134     [PM2000] 1850724 + [PM2000] 1851037.                                    Gvr2010 
19348+1313   BPMA114     [PM2000] 1850385 + [PM2000] 1850769.                                    Gvr2010 
19348+1233   BPM1133     [PM2000] 1850300 + [PM2000] 1849878.                                    Gvr2010 
19348+1228   BPMA116     [PM2000] 1851059 + [PM2000] 1849340.                                    Gvr2010 
19348+1142   BPMA113     [PM2000] 1850253 + [PM2000] 1848986.                                    Gvr2010 
19349+4154   KOI 270     Distance is 260.11 +/- 13.15 pc. Ma (Mb) = 0.84 (0.77) +/- 0.1 \msun.   Hor2024 
19349+3649   WTS   2     The primary is orbited by a close-in 1.12Mjup planet (P = 1.02d),               
                         discovered during the WFCAM Transit Survey.                             Bkb2014 
19349+1202   BPM1135     [PM2000] 1851237 + [PM2000] 1852178.                                    Gvr2010 
19349+1147   BPM1137     [PM2000] 1851305 + [PM2000] 1852027.                                    Gvr2010 
19349+1134   BPM1136     [PM2000] 1851239 + [PM2000] 1852197.                                    Gvr2010 
19349+1132   BPMA117     [PM2000] 1851497 + [PM2000] 1851437.                                    Gvr2010 
19350+2328   A   162     Only elements P, T, and a have been amended by Starikova (1982) from    Sta1982b
                         the orbit of Erceg (1975).                                              Erc1975 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.63 +/- 2.16, 3.21, and 2.24 Msun, respectively.             Mlk2012 
19350+1534   BPM1138     [PM2000] 1852284 + [PM2000] 1851898.                                    Gvr2010 
19350+1108   BPM1139     [PM2000] 1852647 + [PM2000] 1852780.                                    Gvr2010 
19351+5038   HU  679     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.48 +/- 1.42, 2.35, and 1.10 Msun, respectively.             Mlk2012 
19351+1656   BPM1142     [PM2000] 1853512 + [PM2000] 1853407.                                    Gvr2010 
19351+1317   BPM1141     [PM2000] 1853394 + [PM2000] 1854389.                                    Gvr2010 
19351+1251   BPM1140     [PM2000] 1853138 + [PM2000] 1854176.                                    Gvr2010 
19351+1121   BPM1143     [PM2000] 1853687 + [PM2000] 1854074.                                    Gvr2010 
19364+5013   STT 591     AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
19366+2830   BRT  38     A likely plate flaw.                                                    Grv2021b
19385-2031   ARA1192     A likely plate flaw.                                                    Grv2021a
19423+1937   HJ 2891     Rectilinear solution by Hurowitz et al. (2014).                         USN2014b
19429+0115   HJ  895     AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
19464+3344   STF2580     AC: Rectilinear solution by Friedman et al. (2011).                     USN2011a
                         BC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
             STF2576     FI: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
19496-2954   BRT3087     A likely plate flaw.                                                    Grv2021b
19500+0637   J  1336     AB: Rectilinear solutions by Cvetkovic (2015)                           Cve2015b
                         and Cvetkovic et al. (2016).                                            Cve2016 
19507-5912   I   121     Aa,Ab: Rectilinear solution by Zirm (2013).                             Zir2013d
19510+1025   J   124     AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
19532+2017   H 3 105     A component = C component of 19534+2020 GUI  28AC.                              
19352+1140   BPM1144     [PM2000] 1854270 + [PM2000] 1853601.                                    Gvr2010 
19352-2508   B   442     HIP 96333. See Allen et al. (2000) for information on metallicity,      AlC2000 
             LDS 682     age, galactic orbital parameters, etc.                                          
19353+1438   BPM1147     [PM2000] 1855514 + [PM2000] 1856084.                                    Gvr2010 
19353+1340   BPM1148     [PM2000] 1855728 + [PM2000] 1856466.                                    Gvr2010 
19353+1147   BPM1145     [PM2000] 1855273 + [PM2000] 1855112.                                    Gvr2010 
19353+1125   BPMA118     [PM2000] 1855302 + [PM2000] 1853700.                                    Gvr2010 
19353+1043   BPM1146     [PM2000] 1855283 + [PM2000] 1854876.                                    Gvr2010 
19534+2020   GUI  28     AC: C component = A component of 19532+2017 H 3 105.                            
19354+1151   BPMA119     [PM2000] 1855955 + [PM2000] 1854428.                                    Gvr2010 
19354+1120   BPMA120     [PM2000] 1856183 + [PM2000] 1857375.                                    Gvr2010 
19355+1311   BPM1151     [PM2000] 1857283 + [PM2000] 1857531.                                    Gvr2010 
19355+1255   BPM1156     AB: [PM2000] 1857557 + [PM2000] 1858058.                                Gvr2010 
             BPM1157     BC: [PM2000] 1858058 + [PM2000] 1858234.                                Gvr2010 
19355+1150   BPM1152     AB: [PM2000] 1857349 + [PM2000] 1858075.                                Gvr2010 
             BPM1153     BC: [PM2000] 1858075 + [PM2000] 1858800.                                Gvr2010 
             BPM1154     CD: [PM2000] 1858800 + [PM2000] 1857788.                                Gvr2010 
19355+1113   BPM1149     [PM2000] 1857013 + [PM2000] 1857322.                                    Gvr2010 
19355+1106   BPM1150     [PM2000] 1857095 + [PM2000] 1857535.                                    Gvr2010 
19356+1258   BPM1155     [PM2000] 1858256 + [PM2000] 1858453.                                    Gvr2010 
19356+0257   J  1677     BAL 2000.                                                                       
19357+1334   BPM1160     [PM2000] 1859221 + [PM2000] 1860138.                                    Gvr2010 
19357+1251   BPM1158     [PM2000] 1858850 + [PM2000] 1858360.                                    Gvr2010 
19357+1154   BPM1159     [PM2000] 1858900 + [PM2000] 1857765.                                    Gvr2010 
19358+1647   BPM1164     AB: [PM2000] 1860090 + [PM2000] 1860759.                                Gvr2010 
             BPM1165     AC: [PM2000] 1860090 + [PM2000] 1859104.                                Gvr2010 
19358+1610   BPM1163     [PM2000] 1859847 + [PM2000] 1859336.                                    Gvr2010 
19358+1206   BPM1162     [PM2000] 1859756 + [PM2000] 1858604.                                    Gvr2010 
19358+1145   BPMA121     [PM2000] 1859621 + [PM2000] 1860423.                                    Gvr2010 
19358+1133   BPM1161     [PM2000] 1860410 + [PM2000] 1861072.                                    Gvr2010 
19359+5659   RAO  87     A is SB1, P=14.1y.                                                      Tok2014d
                         Triple. Its inner system has a preliminary spectroscopic period of 14           
                         yr and low amplitude (D. Latham 2012, private communication). Despite           
                         the estimated semimajor axis of 0".25, the spectroscopic secondary is           
                         too faint for direct resolution without a high-contrast coronagraph.            
                         The 2MASS companion at 10", noted first by Fuhrmann (2004 AN 325, 3),           
                         shares the large PM of A and is located on the MS.                      Rbr2015d
19359+1251   BPM1169     [PM2000] 1861091 + [PM2000] 1860341.                                    Gvr2010 
19359+1248   BPM1170     [PM2000] 1860977 + [PM2000] 1861457.                                    Gvr2010 
19359+1235   BPM1168     [PM2000] 1861031 + [PM2000] 1860555.                                    Gvr2010 
19359+1150   BPM1166     AB: [PM2000] 1861353 + [PM2000] 1860399.                                Gvr2010 
             BPM1167     BC: [PM2000] 1860399 + [PM2000] 1859314.                                Gvr2010 
19360+2924   FYM  43     AE and AF were initially thought to be new pairs AM and AK. Also, his   FyM2014b
                         HJ pair is actually AJ.                                                         
19360+1243   BPM1172     AB: [PM2000] 1861961 + [PM2000] 1863020.                                Gvr2010 
             BPM1173     BC: [PM2000] 1863020 + [PM2000] 1863857.                                Gvr2010 
19360+1151   BPM1171     [PM2000] 1861887 + [PM2000] 1862789.                                    Gvr2010 
19360+0005   A  1188     HIP 96402. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
19360-6624   HJ 5123     B is CPD-66@3438.                                                               
19362+1700   BPM1175     [PM2000] 1864193 + [PM2000] 1865196.                                    Gvr2010 
19362+1636   BPM1174     [PM2000] 1863587 + [PM2000] 1862308.                                    Gvr2010 
19362+1312   BPMA122     [PM2000] 1864352 + [PM2000] 1865811.                                    Gvr2010 
19362+0600   STF2543     Mt. Wilson spectral types are G3 and gM0.                                       
19362-1905   SEE 383     FOX 28.                                                                         
19363+3540   STT 377     AB,C: SEI 646. Incorrectly referred to as STF 377 by Scheiner.          Nsn2017b
19363+1430   TDT1576     The Tycho measure is erroneous, apparently due to problems in                   
                         resolving this close triple.                                                    
19363+1326   BPM1177     [PM2000] 1865360 + [PM2000] 1865658.                                    Gvr2010 
19363+1218   BPM1176     [PM2000] 1864585 + [PM2000] 1864818.                                    Gvr2010 
19364+5013   BU 1131     the Cyg = 13 Cyg. Young & Farnsworth suggested that a faint companion   YAS1924 
                         2' west was physical. Bidelman confirms that the spectral type, M2/3    Bid1980 
                         is consistent with this suggestion.                                             
                         CHARA Array Limb-darkened diameter  0.861 +/- 0.015 mas,                CIA2012e
                         R =  1.697 +/- 0.030 \rsun, L =  4.265 +/-0.090 \lsun,                          
                         Teff = 6381 +/-  65 K, M = 1.342 +/- 0.011 \msun,                               
                         Age =  2.8 +/- 0.2 Gyr.                                                         
             STT 591     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
19364+5013   LDS5881     EF: Originally 19363+5012 LDS5881, but primary found to be E component          
                         of 19364+5013 SKF1976AE.                                                        
19364+1621   BPM1179     [PM2000] 1865915 + [PM2000] 1865978.                                    Gvr2010 
19364+1554   H 5 104     H V 104.                                                                        
19364+1336   BPM1178     [PM2000] 1865819 + [PM2000] 1865694.                                    Gvr2010 
19365+1539   BPM1180     [PM2000] 1866758 + [PM2000] 1866080.                                    Gvr2010 
19365+1526   BPM1183     [PM2000] 1867242 + [PM2000] 1867582.                                    Gvr2010 
19365+1356   BPM1181     AB: [PM2000] 1867176 + [PM2000] 1866880.                                Gvr2010 
             BPM1182     AC: [PM2000] 1867176 + [PM2000] 1868457.                                Gvr2010 
19365+1224   BPMA123     [PM2000] 1867046 + [PM2000] 1869844.                                    Gvr2010 
19366+2700   BRT3345     Originally published as BRT 196.                                        Brt1928 
19366+2020   EVS  46     U Vul                                                                           
19366+1626   BPM1186     [PM2000] 1868243 + [PM2000] 1867949.                                    Gvr2010 
19366+1306   BPM1185     [PM2000] 1868025 + [PM2000] 1867764.                                    Gvr2010 
19366+1208   BPM1184     [PM2000] 1867869 + [PM2000] 1867975.                                    Gvr2010 
19367+3052   BRT 267     SMA.                                                                            
19367+2627   BRT3346     Originally published as BRT 197.                                        Brt1928 
19367+1315   BPM1188     [PM2000] 1869256 + [PM2000] 1870404.                                    Gvr2010 
19367+1246   BPMA124     AB: [PM2000] 1869152 + [PM2000] 1869874.                                Gvr2010 
             BPM1187     BC: [PM2000] 1869874 + [PM2000] 1868916.                                Gvr2010 
19367+0357   BAL2518     A = V418 Aql, eclipsing binary of Algol-type, period 2.234904 days.     Zas2015 
19367-0117   J   118     iot Aql = 41 Aql                                                                
19367-2453   BU  654     52 Sgr. Variable?                                                               
19368+5012   BLL  40     A is the Mira-type variable R Cyg. May be the same as STT 591CD.                
                         B is BD+49@3065.                                                                
19368+1456   BPM1190     [PM2000] 1869969 + [PM2000] 1869161.                                    Gvr2010 
19368+1324   BPMA125     [PM2000] 1870185 + [PM2000] 1869502.                                    Gvr2010 
19368+1139   BPM1189     [PM2000] 1869598 + [PM2000] 1870220.                                    Gvr2010 
19369+1354   BPM1191     [PM2000] 1871160 + [PM2000] 1871395.                                    Gvr2010 
19369+1217   BPMA126     [PM2000] 1871030 + [PM2000] 1873288.                                    Gvr2010 
19369-2003   BHA  31     J 1763.                                                                         
19370+6350   STF2564     Mt. Wilson spectral types are F2s and A8n.                                      
19370+5111   HJ 1426     10deg error in converting NPD to Dec for IDS.                                   
19370+1455   BPM1194     [PM2000] 1871857 + [PM2000] 1872727.                                    Gvr2010 
19370+1243   BPM1196     [PM2000] 1872015 + [PM2000] 1871931.                                    Gvr2010 
19370+1221   BPM1193     [PM2000] 1871785 + [PM2000] 1871002.                                    Gvr2010 
19370+1212   BPM1195     [PM2000] 1871954 + [PM2000] 1872000.                                    Gvr2010 
19370+1203   BPM1192     [PM2000] 1871465 + [PM2000] 1870920.                                    Gvr2010 
19370+1135   BPM1197     [PM2000] 1872170 + [PM2000] 1873056.                                    Gvr2010 
19370+0911   J   171     The FYM 135AC pair was in error and has been deleted.                   FyM2014b
19371+1406   BPM1199     [PM2000] 1873051 + [PM2000] 1871985.                                    Gvr2010 
19371+1210   BPM1198     [PM2000] 1872467 + [PM2000] 1872877.                                    Gvr2010 
19371+0819   GUI  26     AD was incorrectly identified as the CD pair.                                   
19371-1607   BRT 635     J  3343.                                                                Nsn2016 
19371-5134   CRI  23     White dwarf / red drwarf pair.                                                  
                         The A component is SB2. Huelamo et al. (2009) find is also eclipsing.   Hue2009 
                         V magnitudes of Aa and Ab are 12.29 and 12.84, spectral types M1Ve and          
                         M2:Ve, masses 0.59 +/- 0.03 and 0.54 +/- 0.03 Msun; distance to the             
                         system is 42+/-3 pc. They also conclude AB pair is CPM and that the B           
                         component is a pure-helium DB white dwarf, mass 0.648 Msun, distance            
                         46pc. The age of the triple ~400 Myr.                                           
19372+2920   HJ 1423     The Wilson Aa,Ab, AE, AF, and AG components of 19448+2916 were                  
                         previously assigned to this system, but this was a position error on            
                         Wilson's part, leading to the the pairs not being confirmed for many    WRH1950a
                         years. The wider components of Wilson were moved, but retained their            
                         historical component identifiers. The closer Aa,Ab pair had been                
                         independently discovered by Ismailov, so retained its ISM   4Aa,Ab              
                         designation. The problem was noted by Cliff Ashcraft and the correct            
                         system found by James Daley.                                                    
             FYM  97     A star at ~80deg, 1' from the primary has been inadvertently measured           
                         under the assumption it was Wilson's AG pair, so has been given the     FyM2013c
                         designation FYM  97AG.                                                          
19372+2830   GNS   3     Ginski et al. (2012) conclude the companion is physical, and estimate           
                         the mass at 0.239 +/- 0.022 Msun.                                       Gns2012 
                         Ginski et al. (2016) resolved the B component into a ~100 mas pair of           
                         similar magnitude. Masses of Ba and Bb are estimated at 0.165 +/-               
                         0.008 and 0.154 +0.009/-0.008 Msun.                                     Gns2016 
                         CHARA Array Limb-darkened diameter  0.480 +/- 0.033 mas.                CIA2009a
                         R =  2.59 +/- 0.19 \rsun, L =   4.7 +/-  0.1 \lsun,                             
                         Teff = 5283 +/- 186 K.                                                          
19372+1812   BPMA127     [PM2000] 1873903 + [PM2000] 1875055.                                    Gvr2010 
19372+1546   BPM1202     [PM2000] 1874150 + [PM2000] 1873328.                                    Gvr2010 
19372+1201   BPM1201     [PM2000] 1873718 + [PM2000] 1873311.                                    Gvr2010 
19372+1149   BPM1200     [PM2000] 1873562 + [PM2000] 1873200.                                    Gvr2010 
19373+1628   H 6  26     H VI 26. STTA185. eps Sge = 4 Sge. B is BD+16@3919.                             
                         AD: Baranov (1909) measured new companions at (303deg, 29.2", V=7.8)    BnW1909 
                         and (343deg, 160.8", V=9.5), in addition to a measure of the AB pair.           
                         The wide pair was added to the WDS as H 2 26AD, but the 29" pair was            
                         apparently ignored. A check on Aladin shows no hint of either of the            
                         new companions. It appears that Baranov may have accidentally merged            
                         his measure of H 6 26 with measures of the nearby pair 19394+1634 =             
                         H N 84. His 29.2" measure agrees with other measures of that pair, and          
                         a star in the field of H N  84 (V=11.9) matches his wide pair.                  
                         H 6 26AD has therefore been X-coded. Since the identification with              
                         H N 84 is likely but not definite (and since the 12th magnitude star            
                         near H N 84 appears to be a random field star), Baranov's measures              
                         have not been added.  Thanks to Steve Smith and John Nanson for                 
                         alerting us to this discrepancy.                                                
19373+1349   BPM1203     [PM2000] 1874523 + [PM2000] 1874267.                                    Gvr2010 
19373+1255   BPM1204     [PM2000] 1874694 + [PM2000] 1873933.                                    Gvr2010 
19373+1155   BPMA128     [PM2000] 1874848 + [PM2000] 1876811.                                    Gvr2010 
19373+1108   BPM1205     [PM2000] 1874865 + [PM2000] 1874770.                                    Gvr2010 
19374+1532   BPM1207     [PM2000] 1875498 + [PM2000] 1876376.                                    Gvr2010 
19374+1239   BPM1206     [PM2000] 1875489 + [PM2000] 1874397.                                    Gvr2010 
19375+4619   PNT   1     Inadvertently observed for 19374+4619 HJ 1427AB, due to incorrect               
                         precise coordinates in the WDS.                                         Pnt2014a
19375+1451   BPM1208     [PM2000] 1876517 + [PM2000] 1876384.                                    Gvr2010 
19375+1236   BPM1209     [PM2000] 1876535 + [PM2000] 1875882.                                    Gvr2010 
19375+1158   BPM1211     [PM2000] 1876977 + [PM2000] 1876562.                                    Gvr2010 
19375+1126   BPM1210     [PM2000] 1876848 + [PM2000] 1877200.                                    Gvr2010 
19376+1357   BPM1213     [PM2000] 1878242 + [PM2000] 1878433.                                    Gvr2010 
19376+1330   BPM1212     [PM2000] 1877422 + [PM2000] 1876300.                                    Gvr2010 
19377+4645   DEA 389     JKA  69. KIC 9897318/9897328.                                                   
19377+1422   BRT1321     J 2596.                                                                         
19377+1355   BPM1214     [PM2000] 1879059 + [PM2000] 1878837.                                    Gvr2010 
19377+1141   BPMA129     [PM2000] 1878929 + [PM2000] 1879716.                                    Gvr2010 
19377-0958   LV   21     BC: J 1679.                                                                     
19378+3823   KOI 121     AC: Adams et al. (2012) theta values corrected to 360-theta.            Adm2012 
                         (reported by Dressing et al. (2014).                                    Dre2014 
19378+1314   BPMA130     [PM2000] 1880362 + [PM2000] 1881958.                                    Gvr2010 
19378+1225   BPM1216     [PM2000] 1879782 + [PM2000] 1880512.                                    Gvr2010 
19378+1149   BPM1215     [PM2000] 1879734 + [PM2000] 1879899.                                    Gvr2010 
19378+1102   BPM1217     AB: [PM2000] 1880095 + [PM2000] 1880247.                                Gvr2010 
             BPM1218     BC: [PM2000] 1881002 + [PM2000] 1880247.                                Gvr2010 
19379+4917   HJ 1428     Same as STF2559.                                                                
                         AB: 1951.524 : In Hipparcos Catalog, B component is HIP 96569: there            
                         is no such star in the position of HIP 96569 in DSS plates. So, the             
                         measurement of 1991 (realized from Hipparcos) and included in WDS               
                         database probably is not valid. B magnitude uncertain.                          
                         1991.521: proper motion of B is DEC 0"012+-0"004 and AR  0"014+-0"009.          
                         AC: 1991.521: Annual proper motion  of C is DEC -0"004 and AR -0"0010           
                         (in Tycho catalog: DEC -0"003 and AR -0"0004).                                  
                         BD: 1951.524: WDS indicates data for C and D components.                        
                         No star is near C coordinates. Realized measure for B and D components          
                         are very coincident with data for CD indicated in WDS. In WDS where             
                         say components CD, possibly it is BD.                                   FMR1999f
19379+1609   BPM1220     [PM2000] 1880565 + [PM2000] 1879112.                                    Gvr2010 
19379+1104   BPM1219     [PM2000] 1880605 + [PM2000] 1880949.                                    Gvr2010 
19380+3354   STT 379     Apparently an identification error dating back at least as far as the           
                         BDS led to an erroneous WDS designation. Burnham's 1880 coordinates     Bu_1906 
                         correspond to the star HIP 96576 = BD+33 3529. However, no pairs in             
                         the STT 379 system match other stars in that vicinity. The correct              
                         primary is instead HD 185582 = BD+33 3533. The WDS designation has not          
                         been changed, however, since the old ID has been in the literature for          
                         so long.                                                                        
19380+3353   YSC 135     Pair may have a period of less than one year; [Fe/H] = -0.28, spectral          
                         type G5, parallax 31.29 +/- 0.47 mas.                                   Hor2012b
19380+1428   BPM1222     AB: [PM2000] 1881727 + [PM2000] 1881148.                                Gvr2010 
             BPM1223     AC: [PM2000] 1881727 + [PM2000] 1882783.                                Gvr2010 
             BPM1224     BD: [PM2000] 1881148 + [PM2000] 1881734.                                Gvr2010 
             BPM1225     CD: [PM2000] 1882783 + [PM2000] 1881734.                                Gvr2010 
19380+1402   BPMA131     [PM2000] 1882201 + [PM2000] 1880248.                                    Gvr2010 
19380+1242   BPM1226     [PM2000] 1881816 + [PM2000] 1881238.                                    Gvr2010 
19380+1220   BPM1221     [PM2000] 1881638 + [PM2000] 1880660.                                    Gvr2010 
19380+1131   BPM1227     [PM2000] 1882533 + [PM2000] 1882410.                                    Gvr2010 
19381+4409   DEA 421     JKA  70. KIC 8241074/8241071.                                                   
19381+1623   BPM1228     [PM2000] 1883048 + [PM2000] 1883107.                                    Gvr2010 
19382+1300   BPM1230     [PM2000] 1883992 + [PM2000] 1882710.                                    Gvr2010 
19382+1255   BPM1229     [PM2000] 1883709 + [PM2000] 1882605.                                    Gvr2010 
19382+1141   BPM1231     [PM2000] 1884105 + [PM2000] 1883621.                                    Gvr2010 
19384+1236   BPM1232     [PM2000] 1885784 + [PM2000] 1886138.                                    Gvr2010 
19384+1225   BPM1233     [PM2000] 1885939 + [PM2000] 1886588.                                    Gvr2010 
19384+0022   WAK  22     NE of ADS 12708.                                                                
19385+3812   STN  47     Burnham could find no such pair in the vicinity.                        Bu_1906 
19385+1715   BU 1471     J 139.                                                                          
19385+1626   BPM1234     [PM2000] 1887456 + [PM2000] 1887085.                                    Gvr2010 
19386+2455   POU3973     POU3976.                                                                        
             POU3974     POU3977.                                                                        
19386+1428   BPM1236     [PM2000] 1888427 + [PM2000] 1889435.                                    Gvr2010 
19386+1130   BPM1235     [PM2000] 1888397 + [PM2000] 1889326.                                    Gvr2010 
19387+5458   CIA  13     V1143 Cyg.                                                                      
                         Mass (\msun)   : A = 1.361 +/- 0.004; B = 1.332 +/- 0.004.              CIA2019c
                         Radius (\rsun) : A = 1.348 +/- 0.016; B = 1.322 +/- 0.016.                      
                         Teff (deg K)   : A =  6620 +/- 190  ; B =  6570 +/- 220.                        
                         Lum. (\lsun)   : A =  3.35 +/- 0.44 ; B =  3.13 +/- 0.50.                       
                         Semimajor axis = 22.71 +/- 0.03 \rsun. parallax = 41.02 +/- 0.22 pc.            
19387+1552   BPMA132     [PM2000] 1889635 + [PM2000] 1889186.                                    Gvr2010 
19387+1534   BPM1238     [PM2000] 1889780 + [PM2000] 1889127.                                    Gvr2010 
19387+1042   BPM1237     [PM2000] 1889354 + [PM2000] 1889251.                                    Gvr2010 
19387-1009   STF2545     AB: H 1  13.                                                            MEv2010 
19388+1705   BPM1241     [PM2000] 1890365 + [PM2000] 1890596.                                    Gvr2010 
19388+1311   BPM1240     [PM2000] 1890102 + [PM2000] 1889346.                                    Gvr2010 
19388+1219   BPM1239     [PM2000] 1889925 + [PM2000] 1890382.                                    Gvr2010 
19389+5049   DEA 392     JKA  71. KIC 12214504/12214492.                                                 
19389+3512   LDS6336     NLTT 48072/48073                                                        Chm2004 
19389+1626   OSO 110     G142-044. AC, AD, AE, AF, and AH are not common proper motion pairs,            
                         based on comparison with POSS2 red plates                               Oso2004 
19389+1610   BPM1246     [PM2000] 1891493 + [PM2000] 1892540.                                    Gvr2010 
19389+1601   BPM1242     [PM2000] 1891033 + [PM2000] 1891921.                                    Gvr2010 
19389+1250   BPM1244     AB: [PM2000] 1891430 + [PM2000] 1891174.                                Gvr2010 
             BPM1245     BC: [PM2000] 1891174 + [PM2000] 1889909.                                Gvr2010 
19389+1159   BPM1243     [PM2000] 1891081 + [PM2000] 1889913.                                    Gvr2010 
19389+0340   J  1853     Heintz states that this is probably 19384+0414J  1682.                  Hei1995 
19389-1020   STF2547     B is BD-10@5142.                                                                
19390+1708   BPM1248     [PM2000] 1892002 + [PM2000] 1891936.                                    Gvr2010 
19390+1152   BPM1249     [PM2000] 1892685 + [PM2000] 1891603.                                    Gvr2010 
19390+1138   BPM1247     [PM2000] 1891907 + [PM2000] 1892018.                                    Gvr2010 
19391+7625   MLR 224     Combined spectroscopic/interferometric orbit by Balega et al. (2007),   Bag2007 
                         yielding a distance of 32.23 +/- 0.52 pc, or an orbital parallax of             
                         31.0 +/- 0.5 mas.  Derived masses are 0.831 +/- 0.020 and 0.763 +/-             
                         0.019 Msun, luminosities 0.40 +/- 0.02 and 0.26 +/- 0.02 Lsun, and              
                         spectral types K1V and K3V.                                                     
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.24 +/- 0.07, 1.60, and 0.85 Msun, respectively.             Mlk2012 
                         Mass = 0.8216 +/- 0.0037, 0.7491  +/- 0.0022  \msun for A and B.        HJL2020 
                         orbital parallax = 31.26  +/- 0.11  mas.                                        
19391+1345   BPM1250     [PM2000] 1893051 + [PM2000] 1893907.                                    Gvr2010 
19392+1349   BPM1251     [PM2000] 1894115 + [PM2000] 1894531.                                    Gvr2010 
19392+0524   HJ 2886     sig Aql = 44 Aql. A is a Beta Lyrae-type system, spectrum composite.            
                         Spectrum of B G8V.                                                              
19393+1340   BPM1253     [PM2000] 1895356 + [PM2000] 1895060.                                    Gvr2010 
19393+1306   BPM1252     [PM2000] 1894927 + [PM2000] 1895695.                                    Gvr2010 
19394+3009   MCA  57     phi Cyg = 12 Cyg. A double-lined spectroscopic binary now resolved by           
                         speckle interferometry.                                                         
                         Analysis of the spectroscopic/interferometric orbit is given by                 
                         McAlister (1982).                                                       McA1982a
                         1980.7173: Theta and rho were incorrectly given as 77.1 degrees and             
                         0".036, respectively, by McAlister et al. (1983).                       McA1983 
                         P for Armstrong (1992) solution adopted from spectroscopic orbit of     MkT1992d
                         Rach & Herbig (1961). Spectroscopic orbit combined with astrometry              
                         from Mark III to derive distance, masses, absolute magnitudes.                  
                         Data from the Mark III interferometer were combined by Armstrong et.    MkT1992c
                         with a reinterpretation of the Rach & Herbig spectroscopic solution to  Her1961 
                         determine distance, masses, and absolute magnitudes for this pair of            
                         giants. Evolutionary history is discussed. Errors for Mark III                  
                         astrometry are given as "error ellipses"; these values are tabulated            
                         below. Columns include date (BY), major and minor axes of the ellipse           
                         (in mas), and ellipse orientation (in degrees).                                 
                              1989.4053     3.6      0.14     100.5                                      
                              1989.5312     4.8      0.76      81.6                                      
                              1989.6022    10.8      0.64      81.3                                      
                              1989.6050     5.8      0.43      77.1                                      
                              1989.6160     1.04     0.16      74.8                                      
                              1989.6242     1.15     0.117     75.5                                      
                              1989.6351     1.58     0.159     75.2                                      
                              1989.6812     0.45     0.049     92.3                                      
                              1989.6867     2.65     0.31      84.5                                      
                              1989.6894     1.47     0.137     85.7                                      
                              1989.7031     5.5      0.6       85.0                                      
                              1989.7852     6.1      0.44      76.8                                      
                              1989.7962     4.8      0.35      70.9                                      
                              1990.4758     2.3      0.19      85.5                                      
                              1990.4839     1.68     0.39      91.1                                      
                              1990.5111     0.135    0.041    112.4                                      
                              1990.5139     0.181    0.046     94.8                                      
                              1990.5167     0.40     0.114     93.3                                      
                              1990.5195     0.29     0.079     86.9                                      
                              1990.5304     0.109    0.040     87.6                                      
                              1990.5359     0.116    0.038     89.2                                      
                              1990.5388     0.55     0.067     76.1                                      
                              1990.5687     0.25     0.055     85.7                                      
                              1990.5714     0.141    0.042     84.1                                      
                              1990.5741     0.28     0.069     93.8                                      
                              1990.5768     0.178    0.061     96.5                                      
                              1990.5822     0.29     0.064     97.0                                      
                              1990.5931     2.2      0.36      95.3                                      
                              1990.6099     0.63     0.116     69.5                                      
                              1990.6260     0.40     0.091     93.0                                      
                              1990.6343     0.96     0.121     82.1                                      
                              1990.6371     1.17     0.23      76.7                                      
                              1990.6452     0.158    0.028     80.3                                      
                              1990.6535     0.42     0.034     75.3                                      
                              1990.8255     1.03     0.079     72.4                                      
                              1991.4696     0.71     0.120    100.4                                      
                              1991.5490     0.25     0.044     80.6                                      
                              1991.5870     0.23     0.051     95.8                                      
                              1991.5898     0.25     0.038     91.9                                      
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Armstrong et al. (1992).                                                MkT1992c
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 7.49 +/- 0.77, 3.75, and 1.78 Msun, respectively.             Mlk2012 
19394+1634   H N  84     B is BD+16@3935.                                                                
                         BDS 9484, H 5 51 same star. A is a spectroscopic binary.                        
19394+1340   BPM1254     [PM2000] 1896365 + [PM2000] 1897368.                                    Gvr2010 
19394+1201   BPM1255     AB: [PM2000] 1896841 + [PM2000] 1896870.                                Gvr2010 
             BPM1256     AC: [PM2000] 1896841 + [PM2000] 1896872.                                Gvr2010 
             BPM1257     BC: [PM2000] 1896870 + [PM2000] 1896872.                                Gvr2010 
19395+4647   KOI2803     This system hosts a 0.5 Rearth planet candidate with a 2.4 day period   KOI2014a
                         (Burke et al. 2014).                                                    Dre2014 
19395+4138   FOX  29     J  3216.                                                                Nsn2016 
19395+1306   BPM1258     [PM2000] 1896883 + [PM2000] 1897335.                                    Gvr2010 
19395+1124   BPM1261     [PM2000] 1897864 + [PM2000] 1898306.                                    Gvr2010 
19395+1040   BPM1260     [PM2000] 1897829 + [PM2000] 1897567.                                    Gvr2010 
19395+1034   BPM1259     [PM2000] 1897284 + [PM2000] 1896456.                                    Gvr2010 
19396+1800   BPM1263     [PM2000] 1898844 + [PM2000] 1898094.                                    Gvr2010 
19396+1605   BPM1262     [PM2000] 1898021 + [PM2000] 1897264.                                    Gvr2010 
19396+1132   BPMA133     [PM2000] 1897939 + [PM2000] 1897673.                                    Gvr2010 
19397+1542   BPM1264     [PM2000] 1899197 + [PM2000] 1899297.                                    Gvr2010 
19397+1305   BPM1265     [PM2000] 1899354 + [PM2000] 1898922.                                    Gvr2010 
19398+1945   HJ  894     J 1857.                                                                         
19398+1751   BPM1267     [PM2000] 1900830 + [PM2000] 1901586.                                    Gvr2010 
19398+1128   BPM1266     [PM2000] 1900471 + [PM2000] 1900953.                                    Gvr2010 
19398-2326   SEE 389     53 Sgr. Spectrum composite; B9.5V+A3IV.                                         
                         Baize's (1985) value for omega was corrected from 270.0 to 90.0         Baz1985b
                         90.0 degrees by Ruymaekers & Nys (1995).                                Ruy1995 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.88 +/- 1.02, 3.55, and 2.24 Msun, respectively.             Mlk2012 
19399+2402   FYM9002     Designated by author as FYM 204, homever 00129+6150 also designated by  FyM2014 
                         author as FYM 184. Redesignated.                                        FyM2014c
19399+1320   BPMA134     [PM2000] 1901913 + [PM2000] 1902242.                                    Gvr2010 
19399-1451   HO  109     BDS 9497. HDO 154 is probably identical.                                        
19399-2204   I   656     Measures uncertain, too close. Another pair near this place: 64.7@,             
                         7.54". No magnitudes given.                                                     
19399-3926   GAA  10     V4090 Sgr.                                                                      
                         Ma,Mb = 2.15   +/- 0.07  , 1.11   +/- 0.02   \msun,                     GaA2019 
                         orbital parallax = 10.845 +/- 0.083 mas.                                        
19400+1605   BPM1268     [PM2000] 1902278 + [PM2000] 1901032.                                    Gvr2010 
19400+1542   BPM1269     [PM2000] 1902603 + [PM2000] 1902219.                                    Gvr2010 
19400+1331   BPM1270     [PM2000] 1903005 + [PM2000] 1902156.                                    Gvr2010 
19401+3037   J   776     GCB 46.                                                                 J__1952 
19401+1801   J   121     alp Sge = 5 Sge = Sham                                                          
19401+1612   BPM1273     [PM2000] 1903951 + [PM2000] 1903338.                                    Gvr2010 
19401+1424   BPM1271     [PM2000] 1903680 + [PM2000] 1904784.                                    Gvr2010 
19401+1323   BPM1272     [PM2000] 1903854 + [PM2000] 1903826.                                    Gvr2010 
19401-0759   HIP  96754  This SB2 with mass ration 0.882 is apparently too close for resolution          
                         with NICI.                                                              Tok2013b
19402+6030   STF2573     B is BD+60@1992.                                                                
19402+1609   BPMA135     [PM2000] 1905115 + [PM2000] 1903853.                                    Gvr2010 
19402+1605   BPM1276     [PM2000] 1904943 + [PM2000] 1905379.                                    Gvr2010 
19402+1400   BPM1275     [PM2000] 1904680 + [PM2000] 1903673.                                    Gvr2010 
19402+1236   BPM1274     [PM2000] 1904646 + [PM2000] 1904611.                                    Gvr2010 
19403+1758   BPM1281     [PM2000] 1905528 + [PM2000] 1904159.                                    Gvr2010 
19403+1540   BPM1280     [PM2000] 1906222 + [PM2000] 1907344.                                    Gvr2010 
19403+1340   BPM1277     [PM2000] 1905296 + [PM2000] 1905179.                                    Gvr2010 
19403+1240   BPM1278     AB: [PM2000] 1905465 + [PM2000] 1906076.                                Gvr2010 
             BPM1279     BC: [PM2000] 1906076 + [PM2000] 1906320.                                Gvr2010 
19403+1224   BPM1282     [PM2000] 1906348 + [PM2000] 1905434.                                    Gvr2010 
19403-6959   NZO  98     Aka TDS1005.                                                                    
19404+3441   ES 2242     Aka TDT1620.                                                                    
19404+1613   BPM1287     [PM2000] 1907290 + [PM2000] 1906312.                                    Gvr2010 
19404+1527   BPM1285     [PM2000] 1907083 + [PM2000] 1906330.                                    Gvr2010 
19404+1404   BPM1288     [PM2000] 1907293 + [PM2000] 1906295.                                    Gvr2010 
19404+1341   BPM1284     [PM2000] 1906663 + [PM2000] 1907116.                                    Gvr2010 
19404+1303   BPM1283     [PM2000] 1906520 + [PM2000] 1905570.                                    Gvr2010 
19404+1106   BPM1286     [PM2000] 1907169 + [PM2000] 1905636.                                    Gvr2010 
19406+1737   BPM1289     [PM2000] 1908776 + [PM2000] 1907834.                                    Gvr2010 
19406+1504   BPM1297     [PM2000] 1909826 + [PM2000] 1909725.                                    Gvr2010 
19406+1355   BPM1290     AB: [PM2000] 1908990 + [PM2000] 1908938.                                Gvr2010 
             BPM1291     BC: [PM2000] 1908938 + [PM2000] 1909549.                                Gvr2010 
             BPM1292     BD: [PM2000] 1908938 + [PM2000] 1908580.                                Gvr2010 
             BPM1293     CD: [PM2000] 1909549 + [PM2000] 1908580.                                Gvr2010 
             BPM1294     DE: [PM2000] 1908580 + [PM2000] 1907481.                                Gvr2010 
19406+1325   BPM1295     AB: [PM2000] 1909319 + [PM2000] 1909601.                                Gvr2010 
             BPM1296     BD: [PM2000] 1909601 + [PM2000] 1910484.                                Gvr2010 
19407+4305   CHR 260     Hipparcos suspected non-single.                                                 
19407+2343   STF2560     C is a spectroscopic binary.                                                    
19407+1544   BPMA136     [PM2000] 1909931 + [PM2000] 1909790.                                    Gvr2010 
19407+1352   BPM1298     [PM2000] 1910783 + [PM2000] 1910915.                                    Gvr2010 
19407+1328   BPM1299     AB: [PM2000] 1910972 + [PM2000] 1909582.                                Gvr2010 
             BPM1300     AC: [PM2000] 1910972 + [PM2000] 1910384.                                Gvr2010 
19407-0037   CHR  88     45 Aql.                                                                         
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 1.88 +/- 0.45, 3.34, and 2.09 Msun, respectively.  Mlk2012 
19407-1618   HJ  599     54 Sgr = e 1 Sag. Variable, and A is an occultation double.                     
19408+1802   BPM1303     [PM2000] 1911830 + [PM2000] 1910621.                                    Gvr2010 
19408+1325   BPM1301     [PM2000] 1911012 + [PM2000] 1911945.                                    Gvr2010 
19408+1319   BPM1302     [PM2000] 1911324 + [PM2000] 1912141.                                    Gvr2010 
19408+1226   BPM1304     [PM2000] 1911955 + [PM2000] 1910576.                                    Gvr2010 
19408+0913   GCB  45     J 1855.                                                                         
19409+5034   KOI 623     AB: JKA  72. KIC 12068975/12068971.                                             
19409+1818   BPM1305     [PM2000] 1912390 + [PM2000] 1911261.                                    Gvr2010 
19409+1521   BPM1307     [PM2000] 1913173 + [PM2000] 1913884.                                    Gvr2010 
19409+1442   BPM1308     [PM2000] 1913399 + [PM2000] 1914913.                                    Gvr2010 
19409+1217   BPM1306     [PM2000] 1912657 + [PM2000] 1913028.                                    Gvr2010 
19409-0152   TOK 424     HIP 96834 has a spectroscopic orbit with a period of 1yr and expected           
                         semi-major axis of 27mas (Latham 2012, private communication). We               
                         resolved this pair, although the measurement near the diffraction               
                         limit is uncertain. There are some unsolved questions, however. Why,            
                         despite the small magnitude difference dy = 1.2 mag, were double lines          
                         not seen? Why, despite the 1-yr period, was the Hipparcos parallax not          
                         strongly affected and the star appears to be on the main sequence?      Tok2015c
19410+3237   BLL  41     A is the semiregular variable TT Cyg.                                           
19411+1601   BPM1312     [PM2000] 1914844 + [PM2000] 1916003.                                    Gvr2010 
19411+1506   BPM1311     [PM2000] 1914833 + [PM2000] 1914377.                                    Gvr2010 
19411+1359   BPM1313     [PM2000] 1915385 + [PM2000] 1916848.                                    Gvr2010 
19411+1349   KUI  93     A is the Algol-type system QS Aql.                                              
                         1980.7256: This measure was incorrectly attributed to ADS 12973 by              
                         McAlister et al. (1983)                                                 McA1983 
                         Light curve and radial velocity combined solution determined.           Zas2017 
19411+1301   BPM1309     [PM2000] 1914768 + [PM2000] 1915494.                                    Gvr2010 
19411+1207   BPM1310     [PM2000] 1914779 + [PM2000] 1915678.                                    Gvr2010 
19412+1345   BPM1315     [PM2000] 1916483 + [PM2000] 1916167.                                    Gvr2010 
19412+1251   BPM1317     [PM2000] 1916987 + [PM2000] 1916093.                                    Gvr2010 
19412+1248   BPM1314     [PM2000] 1916411 + [PM2000] 1915456.                                    Gvr2010 
19412+1222   BPM1316     [PM2000] 1916586 + [PM2000] 1916630.                                    Gvr2010 
19413+1756   BPM1320     [PM2000] 1917464 + [PM2000] 1918244.                                    Gvr2010 
19413+1703   BPM1318     [PM2000] 1917200 + [PM2000] 1916920.                                    Gvr2010 
19413+1435   BPM1319     [PM2000] 1917363 + [PM2000] 1918671.                                    Gvr2010 
19413+1418   BPM1321     [PM2000] 1917892 + [PM2000] 1918626.                                    Gvr2010 
19413-0128   BAL 605     J 1683.                                                                         
19414+4851   KOI2813     This system hosts a 1.2 Rearth planet candidate with a 0.7 day period           
                         (Burke et al. 2014). We detected a companion 1.43 J mags and 1.82 Ks    KOI2014a
                         mags fainter than KOI2813 at a separation of 1".04. The predicted Kp            
                         mag of the companion is Kp = 14.8 (dKp = 1.3). In the simple                    
                         approximation in which all of the light from the companion star is              
                         captured in the Kepler aperture and the companion orbits the target             
                         star, then the estimated planet radius should be increased by 15% to            
                         correct for the extra light in the aperture. KOI2813 does not exhibit           
                         a significant source offset during transit.                             Dre2014 
19415+3903   KOI2904     This system hosts a 1.2 Rearth planet with a 16.4 day period (Burke et  KOI2014a
                         al 2014). We detected a companion 2.74 J mags and 2.58 Ks mags fainter          
                         than KOI2904 at a separation of 0".68. Using the J-Ks to Kp-Ks color-           
                         color conversion from Howell et al. (2012), we predict that the Kp mag  KOI2012a
                         of the companion is Kp = 15.8 (dKp = 3.1) if the star is a dwarf or             
                         Kp = 15.9 (dKp = 3.2) if the star is a giant. KOI 2904 has also been            
                         observed with speckle imaging using DSSI on WIYN and the companion was          
                         detected with mag differences of 2.83 mag at 692 nm and 2.77 mag at             
                         880 nm. The estimated dilution correction for this system is 3%                 
                         assuming that the planet orbits the target star and that all of the             
                         light from the companion is captured in the Kepler aperture. KOI2904            
                         does not display a significant source offset during transit.            Dre2014 
19415+1710   BPM1323     AB: [PM2000] 1919997 + [PM2000] 1919774.                                Gvr2010 
             BPM1324     BC: [PM2000] 1919774 + [PM2000] 1919188.                                Gvr2010 
19415+1224   BPM1325     [PM2000] 1920381 + [PM2000] 1920714.                                    Gvr2010 
19415+1123   BPM1322     [PM2000] 1919737 + [PM2000] 1919246.                                    Gvr2010 
19416+4259   KOI 266     This system contains a 1.6 Rearth planet candidate with a 25.3 day              
                         period and a second 1.8 Rearth planet candidate with a 47.7 day period          
                         (Burke et al. 2014). It was classified by Slawson et al. (2011) as a    KOI2014a
                         detached eclipsing binary with a period of 25.3 days, suggesting that   KOI2011a
                         the 1.6 Rearth planet candidate with the same period might not                  
                         actually be a planet. Instead, the observed decrease in flux every              
                         25.3 days might be an eclipsing binary diluted by the light of a                
                         nearby star.                                                            Dre2014 
19416+1639   BPM1327     [PM2000] 1921007 + [PM2000] 1920802.                                    Gvr2010 
19416+1602   BPM1326     [PM2000] 1920985 + [PM2000] 1922164.                                    Gvr2010 
19416+1433   BPM1328     AB: [PM2000] 1921223 + [PM2000] 1919726.                                Gvr2010 
             BPM1329     AC: [PM2000] 1921223 + [PM2000] 1922428.                                Gvr2010 
19417+1727   BPM1331     [PM2000] 1923043 + [PM2000] 1923561.                                    Gvr2010 
19417+1505   BPMA137     [PM2000] 1923300 + [PM2000] 1926016.                                    Gvr2010 
19417+1136   BPM1330     [PM2000] 1922222 + [PM2000] 1922572.                                    Gvr2010 
19418+5032   STFA 46     STTA189.                                                                        
                         AB: A is 16 Cyg. B is BD+50@2848. A premature orbit has been computed.          
                         Statistically the same parallax within the errors would indicate the            
                         components are physical.                                                        
                         A family of possible orbital solutions are determined by Romanenko      Rmn1994 
                         (1994), with periods ranging from 124,000 to 451,000 years, using the           
                         method of apparent  motion parameters and incorporating parallax and            
                         radial velocity  information.                                                   
                         Based on combined astrometry, velocity information, and Hipparcos               
                         parallax, Hauser & Marcy (1999) determine a family of possible orbits,  Mrc1999 
                         with periods ranging from 18,200 yr to 1.3 Myr, depending on the                
                         line-of-sight separation between the components. A second family of             
                         possible orbits are determined assuming the C component is physical             
                         with the system.                                                                
                         AB: HJL 266.                                                            HJL1986 
                         AB: SHY  95. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AB: H 5  46.                                                            MEv2010 
                         AB: Kiselev & Romanenko (2011) generate another set of possible         PkO2011 
                         solutions, based in part on photographic measures obtained at Pulkova           
                         Observatory from 1960 to 2007. Periods range from 209 - 290 centuries.          
                         Based on predicted mass sums from these various orbital elements, the           
                         135-century solution of Hauser & Marcy (1999) appears at present to     Mrc1999 
                         give the most realistic results.                                                
                         AB: B has a planet P=2.19y.                                             Tok2014d
                         Asteroseismology from the Kepler data yields for Component A:           KOI2015 
                         R = 1.229+/-0.008 Rsun, 1.08+/-0.02 Msun L = 1.55+/-0.07 Lsun,                  
                         t = 7.07+/-0.26 Gyr, Z = 0.021+/-0.002 Yi = 0.25+/-0.01 and                     
                         log g = 4.292+/-0.03.                        For Component B:                   
                         R = 1.116+/-0.006 Rsun, 1.04+/-0.02 Msun L = 1.25+/-0.05 Lsun,                  
                         t = 6.74+/-0.24 Gyr, Z = 0.022+/-0.003 Yi = 0.26+/-0.01 and                     
                         log g = 4.359+/-0.02.                                                           
                         CHARA Array Limb-darkened diameter of B  0.426 +/- 0.056 mas,           CIA2008c
                         R =  0.98  +/- 0.13  \rsun.                                                     
                         CHARA Array Limb-darkened diameter of A,B :                             CIA2013c
                         R =  1.2551 +/- 0.0261, 1.1689 +/- 0.0274 \rsun,                                
                         L =  1.5572 +/- 0.0179, 1.2768 +/- 0.0148 \lsun,                                
                         Teff = 5760 +/-  57, 5678 +/-  66 K, M = 1.032, 0.989 \msun,                    
                         Age = 7.9, 8.9 Gyr.                                                             
                         Using inversion techniques, a mass of 0.98+/-0.02 Msun, radius of       Blg2016 
                         1.194+/-0.06 Rsun and age of 7.2+/-0.2 Gy for 16 Cyg A and for 16 Cyg B         
                         0.945+/-0.015 Msun and 1.09+/-0.01 Rsun                                         
                         Astroseismology results for the masses 1.07 +/- 0.02, 1.05 +/- 0.02     XXX2020h
                         \msun for A, B, respectively, and an age of 6.88 +/- 0.12 Gyr for the           
                         system.                                                                         
19418+4252   KOI2516     The system hosts a 1.2 Rearth planet candidate with a 2.8 day orbit     KOI2013a
                         (Batalha et al. 2013).                                                  Dre2014 
19418+1808   BPM1332     [PM2000] 1923345 + [PM2000] 1922013.                                    Gvr2010 
19418+1626   BPM1333     [PM2000] 1923392 + [PM2000] 1923646.                                    Gvr2010 
19418+1456   BPM1334     [PM2000] 1923508 + [PM2000] 1925184.                                    Gvr2010 
19418+1409   BPMA138     AB: [PM2000] 1923536 + [PM2000] 1923988.                                Gvr2010 
             BPMA139     AC: [PM2000] 1923536 + [PM2000] 1922370.                                Gvr2010 
             BPMA140     BC: [PM2000] 1923988 + [PM2000] 1922370.                                Gvr2010 
19419+5031   16 Cyg B    Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from Cochran      CPS1997a
                         et al. (1997).                                                          HaI2001 
19419+1507   BPM1335     [PM2000] 1924986 + [PM2000] 1924313.                                    Gvr2010 
19419+1420   BPM1336     [PM2000] 1925767 + [PM2000] 1926609.                                    Gvr2010 
19419-1117   RST4638     BRT 2764.                                                                       
19420+5201   ES  794     B is BD+51@2662.                                                                
19420+4015   KUI  94     Apastron poorly covered. Malkov et al. derive dynamical, photometric,           
                         and spectroscopic masses of 3.42 +/- 1.86, 3.29, and 1.74 Msun,                 
                         respectively.                                                           Mlk2012 
19420+1807   BPM1337     AB: [PM2000] 1926835 + [PM2000] 1925978.                                Gvr2010 
             BPM1338     BC: [PM2000] 1925978 + [PM2000] 1927618.                                Gvr2010 
19420+1710   BPMA141     [PM2000] 1925876 + [PM2000] 1924736.                                    Gvr2010 
19420+1409   BPM1340     [PM2000] 1926118 + [PM2000] 1925270.                                    Gvr2010 
19420+1330   BPM1339     [PM2000] 1926199 + [PM2000] 1926512.                                    Gvr2010 
19421+1731   BPM1347     [PM2000] 1927847 + [PM2000] 1929098.                                    Gvr2010 
19421+1408   BPM1344     AB: [PM2000] 1927719 + [PM2000] 1928033.                                Gvr2010 
             BPM1345     BC: [PM2000] 1928033 + [PM2000] 1928518.                                Gvr2010 
19421+1347   BPM1343     [PM2000] 1927532 + [PM2000] 1927131.                                    Gvr2010 
19421+1340   BPM1342     [PM2000] 1927331 + [PM2000] 1928662.                                    Gvr2010 
19421+1201   BPM1341     [PM2000] 1927203 + [PM2000] 1926235.                                    Gvr2010 
19422+1659   BPM1348     [PM2000] 1929484 + [PM2000] 1929324.                                    Gvr2010 
19422+1531   BPM1346     [PM2000] 1928389 + [PM2000] 1928098.                                    Gvr2010 
19422-1015   RST4639     TDT1656.                                                                        
19423+1744   BPM1352     [PM2000] 1930524 + [PM2000] 1932041.                                    Gvr2010 
19423+1559   BPM1349     [PM2000] 1930010 + [PM2000] 1929961.                                    Gvr2010 
19423+1546   BPM1354     [PM2000] 1930844 + [PM2000] 1930338.                                    Gvr2010 
19423+1346   BPM1353     [PM2000] 1930584 + [PM2000] 1930361.                                    Gvr2010 
19423+1253   BPM1350     [PM2000] 1930081 + [PM2000] 1930140.                                    Gvr2010 
19423+1029   BPM1351     [PM2000] 1930124 + [PM2000] 1930819.                                    Gvr2010 
19424+1753   BPM1356     [PM2000] 1931281 + [PM2000] 1930731.                                    Gvr2010 
19424+1550   BPM1355     [PM2000] 1931052 + [PM2000] 1929391.                                    Gvr2010 
19424+1413   BPM1357     [PM2000] 1931352 + [PM2000] 1932904.                                    Gvr2010 
19424+1313   BPMA142     [PM2000] 1931279 + [PM2000] 1930226.                                    Gvr2010 
19425+3337   J   777     TDT1659.                                                                        
19425+1823   BPM1360     [PM2000] 1932880 + [PM2000] 1932305.                                    Gvr2010 
19425+1813   BPM1359     [PM2000] 1932679 + [PM2000] 1934111.                                    Gvr2010 
19425+1726   STF2563     C is BD+17@4054a.                                                               
                         AB: HJL 265.                                                            HJL1986 
                         AB: H 1  65.                                                            MEv2010 
19425+1332   BPM1358     [PM2000] 1932497 + [PM2000] 1931158.                                    Gvr2010 
19425+1243   BPMA143     [PM2000] 1933088 + [PM2000] 1930040.                                    Gvr2010 
19425+0809   OSO 111     G092-023. Neither is a common proper motion pair, based on color                
                         and/or comparison with POSS2 red plates                                 Oso2004 
19425-1607   BU 1288     55 Sgr = e 2 Sgr                                                                
19426+4002   BUP 196     B is BD+39@3882.                                                                
19426+1710   BPM1363     [PM2000] 1934084 + [PM2000] 1933862.                                    Gvr2010 
19426+1350   BPM1364     [PM2000] 1934291 + [PM2000] 1934914.                                    Gvr2010 
19426+1243   BPM1365     [PM2000] 1934786 + [PM2000] 1933789.                                    Gvr2010 
19426+1235   BPM1361     [PM2000] 1933576 + [PM2000] 1934205.                                    Gvr2010 
19426+1150   STT 380     chi Aql = 47 Aql. A spectroscopic binary.                                       
                         1998.657: Absolute quadrant determined by triple-correlation technique  Pru2002b
19426+1133   BPM1362     [PM2000] 1933886 + [PM2000] 1933148.                                    Gvr2010 
19427+1809   BPMA144     AB: [PM2000] 1935722 + [PM2000] 1931608.                                Gvr2010 
             BPMA145     BC: [PM2000] 1931608 + [PM2000] 1931524.                                Gvr2010 
19427+1719   BPMA146     [PM2000] 1935863 + [PM2000] 1938313.                                    Gvr2010 
19427+1718   BPM1366     [PM2000] 1935513 + [PM2000] 1935669.                                    Gvr2010 
19427+1633   BPM1368     [PM2000] 1935886 + [PM2000] 1936475.                                    Gvr2010 
19427+1242   BPM1367     [PM2000] 1935639 + [PM2000] 1936393.                                    Gvr2010 
19428+3741   STTA188     B is BD+37@3578.                                                                
                         There is a 13th mag star between A and B, 28.73" from A, 30.48" from B          
19428+1755   BPM1370     [PM2000] 1936744 + [PM2000] 1936815.                                    Gvr2010 
19428+1702   BPM1371     [PM2000] 1937083 + [PM2000] 1935558.                                    Gvr2010 
19428+1237   BPM1369     [PM2000] 1936427 + [PM2000] 1938191.                                    Gvr2010 
19428+0823   STF2562     AB: SHY 756. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
19428-1614   ALD  75     LEO 45.                                                                         
19429+1728   BPM1372     [PM2000] 1938533 + [PM2000] 1936865.                                    Gvr2010 
19429-4406   BRG  28     A close companion to 2MASS J19425324-4406278 is detected which is               
                         counted as a physical companion for statistical purposes, although              
                         this has not yet been demonstrated through common proper motion.        Jnn2012 
19430+3433   SEI 663     H 3 110a.                                                               MEv2010 
19430+1753   BPM1375     [PM2000] 1938839 + [PM2000] 1939664.                                    Gvr2010 
19430+1722   BPM1373     AB: [PM2000] 1939526 + [PM2000] 1939513.                                Gvr2010 
             BPM1374     BC: [PM2000] 1939513 + [PM2000] 1938582.                                Gvr2010 
19431+1435   BPM1377     [PM2000] 1941162 + [PM2000] 1940714.                                    Gvr2010 
19431+1324   BPM1376     [PM2000] 1940211 + [PM2000] 1941390.                                    Gvr2010 
19431-0818   STFA 45     B is BD-08@5079.                                                                
                         AB: SHY 757. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
             GC 27279    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
19432+4929   DEA 391     JKA  73. KIC 11515925/11515931.                                                 
19432+2701   BU 1132     The evidence suggests that there may be a question of identification.           
                         BD+26 3650 (5' s) is single (n=2)                                       Hei1963b
                         Pair probably incorrectly identified in ADS. Pair is BD+26 3651, not            
                         the single star BD+26 3650. Probably the negative observations of               
                         Van Biesbroeck and Voute were of the latter star.                       Cou1956 
19432+1559   BPM1378     [PM2000] 1941381 + [PM2000] 1940473.                                    Gvr2010 
19432+1402   BPMA147     [PM2000] 1941571 + [PM2000] 1944765.                                    Gvr2010 
19433+1648   BPMA148     [PM2000] 1943268 + [PM2000] 1945611.                                    Gvr2010 
19433+1638   BPM1381     [PM2000] 1943460 + [PM2000] 1943559.                                    Gvr2010 
19433+1507   BPM1380     [PM2000] 1943356 + [PM2000] 1942137.                                    Gvr2010 
19433+1452   BPM1382     AB: [PM2000] 1943825 + [PM2000] 1945268.                                Gvr2010 
             BPM1383     BC: [PM2000] 1945268 + [PM2000] 1944891.                                Gvr2010 
19434+3855   ES 1969     AC: SEI 672.                                                            Nsn2017b
19434+3158   AG  235     SEI 665.                                                                Nsn2017b
19434+1701   BPM1385     [PM2000] 1944353 + [PM2000] 1945737.                                    Gvr2010 
19434+1500   BPM1384     [PM2000] 1945067 + [PM2000] 1945278.                                    Gvr2010 
19434+1359   BPMA149     [PM2000] 1944225 + [PM2000] 1941724.                                    Gvr2010 
19434+0410   STT 381     Heintz believes this is identical with BAL2520.                         Hei1995 
19434-3722   BRG  29     Only one epoch of imaging exists for this binary system, hence common           
                         proper motion has not yet been confirmed. It is counted as an                   
                         unconfirmed binary here.                                                Jnn2012 
19435+3450   AG  236     AB: SEI 667.                                                            Nsn2017b
19435+3433   SEI 669     B is BD+34@3684.                                                                
                         H 3 110b.                                                               MEv2010 
19435+1752   BPM1389     [PM2000] 1946042 + [PM2000] 1945522.                                    Gvr2010 
19435+1439   BPMA150     [PM2000] 1945210 + [PM2000] 1944677.                                    Gvr2010 
19435+1337   BPM1386     [PM2000] 1945303 + [PM2000] 1946333.                                    Gvr2010 
19435+1312   BPM1387     AB: [PM2000] 1945537 + [PM2000] 1945682.                                Gvr2010 
             BPM1388     BC: [PM2000] 1945682 + [PM2000] 1946222.                                Gvr2010 
19435+1200   BPM1390     [PM2000] 1946355 + [PM2000] 1947704.                                    Gvr2010 
19435+1140   BPM1391     [PM2000] 1946387 + [PM2000] 1945936.                                    Gvr2010 
19436+1608   BPM1394     [PM2000] 1947383 + [PM2000] 1946868.                                    Gvr2010 
19436+1544   BPM1395     [PM2000] 1947390 + [PM2000] 1947362.                                    Gvr2010 
19436+1204   BPM1392     AB: [PM2000] 1946420 + [PM2000] 1947271.                                Gvr2010 
             BPM1393     AC: [PM2000] 1946420 + [PM2000] 1947637.                                Gvr2010 
19436-0904   HO  579     Includes V1461 Aql, an Algol-type eclipsing binary, P = 1.76306d.       Zas2012 
19437+1737   BPM1396     [PM2000] 1948278 + [PM2000] 1948500.                                    Gvr2010 
19437+1611   BPMA152     [PM2000] 1948374 + [PM2000] 1945016.                                    Gvr2010 
19437+1210   BPMA151     AB: [PM2000] 1948028 + [PM2000] 1944249.                                Gvr2010 
             BPM1379     BC: [PM2000] 1944249 + [PM2000] 1943070.                                Gvr2010 
19437+1146   BPM1407     [PM2000] 1948787 + [PM2000] 1949496.                                    Gvr2010 
19437-2908   LDS 685     NLTT 48140/48142                                                        Chm2004 
19438+1542   BPM1400     [PM2000] 1949007 + [PM2000] 1947609.                                    Gvr2010 
19438+1539   BPM1408     [PM2000] 1949885 + [PM2000] 1950853.                                    Gvr2010 
19438+1502   BPM1404     [PM2000] 1949264 + [PM2000] 1948124.                                    Gvr2010 
19438+1450   BPM1409     [PM2000] 1950089 + [PM2000] 1950189.                                    Gvr2010 
19438+1440   BPM1401     AB: [PM2000] 1949239 + [PM2000] 1949481.                                Gvr2010 
             BPM1402     BC: [PM2000] 1949481 + [PM2000] 1949415.                                Gvr2010 
             BPM1403     CD: [PM2000] 1949415 + [PM2000] 1949409.                                Gvr2010 
19438+1426   BPM1405     [PM2000] 1949444 + [PM2000] 1949441.                                    Gvr2010 
19438+1310   BPM1397     AB: [PM2000] 1949553 + [PM2000] 1948529.                                Gvr2010 
             BPM1398     BC: [PM2000] 1948529 + [PM2000] 1947764.                                Gvr2010 
             BPM1399     BD: [PM2000] 1948529 + [PM2000] 1948211.                                Gvr2010 
19438+1213   BPM1406     [PM2000] 1949504 + [PM2000] 1950018.                                    Gvr2010 
19439+2708   BU  658     Spectrum composite;G4III+K3II. Bryant measures a star which may be the  Bry1900 
                         same with an error in angle: 1900.62, 349.4@, 0.3" (BDS 9567).                  
                         1998.657: Absolute quadrant determined by triple-correlation technique  Pru2002b
                         Includes PS Vul, an Algol-type eclipsing binary, P = 3.8173d.           Zas2012 
19439+1514   BPMA153     [PM2000] 1950665 + [PM2000] 1948678.                                    Gvr2010 
19439-0034   RST5142     J  2557.                                                                Nsn2016 
19440+1422   BPM1410     [PM2000] 1952382 + [PM2000] 1953719.                                    Gvr2010 
19440+1406   BPMA154     [PM2000] 1951998 + [PM2000] 1956181.                                    Gvr2010 
19440+1222   HLM  27     Verhas (1993) and Sinachopoulos et al. (2007) mistakenly observed       Ver1993 
                         19441+1222STF2567 rather than this pair, due to coarse coordinates.     Sin2007 
19440-0443   LDS6337     NLTT 48160/48161                                                        Chm2004 
19441+1702   BPMA155     [PM2000] 1953751 + [PM2000] 1950321.                                    Gvr2010 
19441+1547   BPM1416     [PM2000] 1953779 + [PM2000] 1954740.                                    Gvr2010 
19441+1531   BPM1411     [PM2000] 1952847 + [PM2000] 1951868.                                    Gvr2010 
19441+1520   BPM1412     AB: [PM2000] 1953089 + [PM2000] 1952801.                                Gvr2010 
             BPM1413     BC: [PM2000] 1952801 + [PM2000] 1953317.                                Gvr2010 
19441+1433   BPM1415     [PM2000] 1953108 + [PM2000] 1952239.                                    Gvr2010 
19441+1222   STF2567     Same as STF2568.                                                                
                         AB: H 4 132.                                                            MEv2010 
19441+1116   BPM1414     [PM2000] 1953126 + [PM2000] 1954163.                                    Gvr2010 
19442+1706   BPMA156     [PM2000] 1955019 + [PM2000] 1956376.                                    Gvr2010 
19442+1632   BPM1417     [PM2000] 1954346 + [PM2000] 1955493.                                    Gvr2010 
19442+1408   BPM1419     [PM2000] 1954905 + [PM2000] 1955889.                                    Gvr2010 
19442+1334   BPM1418     [PM2000] 1954430 + [PM2000] 1954990.                                    Gvr2010 
19443+5547   HJ 1438     Discrepant 1917 Pettit observation was ealier catalogues as PTT  27,    Ptt1921 
                         although he said observation was of HJ 1438.                                    
19443+2655   L    30     BRT 199.                                                                Brt1928 
19443+1732   BPM1426     [PM2000] 1956345 + [PM2000] 1955244.                                    Gvr2010 
19443+1707   BPM1421     [PM2000] 1955318 + [PM2000] 1955701.                                    Gvr2010 
19443+1623   BPM1424     [PM2000] 1955818 + [PM2000] 1956071.                                    Gvr2010 
19443+1615   BPM1425     [PM2000] 1955847 + [PM2000] 1955527.                                    Gvr2010 
19443+1540   BPM1422     [PM2000] 1955613 + [PM2000] 1955809.                                    Gvr2010 
19443+1434   BPM1420     [PM2000] 1955274 + [PM2000] 1955148.                                    Gvr2010 
19443+1421   BPMA157     [PM2000] 1955185 + [PM2000] 1957757.                                    Gvr2010 
19443+1113   BPM1423     [PM2000] 1955778 + [PM2000] 1955915.                                    Gvr2010 
19444+3859   ALI 899     BRT2226.                                                                Brt1938 
19444+1619   BPM1429     [PM2000] 1956993 + [PM2000] 1956929.                                    Gvr2010 
19444+1618   BPM1427     [PM2000] 1956565 + [PM2000] 1955704.                                    Gvr2010 
19444+1525   BPM1430     [PM2000] 1957389 + [PM2000] 1956845.                                    Gvr2010 
19444+1143   BPM1428     [PM2000] 1956851 + [PM2000] 1955636.                                    Gvr2010 
19445+1353   BPM1434     [PM2000] 1958207 + [PM2000] 1958675.                                    Gvr2010 
19445+1305   BPMA158     [PM2000] 1958416 + [PM2000] 1954806.                                    Gvr2010 
19446+1621   BPM1438     [PM2000] 1959894 + [PM2000] 1960733.                                    Gvr2010 
19446+1557   BPM1431     AB: [PM2000] 1958935 + [PM2000] 1958196.                                Gvr2010 
             BPM1432     BC: [PM2000] 1958196 + [PM2000] 1956912.                                Gvr2010 
19446+1547   BPM1435     [PM2000] 1959194 + [PM2000] 1958976.                                    Gvr2010 
19446+1522   BPMA159     [PM2000] 1959320 + [PM2000] 1960976.                                    Gvr2010 
19446+1509   BPM1433     [PM2000] 1958922 + [PM2000] 1959831.                                    Gvr2010 
19446+1502   BPMA160     [PM2000] 1959396 + [PM2000] 1958965.                                    Gvr2010 
19446+1359   BPMA161     [PM2000] 1959939 + [PM2000] 1957440.                                    Gvr2010 
19446+1352   BPM1436     [PM2000] 1959652 + [PM2000] 1959010.                                    Gvr2010 
19446+1250   BPM1437     [PM2000] 1959876 + [PM2000] 1959238.                                    Gvr2010 
19446+1253   J  1862     Several measures purportedly of this pair were actually of WOR9001,             
                         located about 3' NE.                                                            
19447+1434   BPM1443     [PM2000] 1961118 + [PM2000] 1960634.                                    Gvr2010 
19447+1322   BPM1441     [PM2000] 1960672 + [PM2000] 1960329.                                    Gvr2010 
19447+1304   BPM1440     [PM2000] 1960405 + [PM2000] 1961323.                                    Gvr2010 
19447+1258   BPM1442     [PM2000] 1960835 + [PM2000] 1961549.                                    Gvr2010 
19447+1204   BPMA162     [PM2000] 1960560 + [PM2000] 1957407.                                    Gvr2010 
19447+1158   BPM1439     [PM2000] 1960220 + [PM2000] 1959044.                                    Gvr2010 
19447+0233   J  2183     Aka J   489.                                                            Dam2016d
19448+2916   ISM   4     The Cepheid SU Cyg. This is also known as WRH  23Aa,Ab. The Wilson              
                         component were previously assigned to 19372+2920, but this was a                
                         position error on Wilson's part leading to the the pairs not being      WRH1950a
                         confirmed for many years. The wider components of Wilson will retain            
                         their historical, AE, AF, and AG component identifiers. The closer              
                         Aa,Ab pair will remain ISM   4. The problem was noted by Cliff                  
                         Ashcraft and the correct system found by James Daley.                           
                         Masses are 4.7 and 3.2 Msun. Estimated period = 1.5y,                           
                         a = 2.6au = 0.003".                                                     Evs2013 
19448+1649   STF2569     H 2  32.                                                                MEv2010 
19448+1628   BPM1447     [PM2000] 1962507 + [PM2000] 1963715.                                    Gvr2010 
19448+1542   BPMA163     [PM2000] 1961418 + [PM2000] 1962436.                                    Gvr2010 
19448+1519   BPM1445     [PM2000] 1961884 + [PM2000] 1961399.                                    Gvr2010 
19448+1451   BPM1444     [PM2000] 1961840 + [PM2000] 1961794.                                    Gvr2010 
19448+1406   BPM1446     [PM2000] 1961998 + [PM2000] 1961947.                                    Gvr2010 
19448+1251   WOR9001     Several measures purportedly of J  1862 were actually of this pair.             
                         located about 3' NE of the Jonckheere pair.                                     
19449+1740   BPMA165     [PM2000] 1963285 + [PM2000] 1962695.                                    Gvr2010 
19449+1607   BPM1451     [PM2000] 1963152 + [PM2000] 1963986.                                    Gvr2010 
19449+1411   BPM1450     [PM2000] 1963080 + [PM2000] 1962301.                                    Gvr2010 
19449+1320   BPMA164     [PM2000] 1962675 + [PM2000] 1963861.                                    Gvr2010 
19449+1315   BPM1449     [PM2000] 1963062 + [PM2000] 1964303.                                    Gvr2010 
19449+1225   BPM1452     [PM2000] 1963714 + [PM2000] 1964192.                                    Gvr2010 
19449+1150   BPM1448     [PM2000] 1962985 + [PM2000] 1963987.                                    Gvr2010 
19449+1047   STF2570     AB,C: H 1  91.                                                          MEv2010 
19449-2338   MTG   4     Also known as LP 869-26.                                                        
                         Parallax = 67.87 +/- 1.10 mas.                                          JLB2017 
19450+4508   STF2579     del Cyg = 18 Cyg.                                                               
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Uniform disk diameter  0.874 +/- 0.062 mas,                                     
                         Limb darkened diameter 0.884 +/- 0.062 mas,                                     
                         Teff = 12000 +/- 1400 K based on LDD.                                           
                         Radius is 4.81 +/- 0.36 \rsun.                                          CIA2019a
                         AB: H 1  94.                                                            MEv2010 
19450+1547   BPM1453     [PM2000] 1963817 + [PM2000] 1964221.                                    Gvr2010 
19450+1416   BPM1454     [PM2000] 1963846 + [PM2000] 1963265.                                    Gvr2010 
19450+1412   BPM1462     [PM2000] 1964608 + [PM2000] 1963492.                                    Gvr2010 
19450+1404   BPM1455     [PM2000] 1964328 + [PM2000] 1965951.                                    Gvr2010 
19450+1145   BPM1456     AB: [PM2000] 1964456 + [PM2000] 1965552.                                Gvr2010 
             BPM1457     BC: [PM2000] 1965552 + [PM2000] 1965760.                                Gvr2010 
19451+1705   BPM1458     [PM2000] 1965189 + [PM2000] 1966717.                                    Gvr2010 
19451+1630   BPM1466     [PM2000] 1966293 + [PM2000] 1967712.                                    Gvr2010 
19451+1543   BPM1467     [PM2000] 1966341 + [PM2000] 1966749.                                    Gvr2010 
19451+1533   BPM1459     AB: [PM2000] 1965372 + [PM2000] 1964484.                                Gvr2010 
             BPM1460     AC: [PM2000] 1965372 + [PM2000] 1964882.                                Gvr2010 
19451+1432   BPM1463     [PM2000] 1965961 + [PM2000] 1964870.                                    Gvr2010 
19451+1337   BPM1461     [PM2000] 1965391 + [PM2000] 1966608.                                    Gvr2010 
19451+1244   BPM1464     AB: [PM2000] 1966011 + [PM2000] 1965875.                                Gvr2010 
             BPM1465     AC: [PM2000] 1966011 + [PM2000] 1965784.                                Gvr2010 
19452+1437   BPMA166     [PM2000] 1966969 + [PM2000] 1963147.                                    Gvr2010 
19453+2023   J   817     Measures do not confirm movement seen in Toulouse observations in               
                         1949. Two pairs?                                                        J__1952 
19453+1726   BPM1469     [PM2000] 1968263 + [PM2000] 1968147.                                    Gvr2010 
19453+1629   BPMA167     [PM2000] 1968685 + [PM2000] 1967904.                                    Gvr2010 
19453+1248   BPM1470     [PM2000] 1968277 + [PM2000] 1968645.                                    Gvr2010 
19453+1217   BPM1468     [PM2000] 1967808 + [PM2000] 1969143.                                    Gvr2010 
19453-6823   HDS2806     AB + TOK 425Ba,Bb: We resolved the secondary component of HDS 2806 AB           
                         into a close pair Ba,Bb. This is a K3 dwarf within 50pc from the Sun.           
                         The pair Ba,Bb should be fast and turn around in about 10yrs.           Tok2015c
19454+1705   BPM1472     [PM2000] 1969121 + [PM2000] 1968557.                                    Gvr2010 
19454+1702   BPM1471     [PM2000] 1969100 + [PM2000] 1968684.                                    Gvr2010 
19454+1404   BPMA168     [PM2000] 1968972 + [PM2000] 1970175.                                    Gvr2010 
19454+1313   BPMA169     [PM2000] 1969471 + [PM2000] 1967414.                                    Gvr2010 
19455+1739   BPM1479     [PM2000] 1971291 + [PM2000] 1971365.                                    Gvr2010 
19455+1640   BPM1476     [PM2000] 1970668 + [PM2000] 1972004.                                    Gvr2010 
19455+1623   BPM1473     AB: [PM2000] 1970281 + [PM2000] 1969674.                                Gvr2010 
             BPM1474     AC: [PM2000] 1970281 + [PM2000] 1971325.                                Gvr2010 
19455+1455   BPM1478     [PM2000] 1971058 + [PM2000] 1970767.                                    Gvr2010 
19455+1414   BPM1477     [PM2000] 1970956 + [PM2000] 1971134.                                    Gvr2010 
19455+1309   BPM1475     [PM2000] 1970284 + [PM2000] 1970892.                                    Gvr2010 
19455-1133   BRT2766     J 1685.                                                                         
19456+1655   BPM1482     AB: [PM2000] 1972374 + [PM2000] 1972706.                                Gvr2010 
             BPM1483     BC: [PM2000] 1972706 + [PM2000] 1972788.                                Gvr2010 
19456+1543   BPM1485     [PM2000] 1972439 + [PM2000] 1970997.                                    Gvr2010 
19456+1523   BPM1480     [PM2000] 1971721 + [PM2000] 1971602.                                    Gvr2010 
19456+1341   BPM1481     [PM2000] 1972313 + [PM2000] 1971466.                                    Gvr2010 
19457+4749   CBL  79     JKA  77. KIC 10612448/10612424.                                                 
19457+4230   ES 1563     Aka HJ 2898.                                                                    
19457+3930   ARN 117     JKA  78. KIC 4484238/4386086.                                                   
19457+3612   SEI 677     AC. Tertiary not seen on POSS plate; may be either variable star or             
                         flaw on AC Potsdam plate.                                                       
19457+3605   STF2578     BDS 9591, H N  13 same star. B is BD+35@3787.                                   
                         AB: SEI 676.                                                            Nsn2017b
19457+1550   BPM1488     [PM2000] 1973278 + [PM2000] 1974770.                                    Gvr2010 
19457+1455   BPM1486     [PM2000] 1972802 + [PM2000] 1973021.                                    Gvr2010 
19457+1449   BPM1484     [PM2000] 1972596 + [PM2000] 1973768.                                    Gvr2010 
19457+1406   BPM1487     [PM2000] 1973082 + [PM2000] 1973455.                                    Gvr2010 
19457+1339   BPM1489     [PM2000] 1973316 + [PM2000] 1973731.                                    Gvr2010 
19457+1329   BPM1490     [PM2000] 1973539 + [PM2000] 1973489.                                    Gvr2010 
19458+4622   ES 2674     ARG  86. Incorrectly listed in WDS as 19095+4103. Espin's 1908 measure  Es_1909a
                         was erroneously attributed to Argelander, leading to the ARG 86                 
                         designation.                                                                    
19458+2710   KUI  95     Indeterminate (long) period but useable a^3/P^2.                                
                         Missing in HIP because of poor Input Catalogue position.                Sod1999 
19458+1554   BPM1492     [PM2000] 1974374 + [PM2000] 1974587.                                    Gvr2010 
19458+1510   BPM1491     [PM2000] 1973827 + [PM2000] 1974341.                                    Gvr2010 
19458+1409   BPM1494     [PM2000] 1974694 + [PM2000] 1973860.                                    Gvr2010 
19458+1239   BPM1495     [PM2000] 1975046 + [PM2000] 1973863.                                    Gvr2010 
19458+1118   BPM1493     [PM2000] 1974448 + [PM2000] 1974600.                                    Gvr2010 
19459+3953   A  1404     AB: Too close 1935-1943. Measures uncertain 1943-1958.                          
                         AB,D: SEI 679.                                                          Nsn2017b
19459+3501   H 5 137     H V 137. STTA191. A has composite spectrum; K0II-III+A2V.                       
                         B is BD+34@3702.                                                                
19459+1731   BPM1499     [PM2000] 1976084 + [PM2000] 1977467.                                    Gvr2010 
19459+1625   BPMA171     [PM2000] 1976135 + [PM2000] 1973645.                                    Gvr2010 
19459+1602   BPM1498     [PM2000] 1975573 + [PM2000] 1976937.                                    Gvr2010 
19459+1536   BPMA170     [PM2000] 1975783 + [PM2000] 1975106.                                    Gvr2010 
19459+1459   BPM1496     [PM2000] 1975238 + [PM2000] 1974495.                                    Gvr2010 
19459+1127   BPM1497     [PM2000] 1975478 + [PM2000] 1975507.                                    Gvr2010 
19460+1755   BPM1502     [PM2000] 1977376 + [PM2000] 1976725.                                    Gvr2010 
19460+1447   BPM1501     [PM2000] 1977012 + [PM2000] 1976877.                                    Gvr2010 
19460+1325   BPM1500     [PM2000] 1976651 + [PM2000] 1977886.                                    Gvr2010 
19460+0415   BU  468     B is a flare star, V1406 Aql.                                                   
                         A is SB1, P=3990d.                                                      Tok2014d
19461+4458   ES   83     Fox notes a faint star in 193@, 15" from B and Roe notes another one    Fox1915 
                         65" preceding.                                                          Roe1918 
19461+1705   BPM1503     [PM2000] 1978024 + [PM2000] 1977733.                                    Gvr2010 
19461+1606   BPM1504     [PM2000] 1978454 + [PM2000] 1978611.                                    Gvr2010 
19461-1718   LDS4818     NLTT 48198/48193                                                        Chm2004 
19462+1704   BPM1505     AB: [PM2000] 1978880 + [PM2000] 1977685.                                Gvr2010 
             BPM1506     AC: [PM2000] 1978880 + [PM2000] 1978963.                                Gvr2010 
19462+1557   BPM1510     [PM2000] 1979198 + [PM2000] 1979886.                                    Gvr2010 
19462+1542   BPMA172     [PM2000] 1979371 + [PM2000] 1983217.                                    Gvr2010 
19462+1524   BPM1508     [PM2000] 1979071 + [PM2000] 1977604.                                    Gvr2010 
19462+1334   BPM1511     [PM2000] 1979320 + [PM2000] 1979241.                                    Gvr2010 
19462+1332   BPM1507     [PM2000] 1979043 + [PM2000] 1979069.                                    Gvr2010 
19462+1301   BPM1509     [PM2000] 1979136 + [PM2000] 1979109.                                    Gvr2010 
19463+2437   BKO 734     Aka SCA 202.                                                                    
19463+1755   BPM1519     [PM2000] 1980963 + [PM2000] 1979924.                                    Gvr2010 
19463+1553   BPM1512     [PM2000] 1980153 + [PM2000] 1979972.                                    Gvr2010 
19463+1526   BPM1518     [PM2000] 1980933 + [PM2000] 1980238.                                    Gvr2010 
19463+1336   BPM1515     [PM2000] 1980719 + [PM2000] 1981181.                                    Gvr2010 
19463+1326   BPM1517     [PM2000] 1980879 + [PM2000] 1979324.                                    Gvr2010 
19463+1245   BPM1516     [PM2000] 1980867 + [PM2000] 1981664.                                    Gvr2010 
19463+1227   BPM1513     [PM2000] 1980236 + [PM2000] 1980992.                                    Gvr2010 
19463+1139   BPM1514     [PM2000] 1980705 + [PM2000] 1981320.                                    Gvr2010 
19463+1037   BUP 198     gam Aql = 50 Aql = Tarazed                                                      
19463+1035   BU   55     J 123.                                                                          
19464+3344   STF2580     17 Cyg = chi Cyg. LDS1028. B is probably variable.                              
                         AB: NLTT 48226/48228                                                    Chm2004 
                         Common proper motion with STF 2576. Moved to same WDS coordinate to             
                         formalize the relationship 7 August 2008 at suggestion of Deepak                
                         Raghavan.                                                                       
                         AB: HJL 267.                                                            HJL1986 
                         AB: H 4  11.                                                            MEv2010 
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             KPR   4     AD: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AD: It is doubtful that the AD pair observed by 2MASS and later                 
                         observers is the pair observed by Kamper (1992). Neither his "Af" (AD)  Kpr1992 
                         or "Ag" (AE) pairs seems to correspond to any pairs in the field,               
                         when proper motion of the stars is taken into account.                          
             WNO  56     AF is the same as LEP  93. All measures merged into a single system.            
                         GJ 9670 + LTT 15766. CPM pair.                                          Mkr2008 
                         AF: SHY  96. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
             STF2576     FG: The longitude of periastron determined by Rabe (1948) has been      Rab1948a
                         reversed to represent the quadrant given by all recent observations.            
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Aka H N 109 = SHJ 300.                                                  Bu_1906 
                         FG: Additional notes may be found in Fatou (1941) and                   Fat1941 
                         Duruy (1944).                                                           Dur1944d
                         FG: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.55 +/- 0.84, 1.54, and 0.76 Msun, respectively.  Mlk2012 
             TKA   1     FJ. Tel'nyuk-Adamchuk actually observed the FI pair, but due to the     TkA1966 
                         high proper motion of F and the long time since the previous FI                 
                         measure, his measure was mistakenly assigned to a new component. The            
                         TKA designation has been maintained in order to avoid confusion,                
                         despite the fact that Tel'nyuk-Adamchuk never observed it.                      
19464+3201   KAM   3     NLTT 48223/48224                                                        Chm2004 
                         Masses determined to be 0.49 \Msun and 0.40 \Msun.                      Kiy2015b
                         They also share common parallax: A(B) = 74.90+/-2.93(73.46+/-1.79)mas.          
19464+1643   BPM1522     [PM2000] 1981821 + [PM2000] 1982775.                                    Gvr2010 
19464+1615   BPM1524     [PM2000] 1981631 + [PM2000] 1980689.                                    Gvr2010 
19464+1533   BPM1525     [PM2000] 1982313 + [PM2000] 1983364.                                    Gvr2010 
19464+1433   BPM1523     [PM2000] 1981860 + [PM2000] 1983400.                                    Gvr2010 
19464+1403   BPM1520     AB: [PM2000] 1981229 + [PM2000] 1982197.                                Gvr2010 
             BPM1521     BC: [PM2000] 1982197 + [PM2000] 1982122.                                Gvr2010 
19465+1619   BPM1528     [PM2000] 1983568 + [PM2000] 1983424.                                    Gvr2010 
19465+1449   BPM1526     [PM2000] 1982518 + [PM2000] 1983285.                                    Gvr2010 
19465+1248   BPM1527     [PM2000] 1983124 + [PM2000] 1982761.                                    Gvr2010 
19465-0028   BAL 915     J 2559.                                                                         
19466+4650   KOI 720     This system has four confirmed planets with radii of 2.96, 2.81, 3.05,  KOI2011b
                         and 1.56 Rearth (Borucki et al. 2011; Rowe et al. 2014). We             KOI2014b
                         detected another star 3".86 from the target star and 5.13 Ks mags               
                         fainter. The maximum dilution correction is a 0.2% correction to the            
                         planet radii, unlikely to be significant given the large separation.    Dre2014 
19466+3253   S   726     STTA192 = H N 110.                                                              
19466+1732   BPM1531     [PM2000] 1984205 + [PM2000] 1985156.                                    Gvr2010 
19466+1711   BPM1532     [PM2000] 1984271 + [PM2000] 1985415.                                    Gvr2010 
19466+1321   BPM1530     [PM2000] 1984082 + [PM2000] 1984116.                                    Gvr2010 
19466+1253   BPM1529     [PM2000] 1983869 + [PM2000] 1983051.                                    Gvr2010 
19466+0703   TOK 368     First resolution; est. period 17y, but constant RV according to GCS.    Tok2013b
19467+4421   YSC 136     Slightly sub-solar metallicity ([Fe/H] = -0.11); mass ratio                     
                         0.754 +/- 0.013; spectral type G0.                                      Hor2012b
19467+3143   HJ  898     Doolittle notes a 3rd star in the direction of B. 30" +/- distant,      Doo1932A
                         12th magnitude, 1919.8.                                                         
                         CPM of the components suggests that this pair could be physical;                
                         however, since the relative motion of the components is larger than             
                         their proper motion, the question of whether they are physically bound          
                         remains open.                                                           Kiy2012 
19467+1536   BPM1533     [PM2000] 1985202 + [PM2000] 1986174.                                    Gvr2010 
19467+1422   BPM1535     [PM2000] 1985646 + [PM2000] 1985487.                                    Gvr2010 
19467+1307   BPM1534     [PM2000] 1985377 + [PM2000] 1986136.                                    Gvr2010 
19468+4231   KOI2879     This system was reported to have a 1.4 Rearth planet with a 0.3 day             
                         period (Burke et al. 2014), but this signal has been found to be a      KOI2014a
                         false positive. Our ARIES observations revealed a companion 0.37 J              
                         mags and 0.27 Ks mags fainter than KOI 2879 at a distance of 0".423.            
                         Using the J-Ks to Kp-Ks color-color conversion from Howell et al.               
                         (2012), we predict that the Kp mag of the companion is Kp = 13.8        KOI2012a
                         (dKp = 1.1) if the star is a dwarf or Kp = 13.9 (dKp = 1.2) if the              
                         star is a giant. If any additional planet candidates are detected               
                         around KOI2879, their radii will need to be increased by roughly 17%            
                         to account for the additional light in the aperture.                    Dre2014 
19468+1422   BPM1536     [PM2000] 1986105 + [PM2000] 1986256.                                    Gvr2010 
19468+1339   BPM1537     [PM2000] 1986276 + [PM2000] 1984903.                                    Gvr2010 
19469+3204   BU  147     The relative motion derived from the Pulkovo series is small and has a          
                         large relative error. It remains an open question whether the system            
                         is physically bound.                                                    Kiy2012 
19469+1552   BPM1538     [PM2000] 1987298 + [PM2000] 1987396.                                    Gvr2010 
19469+1550   BPM1541     [PM2000] 1988058 + [PM2000] 1989090.                                    Gvr2010 
19469+1531   BPM1542     [PM2000] 1988436 + [PM2000] 1989298.                                    Gvr2010 
19469+1346   BPM1539     [PM2000] 1987419 + [PM2000] 1987038.                                    Gvr2010 
19469+1315   BPM1540     [PM2000] 1987929 + [PM2000] 1988717.                                    Gvr2010 
19470+3425   HD 187123   No comoving objects found within separation/magnitude range listed.             
                         However, Chauvin et al. (2006) note finding at least one faint          Cvn2006 
                         background object.                                                              
             GNS   4     AF: Ginski et al. (2012) conclude the D and F components are both               
                         background objects.                                                     Gns2012 
19470+1657   BPM1546     [PM2000] 1989512 + [PM2000] 1990517.                                    Gvr2010 
19470+1616   BPM1544     [PM2000] 1989123 + [PM2000] 1988954.                                    Gvr2010 
19470+1614   BPM1543     [PM2000] 1989007 + [PM2000] 1988396.                                    Gvr2010 
19470+1539   BPM1545     [PM2000] 1989466 + [PM2000] 1988054.                                    Gvr2010 
19471+5357   SMA  96     AC: Primary of 19485+5407 SMA  96 was found to be 19471+5357 TDT1744,           
                         but apparently the epoch-1930 coordinates from Smart (1932) were        Sma1932 
                         incorrectly precessed to J2000. The WDS designation has been changed            
                         to that of the TDT pair and the systems merged.                                 
19471+1750   BPM1548     [PM2000] 1990164 + [PM2000] 1990589.                                    Gvr2010 
19471+1657   BPM1547     [PM2000] 1989861 + [PM2000] 1989348.                                    Gvr2010 
19471+1559   BPM1549     [PM2000] 1990369 + [PM2000] 1989661.                                    Gvr2010 
19471+1416   BPM1550     [PM2000] 1990767 + [PM2000] 1990302.                                    Gvr2010 
19472+3141   DAM 374     Observed with the Pulkovo 26-inch refractor starting in 1971. It is             
                         not currently possible to determine whether the system is physically            
                         bound based on comparison with the component proper motions.            Kiy2012 
19472+1610   BPM1553     [PM2000] 1992055 + [PM2000] 1993388.                                    Gvr2010 
19472+1544   BPM1552     [PM2000] 1991651 + [PM2000] 1992225.                                    Gvr2010 
19472+1321   BPM1554     [PM2000] 1992072 + [PM2000] 1991458.                                    Gvr2010 
19472+1032   BPM1551     [PM2000] 1991442 + [PM2000] 1991206.                                    Gvr2010 
19473+4806   KOI 174     Primary is Kepler exoplanet host star.                                  Adm2013 
19473+1805   BPM1558     [PM2000] 1993091 + [PM2000] 1993507.                                    Gvr2010 
19473+1653   BPM1557     [PM2000] 1992881 + [PM2000] 1991691.                                    Gvr2010 
19473+1613   BPM1556     [PM2000] 1992527 + [PM2000] 1993133.                                    Gvr2010 
19473+1529   BPM1559     [PM2000] 1993171 + [PM2000] 1994362.                                    Gvr2010 
19473+1514   BPM1555     [PM2000] 1992498 + [PM2000] 1993860.                                    Gvr2010 
19473+1304   BPM1560     [PM2000] 1993315 + [PM2000] 1994562.                                    Gvr2010 
19474+2542   BRT3349     Originally published as BRT 200.                                        Brt1928 
19474+1832   BLA   6     del Sge = 7 Sge.                                                                
                         Mk III Limb-darkened diameter  9.151 +/- 0.119 mas.                     MkT2003 
                         The composite spectrum offered unfilled hope of observable duplicity.   WRH1941b
                         Disk unresolved in 1975.629 but possible binary.                        Bla1977a
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical and spectroscopic masses                  
                         7.84 +/- 3.26 and 8.70 Msun, respectively.                              Mlk2012 
19474+1543   BPM1563     [PM2000] 1994762 + [PM2000] 1994702.                                    Gvr2010 
19474+1533   BPMA173     [PM2000] 1993506 + [PM2000] 1995428.                                    Gvr2010 
19474+1309   BPM1562     [PM2000] 1994075 + [PM2000] 1993862.                                    Gvr2010 
19474+1222   BPM1561     [PM2000] 1993771 + [PM2000] 1994792.                                    Gvr2010 
19475+4407   UC  246     JKA  81. KIC 8248671/8248626.                                                   
19475+1707   BPMA174     [PM2000] 1995323 + [PM2000] 1996791.                                    Gvr2010 
19475+1620   BPM1564     [PM2000] 1995184 + [PM2000] 1996277.                                    Gvr2010 
19475+1543   BPM1566     [PM2000] 1995402 + [PM2000] 1996754.                                    Gvr2010 
19475+1522   BPM1567     AB: [PM2000] 1995501 + [PM2000] 1996167.                                Gvr2010 
             BPM1568     AC: [PM2000] 1995501 + [PM2000] 1995858.                                Gvr2010 
             BPM1569     BC: [PM2000] 1996167 + [PM2000] 1995858.                                Gvr2010 
             BPM1570     CD: [PM2000] 1995858 + [PM2000] 1997395.                                Gvr2010 
19475+1217   BPM1565     [PM2000] 1995304 + [PM2000] 1995998.                                    Gvr2010 
19476+1556   BPM1572     [PM2000] 1997134 + [PM2000] 1997565.                                    Gvr2010 
19476+1242   BPM1573     [PM2000] 1996715 + [PM2000] 1995045.                                    Gvr2010 
19476+1207   BPM1571     [PM2000] 1996948 + [PM2000] 1996556.                                    Gvr2010 
19476+0105   ENG  67     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             SHY 322     AD: HIP  97384 + HIP  95829. D component = A component of 19294+0032.           
19477+4451   COU2691     KOI 287AB = Kepler  8703887. Howell et al. (2011) quadrant ambiguous.   Hor2011c
19477+3957   SEI 683     AC: incorrectly called SEI 682AC.                                       Nsn2017b
19477+1802   BPMA175     [PM2000] 1997321 + [PM2000] 1998791.                                    Gvr2010 
19477+1716   BPM1578     [PM2000] 1998378 + [PM2000] 1997326.                                    Gvr2010 
19477+1625   BPM1577     [PM2000] 1998235 + [PM2000] 1997409.                                    Gvr2010 
19477+1604   BPM1576     [PM2000] 1997673 + [PM2000] 1998270.                                    Gvr2010 
19477+1308   BPM1574     [PM2000] 1997404 + [PM2000] 1997576.                                    Gvr2010 
19477+1248   BPM1575     [PM2000] 1997549 + [PM2000] 1996557.                                    Gvr2010 
19477+1125   BPMA176     [PM2000] 1997888 + [PM2000] 1995114.                                    Gvr2010 
19478+2334   POU4082     AC: J  3007.                                                                    
19478+1658   BPMA177     [PM2000] 1998999 + [PM2000] 2000904.                                    Gvr2010 
19478+1515   BPM1580     AB: [PM2000] 1999347 + [PM2000] 1999330.                                Gvr2010 
             BPM1581     AC: [PM2000] 1999347 + [PM2000] 1998392.                                Gvr2010 
19478+1352   BPM1579     [PM2000] 1999524 + [PM2000] 1998071.                                    Gvr2010 
19478+1338   BPM1582     AB: [PM2000] 1999606 + [PM2000] 1999037.                                Gvr2010 
             BPM1583     AC: [PM2000] 1999606 + [PM2000] 1998471.                                Gvr2010 
             BPM1584     BC: [PM2000] 1999037 + [PM2000] 1998471.                                Gvr2010 
19479+1750   BPM1593     [PM2000] 2000273 + [PM2000] 2000112.                                    Gvr2010 
19479+1651   BPM1585     [PM2000] 1999756 + [PM2000] 2000716.                                    Gvr2010 
19479+1629   BPM1588     [PM2000] 1999995 + [PM2000] 2000222.                                    Gvr2010 
19479+1439   BPM1587     [PM2000] 1999773 + [PM2000] 1999230.                                    Gvr2010 
19479+1420   BPM1591     [PM2000] 2000187 + [PM2000] 2001600.                                    Gvr2010 
19479+1413   BPM1586     [PM2000] 1999758 + [PM2000] 2000449.                                    Gvr2010 
19479+1407   BPM1592     [PM2000] 2000236 + [PM2000] 1999708.                                    Gvr2010 
19479+1227   BPM1590     [PM2000] 2000149 + [PM2000] 1999760.                                    Gvr2010 
19479+1211   BPM1589     [PM2000] 2000100 + [PM2000] 1999778.                                    Gvr2010 
19479+1002   AG  391     B is BD+09@4262.                                                                
19480+5029   DEA 157     JKA  82. KIC 12024098/12024088.                                                 
19480+2447   DOO  11     Also known as TDT1771.                                                          
19480+1758   BPM1599     [PM2000] 2001874 + [PM2000] 2001852.                                    Gvr2010 
19480+1656   BPM1594     [PM2000] 2001198 + [PM2000] 2002316.                                    Gvr2010 
19480+1621   BPM1600     AB: [PM2000] 2002087 + [PM2000] 2001528.                                Gvr2010 
             BPM1601     BC: [PM2000] 2001528 + [PM2000] 2003026.                                Gvr2010 
19480+1602   BPM1596     AB: [PM2000] 2001569 + [PM2000] 2002312.                                Gvr2010 
             BPM1597     BC: [PM2000] 2002312 + [PM2000] 2003681.                                Gvr2010 
19480+1532   BPM1598     [PM2000] 2001822 + [PM2000] 2002802.                                    Gvr2010 
19480+1218   BPM1602     [PM2000] 2001669 + [PM2000] 2003178.                                    Gvr2010 
19480+0423   J  2279     Identical with J  3006                                                  Hei1995 
19481+6438   J  1354     ID uncertain. Alternatively, may be same as ES  199.                            
19481+1803   BPM1603     [PM2000] 2002656 + [PM2000] 2003994.                                    Gvr2010 
19481+1642   BPM1595     [PM2000] 2002136 + [PM2000] 2000803.                                    Gvr2010 
19481+1556   BPMA178     [PM2000] 2003162 + [PM2000] 2001541.                                    Gvr2010 
19481+1554   BPM1605     [PM2000] 2003082 + [PM2000] 2003577.                                    Gvr2010 
19481+1551   BPM1604     [PM2000] 2002716 + [PM2000] 2001410.                                    Gvr2010 
19482+7016   STF2603     eps Dra = 63 Dra. A spectroscopic binary.                               D__1883 
                         H 1   8.                                                                MEv2010 
19482+1714   BPM1608     [PM2000] 2003505 + [PM2000] 2004189.                                    Gvr2010 
19482+1702   BPM1609     AB: [PM2000] 2003564 + [PM2000] 2004713.                                Gvr2010 
             BPM1610     BC: [PM2000] 2004713 + [PM2000] 2005721.                                Gvr2010 
19482+1650   BPM1606     AB: [PM2000] 2003321 + [PM2000] 2003800.                                Gvr2010 
             BPM1607     AC: [PM2000] 2003321 + [PM2000] 2004735.                                Gvr2010 
19482+1553   BPM1611     [PM2000] 2003939 + [PM2000] 2002610.                                    Gvr2010 
19482+1518   BPM1612     [PM2000] 2003998 + [PM2000] 2004969.                                    Gvr2010 
19482+1324   BPM1614     [PM2000] 2003761 + [PM2000] 2002205.                                    Gvr2010 
19482+0919   RUC  12     OO Aql. Spectral type of resolved companion later than M5V.             Ruc2007 
19483+1651   BPM1613     [PM2000] 2004554 + [PM2000] 2004856.                                    Gvr2010 
19483+1530   BPM1615     [PM2000] 2004826 + [PM2000] 2005784.                                    Gvr2010 
19483+1412   BPM1616     [PM2000] 2005243 + [PM2000] 2006105.                                    Gvr2010 
19484+1541   BPMA180     [PM2000] 2006588 + [PM2000] 2008415.                                    Gvr2010 
19484+1520   BPM1617     [PM2000] 2006406 + [PM2000] 2005667.                                    Gvr2010 
19484+1242   BPMA179     [PM2000] 2006206 + [PM2000] 2007242.                                    Gvr2010 
19485+2309   CHE 149     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match to this pair was correct.                                 Bko2011c
19485+1958   J  1865     Also known as J  2281.                                                          
19485+1638   BPM1623     [PM2000] 2007806 + [PM2000] 2006813.                                    Gvr2010 
19485+1537   BPM1625     [PM2000] 2007058 + [PM2000] 2007556.                                    Gvr2010 
19485+1508   BPM1622     [PM2000] 2007642 + [PM2000] 2008724.                                    Gvr2010 
19485+1333   BPM1618     [PM2000] 2006912 + [PM2000] 2008352.                                    Gvr2010 
19485+1321   BPM1621     [PM2000] 2007122 + [PM2000] 2007870.                                    Gvr2010 
19485+1210   BPMA181     [PM2000] 2007726 + [PM2000] 2008985.                                    Gvr2010 
19486+3339   J   779     SMA  97.                                                                        
19486+1617   BPM1624     [PM2000] 2007894 + [PM2000] 2008800.                                    Gvr2010 
19486+1602   BPM1627     [PM2000] 2008630 + [PM2000] 2009684.                                    Gvr2010 
19486+1539   BPM1619     AB: [PM2000] 2008070 + [PM2000] 2007042.                                Gvr2010 
             BPM1620     BC: [PM2000] 2007042 + [PM2000] 2006549.                                Gvr2010 
19486+1423   BPM1626     [PM2000] 2008384 + [PM2000] 2008794.                                    Gvr2010 
19487+3519   STT 387     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.53 +/- 0.32, 2.74, and 1.17 Msun, respectively.             Mlk2012 
19487+2048   KU  124     B is BD+20@4283.                                                                
19487+1852   MCA  58     1998.657: Absolute quadrant determined by triple-correlation technique  Pru2002b
19487+1703   BPMA182     [PM2000] 2009285 + [PM2000] 2008636.                                    Gvr2010 
19487+1634   GRV 281     B component is +16 4009.                                                        
19487+1537   BPM1628     AB: [PM2000] 2009652 + [PM2000] 2009552.                                Gvr2010 
             BPM1629     AC: [PM2000] 2009652 + [PM2000] 2010786.                                Gvr2010 
19487+1504   A  1658     Only elements P, T, and a of Couteau (1963) were adjusted in orbit      Cou1963c
                         by Starikova (1981).                                                    Sta1981a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.69 +/- 1.11, 3.16, and 1.20 Msun, respectively.             Mlk2012 
19487+1337   BPM1630     [PM2000] 2009970 + [PM2000] 2010307.                                    Gvr2010 
19487+1149   STF2583     pi Aql = 52 Aql                                                                 
                         AB: Absolute quadrant determined in 1998.657 and 1998.660 by                    
                         triple-correlation techniques.                                          Pru2002b
                         AB: H 1  92.                                                            MEv2010 
19488+1532   BPM1631     [PM2000] 2011025 + [PM2000] 2010182.                                    Gvr2010 
19489+1658   BPMA183     [PM2000] 2011894 + [PM2000] 2014738.                                    Gvr2010 
19489+1602   BPMA184     [PM2000] 2011995 + [PM2000] 2013456.                                    Gvr2010 
19489+1601   BPM1632     [PM2000] 2011927 + [PM2000] 2011572.                                    Gvr2010 
19489+1517   BPMA185     [PM2000] 2012417 + [PM2000] 2012372.                                    Gvr2010 
19490+4423   STF2588     A,BC: H 3 112.                                                          MEv2010 
19490+4413   DEA 479     JKA  84. KIC 8316361/8316388.                                                   
19490+3731   ES 2499     ALI 633.                                                                        
19490+3341   SEI 687     Also known as SMA  98.                                                          
                         B = HD 225944, eclipsing binary of W UMa type, period 0.3177 days.      Zas2015 
19490+2227   CHE 150     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. Berko's match to this pair was correct.       Bko2011c
                         See Hartkopf (2012).                                                    Hrt2012b
19490+1909   AGC  11     zet Sge = 8 Sge. A is a suspected spectroscopic binary.                         
                         Probably quadruple. The fast RV variation found at three                        
                         spectrographs, and not explained by the visual motion, suggests a               
                         spectroscopic companion.                                                        
                         AB. A measure on 1980.7256 was incorrectly attributed to ADS 12973 by           
                         McAlister et al. (1983); it actually belongs to HR 7486.                McA1983 
                         This is part of a triple system. Finsen's (1937) observations covered   Fin1937b
                         two periods and yield a separation close to this one.                   BLM1978 
                         Calculated mass sum is 2.23 +/- 0.35 Msun; this is lower than would be          
                         expected for early A stars, perhaps due to parallax error.              Mut2010b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.23 +/- 0.35, 4.39, and 2.19 Msun, respectively.  Mlk2012 
             STF2585     AB,C: H 2  30.                                                          MEv2010 
19490+1627   BPM1635     [PM2000] 2013007 + [PM2000] 2014246.                                    Gvr2010 
19490+1606   BPM1634     [PM2000] 2012591 + [PM2000] 2013649.                                    Gvr2010 
19490+1436   BPM1636     [PM2000] 2013014 + [PM2000] 2012283.                                    Gvr2010 
19490+1419   BPMA186     [PM2000] 2013128 + [PM2000] 2011268.                                    Gvr2010 
19490+1405   BPM1637     [PM2000] 2013339 + [PM2000] 2012882.                                    Gvr2010 
19490+1302   BPM1633     [PM2000] 2012491 + [PM2000] 2011868.                                    Gvr2010 
19490-2236   DON 969     CD-22@14256.                                                                    
19491+2259   CHE 151     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match to this pair was correct.                                 Bko2011c
19491+1720   BPM1638     [PM2000] 2014256 + [PM2000] 2014534.                                    Gvr2010 
19491+1426   BPM1639     AB: [PM2000] 2014612 + [PM2000] 2015530.                                Gvr2010 
             BPM1640     BC: [PM2000] 2015530 + [PM2000] 2016199.                                Gvr2010 
19491+1142   BPM1643     [PM2000] 2014628 + [PM2000] 2015174.                                    Gvr2010 
19491-6149   I   120     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.74 +/- 0.62, 2.31, and 1.11 Msun, respectively.  Mlk2012 
19492+1711   BPM1642     [PM2000] 2015081 + [PM2000] 2016096.                                    Gvr2010 
19492+1543   BPM1641     [PM2000] 2015040 + [PM2000] 2015325.                                    Gvr2010 
19493+4135   LEP  94     NI   40. JKA  87. KIC 6225718/6225816.                                          
19493+4005   UC  247     JKA  86. KIC 4946401/4946433.                                                   
19493+3441   BKO 518     Anon. 30.                                                               Bko2009d
19493+2202   CHE 152     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates, as well as an additional 10' error in his             
                         declination, due to an error in applying the y offset. In addition,             
                         there was a trigonometric error in deriving theta; the correct value    Hrt2012b
                         is 180deg - theta.  Berko (2011) was unable to find a match.            Bko2011c
19493+1551   BPM1645     [PM2000] 2016467 + [PM2000] 2016737.                                    Gvr2010 
19493+1526   BPM1647     [PM2000] 2016617 + [PM2000] 2016229.                                    Gvr2010 
19493+1502   BPM1646     [PM2000] 2016517 + [PM2000] 2017361.                                    Gvr2010 
19493+1216   BPM1644     [PM2000] 2016117 + [PM2000] 2016371.                                    Gvr2010 
19493+0440   WOL   7     HTP  41.                                                                        
19494+3446   BKO 519     Anon. 31.                                                               Bko2009d
19494+1740   BPM1650     [PM2000] 2017823 + [PM2000] 2017371.                                    Gvr2010 
19494+1517   BPM1648     [PM2000] 2017436 + [PM2000] 2016253.                                    Gvr2010 
19494+1328   BPM1649     [PM2000] 2017649 + [PM2000] 2018343.                                    Gvr2010 
19495+2334   BKO 984     Typographical error in WDS designation by Berko - should be +2234.      Bko2011c
19495+2234   CHE 153     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match to this pair was correct.                                 Bko2011c
19495+2230   CHE 154     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
19495+1715   BPM1652     AB: [PM2000] 2018331 + [PM2000] 2018808.                                Gvr2010 
             BPM1653     AC: [PM2000] 2018331 + [PM2000] 2017873.                                Gvr2010 
             BPM1654     BC: [PM2000] 2018808 + [PM2000] 2017873.                                Gvr2010 
             BPM1655     BD: [PM2000] 2018808 + [PM2000] 2018377.                                Gvr2010 
19495+1434   BPM1651     [PM2000] 2018241 + [PM2000] 2018005.                                    Gvr2010 
19495+1140   BPMA187     [PM2000] 2018619 + [PM2000] 2017555.                                    Gvr2010 
19495+0634   TOR  16     Formerly known as PAN  13.                                                      
19496+3950   KOI2971     This system contains a 0.8 Rearth planet candidate with a 6.1 day               
                         period and a second 1.1 Rearth planet candidate with a 31.9 day period  KOI2014a
                         (Burke et al. 2014).                                                    Dre2014 
19496+3939   HJ 2903     AB: SEI 691.                                                            Nsn2017b
19496+3448   SEI 690     Secondary not seen on POSS plate; may be either variable star or flaw           
                         on AC Potsdam plate.                                                            
19496+1700   BPM1658     [PM2000] 2020210 + [PM2000] 2019589.                                    Gvr2010 
19496+1514   BPM1656     [PM2000] 2019638 + [PM2000] 2019915.                                    Gvr2010 
19496+1253   BPM1657     [PM2000] 2019895 + [PM2000] 2020158.                                    Gvr2010 
19497+1720   BPM1660     [PM2000] 2020258 + [PM2000] 2019898.                                    Gvr2010 
19497+1714   BPM1661     [PM2000] 2020530 + [PM2000] 2019910.                                    Gvr2010 
19497+1554   BPMA188     [PM2000] 2020920 + [PM2000] 2019890.                                    Gvr2010 
19497+1549   BPM1659     [PM2000] 2020257 + [PM2000] 2019113.                                    Gvr2010 
19497+1523   BPM1662     [PM2000] 2020940 + [PM2000] 2021137.                                    Gvr2010 
19497+1147   BPM1663     [PM2000] 2021108 + [PM2000] 2020555.                                    Gvr2010 
19497-0226   J  2282     Not found by Heintz at IDS position.                                    Hei1990b
19498+2324   J   496     After correcting for the plate center and trigonometry errors, the      Che1908 
                         pair 19501+2325 CHE 155 was found to match J   496AB, as noted by       Bko2011c
                         Berko. Measures have been merged.                                       Hrt2012b
19498+2310   POU4111     After correcting for the plate center and trigonometry errors, the      Che1908 
                         pair 19501+2311 CHE 156 was found to match POU4111. Measures merged.    Bko2011c
                         Berko's match is actually a new pair.                                   Hrt2012b
19498+1802   BPM1664     [PM2000] 2021624 + [PM2000] 2021364.                                    Gvr2010 
19498+1741   BPM1665     [PM2000] 2021830 + [PM2000] 2020534.                                    Gvr2010 
19498+1737   BPM1666     [PM2000] 2022035 + [PM2000] 2022105.                                    Gvr2010 
19498+1540   BPMA189     [PM2000] 2021573 + [PM2000] 2019857.                                    Gvr2010 
19499+4107   KOI 126     AB, AD: Adams et al. (2012) theta values corrected to 360-theta         Adm2012 
                         (reported by Dressing et al. (2014).                                    Dre2014 
19499+1715   BPM1669     [PM2000] 2023213 + [PM2000] 2024429.                                    Gvr2010 
19499+1658   BPM1668     [PM2000] 2023040 + [PM2000] 2023625.                                    Gvr2010 
19499+1631   BPM1667     [PM2000] 2022608 + [PM2000] 2023162.                                    Gvr2010 
19499+1623   BPM1670     [PM2000] 2023473 + [PM2000] 2023047.                                    Gvr2010 
19499+1145   BPM1671     [PM2000] 2023596 + [PM2000] 2023016.                                    Gvr2010 
19500+3407   SEI 692     J 1068.                                                                         
19500+3235   JOD  18     LHS 3489. Estimated age 1000-10000 Myr; masses 0.34 +/- 0.03 and 0.19           
                         +/- 0.01 Msun; a ~3.8 au.                                               Jnn2014 
19500+1757   H 4  99     AB: H IV 99.                                                                    
19500+1457   BPM1673     [PM2000] 2024667 + [PM2000] 2023729.                                    Gvr2010 
19500+1436   BPM1672     [PM2000] 2024258 + [PM2000] 2023621.                                    Gvr2010 
19501+4748   AG  240     JKA  89. KIC 10616138/10616124.                                                 
19501+4401   DEA 120     JKA  90. KIC 8184081/8184075.                                                   
19501+1712   BPM1675     [PM2000] 2025040 + [PM2000] 2024291.                                    Gvr2010 
19501+1418   BPM1674     [PM2000] 2024825 + [PM2000] 2024795.                                    Gvr2010 
19502+1617   BPM1678     [PM2000] 2026647 + [PM2000] 2025475.                                    Gvr2010 
19502+1559   BPM1677     [PM2000] 2026278 + [PM2000] 2025273.                                    Gvr2010 
19502+1455   BPM1676     [PM2000] 2026237 + [PM2000] 2025137.                                    Gvr2010 
19502+1226   BPM1679     [PM2000] 2026651 + [PM2000] 2026536.                                    Gvr2010 
19503+2240   BU  361     AB: ADS notes that 19506+2241CHE 157 is almost certainly the same pair  A__1932a
                         as BU  361AB. The Chevalier measure from 1907.69 was reassigned to      Che1908 
                         BU  361, as was a 1999.7813 measure from Mason et al.                   WSI2000b
19503+1641   BPM1685     [PM2000] 2027481 + [PM2000] 2028300.                                    Gvr2010 
19503+1629   BPM1683     [PM2000] 2027803 + [PM2000] 2029005.                                    Gvr2010 
19503+1527   BPM1682     [PM2000] 2027544 + [PM2000] 2027239.                                    Gvr2010 
19503+1346   BPM1684     [PM2000] 2027903 + [PM2000] 2027696.                                    Gvr2010 
19503+1148   BPM1680     AB: [PM2000] 2027078 + [PM2000] 2027989.                                Gvr2010 
             BPM1681     BC: [PM2000] 2027989 + [PM2000] 2027664.                                Gvr2010 
19503+0754   CHR  89     This is the variable V1339 Aql.                                                 
19503+0713   A  2994     A,BC: J 1866.                                                                   
19503+0645   TOR  17     Formerly known as PAN  14.                                                      
19504+1708   BPM1687     [PM2000] 2028972 + [PM2000] 2028551.                                    Gvr2010 
19504+1637   BPM1686     [PM2000] 2028490 + [PM2000] 2027666.                                    Gvr2010 
19504+1626   BPM1688     [PM2000] 2029081 + [PM2000] 2028128.                                    Gvr2010 
19505+1625   BPM1690     [PM2000] 2030219 + [PM2000] 2029067.                                    Gvr2010 
19505+1553   BPM1689     [PM2000] 2030147 + [PM2000] 2029989.                                    Gvr2010 
19506+4036   RAO 517     V380 Cyg.                                                                       
19506+4021   KOI2158     This system contains two planet candidates with periods of 4.6 and 6.7          
                         days and radii of 1.6 and 1.0 Rearth, respectively (Batalha et al.              
                         2013). KOI2158 does not exhibit a large source offset during the        KOI2013a
                         transits of either planet candidate.                                    Dre2014 
19506+3843   HJ  603     19 Cyg. A is the irregular variable V1509 Cyg. Berlin Obs. observes     StG1963 
                         Aa,Ab: 1922.7, 312@, 168.6". Ab: 1922.7, 323@, 103.5".                          
                         BE measures from Burnham and Pannunzio et al. were originally           Bu_1903 
                         designated BC, but the secondary was not the same object as measured    Bu_1913 
                         in the AC pair.                                                         Tor1992 
19506+3255   BLL  42     Chi Cyg. A is a Mira-type variable.                                             
                         Smyth published a measure for an additional 9th magnitude component     Smy1844 
                         (1835.67, 72.9deg, 25".7) and noted similar measures by Herschel        H__1906A
                         (1779, 24".8) and South & Herschel (1822.49, 63.3deg, 25".5). However,  SHJ1906A
                         ALADIN indicates nothing at the purported location of this object.              
                         These measures appear to have been assigned to 19464+3344 STF2580AB,            
                         instead.                                                                        
19506+1704   BPM1692     [PM2000] 2030740 + [PM2000] 2030846.                                    Gvr2010 
19506+1703   BPM1694     [PM2000] 2031253 + [PM2000] 2031372.                                    Gvr2010 
19506+1635   BPM1693     [PM2000] 2031224 + [PM2000] 2031182.                                    Gvr2010 
19506+1221   BPM1691     [PM2000] 2030433 + [PM2000] 2029121.                                    Gvr2010 
19506-1917   HJ 2900     BDS 9702, HJ 1446 probably same star (van den Bos).                     B__1949c
19507+2309   BKO 991     Incorrectly identified by Berko as 19508+2310CHE 158.                   Bko2011c
19507+1752   BPM1696     [PM2000] 2031416 + [PM2000] 2031935.                                    Gvr2010 
19507+1743   BPM1698     [PM2000] 2031727 + [PM2000] 2032672.                                    Gvr2010 
19507+1715   BPM1695     [PM2000] 2032501 + [PM2000] 2033258.                                    Gvr2010 
19507+1607   BPM1701     [PM2000] 2032327 + [PM2000] 2033092.                                    Gvr2010 
19507+1533   BPM1700     [PM2000] 2032280 + [PM2000] 2032708.                                    Gvr2010 
19507+1530   BPM1699     [PM2000] 2031912 + [PM2000] 2031345.                                    Gvr2010 
19507+1515   BPM1697     [PM2000] 2031713 + [PM2000] 2031643.                                    Gvr2010 
19507-5912   SHY 759     AB: HIP  97646 + HIP  97581.                                                    
             SHY 761     AC: HIP  97646 + HIP  98174.                                                    
19508+3430   SEI 696     See note to 19509+3429 POP  13.                                                 
             POP  13     AC: Anon. 32.                                                           Bko2009d
19508+2310   CHE 158     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match to this pair was actually a new pair.                     Bko2011c
                         BKO 437.                                                                        
19508+2235   BKO 994     Incorrectly identified by Berko as 19509+2235CHE 160.                   Bko2011c
19508+2234   CHE 159     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match to this pair was actually a new pair.                     Bko2011c
19508+1750   BPMA190     [PM2000] 2033111 + [PM2000] 2034688.                                    Gvr2010 
19508+1543   BPM1702     AB: [PM2000] 2033146 + [PM2000] 2032146.                                Gvr2010 
             BPM1703     BC: [PM2000] 2032146 + [PM2000] 2031352.                                Gvr2010 
19508+1328   BPM1704     [PM2000] 2033642 + [PM2000] 2033308.                                    Gvr2010 
19508+1245   BPMA191     [PM2000] 2033144 + [PM2000] 2030743.                                    Gvr2010 
19508+0852   STFB 10     alp Aql = 53 Aql = Altair. B is BD+08@4232.                                     
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: H 6  46.                                                            MEv2010 
19508-1046   HO  275     51 Aql.                                                                         
19509+4841   DEA 126     JKA  93. KIC 11098013/11098004.                                                 
19509+3429   POP  13     AB was initially incorrectly associated with 19508+3430 SEI 696, with           
                         the Popovic AC measure thought to be a poor measure of SEI 696.         Pop1993 
19509+2235   CHE 160     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match to this pair was actually a new pair.                     Bko2011c
                         BKO 990. BKO 990 was incorrectly identified by Berko as                         
                         19508+2234CHE 159.                                                      Bko2011c
19509+1446   BPM1707     [PM2000] 2034674 + [PM2000] 2034221.                                    Gvr2010 
19509+1116   BPM1705     [PM2000] 2033732 + [PM2000] 2033695.                                    Gvr2010 
19509+1035   BPM1706     [PM2000] 2034024 + [PM2000] 2035252.                                    Gvr2010 
19509-2638   B   452     Primary is eclipsing binary of Beta Lyr -type, period 1.17154 d.        Zas2012 
19510+7524   STF2617     B is BD+75@715.                                                                 
19510+1649   BPM1709     AB: [PM2000] 2035349 + [PM2000] 2034564.                                Gvr2010 
             BPM1710     AC: [PM2000] 2035349 + [PM2000] 2036663.                                Gvr2010 
19510+1644   BPM1713     [PM2000] 2035749 + [PM2000] 2034269.                                    Gvr2010 
19510+1637   BPM1712     [PM2000] 2035681 + [PM2000] 2034958.                                    Gvr2010 
19510+1627   BPM1711     [PM2000] 2035507 + [PM2000] 2034642.                                    Gvr2010 
19510+1556   BPM1708     [PM2000] 2034797 + [PM2000] 2034828.                                    Gvr2010 
19510+1025   J   124     omi Aql = 54 Aql = O Aql                                                        
19510-0252   TOK 213     NICI resolved the astrometric binary with variable RV. Triple system            
                         with a CPM companion at 83".                                            Tok2012a
                         Aa,Ab: Astrometric and SB1,P=14.4y                                      Tok2014d
19511+2323   CHE 161     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match to this pair was correct.                                 Bko2011c
19511+2306   CHE 162     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match was actually CHE 164.                                     Bko2011c
19511+2228   CHE 163     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match is actually a new pair. However, his pair 19508+2227 =    Bko2011c
                         Anon 13 is actually CHE 163.                                                    
19511+1717   BPMA193     [PM2000] 2036789 + [PM2000] 2039040.                                    Gvr2010 
19511+1628   BPM1714     [PM2000] 2036241 + [PM2000] 2035832.                                    Gvr2010 
19511+1441   BPM1715     [PM2000] 2036493 + [PM2000] 2036411.                                    Gvr2010 
19511+1140   BPMA192     [PM2000] 2036270 + [PM2000] 2034646.                                    Gvr2010 
19512+2306   CHE 164     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match is actually CHE 162. His Anon 18Ax is part of this        Bko2011c
                         system.                                                                         
19512-7248   SHY 760     AD: HIP  97690 + HIP 100549.                                                    
19513+2319   POU4120     There was an error in Chevalier's coordinates for 19516+2320 CHE 169,   Che1908 
                         due to incorrect plate center coordinates. After correcting for these           
                         errors, this pair was found to match POU4120, as noted by Berko.        Bko2011c
                         In addition, there was a trigonometric error in deriving theta; the             
                         correct value is 180deg - theta. Measures merged.                       Hrt2012b
19513+2309   CHE 165     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match to this pair was actually a new pair.                     Bko2011c
19513+2308   CHE 166     AB: There was an error in Chevalier's coordinates due to incorrect      Che1908 
                         plate center coordinates. Berko's match to this pair was correct.       Bko2011c
                         AC: Berko's match is actually CHE 165.                                  Hrt2012b
             BKO 997     CD: Originally 19510+2308 BKO 997, but primary found to be the C                
                         component of 19513+2308 CHE 166AC.                                              
                         Incorrectly identified by Berko as 19513+2309CHE 165.                   Bko2011c
19513+2304   CHE 167     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match is actually a new pair. However, his pair 19500+2304 =    Bko2011c
                         Anon 9 is actually CHE 167.                                                     
19513+2222   BKO1005     Incorrectly identified by Berko as 19517+2223CHE 171.                   Bko2011c
19513+1638   BPM1718     [PM2000] 2038336 + [PM2000] 2036969.                                    Gvr2010 
19513+1631   BPM1716     AB: [PM2000] 2038207 + [PM2000] 2038105.                                Gvr2010 
             BPM1717     BC: [PM2000] 2038105 + [PM2000] 2037311.                                Gvr2010 
19513+1451   BPM1719     [PM2000] 2038924 + [PM2000] 2039987.                                    Gvr2010 
19514+3434   J  1161     Pair not found in GSC.                                                  Bko2009d
19514+2227   BKO1009     Incorrectly identified by Berko as 19511+2228CHE 163.                   Bko2011c
19514+1759   BPM1722     [PM2000] 2040136 + [PM2000] 2040751.                                    Gvr2010 
19514+1746   BPM1721     [PM2000] 2040089 + [PM2000] 2040162.                                    Gvr2010 
19514+1629   BPM1720     [PM2000] 2039557 + [PM2000] 2040049.                                    Gvr2010 
19514+1155   BPMA194     [PM2000] 2039580 + [PM2000] 2039263.                                    Gvr2010 
19514-0215   BAL 254     J 2560.                                                                         
19515+7607   LDS1920     NLTT 48431/48440.                                                               
19515+2728   EVS  43     Primary is the Cepheid SV Vul.                                          Evs2016a
19515+2240   CHE 168     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match is actually CHE 174.                                      Bko2011c
19515+1809   BPMA195     [PM2000] 2041250 + [PM2000] 2043601.                                    Gvr2010 
19515+1723   BPM1726     [PM2000] 2041498 + [PM2000] 2040161.                                    Gvr2010 
19515+1632   BPM1723     [PM2000] 2040753 + [PM2000] 2041077.                                    Gvr2010 
19515+1520   BPM1725     [PM2000] 2041375 + [PM2000] 2042816.                                    Gvr2010 
19515+1250   BPM1724     [PM2000] 2041272 + [PM2000] 2042752.                                    Gvr2010 
19516+1712   BPM1728     [PM2000] 2042331 + [PM2000] 2040992.                                    Gvr2010 
19516+1647   BPM1727     [PM2000] 2041712 + [PM2000] 2041440.                                    Gvr2010 
19517+3404   HJ 1447     AB: SEI 704.                                                            Nsn2017b
19517+3108   ES  357     A spectroscopic binary.                                                         
19517+2257   CHE 170     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. Berko's match to this pair was correct.       Bko2011c
                         See Hartkopf (2012).                                                    Hrt2012b
19517+2240   BKO1015     Incorrectly identified by Berko as 19518+2240CHE 174.                   Bko2011c
19517+2239   BKO1015     AC: Originally 19517+2240 BKO1015, but primary found to match that of           
                         19517+2239 TDT1806.                                                             
                         Incorrectly identified by Berko as 19518+2240CHE 174.                   Bko2011c
19517+2223   CHE 171     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match to this pair was actually a new pair.                     Bko2011c
19517+1758   BPM1731     [PM2000] 2043650 + [PM2000] 2042320.                                    Gvr2010 
19517+1626   BPM1729     [PM2000] 2042788 + [PM2000] 2041385.                                    Gvr2010 
19517+1209   BPM1730     [PM2000] 2043474 + [PM2000] 2044018.                                    Gvr2010 
19518+2344   CHE 172     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
19518+2303   CHE 173     Berko's match is actually CHE 175.                                      Bko2011c
                         See Hartkopf (2012).                                                    Hrt2012b
19518+2240   CHE 174     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match to this pair was actually a new pair.                     Bko2011c
19518+1744   BPM1736     [PM2000] 2044900 + [PM2000] 2043861.                                    Gvr2010 
19518+1709   BPM1732     [PM2000] 2044107 + [PM2000] 2043060.                                    Gvr2010 
19518+1658   BPM1735     [PM2000] 2044858 + [PM2000] 2044356.                                    Gvr2010 
19518+1631   BPM1734     [PM2000] 2044309 + [PM2000] 2044090.                                    Gvr2010 
19518+1416   BPM1733     [PM2000] 2044301 + [PM2000] 2044754.                                    Gvr2010 
19518+0537   OSO 112     G023-014. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates                                                        Oso2004 
19518+0204   BAL1533     J 1689.                                                                         
19519+1810   BPM1740     [PM2000] 2045761 + [PM2000] 2044872.                                    Gvr2010 
19519+1643   BPM1737     [PM2000] 2044914 + [PM2000] 2043888.                                    Gvr2010 
19519+1536   BPM1738     [PM2000] 2044928 + [PM2000] 2044169.                                    Gvr2010 
19519+1029   BPM1739     [PM2000] 2045664 + [PM2000] 2046704.                                    Gvr2010 
19520+3802   HJ 1448     HJL 268.                                                                HJL1986 
                         SEI 707.                                                                Nsn2017b
19520+1623   BPM1741     [PM2000] 2046117 + [PM2000] 2046563.                                    Gvr2010 
19520+1543   BPM1742     [PM2000] 2046293 + [PM2000] 2045791.                                    Gvr2010 
19520+1536   BPM1743     [PM2000] 2046492 + [PM2000] 2047260.                                    Gvr2010 
19520+1309   BPM1746     [PM2000] 2047161 + [PM2000] 2047361.                                    Gvr2010 
19521+2918   OSO 113     G125-039. AB, AC, AF, AH, AK, and AL are not common proper motion               
                         pairs, based on comparison with POSS2 red plates                        Oso2004 
19521+2806   RAG   3     Primary is exoplanet host, P=465d. Raghavan (2006) consider as CPM.     Rag2006 
                         However; he does not measure PM or parallax; only ptm evidence.         Tok2014d
19521+1655   BPM1747     [PM2000] 2047296 + [PM2000] 2048285.                                    Gvr2010 
19521+1612   BPM1748     [PM2000] 2047299 + [PM2000] 2045770.                                    Gvr2010 
19521+1546   BPM1749     [PM2000] 2047469 + [PM2000] 2046243.                                    Gvr2010 
19521+1509   BPM1744     AB: [PM2000] 2047284 + [PM2000] 2046768.                                Gvr2010 
             BPM1745     BC: [PM2000] 2046768 + [PM2000] 2045704.                                Gvr2010 
19521+1235   BPMA196     [PM2000] 2048309 + [PM2000] 2049449.                                    Gvr2010 
19522+2309   BKO1025     Incorrectly identified by Berko as 19523+2307CHE 175.                   Bko2011c
19522+6726   OSO 114     G260-036. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates                                                        Oso2004 
19522+1715   BPM1756     AB: [PM2000] 2049253 + [PM2000] 2049852.                                Gvr2010 
             BPM1757     AC: [PM2000] 2049253 + [PM2000] 2048637.                                Gvr2010 
             BPM1758     BC: [PM2000] 2049852 + [PM2000] 2048637.                                Gvr2010 
19522+1703   BPM1750     [PM2000] 2048382 + [PM2000] 2049682.                                    Gvr2010 
19522+1616   BPM1754     [PM2000] 2048814 + [PM2000] 2047304.                                    Gvr2010 
19522+1547   BPM1752     [PM2000] 2048515 + [PM2000] 2048489.                                    Gvr2010 
19522+1519   BPM1751     [PM2000] 2048432 + [PM2000] 2049365.                                    Gvr2010 
19522+1511   BPM1755     [PM2000] 2049011 + [PM2000] 2049913.                                    Gvr2010 
19522+1452   BPM1753     [PM2000] 2048756 + [PM2000] 2047600.                                    Gvr2010 
19522+1153   BPM1762     [PM2000] 2049511 + [PM2000] 2050090.                                    Gvr2010 
19523+4545   KU  125     B is BD+45@2993.                                                                
19523+4445   KOI 137     AB, AD: Adams et al. (2012) theta values corrected to 360-theta         Adm2012 
                         (reported by Dressing et al. (2014).                                    Dre2014 
19523+2307   CHE 175     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match to this pair was actually a new pair.                     Bko2011c
19523+2249   CHE 176     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match to this pair was actually a new pair.                     Bko2011c
19523+1637   BPM1760     [PM2000] 2049691 + [PM2000] 2049238.                                    Gvr2010 
19523+1549   BPM1763     AB: [PM2000] 2050093 + [PM2000] 2049997.                                Gvr2010 
             BPM1764     AC: [PM2000] 2050093 + [PM2000] 2051395.                                Gvr2010 
19523+1514   BPM1759     [PM2000] 2049565 + [PM2000] 2049728.                                    Gvr2010 
19523+1417   BPM1761     [PM2000] 2049737 + [PM2000] 2049712.                                    Gvr2010 
19523+1021   STF2590     AB: Also called J 126. ab: A faint pair 6s p, 2' n of                           
                         STF 2590. ab renamed CD by USNO 06/29/99.                                       
                         AB: H 2  28.                                                            MEv2010 
19524+4633   DEA 306     JKA  95. KIC 9788210/9788227.                                                   
19524+2551   STT 388     Statistically the same parallax within the errors would indicate the            
                         components are physical.                                                        
19524+1840   9 Sge       Aslanov et al. (1984 SvAL 10, 278), Underhill (1995 ApJS 100, 433),             
                         and especially Underhill & Matthews (1995 PASP 107, 513) discuss a              
                         possible 78d orbital period for this system.  Another period, 32.5d,            
                         was found in photometric and radial velocity measurements by Aslanov &          
                         Barannikov (1992 SvAL 18, 58).  However, because of the considerable            
                         scatter in the measurements plus  evidence for wind related line                
                         profile variations (Fullerton 1990), we tentatively place the star in   Ful1990 
                         the "SB1?" category.                                                    Msn1998a
19524+1722   BPM1767     [PM2000] 2051000 + [PM2000] 2050361.                                    Gvr2010 
19524+1702   BPM1766     [PM2000] 2050796 + [PM2000] 2051191.                                    Gvr2010 
19524+1548   BPM1765     [PM2000] 2050635 + [PM2000] 2051144.                                    Gvr2010 
19524+1246   BRT1329     J 2562.                                                                         
19525+2250   BKO1030     AB: Incorrectly identified by Berko as 19523+2249CHE 176.               Bko2011c
19525+2227   HO  580     A is a semiregular variable. Aka L    66.                                       
19525+1612   BPM1768     [PM2000] 2052165 + [PM2000] 2052085.                                    Gvr2010 
19525+1551   BPM1769     [PM2000] 2052425 + [PM2000] 2051858.                                    Gvr2010 
19525+0100   EVS   2     1975.402: oblate correlation peak                                       Bla1977a
                         Primary is Cepheid eta Aql.                                                     
                         Masses are 5.7 and 2.3 Msun. Estimated period = 866y,                           
                         a = 200au = 0.73".                                                      Evs2013 
                         NPOI Limb-darkened diameter 1.73 +/- 0.05 mas,                          NOI1999 
                         R = 66.  +/- 22. \rsun.                                                         
                         NPOI Limb-darkened diameter 1.69 +/- 0.04 mas.                          NOI2001a
                         NPOI Limb-darkened diameter 1.804 +/- 0.007 mas, Sp = G0III,            NOI2018 
                         Teff = 6329 +/-126 K, M = 4.24 +/- 0.58 \msun, Age = 0.15 +/- 0.05 Gyr.         
19525+0039   STF2589     H 2  95.                                                                MEv2010 
19526+4039   KOI2939     KID 5473556 is an eclipsing binary with a single observed planetary     KOI2012b
                         transit (Welsh et al 2012) and is no longer listed in the KOI catalog.  Dre2014 
19526+1809   BPMA197     [PM2000] 2052974 + [PM2000] 2055546.                                    Gvr2010 
19526+1652   BPM1770     AB: [PM2000] 2053641 + [PM2000] 2054254.                                Gvr2010 
             BPM1771     BC: [PM2000] 2054254 + [PM2000] 2052895.                                Gvr2010 
19526+1539   BPMA198     [PM2000] 2053426 + [PM2000] 2051303.                                    Gvr2010 
19526-5458   DUN 227     B is CPD-55@9222.                                                               
19527+2336   CHE 177     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko was unable to find a match to this pair.                          Bko2011c
19527+1848   J   151     J 1217.                                                                         
19527+1638   BPM1772     [PM2000] 2054272 + [PM2000] 2053470.                                    Gvr2010 
19527+1607   BPM1773     [PM2000] 2054329 + [PM2000] 2053976.                                    Gvr2010 
19527+1519   BPM1774     [PM2000] 2054371 + [PM2000] 2054914.                                    Gvr2010 
19527+1026   BPM1775     [PM2000] 2054880 + [PM2000] 2053802.                                    Gvr2010 
19528+6411   STF2604     H N 120.                                                                MEv2010 
19528+2246   CHE 178     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match to this pair was correct.                                 Bko2011c
19528+1856   J  1177     TDT1825.                                                                        
19528+1542   BPM1777     [PM2000] 2055503 + [PM2000] 2054602.                                    Gvr2010 
19528+1257   BPM1776     [PM2000] 2055493 + [PM2000] 2055245.                                    Gvr2010 
19529+4105   HD188307    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
                         Spectroscopic solution to these astrometric pairs given by Griffin      Grf2013a
                         (2013). Periods match "tolerably well," other common elements less so.          
19529+3957   SWB   1     Primary is the eclipsing binary KIC 4862625 (P=20d), which hosts a              
                         transiting circumbinary planet (P = 138.317 +0.040/-0.027 d). Planet            
                         mass < 169 Mearth (0.531 Mjup), planetary system age ~2 Gyr. The B              
                         component is a close visual pair, separation <0.4"; radial velocities           
                         confirm AB as a bound pair. Component parameters, based on model                
                         fitting, are as follows:                                                        
                         Aa = F dwarf, radius 1.734 +/- 0.044 Rsun, mass 1.528 +/- 0.087 Msun            
                         Ab = M dwarf, radius 0.378 +/- 0.023 Rsun, mass 0.408 +/- 0.024 Msun            
                         Ba = G2 dwarf, mass ~0.99 Msun                                                  
                         Bb = M2 dwarf, mass ~0.51 Msun                                          Swb2013 
19529+1702   BPM1778     [PM2000] 2056548 + [PM2000] 2055915.                                    Gvr2010 
19529+1600   BPM1780     [PM2000] 2056997 + [PM2000] 2057151.                                    Gvr2010 
19529+1521   BPM1779     [PM2000] 2056628 + [PM2000] 2056911.                                    Gvr2010 
19529+1425   A  1660     The pair AB has not been seen since discovery.                                  
19529+1239   BPMA199     [PM2000] 2056541 + [PM2000] 2055785.                                    Gvr2010 
19530+4736   KOI 251     AC: Adams et al. (2012) theta values corrected to 360-theta             Adm2012 
                         (reported by Dressing et al. (2014).                                    Dre2014 
19530+1425   BPM1781     [PM2000] 2057181 + [PM2000] 2057281.                                    Gvr2010 
19531+5430   STI2471     CD: Previously known as STI2471a.                                               
19531+1704   BPM1782     [PM2000] 2058476 + [PM2000] 2059570.                                    Gvr2010 
19531+1615   BPM1783     AB: [PM2000] 2059096 + [PM2000] 2058344.                                Gvr2010 
             BPM1784     BC: [PM2000] 2058344 + [PM2000] 2058659.                                Gvr2010 
19531-1436   CHR  90     This is a third component in the eclipsing (Algol-type) and                     
                         spectroscopic binary V505 Sgr, P = 1.18d.                                       
                         Cvetkovic et al. (2010) derive both short- and long-period solutions    Cve2010b
                         (29.14 and 94.24y, respectively). The 29y orbit does not agree with             
                         the light-time effect, so was rejected in favor of the 94y solution.            
                         Assuming a parallax of 8.40 +/- 0.57 (van Leeuwen 2007, A&A 474, 653),          
                         this solutuion yields a mass sum of 7.0 +/- 1.4 Msun.                           
19531-2528   B   454     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.56 +/- 0.97, 2.48, and 1.10 Msun, respectively.             Mlk2012 
19532+2223   CHE 179     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match to this pair was actually a new pair.                     Bko2011c
             BKO1035     BC and BD: Originally 19529+2221 BKO1035AB and AC, but primary found            
                         to be B component of 19532+2223 CHE 179.                                        
                         BC: Incorrectly identified by Berko as 19532+2223 CHE 179AB.            Bko2011c
19532+2017   H 3 105     H III 105. STF2595 rej. There is a 10th magnitude star 37.0@ in 24.0".          
19532+1440   BPM1785     [PM2000] 2059559 + [PM2000] 2060328.                                    Gvr2010 
19532+1439   BPM1786     [PM2000] 2059648 + [PM2000] 2059009.                                    Gvr2010 
19532+1301   BPM1787     [PM2000] 2059831 + [PM2000] 2058481.                                    Gvr2010 
19533+4118   DEA 455     JKA  96. KIC 6067321/6067282.                                                   
19533+1630   BPM1788     [PM2000] 2060590 + [PM2000] 2060997.                                    Gvr2010 
19533+0820   AG  241     TDT1826. An incorrect cross reference (BD+07 4270 rather than 4278)             
                         resulted in the AG pair being assigned incorrect coordinates and its            
                         later "rediscovery" as a Tycho pair. The merged pair was assigned the   TYC2002 
                         AG discovery designation (as this long preceded the TDT designation),           
                         but together with the correct WDS designation.                                  
19534+6052   VAT   4     Aka ES 1797.                                                                    
19534+4740   KOI 106     AB: Adams et al. (2012) theta values corrected to 360-theta             Adm2012 
                         (reported by Dressing et al. (2014).                                    Dre2014 
19534+2246   CHE 180     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match to this pair was actually a new pair.                     Bko2011c
19534+2020   STFA 48     STTA193. B is BD+19@4196.                                                       
             GUI  28     AC: The C component is 19532+2017H 3 105.                                       
             STFA 48     AB: H 5 106.                                                            MEv2010 
19534+1637   BPM1789     [PM2000] 2061446 + [PM2000] 2062442.                                    Gvr2010 
19534-0600   STF2591     B is BD-06@5295.                                                                
19535+2405   DJU   4     13 Vul.                                                                         
                         Additional notes may be found in Muller (1955).                         Mlr1955c
19535+1846   MAA   2     Aka SKF1159. First noted by van Maanen.                                 Maa1935 
19535+1810   BPMA200     [PM2000] 2063230 + [PM2000] 2065902.                                    Gvr2010 
19535+1436   BPM1790     AB: [PM2000] 2063073 + [PM2000] 2062054.                                Gvr2010 
             BPM1791     BC: [PM2000] 2062054 + [PM2000] 2062687.                                Gvr2010 
19536+5943   STTA194     B is BD+59@2136. A is a spectroscopic binary.                                   
19536+1204   BPM1792     [PM2000] 2063672 + [PM2000] 2062566.                                    Gvr2010 
19537+4504   KOI2421     The system hosts a 0.7 Rearth planet candidate with a 2.3 day orbit             
                         (Batalha et al. 2013). We detected two companions 0.42 and 2.62 Ks      KOI2013a
                         mags fainter than KOI 2421 at separations of 1".12 and 4".0,                    
                         respectively. The closer companion is predicted to be Kp = 15.1 (dKp =          
                         0.7), the farther companion Kp = 17.8 (dKp = 3.5). Due to the similar           
                         brightness of the innermost companion and KOI2421, this system will             
                         require a significant dilution correction. If all light from the                
                         innermost companion is captured in the Kepler aperture and the planet           
                         orbits the target star, the planet radius measurement will need to be           
                         increased by 23% to account for dilution. KOI2421 does not exhibit a            
                         large source offset during transit, which lends support to the theory           
                         that the planet candidate orbits the target star, but the system                
                         should be inspected closely to confirm this.                            Dre2014 
19537+2242   BKO1041     Incorrectly identified by Berko as 19534+2246CHE 180.                   Bko2011c
19537+1502   BPM1794     AB: [PM2000] 2065309 + [PM2000] 2066070.                                Gvr2010 
             BPM1795     BC: [PM2000] 2066070 + [PM2000] 2065752.                                Gvr2010 
19537+1036   BPM1793     [PM2000] 2064957 + [PM2000] 2065589.                                    Gvr2010 
19538+2328   BKO1042     Incorrectly identified by Berko as 19540+2333CHE 182.                   Bko2011c
19538+2237   COU 825     There was an error in Chevalier's coordinates for 19541+2238 CHE 184,   Che1908 
                         due to incorrect plate center coordinates. After correcting for this            
                         error, the pair was found to match COU 825AC. In addition, there was            
                         a trigonometric error in deriving theta; the correct value is                   
                         180deg - theta.  Measures have been merged.  Berko's match is actually  Bko2011c
                         a new pair.                                                             Hrt2012b
19538+1820   BPM1798     [PM2000] 2066004 + [PM2000] 2065357.                                    Gvr2010 
19538+1725   BPM1799     [PM2000] 2066009 + [PM2000] 2064812.                                    Gvr2010 
19538+1628   BPM1797     [PM2000] 2065652 + [PM2000] 2064970.                                    Gvr2010 
19538+1449   BPM1796     [PM2000] 2065744 + [PM2000] 2065516.                                    Gvr2010 
19539+4425   MCY   3     Aa,Ab: Discovery designation is per Todd Henry 03/02/98.                        
                         Aa,Ab: LSPM J1953+4424 = GJ 1245. Law et al (2008) derive a distance    Law2008 
                         of 4.54 +0.02/-0.02 pc and a projected separation of                            
                         4.6 +0.05/-0.05 au. Estimated spectral types are M5 and M8.5.                   
             GIC 159     AB = the red dwarf binary G208-044/G208-045 = GJ 1245AB = GIC 160.              
                         The A component is the variable star V1581 Cyg.                                 
                         AB: NLTT 48414/48415                                                    Chm2004 
                         Both the A and B components are active M5 stars, and exhibit an                 
                         average of 3.0 and 2.6 flares per day, respectively, based on Kepler            
                         short-cadence observations.                                             Lur2015 
19539+2317   CHE 181     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match is actually a new pair. However, his pair 19536+2316 =    Bko2011c
                         Anon 52 is actually CHE 181.                                                    
19539+1620   BPM1804     [PM2000] 2066826 + [PM2000] 2065990.                                    Gvr2010 
19539+1613   BPM1800     [PM2000] 2066653 + [PM2000] 2066409.                                    Gvr2010 
19540+2333   CHE 182     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match to this pair was actually a new pair.                     Bko2011c
19540+2309   CHE 183     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a trigonometric                
                         error in deriving theta; the correct value is 180deg - theta.           Hrt2012b
                         Berko's match to this pair was correct.                                 Bko2011c
19540+1847   J  3028     Center of a group of stars of magnitudes 14 to 16.                      J__1945 
19540+1741   BPM1801     AB: [PM2000] 2068113 + [PM2000] 2067893.                                Gvr2010 
             BPM1802     BC: [PM2000] 2067893+ [PM2000] 2066682 .                                Gvr2010 
19540+1726   BPMA201     [PM2000] 2068277 + [PM2000] 2070837.                                    Gvr2010 
19540+1635   BPMA202     [PM2000] 2068432 + [PM2000] 2066606.                                    Gvr2010 
19540+1346   BPM1803     [PM2000] 2067904 + [PM2000] 2066917.                                    Gvr2010 
19540-3051   BRT3088     A likely plate flaw.                                                    Grv2021b
19541+1614   BPM1805     AB: [PM2000] 2069006 + [PM2000] 2068605.                                Gvr2010 
             BPM1806     BC: [PM2000] 2068605 + [PM2000] 2068059.                                Gvr2010 
19541+1238   BPM1807     [PM2000] 2069401 + [PM2000] 2068852.                                    Gvr2010 
19541+0733   BRT2184     J 3026.                                                                         
19541-0834   HJ  900     56 Aql.                                                                         
19542+1755   BPM1808     [PM2000] 2069645 + [PM2000] 2069393.                                    Gvr2010 
19542+1305   BPM1810     [PM2000] 2070053 + [PM2000] 2070255.                                    Gvr2010 
19542+1207   BPM1809     [PM2000] 2069951 + [PM2000] 2069716.                                    Gvr2010 
19542+0828   SCA 163     ksi Aql = 59 Aql = Libertas.                                                    
                         CHARA Array Limb-darkened diameter  1.726 +/- 0.008 mas.                CIA2009a
                         R = 10.45 +/- 0.18 \rsun, L =  49.7 +/-  0.9 \lsun,                             
                         Teff = 4742 +/-  26 K.                                                          
                         NPOI Limb-darkened diameter 1.658 +/- 0.025 mas, Sp = G8III,            NOI2018 
                         R = 10.03 +/- 0.22 \rsun, Teff = 5263 +/- 105 K,                                
                         L = 69.6 +/- 5.6 \lsun, M = 2.05 +/- 0.15 \msun,                                
                         Age = 0.98 +/- 0.18 Gyr.                                                        
19542+0157   HZG  14     AB: B is BD+01@4135.                                                            
                         AB: HJL 269.                                                            HJL1986 
                         AB: SHY 323. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
             ABT9002     Previously known as ABT  14.                                                    
                         HIP 97940. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
19543+4437   KOI3111     This system hosts a 2.1 Rearth planet candidate with a 10.8 day period          
                         and a 1.5 Rearth planet candidate with a 4.3 day period (Burke et al.   KOI2014a
                         2014).                                                                  Dre2014 
19543+1746   BPM1811     [PM2000] 2070700 + [PM2000] 2071132.                                    Gvr2010 
19543+1745   BPMA203     [PM2000] 2071447 + [PM2000] 2068678.                                    Gvr2010 
19543+1719   BPM1815     [PM2000] 2071344 + [PM2000] 2071129.                                    Gvr2010 
19543+1713   COU 324     TDT1840.                                                                        
19543+1630   BPM1814     [PM2000] 2071263 + [PM2000] 2070327.                                    Gvr2010 
19543+1500   BPM1812     [PM2000] 2070727 + [PM2000] 2071004.                                    Gvr2010 
19543+1452   BPM1813     [PM2000] 2070857 + [PM2000] 2070306.                                    Gvr2010 
19543-2356   ALP  33     AC: A is also a spectroscopic binary with a period of 46.8d so is a     Fek2017b
                         triple. The wider C companion shares common proper motion.              AlP2012 
             HJ 2094     AB: The B component is optical based on study of relative motion of             
                         the components using the method of apparent motion parameters.          Kiy2008 
19544+3918   HJ 2909     AD: SEI 720.                                                            Nsn2017b
19544+1741   BPM1817     [PM2000] 2072283 + [PM2000] 2072665.                                    Gvr2010 
19544+1508   BPM1816     [PM2000] 2071994 + [PM2000] 2072489.                                    Gvr2010 
19544+1428   BPM1818     [PM2000] 2072306 + [PM2000] 2071552.                                    Gvr2010 
19545+1624   BPM1821     [PM2000] 2073384 + [PM2000] 2074113.                                    Gvr2010 
19545+1455   BPM1820     [PM2000] 2073203 + [PM2000] 2074070.                                    Gvr2010 
19545+1454   BPM1819     [PM2000] 2072990 + [PM2000] 2072538.                                    Gvr2010 
19546+2529   BRT3350     Originally published as BRT 202.                                        Brt1928 
19546+1753   BPMA204     [PM2000] 2074210 + [PM2000] 2074900.                                    Gvr2010 
19546-0814   STF2594     57 Aql. STFA 47. B is BD-08@5155.                                               
                         Both components are spectroscopic binaries.                                     
                         H 4  14.                                                                MEv2010 
19547+4348   KOI3214     AB:Distance is 471.3+/-95.3/67.9 pc. Ma (Mb) = 1.05(0.78)+/-0.1 \msun.  Hor2024 
19547+1714   BPM1823     [PM2000] 2074943 + [PM2000] 2073801.                                    Gvr2010 
19547+1436   BPM1822     [PM2000] 2074700 + [PM2000] 2074212.                                    Gvr2010 
19547+0708   BU  659     J   132.                                                                J__1955 
19548+3724   SMA 110     Also known as ALI 646.                                                          
                         Primary of SMA 110 is also primary of ES 2118. WDS designation of               
                         ES 2118 changed from 19552+3341;                                                
                         ES 2118 given component designations AB, SMA 110 = AC.                          
19548+2710   BRT 203     A likely plate flaw.                                                    Grv2021b
19548+1759   BPM1824     [PM2000] 2075749 + [PM2000] 2075223.                                    Gvr2010 
19548+1438   BPM1825     [PM2000] 2075983 + [PM2000] 2076047.                                    Gvr2010 
19548-0025   J  2698     Not found by Heintz.                                                    Hei1995 
19549+5049   HU  687     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.34 +/- 1.68, 4.56, and 2.24 Msun, respectively.             Mlk2012 
19549+2513   A   275     POU4139. Recent measures are quite scattered.                                   
19549+1319   BPMA205     AB: [PM2000] 2076502 + [PM2000] 2078249.                                Gvr2010 
             BPMA206     BC: [PM2000] 2078249 + [PM2000] 2078204.                                Gvr2010 
             BPMA207     CD: [PM2000] 2078204 + [PM2000] 2077209.                                Gvr2010 
19550+4152   HO  581     Noted as a spectroscopic binary by Griffin.                             Grf1977a
                         One star, probably the primary, is SB1, P = 155.0 d;                    Hei1981e
                         #1187 in Batten et al.                                                  Bte1989 
                         Muller (1953) corrected an error in the semi-major axis by              Mlr1953a
                         Van Biesbroeck.                                                         VBs1927b
                         Martin et al. (1998) derive component masses 1.304 +/- 0.187 and                
                         1.107 +/- 0.172 Msun.                                                   Mig1998 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.94 +/- 1.61, 2.07, and 0.88 Msun, respectively.             Mlk2012 
                         Astroseismic orbit analysis results in masses of 0.99 +/- 0.01 \msun    XXX2018c
                         for A. 0.767 +/- 0.006 \msun for Ba and 0.66 +/- 0.01 \msun for Bb.             
                         The orbital parallax is 21.9 +/- 0.2 mas.                                       
19550+1154   BPM1826     [PM2000] 2078014 + [PM2000] 2076911.                                    Gvr2010 
19551+2317   CHE 185     There was an error in Chevalier's coordinates due to incorrect          Che1908 
                         plate center coordinates. In addition, there was a reduction error in           
                         converting from (dx,dy) to (rho,theta).                                 Hrt2012b
                         Berko's match to this pair was correct.                                 Bko2011c
19551+1731   BPM1828     [PM2000] 2078540 + [PM2000] 2077770.                                    Gvr2010 
19551+1714   BPM1827     [PM2000] 2078388 + [PM2000] 2079334.                                    Gvr2010 
19552+2232   L    46     Not found by Heintz at IDS position.  It was rediscovered by Harshaw    Hei1990b
                         in 2004 somewhat off in position and about 2.5 magnitudes fainter than  Hsw2004 
                         listed by Lewis.                                                        L__1904 
19552+1823   BPM1830     [PM2000] 2079962 + [PM2000] 2079503.                                    Gvr2010 
19552+1602   BPM1829     [PM2000] 2079533 + [PM2000] 2080199.                                    Gvr2010 
19553+3741   SEI 729     SMA 111.                                                                        
19553+3435   ES  200     SEI 727.                                                                Nsn2017b
19553+2959   HIP  98039  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Griffin (1979).                                                         Grf1979b
19553+2813   BRT 204     19554+2813BRT3351.                                                              
19553+1619   BPM1832     [PM2000] 2080904 + [PM2000] 2080259.                                    Gvr2010 
19553+1604   BPM1831     [PM2000] 2080223 + [PM2000] 2080120.                                    Gvr2010 
19553+0624   STT 532     bet Aql = 60 Aql = Alshain. A is variable.                                      
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
19553-0644   STF2597     Typo in publication of 1997.6001 measure; theta value corrected by              
                         author.                                                                 TtB2000 
19556+5226   STF2605     psi Cyg = 24 Cyg                                                                
                         AB: H 2  15.                                                            MEv2010 
19557+4024   HJ  604     B is BD+40@3949. See note in BDS.                                       Bu_1906 
19557+3443   HLM  33     AB: SEI 731.                                                                    
                         AC: SEI 730.                                                                    
                         Scheiner by mistake makes Dec (1900) +34d 37m.                          Es_1925a
19557+2439   HJ 1453     Not found in 1905 (Burnham).                                            Bu_1906 
19558+3803   SMA 112     Also known as ALI 648.                                                          
19558+1527   BPM1833     [PM2000] 2085595 + [PM2000] 2086046.                                    Gvr2010 
19558+1320   BPM1834     [PM2000] 2085597 + [PM2000] 2085253.                                    Gvr2010 
19559+2500   COU1037     Docobo et al. (2010) derive a dynamic parallax of 11.36 +/- 0.30  mas   Doc2010h
                         and a total mass of 1.73 +/- 0.39 Msun.                                         
19559+1723   BPMA208     AB: [PM2000] 2085728 + [PM2000] 2087915.                                Gvr2010 
             BPMA209     BC: [PM2000] 2087915 + [PM2000] 2089247.                                Gvr2010 
19559+1712   BPM1836     [PM2000] 2086312 + [PM2000] 2086821.                                    Gvr2010 
19559+1459   BPM1837     [PM2000] 2086324 + [PM2000] 2085986.                                    Gvr2010 
19559+1256   BPM1835     [PM2000] 2085795 + [PM2000] 2085940.                                    Gvr2010 
19559+1254   BPMA210     [PM2000] 2086409 + [PM2000] 2083932.                                    Gvr2010 
19559+1101   BPMA211     [PM2000] 2086233 + [PM2000] 2088528.                                    Gvr2010 
19560+2038   A  2790     CD follows AB by 20s and is 7' north.                                           
19560+1445   BPM1838     [PM2000] 2087246 + [PM2000] 2086547.                                    Gvr2010 
19561+1442   BPM1839     [PM2000] 2087654 + [PM2000] 2086919.                                    Gvr2010 
19561+0418   OSO 115     G092-039. Neither is a common proper motion pair, based on astrometry           
                         and color                                                               Oso2004 
19562+1659   BPMA212     [PM2000] 2088419 + [PM2000] 2086788.                                    Gvr2010 
19562+1419   BPM1840     [PM2000] 2088611 + [PM2000] 2088808.                                    Gvr2010 
19562-2206   BRT1556     CD-22@14366.                                                                    
19563+3505   BU  980     eta Cyg = 21 Cyg                                                                
             HJ 1455     AD: Rectilinear solution by Friedman et al. (2012).                     USN2012a
19563+1718   BPM1842     [PM2000] 2089692 + [PM2000] 2090208.                                    Gvr2010 
19563+1636   BPMA213     [PM2000] 2089467 + [PM2000] 2087880.                                    Gvr2010 
19563+1353   BPM1841     [PM2000] 2089531 + [PM2000] 2089426.                                    Gvr2010 
19563-3137   HIP  98108  Acceleration and SB, unresolved here.                                   Tok2013b
19564+1750   BPMA214     [PM2000] 2090304 + [PM2000] 2091201.                                    Gvr2010 
19564+1705   BPMA215     [PM2000] 2090948 + [PM2000] 2089897.                                    Gvr2010 
19564+1639   BPM1843     [PM2000] 2090604 + [PM2000] 2090444.                                    Gvr2010 
19564+1533   BPM1844     [PM2000] 2090904 + [PM2000] 2091974.                                    Gvr2010 
19564+1452   BPM1845     [PM2000] 2090960 + [PM2000] 2091674.                                    Gvr2010 
19565+1613   BPMA216     [PM2000] 2091941 + [PM2000] 2094542.                                    Gvr2010 
19565+1311   BPM1846     [PM2000] 2091800 + [PM2000] 2091946.                                    Gvr2010 
19566+5910   GIC 161     LDS2784. G230-021/G230-020.                                                     
                         NLTT 48502/48501                                                        Chm2004 
19566+4057   KOI 148     AB, AC, AE: Adams et al. (2012) theta values corrected to 360-theta     Adm2012 
                         (reported by Dressing et al. (2014).                                    Dre2014 
19567+6346   VAT   5     ES 1850.                                                                        
19567+1751   BPM1847     [PM2000] 2093315 + [PM2000] 2093368.                                    Gvr2010 
19567+1721   BPM1848     [PM2000] 2093726 + [PM2000] 2093471.                                    Gvr2010 
19568+1737   BPM1850     [PM2000] 2094706 + [PM2000] 2095204.                                    Gvr2010 
19568+1436   BPM1849     [PM2000] 2094129 + [PM2000] 2094069.                                    Gvr2010 
19569+1722   BPM1854     [PM2000] 2095759 + [PM2000] 2096417.                                    Gvr2010 
19569+1627   BPM1851     [PM2000] 2094936 + [PM2000] 2095689.                                    Gvr2010 
19569+1451   BPM1853     [PM2000] 2095327 + [PM2000] 2095644.                                    Gvr2010 
19569+1331   BPM1852     [PM2000] 2095103 + [PM2000] 2095107.                                    Gvr2010 
19570+1747   BPMA217     [PM2000] 2096579 + [PM2000] 2096191.                                    Gvr2010 
19571+3105   AG  243     B is BD+30@3819.                                                                
19571+1809   BPM1855     [PM2000] 2096824 + [PM2000] 2095800.                                    Gvr2010 
19571+1643   BPMA218     [PM2000] 2097261 + [PM2000] 2097365.                                    Gvr2010 
19571-2834   LDS4823     NLTT 48456/48457                                                        Chm2004 
19572+4747   DEA 481     JKA  99. KIC 10622511/10557342.                                                 
19572+4416   BLL  43     A is variable.                                                                  
19572+4022   BU 1474     A is a spectroscopic binary. B is BD+39@3966.                                   
19572+3646   SEI 743     B is BD+36@3782.                                                                
19573+4123   KOI 306     AB, AC: Adams et al. (2012) theta values corrected to 360-theta         Adm2012 
                         (reported by Dressing et al. (2014).                                    Dre2014 
19573+1729   BPMA219     [PM2000] 2099058 + [PM2000] 2102123.                                    Gvr2010 
19573+1713   BPM1858     [PM2000] 2099127 + [PM2000] 2098393.                                    Gvr2010 
19573+1614   BPM1860     [PM2000] 2099671 + [PM2000] 2100405.                                    Gvr2010 
19573+1609   BPM1859     [PM2000] 2099235 + [PM2000] 2098969.                                    Gvr2010 
19573+1508   BPM1862     [PM2000] 2099687 + [PM2000] 2100233.                                    Gvr2010 
19573+1500   BPM1856     [PM2000] 2098899 + [PM2000] 2098775.                                    Gvr2010 
19573+1459   BPM1857     [PM2000] 2099028 + [PM2000] 2099545.                                    Gvr2010 
19573+1319   BPM1861     [PM2000] 2099685 + [PM2000] 2099066.                                    Gvr2010 
19573+0513   A   604     Aitken (1937) put together into a single mean his measures in the       A__1937b
                         years 1931 and 1934, but these should be considered separately, as a            
                         reversal of quadrant may have taken place between. Period is probably           
                         of order 50y.                                                           Mlr1954a
                         Toledo's elements, residuals, and ephemeris are mutually                        
                         inconsistent. The quoted elements have been reconstructed by Finsen             
                         to fit the published residuals.                                         Zae1963 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.13 +/- 2.53, 3.07, and 1.10 Msun, respectively.             Mlk2012 
19574+4507   CBL  80     JKA 100. KIC 8909853/8909876.                                                   
19574+1428   BPM1863     [PM2000] 2100467 + [PM2000] 2101415.                                    Gvr2010 
19574+1419   BPM1864     [PM2000] 2100544 + [PM2000] 2100997.                                    Gvr2010 
19574+0128   J  1870     BAL 1537.                                                                       
19575+1739   BPM1867     [PM2000] 2101373 + [PM2000] 2101206.                                    Gvr2010 
19575+1652   BPM1866     [PM2000] 2101180 + [PM2000] 2100444.                                    Gvr2010 
19575+1437   BPM1865     [PM2000] 2100884 + [PM2000] 2099792.                                    Gvr2010 
19576+4711   DEA 366     JKA 101. KIC 10164867/10164839.                                                 
19576+4402   KOI  18     AD: Adams et al. (2012) theta values corrected to 360-theta             Adm2012 
                         (reported by Dressing et al. (2014).                                    Dre2014 
19576+3454   HLM  35     SEI 745.                                                                Nsn2017b
19576+1622   BPM1868     [PM2000] 2101789 + [PM2000] 2101312.                                    Gvr2010 
19576+1539   BPM1870     [PM2000] 2102163 + [PM2000] 2102102.                                    Gvr2010 
19576+1426   BPM1871     [PM2000] 2102641 + [PM2000] 2103428.                                    Gvr2010 
19576+1423   BPMA220     [PM2000] 2101979 + [PM2000] 2099608.                                    Gvr2010 
19576+1202   BPM1869     [PM2000] 2102028 + [PM2000] 2102842.                                    Gvr2010 
19576+0425   BAL2957     Not found at WDS coordinates                                            Hei1992a
19577+3755   HJ 1457     SEI 749.                                                                Nsn2017b
19577+1439   BPM1872     [PM2000] 2103413 + [PM2000] 2104341.                                    Gvr2010 
19578+1652   BPM1873     [PM2000] 2103994 + [PM2000] 2104510.                                    Gvr2010 
19578+1512   BPM1874     AB: [PM2000] 2104490 + [PM2000] 2105137.                                Gvr2010 
             BPM1875     AC: [PM2000] 2104490 + [PM2000] 2105602.                                Gvr2010 
19578+0335   J  2293     Probably BAL2526                                                        Hei1995 
19579+6258   HJ 2923     Single. Burnham measures a star in the field:                           Bu_1906 
                         1905.74, 246.5@, 29.89", 8.0-13.5.                                              
19579+4423   STT 393     B is BD+43@3429.                                                                
19579+4216   STT 392     A is a spectroscopic binary.                                                    
19579+2715   AC   16     STTA195.                                                                        
19579+1804   BPM1877     [PM2000] 2105098 + [PM2000] 2105541.                                    Gvr2010 
19579+1637   BPM1878     [PM2000] 2105365 + [PM2000] 2106475.                                    Gvr2010 
19579+1459   BPM1876     [PM2000] 2104829 + [PM2000] 2105130.                                    Gvr2010 
19579+1154   BPM1879     [PM2000] 2105428 + [PM2000] 2105834.                                    Gvr2010 
19580+1636   BPM1882     AB: [PM2000] 2106066 + [PM2000] 2107128.                                Gvr2010 
             BPM1883     BC: [PM2000] 2107128 + [PM2000] 2107599.                                Gvr2010 
19580+1614   BPM1880     [PM2000] 2105623 + [PM2000] 2106367.                                    Gvr2010 
19580+1442   BPM1881     [PM2000] 2106042 + [PM2000] 2105630.                                    Gvr2010 
19580+0456   A   606     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Period incorrectly given as 125.49 (erratum in Inf. Circ. 93, 1984)     Baz1984b
19581+5355   ARG  35     B is BD+53@2331.                                                                
                         ES  131.                                                                        
19581+1418   BPMA221     [PM2000] 2106958 + [PM2000] 2108130.                                    Gvr2010 
19581+0548   A   607     Not seen for certain after 1936. Needs speckle.                                 
19582+1719   BPM1889     [PM2000] 2108390 + [PM2000] 2108427.                                    Gvr2010 
19582+1329   BPM1884     AB: [PM2000] 2107587 + [PM2000] 2108306.                                Gvr2010 
             BPM1885     AC: [PM2000] 2107587 + [PM2000] 2108263.                                Gvr2010 
             BPM1886     BC: [PM2000] 2108306 + [PM2000] 2108263.                                Gvr2010 
19582+1219   BPM1888     [PM2000] 2107620 + [PM2000] 2107240.                                    Gvr2010 
19582+1203   BPM1887     [PM2000] 2107968 + [PM2000] 2107540.                                    Gvr2010 
19583+3147   KU  126     B is BD+31@3863.                                                                
19583-0037   J  1386     BAL 918.                                                                        
19583-1357   GRE   5     IRAS 19558-1405 = PDS 101 = BZ Sgr                                      Gre1992 
19583-1436   BRT 601     Brt2768.                                                                Brt1947 
19583-5154   DUN 229     B is CPD-52@11587.                                                              
                         Estimated P of AB ~ 400 kyr. B is a spectroscopic binary with P ~ 236d. Tok2022e
19584+3830   J  1070     Primary is eclipsing binary of Algol-type, period 2.6646 d.             Zas2012 
                         SEI 755.                                                                Nsn2017b
19584+3512   Cyg X-1     V1357 Cyg. This is a massive X-ray binary with a probable black hole    Gie1982 
                         companion (Gies & Bolton 1982).                                         Msn1998a
19584+1713   BPM1890     [PM2000] 2109490 + [PM2000] 2110522.                                    Gvr2010 
19584+1235   BPM1891     [PM2000] 2109630 + [PM2000] 2110281.                                    Gvr2010 
19584-5725   DAW  25     Spectrum: G3/5III/IV.                                                           
19585+3553   ROE 146     Also known as COU2209.                                                          
19585+1604   BPM1892     [PM2000] 2111146 + [PM2000] 2110924.                                    Gvr2010 
19585+1400   BPM1893     [PM2000] 2111156 + [PM2000] 2110347.                                    Gvr2010 
19586+4051   KOI2790     This system hosts a 0.9 Rearth planet candidate with a 14.0 day period          
                         (Burke et al. 2014). The approximate increase to the planet radius is   KOI2014a
                         17% assuming that all of the light from the companion is captured in            
                         the Kepler aperture and that the planet orbits the target star.                 
                         KOI2790 does not exhibit a significant source offset during transit.    Dre2014 
19586+3711   COU2410     WDS incorrectly transcribed from paper - should have been +3811                 
19586+1549   BPM1897     [PM2000] 2111847 + [PM2000] 2111671.                                    Gvr2010 
19586+1357   BPM1894     [PM2000] 2111640 + [PM2000] 2111286.                                    Gvr2010 
19586+1356   BPM1895     [PM2000] 2111505 + [PM2000] 2110518.                                    Gvr2010 
19586+1355   BPM1898     [PM2000] 2111883 + [PM2000] 2112449.                                    Gvr2010 
19586+1237   BPM1896     [PM2000] 2111733 + [PM2000] 2110594.                                    Gvr2010 
19587+1034   BPM1899     [PM2000] 2112842 + [PM2000] 2112743.                                    Gvr2010 
19588+4426   KOI 102     AB, AC: Adams et al. (2012) theta values corrected to 360-theta         Adm2012 
                         (reported by Dressing et al. (2014).                                    Dre2014 
19588+4337   KOI2984     This system hosts a 1.1 Rearth planet candidate with a 11.5 day orbit   KOI2014a
                         (Burke et al. 2014).                                                    Dre2014 
19589+1421   BPM1900     [PM2000] 2114305 + [PM2000] 2114887.                                    Gvr2010 
19589-1318   D    31     AC component a.k.a. BU 1476AC.                                                  
19590+3539   SEI 759     HLM  36.                                                                        
19590+1114   BPM1901     [PM2000] 2115322 + [PM2000] 2115349.                                    Gvr2010 
19591+3942   ES 1970     AB: SEI 768.                                                            Nsn2017b
19591+3532   MAD  11     AC: STF 762.                                                            Nsn2017b
19591+1758   BRT1331     J  2566.                                                                        
19591+1450   BPM1902     [PM2000] 2116466 + [PM2000] 2115945.                                    Gvr2010 
19592+1606   BPM1907     [PM2000] 2117189 + [PM2000] 2117644.                                    Gvr2010 
19592+1604   BPM1906     [PM2000] 2117231 + [PM2000] 2117843.                                    Gvr2010 
19592+1419   BPM1903     [PM2000] 2116921 + [PM2000] 2116096.                                    Gvr2010 
19592+1350   BPM1904     AB: [PM2000] 2117182 + [PM2000] 2116519.                                Gvr2010 
             BPM1905     BC: [PM2000] 2116519 + [PM2000] 2117613.                                Gvr2010 
19592-2155   LDS 697     NLTT 48516/48515                                                        Chm2004 
19593+3219   HJ 1461     SEI 764.                                                                Nsn2017b
19593+1613   BPM1908     [PM2000] 2118033 + [PM2000] 2118321.                                    Gvr2010 
19594+2606   BRT3352     Originally published as BRT 205.                                        Brt1928 
19594+1809   BPM1909     [PM2000] 2118526 + [PM2000] 2118664.                                    Gvr2010 
19594+1351   BPM1910     [PM2000] 2118952 + [PM2000] 2119484.                                    Gvr2010 
19594+1214   BPMA222     [PM2000] 2118764 + [PM2000] 2118787.                                    Gvr2010 
19595+2443   BU  469     POU4167. ALADIN shows nothing at the expected coordinates of POU4179.           
                         Pouteau's astrometry and photometry for POU4167 and POU4179 are very    Pou1933 
                         similar and epoch-1900 coordinates differ only in one digit                     
                         (195519.0+2427.1 versus 195559.0+2427.1) - conclude they are the same           
                         pair and coordinate difference is due to a typographical error.                 
19595+1358   BPM1911     [PM2000] 2119417 + [PM2000] 2119886.                                    Gvr2010 
19596+2243   CUD   6     Component A is the central star of the planetary nebula NGC 6853        Skf2013 
                         = Messier 27 = Dumbbell Nebula.                                                 
19596+1720   BPM1912     [PM2000] 2120578 + [PM2000] 2119878.                                    Gvr2010 
19596+1410   BPM1914     [PM2000] 2120691 + [PM2000] 2120230.                                    Gvr2010 
19596+1111   BPM1913     [PM2000] 2120687 + [PM2000] 2121501.                                    Gvr2010 
19597+2450   POU4170     POU4172.                                                                        
19597+1610   BPM1917     [PM2000] 2121164 + [PM2000] 2121739.                                    Gvr2010 
19597+1400   BPM1915     [PM2000] 2121017 + [PM2000] 2120938.                                    Gvr2010 
19597+1355   BPM1916     [PM2000] 2121133 + [PM2000] 2121185.                                    Gvr2010 
19597-3517   ISO  11     the 1 Sgr. A spectroscopic binary, P = 2.10d.                                   
                         The Isobe companion is a third star.                                    Iso1990a
19597-4030   HJ 5159     B is CD-40@13594.                                                               
19598+1553   BPMA223     [PM2000] 2122471 + [PM2000] 2122531.                                    Gvr2010 
19598+1425   BPM1918     [PM2000] 2122365 + [PM2000] 2122177.                                    Gvr2010 
19598-0957   HO  276     Not single, as previously thought.                                              
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.54 +/- 0.13, 2.00, and 1.10 Msun, respectively.             Mlk2012 
19599-3442   I  1410     A: the 2 Sgr                                                                    
20000+1911   RUC  13     CW Sge. Spectral type of resolved companion estimated at G5V.           Ruc2007 
20000+1736   HO  638     Aka SMR   7.                                                            Cgl2024a
                         The unresolved measures were at the former position (20001+1737).       Gii2022 
20001+2410   POU4173/4   Aka POU4176/7.                                                                  
                         Unresolved measures were at the old POU4176/7 position.                 Bko2010b
20001+1737   S   730     B is BD+17@4187.                                                                
                         A is variable.                                                                  
20001+1731   H 4 100     AB: H IV 100. Also known as STF2608. B is BD+17@4184.                           
             BU 1477     13 Sge. A is the irregular variable VZ Sge.                                     
20001+1313   BPMA224     [PM2000] 2124918 + [PM2000] 2124127.                                    Gvr2010 
20001+1245   BPM1919     [PM2000] 2124608 + [PM2000] 2124970.                                    Gvr2010 
20001+1111   HJ 1458     B is BD+10@4133.                                                                
20002+3625   STT 394     AB: SEI 778.                                                            Nsn2017b
20002+1454   BPM1920     AB: [PM2000] 2125495 + [PM2000] 2125884.                                Gvr2010 
20002-5522   I  1041     BC: Rapid direct motion.                                                        
             B   459     BC: Gomez et al. (2016) derive dynamical parallax and  component                
                         masses: 15.36 +/- 0.24 mas, 0.655 +/- 0.005 Msun, 0.643 +/- 0.005 Msun  Doc2016i
20005+5921   JNN 124     Aside from the close companion detected in the AstraLux data, 2MASS             
                         J20003177+5921289 possibly has a wide companion at 14", as noted in             
                         the WDS.                                                                Jnn2012 
20005+1643   BPMA225     [PM2000] 2127672 + [PM2000] 2129933.                                    Gvr2010 
20006+1727   BPM1923     [PM2000] 2128515 + [PM2000] 2128537.                                    Gvr2010 
20006+1657   BPM1921     [PM2000] 2128288 + [PM2000] 2127828.                                    Gvr2010 
20006+1257   BPM1922     [PM2000] 2128371 + [PM2000] 2127737.                                    Gvr2010 
20006+1112   BPM1924     [PM2000] 2129073 + [PM2000] 2128893.                                    Gvr2010 
20006-0911   BRT 554     J  1872.                                                                        
20007+3635   WEB   9     BC: SEI 783.                                                            Nsn2017b
20007+2243   BAK   1     CHARA Array Limb-darkened diameter  0.377 +/- 0.024 mas,                CIA2008c
                         R =  0.788 +/- 0.051 \rsun.                                                     
                         CHARA Array Limb-darkened diameter 0.3848 +/- 0.0055 mas,               CIA2015d
                         L = 0.328 +/- 0.011 \lsun, R = 0.805 +/- 0.016 \rsun,                           
                         Teff = 4875 +/- 43 K, Rp = 1.216 +/- 0.024 \rjup,                               
                         M = 0.846 +/- 0.049 \msun, Mp = 1.162 +/- 0.058 \mjup                           
20008+4500   DEA 468     JKA 102. KIC 8845251/8845205.                                                   
20010+3742   BU 1289     AC: SEI 787.                                                            Nsn2017b
20010+2956   L    32     Measures from Lewis were assigned to both this pair and                 L__1899a
                         19590+2953L    31 in the BDS and ADS. Published coordinates and         Bu_1906 
                         magnitudes are also similar, and only one pair is seen on POSS plates,  A__1932a
                         leading to the conclusion that these are the same system. The L 32              
                         designation was maintained, as its WDS designation was correct.                 
20010+1751   BPM1925     [PM2000] 2131567 + [PM2000] 2131286.                                    Gvr2010 
20011+1551   BPM1928     [PM2000] 2132693 + [PM2000] 2133415.                                    Gvr2010 
20011+1550   BPM1927     [PM2000] 2132620 + [PM2000] 2132660.                                    Gvr2010 
20011+1253   BPM1926     [PM2000] 2132582 + [PM2000] 2132225.                                    Gvr2010 
20012+1642   BPM1929     [PM2000] 2133126 + [PM2000] 2133286.                                    Gvr2010 
20012+1530   BPMA226     [PM2000] 2133727 + [PM2000] 2135156.                                    Gvr2010 
20012-3835   HDO 294     A premature orbit has been computed.                                            
20013+1355   BPM1930     [PM2000] 2133981 + [PM2000] 2134651.                                    Gvr2010 
20014+5006   H 5  47     H V 47. STTA197. 26 Cyg.                                                        
20014+1540   BPM1931     [PM2000] 2134829 + [PM2000] 2135352.                                    Gvr2010 
20014+1234   BPM1932     [PM2000] 2135308 + [PM2000] 2134282.                                    Gvr2010 
20014+1045   TOK  34     Aa,Ab: Close visual pair has estimated period of ~100y.                         
                         Primary is 4.5d SB1.                                                    Tok2006 
             STF2613     A premature orbit has been computed for AB. Period of 2350y.            Tok2006 
20014+0657   STF2612     B is BD+06@4402.                                                                
20015+6449   H 6  38     H VI 38. 64 Dra.                                                                
20015+4018   HJ 1468     SEI 796.                                                                Nsn2017b
20015+1556   BPMA227     [PM2000] 2135687 + [PM2000] 2136381.                                    Gvr2010 
20016+3417   SEI 793     Duplicity not apparent on POSS plate; one component may be either               
                         variable star or flaw on AC Potsdam plate.                                      
20016+1144   BPM1933     [PM2000] 2136500 + [PM2000] 2136117.                                    Gvr2010 
20017+1759   BPM1934     [PM2000] 2137252 + [PM2000] 2136464.                                    Gvr2010 
20017+1746   BPM1935     [PM2000] 2137797 + [PM2000] 2138116.                                    Gvr2010 
20017+1328   BPMA228     [PM2000] 2137438 + [PM2000] 2138515.                                    Gvr2010 
20017-0012   H 1  93     H I 93.                                                                         
20018-0354   J   154     J 1693.                                                                         
20019+4052   STTA196     B is BD+40@3983.                                                                
20019+3139   AG  245     SEI 795.                                                                Nsn2017b
20019+1651   BPM1938     [PM2000] 2139179 + [PM2000] 2140282.                                    Gvr2010 
20019+1541   BPM1939     [PM2000] 2139324 + [PM2000] 2138901.                                    Gvr2010 
20019+1458   BPM1940     [PM2000] 2139387 + [PM2000] 2139936.                                    Gvr2010 
20019+1428   BPM1936     [PM2000] 2138827 + [PM2000] 2138074.                                    Gvr2010 
20019+1114   BPM1937     [PM2000] 2139165 + [PM2000] 2138770.                                    Gvr2010 
20020+2456   STT 395     16 Vul.                                                                         
                         Additional notes may be found in Fatou (1941).                          Fat1941 
20020+1707   BPM1941     [PM2000] 2139739 + [PM2000] 2139452.                                    Gvr2010 
20020+1702   BPM1942     [PM2000] 2140266 + [PM2000] 2139243.                                    Gvr2010 
20021+5439   MLR 580     EF: Originally 20025+5437 MLR 580, but the primary is the E component           
                         of 20021+5439 ENG  68CE.                                                        
20021+1331   BPMA229     [PM2000] 2140807 + [PM2000] 2142019.                                    Gvr2010 
20021+1300   JNN 281     Estimated age 1000-10000 Myr; masses 0.41 +/- 0.11 and 0.22 +/- 0.06            
                         Msun; a ~4.3 au.                                                        Jnn2014 
20021+1253   BPM1944     [PM2000] 2140849 + [PM2000] 2140682.                                    Gvr2010 
20021+1103   BPM1943     [PM2000] 2140610 + [PM2000] 2140656.                                    Gvr2010 
20022+1543   BPM1945     [PM2000] 2141491 + [PM2000] 2142120.                                    Gvr2010 
20022+1537   BPMA230     [PM2000] 2141290 + [PM2000] 2142846.                                    Gvr2010 
20023+6438   STTA200     65 Dra. B is BD+64@1406.                                                        
20023+4547   LDS6338     NLTT 48621/48622                                                        Chm2004 
20023+1317   BPM1946     [PM2000] 2142316 + [PM2000] 2142633.                                    Gvr2010 
20024+3519   ES  202     Listed in ADS as Aa'.                                                           
                         AB: SEI 808.                                                            Nsn2017d
                         AC: SEI 805.                                                            Nsn2017d
                         AD: SEI 806.                                                            Nsn2017d
                         AN: SEI 807.                                                            Nsn2017d
20024+1744   BPM1947     AB: [PM2000] 2143503 + [PM2000] 2143519.                                Gvr2010 
             BPM1948     BC: [PM2000] 2143519 + [PM2000] 2142464.                                Gvr2010 
20024+1609   BPM1949     AB: [PM2000] 2143229 + [PM2000] 2143605.                                Gvr2010 
             BPM1950     BC: [PM2000] 2143605 + [PM2000] 2143142.                                Gvr2010 
20025+3341   HO  117     AB: SEI 809.                                                            Nsn2017d
             BKO 520     AC: Anon. 33.                                                           Bko2009d
20025+1557   BPM1951     [PM2000] 2144066 + [PM2000] 2143786.                                    Gvr2010 
20025+0149   HJ 5510     A very similar pair is 6s following and of the same declination         Doo1915b
                         This is likely the new DAM 384.                                                 
20026+3352   BKO 521     Anon. 34.                                                               Bko2009d
20026-6541   I  1409     Motion probably in brighter star.                                       Mlo1927A
20027+3355   BKO 522     Anon. 35.                                                               Bko2009d
20027+3349   BKO 523     Anon. 36.                                                               Bko2009d
20027+1439   BPM1952     [PM2000] 2146127 + [PM2000] 2146206.                                    Gvr2010 
20028+6752   LDS2447     rho Dra = 67 Dra                                                                
20028+3158   ES  359     Originally listed as WDS 20037+3145, due to an error in DM number. See          
                         note for WDS 20037+3145 SEI 827.                                                
20028+3142   ES  358     Aka HDS2858.                                                            Dam2012 
20028+1747   BPM1953     [PM2000] 2146475 + [PM2000] 2146201.                                    Gvr2010 
20029+1455   BPM1955     [PM2000] 2147769 + [PM2000] 2146986.                                    Gvr2010 
20029+1416   OSO 116     G023-023. None is a common proper motion pair, based on color and               
                         comparison with POSS2 red plates                                        Oso2004 
20029+1328   BPM1954     [PM2000] 2147064 + [PM2000] 2147698.                                    Gvr2010 
20029+1056   AG  397     B is BD+10@4155.                                                                
20029-2026   LDS 700     NLTT 48599/48600                                                        Chm2004 
20030+3416   BKO 524     Anon. 37.                                                               Bko2009d
20030+2818   BD+27 3593  Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from the Geneva           
                         Extrasolar Planet Search Programs home page.                            HaI2001 
                         HD 190228. Combined astrometric/spectroscopic solution, using                   
                         spectroscopic elements (P,T,e,omega) from Perrier et al. (2003 A&A              
                         410, 1039).                                                             SaJ2011 
20030+1328   BPM1956     [PM2000] 2147965 + [PM2000] 2148051.                                    Gvr2010 
20030+0544   V1295 Aql   MWC 325.  Noted as possible binary (separation > 0".020) by Baines et           
                         al. (2006)                                                              Bns2006 
20031+3421   BKO 525     Anon. 84.                                                               Bko2009d
20031+1656   BPM1957     [PM2000] 2148917 + [PM2000] 2149818.                                    Gvr2010 
20031+1221   BPM1958     [PM2000] 2148969 + [PM2000] 2149755.                                    Gvr2010 
20032+2456   L    33     BD may be +24@3987 if double star is real.                                      
20032+1712   BPM1960     [PM2000] 2149905 + [PM2000] 2149749.                                    Gvr2010 
20032+1125   BPM1959     [PM2000] 2149861 + [PM2000] 2148931.                                    Gvr2010 
20032-2229   BRT1558     CD-22@14449.                                                                    
20033+1736   BPM1962     [PM2000] 2150633 + [PM2000] 2150682.                                    Gvr2010 
20033+1354   BPM1961     [PM2000] 2150343 + [PM2000] 2150626.                                    Gvr2010 
20033+1347   BPM1963     [PM2000] 2151039 + [PM2000] 2151715.                                    Gvr2010 
20034+1631   BPM1964     [PM2000] 2151107 + [PM2000] 2151537.                                    Gvr2010 
20035+3837   COU2533     Also known as TDS1037.                                                          
20035+3601   MCA  59     The Aa,Ab pair has been resolved in only 4 of 11 observations, and              
             STF2624     the positions are discrepant (the large errors presumably result from           
                         a large magnitude difference).  The B and C components were also                
                         observed and appeared to be single.                                     Msn1998a
                         Classification of B and C components are from Hoffleit et al. (1983).   Hof1983 
                         Both A and B are SBs, and there is a small light variation.                     
                         AB: H 1  96.                                                            MEv2010 
                         AD: SEI 826.                                                            Nsn2017d
20035+1408   BPM1965     [PM2000] 2151908 + [PM2000] 2152028.                                    Gvr2010 
20036+2954   LDS6339     HIP 98767. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         CHARA Array Limb-darkened diameter  0.698 +/- 0.019 mas,                CIA2008c
                         R =  1.200 +/- 0.033 \rsun.                                                     
                         NLTT 48652/48646                                                        Chm2004 
20036+1634   BPM1966     [PM2000] 2153071 + [PM2000] 2152942.                                    Gvr2010 
20036-3315   OCC1105     Position angle ambiguous. Either the listed 290+/-10 or 235+/-10.       OCC2014d
20037+3820   HJ 1470     B is BD+37@3743.                                                                
                         SEI 831.                                                                Nsn2017d
20037+3626   SEI 830     The primary is an ellipsoidal variable, V1362 Cyg.                              
20037+3145   SEI 827     BD+31 3915. The Scheiner pair was originally listed as the AD pair of           
                         a multiple which included ES 359AB and BC. However, the Espin pair is   Es_1907a
                         actually BD+31 3905, but was incorrectly given the wrong DM number and          
                         coordinates. The Espin triple has been changed to WDS 20028+3158 and            
                         the Scheiner pair changed to a simple binary pair.                              
20038+1512   BPM1968     [PM2000] 2154916 + [PM2000] 2154870.                                    Gvr2010 
20038+1450   BPM1967     [PM2000] 2154631 + [PM2000] 2154546.                                    Gvr2010 
20039+4411   ES   85     HJ 1478.                                                                        
                         BD+43 3470                                                              Doo1915a
20039+1746   BPM1969     [PM2000] 2155125 + [PM2000] 2154574.                                    Gvr2010 
20039+1604   BPMA231     [PM2000] 2155328 + [PM2000] 2157458.                                    Gvr2010 
20040+1704   BPM1970     [PM2000] 2155941 + [PM2000] 2155917.                                    Gvr2010 
20040-6541   I  1411     LDS 698.                                                                        
20040-7847   HJ 5149     B is CPD-79@1051.                                                               
20041+5428   STI2497     MLR 581.                                                                        
20041+3815   TOR  18     Formerly known as PAN  15.                                                      
20041+1704   STT 592     15 Sge. B is BD+16@4117a.                                                       
                         AB and AC: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
             LIM   3     Aa,Ab: GJ 779 = 15 Sge. Due to the high proper motion of the primary,           
                         Liu et al. (2002) determine that the faint companion shares common      LiM2002 
                         proper motion. Spectral type of the companion is estimated at L4.5 +/-          
                         1.5; assuming the two components are coeval, the inferred mass of the           
                         companion is 55-78 Mjup.                                                        
                         Boccaletti et al (2003) derive spectral type for the companion of L4.5  Boc2003 
                         +/- 1.5 and a mass of 60-72 Mjup.                                               
             BUP 202     AD: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             STT 592     AB, AC: Rectilinear solutions by Hurowitz et al. (2014).                USN2014b
             BUP 202     AD: Rectilinear solution by Friedman et al. (2011).                     USN2011a
20041+5428   STI2497     Rectilinear solution by Hurowitz et al. (2014).                         USN2014b
20041+1700   STF2622     PTT  28, formerly listed at 20051+1641 is in reality this object.       Hei1980a
                         AB: H 2  91.                                                            MEv2010 
20041-4547   CPO  87     B is CD-46@13365.                                                               
20042+3755   TOR  19     Formerly known as PAN  16.                                                      
20042+1148   STF2620     Primary is the eclipsing binary V1470 Aql, P = 0.83499 day.             Zas2010 
20044+3820   TOR  20     Formerly known as PAN  17.                                                      
20044+1742   BPM1971     [PM2000] 2158862 + [PM2000] 2159794.                                    Gvr2010 
20045+1638   BPM1972     AB: [PM2000] 2159565 + [PM2000] 2159415.                                Gvr2010 
             BPM1973     AC: [PM2000] 2159565 + [PM2000] 2159146.                                Gvr2010 
             BPM1974     AD: [PM2000] 2159565 + [PM2000] 2158789.                                Gvr2010 
20045+1254   BPM1975     [PM2000] 2160302 + [PM2000] 2159690.                                    Gvr2010 
20046+3213   HJ 1471     A is variable.                                                                  
20046+1729   BPM1978     [PM2000] 2160685 + [PM2000] 2160495.                                    Gvr2010 
20046+1310   BPM1976     [PM2000] 2160414 + [PM2000] 2160684.                                    Gvr2010 
20046+1159   BPM1977     [PM2000] 2160422 + [PM2000] 2160714.                                    Gvr2010 
20047+2443   BRT3354     Aka J   504.                                                            Dam2013 
                         Originally published as BRT 209.                                        Brt1928 
20047+1238   BPM1979     [PM2000] 2161532 + [PM2000] 2161581.                                    Gvr2010 
20048+1554   STT 397     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         H 5 105.                                                                MEv2010 
20048+1346   BPM1980     [PM2000] 2162289 + [PM2000] 2162775.                                    Gvr2010 
20048+1240   BPM1981     [PM2000] 2162400 + [PM2000] 2161971.                                    Gvr2010 
20049+3431   BKO 526     Anon. 38.                                                               Bko2009d
20049+1258   BPM1982     [PM2000] 2163377 + [PM2000] 2163505.                                    Gvr2010 
20050+5426   MGN   1     Primary is the sdM1.5+WD SB1 Wolf 1130 = GJ 781. Companion is a T8              
                         subdwarf which shows common proper motion. Distance to the system is            
                         15.83 +/- 0.96 pc, metallicity [FE/H] = -0.64 +/- 0.17.                 MGN2013 
20050+1544   BPM1983     AB: [PM2000] 2163894 + [PM2000] 2164598.                                Gvr2010 
             BPM1984     BC: [PM2000] 2164598 + [PM2000] 2164634.                                Gvr2010 
20051+3021   ES  497     BRT 277.                                                                Brt1929b
20051+2629   DOO  77     Misdentification by Doolittle, plus misinterpretation of his note       Doo1915a
                         ("Identified by Burnham with BD+26 3785, but this star is not double.           
                         Near BD+26 3780.") led to identification of this pair with BD+26 3785           
                         and confusion with the similar pair 20054+2716HJ 1473.                          
20051+2039   BUP 203     A is the semiregular variable X Sge, P = 196d.                                  
20051+1822   BPM1985     [PM2000] 2164770 + [PM2000] 2165133.                                    Gvr2010 
20051+1241   BPMA232     [PM2000] 2164926 + [PM2000] 2164997.                                    Gvr2010 
20051-1136   H 4   3     H IV 3.                                                                         
20052+3857   BU 1480     SEI 845.                                                                Nsn2017d
20052+1510   BPM1986     [PM2000] 2165082 + [PM2000] 2165200.                                    Gvr2010 
20052+1137   BPMA233     [PM2000] 2165463 + [PM2000] 2167166.                                    Gvr2010 
20053+1654   BPM1987     [PM2000] 2165845 + [PM2000] 2165583.                                    Gvr2010 
20053+1500   BPM1988     [PM2000] 2166204 + [PM2000] 2165684.                                    Gvr2010 
20054+5807   A   866     Aka ARG 106. B is BD+57@2131.                                                   
                         Pair correctly identified by Marco Scardia.                             Sca2018d
20054+1530   BU   57     A is a spectroscopic binary.                                                    
20054+1424   BPMA234     [PM2000] 2166851 + [PM2000] 2165507.                                    Gvr2010 
20055+5800   WSI 164     Pair assumed to be A   866 which is actually at 20054+5807.             Sca2018d
20056+1554   BPM1989     [PM2000] 2168608 + [PM2000] 2168707.                                    Gvr2010 
20057+5925   HJ 2934     This is a measure of BD+59@2175 with respect to A.                              
20057+3905   J  1072     SEI 855                                                                 Nsn2017d
20057+3536   SHJ 316     STTA199. Based on MacEvoy's (2010) conclusion that SHJ 316 and H 6  59  MEv2010 
                         were the same pair, the 1781 measure of 20097+3701 H 6  59 was merged           
                         this much more well-observed pair.                                              
20057+1719   BPM1991     [PM2000] 2169292 + [PM2000] 2170133.                                    Gvr2010 
20057+1617   BPM1992     [PM2000] 2169312 + [PM2000] 2170016.                                    Gvr2010 
20057+1548   BPM1990     [PM2000] 2168865 + [PM2000] 2168089.                                    Gvr2010 
20058+3605   SEI 853     ALI 169.                                                                        
20058+2313   POU4212     LDS1032.                                                                        
20058+1709   BPM1996     [PM2000] 2170013 + [PM2000] 2170325.                                    Gvr2010 
20058+1647   BPM1995     [PM2000] 2170011 + [PM2000] 2169623.                                    Gvr2010 
20058+1533   BPMA235     [PM2000] 2170149 + [PM2000] 2169943.                                    Gvr2010 
20058+1521   BPM1997     [PM2000] 2170045 + [PM2000] 2169500.                                    Gvr2010 
20058+1519   BPM1993     [PM2000] 2169933 + [PM2000] 2169728.                                    Gvr2010 
20058+1507   BPM1994     [PM2000] 2169976 + [PM2000] 2170120.                                    Gvr2010 
20058-1703   FEN  36     LEO 47. J 1697.                                                                 
20059+3755   ES 2119     SEI 868.                                                                        
20060+3547   BU  440     AB: A is a Wolf-Rayet binary, V1676 Cyg or WR 133, spectral types are           
             SHJ 314     WN5+O9.5I/III. The classification is from Wilson (1949).                WOC1949 
                         Spectroscopic Binary, P = 112.7d.                                               
                         Spectrum of B: B3V. Some components previously known as STF2630.                
                         Classification of the B, D, and F  components are from Hoffleit et al.  Hof1983 
                         (1983).                                                                 Msn1998a
                         STF2630.                                                                        
             BU  429     AD: SEI 859.                                                            Nsn2017d
                         AD: H 3 113.                                                            MEv2010 
             DOO  78     FH: SEI 861.                                                            Nsn2017d
20060+3546   ES   25     AB: SEI 860.                                                            Nsn2017d
             SHJ 315     AD: SEI 863.                                                            Nsn2017d
                         AD: 20060+3545 TOB 166.                                                .        
             ES   25     AF: the F component is the A component of 20060+3547BU  440AB.                  
             SEI 865     EG: Originally 20061+3546 SEI 865, but the B component found to be the          
                         E component of 20060+3546 WAL 127AE. Systems were merged, with a                
                         quadrant flip.                                                                  
20062+5310   ENG  70     B is BD+52@2626.                                                                
20063+4427   TB    1     Aka KIC 8462852, Boyajian's Star or Tabby's Star.                               
20063+1550   BPM1998     [PM2000] 2173542 + [PM2000] 2172670.                                    Gvr2010 
20063+1549   BPMA236     [PM2000] 2174177 + [PM2000] 2175581.                                    Gvr2010 
20063+1403   BPMA237     [PM2000] 2174184 + [PM2000] 2174362.                                    Gvr2010 
20063+1229   BPM1999     [PM2000] 2173956 + [PM2000] 2174482.                                    Gvr2010 
20063+0639   J  1337     J 2569 identical. Corrected position by Heintz.                         Hei1987a
20063-4313   I   662     HIP 99029. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
20064+3558   BUP 204     27 Cyg. SEI 878 is identical.                                                   
20064+1329   BPM2000     [PM2000] 2174396 + [PM2000] 2174568.                                    Gvr2010 
20065+3302   GYL  23     SEI 879. The discrepant Scheiner measure was due apparently to a 2s     Sei1908 
                         error in the Astrographic Catalog right ascension of the primary.               
20066+3544   RAO 518     V453 Cyg.                                                                       
20066+1311   BPM2001     [PM2000] 2176133 + [PM2000] 2175639.                                    Gvr2010 
20066+1147   J   503     BRT1335.                                                                        
20066+0735   STTA198     B is BD+07@4366.                                                                
20067+6214   TOR  22     Formerly known as PAN  19.                                                      
20068+3203   SEI 881     HAU   6.                                                                        
20068-1256   STF2625     H 3  63.                                                                MEv2010 
20068-4031   WG  250     Spectrum A7/8III/IV.                                                            
20068-5615   I  1412     LDS 702.                                                                        
20069+1630   BPM2002     [PM2000] 2178259 + [PM2000] 2177364.                                    Gvr2010 
20069-0855   HDO 156     B is the Mira-type variable RY Cap.                                             
                         Winlock includes this star in a list of new doubles; no description     Win1882 
                         is given other than a date of 1868.62.                                          
20070+1803   BPM2003     [PM2000] 2178810 + [PM2000] 2178648.                                    Gvr2010 
20070+1647   BPM2004     [PM2000] 2179019 + [PM2000] 2178022.                                    Gvr2010 
20070+1430   BPM2005     [PM2000] 2179331 + [PM2000] 2179499.                                    Gvr2010 
20071+1247   BPM2006     [PM2000] 2179892 + [PM2000] 2180002.                                    Gvr2010 
20073+1718   BPM2008     [PM2000] 2181023 + [PM2000] 2181292.                                    Gvr2010 
20073+1605   STF2629     H 2  70.                                                                MEv2010 
20073+1418   BPM2010     [PM2000] 2181515 + [PM2000] 2181473.                                    Gvr2010 
20073+1354   BPM2009     [PM2000] 2181026 + [PM2000] 2181994.                                    Gvr2010 
20073+1331   BPM2011     [PM2000] 2181586 + [PM2000] 2180641.                                    Gvr2010 
20073+1236   BPM2007     [PM2000] 2180996 + [PM2000] 2181711.                                    Gvr2010 
20074+3819   POP 187     Aka POP 214.                                                            Dam2016d
20074+3751   POP 191     Aka POP 188.                                                            Skf2016e
20074+3543   STT 398     A is a spectroscopic binary.                                                    
                         AB: The classification and orbit are from Burkholder et al. (1997 ApJ           
                         490, 328).                                                              Msn1998a
20074+1442   BPM2012     [PM2000] 2181875 + [PM2000] 2182120.                                    Gvr2010 
20074-2943   HJ 5168     B is CD-30@17665.                                                               
20075+3236   SEI 895     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
20075+3053   ES  360     Aka TDS1997.                                                                    
20075+1522   BPMA238     [PM2000] 2182947 + [PM2000] 2184083.                                    Gvr2010 
20075-0037   H 4  34     H IV 34.                                                                        
20076+3837   A  1416     Aka STH   8.                                                            Dam2016d
20076+1741   JEF   3     Recurrent nova WZ Sge. Also a W UMa variable.                                   
20076+1700   BPMA239     [PM2000] 2183254 + [PM2000] 2183058.                                    Gvr2010 
20077+1459   BPM2013     [PM2000] 2184218 + [PM2000] 2184866.                                    Gvr2010 
20077+0446   STF2627     C is BD+04@4349.                                                                
20078+1800   BPM2015     [PM2000] 2185135 + [PM2000] 2186050.                                    Gvr2010 
20078+1548   BPM2014     [PM2000] 2184789 + [PM2000] 2185273.                                    Gvr2010 
20078+0924   STF2628     H 2  29.                                                                MEv2010 
                         Additional notes may be found in Fatou (1941).                          Fat1941 
                         B is SB2, P=23.844d                                                     Tok2014d
20079+3605   SEI 908     J 1162.                                                                         
20079+3111   WAK  16     SE of ADS 13406.                                                                
20080+3235   STF2633     AB: SEI 902.                                                            Nsn2017d
20080+1816   BPM2016     [PM2000] 2186666 + [PM2000] 2185982.                                    Gvr2010 
20080-0041   SHY 325     HIP  99171 + HIP  99100. Primary is 64 Aql.                                     
20081+3241   SEI 906     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
20081-3929   RST2134     Gomez et al. (2016) derive dynamical parallax and component masses:             
                         7.35 +/- 0.33 mas, 0.993 +/- 0.021 Msun, 0.909 +/- 0.019 Msun.          Doc2016i
20082+1339   BPM2017     [PM2000] 2187618 + [PM2000] 2187742.                                    Gvr2010 
20083+1533   BPM2018     [PM2000] 2188723 + [PM2000] 2188172.                                    Gvr2010 
20084+3808   HJ  606     B is BD+37@3783.                                                                
20084+3528   ES  203     SEI 909.                                                                Nsn2017d
20084+1627   BPM2020     [PM2000] 2189479 + [PM2000] 2189621.                                    Gvr2010 
20084+1558   BPM2019     [PM2000] 2189115 + [PM2000] 2188480.                                    Gvr2010 
20084+1503   OSO 117     G143-033. None of the OSO components is a common proper motion pair,            
                         based on comparison with POSS2 red plates                               Oso2004 
20085+1806   BPM2021     [PM2000] 2190025 + [PM2000] 2190679.                                    Gvr2010 
20086+1307   BPM2022     [PM2000] 2190578 + [PM2000] 2190710.                                    Gvr2010 
20086-4618   CPO  88     B is CD-46@13400.                                                               
             UC 4100     BD: Originally 20087-4618 UC 4100, but primary was found to be B                
                         component of 20086-4618 CPO  88.                                                
20087+1603   BPM2023     [PM2000] 2191132 + [PM2000] 2190353.                                    Gvr2010 
20087+1223   J  1338     Pair measured in 1948 is indeed the same one measured in 1914. It is            
                         -17s, +0' from BD+11 4154.                                              J__1949a
                         Rectilinear solutions by Cvetkovic (2015)                               Cve2015b
                         and Cvetkovic et al. (2016).                                            Cve2016 
20088+1605   BPM2025     [PM2000] 2192282 + [PM2000] 2192439.                                    Gvr2010 
20088+1537   BPM2024     [PM2000] 2192024 + [PM2000] 2191750.                                    Gvr2010 
20088+1201   BPM2026     [PM2000] 2192296 + [PM2000] 2191695.                                    Gvr2010 
20089+7743   STF2675     kap Cep = 1 Cep                                                                 
                         AB: H 3  70.                                                            MEv2010 
                         AB: Additional notes may be found in Dembowski (1883).                  D__1883 
20089+3450   SEI 918     Secondary not seen on Aladin images; typo or plate flaw in AC Catalog.          
20089+2520   AG  247     This is a distant companion. Original star single.                              
20089+1230   BPMA240     [PM2000] 2192722 + [PM2000] 2190971.                                    Gvr2010 
20089+1127   BPM2027     [PM2000] 2192644 + [PM2000] 2191882.                                    Gvr2010 
20089+1111   BPM2028     [PM2000] 2192677 + [PM2000] 2191969.                                    Gvr2010 
20090+4252   OSO 118     G125-064. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates.                                                  Oso2004 
20090+3516   SEI 919     ALI   8.                                                                        
20090+3258   SEI 916     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
                         A likely plate flaw.                                                    Grv2021b
20090+2718   BRT 210     Misidentified in ADS catalog.                                                   
20090+1535   BPM2029     [PM2000] 2193402 + [PM2000] 2193844.                                    Gvr2010 
20090+1355   BPM2030     AB: [PM2000] 2193571 + [PM2000] 2193636.                                Gvr2010 
             BPM2031     AC: [PM2000] 2193571 + [PM2000] 2192886.                                Gvr2010 
             BPM2032     BC: [PM2000] 2193636 + [PM2000] 2192886.                                Gvr2010 
20090+0127   BAL1544     J 1698.                                                                         
20091+1638   BPM2034     [PM2000] 2194255 + [PM2000] 2194438.                                    Gvr2010 
20091+1117   BPM2033     [PM2000] 2194221 + [PM2000] 2194724.                                    Gvr2010 
20091-2613   MET  88     All seven faint companions appear to be background stars.                       
             VIG  19                                                                             Vig2012 
20092-4105   GRV1264     Both A and B have approximately the same radial velocity.               Grv2019b
                         Also known asKPP3108.                                                           
20093+1549   BPM2035     [PM2000] 2195432 + [PM2000] 2195376.                                    Gvr2010 
20093-1925   HU   80     SEE 406.                                                                        
20094+3651   BNW   2     28 Cyg = V1624 Cyg.                                                             
20094+3630   SEI 928     D is BD+36@3905.                                                                
             ABH 131     AF: BKO  96AO.                                                                  
20094+3309   GIC 162     G125-066/G125-065.                                                              
                         NLTT 48819/48820                                                        Chm2004 
20094+3244   SEI 925     Secondary not seen on POSS plate; may be flaw on AC Potsdam plate.              
20094+1613   BPM2036     [PM2000] 2196152 + [PM2000] 2196147.                                    Gvr2010 
20095+4752   BLL  45     A is the irregular variable SV Cyg. B is BD+47@3034.                            
20096+1648   STF2634     Mt. Wilson spectral type of B is K5.                                            
                         Aka H 2  70 = S   734.                                                  Bu_1906 
20096+1540   BPM2037     [PM2000] 2197958 + [PM2000] 2197337.                                    Gvr2010 
20096-8248   SHY 766     HIP  99318 + HIP  96923.                                                        
20097+3240   SEI 933     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
                         A likely plate flaw.                                                    Grv2021b
20097-2216   BRT1561     CD-22@14512.                                                                    
20097-4522   RSS  35     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
20098+3130   SEI 932     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
20098+1215   TOR  21     Formerly known as PAN  18.                                                      
20099+2055   STF2637     the Sge = 17 Sge. STTA201 = STFA 49. B is BD+20@4455.                           
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         BC: Mt. Wilson spectral type of B is G3, C is K1.                               
                         AB: HJL 272.                                                            HJL1986 
                         AB: H 3  24.                                                            MEv2010 
20100+7711   PLT   8     SZ Cep.                                                                 Plt1934 
20100+1457   BPM2039     [PM2000] 2200353 + [PM2000] 2200006.                                    Gvr2010 
20100+1216   BPM2038     [PM2000] 2200118 + [PM2000] 2199900.                                    Gvr2010 
20100+1021   A  1199     A is the Algol-type system V346 Aql.                                            
20100-2802   BRG  30     Given the relatively small separation (~0.62") and the similar                  
                         brightnesses of the two components in the 2MASS J20100002-2801410               
                         system, it is likely that they form a physical pair. However, only one          
                         epoch of imaging exists at this point.                                  Jnn2012 
20102+4357   STT 400     Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         Eccentricity incorrectly given as 0.468 by Heintz (1985); correct       Hei1985d
                         value 0.486 (Erratum noted in Inf. Circ. 98, 1986)                              
                         Incorrect value of omega given by Burnham (1898); corrected by          Bu_1898 
                         Doberck (1898)                                                          Dob1898c
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.67 +/- 0.26, 2.08, and 0.98 Msun, respectively.             Mlk2012 
20102+3644   ES   87     SEI 940.                                                                Nsn2017d
20102+1723   BPM2040     AB: [PM2000] 2201513 + [PM2000] 2202022.                                Gvr2010 
             BPM2041     BC: [PM2000] 2202022 + [PM2000] 2202081.                                Gvr2010 
             BPM2042     CD: [PM2000] 2202081 + [PM2000] 2202900.                                Gvr2010 
20102+1646   BPMA241     [PM2000] 2201645 + [PM2000] 2201527.                                    Gvr2010 
20103-2147   PRB   8     Primary is WD 2007-21 = GJ 781.3 = NLTT 48815, secondary is NLTT                
                         48706. Possible CPM pair, according to Probst (1983).                   Prb1983 
20104+3644   SEI 946     AC. Very faint object seen on POSS plate near purported position of C           
                         component; uncertain whether Scheiner's tertiary is a variable star or          
                         a flaw on AC Potsdam plate.                                                     
                         C may be at 292 deg & 15.1" with a 120 deg error by Scheiner.           Dam2011 
                         The alternate measure for AC by Scheiner matches 20105+3614 = SEI 947.  Smr2022 
20105+4923   ES 1099     Appears to be the same as FOX  34.                                      Dam2013 
20105+3614   SEI 947     This pair matches the alternate measure of 20104+3644AC by Scheiner.    Smr2022 
20105+3225   SEI 943     Secondary not seen on POSS plate; may be flaw on AC Potsdam plate.              
20105+2920   BRT  46     W Uma (EW) type eclipsing binary, P = 0.63757 d.                        Zas2011 
20106+3751   SEI 949     SLE 951.                                                                        
20106+3338   S   738     B is BD+33@3780.                                                                
20106+1701   BPM2043     [PM2000] 2204551 + [PM2000] 2204361.                                    Gvr2010 
20106+0632   LUH  15     LSPM J2010+0632 + 2MASS J20103539+0634367.                              Luh2012b
20107+3703   STT 399     AB: SEI 955.                                                            Nsn2017d
20107+1750   BPM2044     [PM2000] 2204621 + [PM2000] 2204839.                                    Gvr2010 
20108+3320   SEI 952     Precise coordinates are of object observed by Heintz, who notes that    Hei1985a
                         nothing was seen at IDS position. Identification with the SEI pair is           
                         uncertain.                                                                      
20108+2358   OSO 119     Not a common proper motion pair, based on comparison with POSS2 red             
                         plates                                                                  Oso2004 
20108+1614   BKO 527     Anon. 39.                                                               Bko2009d
20108+1541   BPM2045     [PM2000] 2205696 + [PM2000] 2205391.                                    Gvr2010 
20110+5717   ARG  36     HJL 273.                                                                HJL1986 
20111+4131   HJ 1491     20102+4130WFC 229.                                                              
                         Pair is BD+41 3634 and is about 1.5mag brighter than stated.            Brt1939a
20111+1611   GIC 163     Aa = G143-034/G143-035 = GJ 783.2AB.                                            
                         Aa,Ab: NLTT 48851/48854                                                 Chm2004 
             HZG  15     AD: Rectilinear solution by Friedman et al. (2011).                     USN2011a
20111-1252   HO  119     J 2299.                                                                         
20111-5731   HDO 295     Spectroscopic triple.                                                           
20112-3606   HJ 5173     Proper motion +465 -1581.                                                       
                         HIP 99461. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
20113+3550   HJ 1489     AD: SEI 967.                                                            Nsn2017d
20113+1209   BPM2046     [PM2000] 2208957 + [PM2000] 2208828.                                    Gvr2010 
20113-0008   S   735     B is BD-00@3935.                                                                
                         H 5 136.  H 6  27.                                                      MEv2010 
20113-0049   ISO  12     the Aql = 65 Aql. A is a spectroscopic binary, P = 17.12d.                      
                         The Aa,Ab pair cannot be this object.                                           
             BU 1540     AB: Incorrectly identified as H 6  27 in BDS. Error noted by MacEvoy.   MEv2010 
             MKT  10     the Aql.                                                                        
                         Visual orbit by Hummel et al. (1995) based on astrometry from Mark III  MkT1995 
                         interferometer. Additional spectroscopic data yield component masses,           
                         luminosities, radii, effective temperatures, and distance.                      
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Hummel et al. (1995).                                                   MkT1995 
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 10.09 +/- 0.66, 9.08, and 2.88 Msun, respectively. Mlk2012 
                         Ma,Mb = 3.564 +/- 0.049, 2.739 +/- 0.037 \msun.                                 
                         Ra,Rb = 4.76 +/- 0.14, 2.34 +/- 0.07 \rsun.                                     
                         Teff_a,Teff_b = 10300 +/- 200, 10230 +/- 220 K.                                 
                         La,Lb = 229.8 +/- 22.5, 54.0 +/- 5.8 \lsun. distance = 76.3 +/- 0.3 pc. CIA2022e
20114+3552   HJ 1490     SEI 969.                                                                        
20114+1102   BPM2047     [PM2000] 2209600 + [PM2000] 2210110.                                    Gvr2010 
20115+3539   SEI 968     HLM  37.  BRT3253.                                                      Brt1951 
                         SEI 970.                                                                Nsn2017d
20115+1524   BPM2048     [PM2000] 2209955 + [PM2000] 2209806.                                    Gvr2010 
20116+6205   LDS2791     Primary is 68 Dra, X-ray source, SB. Rapid rotator?                     Tok2014d
20116+3853   A  1418     SEI 981.                                                                Nsn2017d
20116+1417   BPM2050     [PM2000] 2210831 + [PM2000] 2211559.                                    Gvr2010 
20116+1336   BPM2049     [PM2000] 2210557 + [PM2000] 2210979.                                    Gvr2010 
20117+1221   BPM2051     AB: [PM2000] 2211498 + [PM2000] 2211470.                                Gvr2010 
             BPM2052     BC: [PM2000] 2211470 + [PM2000] 2211313.                                Gvr2010 
20118+7614   MLR 232     No significant movement since first resolution.                         Drd2009 
20118+1117   BPM2053     [PM2000] 2212269 + [PM2000] 2212364.                                    Gvr2010 
20118-1205   H 6  92     H VI 92. B is BD-12@5662.                                                       
20119+6431   STF2660     LDS2448. B is BD+64@1424.                                                       
20119+3612   BLL  46     A is the irregular variable V1042 Cyg.                                          
20119+3551   SEI 983     J  1164.                                                                Nsn2016 
20119+3510   SEI 988     J 127.                                                                          
20119+2351   POU4262     J 1768.                                                                         
20119+2020   HRL   1     A is the Mira-type variable FG Sge.                                             
20120+3429   HO  121     AB,C: SEI 986.                                                          Nsn2017d
20120+3227   SEI 984     Not found by Heintz at IDS position.                                    Hei1990b
20120-0039   J   548     Aka J  2402.                                                                    
20120+2350   POU4263     J 1769.                                                                         
20121+4618   OSO 120     G209-020. Neither AB nor AD is a common proper motion pair, based on            
                         comparison with POSS2 red plates                                        Oso2004 
20122+3827   STT 401     H N  86.                                                                MEv2010 
20122+3810   SEI 998     J 1166.                                                                         
20122+1712   BPM2054     [PM2000] 2214471 + [PM2000] 2214253.                                    Gvr2010 
20122+1534   BKO 528     Anon. 40.                                                               Bko2009d
20122+0255   BAL2019     J 1387.                                                                         
20123+3205   STF2649     B is BD+31@3989.                                                                
                         AB: SEI 993.                                                            Nsn2017d
20123+1650   BPM2056     [PM2000] 2215567 + [PM2000] 2215701.                                    Gvr2010 
20123+1525   BPM2055     [PM2000] 2215401 + [PM2000] 2215107.                                    Gvr2010 
20124+2224   GRV 322     AC: Also known as GRV 321AB.                                                    
20124-1237   BUP 206     xi 2 Cap = xi Cap = 2 Cap                                                       
             TDT2085     AC: SHY 326. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
20124-2237   RST3250     CD-22@14551.                                                                    
20125+1634   BPM2057     [PM2000] 2216856 + [PM2000] 2216408.                                    Gvr2010 
20126+4016   HD 192281   Barannikov (1993 SvAL 19, 420) suggests a possible low-amplitude orbit          
                         with a period of 5.5d, but we have placed the star in the "C" category  Gie1986 
                         based on the constancy found by Gies & Bolton (1986).                   Msn1998a
20126+2529   BRT3355     Originally published as BRT 211.                                        Brt1928 
20126+1616   CHE  67     Error in transcribing original 1910 coordinates led to this system              
                         being listed in WDS as 02136+1626.                                              
             BKO 529     Anon. 41.                                                               Bko2009d
20126+1553   BKO 530     Anon. 42.                                                               Bko2009d
20126+0052   STF2644     H 2  96.                                                                MEv2010 
20127+1514   BPM2058     [PM2000] 2217990 + [PM2000] 2218378.                                    Gvr2010 
20128+2725   MLB 706     One of a group of faint stars = BD+27 3650.                             Mlb1932 
20128+2312   POU4276     LDS1034.                                                                        
20129+3429   AG  250     SEI1009.                                                                Nsn2017d
20129+1548   CHE 201     AB: Same as 20128+1548SMA 113                                                   
             CHE 202EF   Aka BKO 531 or Anon. 43.                                                Bko2009d
20129+1246   BPM2059     [PM2000] 2219265 + [PM2000] 2218952.                                    Gvr2010 
20130+1624   BPM2061     [PM2000] 2220054 + [PM2000] 2219442.                                    Gvr2010 
20130+1211   BPM2060     [PM2000] 2220051 + [PM2000] 2219881.                                    Gvr2010 
20130+1029   J   549     J 176.                                                                          
20131+3411   STT 203     B is BD+33@3809.                                                                
20131+1713   BPM2062     [PM2000] 2220519 + [PM2000] 2221274.                                    Gvr2010 
20131-1111   BRT2771     Aka J  2304.                                                                    
20132+1541   BKO 532     Anon. 44.                                                               Bko2009d
20133+1529   BKO 533     Anon. 45.                                                               Bko2009d
20134+3844   BLL  47     A is the semiregular variable RS Cyg.                                           
                         B is BD+38@3956.                                                                
20134+1536   BKO 534     Anon. 46.                                                               Bko2009d
20134-1526   KUI  96     B has negative V-K but J-K=0.69. Is B a white dwarf?                    Tok2014d
20134-4612   CD-4613445  HD 191760. Combined astrometric/spectroscopic solution, using                   
                         spectroscopic elements (P,T,e,omega) from Jenkins et al. (2009 MNRAS            
                         398, 911).                                                              SaJ2011 
20136+5307   STF2658     Mt. Wilson spectral type of A is F4s, of B K2.                                  
                         AB: H N  72.                                                            MEv2010 
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         BC: Rectilinear solution by Friedman et al. (2012).                     USN2012a
20136+4644   WRH  33     Aa,Ab: 31 Cyg = omi 1 Cyg. A spectroscopic, eclipsing, astrometric,             
                         interferometric binary. A is the zeta Aurigae-type binary V695 Cyg.             
                         It is spectrum K4Ib+B3-4.                                                       
                         Aa,Ab: Star D noted as single. See Wilson (1950) for extensive notes            
                         on comparison of measures with orbits, mass estimates, etc.             WRH1950a
                         Aa,Ab: Reality of these measures would seem more questionable than              
                         those published in 1950.                                                WRH1951 
                         Aa,Ab: Attempted to observe visually this 10yr binary which passed              
                         eclipse late in 1951.                                                   WRH1954b
                         Aa,Ab: Correction for magnitude difference should increase this                 
                         estimated separation.                                                   WRH1955 
                         Aa,Ab seen single in 1953, resolved once again by McAlister in 1980.    McA1983 
                         1983.4905: Our ACFs do not resolve the system with much confidence              
                         (theta ~168 deg, rho ~0".029).                                          Bag1984a
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Wright (1970).                                                          Wri1970 
                         Mk III Limb-darkened diameter  4.47  +/- 0.06  mas.                     MkT2001 
                         Mk III Limb-darkened diameter  4.362 +/- 0.044 mas.                     MkT2003 
                         NPOI Limb-darkened diameter    4.49  +/- 0.06  mas.                     NOI2001b
             GUI  30     D: 30 Cyg.                                                                      
             STFA 50     STTA204.                                                                        
                         AC: H 6  10.                                                            MEv2010 
20136+1537   BKO 535     Anon. 47.                                                               Bko2009d
20136+1205   BPM2063     [PM2000] 2224188 + [PM2000] 2224790.                                    Gvr2010 
20136-1521   HJ 5511     Originally assigned to KUI  96.                                         WSI2011b
                         Correct ID provided by Friedrich Damm.                                  Dam2013 
20136-3827   GC 28055    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
20137+4050   DOO  13     A  1385.                                                                        
20137+1609   SHY 768     AC: HIP  99689 + HIP 100451. C component = B component of 20222+1623.           
20138+2021   HJ 2941     HJL 274.                                                                HJL1986 
20138+1609   BKO 536     Anon. 48.                                                               Bko2009d
20138+1450   BKO 537     Anon. 49.                                                               Bko2009d
20138+1342   BPM2064     [PM2000] 2225094 + [PM2000] 2224508.                                    Gvr2010 
20139+2358   POU4290     Also known as NYS   6.                                                          
20139+1806   BPMA242     [PM2000] 2225750 + [PM2000] 2225233.                                    Gvr2010 
20139+1751   BPM2067     [PM2000] 2225937 + [PM2000] 2225475.                                    Gvr2010 
20139+1611   BPM2065     AB: [PM2000] 2225681 + [PM2000] 2225995.                                Gvr2010 
             BPM2066     BC: [PM2000] 2225995 + [PM2000] 2225512.                                Gvr2010 
20139+0641   GIC 164     G024-010/G024-009 = GJ 784.2AB.                                                 
20140+5557   TOK   5     1984.778: This object, first resolved here, was suspected to be an              
                         astrometric binary with period about 11 years and semiamplitude about           
                         0".1 by A.A. Voltchkov.  The observed orbital motion is not                     
                         incompatible with the astrometric data.                                 Tok1985 
20140-0052   BU 1485     A,BC: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
             J   551     BC: Not seen after 1916.                                                        
             BU 1485     BC,D: Additional notes may be found in Jonckheere (1949).               J__1949b
             GC 28080    Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from Vogt et al.  CPS2000c
                         (2000).                                                                 HaI2001 
             BU 1485     No comoving objects found within separation/magnitude range listed.             
                         However, Chauvin et al. (2006) note finding at least one faint          Cvn2006 
                         background object.                                                              
20140-1640   HIP  99708  No RV data, the acceleration could be spurious. Elongated image?        Tok2013b
20141+2213   STF2655     AB: H N  55.                                                            MEv2010 
20141+1553   BPM2068     [PM2000] 2227104 + [PM2000] 2227074.                                    Gvr2010 
20141+1222   BPM2069     [PM2000] 2227475 + [PM2000] 2227524.                                    Gvr2010 
20142+3522   ES  204     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         SEI1032.                                                                Nsn2017d
20142+1508   BKO 538     Anon. 50.                                                               Bko2009d
20142+1202   HJ 1494     Obvious discrepancy in separation between Doolittle and WFC measures    Doo1915a
                         versus those of other observers suggest they did not observe the        WFC1998 
                         Herschel pair. Precise coordinates are those of the 9" pair; no 3"              
                         pair is found in the vicinity of Burnham's coordinates.                         
20142+0635   S   740     B is BD+06@4479.  Also known as LDS1036.                                        
                         HJL 275.                                                                HJL1986 
                         SHY 770. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
             TOK 627     AC: C and D components comprise 20156+0615 HJL 277.                             
20143+4648   ES   27     Also known as WFC 230.                                                          
20143+1648   BPM2070     [PM2000] 2228160 + [PM2000] 2227349.                                    Gvr2010 
20143+1507   BKO 539     Anon. 51.                                                               Bko2009d
20144+3822   SEI1038     J 1230. Probably J 1167. See ADS.                                       A__1932a
20144+1608   BKO 540     Anon. 52.                                                               Bko2009d
20144+1505   BKO 541     Anon. 53.                                                               Bko2009d
20144+1242   BPM2071     [PM2000] 2229049 + [PM2000] 2228314.                                    Gvr2010 
20145+3648   ENG  72     29 Cyg. A Delta Scuti-type variable, V1644 Cyg.                                 
20145+3640   RJJ   1     Aa,Ab: Primary is Wolf-Rayet WR 137, distance 1300pc. First resolved            
                         with IOTA array by Rajagopal (2010), later confirmed with  CHARA Array  RjJ2010 
                         by Richardson et al. (2016). Richardson et al. infer the following              
                         stellar parameters for the WR star and its close companion:                     
                            Spectral types:    WC7pd                 O9 V                                
                            T* (K)             60000 +/- 5000        32000 +/- 2000                      
                            log L (Lsun)       5.22  +/-0.05         4.75  +/- 0.05              .     
                            R* (Rsun)          3.8   +/- 1           7.7   +/- 1                 CIA2016b
20145+1555   BKO 542     Anon. 54.                                                               Bko2009d
20145+1502   TOB 309     Anon. 55.                                                               Bko2009d
20145+1418   BPM2072     [PM2000] 2229844 + [PM2000] 2229727.                                    Gvr2010 
20148+1439   BPM2074     [PM2000] 2231769 + [PM2000] 2231916.                                    Gvr2010 
20148+1214   BPM2073     [PM2000] 2231608 + [PM2000] 2230912.                                    Gvr2010 
20149+1808   BPM2075     [PM2000] 2232092 + [PM2000] 2232962.                                    Gvr2010 
20149-5659   RMK  25     Rectilinear solution by Letchford et al. (2018).                        LRR2018a
20150+3500   ES  205     SEI 1042. J 128.                                                                
20150+1239   BPM2076     [PM2000] 2233220 + [PM2000] 2232453.                                    Gvr2010 
20150+0835   J   552     HJL 276.                                                                HJL1986 
20151+4118   A   387     A 7" faint pair is in the field about 22" from A in 220@.               A__1932a
20151+3742   COU2416     Systemic mass is estimated at 2.8 +/- 0.7 Msun, assuming a dynamical            
                         parallax of 10.69 +/- 0.30 mas.                                         Doc2008a
20151+1552   BKO 543     Anon. 56.                                                               Bko2009d
20151+1450   BPM2077     [PM2000] 2233525 + [PM2000] 2233870.                                    Gvr2010 
20152+5409   HO  455     Hough's (1894) original component designations were altered by the      Ho_1894b
                         time the ADS was published; his A,B,C,D, and E components are now       A__1932a
                         designated A,E,D,B, and C.                                                      
20152-0330   STF2654     B is BD-03@4824.                                                                
                         Additional notes may be found in Muller (1950).                         Mlr1950b
20153+2536   BU  983     The primary may be a long-period spectroscopic binary.                          
20153+1807   BPM2079     [PM2000] 2234918 + [PM2000] 2234586.                                    Gvr2010 
20153+1145   BPM2078     [PM2000] 2234765 + [PM2000] 2234892.                                    Gvr2010 
20154+6412   SHY 772     AD: HIP  99832 + HIP  98613.                                                    
             MLR  60     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.60 +/- 0.87, 2.37, and 0.95 Msun, respectively.  Mlk2012 
20154+4743   omi2 Cyg    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Wright (1970).                                                          Wri1970 
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Griffin (2008).                                                         Grf2008 
20155+4743   S   743     32 Cyg = omi 2 Cyg = the 2 Cyg. A is the zeta Aurigae-type binary V1488         
                         Cyg. With a period of 1148d this cannot be this pair. B is BD+47@3060.          
                         H 6  33.                                                                MEv2010 
20155+1455   BKO 544     Anon. 57.                                                               Bko2009d
20155+1452   BKO 545     Anon. 58.                                                               Bko2009d
20156+3910   SEI1046     J 1148. ES 2048.                                                                
20156+1958   ROE 101     AB: HJL 278.                                                            HJL1986 
20156+1527   BKO 546     Anon. 59.                                                               Bko2009d
20157+4339   A  2095     Variability of one component has been suspected.                                
                         Ling (2004) derived an orbital parallax 0".01636                        Lin2004a
                         AB,C: Also known as SCA 182.                                            Sca2018b
20157+1534   BKO 547     Anon. 60.                                                               Bko2009d
20157+1509   BKO 548     Anon. 61.                                                               Bko2009d
20157+1508   BKO 549     Anon. 62.                                                               Bko2009d
20157+1457   BKO 550     Anon. 63.                                                               Bko2009d
20157+1003   J   135     J 175. J 2190. OL  193.                                                         
20158+5230   STT 404     ADS 13616a.                                                                     
20158+2749   CHR  94     23 Vul.                                                                         
                         Aa,Ab: 1991.893: These two observations confirm the discovery                   
                         measurement of this close component, made in 1985, and indicate         McA1987b
                         considerable motion during this interval.                               Hrt1994 
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 2.39 +/- 0.73, 6.47, and 2.40 Msun, respectively.  Mlk2012 
20158+1628   BPM2080     [PM2000] 2237900 + [PM2000] 2238465.                                    Gvr2010 
20158+1536   BKO 551     Anon. 64.                                                               Bko2009d
20158+1510   BKO 552     Anon. 65.                                                               Bko2009d
20159+1505   BKO 553     Anon. 66.                                                               Bko2009d
20159+1457   BKO 554     Anon. 67.                                                               Bko2009d
20160+1819   BPMA243     [PM2000] 2239594 + [PM2000] 2238354.                                    Gvr2010 
20160+1510   BKO 555     Anon. 68.                                                               Bko2009d
20161+3854   CHR  95     Hipparcos Acceleration Double Solution.                                         
                         This system, first announced by McAlister and recalled in a later       McA1984b
                         McAlister paper after repeated attempts at confirmation, has been       McA1993 
                         restored. While perhaps still spurious, the subsequent confirmation or          
                         suspected duplicity (by another technique) makes the discovery                  
                         measurement somewhat more probable.                                             
20161+1553   BKO 556     Anon. 69.                                                               Bko2009d
20161+1552   BKO 557     Anon. 70.                                                               Bko2009d
20163+1407   BPM2082     [PM2000] 2241196 + [PM2000] 2241835.                                    Gvr2010 
20163+1353   BPM2081     [PM2000] 2241007 + [PM2000] 2241190.                                    Gvr2010 
20163+1343   BPM2083     [PM2000] 2241217 + [PM2000] 2241516.                                    Gvr2010 
20164-1220   BU  294     3 Cap.                                                                          
20165+4339   ES 1439     FOX 40.                                                                         
20165+3739   BU  442     R is BD+37@3859.                                                                
             SLE 982     AL:  Soulie (2006) measure corrected for an apparent 30" error in       Sle2006b
                         declination of L component.                                                     
                         AQ: Additional notes may be found in Doolittle (1901).                  Doo1901 
                         Confusion is component designations: BO was initially listed as BD,             
                         BD as BW, and CD as CW.                                                         
20165+3739   BU  442     Confusion is component designations: BO was initially listed as BD,             
                         BD as BW, and CD as CW.                                                         
                         AB: SEI1055.                                                            Nsn2017d
             SLE 982     AL:  Soulie (2006) measure corrected for an apparent 30" error in       Sle2006b
                         declination of L component.                                                     
             BU  442     AP: SEI1052.                                                            Nsn2017d
                         AQ: Additional notes may be found in Doolittle (1901).                  Doo1901 
                         AR: SEI1053.                                                            Nsn2017d
                         BC: SEI1054.                                                            Nsn2017d
                         BD: SEI1057.                                                            Nsn2017d
                         BT: SEI1058.                                                            Nsn2017d
                         BU: SEI1056.                                                            Nsn2017d
20165+1602   BKO 558     Anon. 71.                                                               Bko2009d
20165+1601   BKO 559     Anon. 72.                                                               Bko2009d
20165-7011   HEI 274     CD given, not in CPD.                                                   Hei1985a
20166+1431   BPM2085     [PM2000] 2243469 + [PM2000] 2242918.                                    Gvr2010 
20166+1138   BPM2084     [PM2000] 2243057 + [PM2000] 2242845.                                    Gvr2010 
20166+0405   J  1641     BAL 2530.                                                                       
20166-0712   JNN 125     Due to the very small separation of the detected companion to 2MASS             
                         J20163382-0711456, this is likely to be a physical binary, although a           
                         second epoch to confirm common proper motion has not been acquired.     Jnn2012 
20167+2932   OSO 121     G186-018. Neither AB nor AC is a common proper motion pair              Oso2004 
20167+2425   BRT3356     POU4333. Originally published as BRT 212.                               Brt1928 
20167+1925   GCB  52     Heintz confirm J  3069 as identical, and corrects both positions.       Hei1983a
20167+1459   BPM2086     [PM2000] 2243647 + [PM2000] 2243201.                                    Gvr2010 
20168+4158   ES 1568     A is a W UMa-type system, V1191 Cyg.                                            
20168+3943   STF2663     AB: SEI1062.                                                            Nsn2017d
                         WDS 20167+3938 = HO  590AB and AC were incorrectly merged with this             
                         system and designated as the CD and CE pairs.                                   
20168+3633   KRV  10     Classical Cepheid V1046 Cyg.                                                    
20168-0329   TOK 337     AC: C is white dwarf candidate (Tokovinin & Lepine (2012))              Tok2012c
20169+5017   ENG  73     AB, AC, and AE: Optical pairs, based on study of relative motion of             
                         the components using the method of apparent motion parameters.          Kiy2008 
                         A: Hipparcos astrometric solution assumed circular orbit (e=omega=0).   HIP1997d
                         A: Ren & Fu (2013) calculated an astrometric orbit, combining                   
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Griffin (2002). They derived component masses 0.90 and 0.74 Msun and    Grf2002a
                         an estimated semimajor axis of 38.89 mas.                               Ren2013 
                         AB: A is SB1 (CfA: P=418.6d=1.146yr) and astrometric binary (Ren & Fu   Ren2013 
                         2013). B is SB1, P=3.616d                                               Tok2014d
             GIC 155     AF: G230-032/G230-031. A typographical error led to this pair being             
                         originally entered in the WDS as 19168+5014.                                    
             BUP 243     DF: Originally listed in the WDS erroneously as DH.                             
20169+3307   OSO 122     G210-012. Neither AC nor AD is a common proper motion pair, based on            
                         comparison with POSS2 red plates                                        Oso2004 
20170+3725   CIA   9     Aa1,Aa2: Primary is Wolf-Rayet WR 138, distance 1380pc. Resolved with           
                         CHARA Array by Richardson et al. (2016), who infer the following                
                         stellar parameters for the WR star and its close companion:                     
                            Spectral type      WN5o                  O9 V                                
                            T* (kK)            56000 +/- 5000        31000 +/- 2000                      
                            log L (Lsun)       5.35  +/- 0.05        4.82  +/- 0.05              .     
                            R* (Rsun)          4.8   +/- 2           8.9   +/- 2                 CIA2016b
20170+3153   SEI1061     Heintz identifies this with ES 2432.                                    Hei1995 
20170+1716   OSO 123     G143-043. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
20171+1641   BPM2087     [PM2000] 2246373 + [PM2000] 2246561.                                    Gvr2010 
20171+1434   BPMA244     [PM2000] 2246248 + [PM2000] 2248348.                                    Gvr2010 
20172+1553   BKO 560     Anon. 73.                                                               Bko2009d
20172+1446   BPM2088     [PM2000] 2246994 + [PM2000] 2246829.                                    Gvr2010 
20173+3420   SEI1064     B is BD+33@3839.                                                                
20173+2604   BRT3357     Originally published as BRT 213.                                        Brt1928 
20174+1430   BPM2089     [PM2000] 2248646 + [PM2000] 2248440.                                    Gvr2010 
20175+3205   SEI1065     BRT 278.                                                                Brt1929b
                         J  1169.                                                                Nsn2016 
20176+3835   ALI 927     Aka MLB 952.                                                                    
20176+1224   BPM2090     [PM2000] 2249560 + [PM2000] 2249051.                                    Gvr2010 
20176-1230   WZ   15     Aa,Ab: Previously known as HDS2895Aa,Ab. The Wirtz measure which had    Wz_1912 
                         been assigned to Aa,Ab belongs here.                                            
             BU  295     A: alp 1 Cap = 5 Cap, a spectroscopic binary. Wilson measured a star            
                         nearby: 1882.62, 96.3@, 8.32", 9.0-9.5. Not found by Burnham in 1902.           
             HJ  607     Also known as DA   16EF (as part of the system HJ  608 = ADS 13645).            
20177+1755   J  1340     Published in JO XXIV, 21 as J 1370. Jonckheere calls it 1340 in his     J__1941a
                         1962 catalogue.  Thorel (private comm.) says J 1370 is a novae,         J__1962a
                         however.                                                                        
20177+1739   BPMA245     [PM2000] 2250029 + [PM2000] 2249323.                                    Gvr2010 
20177+1504   BPM2091     [PM2000] 2250170 + [PM2000] 2250690.                                    Gvr2010 
20177+1429   BPM2092     [PM2000] 2250573 + [PM2000] 2250205.                                    Gvr2010 
20178+3956   HJ 2951     AB: SEI1074.                                                            Nsn2017d
20178+3802   P Cyg       1975.636: Disk unresolved in H alpha emission but resolved (0".020              
                         +/- 0".008) in H beta emission.                                         Bla1977a
                         1976.402: Disk resolved (0".022 +/- 0".006) in H beta emission.         Bla1977a
20178+1417   BPM2093     AB: [PM2000] 2251022 + [PM2000] 2251813.                                Gvr2010 
             BPM2094     BC: [PM2000] 2251813 + [PM2000] 2251414.                                Gvr2010 
20179+1520   SMA 116     It was initially thought that SMA 116 = CHE 290, but SMA 116 has been           
                         assigned to another, more likely pair.                                          
20179+0040   BAL1214     J  3207.                                                                        
20180+3613   SEI1073     J  1147.                                                                        
20180+3311   HO  592     BAR  54.                                                                        
20180+1325   BPM2095     [PM2000] 2252360 + [PM2000] 2252349.                                    Gvr2010 
20181+4122   ES 1674     The listed spectral type for this system is B0, however, colors from            
                         Daley suggest a very red primary with a closely matching secondary.     Dal2007 
                         V-I for primary (secondary) is 1.72(1.71).                                      
20181+4044   CHR  96     Aa,Ab: 1985.8396, 1988.6630, 1989.7061: These new observations were             
                         found from reprocessing unpublished archival data. We are currently     McA1993 
                         undertaking a duplicity survey of all bright (V<8) galactic O stars;            
                         this is one of four new binaries found by us so far in this survey.     McA1987a
                         This system is also a known spectroscopic binary, and we are                    
                         reanalyzing archival radial velocity data in an attempt to derive               
                         masses via a combined interferometric/spectroscopic orbit (see Gies et  Gie1993 
                         al. 1993 for a similar combined solution of the O star 15 Mon).                 
                         The estimated period of the speckle binary orbit (CHR 96 Aa) is 31 y.           
                         The orbit quality rating in Table 1 is our own.  The system is                  
                         currently unresolved with the Mt. Wilson Hooker telescope, but we               
                         continue to observe this target.  The brighter star of the speckle              
                         pair is also a 311-day, single-lined spectroscopic binary (McKibben et  Bgn1998 
                         al. 1998).  The classifications of the C and D components are from      Hof1991 
                         Hoffleit & Warren (1991).                                               Msn1998a
                         Cluster/Main-Sequence fitting determines a cluster distance of          Rbr2010b
                         741 +/- 36 pc.                                                                  
             CHR  96     ten Brummelaar et al. (2011) use a combination of spectroscopic and     CIA2011b
             CIA   6     astrometric data, including speckle and CHARA Array long-baseline               
                         interferometry, to derive orbits for both the Aa,Ab and Ab1,Ab2 pairs.          
                         Masses for Aa, Ab1, and Ab2 are 21, 23, and 9 Msun, respectively,               
                         effective temperatures are 33, 32.5, and 20 kK.                                 
                         Distance to Collinder 419 is 1006(+37-34) pc, yielding a mass sum of    MzA2019b
                         76.1(+9.9-7.4) \msun.                                                           
20181+1605   BKO 561     Anon. 74.                                                               Bko2009d
20181+1555   J   553     Also known as CHE 288.                                                          
20181+1519   CHE 290     It was initially thought that SMA 116 = CHE 290, but SMA 116 has been           
                         assigned to another, more likely pair.                                          
20181+1452   BPM2096     [PM2000] 2253046 + [PM2000] 2253052.                                    Gvr2010 
20181-1233   HJ  608     A: alp 2 Cap = 6 Cap = Algedi                                                   
                         Aka H 6   4 = SHJ 319.                                                  Bu_1906 
             STFA 51AE   E component is A of 20176-1230 but non-physical, so not merged.                 
20182+2319   POU4348     AB: Rectilinear solution by Friedman et al. (2011).                     USN2011a
20182+1504   BPM2097     [PM2000] 2253336 + [PM2000] 2253310.                                    Gvr2010 
20183+3825   ES 2049     OL  181.                                                                        
20183+2539   BU  985     A is a spectroscopic binary.                                                    
20183+1508   BPM2098     [PM2000] 2254089 + [PM2000] 2254981.                                    Gvr2010 
20184+5524   STF2671     AB: H 1  95.                                                            MEv2010 
                         Both A and B are spectroscopic binaries.                                        
20184+1719   BPM2099     [PM2000] 2254727 + [PM2000] 2255457.                                    Gvr2010 
20185+6313   HJ 2958     STI 963.                                                                        
20185+1519   BPM2100     [PM2000] 2255235 + [PM2000] 2255961.                                    Gvr2010 
20185+0626   J  2191     J 3219.                                                                         
20186+4136   ES 1675     Not found by Heintz.                                                    Hei1995 
                         Aka TDT2156.                                                            Dam2013 
20186+1711   BPM2101     [PM2000] 2256011 + [PM2000] 2255598.                                    Gvr2010 
20186+1600   BPM2102     [PM2000] 2256240 + [PM2000] 2256598.                                    Gvr2010 
20188+5212   ES 2692     B is BD+51@2832.                                                                
20188+3620   SEI1077     A is the Beta Lyrae-type system V382 Cyg.                                       
20188+3507   A   286     AB: Rectilinear solution by Rica & Zirm (2012).                         FMR2012i
20189+3817   A  1425     AB: The classification is from Conti et al. (1977) and refers to the    Cti1977 
                         combined AB pair.                                                       Msn1998a
20189+3635   BKO 562     Anon. 75.                                                               Bko2009d
20190+1540   BPM2103     [PM2000] 2258256 + [PM2000] 2258261.                                    Gvr2010 
20190+1530   BKO 563     Anon. 76.                                                               Bko2009d
20190+1526   BPM2104     [PM2000] 2258557 + [PM2000] 2257972.                                    Gvr2010 
20191+1647   BPM2105     [PM2000] 2259092 + [PM2000] 2258511.                                    Gvr2010 
20191-1947   BHA  38     CPD-20@7832.                                                                    
20192+3235   KLT  21     A has a hot jupiter with P ~ 3.613d and a radius of 1.586(0.040) \rJup  KLT2018 
                         A properties: Teff = 7598 +/- 83 K, M = 2.458 +/- 0.029 \msun,                  
                         R = 1.638 +/- 0.034 \rsun.                                                      
                         Projected separation of AB, AC, BC = 523(62), 504(60), 22.9(7.1) au.            
                         Mass of B,C = 0.13(0.02), 0.11(0.01) \msun.                                     
20192+1753   BPM2106     [PM2000] 2259658 + [PM2000] 2259767.                                    Gvr2010 
20192+1517   BPM2107     [PM2000] 2259927 + [PM2000] 2259448.                                    Gvr2010 
20193+3641   BKO 564     Anon. 77.                                                               Bko2009d
20193+3635   AG  253     AB: SEI1082.                                                            Nsn2017d
20193+1705   BPM2109     [PM2000] 2260163 + [PM2000] 2259940.                                    Gvr2010 
20193+1619   BPM2108     [PM2000] 2260136 + [PM2000] 2259430.                                    Gvr2010 
20194+5607   STF2669     B is BD+55@2372.                                                                
20194+3644   BKO 565     Anon. 78.                                                               Bko2009d
20194+1507   BPM2110     [PM2000] 2260873 + [PM2000] 2260336.                                    Gvr2010 
20194+1422   STF2665     A, HD 193349/50, is a 1071 d spectroscopic binary whose secondary may   REG2018 
                         be a former binary who is now merged.                                           
20194-1907   H 5  87     H V 87. SHJ 380. sig Cap = 7 Cap. B is BD-19@5777.                              
20195+1223   BPM2111     [PM2000] 2261276 + [PM2000] 2260645.                                    Gvr2010 
20196+6215   GUL   2     Also an unresolved 5.298d spectroscopic binary.                         Mug2017b
20196+4754   BLL  49     A is the Mira-type variable U Cyg. B is BD+47@3078.                             
20196+3820   A  1426     A is the Algol-type system V478 Cyg.                                            
20196+1502   BPM2112     [PM2000] 2262181 + [PM2000] 2262893.                                    Gvr2010 
20197+4108   STTA205     B is BD+40@4120.                                                                
20197+1507   BPM2113     [PM2000] 2262593 + [PM2000] 2262628.                                    Gvr2010 
20197+1333   BPM2114     [PM2000] 2262698 + [PM2000] 2262468.                                    Gvr2010 
20197-2138   BRT1562     CD-22@14621.                                                                    
20198+4522   STT 406     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.33 +/- 1.30, 2.47, and 1.35 Msun, respectively.             Mlk2012 
20199+3933   HO  593     Also known as SEI1086.                                                          
20199-0215   STF2661     B is BD-02@5239.                                                                
20200+1412   BPM2115     [PM2000] 2264323 + [PM2000] 2264225.                                    Gvr2010 
20201+3700   SEI1087     AC: Also known as ALI 422.                                                      
20201+3357   RAO 519     MY Cyg.                                                                         
20201+2338   HD193554    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
                         Spectroscopic solution to these astrometric pairs given by Griffin      Grf2013a
                         (2013). Periods match "tolerably well," other common elements less so.          
20202+1734   BPM2116     [PM2000] 2265784 + [PM2000] 2266248.                                    Gvr2010 
20202-1046   J  1389     J 1771.                                                                         
20202-2908   GLP  18     B is CD-29@16976.                                                               
20203+3924   A  1427     Spectral types and masses of components assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
20203+3919   BKO 566     Anon. 79.                                                               Bko2009d
20203+1525   BPM2117     [PM2000] 2265937 + [PM2000] 2266480.                                    Gvr2010 
20203+1350   BPM2118     [PM2000] 2266391 + [PM2000] 2266776.                                    Gvr2010 
20203+1036   TOR  23     Formerly known as PAN  20.                                                      
20204+1447   BPM2119     [PM2000] 2266622 + [PM2000] 2266983.                                    Gvr2010 
20204+1427   BPM2120     [PM2000] 2266848 + [PM2000] 2267027.                                    Gvr2010 
20205+4351   IOT   2     Aa,Ab: Monnier et al (2011) derive a distance of 1.67 +/- 0.03 kpc;             
                         masses for the WR and O star are 14.9 +/ 0.5 and 35.9 +/- 1.3 \msun,            
                         respectively.                                                           CIA2011d
                         Aa,Ab: Thomas et al. (2021) derive a distance of 1.518 +/- 0.021 kpc;           
                         masses for the WR and O star of 10.31 +/- 0.45 & 29.27 +/- 1.14 \msun;          
                         and semi-axis major of 13.55 +/- 0.21 AU.                               CIA2021a
20205+4351   BU 1207     Spectrum: WC6/7+O5/6; classification from Smith (1968 MNRAS 138, 109).  Msn1998a
                         Variable, V1687 Cyg = WR 140. Large IR variations associated with               
                         circumstellar dust shell.                                                       
                         May be a long-period spectroscopic binary.                                      
                         AB and TRN  29AC: The image rotator was in an unknown state, so no              
                         theta values were determined for the 2001.7447 observations.            Trn2008 
                         Dust forms near periastron and quickly dissipates. Polarization appears IAU2014b
                         related to the dust formation.                                                  
20205-2912   HJ 5188     B is BD-29@16981.                                                               
20206+3917   BKO 567     Anon. 80.                                                               Bko2009d
20206+3726   SEI1093     No Astrographic Catalog objects near Scheiner's coordinates and         Sei1908 
                         no obvious binary in field - typo in original catalog?                          
20206+1519   BPM2122     [PM2000] 2267984 + [PM2000] 2268719.                                    Gvr2010 
20206+1254   BPM2121     [PM2000] 2267950 + [PM2000] 2267350.                                    Gvr2010 
20206-5844   HJ 5185     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
20207-1246   LAM   5     nu Cap = 8 Cap = Alshat                                                         
20208+3922   BKO 568     Anon. 81.                                                               Bko2009d
20209+1604   BPM2123     [PM2000] 2269461 + [PM2000] 2269687.                                    Gvr2010 
20210+4437   A   725     Erratum to Ling (1989) orbit noted in IAU Circ 113, 1991: Omega = 50.2  Lin1989a
20210+1033   TOR  24     Formerly known as PAN  21.                                                      
20210+1028   J   838     Pair is 4s after BD+10 4257.                                            J__1948 
                         Linear solution first suggested and alternative linear solution in      Cve2022 
                         Despite having an orbit, an optical pair based on parallax and proper   Mlk2022 
                         motion.                                                                 Ole2002b
20210-1447   BLA   7     Aa,Ab: bet 1 Cap = Dabih. A is an occultation and interferometric               
                         binary, and is physical with the multiple system STFA 52 at 205".               
                         First detected as an occultation binary by Evans & Fekel (1979),        Evn1979 
                         who derive an orbit based upon spectroscopic, occultation, and                  
                         interferometric observations.                                                   
                         Period and eccentricity for Mason et al. (1994) orbit adopted from      Msn1994 
                         Evans & Fekel (1979); other elements generated from occultation and             
                         speckle data.                                                                   
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Evans & Fekel (1979).                                                           
                         Alden (1936) orbit adopted P, T, and e from the spectroscopic orbit     Ald1936b
                         of Spencer Jones (Ann. Cape Obs. 10, pt. 8, 76, 1928)                           
                         Alden orbit rejected from Fourth Orbit Catalog                          Wor1983 
                         ("object still suspected to be binary by some, but no even                      
                         approximately reliable or complete elements yet available")                     
             STFA 52     AB: H 6  28.                                                            MEv2010 
                         A: bet 1 Cap = 9 Cap                                                            
                         B: bet 2 Cap                                                                    
             HJ 2948     AD: mistakenly listed as BD pair.                                               
             BAR  12     Ba,Bb: Physical with bet Cap. A is an 8.7d SB and may eclipse; it is            
                         also an occultation double.                                                     
                         Ba,Bb: Additional notes may be found in Barnard (1898).                 Bar1898b
20212+1553   BPM2124     [PM2000] 2271412 + [PM2000] 2271833.                                    Gvr2010 
20212-0158   BRT 499     A likely plate flaw.                                                    Grv2021b
20213+3758   LDS1040     AC: Originally 20214+3758 LDS1040; found to share primary with                  
                         20213+3758 SEI1098, so systems merged.                                          
20213+0250   HLD 158     Misidentified in IDS as BD+02 4138 rather than +02 4139. Position and           
                         proper motion corrected.                                                        
                         Pair called "too close" by van den Bos in 7 nights in 1961 and 1962.    Wor1967b
                         Confirms comment by Couteau that BD+02 4138 7s s is single.             Mrl1968a
                         Meas attributed to ADS 13738 = BD+02 4138 appear to match this pair.    Mrl1970d
                         This is BD+02 4139, observed my Morel (1968). Coordinates are those             
                         given by Aitken for ADS 13738 = HLD 158 = BD+02 4138 -7s, which was             
                         found to be single. Probably ADS 13738 = BD+02 4139.                    Cou1970c
20214+3656   BLL  50     A is the irregular variable BI Cyg. B is BD+36@4028.                            
20215+1511   BPM2125     [PM2000] 2272762 + [PM2000] 2272661.                                    Gvr2010 
20216+1930   COU 327     Measures by ISM are anomalous. A preliminary visual orbit gives:        Ism1992 
                         P =35y, a = 0.16", motion direct.                                               
                         One component is a spectroscopic binary, P = 70.53d.                            
                         Systemic mass is estimated at 3.0 +/- 0.7 Msun, assuming an estimated           
                         parallax of 8 +/- 2 mas.                                                Doc2008a
20216+1556   BPM2127     [PM2000] 2273651 + [PM2000] 2273461.                                    Gvr2010 
20216+1546   BPM2126     [PM2000] 2273365 + [PM2000] 2273135.                                    Gvr2010 
20216-5449   COO 239     A is SB, no orbit.                                                      Tok2014d
20218+1729   BPM2128     [PM2000] 2274797 + [PM2000] 2274310.                                    Gvr2010 
20218-3654   HJ 5189     AB period estimated at 25 kyr. A is a spectroscopic binary P ~ 791d.    Tok2022e
20219+1504   BPM2129     [PM2000] 2274995 + [PM2000] 2275260.                                    Gvr2010 
20220-1854   DON1119     BHA 39.                                                                         
20221+4548   HR 7798     Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Griffin & Eitter (2000).                                                Grf2000 
20221+1501   BPM2130     [PM2000] 2276024 + [PM2000] 2275965.                                    Gvr2010 
20221+1117   BPM2131     [PM2000] 2276098 + [PM2000] 2276075.                                    Gvr2010 
20222+4015   BU  665     gam Cyg = 37 Cyg = Sadr                                                         
20222+2116   BRT2470     Not found by Heintz at IDS position.                                    Hei1990b
20222-1647   H N 138     BDS 10151 same star.                                                            
20223+4748   HJ 1510     E is A of HJ 1511. Opik also measures a wide pair 5'in 90@ from AD:     Opi1927 
                         230@ +/-, 35" +/-, 9.1-10.6.                                                    
20223+3326   OSO 124     G210-016. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
20224+2006   BUP9009     Primary is variable NT Del, central star of planetary nebula NGC 6905.          
20224+1745   BPM2132     [PM2000] 2277987 + [PM2000] 2277362.                                    Gvr2010 
20224-1841   B   479     SEE.                                                                            
20224-2014   ARG  38     CPD-20@7864.                                                                    
20225-4203   HJ 5190     kap 1 Sgr                                                                       
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
20226+1529   BPM2133     [PM2000] 2278642 + [PM2000] 2278714.                                    Gvr2010 
20226-1223   H N 127     See BDS Vol. II for note.                                                       
20227+6224   STI 973     Aka TDT2217.                                                            Dam2013 
20227+1406   BPM2134     [PM2000] 2279324 + [PM2000] 2278861.                                    Gvr2010 
20228+1156   BPM2135     [PM2000] 2279726 + [PM2000] 2279390.                                    Gvr2010 
20229+4259   HO  128     B is called variable in the Bright Star Catalogue. This is doubtful.            
             STTA207     Statistically the same parallax within the errors would indicate the            
                         components are physical.                                                        
20229+3856   SEI1106     A likely plate flaw.                                                    Grv2021b
20229+2707   ARN  50     AD: HJL 279.                                                            HJL1986 
20229+1728   BPMA246     [PM2000] 2280409 + [PM2000] 2279731.                                    Gvr2010 
20230+3913   STTA206     B is BD+38@4050.                                                                
20230+1533   BPM2136     [PM2000] 2280889 + [PM2000] 2280389.                                    Gvr2010 
20231+5745   STI2523     LDS1472.                                                                        
20231+5504   OL   74     Although listed as a measure of OL   77 by Olivier (1920), neither      Ol_1920a
                         the coordinates nor the measure agreed with that pair, so it has been           
                         assigned a new designation. Previously listed in the WDS as OL   80.            
                         Although this measure (40.7deg, 3.79") could conceivably be a measure           
                         of OL   80 with a 100deg theta error (expected values are about                 
                         140deg, 3.5"), the near-zero magnitude difference does not agree with           
                         the ~2 magnitude estimates for OL   80. Finally, the coordinates of             
                         OL   80 are 18547-1946, making such a misidentification implausible.            
20231+4047   J   787     CD. This pair was previously known as BU 1487CD, however Burnham        Bu_1913 
                         actually measured STTA207CD at 20229+4259.                                      
20231+2052   A   288     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 5.25 +/- 4.58, 4.10, and 1.35 Msun, respectively.             Mlk2012 
20231+1508   BPM2137     [PM2000] 2281737 + [PM2000] 2281548.                                    Gvr2010 
20232+3542   HJ 1506     AB: SEI1108.                                                            Nsn2017d
20233+6710   LAW  19     LSPM J2023+6710 = NLTT 49224. Law et al (2008) derive a distance of     Law2008 
                         13.6 +5.9/-2.5 pc and a projected separation of 12.8 +6.5/-2.6 au.              
                         Estimated spectral types are M5 and M5.                                         
20233+1515   BPM2138     AB: [PM2000] 2282543 + [PM2000] 2282550.                                Gvr2010 
             BPM2139     AC: [PM2000] 2282543 + [PM2000] 2282527.                                Gvr2010 
             BPM2140     BD: [PM2000] 2282550 + [PM2000] 2282126.                                Gvr2010 
20234+3053   ARG  91     B is BD+30@4010a.                                                               
20236+1421   BPM2141     [PM2000] 2284047 + [PM2000] 2284166.                                    Gvr2010 
20237+3729   CIA  20     V2119 Cyg.                                                                      
20238+3830   BUP 209     A is the irregular variable V1322 Cyg. C is BD+38@4062.                         
20239+4655   PLT   9     ZZ Cyg.                                                                 Plt1934 
20239+1107   BPM2142     [PM2000] 2286055 + [PM2000] 2286221.                                    Gvr2010 
20239-4225   BU  763     kap 2 Sgr                                                                       
20240+1443   BPM2143     [PM2000] 2286627 + [PM2000] 2286267.                                    Gvr2010 
20241+2453   POU4448     POU4450.                                                                        
20242+3516   ES 2303     Aka POP 202.                                                            Dam2013 
20243+1617   BPM2144     [PM2000] 2287920 + [PM2000] 2288313.                                    Gvr2010 
20244+2417   COU 125     1998.65: Absolute quadrant determined by triple-correlation techniques  Pru2002b
20245+0916   HJ 2959     J 1881.                                                                         
20246+4842   ES 2694     Hipparcos suspected non-single.                                                 
20246+1459   BPM2145     [PM2000] 2289896 + [PM2000] 2290028.                                    Gvr2010 
20246+0531   BU  664     H. Struve notes a 12th magnitude star at 9.2@, 20".                             
20246+0104   STF2677     Aka H 5  35. BDS 10170.                                                 Bu_1906 
20247+1747   BPMA247     [PM2000] 2290330 + [PM2000] 2291140.                                    Gvr2010 
20247+1438   HJ 1507     This is identical with BDS 10185, HJ 1508. Pair is 14s p and 7' n of            
                         BD+14 4285.                                                             Doo1915a
20248+8636   LDS1935     NLTT 49600/49597.                                                               
20248+4009   HO  278     BD+39 4172. Pair was first taken to be a new pair, as Hough (hence              
                         Burnham in BDS) identified discovery as BD+39 4186, a star of about             
                         the same mag about 1m f and 15' n of double. The doubtless accounts             
                         for Doolittle's failure to secure measures in 1905.                     A__1914d
20248+2503   OSO 125     G186-026.                                                                       
20249+1309   J   841     Not seen by any observer other than Jonckheere since discovery.         J__1912g
20250+1443   BPM2147     [PM2000] 2291857 + [PM2000] 2292356.                                    Gvr2010 
20250+1108   BPM2146     [PM2000] 2291671 + [PM2000] 2292066.                                    Gvr2010 
20251+5936   A   730     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 6.38 +/- 3.96, 4.95, and 2.19 Msun, respectively.             Mlk2012 
20252+1416   BPM2148     [PM2000] 2292741 + [PM2000] 2293159.                                    Gvr2010 
20253+1609   BPM2150     [PM2000] 2293480 + [PM2000] 2292923.                                    Gvr2010 
20253+1420   BPM2149     [PM2000] 2293274 + [PM2000] 2293173.                                    Gvr2010 
20254+4014   MLR   1     Muller suggests the observation attributed by Aitken in 1906 to HO 278          
                         (34s p and 4' s) actually is of this pair.                              Baz1954a
20254-2840   CHR  97     Also a spectroscopic binary with P = 377.6d (Bopp et al. (1970 MNRAS,           
                         147, 355). The correspondence of this component with the spectroscopic          
                         system can only be established by further observation.                          
                         1983.4258: This autocorrelogram was remeasured; the new results are             
                         listed here.                                                                    
20255+5434   GIC 157     G230-039/G230-038. LDS6341. A typographical error led to this pair              
                         being originally entered in the WDS as 19252+5430.                              
20255+1555   BPM2152     [PM2000] 2294827 + [PM2000] 2294524.                                    Gvr2010 
20255+1431   BPM2151     [PM2000] 2294520 + [PM2000] 2294256.                                    Gvr2010 
20256+2723   J  2310     A is the Algol-type system BE Vul.                                              
20256+2642   BU 1488     B is BD+26@3898.                                                                
20256-5644   HJ 5193     alp Pav = Peacock. A is a spectroscopic binary.                                 
                         Intensity Interferometer Limb-darkened diameter 0.80 +/- 0.05 mas.      HBr1974 
20257+4004   TOR  25     Formerly known as PAN  22.                                                      
20257+2258   BRT2474     Not found by Heintz.                                                    Hei1995 
20257+1510   BPM2153     [PM2000] 2295705 + [PM2000] 2296242.                                    Gvr2010 
20257+0304   BAL2024     Due to a typographical error, this pair was previously listed as                
                         22058+0313.                                                                     
20259+3914   SEI1122     SEI1124.                                                                Nsn2017d
20259+1549   BPM2154     [PM2000] 2297041 + [PM2000] 2296791.                                    Gvr2010 
20260+3414   COU1953     TDT2267.                                                                        
20260+1257   BPM2155     [PM2000] 2297163 + [PM2000] 2297560.                                    Gvr2010 
20260+1102   BPM2156     AB: [PM2000] 2297545 + [PM2000] 2297853.                                Gvr2010 
             BPM2157     BC: [PM2000] 2297853 + [PM2000] 2298536.                                Gvr2010 
20261+2910   MLB 479     Heintz believes HJ 1512 is probably identical.                          Hei1985a
20262+1721   BPM2158     [PM2000] 2298374 + [PM2000] 2297717.                                    Gvr2010 
20262-6551   B   989     The middle of three stars, all given in the Draper Catalog but only             
                         one in the CPD; the preceding also G0, the following and brighter K2.   B__1928b
20263+3728   AG  255     SEI1126.                                                                Nsn2017d
20264+5638   STF2687     H N  89.                                                                MEv2010 
                         A spectroscopic binary. B is BD+56@2422.                                        
20264+5402   FRK   9     B is BD+53@2404.                                                                
20264+1103   BPM2159     AB: [PM2000] 2299757 + [PM2000] 2299966.                                Gvr2010 
             BPM2160     AC: [PM2000] 2299757 + [PM2000] 2299958.                                Gvr2010 
20266+1148   BPM2161     [PM2000] 2300858 + [PM2000] 2300664.                                    Gvr2010 
20266-3955   SCT   2     B is CD-40@13861.                                                               
20267+1431   BPM2162     [PM2000] 2301154 + [PM2000] 2300920.                                    Gvr2010 
20268-0225   BRT 500     A likely plate flaw.                                                    Grv2021b
20269+1747   BPM2163     [PM2000] 2301992 + [PM2000] 2302355.                                    Gvr2010 
20269+1727   BPM2164     [PM2000] 2302089 + [PM2000] 2302325.                                    Gvr2010 
20270+1736   BPM2167     [PM2000] 2302950 + [PM2000] 2302653.                                    Gvr2010 
20270+1541   BPM2165     [PM2000] 2302579 + [PM2000] 2302562.                                    Gvr2010 
20270+1312   BPM2166     [PM2000] 2302677 + [PM2000] 2302801.                                    Gvr2010 
20271+1549   BPM2168     [PM2000] 2303338 + [PM2000] 2303898.                                    Gvr2010 
20272+1306   BPM2169     [PM2000] 2303974 + [PM2000] 2303799.                                    Gvr2010 
20273-1813   CHR 184     Aa,Ab: pi Cap = 10 Cap. The suspected radial velocity variation may             
                         well be explained by the close pair.                                            
                         Abt & Biggs (1972) note variable RV.                                    AbH1972 
20275-0206   S   749     AB: B is BD-02@5282.                                                            
                         AB: HJL 280.                                                            HJL1986 
                         AB: SHY 331. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         This cannot be the close 160.8-d spectroscopic binary.                  Grf2014b
                         AB: A is SB2, P=160.83d (Halbwachs et al. 2012)                         HJL2012b
                         AC: H 5  35.                                                            MEv2010 
20275-0734   LDS5906     LDS6342.                                                                        
20277+3605   ES 2193     AD: SEI1128.                                                            Nsn2017d
20277+0803   HJ 2966     Aka J  1298.                                                            Dam2013 
20278+0311   HJ  917     BAL2026.                                                                        
20279+3047   RAO 520     V442 Cyg.                                                                       
20279+1515   BPMA248     [PM2000] 2307738 + [PM2000] 2307024.                                    Gvr2010 
20279+0958   AG  256     1s f and 7' n of BD-07 5308.                                            Doo1915a
20280+1624   BPM2170     [PM2000] 2308128 + [PM2000] 2307893.                                    Gvr2010 
20280-0009   SHY 333     BC: HIP 100940 + HIP 101852.                                                    
20280-4237   RSS  36     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
                         SHY 776. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
20281+0140   BAL1560     J 1774.                                                                         
20282+8125   BUP 211     75 Dra.                                                                         
20283+1846   HO  131     HIP 100970. See Allen et al. (2000) for information on metallicity,     AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: Primary is exoplanet host, P=18.2d, and acceleration binary in HIP  Tok2014d
             GC 28482    A: Combined solution, based on reduction of Hipparcos intermediate              
                         astrometric data together with spectroscopic elements from Fischer      CPS1999c
                         et al. (1999).                                                          HaI2001 
20284+5430   STF2693     B is BD+54@2357.                                                                
20284+3007   OL   75     Aka TDT2310.                                                                    
20284+0746   BRT2186     Aka J  1299.                                                            Dam2013 
                         J  3345. Damm match to J  1299 believed incorrect.                      Nsn2016 
20284-0321   RST4667     68 Aql.                                                                         
20284-1309   STF2683     B is BD-13@5678.                                                                
20285+1110   BPM2171     [PM2000] 2310876 + [PM2000] 2311010.                                    Gvr2010 
20286+5039   HJ 1524     HJL 281.                                                                HJL1986 
20286+0351   HJ 2967     BAL 2534.                                                                       
20288+3810   ES  206     SEI1131.                                                                Nsn2017d
20289-0652   HJ  918     J  1391. HDO 158.                                                               
20289-1749   SHJ 323     rho Cap = 11 Cap.                                                               
                         Dob1927 DE measure earlier also erroneously attributed to BC.                   
                         AB: H 2  51.  AD: H 6  29.                                              MEv2010 
                         AB: Quadrant determined in 1994.5246 by speckle imaging analysis.       Hor1996 
                         AD: H 6  29 = SHJ 322. AB: SHJ 323 = H 2  51.                           Dam2011 
20290+0710   A   610     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.72 +/- 1.14, 2.01, and 1.05 Msun, respectively.             Mlk2012 
20291+1622   BPM2172     [PM2000] 2313773 + [PM2000] 2313902.                                    Gvr2010 
20291+0325   HJ 2968     BAL 2535.                                                                       
20292+1735   BPMA249     [PM2000] 2314520 + [PM2000] 2315236.                                    Gvr2010 
20293+3731   WEI  35     AB: SEI1133.                                                            Nsn2017d
                         CD: SEI1135.                                                            Nsn2017d
20293+2700   DOO  93     AC: 9s p and 3' n of BD+26 3912. Many other faint stars. One was                
                         measured 6s p, which may be the HJ pair.                                Doo1915a
20293+1155   BPM2173     [PM2000] 2314838 + [PM2000] 2314955.                                    Gvr2010 
20294+4011   ALV   6     RAFGL 2591. Massive YSO associated with optical/near-IR nebula.         Alv2004 
20294+3447   GCB  53     ADP   7. ADP measures corrected from 27deg to 360-27=333deg.                    
20294+1617   BPM2174     [PM2000] 2315826 + [PM2000] 2315584.                                    Gvr2010 
20294+0330   HJ 2970     BAL 2536.                                                                       
20295+8105   STT 593     AB: 74 Dra. LDS1932. A spectroscopic binary. B is BD+80@662.                    
                         AB: HJL 283.                                                            HJL1986 
                         AB: SHY 777. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
20295+5604   KUI  97     B probably variable, according to Couteau. Not see by me 1940, 1941,            
                         1942, nor by Muller in 1953 with the 36inch at Lick, or by Couteau in           
                         1957 at Nice.                                                           Baz1972 
20295+1512   BPM2175     [PM2000] 2316202 + [PM2000] 2316059.                                    Gvr2010 
20296+6300   the Cep     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Abt (1961).                                                             AbH1961 
20296-0650   DOO  85     J  1393.                                                                        
20296-4609   I  1422     Measures uncertain, too close. Needs speckle.                                   
20297+3808   STF2691     SEI1138.                                                                Nsn2017d
20297-2719   COO 240     WHC  20.                                                                        
20298+1154   J  1243     Not found in this position by Heintz.                                   Hei1987a
20298+0941   AST   2     AB: GJ 791.2 = HU Del. HST Fine Guidance Sensor data were used by               
                         Benedict et al. (2000) to derive perturbation orbital parameters,       AST2000 
                         distance, component masses, and absolute magnitudes for this nearby             
                         low-mass binary. Published measures are of the primary relative to the          
                         barycenter. The authors calculate a true semi-major axis of 108.8               
                         +/- 0.7 mas, while Harrington (1971) calculates a value of 0".10.       Hrr1971 
                         Harrington determined a delta-m in excess of 3, in agreement with the           
                         HST measures.                                                                   
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         As the measures relative to the barycenter were cataloged as measures   AST2000 
                         of AB, the first measure of AB was cataloged as JNN 282. The pair is    Jnn2014 
                         a simple binary. Identity first suggested by Knapp.                     Kpp2019n
                         Estimated age 30-300 Myr; masses 0.19+/-0.08 and 0.05+/-0.03 Msun       Jnn2014 
                         a ~1.4au.                                                                       
20299+4022   HJ 1525     There is no star in the vicinity at all corresponding to O. Stone 50.   Doo1915a
                         AB: SEI1139.                                                            Nsn2017d
20299+2624   S   750     B is BD+25@4260.                                                                
20299-1835   SHJ 324     12 Cap = omi Cap. B is BD-19@5830.                                              
                         H 4  71.                                                                MEv2010 
20300+0023   JNN 283     Estimated age 1000-10000 Myr; masses 0.28 +/- 0.07 and 0.16 +/- 0.03            
                         Msun; a ~6.7 au.                                                        Jnn2014 
20301+4857   BU  669     ome 1 Cyg = 45 Cyg = V2014 Cyg                                                  
20301+4007   ES  245     SEI1140.                                                                Nsn2017d
20301+1103   BPM2176     [PM2000] 2319298 + [PM2000] 2318980.                                    Gvr2010 
20301+0730   LDS4846     Aka GWP2962.                                                            Dam2016d
20302+2651   BUP 213     AE: Distance 1324.4".                                                           
20302+1925   S   752     C: Bidelman says a 1958 plate "shows very strong reversal at H-alpha".          
20303+1054   BU   63     1 Del.                                                                          
20306+4419   HD 195592   The star is close to and probably associated with WR 140.               Msn1998a
20306+2158   BRT2478     J 2597.                                                                         
20307+4137   CAN   1     [MT91] 5. Primary is an O6 star in the Cygnus OB2 Association.                  
                         Caballero-Nieves et al. (2014) find some suggestion that the primary            
                         may itself have a close companion.                                      CaN2014 
20307+3521   HJ 1526     A,BC: SEI1143.                                                          Nsn2017d
20307+1718   BPM2178     [PM2000] 2322413 + [PM2000] 2321986.                                    Gvr2010 
20307+1233   BPM2177     [PM2000] 2322349 + [PM2000] 2322075.                                    Gvr2010 
20308+1347   STF2688     Same as STF2689.                                                                
20308+1059   BPM2179     [PM2000] 2322753 + [PM2000] 2322972.                                    Gvr2010 
20308-1258   BRT2773     A likely plate flaw.                                                    Grv2021b
20309+4913   S   755     AB: H 4  23.                                                            MEv2010 
                         B is BD+48@3146.                                                                
20309+1126   LAU   4     BRT1344. Barton derived his measurement from a Toulouse plate observed  Brt1935a
                         as part of the Astrographic Catalogue project.  However, his secondary          
                         was apparently either a plate flaw measured as a star, a reduction              
                         error, or a typographical error in the preparation of the catalogue.            
                         Thanks to John Nanson (2014, private comm.) for alerting us to this             
                         missing measurement.                                                            
20309+0626   DAE  10     WSP   2.                                                                        
20310+3656   AC   18     44 Cyg.                                                                         
20310+2054   GCB  55     J 3090 is identical                                                     Hei1983a
                         Also appears to be the same as GCB  56 with a typo in that separation.  Dam2013 
20310+1402   BPM2180     [PM2000] 2323697 + [PM2000] 2323379.                                    Gvr2010 
20311+5814   LDS1474     LDS4849.                                                                        
20311+3935   LDS6414     NLTT 49394/49393                                                        Chm2004 
20311+3847   SEI1150     LDS1043.                                                                        
20311+3333   COU1962     More speckle obs needed to cover the orbit.                                     
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.03 +/- 0.31, 1.82, and 0.85 Msun, respectively.             Mlk2012 
20311+1600   BPM2181     [PM2000] 2324585 + [PM2000] 2325030.                                    Gvr2010 
20311+1548   A  1675     A measure on 1980.7257, incorrectly attributed to ADS 13944 by                  
                         McAlister et al. (1983), actually  belongs to ADS 14761.                McA1983 
                         1980.4771: Theta was incorrectly given as 313.7 degrees                 McA1983 
                         1980.7257: This measure was incorrectly attributed to HR 8059           McA1983 
                         1986.578: Separation for this partially resolved pair was calculated            
                         under the assumption of zero or otherwise known magnitude difference.   Tok1985 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 5.97 +/- 2.33, 4.29, and 2.09 Msun, respectively.             Mlk2012 
20312+5653   RAO  22     Acceleration binary (Makarov & Kaplan 2005) first resolved by Riddle    Mkr2005 
                         et al. (2015). The position angle in this paper measured on 2013.8367   RAO2015 
                         differs by 27° from the 2012.7592 measurement. That is not the only     .      
                         discrepancy between the two data sets. The photometry with P3K shows            
                         large magnitude differences (dJ = 2.5 and dK = 2.3), while Robo-AO              
                         detected a binary of equal brightness. The separation between the two           
                         components is fairly small and in the P3K data, the companion lies on           
                         the Airy ring of the primary, which could increase the errors. The              
                         primary is a high PM star, the pair AB is most likely a physical                
                         binary. Additional observations are needed to understand this system.   Rbr2015d
20312+1116   STF2690     A,BC: H 3  16.                                                          MEv2010 
             DA    1     BC: STT 407.                                                                    
                         BC: Malkov et al. (2012) derive dynamical and photometric masses of             
                         0.20 +/- 0.38 and 2.46 Msun, respectively.                              Mlk2012 
20312+0513   AG  257     Primary is eclipsing binary MR Del (period 0.52169 day).                Zas2010 
20313+4913   S   756     ome 2 Cyg = 46 Cyg                                                              
20314+3833   JNN 284     LHS 3559. Estimated age 1000-10000 Myr; masses 0.21 +/- 0.04 and 0.13           
                         +/- 0.02 Msun; a ~1.8 au.                                               Jnn2014 
20314+2421   POU4563     J  3315.                                                                        
20314+2054   J   844     Heintz says GCB 54 and J 844 are identical, with erroneous position     Hei1983a
                         and angle by Jonckheere. Designation J 844 retained, based on earlier           
                         discovery.                                                                      
                         Same as GCB  57.                                                        Dam2013 
20317+3831   ES  246     AB: SEI1153.                                                            Nsn2017d
                         AC: SEI1154.                                                            Nsn2017d
20315+3347   LAF  62     Due to the large number of components (exceeding the number of upper-           
                         case letters), a non-standard component designation was necessary,              
                         hence the pairings A,Za; A,Zb; etc. For this pair, as well as LAF  59           
                         and LAF  71, the lower-case designations (such as Za and Zb) do not             
                         refer to components of a close pair.                                            
20317+2055   J  3222     Same as GCB  58.                                                        Dam2013 
20317+1124   BPM2182     [PM2000] 2327286 + [PM2000] 2326847.                                    Gvr2010 
20319+1758   BPM2183     [PM2000] 2328243 + [PM2000] 2328848.                                    Gvr2010 
20319-4054   I  1627     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
20319+3920   HJ 1531     SEI1155.                                                                Nsn2017d
20320+2548   STF2695     Absolute quadrant determined in 1998.657 and 1998.660 by                        
                         triple-correlation techniques.                                          Pru2002b
                         Malkov et al. (2012) derive dynamical and photometric masses of                 
                         4.21 +/- 1.25 and 3.12 Msun, respectively.                              Mlk2012 
20321+2051   GCB  57     Same as J  3222?                                                                
20322+1754   GWP2966     Incorrectly added as 20322+1759 due to typo in coordinates.                     
20322-2209   HJ 2973     B is BD-22@5458.                                                                
20322-4521   RST5470     The close pair may be in rapid motion.                                          
20324+4118   HER   3     Measures disagree.                                                              
                         Includes V729 Cyg, a Beta Lyr type eclipsing binary, P = 6.59787d.      Zas2012 
                         Schulte 5 = V729 Cyg was first resolved by Herbig (1967). The primary   Her1967 
                         is a short-period eclipsing binary, consisting of two luminous evolved          
                         stars.                                                                  CaN2014 
20324-0951   BU  668     CHARA Array Limb-darkened diameter of A :                               CIA2013c
                         R =  1.8673 +/- 0.0833 \rsun, L =   2.7046 +/-0.0466 \lsun,                     
                         Teff = 5421 +/- 118 K, M = 1.097 \msun, Age = 8.2 Gyr.                          
20325-1637   SEE 512     Docobo et al. (2010) derive a dynamic parallax of 10.54 +/- 0.30 mas    Doc2010h
                         and a total mass of 3.08 +/- 0.29 Msun.                                         
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.93 +/- 0.91, 2.54, and 3.69 Msun, respectively.             Mlk2012 
20325-2142   SEE 420     CD-22@14788. A is the Mira-type system RU Cap.                                  
20327+4114   CAN   5     Primary is [MT91] 304 = VI Cyg 12, an early B-type hypergiant in the            
                         Cygnus OB2 Association. Ambiguity in the position of the secondary              
                         along one FGS coordinate leads to two possible position angles for the          
                         measure.                                                                CaN2014 
20327+2903   ARY  27     BC and BD: Originally 20328+2903 ARY  27AB and AC, but primary found            
                         to be B component of 20327+2903 ARY  47.                                        
20327+1932   OSO 126     G144-009. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
20327+1151   BPM2184     [PM2000] 2332308 + [PM2000] 2331994.                                    Gvr2010 
20327-8155   HJ 5175     AB and AC: Additional notes may be found in van den Bos (1956).         B__1956a
20328+3954   ES 1680     BC: 20327+3995ES 1977.                                                          
20329+4636   KRV  41     Classical Cepheid SZ Cyg.                                                       
20329+4154   BLA   8     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Duquennoy & Mayor (1991).                                               Duq1991 
                         Combined spectroscopic/interferometric orbit by Torres et al. (2002),   Trr2002 
                         including visibility data from the Palomar Testbed Interferometer.              
                         Additional elements for this metal-poor binary are:                             
                            gamma    = -5.841          0.037   km/sec                                    
                            KA       = 28.926          0.046   km/sec                                    
                            KB       = 36.72           0.21    km/sec                                    
                            dm       = 1.056           0.013   mag (K band)                              
                                       1.154           0.065   mag (H band)                              
                            parallax = 46.08           0.27    mas                                       
                            masses   = 0.844           0.018   Msun                                      
                                       0.6650          0.0079  Msun                                      
                         Orbit determined by fitting revised Hipparcos intermediate astrometric          
                         data. Derived component masses 0.84 +/- 0.05 and 0.67 +/- 0.04 Msun.    Ren2010 
                         Improved resolved SB2 orbit for this pair.                              Kie2018 
                         A: Teff = 5296 +/- 19 K, M = 0.8420 +/- 0.0014 \msun.                           
                         B: Teff = 4360 +/- 87 K, M = 0.66201 +/- 0.00076 \msun.                         
                         Orbital parallax = 46.131 +/- 0.084 mas.                                        
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.58 +/- 0.05, 1.73, and 0.88 Msun, respectively.             Mlk2012 
20329+1357   BU  670     AB: Additional notes may be found in Voute (1951).                      Vou1951 
             L    35     CD: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.20 +/- 1.00, 1.66, and 0.85 Msun, respectively.  Mlk2012 
20332+4122   CAN   6     Primary is [MT91] 429 = V2186 Cyg, a short-period eclipsing binary in           
                         the Cygnus OB2 Association.                                             Can2014 
20332+4028   HJ  609     B is BD+39 4236.                                                                
20332+1659   BPM2185     [PM2000] 2334751 + [PM2000] 2335156.                                    Gvr2010 
20333+3323   HJ 1535     AB: A is SB1 (CfA: P=1342d = 3.67y) and astrometric binary (Goldin &    Gln2007 
                         Makarov 2007, P=1437d)                                                  Tok2014d
                         AC and AD: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         A new 2+2 quadruple system. The outer 17" binary HJ 1535 AB has been            
                         known since 1828 (Herschel 1831). If B were a background star, the PM   HJ_1831 
                         of A, 0".208/y, would have moved it by 38" in 185 yr. The pair AB is            
                         therefore undoubtedly physical. The discrepant PM of B reported in              
                         the WDS could be caused by the subsystem Ba,Bb discovered here. The A           
                         component has an astrometric subsystem Aa,Ab with P = 3.9 yr (Goldin            
                         & Makarov 2007), confirmed spectroscopically by D. Latham. The B        Gln2007 
                         component was tentatively resolved by Robo-AO, but was thought to be            
                         too uncertain to publish in Riddle et al. (2015). Now Ba,Bb is          RAO2015 
                         clearly resolved at 0".17. Its estimated period is ~30 yr. The field            
                         is extremely crowded and another faint star E is detected at 12".1              
                         from A by both Robo-AO and PALM-3000. Comparison with 2MASS shows               
                         relative motion opposite to PM(A), so AE is optical.                    Rbr2015d
             RBR  30     Ba,Bb: incorrectly labelled RBR 29 in Table 1 of Roberts et al.         Rbr2015d
             HJ 1535     AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
20333-8058   HJ 5182     B is CPD-81@900.                                                                
20334+1544   BPM2186     [PM2000] 2336060 + [PM2000] 2336338.                                    Gvr2010 
20335-1333   OCC1089     OCC9193.                                                                        
20337+4123   CAN   8     Primary is a double-lined SB in the Cygnus OB2 Association.             CaN2014 
20337+2322   JNN 285     G 186-29. Estimated age 1000-10000 Myr; masses 0.46 +/- 0.13 and 0.28           
                         +/- 0.09 Msun; a ~20.1 au.                                              Jnn2014 
20337+1222   BPM2187     [PM2000] 2337288 + [PM2000] 2336741.                                    Gvr2010 
20338+3336   HJ 1538     SEI1167.                                                                Nsn2017d
20338+1704   BPM2188     [PM2000] 2337689 + [PM2000] 2337140.                                    Gvr2010 
20339+4642   BU 1489     B is +46@2978.                                                                  
20339+3515   WRH  34     AB: 47 Cyg.                                                                     
                         Absolute quadrant determined in 1998.657 by triple-correlation                  
                         techniques                                                              Pru2002b
                         NPOI Limb-darkened diameter 4.472 +/- 0.017 mas, Sp = K4I,              NOI2018 
                         Teff = 3671 +/-304 K,                         M = 4.49 +/- 0.66 \msun,          
                         Age = 0.15 +/- 0.06 Gyr.                                                        
20339+1032   BPM2189     [PM2000] 2338021 + [PM2000] 2337651.                                    Gvr2010 
20339-2710   CBL 178     A 355d spectroscopic solution for the A component has been found        Tok2019g
                         making this a triple system.                                                    
20340+4118   CAN  10     [MT91] 696. Primary is an O9.5 eclipsing, double-lined SB in the                
                         Cygnus OB2 Association. Ambiguity in the position of the secondary              
                         along one FGS coordinate leads to two possible position angles for the          
                         measure.                                                                CaN2014 
20340+1659   BPM2190     [PM2000] 2338597 + [PM2000] 2338116.                                    Gvr2010 
20340+0433   A  2282     Not seen for certain since 1946.                                                
20341+2814   L    48     AB: BRT  49                                                                     
20342-0045   BAL 613     J 1708.                                                                         
20342-2024   BHA  40     CPD-20@7956.                                                                    
20345+3759   BKO 569     Anon. 82.                                                               Bko2009d
20345+1735   BPM2191     [PM2000] 2341006 + [PM2000] 2340720.                                    Gvr2010 
20345+1036   BPM2192     [PM2000] 2341239 + [PM2000] 2341085.                                    Gvr2010 
20346+3334   GRV 356     AC: Also known as GRV 355AB.                                                    
20346+2914   J   565     Pair observed in 1947 is indeed the same BD+28 3797 observed in 1911.           
                         Pair is +3s, -5' from BD+28 3796.                                       J__1948 
20346+1423   BPM2194     [PM2000] 2341642 + [PM2000] 2342038.                                    Gvr2010 
20346+1255   BPM2193     [PM2000] 2341441 + [PM2000] 2340925.                                    Gvr2010 
20346-2219   LDS4850     NLTT 49474/49477                                                        Chm2004 
20347+3230   STF2700     Spectrum of B: F2IV-V.                                                          
20348+1644   BPM2195     AB: [PM2000] 2342658 + [PM2000] 2342333.                                Gvr2010 
             BPM2196     BC: [PM2000] 2342333 + [PM2000] 2342607.                                Gvr2010 
20349+4651   STTA208     B is BD+46@2982.                                                                
                         Pair appears in an appendix list, not part of discoverer's regular              
                         numbering sequence.                                                             
20350+3757   BKO 570     Anon. 83.                                                               Bko2009d
20350+3419   J   791     AC: SEI1175.                                                            Nsn2017d
20350+3323   HJ 1543     SEI1174.                                                                Nsn2017d
20350+2754   FOX  95     BRT 50.                                                                         
20351+5624   HJ 1551     Burnham switched his observations of this 40" pair and the nearby 20"           
                         pair 20352+5622 HJ 1552. His coordinates agree with the relative                
                         locations of these two pairs, however.                                  Bu_1906 
20351+1439   BPM2197     AB: [PM2000] 2343723 + [PM2000] 2343678.                                Gvr2010 
             BPM2198     BC: [PM2000] 2343678 + [PM2000] 2343784.                                Gvr2010 
20351-6042   RST4670     CD-61@6424.                                                                     
20352+5622   HJ 1552     Burnham switched his observations of this 20" pair and the nearby 40"           
                         pair 20351+5624 HJ 1551. His coordinates agree with the relative                
                         locations of these two pairs, however.                                  Bu_1906 
20352+1803   BPM2200     [PM2000] 2344368 + [PM2000] 2344014.                                    Gvr2010 
20352+1659   BPM2199     [PM2000] 2344120 + [PM2000] 2343961.                                    Gvr2010 
20352+0608   HWE  98     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
20353+1440   DRS  32     Zet Del. De Rosa et al (2014) derive a system age of 525 +/- 125 Myr.           
                         The B component is estimated as L5 +/- 2, with mass 55 +/- 10 Mjup.     DRs2014b
20354+6454   GIC 165     B is a double-lined spectroscopic binary.                                       
                         AG = G262-021/G262-022. None of the OSO components are proper motion            
                         companions                                                              Oso2004 
20356+1315   BPM2201     [PM2000] 2345880 + [PM2000] 2345942.                                    Gvr2010 
20357+3901   SEI1185     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
                         A likely plate flaw.                                                    Grv2021b
20357+2741   BRT3359     Originally published as BRT 214.                                        Brt1928 
20359+3615   GII  52     Gili (2016) associates this triple with 20359+3617 TDT2405, but the             
                         systems differ in position by 1.7'. GII  52Aa,Ab = GII  69 = GII  98.   Gii2016 
20361+3852   SEI1189     Duplicity not apparent on POSS plate; one component may be either               
                         variable star or flaw on AC Potsdam plate.                                      
                         A likely plate flaw.                                                    Grv2021b
20362+1311   BPM2202     [PM2000] 2348831 + [PM2000] 2349269.                                    Gvr2010 
20363+1328   BPM2203     AB: [PM2000] 2348914 + [PM2000] 2348707.                                Gvr2010 
             BPM2204     AC: [PM2000] 2348914 + [PM2000] 2348886.                                Gvr2010 
20364+1651   BPM2205     [PM2000] 2349398 + [PM2000] 2349432.                                    Gvr2010 
20364+1339   BPM2206     [PM2000] 2349548 + [PM2000] 2349717.                                    Gvr2010 
20365-0311   TOR  26     Formerly known as PAN  23.                                                      
20366+6226   H 4  78     H IV 78. Same as STF2712.                                                       
20366+3825   HJ 1548     SEI1191.                                                                Nsn2017d
20366+1553   BPM2207     [PM2000] 2350503 + [PM2000] 2350667.                                    Gvr2010 
20366+0123   HJ 5513     Herschel coordinates 20 27 NPD 89 12 (1830). He notes: "Curiously       HJ_1870 
                         quadruple; four small stars alternately 15m and 18m, and very close;            
                         in a line very nearly coincident with the parallel."                            
20366-7104   DUN 231     B is CPD-71@2562.                                                               
20368+3157   J   568     BRT 282.                                                                Brt1929b
20368+1444   STF2703     AB: H 4  92.                                                            MEv2010 
20369+2538   BRT3360     Originally published as BRT 215.                                        Brt1928 
20369-1244   STF2699     BDS 10334, H N 134 and BDS 10348, WEI  36 same as this star.                    
20370+0452   SMA 118     BAL 2969.                                                                       
20371+6122   SHY 780     HIP 101719 + HIP 102727.                                                        
20371+1738   BPM2208     [PM2000] 2352538 + [PM2000] 2352821.                                    Gvr2010 
20372+1224   BPM2209     [PM2000] 2352819 + [PM2000] 2352639.                                    Gvr2010 
20372+1143   BPM2210     [PM2000] 2353126 + [PM2000] 2352937.                                    Gvr2010 
20372+0135   J  2574     BAL 1565.                                                                       
20372-0225   BRT 503     A likely plate flaw.                                                    Grv2021b
20372-4445   TOK 369     First resolution; estimated period 70yr, constant RV. This binary was           
                         not resolved by speckle interferometry, possible because the companion          
                         is too faint in the visible. It is an X-ray source and a "PMS" star             
                         according to SIMBAD.                                                    Tok2013b
20373+2157   MCT  11     Initially catalogued in error as 20273+2157.                                    
20374+7536   HEI   7     The primary is the class W eclipsing SB VW Cep, P = 0.278 d. The                
                         light amplitude is 0.5 mag. and the light curve is variable.                    
                         The Hershey (1975) orbit is astrometric; only the value of the          Hry1975 
                         semi-major axis was computed after the companion was resolved. The              
                         ascending node is tentatively identified from what appears to be a              
                         lighttime effect superimposed on intrinsic period changes in the                
                         eclipsing pair.                                                                 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         BD+74@889, (mag. 7.9, G5) one degree distant, shares common proper              
                         motion and radial velocity.                                                     
                         Pribulla & Rucinski (2006) estimate the mass of the contact pair at     Pbl2006 
                         1.781 Msun and the minimum mass of the wider component at 0.42 Msun.            
20374+1735   BPM2211     [PM2000] 2353944 + [PM2000] 2353484.                                    Gvr2010 
20374+1626   BPM2212     [PM2000] 2354073 + [PM2000] 2353760.                                    Gvr2010 
20374-0254   TOR  27     Formerly known as PAN  24.                                                      
20374-4202   CPO  89     LDS 716.                                                                        
20375+3134   STFA 53     B is BD+31@4160.                                                                
20375+1557   BPM2214     [PM2000] 2354200 + [PM2000] 2354541.                                    Gvr2010 
20375+1436   BU  151     bet Del = 6 Del = Rotanev.                                              Mlr1955c
                         1975.545, 1975.956: The elements quoted by Finsen (1938) and            Fin1938a
                         Couteau (1962) each give theta and rho greater than those               Cou1962e
                         observed.                                                               BLM1978 
                         Primary is a giant, according to isochrone fit.                         Sod1999 
                         Two AO photometric analyses by ten Brummelaar et al. both include       TtB1996b
                         mass determination and spectral typing.                                 TtB2000 
             HJ 5545     AB,C: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
             STF2704     AB,D: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB,D: H 4  35.                                                          MEv2010 
             HJ 5545     AB,C: Rectilinear solution by Hurowitz et al. (2014).                   USN2014b
             STF2704     AB,D: Rectilinear solution by Friedman et al. (2012).                   USN2012a
20375+1130   BPM2213     [PM2000] 2354156 + [PM2000] 2353691.                                    Gvr2010 
20375-0303   J  1775     Barton listed at this position, from the San Fernando astrographic              
                         catalog, a triple star which does not resemble the one observed.        J__1941d
20375-2817   BRT3093     A likely plate flaw.                                                    Grv2021b
20376-4717   HJ 5209     alp Ind. Spectrum K0IIICNIII-IV.                                                
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
20377+3322   STF2705     Spectrum: K0IIb/IIIBa0.2.                                                       
20377+1736   BPM2215     [PM2000] 2355077 + [PM2000] 2355402.                                    Gvr2010 
20377+0152   J  3255     Aka J  1776.                                                            Dam2016d
20378+3224   ARY  48     HJL 284.                                                                HJL1986 
20378-2451   BRT3094     A likely plate flaw.                                                    Grv2021b
20379+5144   OSO 128     G230-044. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates.                                                  Oso2004 
20379+2522   POU4757     A is a Beta Lyrae-type system..                                                 
20379-6038   MUG   4     AB are CPM. Followup spectroscopy confirmed the B component is                  
                         a dwarf; estimated mass is 0.363 +- 0.018 Msun.                         Mug2005 
                         AB pair bound. Primary is G3, and is planet host star.                  Egn2007 
                         AB: A is exoplanet host, P=1316d                                        Tok2014d
             EGN  25     Ba,Bb pair bound; spectral types estimated as M1.5-M4.5 and M2.5-M5.5           
                         dwarfs, masses 0.29 +/- 0.02 and 0.19 +/- 0.02 Msun.                    Egn2007 
20380+3806   SEI1197     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
20381+3601   HJ 1553     SEI1200.                                                                Nsn2017d
20383+4804   ES   89     H 4  24.                                                                MEv2010 
20383+3814   SEI1202     Primary not seen on POSS plate; may be either variable star or flaw on          
                         AC Potsdam plate.                                                               
20383+1623   BPM2216     [PM2000] 2357756 + [PM2000] 2357789.                                    Gvr2010 
20383-0106   BU  672     71 Aql. A is a long-period spectroscopic binary.                                
20384-2100   RST9008     Previously known as RST5551a.                                                   
                         Measures uncertain, needs speckle.                                              
20386+1000   BRT2187     J 3100.                                                                         
20387+3838   STF2708     AB and AC: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB: H N  87.                                                            MEv2010 
20388+0202   HJ  920     BAL 1566.                                                                       
20390+1400   BPM2217     [PM2000] 2360815 + [PM2000] 2360528.                                    Gvr2010 
20390-3445   BRT1811     A likely plate flaw.                                                    Grv2021b
20391+3103   J  1238     BRT 284.                                                                Brt1929b
20391+1550   BU  288     AE: Kuiper (1961) lists the measure as AC, but notes "This is, of               
                         course, not the companion C measured by Burnham as given in the ADS,            
                         but, like D, a fainter and closer companion not previously seen.        Kui1961b
20391+1526   BPM2219     [PM2000] 2361308 + [PM2000] 2361380.                                    Gvr2010 
20391+1243   BPM2218     [PM2000] 2361255 + [PM2000] 2360960.                                    Gvr2010 
20391+1005   STT 533     kap Del = 7 Del. AC = LDS1044.                                                  
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: SHY 334. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
             kap Del     Gontcharov & Kiyaeva (2010 detect variation in Hipparcos data which             
                         they conclude is due to an unseen companion, orbiting the primary with          
                         a period of 45 +/- 5 years. The companion is >4 mag fainter than the            
                         primary; spectral type estimated as WD or RD, mass 0.4 +/- 0.3 Msun.    Gon2010 
20392-0609   RAS  31     Silicon star, type A0; companion close to F0.                           Ras2014 
20393-1457   HU  200     tau 2 Cap = 14 Cap.                                                             
20394+0029   HJ 2984     1 Aqr.                                                                          
20395+1812   BPM2220     [PM2000] 2362752 + [PM2000] 2362234.                                    Gvr2010 
20396+2018   WFC 257     HJL 285.                                                                HJL1986 
20396+1555   WCK   2     Aa,Ab: alp Del = 9 Del = Sualocin. Spectroscopic binary now resolved by         
                         interferometry.                                                                 
                         Uniform disk diameter  0.407 +/- 0.022 mas,                                     
                         Limb darkened diameter 0.420 +/- 0.022 mas,                                     
                         Teff = 13300 +/- 1300 K based on LDD.                                           
                         Radius is 3.02 +/- 0.19 \rsun.                                          CIA2019a
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 6.43 +/- 3.52, 4.55, and 2.82 Msun, respectively.  Mlk2012 
20396+1120   BPM2221     [PM2000] 2363164 + [PM2000] 2362824.                                    Gvr2010 
20396+0458   KUI  99     For initial attempt I recorded 1950,497, 44.2deg, 0.31, dm 1.0 for a            
                         star 2 arcmin south of this pair. Such star was not found on later              
                         occasions when, however, the seeing was less satisfactory.              WRH1951 
             BAG  14     Visual primary is 920d SB2 (#1253 in Batten et al. 1989). There is      Bte1989 
                         some spectroscopic evidence for a third star.                                   
                         Malogolovets et al. (2007) derive spectral types for Aa, Ab, and B of   Mlg2007 
                         K5, K9, and K8, respectively. Mass of Aa+Ab is 1.28 +/- 0.15 Msun,              
                         entire triple has mass 1.69 +/- 0.27 Msun. The system is weakly                 
                         hierarchical.                                                                   
20399+1115   ENG  75     AB: Components share CPM. Spectral type of B component M1V +/- 1.       Cvn2007 
                         CHARA Array Limb-darkened diameter  0.494 +/- 0.046 mas,                CIA2008c
                         R =  1.79  +/- 0.17  \rsun.                                                     
             CVN  17     Aa,Ab: Companion is a probable late-K dwarf.                            Cvn2006 
                         Chauvin et al. (2011) make a combined astrometric/RV study of the               
                         expoplanet host binary HD 196885, and derive a mass function for the            
                         planet (M_Aa1 sin i) = 2.98 +/- 0.05 Mjup and a mass for the stellar            
                         companion M_Ab = 0.45 +/- 0.01 Msun. (Note: their paper refers to the           
                         700mas pair as AB and the planet as Ab)                                 Cvn2011 
20400+1749   BPM2222     [PM2000] 2365017 + [PM2000] 2364633.                                    Gvr2010 
20401-2411   HJ 5212     Spectrum: G6/8IIICNIV.                                                          
20402+1248   BPM2223     [PM2000] 2365687 + [PM2000] 2365276.                                    Gvr2010 
20402+1126   BPM2224     [PM2000] 2365763 + [PM2000] 2365528.                                    Gvr2010 
20403+6030   TOK 679     Estimated mass(B)=0.34. DSS2 indicates that B is physical.              Tok2014d
20403+5413   OSO 129     G230-045. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
20403-4956   KRW   2     Based on a comparison of images spanning 23 years, Krawczenko (2014)            
                         determined that this pair shares common proper motion. From colors,             
                         spectral types for the primary and secondary appear to be about K0 and          
                         G8V, repectively; distances are 640 and 870 pc, masses about 0.79 and           
                         0.81 Msun.                                                              Krw2014a
20404-3251   SHY 781     HIP 102021 + HIP 101693.                                                        
20406+2948   HO  137     A is a spectroscopic binary.                                                    
20406+1559   BPM2225     [PM2000] 2367645 + [PM2000] 2367729.                                    Gvr2010 
20406+1539   HDS2947     New observations of this object indicate that the orbit is eccentric,           
                         and that we observed the system near periastron (and below the                  
                         diffraction limit of the DCT). The orbital elements obtained confirm            
                         that picture, yielding a total mass of 3.4 +/- 0.5 Msun. The composite          
                         spectral type is F5 and the system has a magnitude difference of about          
                         1, so that we might suggest that the individual spectral types are F4           
                         and F9. If so, then the total mass would be on the order of 2.5 Msun,           
                         which is about 2 sigma lower than the value implied by the current              
                         orbital elements and the parallax of 13.96 +/- 0.55 mas. However,               
                         because there is only one point near periastron at the moment, the              
                         orbital elements will of course be modified with time.                  Hor2015b
20406-2639   CHR 186     Reported by Andersen et al. (1985 AAA 59, 15) as SB2, with 13 RVs       Bvr1986 
                         measured by Beavers & Eitter (1986).                                    McA1993 
20408+1956   LDS1045     AC: NLTT 49682/49681                                                    Chm2004 
20408+1733   BPM2226     [PM2000] 2368241 + [PM2000] 2367862.                                    Gvr2010 
20410+3905   MCA  62     Also a spectroscopic binary.                                                    
20410+3218   BNU   7     Aa,Ab: 49 Cyg. B is a spectroscopic binary.                                     
             STF2716     AB: H 2  98.                                                            MEv2010 
20412+0338   BAL2543     J 1777.                                                                         
20412-1320   WSI 163     Optical/physical nature ascertained from Gaia DR2.                      FMR2019b
20413+1327   BPM2227     AB: [PM2000] 2370282 + [PM2000] 2370311.                                Gvr2010 
             BPM2228     BC: [PM2000] 2370311 + [PM2000] 2370671.                                Gvr2010 
20413+1111   BPM2229     [PM2000] 2370391 + [PM2000] 2370466.                                    Gvr2010 
20414+4517   H N  73     alp Cyg = 50 Cyg = Deneb                                                        
20414-0835   HDO 159     BD-09@5552 at 20 37.0 -09 00 has a companion 1895: 238.8@, 7.65",               
                         mags 9.3-11.6.                                                                  
20414-1352   BRT2776     A likely plate flaw.                                                    Grv2021b
20415-2012   ARA1213     A likely plate flaw.                                                    Grv2021b
20416+5730   OSO 130     G230-047. AC is not a common proper motion pair                         Oso2004 
20416+3637   SEI1218     20416+3637ALI 423                                                               
20417+1716   BPM2230     [PM2000] 2372161 + [PM2000] 2372227.                                    Gvr2010 
20417-7521   DUN 232     mu 2 Oct                                                                        
                         A is exoplanet host P=4100d                                             Tok2014d
20418+1404   J  2575     Jonckheere unable to recover                                            J__1962a
20418-1057   HIP 102130  Unresolved. SB according to both GCS and CfA.                           Tok2013b
20420+1212   BPM2231     [PM2000] 2373040 + [PM2000] 2372773.                                    Gvr2010 
20421+1341   BPM2232     [PM2000] 2373427 + [PM2000] 2373357.                                    Gvr2010 
20422+5020   BU  675     51 Cyg.                                                                         
20423+4549   STT 411     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
20424+5611   VKI  47     Wolf 1082.                                                                      
20424+1117   OSO 131     G144-028. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
20424-3031   H N 101     B is CD-30@18114.                                                               
20425+4916   ARG  39     AB: ES   92.                                                                    
20425+2310   LDS6416     NLTT 49744/49741                                                        Chm2004 
20427+2355   POU4907     AB: Original Pouteau theta value (136.1deg) appears to have been in     Pou1933 
                         error. His actual value was probably 360-136.1 = 223.9deg.                      
20427+1440   BPM2233     [PM2000] 2376049 + [PM2000] 2375997.                                    Gvr2010 
20428+1244   BPM2234     [PM2000] 2376292 + [PM2000] 2376109.                                    Gvr2010 
20429+1152   BPM2235     [PM2000] 2376640 + [PM2000] 2376989.                                    Gvr2010 
20429-1856   WOR  41     Worley (1989) measures were originally listed as confirmations of       Wor1989 
                         Kuiper's 1943 observation of 20429-1857 KUI 100AB. However, the A comp  Kui1943 
                         of KUI 100 has very high proper motion; separation and angle in 1978            
                         would be very different. We assume that Worley measured this pair near          
                         KUI 100; the separation and angle agree, but Worley's magnitude                 
                         difference estimates are rather different.                                      
20429-1857   KUI 100     See note to 20429-1856 WOR  41.                                                 
20430+1734   BPM2236     [PM2000] 2377293 + [PM2000] 2377091.                                    Gvr2010 
20431+3645   SEI1227     B is BD+36@4205.                                                                
20431+1705   BLL  51     A is the variable S Del. B is BD+16@4350.                                       
20432+5707   V379 Cep    Harmanec et al. find spectroscopic and photometric evidence to suggest  Hmn2007 
                         V379 Cep is a quadruple system comprised of two close binaries.                 
                         Components Aa+Ab orbit with a period of 99.76d and i=90deg, and have            
                         masses of 10.56 and 6.09 Msun. Components Ba+Bb orbit in 158.71d, and           
                         have a combined mass of about 11Msun. A+B orbit with an estimated               
                         period of 7878d, and assuming a distance of ~500pc may reach a                  
                         separation of roughly 50mas. Angular separations of the close pairs             
                         are each in the 1-2 mas range.                                                  
20432-2049   CHR 222     First detected as an occultation binary by Evans.                       Evn1971 
20433+5521   LLO   1     GJ 802.  Using dH and 2MASS H magnitude, plus a parallax of 64.5 +- 2           
                         mas, Lloyd et al. (2006) derive absolute H magnitudes of 8.11 +/- 0.07  Llo2006 
                         and 12.79 +/- 0.3 mag for the two components.  They also derive an              
                         orbit using this resolved measure with STEPS astrometric observations.          
                         This orbit yields dynamical masses of 0.175 +/- 0.021 and 0.064 +/-             
                         0.032 Msun for A and B, respectively.                                           
                         Ireland et al. (2008) combine spectroscopic data with aperture-masking  Ire2008 
                         observations, plus earlier astrometry by Pravdo et al. (2005; measures  Prv2005 
                         extracted from their figures) for orbital solutions of this young               
                         triple. The inner Aa,Ab pair are equal-mass stars in an orbit of                
                         period 0.795 days and an inclination in the range 74-83deg, which may           
                         indicate coplanarity with the wider orbit. The total mass of the inner          
                         pair is 0.280 +/- 0.010 Msun, that of the B component is 0.063 +/-              
                         0.005 Msun. Absolute magnitudes are determined for all components in            
                         the J-, H-, and K-bands. Data are compared with evolutionary models.            
                         GJ 802. This is a well-studied close triple system (e.g. Ireland et     Ire2008 
                         al. 2008). It consists of a spectroscopic pair with a period of only            
                         19 h, and a brown dwarf at a separation of ∼90 mas. Both are too close  .     
                         to be resolved with AstraLux, and there are no other candidates in the          
                         field of view.                                                          Jnn2014 
20433+4456   ES 2699     B is BD+44@3552.                                                                
20434+3535   ISM   5     The Cepheid X Cyg.                                                              
20435+1504   CIA  11     del Del.                                                                        
                         CHARA Array Limb-darkened diameter of A,B:                              CIA2018a
                           =   0.500 +/- 0.014,  0.507 +/- 0.014 mas,                                    
                         R =   3.43  +/- 0.11 ,  3.48  +/- 0.11 \rsun,                                   
                         L =  32.4   +/- 4.2  , 28.8   +/- 3.4  \lsun,                                   
                         M =   1.78  +/- 0.07 ,  1.62  +/- 0.07 \msun,                                   
                         Teff = 7440 +/- 210  , 7110   +/- 180 K.                                        
                         Orbital parallax = 15.72 +/- 0.22 mas.                                          
20436+4514   CBL  85     NI   41.                                                                        
20437+1635   BPM2237     [PM2000] 2379651 + [PM2000] 2380014.                                    Gvr2010 
20438+1330   BPM2238     [PM2000] 2380121 + [PM2000] 2380344.                                    Gvr2010 
20439+3119   ES  366     According to Vyssotsky & Mateer, ES 366 is probably BD+30@4155.         Vys1952 
                         Aka HDS2950.                                                            Dam2013 
                         A is also a 21d spectroscopic binary.                                   Tok2019b
20439+1113   BPM2239     [PM2000] 2380769 + [PM2000] 2381099.                                    Gvr2010 
20440+1225   HJ 1566     C component is galaxy = UGC 11620 = LEDA 65281.                         Dam2010 
20440-3147   JSP 816     Not in Michigan Vol. XI.                                                        
20442+2154   OSO 132     G144-033.  Not a common proper motion pair, based on comparison with            
                         POSS2 red plates.                                                       Oso2004 
20442+1731   BPM2241     [PM2000] 2381821 + [PM2000] 2381675.                                    Gvr2010 
20442+1209   BPM2240     [PM2000] 2381758 + [PM2000] 2381888.                                    Gvr2010 
20443+1101   BPM2242     [PM2000] 2382256 + [PM2000] 2382347.                                    Gvr2010 
20444+1500   BPM2243     [PM2000] 2382565 + [PM2000] 2382639.                                    Gvr2010 
20445+1415   BPM2244     [PM2000] 2382992 + [PM2000] 2382792.                                    Gvr2010 
20446+4041   HJ 1574     HJ 1573 and HJ 1574 are obvious on ALADIN, forming roughly 10" and 8"           
                         pairs are roughly Herschel's position angles. Burnham's observation of  Bu_1906 
                         HJ 1574 appears discrepant.                                                     
20446+4040   HJ 1573     Burnham (BDS, part II) notes that HJ 1573 and 1574 form "a double-      Bu_1906 
                         double star; a curious object".                                                 
20446+1642   BPM2246     AB: [PM2000] 2383150 + [PM2000] 2383263.                                Gvr2010 
             BPM2247     AC: [PM2000] 2383150 + [PM2000] 2383211.                                Gvr2010 
20446+1635   BPM2248     AB: [PM2000] 2383182 + [PM2000] 2383659.                                Gvr2010 
             BPM2249     AC: [PM2000] 2383182 + [PM2000] 2383425.                                Gvr2010 
             BPM2250     BC: [PM2000] 2383659 + [PM2000] 2383425.                                Gvr2010 
20446+1605   BPM2245     [PM2000] 2383050 + [PM2000] 2382885.                                    Gvr2010 
20446+1154   BPM2251     [PM2000] 2383255 + [PM2000] 2383542.                                    Gvr2010 
20447+2032   BRT2484     J  3347.                                                                Nsn2016 
20448+3022   AG  410     HJL 286.                                                                HJL1986 
20448+2500   BRT3361     Originally published as BRT 216.                                        Brt1928 
20448+1730   BPM2252     [PM2000] 2384052 + [PM2000] 2383917.                                    Gvr2010 
20448+1512   BPM2253     [PM2000] 2384091 + [PM2000] 2383815.                                    Gvr2010 
20449+1219   B  2910     Aa,Ab: Needs speckle confirmation. One component possibly variable.             
20450+1244   D    32     CD: Measures listed as new CE pair were all actually of DC.                     
20450-0140   LDS 722     NLTT 49821/49819                                                        Chm2004 
20452+1108   BPM2254     [PM2000] 2385504 + [PM2000] 2385162.                                    Gvr2010 
20452-3057   FAL  70     Upon discovery of the wide COM pair TOK 340AC by Tokovinin & Lepine,    Tok2012c
             JSP 817     the C component was found to be the primary of 20447-3102 JSP 817.              
                         The WDS designation of the JSP pair was changed to deflect its                  
                         membership in this CPM multiple.                                                
20452-3120   LDS 720     AB: Distance 4600". A is the BY Dra-type variable AU Mic, also nearby           
                         star Gliese 803. High common proper motion pair.                                
                         AB: SHY  99. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         BC: Due to its large distance from A, the WDS designation for BC was            
                         originally 20419-3226.  Also known as BRT1812 or HDS2953 and as nearby          
                         star Gliese 799 AB. Discovered by Barton in 1913 but later incorrectly  Brt1936a
                         called Luyten by Voute, the BC pair became known as LDS 720 despite     Vou1947a
                         having never been observed by Luyten. See also the following note for           
                         20452-3122WOR  40.                                                              
                         GJ 799. Member of the bet Pic moving group.                             Zuc2001b
                         BC: Premature orbits have been computed. A flare star, AT Mic, sharing          
                         common proper motion with -32@16135 at 34@, 77.5'.                              
                         Measure of 1927.70 made by triangulation of multiple measures.                  
                         Measure of 1928.57 made by triangulation of multiple measures.                  
                         Star A (mag 8.6, M0Ve) 1.3 deg distant; position 204509.5-312027                
                         (2000) shares the large proper motion. Star C is the flare star                 
                         AT Mic.                                                                         
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
20452-3122   WOR  40     Located ~80" south of LDS 720A, this pair has been inadvertently                
                         observed as LDS 720BC (located ~80' south of A) on numerous occasions.          
                         Preliminary orbital analysis of LDS 720BC showed discrepancy in                 
                         orbital motion beginning with Worley measure of 1978, hence the WOR             
                         designation.                                                                    
20453+6150   BU 1493     eta Cep = 3 Cep.                                                                
                         NPOI Limb-darkened diameter    2.518 +/- 0.009 mas,                             
                         R =    3.86 (+/- 0.02   )  \rsun,  Teff = 5000 +/-   9 K,                       
                         L =    8.4 +/-   0.0 \lsun.                                             NOI2023 
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2014).                         USN2014b
20453-0239   BRT 506     A likely plate flaw.                                                    Grv2021b
20454+5906   ES 2700     STI 2552.                                                                       
20454+5735   ENG  76     AB: A is an SB. B is BD+57@2241.                                                
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
             CIA   1     Aa,Ab: Farrington et al. (2010) present two possible orbits for this    CIA2010 
                         F8IV-V + F9IV-V pair. One is based on speckle plus K'-band CHARA Array          
                         separated fringe packet observations, the other is a combined solution          
                         including spectroscopic data.  The resulting orbital parallax is                
                         39.8+/-4.8 mas, the masses 1.071+/-0.037 and 1.047+/-0.037 Msun.                
                         The aperture and method, 8m and speckle, are set to give the                    
                         resolution capability of this technique, which is less than classical           
                         interferometric methods.                                                        
                         Aa,Ab: Orbit determined by fitting revised Hipparcos intermediate               
                         astrometric data. Derived component masses are 0.47 +/- 0.22 and                
                         0.45 +/- 0.21 Msun.                                                     Ren2010 
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 2.72 +/- 0.16, 2.39, and 2.38 Msun, respectively.  Mlk2012 
             ENG  76     AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
20454+4023   OSO 133     G210-033.  None is a common proper motion pair, based on comparison             
                         with POSS2 red plates.                                                  Oso2004 
20456+3043   STF2726     52 Cyg.                                                                         
                         H 2  25.                                                                MEv2010 
20456+2553   J  1074     Precise coordinates have been corrected, following an examination of            
                         this system by Nanson & Knapp (2017).                                   Nsn2017e
20456-0853   HDO 160     J 1778.                                                                         
20457+1537   BPM2255     [PM2000] 2387348 + [PM2000] 2387644.                                    Gvr2010 
20457+1017   OSO 134     G025-001.  Not a common proper motion pair, based on comparison with            
                         POSS2 red plates.                                                       Oso2004 
20458+1405   BPM2256     [PM2000] 2387581 + [PM2000] 2387513.                                    Gvr2010 
20459+4448   ES 2701     B is BD+44@3570.                                                                
20461+4452   ES   30     A is the semiregular variable RR Cyg. BD+44@3571a.                              
20461-2516   EHR  17     Primary is psi Cap. Companion appears to be a background star.          Ehr2010 
20462+3358   CHR 100     eps Cyg = 53 Cyg = Aljanah. A spectroscopic binary.                             
                         van Maanan notes a common high-proper motion companion located 1'.3     Maa1934 
                         west and 0'.1 south of eps Cyg. The companion (photographic magnitude           
                         ~14.8) was found on two plates taken with the Mt. Wilson 60inch over            
                         an interval of 12 years.                                                        
                         1991.8987: This finally confirms the discovery observation of this              
                         component, made in 1983 (McAlister et al 1987). A number of unresolved  McA1987b
                         observations of this very close system, dating from 1979 to 1981, were          
                         published by Hartkopf & McAlister (1984).                               Hrt1984 
                         A single lined spectroscopic binary with a period of 55 yr yields an    Grf1994a
                         estimated semi-major axis of 1.05", so the companion has only escaped           
                         visual resolution only due to its faintness. MK III measures of the     MkT2003 
                         diameter and no loss of coherence rules out companions with dm < 5.7.           
                         It is possible that CHR 100 is an artifact caused by wave-front         Tok2010b
                         distortions in the dome. The star was likely observed near the zenith           
                         and the separation of the putative companion is close to the first              
                         diffraction ring, as typical for such artifacts.                                
                         Mk III Limb-darkened diameter  4.62 mas.                                MkT1991 
                         Mk III Limb-darkened diameter  4.612 +/- 0.046 mas.                     MkT2003 
             STT 594     AB: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB: Rectilinear solution by Friedman et al. (2012).                     USN2012a
20462+1554   STF2725     AB: H 2  66.                                                            MEv2010 
                         A premature orbit has been computed.                                            
20463+2740   BRT3362     Originally published as BRT 218.                                        Brt1928 
20463+1624   BPM2257     [PM2000] 2389395 + [PM2000] 2389229.                                    Gvr2010 
20465+2403   POU4975     Aka POU4989.                                                            Dam2016d
20465+1439   BPM2259     [PM2000] 2390103 + [PM2000] 2389732.                                    Gvr2010 
20465+1429   BPM2260     [PM2000] 2390184 + [PM2000] 2390538.                                    Gvr2010 
20465+1131   BPM2258     [PM2000] 2389941 + [PM2000] 2390160.                                    Gvr2010 
20465-2652   HJ 5220     B is CD-27@15024.                                                               
20466+5951   MLR 236     G230-049.  Not resolved in our images                                   Oso2004 
20466+4632   KUI 101     Elongation suspected by Hough in 1885.                                          
20466+1616   BPM2261     [PM2000] 2390546 + [PM2000] 2390422.                                    Gvr2010 
20466+1532   J  3110     Aka OL  219.                                                            Dam2013 
20467+2044   HJ 2999     Erroneously designated as HJ 2899 in BDS.                               Bu_1906 
20467+1607   STF2727     gam Del. A premature orbit has been computed. 1865.74 observation of    Tal1868 
                         Talmadge lists 16.537 in the Table for the separation but 11.536 in             
                         the notes. The 11.536 value is included.                                        
                         NLTT 49870/49868                                                        Chm2004 
                         H 3  10.                                                                MEv2010 
                         Toyota et al. (2009) monitored the RV of both the A and B components            
                         every 1-2 months between 2003 Mar - 2007 Nov, using a high-dispersion           
                         echelle (precision ~10 m/s).   Standard deviations of the RVs of both           
                         components are <40 m/s and velocities show no periodic variation.               
                         These results rejects the association of a planet of mass > 1.8 Mjup            
                         with either star.                                                       Toy2009 
             FYM  18     The purported AC pair was in error and has been deleted.                FyM2014b
20467+1523   BPM2263     [PM2000] 2390967 + [PM2000] 2390725.                                    Gvr2010 
20467+1343   BPM2262     [PM2000] 2390840 + [PM2000] 2390664.                                    Gvr2010 
20468+1602   BPM2264     [PM2000] 2391076 + [PM2000] 2390777.                                    Gvr2010 
20468+0733   GAA   8     NN Del.                                                                         
                         Ma,Mb = 1.4445 +/- 0.0029, 1.3266 +/- 0.0021 \msun,                     GaA2019 
                         orbital parallax =  5.953 +/- 0.023 mas.                                        
20469+3252   ARG  93     B is BD+32@3936a.                                                               
20471+1257   BPM2265     [PM2000] 2392193 + [PM2000] 2392270.                                    Gvr2010 
20472+3422   BU  677     A is the irregular variable T Cyg.                                              
20473-0408   LDS4858     NLTT 49881/49880                                                        Chm2004 
20474+3629   MCA  63     Aa,Ab: lam Cyg = 54 Cyg. A is a spectroscopic binary, which has now             
                         been resolved by interferometry into a close and rapidly moving pair.           
                         1986.567: The separation of this partially resolved pair was                    
                         calculated under the assumption of zero or otherwise known magnitude            
                         difference.                                                             Tok1985 
             STT 413     Only elements P and T have been amended by Starikova (1982) from the    Sta1982b
                         orbit of Baize (1983).                                                  Baz1983a
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
             S   765     AC: H 6  32.                                                            MEv2010 
20474+2808   BRT3363     Originally published as BRT 219.                                        Brt1928 
20477+1519   BPM2266     [PM2000] 2394416 + [PM2000] 2393992.                                    Gvr2010 
20478+4750   ES  810     A is a spectroscopic binary.                                                    
20478+2519   POU4996     DH: Originally 20476+2518 POU4996, but primary found to be D component          
                         of 20478+2519 BUP 218AD.                                                        
                         DH: DAM 514DH.                                                                  
20478+1109   BPM2267     [PM2000] 2394709 + [PM2000] 2394870.                                    Gvr2010 
20478+0600   BU   65     13 Del. Variable.                                                               
                         This system has an estimated delta m of 3.6 magnitudes; the secondary           
                         probably lies just outside the observed window in the CFHT observation          
                         of 1985.521.                                                                    
20478-3636   LWR  17     BO Mic                                                                          
20480+3917   A  1434     One component is the Beta Lyrae-type system V367 Cyg, P = 18.6d.                
                         Variability of both components suspected.                                       
                         This observation was listed in Blazit et al. (1977) under its correct   Bla1977a
                         GC number, but misidentified as ADS 14394.                                      
                         AB,C: Additional notes may be found in Aitken (1932).                   A__1932a
20480+1816   BPM2268     [PM2000] 2395534 + [PM2000] 2395797.                                    Gvr2010 
20481+2727   BU   66     Includes V402 Vul, a Beta Lyr type eclipsing binary, P = 1.49938d.      Zas2012 
20481+1601   BPM2269     [PM2000] 2395849 + [PM2000] 2395614.                                    Gvr2010 
20482+3326   ES 2377     ES 2377a. See note for 20487+3334ES 9006.                                       
20482+2622   COU 827     Aka TDT2548.                                                                    
20484+4002   SEI1255     AB: Also known as J  1237AB.                                                    
20484+1134   BPM2270     [PM2000] 2396972 + [PM2000] 2396824.                                    Gvr2010 
20484+0426   AG  267     HJL 287.                                                                HJL1986 
20484-1812   S   763     AB: H N  10.                                                            MEv2010 
                         B is BD-18@5778.                                                                
                         CD: ARA 501.                                                                    
20485+1628   BPM2271     [PM2000] 2397156 + [PM2000] 2397510.                                    Gvr2010 
20485+1545   BPM2272     [PM2000] 2397328 + [PM2000] 2397127.                                    Gvr2010 
20485-4359   DON 992     iot Mic                                                                         
20486+1223   BPM2273     [PM2000] 2397439 + [PM2000] 2397606.                                    Gvr2010 
20487+5155   STF2732     H 2 100.                                                                MEv2010 
20487+3334   ES 9006     This pair was not given a designation in Es_1930, but followed ES 2377          
                         in Espin's list of measures. As a result, it was erroneously listed     Es_1930 
                         as ES 2377AC. Also, ES 2377 was incorrectly assigned this pair's WDS            
                         designation.                                                                    
20488+3426   SEI1256     V2247 Cyg. Primary is eclipsing binary of Algol-type, period 1.25486d.  Zas2014 
20488+1943   JNN 286     G 144-39. Estimated age 1000-10000 Myr; masses 0.50 +/- 0.07 and 0.24           
                         +/- 0.05 Msun; a ~7.4 au.                                               Jnn2014 
20488+1106   BPM2274     [PM2000] 2398470 + [PM2000] 2398468.                                    Gvr2010 
20488+0512   OSO 135     C is not a common proper motion companion to A                          Oso2004 
20489+4607   HJ 1581     55 Cyg. Variable.                                                               
20489+1558   BPM2275     [PM2000] 2398740 + [PM2000] 2398905.                                    Gvr2010 
20489-6847   SHY 782     HIP 102725 + HIP 103917.                                                        
20491+3640   SEI1260     ALI 428.                                                                        
20493+5845   STTA211     B is BD+58@2176.                                                                
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
20493+3923   ALI 952     BC: Originally 20492+3917 ALI 952AB, but primary found to be B                  
                         component of 20493+3923 SEI1263AB.                                              
                         Hipparcos suspected non-single.                                                 
             DAM  26     BD: Originally 20492+3917 DAM  26AC.                                            
20493+3314   ES   31     A is a semiregular variable.                                                    
20493+0156   OSO 136     G025-005. Not a common proper motion pair, based on color and                   
                         comparison with POSS2 red plates.                                       Oso2004 
20493-1945   ALP  25     2MASSW J2049197-194432                                                          
                         Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
20494+1124   J   194     Triple solution together with C (HIP 102784), which is clearly                  
                         optical with a faulty HIP position.                                     Sod1999 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.09 +/- 0.67, 1.42, and 0.65 Msun, respectively.  Mlk2012 
20495+1106   BPM2276     [PM2000] 2400680 + [PM2000] 2400282.                                    Gvr2010 
20496+5008   ES   94     Spectrum of B: F8V.                                                             
20496+1233   BU 1495     15 Del.                                                                         
20497+2825   MLB 534     Aka  J  2323.                                                           Dam2013 
20497+1331   BPM2277     [PM2000] 2401465 + [PM2000] 2401398.                                    Gvr2010 
20498-2829   LDS 725     NLTT 49943/49942                                                        Chm2004 
20499+3531   SEI1266     ALI 208.                                                                        
20500+0533   STTA210     B is BD+04@4556.                                                                
20500-1154   BRG  31     2MASS J20500010-1154092 has a close companion detected with AstraLux,           
                         but it has not yet been confirmed through common proper motion.                 
                         However, since the separation is quite small (~0.47") and the                   
                         brightness and color of the companion is consistent with expectations,          
                         the system counts as binary for statistical purposes.                   Jnn2012 
20500-3347   HJ 5224     alp Mic                                                                         
20501+4404   STT 595     AB: 56 Cyg.                                                                     
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
20501+1556   BPM2278     [PM2000] 2402829 + [PM2000] 2402581.                                    Gvr2010 
20501-2722   HJ 5226     B is CD-27@15066.                                                               
20503+1317   BPM2279     [PM2000] 2403584 + [PM2000] 2403791.                                    Gvr2010 
20504+1459   BPM2280     [PM2000] 2403969 + [PM2000] 2404177.                                    Gvr2010 
20506+1601   BPM2281     [PM2000] 2404763 + [PM2000] 2404604.                                    Gvr2010 
20507+1959   ROE  16     J 1141.                                                                         
20507-3116   B   997     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.39 +/- 0.85, 2.28, and 1.10 Msun, respectively.             Mlk2012 
20509+1544   BPM2282     [PM2000] 2405705 + [PM2000] 2405767.                                    Gvr2010 
20510+3915   SEI1279     ALI 953.                                                                        
20510+3717   SEI1277     ALI 430.                                                                        
20511+3837   SEI1281     ID uncertain - no sign of SEI pair, and ALADIN only indicates one               
                         Astrographic Catalog star in vicinity of Scheiner's coordinates.        Sei1908 
20511+0526   GCB  59     Aka BAL3016.                                                                    
20511-0135   LDS 727     NLTT 50000/49999                                                        Chm2004 
20514+1619   BPM2283     [PM2000] 2407606 + [PM2000] 2407437.                                    Gvr2010 
20514-0538   STF2729     4 Aqr. Alternative spectra F5V+F7V.                                             
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: H 1  44.  AC: H 6  58.                                              MEv2010 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.78 +/- 2.08, 2.50, and 1.27 Msun, respectively.  Mlk2012 
20516-6226   RMK  26     Rectilinear solution by Letchford et al. (2018).                        LRR2018a
20517-4054   HJ 5228     B is CD-41@14265.                                                               
20519-1631   HJ 3001     Aka HJ 1590.                                                            Dam2013 
20520+1422   BRT1956     J 1891.                                                                         
20521+4438   HER  18     Additional notes may be found in Herbig (1962).                         Her1962 
20521+3439   RAO 521     Y Cyg.                                                                          
                         The classification is from Burkholder et al. (1997 ApJ 490, 328). This          
                         eclipsing binary is one of two known double-lined spectroscopic                 
                         binaries which are a runaway objects based on a  large absolute value   Gie1986 
                         of systemic velocity (Gies & Bolton 1986).                              Msn1998a
20522-1904   I   667     See listed this pair twice, as SEE 431 and SEE 432, both misidentified.         
                         Gogshall gave the correct BD identification, but with an erroneous              
                         position; see BDS 10561. Innes rediscovered the pair independently as           
                         I 667. See's angle for SEE 432 requires a correction of +16.9deg.               
                         This correction, the result of an erroneous position of the micrometer          
                         on the telescope, which remained unnoticed because See omitted the              
                         usual precaution of a determination of the parallel, must be applied            
                         to all measures made at the Lowell Observatory during the period                
                         1897.758 to 1897.793.                                                   B__1950c
20522-7519   HJ 5214     B is CPD-75@1660.                                                               
20523+1144   BPM2284     [PM2000] 2410767 + [PM2000] 2410355.                                    Gvr2010 
20523-0030   BAL 927     J 1712.                                                                         
20524+3724   SEI1287     No Astrographic Catalog objects near Scheiner's coordinates and         Sei1908 
                         no obvious binary in field - typo in original catalog?                          
20524+2008   HO  144     Rapid change. Distance < 0.1" 1933-1941. Quadrant uncertain.                    
20524+1353   BPM2285     [PM2000] 2411079 + [PM2000] 2411467.                                    Gvr2010 
20526-1609   SPF   2     Stumpf et al. (2011) estimate the period at 21 +/- 1 yr and the system  Spf2011 
                         mass at > 78 Mjup.  Near-IR colors suggest spectral types T1 +1/-4 and          
                         T2.5 +/- 1.                                                                     
                         SDSS J205235.31-160929.8. Bardalez Gagliuffi et al. (2015) derive a             
                         preliminary orbit for this very low-mass binary, deriving a system              
                         mass of 0.0823 +0.0037/-0.0027 Msun and spectral types L6.0 +/- 2.0             
                         and T2.0 +/- 0.05. (Note: the quoted 2453654.31 Julian date for tau_0           
                         does not appear to correspond to the best-fit T0. To was adjusted to            
                         2455054.31 for the orbit catalog figure.)                               BGg2015 
20527+4607   A   750     Only elements P and T of Muller (1955) were adjusted in computing       Mlr1955b
                         the solution of Starikova (1981).                                       Sta1981a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.02 +/- 0.42, 1.76, and 0.91 Msun, respectively.             Mlk2012 
20527+0720   STF2733     B is BD+06@4675.                                                                
20527-0859   MCA  64     mu Aqr = 6 Aqr. A long-period spectroscopic binary, P = 1782d, now              
                         resolved by speckle interferometry.                                             
20528+3925   SEI1290     ALI1149.                                                                        
20529+0529   GCB  60     J  3208.                                                                        
20531-1134   CHR 101     This system, first announced by McAlister and recalled in a later       McA1984b
                         McAlister paper after repeated attempts at confirmation, has been       McA1993 
                         restored. While perhaps still spurious, the subsequent confirmation or          
                         suspected duplicity (by another technique) makes the discovery                  
                         measurement somewhat more probable.                                             
20532-0221   JNN 126     LP 636-19.                                                                      
                         The M3.0 equal-flux binary was first resolved by Janson et al. (2012),  Jnn2012 
                         and has seen significant orbital motion. Its parallactic distance of            
                         37.9 +/- 5.7 pc (Shkolnik et al. 2012 ApJ 758, 56) implies a physical           
                         separation of ~3-5 au. The expected orbital period is 10-20y.           Bwl2015 
20533+6209   BUP 219     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
20534+3220   ES 2380     Aka BRT 285.                                                                    
20534+1742   BPM2286     [PM2000] 2414347 + [PM2000] 2414479.                                    Gvr2010 
20534-0227   BRT 509     BAL 259.                                                                        
20534-4923   SHY 784     HIP 103107 + HIP 103139.                                                        
20537+5918   A   751     Theta and rho for 1979.7699 were incorrectly given as 178.6 degrees             
                         and 0".106, respectively, by McAlister & Hendry (1982).                 McA1982d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.91 +/- 0.58, 3.41, and 2.69 Msun, respectively.             Mlk2012 
20537+2803   HJ 1589     Doolittle measure 1915.55: 2.3@, 6.65", 10.0-10.1 was assigned to       Doo1923 
                         20535+2751 MLB 572.                                                             
20538+3723   SEI1299     AB: ALI 675.                                                                    
             SEI1301     AC: No star seen on Aladin at AC2000 coordinates of primary. Published          
                         measure corresponds to difference between nonexistent primary and real          
                         B component. Thus the AC measure appears to be another AB measure but           
                         with an error in the coordinates of the A component.                            
20538+3702   SEI1300     J 1075.                                                                         
20538+1451   BPM2287     [PM2000] 2415723 + [PM2000] 2415593.                                    Gvr2010 
20539+1700   BPM2288     [PM2000] 2416138 + [PM2000] 2415981.                                    Gvr2010 
20539-5535   B   505     Measures uncertain, too close. Needs speckle.                                   
20541+4507   STT 422     Morlet et al. note that this has similar position angle, separation,    Mor2000 
                         and delta-m as HDS2979. HDS2979 removed.                                        
20542+1619   BPM2289     [PM2000] 2416997 + [PM2000] 2417339.                                    Gvr2010 
20542-2730   B   509     AC: Also known as TDT2618. The identical nature of these first                  
                         noted by Francisco Manuel Rica Romero.                                  FMR2001 
20543+2405   POU5056     30m error in transcribing epoch-1900 RA led to the incorrect WDS                
                         designation 20242+2401.                                                         
             POU5057     30m error in transcribing epoch-1900 RA led to the incorrect WDS                
                         designation 20242+2401.                                                         
20545+1054   BPM2290     [PM2000] 2417909 + [PM2000] 2417853.                                    Gvr2010 
20548+1403   BPM2291     [PM2000] 2419129 + [PM2000] 2419226.                                    Gvr2010 
20548-5827   B  2487     bet Ind                                                                         
20549+1236   BPM2292     [PM2000] 2419307 + [PM2000] 2419442.                                    Gvr2010 
20550+3929   SEI1311     ALI1150.                                                                        
20550+2805   BU  367     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.62 +/- 0.40, 2.21, and 1.02 Msun, respectively.  Mlk2012 
20550+1423   BPM2294     [PM2000] 2419657 + [PM2000] 2419593.                                    Gvr2010 
20550+1259   BPM2293     [PM2000] 2419506 + [PM2000] 2419671.                                    Gvr2010 
20551-5207   I    18     The known 3".9 pair I 18 with estimated period ~1700 yr cannot explain          
                         the acceleration.                                                       Tok2012a
                         CPM. Is the acceleration caused by this binary or sub-system?           Tok2014d
20552+3755   SEI1312     ALI 677.                                                                        
20553+4218   OSO 137     G212-007. AB, AC, AD, AF and AG are not common proper motion pairs,             
                         based on comparison with POSS2 red plates                               Oso2004 
20553+1236   BPM2295     [PM2000] 2420673 + [PM2000] 2420662.                                    Gvr2010 
20554+1442   BPM2296     [PM2000] 2420873 + [PM2000] 2420634.                                    Gvr2010 
20555-1400   LDS6418     Proper motion +1413 -459. Possible companion 2",                                
                         16th magnitude.                                                                 
                         Both components show false companions due to differential refraction    Skf2013 
                         in SDSS u-band images; but both stars are single at the resolution of           
                         the other SDSS images (well under 2" separation).                               
20556+3912   SEI1319     Primary not seen on POSS plate; may be either variable star or flaw on          
                         AC Potsdam plate.                                                               
20556+2845   BRT  53     Not found by Heintz at IDS position.                                    Hei1990b
                         A likely plate flaw.                                                    Grv2021b
20556+1744   BPM2297     [PM2000] 2421454 + [PM2000] 2421562.                                    Gvr2010 
20556+1234   HJ 1592     16 Del = chi Del. A is a spectroscopic binary.                                  
20557+0432   STF2735     H 1  61.                                                                MEv2010 
20558-1707   JAY   1     Upon discovery of the wide COM pair TOK 343AC by Tokovinin & Lepine,    Tok2012c
             JAY   2     the C component was found to be the primary of 20560-1711 JAY 2. The            
                         WDS designation of the JAY pair was changed to deflect its membership           
                         in this CPM multiple.                                                           
             TOK 343     AC : Also known as CAB  10.                                                     
                         Member of the bet Pic moving group.                                     Zuc2001b
20559-5555   HJ 5232     B is CPD-56@9562.                                                               
20560+0837   J  1346     J 1355.                                                                         
20561+3731   SEI1322     ID uncertain - no sign of SEI pair, and ALADIN only indicates one       Sei1908 
                         Astrographic Catalog star in vicinity of Scheiner's coordinates. Also           
                         not found by Heintz at IDS position.                                    Hei1985a
20564+5044   BU 1137     A is a spectroscopic binary.                                                    
20565+3048   LDS2935     Aka KPP3421.                                                                    
20565-0134   HJ  927     B is BD-02@5407.                                                                
20566+4455   TRN  30     The image rotator was in an unknown state, so two possible theta                
                         values are listed for the 2001.7338 observation - one for zenith up             
                         and one for north up.                                                   Trn2008 
20567+5656   A   755     Possible quadrant change.                                                       
20567+1818   BPM2298     [PM2000] 2425028 + [PM2000] 2424959.                                    Gvr2010 
20567+1300   STF2736     HJ 1593 identified with this. Also, see Heintz.                         Hei1985a
20568+4254   ENG  77     AB and AC: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
20568-0449   LDS6420     NLTT 50192/50189                                                        Chm2004 
                         This star has a wide companion at about 14" as noted in e.g. the WDS            
                         catalog. It is however single in the separation range covered by the            
                         AstraLux data.                                                          Jnn2012 
20569-0942   BU 1034     7 Aqr.                                                                          
20570+2340   A   175     aka HO  639                                                                     
20571+1131   BPM2299     [PM2000] 2426496 + [PM2000] 2426811.                                    Gvr2010 
20571+0128   J  2332     BAL 1576.                                                                       
20572+4110   HDS2986     System looks triple; 1989.7114 measurement concerns the close binary.   Msn1999b
20573+1515   BPM2300     [PM2000] 2426904 + [PM2000] 2426494.                                    Gvr2010 
20573+1434   BPM2301     [PM2000] 2426917 + [PM2000] 2427177.                                    Gvr2010 
20575-3435   BRT1816     A likely plate flaw.                                                    Grv2021b
20577+5849   YSC 117     Da,Db: Originally 20572+5849YSC 117, but found to be D component of             
                         20577+5849ARN  34AD.                                                            
20577+2624   RAO  24     A new 0".6 binary detected by Robo-AO. It was targeted because of its           
                         variable velocity (Nordstrom et al. 2004) and astrometric               Nrd2004 
                         acceleration (Makarov & Kaplan 2005). The binary is confirmed here,     Mkr2005 
                         helped by the large PM of the primary. Our photometry places B above            
                         the MS. According to Guillout et al. (2009 A&A 504, 829), the target            
                         is young, so its companion could indeed be a PMS star. The object was           
                         already targeted by Metchev & Hillenbrand (2009) in their survey of     Met2009 
                         young stars, but the binary was not detected. After learning of our             
                         discovery, Metchev was able to extract a measurement of the star from           
                         the archival data (S. Metchev 2015, private communication).             Rbr2015d
20579-3339   RED  26     M3, spectroscopic distance 73pc. 19" south of G1 dwarf HD 199410 =              
                         HIP 103481 = 2MASS J20575667-3338566. Proper motion for the G dwarf             
                         +057-079, appears to be minimal relative proper motion. Further                 
                         observations are required to confirm whether the two stars form a               
                         wide binary system.                                                     Red2007a
20580+3713   J  1076     SEI 1337.                                                                       
20580+1426   BPM2302     [PM2000] 2429096 + [PM2000] 2429082.                                    Gvr2010 
20582+1756   BPM2303     [PM2000] 2429755 + [PM2000] 2430103.                                    Gvr2010 
20582+0356   WSI  39     Aka BAL2551.                                                                    
20583+4428   GC 29274    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Radford & Griffin (1975).                                               Grf1975b
20583+3904   SEI1340     ALI 956.                                                                        
20583+1542   JNN 154     2MASS J20581756+1541315 and J20581836+1541211, both from the Riaz et    Ria2006 
                         al. (2006) sample, are separated by only 10" and have comparable                
                         estimated distances (144 and 119 pc) as well as similar proper motions  XXX2010 
                         (e.g. Roser et al. 2010) and thus likely form a physical pair.          Jnn2012 
20584+1050   ENG  78     A is 18 Del = Musica, B is BD+10@4426. BD measures from Burnham,        Bu_1913 
                         WFC, Sturdy, and 2MASS were earlier                                     WFC1998 
                         erroneously labelled as being of the                                    Stu1994 
                         BC pair                                                                 TMA2003 
                         CHARA Array Limb-darkened diameter  1.111 +/- 0.028 mas.                CIA2009a
                         R =  9.00 +/- 0.31 \rsun, L =  47.6 +/-  1.8 \lsun,                             
                         Teff = 5054 +/-  81 K.                                                          
             MUG  16     AE: Spectral type of comoving E comp estimated M4-5, mass 0.19 Msun.    Mug2014 
20585+5028   STF2741     AB: H 1  97.                                                            MEv2010 
20585+1239   BPM2304     [PM2000] 2430706 + [PM2000] 2430642.                                    Gvr2010 
20587+3725   SEI1343     Secondary not seen on POSS plate at published coordinates; later                
                         matches assume there was a 2s error in published RA of the secondary.           
20587-7025   HJ 5231     A is the Algol-type system KZ Pav.                                              
                         Spectrum composite; F2+A2.                                                      
20588+1701   BPM2305     [PM2000] 2431836 + [PM2000] 2431563.                                    Gvr2010 
20589+1741   BRT2487     J 2335. J notes that these are two different pairs.                             
20591+0418   STF2737     eps Equ = 1 Equ. Primary is 2.03d SB1.                                  Tok2006 
                         AC: Star C (mag. 7.3, dF4) is in slow retrograde motion at 10".                 
                         Period of AC estimated at 5200y.                                        Tok2006 
                         AB,C: Hyperbolic orbit by Zeller (1965). Ephemeris covers 1831-2042.    Zel1965 
                         sigma = areal constant in the true orbit = 0.1952 arcsec^2/yr                   
                         q = periastron distance in the true orbit = 10".78                              
                         AB,C: HJL 288.                                                          HJL1986 
                         BC: H 3  21.                                                            MEv2010 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 4.17 +/- 2.42, 2.73, and 1.33 Msun, respectively.  Mlk2012 
20591-1313   HU   83     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 6.80 +/- 7.32, 3.36, and 1.45 Msun, respectively.             Mlk2012 
20592+3718   ALI 434     AC2000 position of secondary shows no star on Aladin images. Appears            
                         to be error in AC coordinates of secondary. Possibly an error in the            
                         reduction of the secondary measure. The companion at 45" appears to be          
                         the most likely intended companion.                                             
20592+1513   BPM2306     [PM2000] 2432866 + [PM2000] 2432830.                                    Gvr2010 
20592+1132   JCT   4     HJL 289.                                                                HJL1986 
20593+5303   JNN 287     Estimated age 1000-10000 Myr; masses 0.54 +/- 0.05 and 0.28 +/- 0.03            
                         Msun; a ~22.8 au.                                                       Jnn2014 
20594+1614   BPM2307     [PM2000] 2433655 + [PM2000] 2433548.                                    Gvr2010 
20596+3558   SEI1355     J 1151.                                                                         
20598+4731   MCA  65     59 Cyg. A is an irregular variable, V832 Cyg, and an interferometric            
                         binary. B is BD+46@3134.                                                        
             STF2743     AB: H 4  22.                                                            MEv2010 
                         AD: A 71" measure by Guillaume (1931) was incorrectly assigned to AD,   Gui1931 
                         resulting in later measures of that wide pair being similarly labelled          
                         as AD measures. These pairs have now been assigned to STF2743AE. A              
                         "rediscovery" of the 39" AD pair by Fay (2013) was incorrectly given    FyM2013d
                         the designation FYM 99AE. This measure has been merged with AD.                 
20598+3126   GYL  44     B is BD+30@4272.                                                                
20598+1649   STTA213     B is BD+16@4426.                                                                
                         Pair appears in an appendix list, not part of discoverer's regular              
                         numbering sequence.                                                             
20598+1455   BPM2308     [PM2000] 2434777 + [PM2000] 2434672.                                    Gvr2010 
20598-2028   TOK 370     First resolution of the close pair with acceleration. No RV data. This          
                         is an X-ray source.                                                     Tok2013b
20599+4016   COU2431     Aa: First resolution of primary, which was a known SB (period 112d).            
                         Metallicity estimates range from -0.78 to -0.14.                        Hor2012b
             LSC   1     Aa1,2: Docobo et al. (2014) use the spectroscopic elements of Goldberg          
                         et al. (2002 AJ 124, 1132), together with speckle data and Hipparcos            
                         parallax, to derive the remaining orbital elements. The resulting               
                         masses are 1.05 +/- 0.05 and 0.89 +/- 0.05 Msun.                        Doc2014h
                         Aa1,2: SB2, P=112.56d                                                   Tok2014d
             LEP  98     AD: SHY 337. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
             SEI1363     CR: Also known as BUP 221CR or LDS2480.                                         
             NLTT 50309  Combined spectroscopic/astrometric solution, based on high-resolution           
                         echelle spectra plus archival PTI visibility measurements.                      
                         Derived masses 1.1861 +/- 0.0057 and 0.9407 +/- 0.0049 Msun,                    
                         distance 40.571 +/- 0.052 pc.                                           Knc2010 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses 2.18 +/- 0.15, 2.37, and 1.10 Msun, respectively.                Mlk2012 
             HDS2989     Da,Db: Previously known as 20582+4011 HDS2989AB, but found to be the D          
                         component of the CPM pair LEP  98.                                              
                         Da,Db: Rectilinear solution by Hartkopf & Mason (2013).                 Hrt2013b
21000+4004   KUI 103     V1396 Cyg.                                                                      
                         Astrometric orbit by Lippincott (1975), with only the semi-major axis   Lip1975 
                         derived from visual separations. The longitude of periastron has been           
                         reversed to correspond to the visual position angles.                   Lip1975 
                         An observation by Tokovinin (1982) - 1981.370, 48.1 degrees, 0".377 -   Tok1982a
                         was reduced improperly, so has been removed.                            Tok1982b
                         Visual primary is a BY Dra-type variable, and 3.3d SB2 (#1280 in                
                         Batten et al., 1989).                                                   Bte1989 
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         GJ 815. In addition to the component that we resolve with AstraLux,             
                         which was previously known and has been studied over a long timescale           
                         (e.g. Lippincott 1975), the primary component of the resolved pair is   Lip1975 
                         a 3.3 day spectroscopic binary (Pourbaix 2000). Estimated age 30-300            
                         Myr; masses 0.58 +/- 0.05 and 0.26 +/- 0.09 Msun; a ~10.5 au.           Jnn2014 
21001+2555   GRV 401     BC: Also known as GRV 402AB.                                                    
21001+0731   KUI 102     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.08 +/- 0.94, 3.20, and 1.40 Msun, respectively.             Mlk2012 
21003+3543   SEI1361     SEI1362.                                                                        
21004+3426   FAR   1     SKF 321. Primary is DB white dwarf GD 392. Comparison of POSS I and II          
                         plates indicate FAR 1 comprises a common proper motion pair                     
                         (pm 0.17+/-0.01 "/yr at 44+/-5 deg). Spectroscopy and multi-color               
                         photometry indicate companion is a DC white dwarf. Assuming a log g             
                         value for the primary of 8.0, distance is about 57.8 pc, masses ~0.59           
                         and 0.153 Msun, and T_eff 11,625 and 3,509K.                            Far2004 
                         Primary is white dwarf WD 2058+342 = GD 392.                            Far2005b
21005+1920   BU 1497     B is BD+18@4674.                                                                
21006+5432   HJ 1606     Also known as VBS  33.                                                          
             HJ 1605     Original C component of HJ 1605 = HJ 1606A.                                     
                         WDS designation of HJ 1605 changed from 21003+5430,                             
                         HJ 1605AC --> HJ 1605AD, HJ 1605AB --> HJ 1605DE                                
21006+1449   BPM2309     [PM2000] 2437142 + [PM2000] 2437114.                                    Gvr2010 
21007+3353   BUP 222     G211-005. None of the OSO components are common proper motion                   
                         companions, based on comparison with POSS2 red plates. Also, the B              
                         component is not confirmed using their data and images from the                 
                         Digitized Sky Survey.                                                   Oso2004 
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             OSO 138     Further analysis shows that Osorio et al. did not take into account             
                         the very high proper motion of the A component. Their AF pair                   
                         corresponds to Burnham's AB, while their AG pair is the same as Opik's  Bu_1913 
                         AD. (note added 10/2004)                                                Opi1927 
21007+2844   BRT  54     ADS 14537, MLB 486 is the same star.                                            
21008+4635   BU  156     Also known as HDS2994.                                                          
21008+3940   SEI1364     ALI 1152.                                                                       
21009+5929   MLR 241     No significant movement since first resolution.                         Drd2009 
21009+3224   TDT2694     Two possibilities for TDT2694 have been measured. Neither matches the   Cve2019b
                         morphologically matches the discovery measure. The position of their            
                         target (1) matches that of the discovery measure, and the magnitude             
                         agrees with that of Tycho2 for the primary so it is folded. Target (2)          
                         which is folded but "X" coded is off slightly but matches better in             
                         magnitude difference.                                                           
21009+1552   BPM2310     [PM2000] 2437811 + [PM2000] 2437977.                                    Gvr2010 
21011+3315   JNN 288     BC: Originally 21013+3314 JNN 288, but found to be B component of               
                         21011+3315 LDS1049.                                                             
21011-4426   HJ 5238     B is CD-44@14241.                                                               
21012+4609   STT 426     60 Cyg. A is probably a spectroscopic binary, and is the variable               
                         V1931 Cyg.                                                                      
21012-3511   TOK 344     A is astrometric and SB, no SB orbit. Tokovinin & Lepine (2012): B is   Tok2012c
                         white dwarf candidate.                                                  Tok2014d
21013+3554   SEI1368     ALI 210. Ali observation in 1933 indicates a large change. Proper       Ali1955 
                         motion or error in one measure?                                                 
21013+3314   JNN 288     G 187-14. Estimated age 1000-10000 Myr; masses 0.24 +/- 0.08 and 0.18           
                         +/- 0.06 Msun; a ~2.4 au.                                               Jnn2014 
21013-3215   RST5475     gam Mic                                                                         
21014+2043   JNN 289     LHS 3610. Estimated age 1000-10000 Myr; masses 0.25 +/- 0.04 and 0.13           
                         +/- 0.02 Msun; a ~8.9 au.                                               Jnn2014 
21017+1652   BPM2311     AB: [PM2000] 2440174 + [PM2000] 2440516.                                Gvr2010 
             BPM2312     BC: [PM2000] 2440516 + [PM2000] 2440753.                                Gvr2010 
21018-1440   BRT2778     A likely plate flaw.                                                    Grv2021b
21019+2340   COU 128     This object was misidentified as HR 8059 by McAlister & Fekel (1980).   McA1980b
21022+1426   A  1688     Close, rapidly moving binary. Too close at times and quadrant always            
                         uncertain.                                                                      
21022-3128   LDS 731     LDS5916.                                                                        
21022-4300   DUN 236     B is CD-43@14327.                                                               
21022-4300               A is ~1090d spectroscopic binary (G3IV+K0IV), B is a K0III.             Tok2023b
                         SHY 788. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
21023+3931   H 4 113     H IV 113. B is BD+38@4320. Also known as STF2748.                               
             SMY   6     AD: Based on his magnitude estimates, the 1875 Ward measure attributed  Wrd1876 
                         to EH was more likely AD.                                                       
             WRD   4     AG: Ward's 1875 EG measure doesn't correspond to any likely companion,          
                         but given his magnitudes, the measure was probably between A and a              
                         companion now labelled as G. The old EG pair has been removed. The              
                         WRD 4ED should more appropriately have been designated SMY 6ED, but             
                         will not be changed, in order to minimize confusion.                            
21024+3739   STF2747     NLTT 50404/50405                                                        Chm2004 
21024+2748   TOK 345     A is ER Vul, W UMa-type eclipsing, X-ray source, SB2E, P=0.698d. Third          
                         body around ER Vul is suggested from (O-C) period, ~30yr?               Tok2014d
21025+1606   BPM2313     [PM2000] 2442264 + [PM2000] 2442031.                                    Gvr2010 
21028+4551   BU 1138     Called a spectroscopic binary in BSC. This may be due to motion in the          
                         close visual pair.                                                              
                         AB: Additional notes may be found in Muller (1955).                     Mlr1955c
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             KUI 104     CD: C is at 21 02.6 +45 53. CE is optical.                                      
             BU 1138     AB: Rectilinear solution by Friedman et al. (2011).                     USN2011b
                         CE: Rectilinear solution by Friedman et al. (2011).                     USN2011a
21028+3534   SEI1375     Coordinate confusion led to mislabelling of some components. The BTG 6          
                         AD pair was actually BD, the BTG 6 AE pair was actually BC.                     
21029+1708   BPMA250     [PM2000] 2443474 + [PM2000] 2443895.                                    Gvr2010 
21030+1529   BPM2314     [PM2000] 2443644 + [PM2000] 2443653.                                    Gvr2010 
21031+2929   OSO 139     G187-018. AC and AD are not common proper motion pairs, based on                
                         comparison with POSS2 red plates                                        Oso2004 
21031+1434   A  1689     OL 131 is identical                                                     Hei1980a
21031+0132   STF2744     A premature orbit has been computed.                                            
21032+1305   SLE 513     Error in Soulie (1986) measure due to typo in coordinates of primary .  Sle1986a
21032+3645   SEI1380     AB = 21028+3645 HLM  38AB.                                                      
             WAL 134     AC; WDS designation changed from 21028+3645 due to merger of SEI1380            
                         and HLM  38.                                                                    
21032+1305   SLE 513     Large change in separation over 21 years                                Los2005 
21033+1259   HJ  272     Rabe measure: 1913.76, 259.6, 25.92", 9-10 later associated with        Rab1923 
                         21023+3931 H 4 113AC.                                                           
21034+1508   BPM2315     [PM2000] 2444745 + [PM2000] 2444538.                                    Gvr2010 
21035+5925   MLR 243     Algol-type eclipsing binary, P = 9.9634 d.                              Zas2011 
21035+2400   HO  281     A is the irregular variable DY Vul.                                             
21036+5358   ES 2704     B is BD+53@2541.                                                                
21037-0258   J  1717     J  1780.                                                                        
21038-4041   RSS  37     This previously uncataloged double star was a Hipparcos double entry            
                         system. The first measure is determined from the individual positions           
                         listed by Rousseau et al.                                               Rss1996 
21039+4138   STTA214     AB: HJL1104.                                                            HJL1986 
21041+4225   GII  54     SCA 179.                                                                        
21041+0359   TOK 371     First resolution; estimated period 10yr. Pair is on the Keck exoplanet          
                         search program.                                                         Tok2013b
21041+0300   WSI   6     AB: The 1yr SB with large acceleration has been resolved with speckle.          
                         However, we cannot exclude that it is a triple system.                  Tok2012a
                         Horch et al. (2012) confirm that the known double is comprised of at            
                         least one additional star. Object is a known SB, with period 378 days           
                         (Latham et al. 1992). Metal-poor ([Fe/H] = -1.01). The wider AB pair    Lat1992 
                         has an estimated orbital period of 20 years; Jancart et al. (2005)      Jnc2005 
                         confirm the spectroscopic period with their astrometric orbit of the            
                         inner pair.                                                             Hor2012b
             DSG   6     Aa,Ab: For the Horch et al. (2015) combined solution, spectroscopic             
                         elements are fixed to those of Latham et al. (1992). Assigned spectral  Lat1992 
                         types for Aa, Ab, and B are F9V, G9V, and K0V; derived masses for Aa            
                         and Ab are 1.12 and 0.82 Msun.                                          Hor2015 
21041-0549   MCA  66     Aa,Ab: 12 Aqr.                                                                  
                         A measure on 1980.7257 was incorrectly attributed to HR 8059 by                 
                         McAlister et al. (1983); it actually belongs to ADS 13944.              McA1983 
21042+3542   SEI1387     ALI 213.                                                                        
21042+1558   BPM2316     [PM2000] 2446963 + [PM2000] 2446899.                                    Gvr2010 
21044+4646   DAL  49     Pair mistakenly observed by Daley (2002) for 21046+4627 BRT1140.        Dal2002b
21044+1625   BPM2317     [PM2000] 2447442 + [PM2000] 2447410.                                    Gvr2010 
21044-1951   FIN 328     eta Cap = 22 Cap.                                                               
                         Spectral types and masses of components assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
                         Ruymaekers & Nys (1955) noted discrepancies in the orbit of Zulevic     Ruy1995 
                         (1993), so calculated orbital elements from the Thiele-Innes elements   Zul1993b
                         originally given.                                                               
                         This system has a Delta m of about 1.7 +/- 0.7 magnitudes, as                   
                         determined from lunar occultation measures (Evans & Edwards 1983).      Evn1983a
                         Masses and bolometric magnitudes are derived for the two components             
                         of this system, based on assumed spectral types and available                   
                         parallaxes.                                                             Msn1999a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.91 +/- 1.61, 3.24, and 3.25 Msun, respectively.             Mlk2012 
                         Docobo & Andrade (2013) derive a dynamical parallax of 19.49 +/- 0.29           
                         mas and component masses 2.03 +/- 0.12 and 1.21 +/- 0.07 Msun (for              
                         spectral type A5V) or 20.46 +/- 0.32 mas, 1.75 +/- 0.11 and 1.05 +/-            
                         0.06 Msun (for A3IV). See paper for extensive notes on this system.     Doc2013d
21045+2350   POU5130     Aka POU5124.                                                                    
21045+0746   BU  269     H 1  62.                                                                MEv2010 
                         BU 835. H I 62 probably same star with an error of 10@ in declination.          
21045-4615   TOK  35     Period of visual pair ~85,000y.                                         Tok2006 
                         A is SB2, P=19.698d                                                     Tok2014d
21046+3345   CXT   1     ROE  53 or J 3123.                                                              
21046+1400   BPM2318     [PM2000] 2447922 + [PM2000] 2448172.                                    Gvr2010 
21046+0530   BUP 223     3 Equ.                                                                          
21047+1152   MLR 541     Also known as HEI 405.                                                          
21047+0332   SE    3     Aa,Ab: This is called AD in the Greenwich Observations. The measures    L__1895a
                         are probably of BC.                                                             
21048+3545   SEI1392     J 1153.                                                                         
21048+3531   S   773     B is BD+34@4265.                                                                
21048+1506   BPM2319     [PM2000] 2448398 + [PM2000] 2448470.                                    Gvr2010 
21049+1549   BPM2320     [PM2000] 2448685 + [PM2000] 2448769.                                    Gvr2010 
21050+1243   STF2750     A,BC: HJL 290.                                                          HJL1986 
21053+0704   ENG  80     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
21054+1139   BPM2321     [PM2000] 2449963 + [PM2000] 2449716.                                    Gvr2010 
21054+0557   BUP 224     4 Equ.                                                                          
                         Rectilinear solution by Hurowitz et al. (2014).                         USN2014b
21056+1443   TDT2738     CD: Originally 21056+1442 TDT2738, but primary found to be C component          
                         of 21056+1443 HEI  78AC.                                                        
21056+1133   BPM2323     [PM2000] 2450497 + [PM2000] 2450364.                                    Gvr2010 
21056+1113   BPM2322     [PM2000] 2450385 + [PM2000] 2450183.                                    Gvr2010 
21058+1432   LDS1050     AC: NLTT 50497/50489                                                    Chm2004 
21059+0803   OSO 140     G025-017. Not a common proper motion pair, based on color               Oso2004 
21060+1443   BPM2324     [PM2000] 2451551 + [PM2000] 2451691.                                    Gvr2010 
21061+0217   RST5476     BAL 1578.                                                                       
                         Algol-type eclipsing binary, period 0.59338 d.                          Zas2019 
21063+1824   BPM2326     [PM2000] 2452405 + [PM2000] 2452242.                                    Gvr2010 
21063+1233   BPM2325     [PM2000] 2452281 + [PM2000] 2452299.                                    Gvr2010 
21064-4123   SEE 437     eta Mic.                                                                        
21064+1336   SLE 523     Soulie (1986) measure in error, apparently due to typo in coordinates           
                         of secondary.                                                           Sle1986a
21065+2655   COU 527     There is another pair in the field: 1905.93, 285.6@, 79.24".                    
21066+4739   ES   32     63 Cyg.                                                                         
21066+3623   SEI1405     ALI 214.                                                                        
21067+3715   SEI1406     J 1079.                                                                         
21069+3845   STF2758     61 Cyg. According to R.G. Aitken, this was discovered in 1753 by        A__1935f
                         Bradley. Premature orbits have been computed for AB. This is an         Bdy1832A
                         example of a binary known by its common parallax and proper motion              
                         rather than the orbital motion, which has completed approximately               
                         one-sixth of an orbit in the past 200 years. The extremely large                
                         proper motion of this pair has led to some confusion in identification          
                         of others stars measured relative to the primary. Precise epoch-2000            
                         coordinates and UCAC2 catalog cross-identifications are listed below:           
                             A = UCAC2 50084730 = 2106539+384457  pm = +5328 +3258                       
                             B = UCAC2 50084732 = 2106552+384431  pm = +5267 +3143                       
                             C = UCAC2 45407969 = 2106142+383502       +007+006                          
                             D = UCAC2 45407870 = 2105597+384133       +002-006                          
                             E = UCAC2 45408060 = 2106306+384532       +012-007                          
                             F = UCAC2 45408067 = 2106322+384246       +019-002                          
                             G = UCAC2 45408111 = 2106413+384325       +000-002                          
                             H = UCAC2 45408157 = 2106502+384551       -004-006                          
                         The Aa pair was renamed AF. The G and H components were both initially          
                         believed to be the C component. B is BD+38@4344.                                
                         AB: Statistically the same parallax within the errors would indicate            
                         the components are physical.                                                    
                         AB: H 4  18.                                                            MEv2010 
                         An estimated mass has been used by Josties (1981) to compute the        Jti1981 
                         otherwise nearly indeterminate orbit; thus the orbit should not be              
                         used to compute the mass. The RV difference from which the ascending            
                         node is inferred is quite small. Various small variations, formerly             
                         suspected in the period range of about 5-10 years, are absent in the            
                         strong photographic coverage of the last decades.                               
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Resulting component masses are 0.74 +/- 0.13 and 0.46 +/- 0.07 Msun.    PkO2006b
                         HIP 104214. See Allen et al. (2000) for information on metallicity,     AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         CHARA Array Limb-darkened diameter of A,B:                              CIA2008e
                         1.775 +/- 0.013, 1.581 +/- 0.022 mas.                                           
                         R =  0.665 +/- 0.005, 0.595 +/- 0.008 \rsun,                                    
                         L =  0.153 +/- 0.010, 0.085 +/- 0.007 \lsun,                                    
                         Teff = 4400 +/- 100, 4040 +/- 80 K.                                             
                         AB: NLTT 50559/50560                                                    Chm2004 
                         BC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         Inclination of orbit flipped by 180 deg in accordance with available    Pko2017b
                         data by cataloger.                                                              
                         Analysis of long term photometric variability of both components        PkO2018a
                         reliable photometric variability with periods of about 15 years and             
                         variation of 0.05(0.02) magnitudes for both components as well as a             
                         9 year variation for B.                                                         
                         Total system mass is 1.132 +/0 0.032 /msun.                             Izm2024 
             HZE   4     Heinze et al. (2010) determine that the J, K, and L components are all          
                         background objects.                                                     Hze2010 
             STF2758     AC, AE, AF, AG, AH: Rectilinear solutions by Mason & Hartkopf (2016).   Msn2016a
             SMR   1     AI: Rectilinear solution by Mason & Hartkopf (2016).                    Msn2016a
             SMR  40     AO, AP: Rectilinear solutions by Mason & Hartkopf (2016).               Msn2016a
             STF2758     BC: Rectilinear solution by Mason & Hartkopf (2016).                    Msn2016a
             FYM 106     BN: Rectilinear solution by Mason & Hartkopf (2016).                    Msn2016a
21070+1500   BPM2327     [PM2000] 2454037 + [PM2000] 2453969.                                    Gvr2010 
21071+1558   BPM2328     [PM2000] 2454427 + [PM2000] 2454414.                                    Gvr2010 
21071+1042   J  2576     Not found by Heintz at IDS position.                                    Hei1990b
21071-2500   SEE 439     24 Cap.                                                                         
21072+3657   SEI1407     ALI 438.                                                                        
21072-1355   BU  157     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
21073-0021   BAL 930     J 3209.                                                                         
21073-5702   HDS3009     This is the C component of 21078-5702.                                  Dam2015b
21074-0814   BU  368     Baize (1985) value of omega corrected from 12.0 to 192.0 degrees by     Baz1985b
                         Ruymaekers & Nys (1985).                                                Ruy1995 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.23 +/- 1.27, 3.31, and 2.24 Msun, respectively.  Mlk2012 
21075+3831   SEI1408     ALI 961.                                                                        
21075-3842   WG  266     CPD-39@8869.                                                                    
21076+1442   BPM2329     [PM2000] 2455520 + [PM2000] 2455335.                                    Gvr2010 
21078+3834   BRT2233     ALI 962.                                                                        
21078+3421   FYM 125     The JK pair was initially listed incorrectly as a new JN pair.          FyM2014b
21078+1345   BPM2330     [PM2000] 2456137 + [PM2000] 2455874.                                    Gvr2010 
21078-5702   HJ 5243     B is CPD-57@9794.                                                               
                         The C component is 21073-5702HDS3009.                                   Dam2015b
21079+3324   TRN  31     The image rotator was in an unknown state, so two possible theta                
                         values are listed for the 2001.7367 observation - one for zenith up             
                         and one for north up. However, the 2MASS measure effectively rules              
                         out one option.                                                         Trn2008 
             HD 201345   Aslanov et al. (1984 SvAL 10, 278) discuss the radial velocities and            
                         the possibility of a low-mass companion.                                Msn1998a
21079+1229   BPM2331     [PM2000] 2456493 + [PM2000] 2456492.                                    Gvr2010 
21080-0104   J  1402     BAL 618.                                                                        
21082+3628   SEI1410     Primary is V2483 Cyg, eclipsing binary of Beta Lyr -type, period                
                         112.4 d.                                                                Zas2012 
21083+2437   SLE 531     Ten arcminute error in declination of primary.                          Sle1986a
21083+3816   SEI1411     ALI 679.                                                                        
21083+1757   BPM2332     [PM2000] 2457297 + [PM2000] 2457104.                                    Gvr2010 
21085+3614   SEI1412     ALI 216.                                                                        
21086+3012   STF2762     A is probably an Alpha CVn-type variable, V389 Cyg. There also may be           
                         a long-period spectroscopic binary in the system.                               
                         AB: H 2  97.                                                            MEv2010 
21086-2112   HJ 3009     chi Cap = 25 Cap                                                                
                         HJ 1617.                                                                        
             VIG  20     The E and F components appear to be co-moving with the primary; the             
                         masses of E and F are estimated at 0.09-0.13 and 0.09-0.14 Msun,                
                         respectively. Optical/physical nature of the G component is undefined.  Vig2012 
21087+7342   OSO 141     G261-038 . Not a common proper motion pair, based on comparison with            
                         POSS2 red plates.                                                       Oso2004 
21087+1145   BPM2333     [PM2000] 2458372 + [PM2000] 2458147.                                    Gvr2010 
21088+1113   BPM2334     [PM2000] 2458615 + [PM2000] 2458474.                                    Gvr2010 
21089+2417   OSO 142     G187-024. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates.                                                  Oso2004 
21090+0410   HJ 5515     Nothing in the vicinity matches Herschel's theta value. However, if             
                         either he meant the separation was 15" or his theta has a 90deg error,          
                         this pair appears to be the most likely match.                                  
21091+3844   S   779     B is BD+38@4363.                                                                
21092-0814   JNN 128     The binary 2MASS J21091375-0814041 is as of yet uncomfirmed with                
                         regards to common proper motion, but the components have similar                
                         colors and brightnesses, and a relatively small separation of ~0.97"            
                         hence the pair is probably physically bound, and counts as such in the          
                         statistical analysis.                                                   Jnn2012 
21094-7310   I   379     Measures uncertain, too close. Duplicity doubtful. Needs speckle.               
                         Hipparcos stochastic double solution.                                           
                         AB: Additional notes may be found in Finsen (1951).                     Fin1951a
                         AB: A is SB and astrometric binary, P=6.65y (Goldin & Makarov 2006).    Gln2006 
                         Resolved at 0.14".                                                      Tok2014d
21096-1622   HJ 1612     J 1783.                                                                         
21097+1434   OL  132     Scardia et al. (2013) note that the ID is uncertain for their 2011              
                         measure.                                                                Sca2013c
21098+4001   GRV 429     AC: Also known as GRV 430AB.                                                    
21098+2915   DU    3     Aka WFC 234. DM number incorrectly listed as BD+28 4015 in BDS.                 
21098-1834   HJ 3010     B is BD-19@6033.                                                                
21098-5155   RST1084     CD-52@9770.                                                                     
21099+1648   BPM2335     [PM2000] 2461379 + [PM2000] 2461405.                                    Gvr2010 
21101+1311   BPM2336     [PM2000] 2461843 + [PM2000] 2461635.                                    Gvr2010 
21101-4851   HJ 5247     B is CD-49@13357.                                                               
21102+2045   RAO  25     Pair has a variable RV (Nordstrom et al. 2004), so the 3".3 companion   Nrd2004 
                         B discovered by Robo-AO makes it a triple system (estimated period of           
                         AB is 2000 yr, too long to cause the RV variation). We found the B              
                         component to be on the [Fe/H] = -0.5 isochrone, in agreement with               
                         [Fe/H] = -0.54 measured for A (Reddy et al. 2003 MNRAS 340, 304).       Rbr2015d
21103+1008   KNT   5     A: gam Equ = 5 Equ. A is an Alpha CVn-type variable. There apparently           
                         is a long-period spectroscopic binary present.                                  
             BU   71     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
21103-0016   LDS4866     NLTT 50691/50692                                                        Chm2004 
21104-0042   BAL 620     J 2338.                                                                         
21105+4742   BU  159     AE: Leavenworth refers to a 14th magnitude star in 337.0".              Lv_1930 
                         Kuiper's 1934 measure was initially added incorrectly as an additional  Kui1961b
                         component, designated KUI 105AF, although he identified his measure             
                         with the Leavenworth pair.                                                      
21105+2227   STF2769     B is BD+21@4485.                                                                
                         One component is a spectroscopic binary.                                        
             SHY 793     BC: HIP 104536 + HIP 102981.                                                    
             STF2769     H N   8.                                                                MEv2010 
21106+3737   HU 1310     Pair certainly identical to ADS 14717 = ES 253, but measures are                
                         discordant (Espin's rho in 1905.75 and his theta in 1923.75). One star          
                         may be variable.                                                        Baz1948d
21106+1307   BPM2338     [PM2000] 2463302 + [PM2000] 2463345.                                    Gvr2010 
21106+1126   BPM2337     [PM2000] 2463104 + [PM2000] 2463308.                                    Gvr2010 
21109+4658   GIC 166     AB: G212-026/G212-027.                                                          
                         NLTT 50746/50747                                                        Chm2004 
21109+4658   JNN 290     BC and BD: G 212-27. Both of the point sources in the AstraLux field            
                         of view are consistent with static background objects that do not               
                         share a common proper motion with the primary star, hence they are              
                         contaminants rather than physical companions. Their colors (dz' = 4.0           
                         +/- 0.3 mag and di' = 3.3 +/- 0.5 mag for the closer point source and           
                         dz' = 4.8 +/- 0.3 mag and di' = 4.3 +/- 0.1 mag for the farther one)            
                         verify this conclusion.                                                 Jnn2014 
21109+2925   BAG  29     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.26 +/- 0.32, 1.20, and 0.47 Msun, respectively.             Mlk2012 
21110+2642   BRT3364     Originally published as BRT 221.                                        Brt1928 
21110+1113   BPM2339     [PM2000] 2464166 + [PM2000] 2464300.                                    Gvr2010 
21110+0933   STF2765     AB: H 1  63.                                                            MEv2010 
21111+3618   HO  283     Aa,Ab: The primary was suspected to be a close pair by Hough in 1884,   Ho_1890 
                         but it it was not confirmed later by Hough, Burnham, or                 Bu_1906 
                         Worley.                                                                 Wor1967a
21112+3855   ES 1991     Not found by Heintz at IDS position.                                    Hei1987a
21112+3332   VKI  48     Ross 825.                                                                       
21112-0100   LDS4867     NLTT 50718/50720                                                        Chm2004 
21114+7140   OSO 143     G262-035. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
21114-5220   HU 1626     Primary is eclipsing binary BR Ind (period 0.89277 day).                Zas2010 
                         Light curve and radial velocity combined solution determined.           Zas2017 
21115+3033   ALD   5     J  3224.                                                                        
                         Olivier's angle of 1915, given in ADS, is 90deg too small.              B__1962d
21115-1132   VOU  30     RST 4076.                                                                       
21117+3818   SMA 136     ALI 683. BRT 2234.                                                              
21117+3621   TOB 213     BC: Originally 21117+3619 TOB 213, but secondary was found to be same           
                         as that of 21117+3621 SEI1439. Systems merged, with quadrant flipped            
                         for TOB pair.                                                                   
21117+1821   LDS1051     LDS5246.                                                                        
                         NLTT 50751/50759                                                        Chm2004 
21117+1350   BPM2340     [PM2000] 2465837 + [PM2000] 2466174.                                    Gvr2010 
21118+5959   MCA  67     Aa,Ab: 1983.4341, 1983.7100, 1984.7118:  These three autocorrelograms           
                         were remeasured; the new results are listed.                            McA1987b
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 02.07 +/- 52.22, 27.33, 25.11 Msun, respectively.  Mlk2012 
21120+2410   STT 430     HIP 104660. See Allen et al. (2000) for information on metallicity,     AlC2000 
                         age, galactic orbital parameters, etc.                                          
21121+4543   ES 9005     Previously known as BU  160. Espin refers to it as a faint              Es_1914 
                         star following BU 160.                                                          
21121+1607   BPM2341     [PM2000] 2466649 + [PM2000] 2466492.                                    Gvr2010 
21122+5854   ARG 107     B is BD+58@2236.                                                                
21122+3828   SMA 137     ALI 964.                                                                        
21123+1105   BPMA251     [PM2000] 2467284 + [PM2000] 2466736.                                    Gvr2010 
21123-0142   BAL 263     LYS  37AB. Designation match was originally missed because BAL 264              
                         measure was incorrectly attributed to BAL 263.                                  
21124+1432   HJ 1619     HJ 1620.                                                                        
21124-1500   H 1  47     H I 47.                                                                         
                         Hopmann orbit rejected from Fourth Orbit Catalog ("P over 4000 years")  Wor1983 
                         Apparent typographical error in Hopmann value for semi-major axis       Hop1974 
                         (5".909); value of 15".909 appears better. Still unable to match his            
                         orbit with data, however, despite various quadrant flips of angles,             
                         et cetera. A least-squares fit for remaining elements using data                
                         available to Hopmann and fixing P, T, and e at his published values             
                         yields a = 10".03, i = 101.0, Omega = 312.0, and omega = 343.4                  
                         This is much better fit by linear solution. Orbit still in 6th Catalog,         
                         but default solution now linear and orbit is rejected. Proper motion            
                         of A and B very different.                                                      
21125+1727   BPMA252     [PM2000] 2467718 + [PM2000] 2467798.                                    Gvr2010 
21126+1706   BPM2342     [PM2000] 2467848 + [PM2000] 2467725.                                    Gvr2010 
21127+3807   GUR  12     Incorrectly identified as ES 257 by Guerrero et al.(2014)               Gur2014 
21127-0045   J  1403     BAL 622. RST 5159.                                                              
21128+3907   SEI1447     ALI 965.                                                                        
21128+3014   BAS   7     Aa,Ab: This is likely the 17.8-yr spectroscopic binary of Griffin &             
                         & Keenan                                                                Grf1992b
21129+3014   BUP 227     zet Cyg = 64 Cyg. A is a spectroscopic binary. The Bright Star                  
                         Catalogue lists the spectral type as G8III-IIIaBa0.6.                           
                         Mk III Limb-darkened diameter  2.821 +/- 0.028 mas.                     MkT2003 
21131+1028   BU 1501     J 177.                                                                          
21133+4655   A   884     Rectilinear solution by Rica & Zirm (2012).                             FMR2012i
21134+2813   BRT3365     Originally published as BRT 223.                                        Brt1928 
21135+1559   HU  767     1979.7700: This measure is an average of a power spectrum and an                
                         autocorrelogram measure, listed separately by McAlister & Hendry.       McA1982d
                         1980.7257  This measure was incorrectly attributed to ADS 13944 by              
                         McAlister et al. (1983).                                                McA1983 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.96 +/- 0.66, 3.40, and 1.82 Msun, respectively.             Mlk2012 
21135+0713   BU  270     Star C (mag. about 12, 32") may be physical. Star D (BD+06 4777, 3')            
                         probably is not physical.                                                       
21135-0905   BRT 515     J  3348.                                                                J__1962a
21136+1315   BPM2343     AB: [PM2000] 2470222 + [PM2000] 2470354.                                Gvr2010 
             BPM2344     BC: [PM2000] 2470354 + [PM2000] 2470555.                                Gvr2010 
21137+6424   H 1  48     H I 48.                                                                 Mlr1950b
                         Only elements P and T have been amended by Starikova (1977) from the    Sta1977a
                         orbit of Baize (1950).                                                  Baz1950b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.85 +/- 0.55, 2.04, and 2.52 Msun, respectively.             Mlk2012 
21137+3602   SEI1455     J 1329.                                                                         
21137+2510   POU5273     Many published measures, previously assigned to POU5269, are            Dam2016d
                         re-assigned here with a quad flip.                                              
21137+1115   BPM2345     [PM2000] 2470413 + [PM2000] 2470438.                                    Gvr2010 
21139+1140   BPM2346     [PM2000] 2471075 + [PM2000] 2471020.                                    Gvr2010 
21140+6606   MLB 221     Also known as WFC 236.                                                          
21140+3755   SEI1457     ALI 685. SMA.                                                                   
21140+1305   BPM2347     [PM2000] 2471285 + [PM2000] 2471380.                                    Gvr2010 
21140+1219   BPM2348     [PM2000] 2471301 + [PM2000] 2471385.                                    Gvr2010 
21141+1741   BPM2349     [PM2000] 2471552 + [PM2000] 2471686.                                    Gvr2010 
21141-5428   LDS 735     TSN  38.                                                                        
21142+1135   BPM2350     [PM2000] 2471654 + [PM2000] 2471705.                                    Gvr2010 
21143+3418   STTA216     B is BD+33@4205.                                                                
                         Pair appears in an appendix list, not part of the discoverer's regular          
                         numbering sequence.                                                             
21143+3332   ES 2316     A 1998.8 measure by Lampens et al. (2007) was erroneously attributed    Lmp2007 
                         to this pair and has been withdrawn by the author.                              
21143+1145   BPM2351     [PM2000] 2471993 + [PM2000] 2471708.                                    Gvr2010 
21143-3835   HJ 5253     AC: The C component was found to have a spectroscopic companion with a  Tok2020h
                         period of 11d. The close AB pair, estimated period 1.3k yr, may be              
                         responsible for proper motion differences, and this may be a physical           
                         quadruple.                                                                      
21144+3803   SEI1461     ALI 686. SMA.                                                                   
21145+1000   STT 535     del Equ = 7 Equ.                                                                
                         Spectral types and masses of components assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
                         This is an example of a system whose earlier long period, low-                  
                         eccentricity orbit has been supplanted by a high-eccentricity orbit             
                         of half P due to correct quadrant determination.                                
                         The motion causes double spectral lines over part of the orbit, but             
                         the components are indistinguishable in the spectrum as well as                 
                         visually. The RV curve gives the elements T, e, and the longitude of            
                         periastron somewhat in variance with those of the visual orbit; cf.             
                         Dworetsky et al. (1971).                                                Dwo1971 
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         Arenou (2000) gives combined solution of astrometric orbits and DSBs.   Are2000 
                         Paper includes masses and distances.                                            
                         Muterspaugh et al. (2008) combine PHASES astrometry with speckle and    Mut2008 
                         radial velocity data to derive an orbit for this nearby pair. The               
                         derived parallax is 54.41 +/- 0.14 mas (distance 18.379 +/- 0.048 pc).          
                         Masses of A and B components are nearly identical, at 1.192 +/- 0.012           
                         and 1.187 +/- 0.012 Msun.                                                       
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.43 +/- 0.34, 2.45, and 2.33 Msun, respectively.  Mlk2012 
             STF2777     AB,C: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB,C: H 4  37.                                                          MEv2010 
21146-2849   LDS4872     NLTT 50827/50824                                                        Chm2004 
21146-4337   CPO 621     A likely plate flaw.                                                    Grv2021b
21147-0050   A   883     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 21.20 +/- 18.02, 6.44, 2.19 Msun, respectively.    Mlk2012 
             STF2775     AB,C: Star C (mag. 10.52, 21") is probably physical.                            
                         Egbert observed a wide new pair (1879.656, 59.9deg, 99".40, mags 9.0    Egb1879 
                         and 9.5), but listed only a coarse epoch-1880 RA and no other                   
                         identifier other than his initials. Since his RA matched that of                
                         STF2775, the pair was catalogued as STF2775PQ. There appears to be              
                         nothing in the field of STF2775 which matches this pair, however, so            
                         it has been removed from the WDS.                                               
21148+3803   AGC  13     tau Cyg = 65 Cyg.A is a Delta Scuti-type variable.                              
                         Spectral types and masses of components assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
                         Identification of the ascending node is probable although small                 
                         variations of non-orbital origin superimpose on the RV. A is a Delta            
                         Scuti-type variable. A faint star listed as component F is physical;            
                         linear formula given by Heintz.                                                 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         NPOI Limb-darkened diameter    2.169 +/- 0.028 mas,                             
                         R =    4.70 (+/- 0.07   )  \rsun,  Teff = 4771 +/-  31 K,                       
                         L =   10.3 +/-   0.2 \lsun.                                             NOI2023 
                         AC and AB,D: Optical pair, based on study of relative motion of the             
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB: The Soderhjelm (1999) orbit predicts a separation of 0.734", but    Sod1999 
                         the magnitude difference (published value 2.7mag) may have been too             
                         great.                                                                  Hrt2009 
                         Calculated mass sum is 2.63 +/- 0.12 Msun. There is some indication of          
                         a substellar companion orbiting one of the two stars, but this is               
                         uncertain. This solution uses only a single Keplerian model.            Mut2010b
                         AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
21148-1713   RST3279     Position angles discordant, no doubt due to the large magnitude                 
                         difference and closeness of the pair.                                           
21148-2555   HJ 3014     Spectrum: A3/5mA5-F3/5.                                                         
21149+3037   BRT 287     Also known as J  3225.                                                          
21150+1750   BPM2352     [PM2000] 2473568 + [PM2000] 2473840.                                    Gvr2010 
21150-2047   HD 202206   GC 29701. Combined solution, based on reduction of Hipparcos                    
                         intermediate astrometric data together with spectroscopic elements              
                         from the Geneva Extrasolar Planet Search Programs home page.            HaI2001 
                         No comoving objects found within separation/magnitude range listed.             
                         However, Chauvin et al. (2006) note finding at least one faint                  
                         background object.                                                      Cvn2006 
                         HD 202206 is a nearly face-on binary orbitted by a brown dwarf.                 
                         Benedict & Harrison (2017) determine astrometric solutions for AB and           
                         AB,c based on HST Fine Guidance Sensor astrometry and published radial          
                         velocities. The resulting period ratio (P_c/P_B = 4.92 +/- 0.01)                
                         supports past assertions that the system architecture requires a 5:1            
                         mean motion resonance. They derive a parallax 21.96 +/- 0.12mas and             
                         masses 0.089 +0.007/-0.006 Msun for B and 17.9 +2.9/-1.8 Mjup for c.    AST2017 
21154-1021   STF2776     B is BD-10@5631.                                                                
                         BC: H 1  46.                                                            MEv2010 
21156+7836   STF2796     B is BD+77@812.                                                                 
                         H 4 103.                                                                MEv2010 
21157+3235   HJ 1628     GYL  50. Goyal identified his pair as BD+31@4102, but his epoch-1900    Gyl1966 
                         coordinates precess to the location of BD+32@4102. No 16" pair is               
                         found in the vicinity of BD+31@4102, and AC2000 notes no "plate flaws"  WFC1998 
                         mistaken for stars on the Potsdam plates used to generate Goyal's               
                         measure. His value of theta may be reconciled with the position angle           
                         of HJ 1628 by assuming he swapped the dx and dy measures between the            
                         two Potsdam coordinates.                                                        
21158+1745   LDS1052     This star possibly has a wide companion at about 9" as noted in e.g.            
                         the WDS catalog. It is however single in the separation range covered           
                         by the AstraLux data.                                                   Jnn2012 
21158+0515   WRH  35     alp Equ = 8 Equ = Kitalpha                                                      
                         A measure on 1980.4853 was incorrectly attributed to HR 8131 in                 
                         McAlister et al. (1983); it actually belongs to ADS 14893.              McA1983 
                         The equinox-1900 coordinates of this star are incorrectly given as              
                         21158+0430 in the first speckle catalogue.                              McA1984b
                         P = 98.800 d, adopted from Rosvick & Scarfe (1991); T = 2447592.1 for   Scf1991b
                         combined spectroscopic/astrometric orbit by Armstrong et al. (1992).    MkT1992b
                         Quoted errors in T and omega are +3.6/-10.1d and +14/-37deg,                    
                         respectively. Errors to Mark III astrometry are given as "error                 
                         ellipses" ; these values are tabulated below, together with filters             
                         used.  Columns include date (BY), major and minor axes of the ellipse           
                         (mas), ellipse orientation (deg), filter effective wavelength (nm):             
                              1989.4493     1.94     0.081     90.9     800,550,450                      
                              1989.4628     0.45     0.049    104.5     800,550,450                      
                              1989.4712     1.23     0.095     90.8     800,550,450                      
                              1989.4766     3.19     0.16      94.7     800,550,450                      
                              1989.5177     3.84     0.57      80.6     800,550,450                      
                              1989.5313     3.69     2.24     114.8     800,550,450                      
                              1989.6021     2.51     0.48     106.5     800,550,450                      
                              1989.6050     1.39     0.36      88.9     800,550,450                      
                              1989.6159     0.99     0.18      88.6     800,550                          
                              1989.6349     0.45     0.22      78.1     800,550                          
                              1989.6430     1.13     0.22     108.2     800,550,450                      
                              1989.6540     2.86     0.10      99.4     800,550                          
                              1989.7060     2.06     0.24      85.5     800,550,450                      
                              1989.7854     4.10     1.65      74.4     800,550,450                      
                              1989.7934     3.04     0.63      75.4     800,550,450                      
                              1989.7961     1.39     0.38      77.9     800,550,450                      
                              1989.8373     0.94     0.091     69.9     800,550                          
                              1989.8482     0.73     0.085     76.1     800,550,450                      
                              1990.4840     1.35     0.22     103.7     800,550,500                      
                              1990.4896     4.72     0.74      93.2     800,550,500                      
                              1990.5743     0.15     0.042     86.4     800,550,500                      
                              1990.5770     0.33     0.080     88.8     800,550,500                      
                              1990.5824     0.26     0.059     94.9     800,550,500                      
                              1990.6536     0.19     0.041     82.4     800,550,500                      
                              1990.6616     0.41     0.079     86.3     800,550,500                      
                              1990.6644     0.29     0.054     85.8     800,550,500                      
                              1990.6698     0.20     0.050     96.2     800,550,500                      
                              1990.6727     0.66     0.086     81.4     800,550,500                      
                              1990.7054     0.34     0.081     81.4     800,550,500                      
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.68 +/- 0.20, 5.08, and 3.52 Msun, respectively.             Mlk2012 
                         Mass = 2.20   +/- 0.16  , 1.883   +/- 0.083   \msun for A and B.        HJL2020 
                         orbital parallax = 18.11  +/- 0.24  mas.                                        
21158-5316   FIN 329     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 05.99 +/- 37.68, 3.70, and 1.88 Msun, respectively.           Mlk2012 
                         Docobo & Andrade (2013) derive a dynamical parallax of 8.36 +/- 0.17            
                         mas and component masses 2.32 +/- 0.18 and 2.09 +/- 0.16 Msun (for              
                         spectral type A2.5V) or 8.74 +/- 0.17 mas, 2.04 +/- 0.15 and 1.82 +/-           
                         0.14 Msun (for A6IV). See paper for extensive notes on this system.     Doc2013d
21159+2858   HDS3025     A is also a 52d spectroscopic binary.                                   Tok2019b
21160+1639   BPM2353     [PM2000] 2475843 + [PM2000] 2475787.                                    Gvr2010 
21161+2951   LDS1053     NLTT 50902/50901                                                        Chm2004 
                         Luyten measure flipped around the E/W line: pa 282 -> 258.              Luy1969 
21162+1629   BPM2354     [PM2000] 2476243 + [PM2000] 2476288.                                    Gvr2010 
21163+4414   HIP 105017  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Griffin (2000).                                                         Grf2000b
21163-0913   D    24     IW Aqr = 14 Aqr                                                                 
21165+3959   SEI1484     J 1152.                                                                         
21165-3431   BRT1818     A likely plate flaw.                                                    Grv2021b
21167-0739   STF2781     H I 90, BDS 10874 probably same star.                                           
                         H 1  90.                                                                MEv2010 
21169+3001   MLB 538     MLB 716 may be same star.                                               Hei1978b
21170+4020   SEI1487     V2486 Cyg, Algol-type eclipsing binary, P = 1.27268 d.                  Zas2011 
21171+4001   A  1441     AB: Rectilinear solution by Rica & Zirm (2012).                         FMR2012i
21172-0414   BU  161     B is BD-04@5403.                                                                
21173+5837   BU 1140     A is a spectroscopic triple system, with a period of 5.4d, which may            
                         constitute an eclipsing system, and a long period of 225d.                      
21174+2053   KUI 106     G 145-31. Estimated age 1000-10000 Myr; masses 0.21 +/- 0.08 and 0.15           
                         +/- 0.05 Msun; a ~93.9 au.                                              Jnn2014 
21175+7658   LDS1948     HJL 291.                                                                HJL1986 
21175+1221   HJ  279     C is probably BD+11@4531.                                                       
21176+2556   SLE 380     Soulie (1985) measure in error, apparently due to typo in right                 
                         ascension of secondary.                                                 Sle1985 
21176+2841   MLB 489     BRT 55 is identical                                                     Hei1983a
21176+1711   BPM2356     [PM2000] 2479523 + [PM2000] 2479772.                                    Gvr2010 
21176+1614   BPM2355     [PM2000] 2479500 + [PM2000] 2479720.                                    Gvr2010 
21177+2449   POU5319     AC appears to be the same pair as POU5320, with a quadrant flip.                
21179+3454   STT 433     AB: ups Cyg = 66 Cyg. Burnham refers to a star twice the distance of C  Bu_1906 
                         in 60@. A Variable?                                                             
                         BC: Hipparcos acceleration double solution.                                     
21180-2203   RSS 558     CD-22@15309                                                                     
21181-2931   LDS 738     A is PMS star and X-ray source.                                         Tok2014d
21182+3035   HO  154     Includes V2150 Cyg, a W UMa type eclipsing binary, P = 0.59186d.        Zas2012 
21182+1807   BPMA253     [PM2000] 2480776 + [PM2000] 2480163.                                    Gvr2010 
21183+4244   HJ 1634     B is BD+42@4052.                                                                
                         STF2782.                                                                        
21184+3943   SEI1497     ALI 1156.                                                                       
21184+3749   SEI1495     ALI 687. SMA.                                                                   
21185+4357   TRN  32     68 Cyg = V1809 Cyg.                                                             
                         Reports of small radial velocity variability (Alduseva et al. 1982              
                         SvAL 8, 386; Hanni & Pelt 1988 Tartu Astrof. Obs. Teated 89, 200;               
                         Zeinalov et al. 1987 SvAL 13, 90; Musaev & Snezhko 1988 SvAL 14, 68)            
                         probably reflect the presence of line profile variations (Fullerton     Ful1990 
                         1990).                                                                  Msn1998a
21185+1541   BPMA254     [PM2000] 2481450 + [PM2000] 2481288.                                    Gvr2010 
21185+0236   OSO 144     G093-001. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
21186+6235   BU 1502     alp Cep = 5 Cep = Alderamin. Variable?                                          
                         NPOI Limb-darkened diameter    1.677 +/- 0.007 mas,                             
                         R =    2.71 (+/- 0.01   )  \rsun,  Teff = 7151 +/-  15 K,                       
                         L =   17.3 +/-   0.1 \lsun.                                             NOI2023 
21186+1134   BU  163     A is a double-lined spectroscopic binary, period 4.0d.                          
                         1986.395, 1986.565: The separation of this difficult partially                  
                         resolved pair was calculated under the assumption that delta V = 1.2            
                         magnitude, but the large number of measurements makes the result                
                         reliable.  The strange character of the observed motion (Tokovinin,             
                         1986 Astron. Circ. No. 1415) is confirmed.                              Tok1985 
                         Spectral types and masses of components assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
                         Mass-sum in good agreement with the complete speckle/spectroscopic      Fek1997 
                         analysis by Fekel et al. (1997).                                        Sod1999 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.44 +/- 1.33, 2.19, and 1.99 Msun, respectively.  Mlk2012 
21187+1417   J  1785     Heintz believes BRT1351 is identical.                                   Hei1985a
21188+0245   BAL2051     Aka OL  220.                                                                    
21188-0847   BU 1503     AC (137.4" @ 99deg): C is the galaxy NGC 7051.                          Dam2010 
21190+3945   STT 434     AB: H 4  39.                                                            MEv2010 
21190+2614   MET  92     Metchev & Hillenbrand (2009) find 5 optical companions within 12" and   Met2009 
                         a physical brown dwarf companion at 11.9", 109d, dK=9.58. Estimated             
                         mass of B 0.02 Msun.                                                    Tok2014d
21190-6013   R   328     B is CPD-60@7460.                                                               
21191+3954   SEI1502     ALI 1157.                                                                       
21191+1244   BPM2357     [PM2000] 2482869 + [PM2000] 2482944.                                    Gvr2010 
21193+5837   BAG   9     Aa,Ab: This companion could be the blue component of the VV Cep system          
                         M1Ib ep + B2V (Cowley, 1969 PASP, 81, 297).                             Bag1984b
21193+1640   BPM2358     [PM2000] 2483419 + [PM2000] 2483504.                                    Gvr2010 
21194+3814   HO  286     Often seen single. Rapid binary, distances small and quadrants                  
                         uncertain. One component is a Cepheid, V1334 Cyg.                               
             CIA   5     Aa,Ab: Gallenne et al. (2013) resolved the primary into an 8,as pair,           
                         and derived a combined spectroscopic/interferometric orbit. Spectral            
                         type of the companion is earlier than B5.5V.                            CIA2013a
                         Masses are 4.9 and 4.0 Msun. Estimated period = 5.3y,                           
                         a = 6.3au = 0.01".                                                      Evs2013 
                         Limb darkened diameter of Cepheid = 0.524 +/- 0.039 mas.                        
                         Limb darkened diameter of Cepheid = 40.6 +/- 3.0 \rsun.                         
                         Mass of A,B = 4.288 +/- 0.133, 4.040 +/- 0.048 \msun.                           
                         Mass of secondary = 4.288 +/- 0.133 \msun.                              GaA2018 
                         Mass of A,B = 4.6 +/- 0.7. 3.80 +/- 0.57 /msun.                         Krv2019a
21196+3948   SEI1503     ALI 1158.                                                                       
21196+1153   BPM2359     [PM2000] 2483964 + [PM2000] 2484103.                                    Gvr2010 
21197+5303   S   786     STTA217. B is BD+52@2911.                                                       
21198+0026   WAA  50     SLW1237.                                                                        
21198-2621   BU  271     A is a spectroscopic binary.                                                    
21199+5841   HLM  39     STI 2565.                                                                       
21199+3948   SEI1507     ALI 1159.                                                                       
21199-5327   HJ 5258     the Ind                                                                         
             MRN   3     Aa,Ab:  Marion et al. (2014) estimate the companion as A5V. Since               
                         Lagrange et al. (2009) have shown the star to have a constant radial    Lgr2009c
                         velocity, the odds for a face-on orbit are high.  Assuming a circular           
                         orbit, the period would be ~1.3y.                                       Mrn2014 
21200+5436   SKF1978     Originally listed as SKF 250, a discoverer designation already in use,          
                         so DD was changed to next available value.                                      
21200+3854   SEI1505     ALI 968.                                                                        
21200-6018   HJ 5256     B is CPD-60@7465. Spectral types F8? F2?                                        
21203-1048   HU   86     A is an Algol-type binary, RY Aqr.                                              
21205+4528   KRV   9     Classical Cepheid V0532 Cyg.                                                    
21205+1415   BPM2360     [PM2000] 2485989 + [PM2000] 2485929.                                    Gvr2010 
21206+1537   AG  416     B is BD+15@4392.                                                                
21208-5302   SHY 340     AC: HIP 105388 + HIP 105404. C component = BS Ind.                              
21209+1140   BPM2361     [PM2000] 2486701 + [PM2000] 2486892.                                    Gvr2010 
21209-0136   RST5161     J 1722.                                                                         
21209-0302   JNN 130     LP 697-26.                                                                      
                         2MASS J21205172-0301545 has a companion with brightness and color that          
                         is consistent with expectation, but no common proper motion test has            
                         yet been done.                                                          Jnn2012 
21210+0217   HEI 408     AB: TDT2913.                                                                    
                         AC: (273@, 54.5") may be BAL 1586. A close pair reported Walker was     Wak1966 
                         not seen by Heintz.                                                     Hei1987a
21210-5229   CVN  66     BS Ind.                                                                         
21212+0001   BAL 931     Baillaud appears to have made an error in reducing 1896 AC data.        Bal1944 
21212-2744   HDS3040     LSC  97.                                                                        
21213+1724   BPM2362     [PM2000] 2487714 + [PM2000] 2487808.                                    Gvr2010 
21214+1020   A   617     Both spectra are visible.                                                       
                         For the visual pair West (1976) computed the elements P, T, e, and      Wst1976 
                         longitude of periastron also from the RV's (orbit 3); tentative                 
                         elements a, i, and the node were added by Heintz in order to have a             
                         complete listing in the Fourth Orbit Catalog. Since the components are          
                         visually indistinguishable, the quadrant of the ascending node (but             
                         not the longitude of periastron) is arbitrary; with the node chosen as          
                         listed, the close pair would be the eastern component when the visual           
                         pair is at maximum separation.                                                  
                         The pair was long assumed to have a 12 yr period.                               
                         1980.4853  This measure was incorrectly identified with HR 8131 =               
                         alp Equ in McAlister et al. (1983).                                     McA1983 
                         The component with the slightly weaker lines is an SB1, P = 2.24 d.             
                         (#1297 in Batten et al., 1989).                                         Bte1989 
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         West & McAlister (1981).                                                Wst1981 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.60 +/- 0.44, 2.43, and 1.13 Msun, respectively.             Mlk2012 
21214-0310   RUC  14     HV Aqr. Spectral type of resolved companion estimated at K2-3V.         Ruc2007 
21214-1219   HJ  280     B is BD-12@5971.                                                                
21214-6655   HJ 5255     A 4.6d spectroscopic solution for the A component has been found        Tok2018d
                         making this a triple system, quadruple is Ba,Bb is physical.                    
21215+1122   BPM2363     [PM2000] 2487987 + [PM2000] 2487954.                                    Gvr2010 
21216-1825   ARA 502     aka J  1405. Jonckheere gives the location as "+40s, -1' de la          Skf2009 
                         BD-19 6082".  If you take a sign error in the RA offset (i.e. 40s west          
                         of the BD star rather than east), you land dead on WDS 21216-1825 =             
                         ARA 502 with which it matches.                                                  
21217+1731   BPM2364     [PM2000] 2488508 + [PM2000] 2488731.                                    Gvr2010 
21218+3230   HLM  40     Also appears to be POP1232CD which is not related to 21208+3227.                
                         WDS position of HLM  40 far off and is corrected here.                          
21218+0202   STF2787     B is BD+01@4465a.                                                               
21220+2727   OSO 145     G187-040. Not a common proper motion pair, based on color and                   
                         comparison with POSS2 red plates.                                       Oso2004 
21220-2224   HJ 5265     CD-22@15347.                                                                    
21221+1948   STFB 11     1 Peg. STTA218. B is a spectroscopic binary, P = 1111d, and is                  
                         BD+19@4690. Spectrum K0V.                                                       
                         Mk III Limb-darkened diameter  4.7   +/- 0.4   mas.                     MkT1989 
                         NPOI Limb-darkened diameter 2.315 +/- 0.023 mas, Sp = K1III,            NOI2018 
                         R = 11.89 +/- 0.15 \rsun, Teff = 4725 +/- 64 K, L = 63.5 +/- 3.3 \lsun,         
                         M = 1.60 +/- 0.18 \msun, Age = 2.04 +/- 0.54 Gyr.                               
                         AB: H 5  20.                                                            MEv2010 
21222+1725   BPM2365     [PM2000] 2489519 + [PM2000] 2489474.                                    Gvr2010 
21223+5734   POP1233     AC: HJL1107.                                                            HJL1986 
21223+1111   BRT1355     J 2577.                                                                         
21223-1455   BU 1262     H N 139.                                                                        
21224+5218   ES 2708     B is BD+51@3051.                                                                
21225+1207   BPM2366     [PM2000] 2490242 + [PM2000] 2490400.                                    Gvr2010 
21226-5547   HU 1536     A is SB, no orbit. No acceleration in the HIP1, only HIP2.              Tok2014d
21227+2737   LSC 130     35 Vul.                                                                         
21227+1101   BPM2367     [PM2000] 2490630 + [PM2000] 2490551.                                    Gvr2010 
21229+2639   BRT3366     Originally published as BRT 224.                                        Brt1928 
21229+0649   HJ 3023     bet Equ = 10 Equ. A is a spectroscopic binary.                                  
21229+0644   ALD  76     BRT 2191.                                                                       
21231+4831   HDS3045     Primary is V2154 Cyg, an Algol-type eclipsing binary, period 2.63064d.  Zas2011 
21232-8703   I   337     Combined solution.                                                      Tok2018d
21234+1543   BPM2368     [PM2000] 2492166 + [PM2000] 2491909.                                    Gvr2010 
21236+1030   BRT1356     J 1787.                                                                         
21237+0422   STF2791     J  1244.                                                                J__1962a
21238+3721   STFA 55     B is BD+36@4537.                                                                
                         Toyota et al. (2009) monitored the RV of the A component every 1-2              
                         months between 2003 Mar - 2007 Nov, using a high-dispersion echelle             
                         (precision ~10 m/s). The star shows a large RV variation; a Keplerian           
                         fit gives a period of 863.8d and an eccentricity of 0.20, which may be          
                         induced by a companion of mass ~8.1 Mjup, by stellar rotation or by             
                         non-radial pulsation.                                                   Toy2009 
21238-0635   S   788     B is BD-07@5550.                                                                
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
21241+2519   BU  447     A is a spectroscopic binary.                                                    
21242+1504   BPM2369     [PM2000] 2493806 + [PM2000] 2493594.                                    Gvr2010 
21242-1253   HJ 5517     18 Aqr.                                                                         
21244+1425   BPM2370     [PM2000] 2494287 + [PM2000] 2494124.                                    Gvr2010 
21244-1248   BU  272     BRT2783.                                                                Brt1947 
21244-4100   BU  766     the 2 Mic                                                                       
21247-6814   GC 29928    Hipparcos astrometric solution assumes circular orbit (e = omega = 0).  HIP1997d
21249+4919   ES 2710     Spectral type B9pSi:Cr:Sr:. Variable, V1934 Cyg.                                
21250-5004   BRT1118     A likely plate flaw.                                                    Grv2021b
21251+1740   BPM2371     [PM2000] 2495561 + [PM2000] 2495394.                                    Gvr2010 
21251+0923   STF2793     AB,C: According to Le Beau, this pair is physical.                      LBu1990c
21251+0157   BAL1588     Secondary not visible in Aladin; probably plate flaw or typographical           
                         error in AC Catalog.                                                            
21252+1742   BPM2372     [PM2000] 2495861 + [PM2000] 2495959.                                    Gvr2010 
21254+1428   BPM2373     [PM2000] 2496287 + [PM2000] 2496260.                                    Gvr2010 
21254+1121   A   887     AB: Closed in in the last 30 years. Needs speckle.                              
                         AC: Based on inspection of the field, the Aitken measure apparently     A__1932a
                         had a typographical error in theta - 112.4 should be 312.4.                     
                         AB: Rectilinear solution by Rica & Zirm (2012).                         FMR2012i
21255+0203   A  2289     Little observed in recent years despite considerable orbital motion.            
21257+1140   BPM2374     [PM2000] 2496973 + [PM2000] 2497086.                                    Gvr2010 
21258+3640   S   790     69 Cyg.                                                                         
                         AC: H 5  44.                                                            MEv2010 
21258+3329   GYL  56     Hipparcos stochastic double solution.                                           
21260+4144   BLL  54     B is BD+41@4133.                                                                
21264-2025   HWE  56     AC = HDO 165                                                                    
21265+5245   BU  369     There is a 14th mag star a little farther than the companion measured,          
                         in the direction 336deg.                                                Bu_1894 
21266+1611   BPM2375     [PM2000] 2498708 + [PM2000] 2498833.                                    Gvr2010 
21266-4604   HJ 5267     AD = LDS 742.                                                                   
                         A: Unresolved. Variable RV. The companion HJ 5267 at 5" is listed in            
                         the WDS with one measurement and is not seen here. It should be                 
                         considered spurious.                                                    Tok2013b
                         AB: A is SB, no orbit. AB unresolved  with NICI in Tokovinin et al.     Tok2012a
                         (2012), the companion at 5" is not seen.                                Tok2014d
21267+1341   STF2797     B is a Beta Lyrae-type system. A is the variable KP Peg.                        
21267+0527   OSO 146     G025-029. Neither is a common proper motion pair, based on color or             
                         comparison with POSS2 red plates                                        Oso2004 
21267-2225   SEE 446     zet Cap = 34 Cap. CD-22@15388. A is a spectroscopic binary.                     
21268+3732   COU1821     TDT2972.                                                                        
21270+7339   ZUC  15     Primary is white dwarf WD 2126+734 = GJ 828.5 = G261-43. The companion          
                         appears to also be a white dwarf, of temperature ~5000K.                Zuc1997 
21271+3402   ES 2262     Aka TDS1129.                                                            Dam2016d
21271+2405   POU5372     Aka COU 133.                                                            Dam2013 
21271-6239   CTI9698     V400 Pav.                                                                       
21272+1408   BPM2376     [PM2000] 2499912 + [PM2000] 2499781.                                    Gvr2010 
21274-0701   HDS3053     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.27 +/- 1.37, 2.18, and 2.01 Msun, respectively.             Mlk2012 
                         Combined solution.                                                      Tok2018d
21278+6659   DCH 115     7 Cep.                                                                          
21278+3715   SEI1518     ALI 442.                                                                        
21281-4427   CPO 622     CPD-44@10026.                                                                   
21282+1440   BPM2377     [PM2000] 2501916 + [PM2000] 2502158.                                    Gvr2010 
21282-1906   HJ 3029     Primary is eclipsing binary of W UMa -type, period 0.4733 d.            Zas2012 
21282-2144   EGN  26     Single epoch; bound/unbound nature of pair unknown.                     Egn2007 
21282-5510   R   331     CPD-55@9593.                                                                    
21285+3636   ES 2127     ALI 443.                                                                        
21285-0210   BRT 516     BAL 265.                                                                        
21285-1751   LDS 744     NLTT 51319/51320                                                        Chm2004 
21287+7034   LAB   6     Aa,Ab: bet Cep = 8 Cep = Alfirk. The third component was discovered             
                         recently by speckle interferometry.                                             
                         1971.48: Estimated delta m ~ 3 - 4.  Attempts by Couteau (1973 private          
                         communication) to observe the companion visually were unsuccessful,             
                         supporting this large magnitude difference. Some anisotropic features           
                         in the Fourier transform may indicate other companions or                       
                         circumstellar matter.                                                   Lab1974 
                         1975.545, 1975.956: This is the primary of the system bet Cep and is            
                         believed to be a binary of period ~50 yr. There is also evidence of             
                         radial velocity variations. Labeyrie et al (1974) noted anisotropic     Lab1974 
                         features in the power spectrum which might indicate other companions,           
                         but such features were not observed in the power spectrum derived from          
                         these observations.                                                     BLM1978 
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 9.98 +/- 3.28, 12.04, 12.02 Msun, respectively.    Mlk2012 
                         Uniform disk diameter  0.274 +/- 0.016 mas,                                     
                         Limb darkened diameter 0.280 +/- 0.016 mas,                                     
                         Teff = 29500 +/- 2500 K based on LDD.                                           
                         Radius is 7.22 +/- 0.42 \rsun.                                          CIA2019a
             STF2806     AB: H 3   6.                                                            MEv2010 
                         AB: Additional notes may be found in Dembowski (1883).                  D__1883 
21287+1627   BPM2378     [PM2000] 2502826 + [PM2000] 2502886.                                    Gvr2010 
21288+6537   OSO 147     G264-006. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
21289+1105   STF2799     STF2911.                                                                        
21290+5844   HDS3058     Aa,Ab: Classification is from Garmany & Stencel (1992 A&AS 94, 211).    HIP1997a
                         The Hipparcos results confirm the CHR 211Aa,Ab pair.                    Msn1998a
                         1994.7001: Very weak detection, possibly an artifact.                   Msn1999b
21290+2211   HJ 1647     AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
21291+3102   BRT 288     ES 2441 is identical                                                    Hei1983a
21291+1211   BAR  56     G126-002. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AC: Additional notes may be found in van den Bos (1963).                B__1963a
21293+1611   BPM2379     [PM2000] 2503886 + [PM2000] 2504152.                                    Gvr2010 
21295+3728   SEI1519     ALI 692.                                                                        
21296+1340   BPM2380     [PM2000] 2504557 + [PM2000] 2504574.                                    Gvr2010 
21297-6016   R   332     CD-60@7720.                                                                     
21299+5256   STF2803     B is BD+52@2951.                                                                
21299+2338   BU  685     2 Peg.                                                                          
                         Mk III Limb-darkened diameter  4.521 +/- 0.047 mas.                     MkT2003 
21299-0220   JNN 131     The close companion to 2MASS J21295166-0220070 has consistent                   
                         brightness and color with the expectation for a physical companion.             
                         Only one epoch of images exists, hence common proper motion has yet to          
                         be confirmed.                                                           Jnn2012 
21301+1629   BPM2381     [PM2000] 2505701 + [PM2000] 2505863.                                    Gvr2010 
21301+1514   J   198     The 1958 Van Biesbroeck measure is inconsistent with other measures.    VBs1960 
21303-7200   HEI 595     TDT3001.                                                                        
21304+1508   BPM2382     [PM2000] 2506419 + [PM2000] 2506318.                                    Gvr2010 
21305+3701   SEI1521     J  1155.                                                                        
21305-0707   LDS6355     Wolf 921                                                                        
21306+4852   OSO 148     G232-018. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates.                                                  Oso2004 
21306+1140   BPM2383     [PM2000] 2506817 + [PM2000] 2506871.                                    Gvr2010 
21308+4827   A   770     Also a spectroscopic binary of indeterminate period.                    Tok2019b
                         Espin calls this HJ 1657, BDS 11057.                                    Es_1932B
21308-2204   OL   76     CD-22@15423.                                                                    
21309+1427   BPM2384     [PM2000] 2507331 + [PM2000] 2507309.                                    Gvr2010 
21310-4822   HJ 5273     LDS 746.                                                                        
21312+8652   STF2858     LDS1957.                                                                        
                         HJL 297.                                                                HJL1986 
21313-0947   BLA   9     Wolf 922. Proper motion +1170 -060.                                             
                         Combined solution by Segransan et al. (2000) from astrometry,           Sgr2000 
                         spectroscopy, and parallax. Solution yields mass and orbital parallax           
                         determination.                                                                  
                         Possible tertiary companion mentioned in Henry et al. (1999) is here    Hen1999 
                         retracted.                                                              TSN2015 
21314+1414   BPM2386     [PM2000] 2508247 + [PM2000] 2508486.                                    Gvr2010 
21314+1302   BPM2385     [PM2000] 2508225 + [PM2000] 2508285.                                    Gvr2010 
21314-2217   HJ 3030     CD-22@15433.                                                                    
21315+1744   BPM2387     [PM2000] 2508419 + [PM2000] 2508303.                                    Gvr2010 
21316-0534   H 5  76     H V 76. bet Aqr = 22 Aqr = Sadalsuud                                            
                         Common proper motion pair with 22058-0019 = alp Aqr.                    Skf2013 
21317-1330   SCJ  29     B is BD-14@6050.                                                                
21318-0155   LDS6356     G026-008. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 51459/51458                                                        Chm2004 
21318-4701   RST3287     Not in Michigan Pub. Vol. XI.                                                   
21319+7034   H 5  28     H V 28.                                                                         
21321+1740   BPM2388     [PM2000] 2509576 + [PM2000] 2509430.                                    Gvr2010 
21322+3341   ES 2383     Identical with ES 2384                                                  Hei1995 
21322+1731   BPM2389     [PM2000] 2509800 + [PM2000] 2509636.                                    Gvr2010 
21322+1342   SIG   6     2MASS J21321145+1341584.                                                        
                         Derived spectral types L5 +/- 0.5 and L7.5 +/- 0.5, luminosities 6.3            
                         +/- 1.9 and 3.0 +/- 1.0 (units 10-5 Lsun). Distance 28 +/- 4 pc         Sig2007 
21322+0013   KUI 107     LDS 749. Red and white dwarfs. The primary is a double-lined                    
                         spectroscopic binary, P = 3.76d. G026-009.  Known proper motion                 
                         companion (G026-010, V=14.58) at 2.2' and PA=29 deg. According to       AlC2000 
                         Allen et al., there is a brighter companion at 0.7"                     Oso2004 
21322-3357   B  1009     6 PsA.                                                                          
21324+1553   BPM2390     [PM2000] 2510128 + [PM2000] 2510260.                                    Gvr2010 
21324+1054   LDS4894     aka KPP3371.                                                                    
21324-2058   LDS6354     CPD-21@7952.  Also known as RSS 562.                                            
                         NLTT 51476/51475                                                        Chm2004 
                         SHY 342. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
21325+4436   POP 136     BC: The BC component of this group is the small planetary nebula        Skf2009 
                         IC 5117 = HD 205211.                                                            
21325-2631   RST1093     Spectral type M?                                                                
21326+1121   J  1788     Not found by Heintz at IDS position.                                    Hei1990b
21327+3948   HO  604     Variable of unknown class.                                                      
21329+4959   CHR 102     A spectroscopic binary.                                                         
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 6.12 +/- 1.01, 5.92, and 2.24 Msun, respectively.             Mlk2012 
21330+2408   OSO 149     G126-008. Neither AB nor AC is a common proper motion pair, based               
                         on color and comparison with POSS2 red plates                           Oso2004 
21330+2043   STF2804     Mt. Wilson spectral types F5s and F8.                                           
                         Nearly identical parallax but very different proper motion.                     
21331+7059   MLB 367     Not found by Heintz at IDS position.                                    Hei1987a
21331+3938   MLB 899     As ascertained by Skiff, the MLB 899 pair is actual the "hourglass-     Skf2007 
                         shaped" double planetary nebula first noted by Humason.                 Hum1921 
21332+6410   MLB 223     Aka TDT3027.                                                                    
21334+3058   KU  132     AB: HJL 292.                                                            HJL1986 
21337+1554   BPM2391     [PM2000] 2512487 + [PM2000] 2512392.                                    Gvr2010 
21338+0147   BLZ   1     LDS5247.                                                                        
21339+5045   HDS3070     Includes V2165 Cyg, an Algol-type eclipsing binary, P = 1.962385d.      Zas2012 
21339+1625   BPM2392     [PM2000] 2512801 + [PM2000] 2512746.                                    Gvr2010 
21341+0651   REE   1     PG 2131+066 = IR Peg. White dwarf plus early M main-sequence star.              
                         Distance estimated from photometry and seismology as 632 +150/-111 pc.  Ree2000 
21342+5029   ES   33     Aka TOI 1331.                                                                   
21342-0327   BU  165     HDO 166. Included in list of new doubles (discovery date 1868.62) by            
                         Pei1882; no description given.                                                  
21344+6644   STFA 57     B is BD+66@1416.                                                                
21344+5349   GIC 167     G232-020/G232-021.                                                              
21344+1816   BPM2393     [PM2000] 2513723 + [PM2000] 2513818.                                    Gvr2010 
21345+0930   STF3112     HJL 293. STT 528.                                                       HJL1986 
21346+1551   BPM2394     [PM2000] 2514076 + [PM2000] 2514061.                                    Gvr2010 
21348+3304   GYL  61     Goyal's coordinates match this pair, but his original measure does      Gyl1966 
                         not match anything in the field. Perhaps 182deg was erroneously                 
                         written as 82deg before a quadrant flip?                                        
21348+3204   LSL   1     Some component designations corrected or changed Dec 2004:                      
                         Aa pair --> AD                                                                  
                         Ab pair --> BF                                                                  
                         CD pair --> CG                                                                  
                         Also 11" companion noted in BDS added as AE pair.                       Bu_1906 
21349-4948   HIP 106560  Unresolved. Astrometric and SB with high proper motion and low                  
                         metallicity.                                                            Tok2013b
21351+1433   BPM2395     [PM2000] 2514918 + [PM2000] 2514984.                                    Gvr2010 
21352+4634   LDS4898     aka RAO 463.                                                                    
21352-3033   HJ 5280     Spectral type M?                                                                
21353+4612   TOR  28     Formerly known as PAN  25.                                                      
21353+2812   CHR 103     A spectroscopic binary, P = 12.2d. Hence triple.                                
                         This system, first announced by McAlister and recalled in a later       McA1984b
                         McAlister paper after repeated attempts at confirmation, has been       McA1993 
                         restored. While perhaps still spurious, the subsequent confirmation or          
                         suspected duplicity (by another technique) makes the discovery                  
                         measurement somewhat more probable.                                             
21354+3837   ES 1995     Not found by Heintz.                                                    Hei1995 
21354-5523   HJ 5276     CD-55@8863.                                                                     
21355+2427   HU  371     Possibly triple; Dominion Astrophysical Observatory spectra showed              
                         a double spectrum.                                                              
                         Only elements P and T have been amended by Starikova (1977) from the    Sta1977a
                         orbit of Baize (1961).                                                  Baz1961a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.87 +/- 3.02, 6.02, and 2.00 Msun, respectively.             Mlk2012 
21355-1846   I   380     HU  965.                                                                        
21356+1731   BPM2398     [PM2000] 2515757 + [PM2000] 2515954.                                    Gvr2010 
21356+1448   BPM2396     AB: [PM2000] 2515709 + [PM2000] 2515636.                                Gvr2010 
             BPM2397     BC: [PM2000] 2515636 + [PM2000] 2515401.                                Gvr2010 
21359+2622   HJ 1661     B is BD+25@4575a.                                                               
21359+1723   BPM2399     [PM2000] 2516368 + [PM2000] 2516253.                                    Gvr2010 
21359+0041   HJ 3039     AB: HJL 294.                                                            HJL1986 
21360+5728   STF2813     Also known as HJ 1672.                                                          
21363+2917   BRT  56     MLB 490 is identical                                                    Hei1980a
21365+1511   BPM2400     [PM2000] 2517297 + [PM2000] 2517260.                                    Gvr2010 
21366+3928   VYS  10     AC+39 60670. VYS 836.                                                           
21369+4025   74 Cyg      Hipparcos astrometric solution assumes circular orbit (e = omega = 0).  HIP1997d
21369-0841   JNN 132     Due to the small separation (~0.24") of the companion detected in the           
                         AstraLux images, physical companionship is very likely, although only           
                         one epoch of images exists so far.                                      Jnn2012 
21370-0617   RST4696     J 3302.                                                                         
21370-3553   CBL 184     SHY 798. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
21371-1928   H 6   6     H VI 6. eps Cap = 39 Cap. A is a Cepheid and shell star. It is also an          
                         occultation double. B is BD-20@6253.                                            
21372+2511   POU5436     Aka POU5432.                                                                    
21373+5900   HJ 1677     Same as BDS 11149.                                                              
                         KR   54.                                                                        
21374-6811   DON1012     Spectrum: G5/8(V)+(F).                                                          
21375-1618   HJ 5284     B is BD-16@5898.                                                                
21376+0643   STT 443     H 2  62.                                                                MEv2010 
21376+0137   JNN 291     2MASS J21374019+0137137. This newly discovered binary candidate is a            
                         probable member of the bet Pic moving group according to the Schlieder          
                         et al. (2012 AJ 144, 109) study. Its relatively small projected                 
                         separation of ∼4.5 au implies that its orbit could be dynamically       .     
                         constrained in a reasonable timeframe, which makes it a potential               
                         benchmark binary in the future. Estimated age 10-20 Myr; masses 0.11            
                         +/- 0.04 and 0.05 +/- 0.02 Msun; a ~5.2 au.                             Jnn2014 
21376-0023   STF2809     H 4  38.                                                                MEv2010 
             FYM9001AC   Designated by author as FYM 184, homever 00345+5513CD and DE also       FyM2014 
                         designated by author as FYM 184. Redesignated.                          FyM2014c
21376-0744   HJ 1662     LDS 750.                                                                        
21376-2026   YSC 119     BQ Cap. Primary is Beta Lyr type eclipsing binary, period 1.47409d.     Zas2017b
21377+0637   STFA 56     3 Peg. STTA219. A is an occultation double. B is BD+05@4829.                    
                         AB: HJL 295.                                                            HJL1986 
                         AB: H 5  98.                                                            MEv2010 
21378-0751   MCA  68     xi Aqr = 23 Aqr. A long-period spectroscopic binary now resolved by             
                         speckle interferometry. Also an occultation pair.                               
                         This object was misidentified as HR 8265                                McA1978c
             xi Aqr      Gontcharov & Kiyaeva (2002) photocentric (astrometric) orbit is based   Gon2002a
                         on a combination of ground-based catalogs with Hipparcos.                       
21379+2743   MLB1093     AB: COU 13.                                                                     
             HDS3080     Aa,Ab: CC 1299                                                                  
                         Marginal detection of 14th mag secondary, but mass-sum too large and            
                         more GB obs needed to define orbit. (HIP solution is slit-error).       Sod1999 
                         McCarthy (1983) says he resolved this pair using IR speckle             Mcy1983 
                         interferometry at 2.2 and 3.4 microns, but does not include any values          
                         for rho or theta.                                                               
21380+4829   ES  102     Includes V2169 Cyg, a Beta Lyr type eclipsing binary, P = 1.23372d.     Zas2012 
21381+4616   TOR  29     Formerly known as PAN  26.                                                      
21382-8435   TDT3070     This may be the lost pair R   334 with an unusually large error by      Dam2013 
                         Russell.                                                                        
21384+5658   LEE   1     AB: Classification is from Garmany & Stencel (1992 A&AS 94, 211).       Msn1998a
21384+2953   MLB 491     BRT 289.                                                                Brt1929b
21385+0546   HJ  941     4 Peg.                                                                          
21387+2530   CHR 104     This system, first announced by McAlister and recalled in a later       McA1984b
                         McAlister paper after repeated attempts at confirmation, has been       McA1993 
                         restored. While perhaps still spurious, the subsequent confirmation or          
                         suspected duplicity (by another technique) makes the discovery                  
                         measurement somewhat more probable.                                             
21388-0121   BAL 624     J 3278.                                                                         
21390+5729   BU 1143     The classification and orbit of the primary are from Burkholder et al.          
             STF2816     (1997 ApJ 490, 328).  Stickland (1995) found that the spectral line     Stc1995 
             GUI  36     variations result from one close binary (with weak secondary lines)             
             FLE   3     and a stationary component, a conclusion later confirmed by Burkholder          
                         et al.  The speckle resolution of the system (CHR 212Aa,Ab) clearly             
                         supports the view that this is an SB2 plus a distant O star companion.          
                         The C and D components were also observed and appeared to be single.    Msn1998a
                         Classifications of the C and D components are from Hoffleit & Warren            
                         (1991).                                                                 Hof1991 
             STF2816     AC: H 3  71.                                                            MEv2010 
21391+4421   HJ 1673     Also known as HJ 1679 and TDT3082.                                      Dam2010 
21391-1221   VBS  34     RST 5555. A difficult pair. For AB,C see note by van den Bos.           B__1960b
21392+4311   GIC 168     G212-052/G212-051.                                                              
21393+6017   OSO 150     G231-052. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
21393+2043   STT 445     One component may be variable.                                                  
21395+4144   STT 447     AC and AE identified with H 3 110a and H 3 110b. BDS 11145.             Bu_1906 
             ABH 148     AG was incorrectly identified as the EG pair.                                   
21395+3009   A   772     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.37 +/- 2.56, 3.29, and 1.82 Msun, respectively.             Mlk2012 
21395-0003   BU 1212     24 Aqr.                                                                         
                         One component is SB; the RV range in the combined light is 45 km/s.             
                         Branham (2005) uses this system illustrate a method for calculating     Bnh2005 
                         orbital elements. His elements are not included in the catalog, as              
                         he considers them only an example.                                              
                         Combined spectroscopic/visual solution by Branham (2007). Additional    Bnh2007 
                         elements: V0 = -13.339 +/- 0.010 km/sec, K1 = -6.921 +/- 0.022 km/sec,          
                         K2 = -9.061 +/- 0.020 km/sec, parallax = 0".014 +/- 0".008,                     
                         fractional mass = 0.433 +/- 0.002.                                              
                         AB,C: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB,C: Rectilinear solution by Hurowitz et al. (2014).                   USN2014b
21395-1913   HJ 3043     B is BD-19@6143.                                                                
21396+4712   HJ 1676     Magnitude of A is from Tycho Catalog; magnitude of B is from the Guide          
                         Star Catalog, but Romero previously calibrated GSC magnitude to         FMR1999g
                         standard photometry.                                                            
21396+0215   BUP 229     25 Aqr.                                                                         
21399+2737   HDS3083     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 0.92 +/- 0.21, 0.86, and 0.75 Msun, respectively.             Mlk2012 
21399+0623   OSO 151     G093-027. AB comprise a common proper motion pair, but AC do not.               
                         According to Carney et al., AB is a visual binary, but nothing is       Crn1994 
                         found in either SIMBAD or the archives.                                 Oso2004 
21399-0842   RST4091     J 1407.                                                                         
21400+5407   GIC 169     Ross 200                                                                        
21400+0911   CHR 105     Lacy & Popper (1984) discovered a previously unknown companion to the   Ppp1984 
                         eclipsing binary EE Peg through its effects on radial velocity and              
                         times of primary eclipse.  Their third component, with a period of              
                         1464 days and a mass ratio of roughly 5 - 12, would be expected to              
                         exhibit a separation from the primary of ~0".03. It thus seems likely           
                         that the object listed here is yet another long-period member of this           
                         system.                                                                         
21401+2632   BRT3367     Originally published as BRT 226.                                        Brt1928 
21401-1640   gam Cap     Hipparcos astrometric solution assumes circular orbit (e = omega = 0).  HIP1997d
                         = Nashira                                                                       
21401-1757   LDS6357     NLTT 51781/51782                                                        Chm2004 
21402+4316   AC   20     A: 75 Cyg                                                                       
21402+3703   SEI1531     J 1146.                                                                         
21404+5735   STF2819     HJL 296.                                                                HJL1986 
                         H 3  72.                                                                MEv2010 
21405+1625   CLO   2     2MASSW J2140293+162518                                                          
                         Aa,Ab: Konopacky et al. (2010) derive a distance of 25 +/- 10 pc and a          
                         system mass of 0.10 +/- 0.08 Msun.                                      Kon2010 
             ALP  26     Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
21406+5419   ES   35     A is the semiregular variable RU Cyg.                                           
21412-0729   OSO 152     G026-022. Not a common proper motion pair                               Oso2004 
21414+1245   BPM2401     [PM2000] 2525223 + [PM2000] 2525353.                                    Gvr2010 
21415+8555   TDT3110     See note for 21452+8554 A   775.                                                
21415+5035   COU2444     COU2547.                                                                        
21415+3817   SEI1532     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
                         A likely plate flaw.                                                    Grv2021b
21415-7723   BLM   6     Astrometric orbit by Alden (1939) used P, T, e taken from the           Ald1939b
                         spectroscopic orbit by Colacevich (1935). Not reinvestigated since.     Cla1935 
                         Speckle companion not real.                                                     
                         nu Oct.                                                                         
21416+4048   S   796     76 Cyg. A is a spectroscopic binary. B is BD+40@4610.                           
                         AB: H 5  43.                                                            MEv2010 
21417+1735   OSO 153     G126-024. Not a common proper motion pair, based on color and                   
                         comparison with POSS2 red plates.                                       Oso2004 
21417+0625   HU  278     Purported FYM 56AD pair removed on request of author.                   FyM2014b
21417-0036   J  1409     BAL 625.                                                                        
21418+1151   BPM2402     [PM2000] 2525829 + [PM2000] 2525828.                                    Gvr2010 
21418+0145   HJ 3049     Rectilinear solution by Hurowitz et al. (2014).                         USN2014b
21420+1856   LBU   2     Aa,Ab: A 1999 measure of 21426+1900 HO  165 by Mason et al. was         WSI2000b
                         erroneously listed under this pair.                                             
             STF2818     Lewis measure erroneously listed as 21426+1900L    50AC, companion      L__1899a
                         to HO  165.                                                                     
21420-2316   SEE 454     41 Cap.                                                                         
21421+3602   ALI 220     No star at AC2000 position of companion - possible plate flaw or                
                         reduction error.                                                                
21421+1328   LDS4904     LDS4855.                                                                        
                         NLTT 51877/51874                                                        Chm2004 
21422+3100   OSO 154     G188-020. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
21422+3008   MLB 575     Heintz described MLB's                                                  Hei1985a
                         confused description.                                                   Mlb1929 
21422-1221   J  1410     BRT 2784.                                                                       
21423+0555   HU  280     Distance in measure given by ADS for 1908.2 (6n, Bry) needs correction.         
                         It represents two annual means: 0.18" in 1907 and 0.30" in 1908; the            
                         latter includes values 0.52", 0.19", 0.18", the first of which must be          
                         rejected, the observer having even noted in addition "not separated".           
                         The same kind of error exists for some other objects on the same night          
                         (BU 151 and HU 371, for example).                                       Mlr1954a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.51 +/- 1.89, 3.75, and 1.82 Msun, respectively.             Mlk2012 
21424+4105   KUI 108     77 Cyg.                                                                         
                         One component is an SB1, P = 1.73 d.                                            
                         The system may be physically related to 21426+4103BU 688 according to   Egg1965b
                         Eggen, and thus quintuple.                                                      
21424+1750   HU  373     BU  691.  The two single star detections of Couteau and van den Bos             
                         may be of the incorrectly identified primary, BD+17 4629.                       
21425+1526   BPM2403     [PM2000] 2526981 + [PM2000] 2527063.                                    Gvr2010 
21425-3756   HJ 5288     B is CD-38@14687.                                                               
21426+4103   BU  688     See KUI 108 note (21424+4105).                                                  
                         Only elements P and T have been amended by Starikova (1984) from the    Sta1984 
                         orbit of Baize (1981).                                                  Baz1981a
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 8.73 +/- 5.21, 3.07, and 1.35 Msun, respectively.  Mlk2012 
21426+1900   HO  165     An 1899 measure by Lewis was erroneously listed as the AC components    L__1899a
                         under the designation L    50. It actually was a measure of STF2818.            
                         A 1999 measure by Mason et al. was erroneously listed under the pair    WSI2000b
                         21420+1856LBU   2Aa,Ab, the A component of STF2818.                             
21429+2152   HJ 1683     AC: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
21429+1537   BPM2404     [PM2000] 2527540 + [PM2000] 2527452.                                    Gvr2010 
21430-2025   SEE 456     HU  967.                                                                        
21431+1338   HJ 1682     Rectilinear solution by Hurowitz et al. (2014).                         USN2014b
21432+3801   BLL  55     A is the semiregular variable RV Cyg.                                           
21434+3817   S   799     79 Cyg.                                                                         
                         AB: H 6  57.                                                            MEv2010 
21434+1432   BPM2405     [PM2000] 2528288 + [PM2000] 2528171.                                    Gvr2010 
21435+5847   BU  690     mu Cep = Erakis = Herschel's Garnet Star. A is a semiregular variable.          
                         Mk III Uniform-disk  diameter 17.7   +/- 0.3   mas.                     MkT1989 
                         Mk III Limb-darkened diameter 20.584 +/- 0.480 mas.                     MkT2003 
21435+2721   A   299     The DE and DF pairs were incorrectly listed as AE and AF in the IDS.            
                         See the ADS for 1875 and 1910 rectangular measures of AD and DE.                
             OSO 155     DG: G188-022. Common proper motion pair.                                Oso2004 
                         Previously entered in WDS as 21440+2723, before primary was identified          
                         as the D component of the A 299 multiple.                                       
21437+0030   CHE 315     There was an error in Chevalier's printed declination, but the offset   Che1909 
                         from his plate center gives coordinates of a pair which agrees with             
                         his measures.                                                           Hrt2012b
21439+2751   HO  166     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.70 +/- 1.25, 2.79, and 1.17 Msun, respectively.             Mlk2012 
21440+1705   LDS6358     NLTT 51967/51965                                                        Chm2004 
21440-5720   JC   25     AB: B is CPD-57@9941. Spectral type F6/8IV/V.                                   
                         AB: SHY 344. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
21441+2845   STF2822     mu Cyg. The A component is a double-lined spectroscopic binary.                 
                         AB: H III 15. D is the principal component of ES 521.                           
                         AC and AD: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB: H 3  15.                                                            MEv2010 
             ES  521     DE: D is SB2                                                            Tok2014d
             FYM  25     DG pair initially listed incorrected as DH.                             FyM2014b
             STF2822     AC: Rectilinear solution by Friedman et al. (2011).                     USN2011a
21441+0709   STTA222     B is BD+06@4891.                                                                
21441-2200   DON1017     CD-22@15541.                                                                    
21442+0953   S   798     eps Peg = 8 Peg = Enif. STTA223 = H 6 103.                                      
                         The primary is variable.                                                        
21443+4234   OSO 156     G212-055. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates.                                                  Oso2004 
21443-2348   LDS6360     NLTT 51951/51952                                                        Chm2004 
21444+0008   CHE 316     Also known as DUF   3.                                                          
21445+1446   LUH   4     GJ 9751 = HN Peg                                                                
                         CHARA Array Limb-darkened diameter of A :                               CIA2013c
                         R =  1.0189 +/- 0.0291 \rsun, L =   1.0992 +/-0.0190 \lsun,                     
                         Teff = 5860 +/-  83 K, M = 0.975 \msun, Age = 5.8 Gyr.                          
                         Common proper motion for both components was determined through                 
                         comparison of relative location with that obtained by 2MASS. The B              
                         component is determined to be a possible T dwarf (T2.5 +/- 0.5) based           
                         on mid-IR colors and magnitudes. Age is determined as 0.3 +/- 0.2 Gyr           
                         and mass of secondary 0.021 +/- 0.009 Msun.                             Luh2007 
21446+2539   BU  989     AB: kap Peg = 10 Peg.                                                           
             kap Peg     Double lines have been observed in the spectrum of A.                   Tok2006 
                         The SB1 with P = 5.97 d (#1329 in Batten et al., 1989) is believed to   Bte1989 
                         to be the visual component B, and a set of double lines is observed             
                         which is ascribed to star A (Beardsley & King 1976).                    Bey1976 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Combined solution by Muterspaugh et al. (2006), using PHASES            Mut2006 
                         differential astrometry, iodine cell radial velocities, and published           
                         visual and speckle data. Mass of A is 1.549 +/- 0.050 Msun. Center of           
                         light motion of Ba,Bb pair is seen, allowing determination of masses            
                         for both components: 1.662 +/- 0.064 and 0.814 +/- 0.046 Msun.                  
                         Semimajor axis and error in catalog derived from their values of a              
                         (AU) and parallax, plus errors in those quantities. No sign of                  
                         purported spectroscopic companion to A component. Original tabulated            
                         data are listed below, including date (MJD), dRA and dDEC (mas),                
                         errors in dRA and dDEC (microarcsec):                                           
                         52591.15558   139.4192   -68.9527     337.2   144.9                             
                         52809.42172   176.3305   -52.8124     313.0   223.8                             
                         52834.42590   178.7642   -49.5003     142.0   142.0                             
                         52836.47700   178.2380   -48.6352     377.6   146.9                             
                         52862.26351   179.1262   -46.6494     142.0   142.0                             
                         52864.43495   180.0359   -45.8604     142.0   142.0                             
                         52865.25769   180.3088   -45.0103     142.0   142.0                             
                         52868.42699   179.3844   -45.8741     142.0   142.0                             
                         52891.30945   180.2407   -42.5429     142.0   142.0                             
                         52893.35153   180.8695   -42.7435     312.8   142.0                             
                         52894.33761   181.2314   -42.0489     142.0   142.0                             
                         52895.31028   181.5086   -41.4518     142.0   142.0                             
                         52896.29061   180.7701   -41.3602     142.0   142.0                             
                         52897.28730   180.3950   -41.7411     142.0   142.0                             
                         52915.28300   180.4724   -39.4518     142.0   142.0                             
                         52916.29333   179.8880   -39.7969     329.0   142.3                             
                         52918.11818   181.2814   -38.7883     482.5   330.8                             
                         52919.28864   181.3653   -38.3103     142.0   142.0                             
                         52920.12057   180.8864   -38.2854     661.1   422.9                             
                         52929.26987   181.2990   -38.0007     197.9   142.4                             
                         52930.25991   181.2730   -37.3111     287.3   142.6                             
                         52950.22128   179.7824   -34.3888     839.4   174.7                             
                         52952.20159   180.7612   -35.0063     510.9   145.2                             
                         52983.12402   179.3421   -30.6844     354.1   144.9                             
                         53130.50643   168.6227    -9.8442     467.3   362.7                             
                         53145.46573   168.9574    -7.4882    1766.2  1329.6                             
                         53152.47072   166.1418    -4.9533     142.0   142.0                             
                         53168.42321   164.7537    -3.8669     533.3   376.6                             
                         53172.46749   162.4907    -2.9062     142.0   142.0                             
                         53173.44399   162.7425    -3.3484     142.0   142.0                             
                         53181.41157   162.9387    -0.9785     142.0   142.0                             
                         53182.40964   162.5248    -0.6694     142.0   142.0                             
                         53186.41943   161.7325    -0.6729     142.0   142.0                             
                         53187.40125   162.1831    -0.1186     142.0   142.0                             
                         53197.36300   159.6357     0.5078     142.0   142.0                             
                         53198.39162   160.0532     1.0905     142.0   142.0                             
                         53199.40299   160.6171     1.6181     172.7   147.8                             
                         53200.41220   159.4821     1.7555     389.4   251.1                             
                         53207.41109   157.6318     2.4027     142.0   142.0                             
                         53208.36518   157.5593     2.1577     233.8   165.6                             
                         53215.32511   156.9988     3.2377     142.0   142.0                             
                         53221.38836   156.3834     3.9629     142.0   142.0                             
                         53228.29947   155.6012     5.6284     142.0   142.0                             
                         53229.29186   156.0978     6.1869     142.0   142.0                             
                         53233.24062   154.8590     5.5446     664.9   474.4                             
                         53234.26794   154.9441     6.3985     142.0   142.0                             
                         53235.27795   155.2394     7.0247     142.0   142.0                             
                         53236.24000   154.6541     7.2600     142.0   142.0                             
                         53249.22289   151.8710     8.8380     142.0   142.0                             
                         53270.22848   148.9036    11.8975     243.7   158.7                             
                         53285.23449   145.3500    13.9405     142.0   142.0                             
                         53313.10718   142.2377    18.5964     142.0   142.0                             
                         AB: Martin et al. (1998) derive component masses 1.561 +/- 0.197 and            
                         2.602 +/- 0.284 Msun.                                                   Mig1998 
                         Muterspaugh et al. (2008) combine PHASES astrometry with speckle and    Mut2008 
                         radial velocity data to derive orbits for both the AB and Ba,Bb pairs           
                         of this triple. The parallax is determined at 28.93 +/- 0.18 mas                
                         (distance 34.57 +/- 0.21 pc). Masses of the A, Ba, and Bb components            
                         are 1.533 +/- 0.050, 1.646 +/- 0.074, and 0.825 +/- 0.059 Msun.                 
             STF2824     AB,C (separation 14") has estimated 6200y period.                       Tok2006 
                         AB,C: H N  43.                                                          MEv2010 
                         AB,C: Additional notes may be found in Burnham (1894).                  Bu_1894 
21447+3332   GIC 170     G213-012/G213-013.                                                              
21449+6228   TRN  33     AC: The image rotator was in an unknown state, so two possible theta            
                         values are listed for the 2001.7364 observation - one for zenith up             
                         and one for north up.                                                   Trn2008 
21449-3302   I  1051     iot PsA = 9 PsA. A is a spectroscopic binary. Some doubt as to the              
                         reality of the companion.                                                       
21452+8554   A   775     There is uncertainty due to the high declination, but A   775 appears           
                         to be the same pair as 21416+8555 LDS1959. Systems merged. The pair             
                         21415+8555 TDT3110 has similar separation, but a much different                 
                         position angle.                                                                 
21456+2709   MLB1050     J  2357.                                                                        
21458+1545   STTA224     B is BD+15@4492.                                                                
                         Pair appears in an appendix list, not part of the discoverer's regular          
                         numbering sequence.                                                             
21459+1153   A  1223     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.65 +/- 1.92, 2.54, and 1.05 Msun, respectively.  Mlk2012 
21459-8247   R   334     This may be the new pair TDT3070 with an unusually large error by       Dam2013 
                         Russell.                                                                        
21461+2855   BRT  58     J 2598.                                                                         
21465+0635   UC 4556     aka ITF  69.                                                                    
21466-5742   FIN 283     Soderhjelm feels that there is a probable secondary sub-system. Speckle Sod1999 
                         and spectroscopic observations needed.                                          
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.42 +/- 0.77, 1.27, and 0.60 Msun, respectively.             Mlk2012 
21467-0010   BNG   2     Burningham et al. (2009) determine that ULAS J214638.83-001038.7 is a   Bng2009 
                         CPM companion to the high proper motion M4 dwarf Wolf 940. Spectral             
                         type of the companion is T8.5 +/- 0.5. Given the distance to Wolf 940           
                         = 12.50 +0.75/-0.67 pc, the 32" angular separation corresponds to a             
                         projected separation of 400 +/- 22 au. Mass of the companion is 20-32           
                         Mjup, Teff 570 +/- 25K, radius 0.094 +/- 0.004 Rsun. Observations               
                         using Keck laser guide star AO indicated no evidence of any close               
                         companion to the T8 companion. JHK photometry of the primary is from            
                         2MASS.                                                                  TMA2003 
21468+4919   MIU   3     pi 2 Cyg = 81 Cyg. Spectroscopic binary, P = 72d.                               
21470-1608   HJ 3056     del Cap = 49 Cap = Deneb Algedi. A is an Algol-type eclipsing binary,           
                         and is also an occultation double.                                              
21472+5310   GIC 171     G232-035/G232-034.                                                              
21472+2648   HJ  943     Not found by Heintz.                                                    Hei1995 
21475+1352   BPM2406     [PM2000] 2534610 + [PM2000] 2534626.                                    Gvr2010 
21476+1116   BPM2407     [PM2000] 2534858 + [PM2000] 2534908.                                    Gvr2010 
21477+5942   HD 207538   The classification given in Mason et al. (1998) is from Conti et al.    Msn1998a
                         (1977).                                                                 Cti1977 
21477-1813   CHR 223     First detected as an occultation binary by Evans et al.                 Evn1985 
21477-3054   FIN 330     the PsA = 10 PsA                                                                
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 5.52 +/- 1.62, 5.30, and 2.09 Msun, respectively.  Mlk2012 
                         AB: Docobo & Andrade (2013) derive a dynamical parallax of 11.17 +/-            
                         0.41 mas and component masses 2.32 +/- 0.33 and 2.32 +/- 0.33 Msun.             
                         See paper for extensive notes on this system.                           Doc2013d
21477-7759   LDS6362     Spectrum M?                                                                     
21479+3306   OSO 157     G214-001. Based on astrometry and color, AB comprises the only common           
                         proper motion pair in this system                                       Oso2004 
21479+1824   BPM2409     [PM2000] 2535246 + [PM2000] 2535118.                                    Gvr2010 
21479+1136   BPM2408     [PM2000] 2535182 + [PM2000] 2535291.                                    Gvr2010 
21479-7414   HJ 5287     WFC 237.                                                                        
21480-4736   LDS 755     Bresciano (2012) noted a factor of 10 error noted in Luyten's (1941)    Luy1941 
                         published separation.                                                   Bsc2012 
21483+0518   BRT2294     BAL 2982.                                                                       
21483-3742   B   538     All plates overexposed.                                                 Vou1947a
21483-4718   BSO  15     B is CD-47@13929.                                                               
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
21484-5446   RST1109     A is the Beta Lyrae-type variable RU Ind.                                       
21485+6137   D    33     Aka MLB 176 and FOX 99. Identity with Milburn pair first noted by Clif          
                         Ashcraft.                                                                       
21491+6648   STF2836     A is a spectroscopic binary, P = 2.73d.                                         
21492+2256   LDS4910     LDS4911.                                                                        
21492+0543   GIC 172     G093-040/G093-041 = GJ 838.1AB.                                                 
21492-4133   WTR   1     Rectilinear solution by Miles & Mason (2016)                            Msn2016b
                         and Mason et al. (2018).                                                Msn2018a
21494+3045   STF2829     B is BD+30@4538.                                                                
21494-4759   SKF1175     The photometry implies a red companion. This wide companion cannot              
                         explain the acceleration.                                               Tok2013b
                         A is possibly an astrometric binary (Makarov & Kaplan 2005).            Mkr2005 
                         The estimated period of the visual pair is about 4k yr. However, the A  Tok2020h
                         component also has a close spectroscopic companion with P ~470d.                
21495+5834   STI2588     STI 2588a.                                                                      
21495-3749   LDS5927     LDS6363.                                                                        
21496-0208   BAL 266     J  3349.                                                                Nsn2016 
21499-2509   B   540     Measures uncertain, too close. Needs speckle.                                   
21500-2127   LDS4913     NLTT 52199/52196                                                        Chm2004 
21500-6319   RST9009     Previously known as RST1110a.                                                   
21501+1717   COU  14     13 Peg. A possible Delta Scuti-type variable. According to Tamazian             
                         et al. secondary is a T Tauri-type variable.                            Tam1999 
                         Calculated mass sum is 2.65 +/- 0.21 Msun.  Spectral classification is          
                         a pair of early F giant or subgiant stars, but this mass sum is more            
                         consistent with dwarfs.                                                 Mut2010b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.56 +/- 0.14, 2.19, and 1.51 Msun, respectively.             Mlk2012 
21501-3837   TOK  36     Confirmed as physical pair by 2nd epoch observation and J-K color.              
                         Primary is 4.9d SB. Estimated period of visual pair 900 y.              Tok2006 
21502+7146   A  1225     Aitken could not find the pair described as HJ 3067,                            
                         allegedly occupying this position.                                              
21503-7521   FAH   2     A : Teff = 2118 +/- 62, M = 72 +/- 12 \mjup, R = 1.03 +/- 0.06 \rjup.   Fah2020 
                         B : Teff =  719 +/- 61, M = 34 +/- 22 \mjup, R = 0.95 +/- 0.16 \rjup.           
21506+6024   STI1059     One deg error in WDS designation.                                               
21506+2216   HO  467     Different proper motion. Despite having an orbit,                       Izm2019 
                         an optical pair based on parallax.                                      Mlk2022 
21509-4052   CRU   2     AB = LDS 757.                                                                   
21509-8243   HJ 5278     lam Oct = 10 Oph                                                                
21510+2911   A   889     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.04 +/- 0.47, 1.76, and 0.85 Msun, respectively.             Mlk2012 
21511+6650   HU  972     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 7.17 +/- 3.71, 2.43, and 1.19 Msun, respectively.             Mlk2012 
21512+0321   J  1724     BAL 2059.                                                                       
21515+1806   GIC 173     G126-039.                                                                       
21516+6545   STF2843     AB: Absolute quadrant determined by triple-correlation techniques       Pru2002b
21516+1950   HJ  947     AB: H N  74.                                                            MEv2010 
21518+6453   STF2844     Also known as STI1054.                                                          
21519+4221   HO  172     AD: See ADS for rectangular measures.                                           
                         AD: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
21520+5548   STF2840     A is a spectroscopic binary. B is BD+55@2638.                                   
                         Spectrum A1pSi.                                                                 
                         AB: H 4  79.                                                            MEv2010 
21520+3653   TDT3202     AC: Originally 21520+3652 TDT3202, but share common primary with                
                         21520+3653J  3149, so systems merged.                                           
21521+0739   OSO 158     G093-047. Neither is a common proper motion pair, based on color and            
                         comparison with POSS2 red plates                                        Oso2004 
21522+3252   ES 2321     Aka DOO  88.                                                                    
21524+0938   RED  18     2MASS J21522609+0937575. Spectral types L6: and L6:                     Red2006b
21524+0623   SKF1871     Typographical error in initial WDS designation (21524+0829).                    
21526+3841   MLB 991     ALI 981.                                                                        
21527+1650   BPM2410     [PM2000] 2542347 + [PM2000] 2542248.                                    Gvr2010 
21529-7454   HJ 5295     B is CPD-75@1735.                                                               
21530+2939   BRT  59     This is the same as MLB 494.                                                    
21531+6806   STTA226     BD. Pair initially listed as AD in WDS, but no star of appropriate              
                         magnitude at quoted separation and angle from A. GSC2.3 N1G0000360              
                         appears to be reasonable match in rho and theta (measured from B) and           
                         magnitude, however.                                                             
21532+4324   GRV 517     B component is +42 4236.                                                        
21532+3205   ES 2322     Espin (1928) gives a measure of the pair now designated DE, with the    Es_1928 
                         note "Forms distant comes to B.D. +31 4569, which star has at P. 80deg          
                         an 11.5 nearer, with a 14 mag. S.F." The note is perhaps garbled, as            
                         there is no obvious companion in this system at an angle of 80deg. The          
                         value "11.5" was taken as a separation, but is perhaps more likely a            
                         magnitude. If Espin meant to quote a position angle of 50deg rather             
                         than 80deg, the 11.5 and 14. mag stars may refer to the pair now                
                         designated BC.                                                                  
21534-1411   RST4092     Spectrum: Fm Delta Del.                                                         
21535+5417   BU  841     Perhaps HJ 3066.                                                                
21536+3551   OSO 159     G188-029. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates.                                                  Oso2004 
21536-1019   FIN 358     Also an occultation double.                                                     
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 15.09 +/- 14.75, 8.38, and 2.57 Msun, respectively.           Mlk2012 
21538+6237   S   800     A is the Beta Lyrae-type system EM Cep, P = 0.81d.                              
                         Spectrum B0.5V+b1Ve. B is BD+61@2217, spectrum B1III/V.                         
21538-2000   BU  168     A,BC: Aka HDO 168.                                                              
             HU  380     BC: A premature orbit has been computed.                                        
21539+2821   GC 30661    Hipparcos astrometric solution assumes circular orbit (e = omega = 0).  HIP1997d
21540-8036   HJ 5289     B is CPD-81@978.                                                                
21541+1346   BPM2411     [PM2000] 2544365 + [PM2000] 2544356.                                    Gvr2010 
21541-0117   FAR  50     GJ 4236 = NLTT 52377. Primary is white dwarf WD 2151-015.               Far2006 
21541-1710   HIP 108095  NICI images contain a hint of faint companion at ~280deg, 0".12, not            
                         accepted as real.                                                       Tok2012a
21542+0459   OSO 160     G018-005. Neither is a common proper motion pair, based on color or             
                         comparison with POSS2 red plates                                        Oso2004 
21543+1943   STF2841     A,BC: H N  14.                                                          MEv2010 
21543-3957   HJ 5299     B is CD-40@14544.                                                               
21544+1427   BPM2412     [PM2000] 2544898 + [PM2000] 2545037.                                    Gvr2010 
21546-0318   STF2838     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
21549+6159   OSO 161     G264-015. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
21550-1158   HJ  616     Also known as STF2839.                                                          
21552-6153   HDO 296     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.69 +/- 0.39, 2.32, and 1.64 Msun, respectively.  Mlk2012 
             SHY 348     AD: HIP 108195 + HIP 107947.                                                    
                         Also known as CAB   7.                                                  Cab2011 
             SHY 348     AE: HIP 108195 + HIP 107345.                                                    
             SHY 347     DE: HIP 107947 + HIP 107345.                                                    
21553+3239   OSO 162     G188-030. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates.                                                  Oso2004 
21554+5938   JNN 292     Estimated age 30-300 Myr; masses 0.14 +/- 0.07 and 0.09 +/- 0.05 Msun;          
                         a ~2.7 au.                                                              Jnn2014 
21554+5608   OSO 163     G232-040. Neither is a common proper motion pair.                       Oso2004 
21555+2942   HO  609     Pair is much fainter than given in the ADS; hence the discordant                
                         separations. Three faint stars are in the field, two south following,           
                         one north preceding.                                                    B__1963a
21555+1053   BU   75     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.87 +/- 0.60, 2.05, and 0.95 Msun, respectively.  Mlk2012 
21556+3849   A  1449     Baize (1982) orbit rejected from Fourth Orbit Catalog                   Baz1982 
                         ("rescinded by author; omitted from publication")                       Wor1983 
21556+3505   SEI1544     Hipparcos suspected non-single.                                                 
21557+1752   BPM2413     [PM2000] 2546920 + [PM2000] 2546869.                                    Gvr2010 
21558+3716   HO  174     Schembor measures a companion he calls C. 1925.57, 109.5@, 89.74".      Sch1927b
                         CD: Also known as ALI 445.                                                      
21559+3141   ES 2360     BRT 290.                                                                Brt1929b
                         The primary is a spectroscopic binary, P = 6.48d.                               
                         Very different parallax. Despite having an orbit,                       Izm2019 
                         an optical pair based on parallax.                                      Mlk2022 
21560-4234   HJ 5303     B is CD-43@14793.                                                               
21563+7321   MLB 427     LDS1963.                                                                        
21563+1604   BPM2414     [PM2000] 2547721 + [PM2000] 2547747.                                    Gvr2010 
21564+3156   HJ 1707     B is a spectroscopic binary, P = 15.95d.                                        
21565-4102   HJ 5305     A is CPD-41@9730, and B is CPD-41@9729.                                         
21567+6338   WRH  36     zeta Aurigae-type binary VV Cep. Visual duplicity uncertain.                    
                         Spectrum of the eclipsing pair composite; M21aep+B8Ve.                          
                         Fredrick orbit rejected from Fourth Orbit Catalog                       Frd1960 
                         ("amplitude below noise level")                                         Wor1983 
21567+1607   STT 455     Mt. Wilson spectral classes are F5 and G5.                                      
21567+1335   BPM2415     [PM2000] 2548460 + [PM2000] 2548269.                                    Gvr2010 
21568+3125   BRT 291     Not found by Heintz.                                                    Hei1995 
                         A likely plate flaw.                                                    Grv2021b
21575+2856   LEP 104     NI   42.                                                                        
21575+0409   STTA225     B is BD+03@4639.                                                                
21576+1157   STTA227     B is BD+11@4701.                                                                
21577+1629   BPM2416     [PM2000] 2549795 + [PM2000] 2549712.                                    Gvr2010 
21577-5059   LDS 765     LDS5938.                                                                        
21578-1507   HJ 3071     H N 131.                                                                        
21579+6101   MLR  17     Primary is the Cepheid IR Cep.                                          Evs2016a
21579-4327   LDS 766     Spectrum of A is DA. Spectrum of B M?                                           
21579-5500   FIN 307     del Ind.                                                                        
                         Finsen called attention to quasi-periodic residuals in position                 
                         angle which neither of the alternative orbits explains.                         
                         Illustrative solutions with useable astrometric mass-ratios. Short-P            
                         solution marginally better, but indeterminate with strong element-              
                         correlations. Probably giant primary, more speckle-data needed.         Sod1999 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 5.24 +/- 0.83, 3.26, and 1.58 Msun, respectively.             Mlk2012 
                         Docobo & Andrade (2013) derive a dynamical parallax of 22.71 +/- 0.69           
                         mas and component masses 1.78 +/- 0.21 and 1.33 +/- 0.16 Msun. See              
                         paper for extensive notes on this system.                               Doc2013d
21580+0556   STF2848     H 3  74.                                                                MEv2010 
21581+1541   BPM2417     [PM2000] 2550355 + [PM2000] 2550535.                                    Gvr2010 
21582+8252   STF2873     LDS1965.  B is BD+82@674.                                                       
                         B comp is 1.2d eclipsing SB2 V376 Cep. Estimated period of AB 7300y.    Tok2006 
                         AB: HJL 298.                                                            HJL1986 
                         AB: A is SB1 (CfA: P=8165d = 22.35y), astrometric binary (Gorshamov et  PkO2006b
                         al. 2006, P=23y), and X-ray source. B is SB2E, P=1.152d                 Tok2014d
                         Aa,Ab : M_Aa = 1.10 +/- 0.07 \msun, M_Ab = 0.59 +/- 0.07 \msun.         PkO2024 
21582-2315   LDS4928     NLTT 52553/52552                                                        Chm2004 
21584+4423   LYS  11     The pair previously listed as 22003+4423SMA 156 was found to be this            
                         pair as well. It is actually identified as SMA 143 in the original      Sma1931 
                         publication. The null detection of SMA 156 was therefore, at the        ACA2007 
                         wrong location. Solution to the quandry determined by Wayne Osborn.             
21584-1834   SEE 463     Misidentified in BDS as BD-19@6197.                                             
21585+0347   RAO  73     A is SB1, P=7.184y                                                      Tok2014d
                         A single-lined AB with P = 7.18 yr (Nidever et al. 2002) and a large    Nid2002 
                         PM of 0".28/y. The distant component B at 12".3 is confirmed as                 
                         physical by 2MASS, Robo-AO, and this work. It is located slightly               
                         below the MS, just like HIP 104514B. The object is also metal-                  
                         deficient relative to the Sun, [Fe/H] = (Zielke 1970 A&A 6, 206).       Rbr2015d
21585-5901   kap 1 Ind   Hipparcos astrometric solution assumes circular orbit (e = omega = 0).  HIP1997d
21586+0601   SHJ 336     B is BD+05@4913.                                                                
21589-0422   LDS4931     NLTT 52596/52593                                                        Chm2004 
21589-1115   HJ 3075     J 1412.                                                                         
21589-3227   LDS4929     Also known as LHS3739/8. Parallax = 50.92 +/- 0.77 mas.                 TSN2010 
21592+7311   BU 1509     16 Cep.                                                                         
21592+4102   OSO 164     G214-005. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
21592-3556   LDS 768     LDS5940.                                                                        
21593-3110   BRT3104     A likely plate flaw.                                                    Grv2021b
21594-1012   LEO  51     J 2362.                                                                         
21595+0617   HJ 3079     AG  279.                                                                        
21597+4907   HU  774     Ambiguous case, although only one solution has been tested.                     
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 9.18 +/- 5.22, 5.27, and 2.24 Msun, respectively.             Mlk2012 
21598+2356   STF2850     A is an irregular variable.                                                     
21599+5928   STI1078     SMA 155.                                                                        
22000-3039   BUG   6     DENIS J220002.05-303832.9                                                       
                         Serendipitously discovered with SpeX near-IR imager/spectrograph.               
                         Spectral types M9 + L0, masses 0.072-0.085 and 0.069-0.083 Msun.        Bug2006b
22001+2909   BRT  60     The pair MLB 496 is identical                                           Hei1980a
22002+0822   OSO 165     G018-012. Not a common proper motion pair, based on color               Oso2004 
22003-0724   LDS4935     NLTT 52648/52649                                                        Chm2004 
22007-5002   I  1450     Heintz (1984) value of omega was corrected from 313.5 to 133.5          Hei1984a
                         degrees by Ruymaekers & Nys (1985).                                     Ruy1995 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 8.36 +/- 8.51, 1.75, and 1.05 Msun, respectively.             Mlk2012 
                         Gomez et al. (2016) derive dynamical parallax and component masses:             
                         14.88 +/- 0.61 mas, 0.825 +/- 0.016 Msun, 0.778 +/- 0.015 Msun.         Doc2016i
22008-2827   BU  276     eta PsA = 12 PsA. Bidelman calls A a spectroscopic binary, and says a           
                         1972 plate shows a fairly strong H-alpha self-reversal.                         
22010+1626   BPM2418     [PM2000] 2554557 + [PM2000] 2554441.                                    Gvr2010 
22010+1116   BPM2419     [PM2000] 2554645 + [PM2000] 2554572.                                    Gvr2010 
22011+3915   A  1451     Usually too close for visual measures. Needs speckle.                           
                         AB,C: Possibly a 30" error in the declination of the secondary led to   Sei1908 
                         the erroneous 1894 Scheiner (1908) and WFC measures.                    WFC1998 
22011+1307   HJ  289     20 Peg.                                                                         
22013+4621   HJ 1714     B is BD+45@3762.                                                                
22015+0310   J  1726     BAL 2060.                                                                       
22015-1537   HWE  59     The fainter star is apparently BD-16@5997.                                      
22016+4921   ES  831     AD: Rectilinear solution by Hartkopf & Mason (2015).                    WSI2015 
                         AE: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
22017-0925   JNN 135     The two components of the 2MASS J22014336-0925139 system that have              
                         been resolved with AstraLux have very similar brightnesses and colors,          
                         and it is therefore likely that they form a physical binary pair.               
                         Common proper motion has not yet been demonstrated.                     Jnn2012 
22017-1200   STF2851     Spectrum: G8/K0III/IV. B is BD-12@6153.                                         
22018-0952   RST4095     Position angles discordant in 1950. 220@, 5 nights.                             
22019+5506   HJ 1718     AB: HJ 1719 = STI2607. Burnham's note for HJ 1719 quotes Herschel as    Bu_1906 
                         mentioning "a third star 12m from B, 4arcsec; also a fourth." Burnham           
                         also says "The other stars referred to are 12.5m, 268.2deg:                     
                         15.9arcsec; and 12.0m, 145.4deg: 30.9arcsec." These appear to match             
                         the BC, AC, and AE pairs in the HJ 1718 mutiple system. We therefore            
                         conclude that HJ 1719AB and HJ 1718AB are the same pair.                        
22019+1407   BPM2420     [PM2000] 2555948 + [PM2000] 2555937.                                    Gvr2010 
22019+0446   STTA228     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
22021+5800   TRN  34     14 Cep = LZ Cep.                                                                
                         The image rotator was in an unknown state, so two possible theta                
                         values are listed for the 2001.7341 observation - one for zenith up             
                         and one for north up.                                                   Trn2008 
                         The classification is from Conti & Alschuler (1971). Radial velocity    Cti1971 
                         and light curve solutions are given by Harries et al. (1998 MNRAS 295,          
                         386).                                                                   Msn1998a
22024-1658   S   802     29 Aqr. A is the Beta Lyrae-type system DX Aqr.                                 
                         A orange, B white. The spectral type A2 given in the ADS must be the            
                         companion's.                                                            B__1963a
22025-7719   SHY 786     BC: HIP 108799 + HIP 103587.                                                    
22027+1110   BPM2421     [PM2000] 2557008 + [PM2000] 2557200.                                    Gvr2010 
22028+1207   GIC 174     G018-017/G018-018.                                                              
                         NLTT 52768/52770                                                        Chm2004 
22029+4439   BU  694     A is variable, V1942 Cyg.                                                       
22029+1547   HDS3129     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.67 +/- 0.75, 2.80, and 1.25 Msun, respectively.             Mlk2012 
22029+1511   BPM2422     [PM2000] 2557327 + [PM2000] 2557452.                                    Gvr2010 
22031-7607   HJ 5306     A is a spectroscopic binary.                                                    
22032+5937   WNO  48     BC: Identified as WNO  18 in USN1976.                                           
22032+0157   ARG  96     BAL 1594.                                                                       
                         HJL 299.                                                                HJL1986 
22032-0113   OSO 166     G027-008.                                                                       
             LDS4938     AB: NLTT 52787/52786                                                    Chm2004 
22033+5944   STI1083     Also known as SMA 160.                                                          
22033-4816   CPO  90     Aka SKF1179.                                                            Dam2015b
22034+3634   DAM 662     Identified by Damm as ALI 450, but apparently a different system.       Dam2013 
22034-5647   VLK   1     Ba,Bb: eps Ind. Cardoso et al. (2009) derive a system mass of                   
                         0.116 +/- 0.001 Msun = 121 +/- 1 Mjup for this pair of T dwarfs.        Mcg2009 
                         VLTI uniform disk diameter of A:       1.834 +/- 0.016 mas,             LTI2009 
                         VLTI limb-darkened disk diameter of A: 1.881 +/- 0.017 mas,                     
                         R = 0.732 +/- 0.006 \rsun, Teff = 4568 +/-  59 K,                               
                         M = 0.762 +/- 0.038 \msun.                                                      
                         Mass for Ba & Bb : 75.0 +/- 0.82 and 70.1 +/- 0.68 \mjup.               Die2018 
                         Teff for Ba & Bb : 1320 and 910 K.                                              
                         The orbital parallax is 276.88 +/- 0.81 mas.                                    
22035+4841   ES  530     Includes V394 Lac, a Beta Lyr type eclipsing binary, P = 1.65000d.      Zas2012 
22035+0340   JNN 293     Estimated age 1000-10000 Myr; masses 0.24 +/- 0.10 and 0.13 +/- 0.04            
                         Msun; a ~6.8 au.                                                        Jnn2014 
22036+1108   BPM2423     [PM2000] 2558304 + [PM2000] 2558485.                                    Gvr2010 
22037+0318   HJ  952     BAL 2062.                                                                       
22038+6438   MCA  69     xi Cep = 17 Cep = Kurhah                                                        
                         Aa,Ab is an astrometric binary and SB2, with elements by Vickers &      Scf1976 
                         Combined solution by Farrington et al. (2014) yields masses 1.045 +/-           
                         0.032 and 0.409 +/- 0.066 Msun, as well as an orbital parallax 38.11            
                         +/- 2.82 mas.                                                           CIA2014a
             STF2863     Scarfe (1976). The McAlister (1980) orbit is from speckle               McA1980a
             xi Cep      interferometry, and in good agreement with the spectroscopic result.            
                         Mt. Wilson spectrum of B F8s. Spectrum of A: A3m.                               
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
             STF2863     AB: H 2  16.                                                            MEv2010 
22039+5949   STT 461     15 Cep.  STTA229.                                                               
                         EF: F is BD+59@2463.                                                            
                         E comp is V442 Cep, a Beta Lyr type eclipsing binary, P = 2.12919d.     Zas2012 
22039+2406   J  1246AB   POU5624.                                                                        
22039-2451   LDS6378     AC: 22039-2451 found to be same system as 22038-2450. LDS4939AB merged          
                         with LDS6378AC, LDS4939AC changed to AD.                                        
22041+7328   MLR 255     No significant movement since first resolution.                         Drd2009 
22042+3804   FYM 296     Aka CVE  13.                                                                    
22042+3507   SEI1554     A is the Mira-type variable RT Peg.                                             
22043+2401   J  1224     BC : assumed to be equivalent with the former GCB  63.                  Cgl2024a
                         First known suggestion of this identity was Berko.                      Bko2010b
22043+1720   BPM2424     [PM2000] 2559313 + [PM2000] 2559495.                                    Gvr2010 
22044+2500   POU5629     LDS1488.                                                                        
22045+2915   GRV 539     AC: Also known as GRV 538AB.                                                    
22045+1551   BU  696     AC and AE: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         CE: The previous AD pair was determined to actually be CE by Arnold.    Arn2008a
22046+3854   SEI1556     ALI 983.                                                                        
22046+1122   OSO 167     G018-021. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
22048+3637   ALI 450     No star seen at AC catalog location of the purported secondary                  
                         - probably a plate flaw. Triple identified by Damm as matching ALI 450  Dam2013 
                         moved to 22034+3634.                                                            
22049+2158   GAU  18     Measured for HJ 3089 which Gauchet could not find.                      Gau1926a
22050+1223   BPM2425     [PM2000] 2560281 + [PM2000] 2560265.                                    Gvr2010 
22050+1130   HJ  290      Erroneously merged with 22050+1128HJ  291. Corrected.                  Cur2018 
22050+0838   OSO 168     G018-024. AB is not a common proper motion pair, based on comparison            
                         with POSS2 red plates.                                                  Oso2004 
             LDS4942     See Allen et al. (2000) for information on metallicity, age,            AlC2000 
                         galactic orbital parameters, etc.                                               
22051+6217   BU  697     19 Cep.                                                                         
             TRN  35     AD and AE: The image rotator was in an unknown state, so two possible           
                         theta values are listed for the 2001.7367 observation - one for                 
                         zenith up and one for north up.                                         Trn2008 
22052+5502   STI2612     Primary appears to be typos or plate flaw in AC catalog.                        
22052+4403   HJ 1723     AB: Also known as LYS  19 and FAL  73.                                          
22053-0125   STF2855     B is BD-02@5688.                                                                
22056+3620   TOB 224     Two 2010 measures of SEI1558 by Azcona et al. (2011) were actually of           
                         this pair.                                                              SDA2011 
22057+1223   HIP 109067  NLTT 52896. The 4.6 yr SB1 with estimated q > 0.23 and axis 53 mas is           
                         below the NICI detection limit. This is a sub-dwarf with large PM,              
                         below the main sequence.                                                Tok2012a
22058+3618   SEI1558     Secondary not seen on Aladin; apparently either a typographical error           
                         or a plate flaw in the AC Catalog.                                              
22058+3059   ES 2361     SMA.                                                                            
22058+0452   STF2856     BDS 11412 probably same star with error in position.                            
                         WHC  25.                                                                        
22058-0019   BUP 232     alp Aqr = 34 Aqr = Sadalmelik                                                   
                         Mk III Limb-darkened diameter  3.20  +/- 0.05  mas.                     MkT2001 
                         Mk III Limb-darkened diameter  3.237 +/- 0.057 mas.                     MkT2003 
                         NPOI Limb-darkened diameter    3.08  +/- 0.03  mas,                     NOI1999 
                         R = 77.  +/- 15. \rsun.                                                         
                         NPOI Limb-darkened diameter    3.11  +/- 0.04  mas.                     NOI2001b
                         Common proper motion pair with 21316-0534 = bet Aqr.                    Skf2013 
22059+4135   ES 1586     Aka DOO  90.                                                            Dam2016b
22059+3330   PLT   7     A is RZ Peg, B is RY Peg.                                               Plt1934 
22059-1155   WNO  57     GJ 4254 + LP 759-25. CPM pair.                                          Mkr2008 
22061+4159   A   407     An 11th magnitude star at 058@, 13".                                            
22061+1623   BPM2426     [PM2000] 2561783 + [PM2000] 2561926.                                    Gvr2010 
22061-0521   TOK 373     SB with preliminary 13y period (CfA) and expected semi-major axis of            
                         0".19 is tentatively resolved here for the first time at 0".07 and              
                         dK=1.7. Strangely, it was not resolved previously be speckle or AO.             
                         This is the young BY Dra variable NT Aqr and an X-ray source.           Tok2013b
22064-2047   CLO   3     Assuming a parallactic distance of 26.67 +/- 2.63 pc (Costa et al.      Jao2006 
                         2006), Konopacky et al. (2010) derive system mass 0.16 +/- 0.05 Msun.   Kon2010 
                         Dupuy et al. (2009) also reprocessed the HST/WFPC2 data originally              
                         published by Bouy et al. (2003), as well as the Gemini/Hokupa'a data    Boy2003 
                         originally published by Close et al. (2002). From their orbital         Clo2002a
                         solution they derive a total system mass of 0.15 +0.05/-0.03 Msun.              
                         Spectral types appear to be M8.0 +/- 0.5 for both components. Distance          
                         is estimated at 26.7 +2.6/-2.1 pc.                                      Dup2009b
22066+1416   HEI 293     TDT3346.                                                                        
22067-4913   RSS 566     Also known as ENO   7.                                                          
22068+7058   HJ 3096     LDS1968.                                                                        
22068+1444   BPM2427     [PM2000] 2562714 + [PM2000] 2562648.                                    Gvr2010 
22069+6405   WYL   1     Not found by Heintz at 22093+6401. This has been equated with TDT3347.  Hei1987a
22069+4752   ES 2715     B is BD+47@3694.                                                                
22069+1807   BPM2429     [PM2000] 2562935 + [PM2000] 2563110.                                    Gvr2010 
22069+1313   BPM2428     [PM2000] 2562917 + [PM2000] 2562751.                                    Gvr2010 
22070+5930   OSO 169     G232-056. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
22070+2521   STT 596     iot Peg = 24 Peg. The primary is a spectroscopic binary.                        
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
             PTI   1     SB2. Combined solution by Boden et al. (1999), including visibilities   Bod1999a
                         from the Palomar Testbed Interferometer, plus spectroscopy. Authors             
                         give two very similar solutions, made using two data sets. Values were          
                         averaged in the orbit catalog.                                                  
                         See also discussion of iot Peg system by Morel et al. (2000).           Mrl2000 
                         Combined spectroscopic/astrometric solution, based on high-resolution           
                         echelle spectra plus archival PTI visibility measurements.                      
                         Derived masses 1.33249 +/- 0.00086 and 0.83050 +/-0.00055 Msun,                 
                         distance 11.534 +/- 0.019 pc.                                           Knc2010 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.27 +/- 4.55, 2.36, and 1.20 Msun, respectively.             Mlk2012 
22071-5908   HJ 5316     Spectrum: G8/K1V+F/G.                                                           
                         A=SB? No SB orbit. B at 3.3" is above MS, suspicious ptm in 2MASS.      Tok2014d
22072+3555   SEI1559     ALI 223. GYL  94.                                                               
22075+3841   MLB 792     J 3158.                                                                         
22075+2538   A   308     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.93 +/- 2.45, 3.66, and 2.09 Msun, respectively.             Mlk2012 
22077+0913   HJ 3090     J  1792. Not found by Heintz at IDS position.                           Hei1990b
22082+2921   ALP  27     2MASSW J2208136+292121                                                          
                         Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
22082+1645   BPM2430     [PM2000] 2564634 + [PM2000] 2564663.                                    Gvr2010 
22082-4658   RST5483     alp Gru = Alnair. Not seen by Holden on four nights 1963-1969.                  
                         Intensity Interferometer Limb-darkened diameter 1.02 +/- 0.07 mas.      HBr1974 
22083+4913   ES  685     Primary is V401 Lac, an Algol-type eclipsing binary, P = 1.95012d.      Zas2012 
22083+2409   HDS3145     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.58 +/- 0.33, 2.86, and 1.00 Msun, respectively.             Mlk2012 
22084-3259   VSP  56     Mu PsA = 14 PsA.                                                                
22086+5917   STF2872     A,BC: H 4 126.                                                          MEv2010 
22088-2546   SEE 469     Previously known as HDS3147. Pair included in the BDS but               Bu_1906 
                         removed from the ADS and IDS. It matches the HDS observation            A__1932a
                         quite well.                                                             IDS1963A
22089+1539   BPM2431     [PM2000] 2565599 + [PM2000] 2565465.                                    Gvr2010 
22091-1831   BU  170     The wide pair in the field nf is HJ 3092.                               Bu_1906 
22092+3310   BU 1511     pi 1 Peg = 27 Peg                                                               
22093+6401   FOX  44     Aka TDT3369.                                                                    
22093+4451   HJ 1735     Primary is V402 Lac, an eccentric Algol-type eclipsing binary, period           
                         3.78202d. B is BD+44@4060.                                              Zas2011 
22093+1142   OSO 170     G126-056. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
22093-0755   KUI 111     LDS4947. NLTT 53061/53062                                               Chm2004 
22093-1859   HU  284     This is identical with HU, BDS 11518.                                   Doo1915a
22094+1730   BPM2432     [PM2000] 2566327 + [PM2000] 2566245.                                    Gvr2010 
22095+0542   HWE  61     BDS 11521. BU 842.                                                              
22095-0733   GJ 9769     Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from Marcy        CPS1999a
                         et al. (1999).                                                          HaI2001 
22095-1827   HJ 3092     B is BD-19@6231, spectrum A8/F0V.                                               
22100+1346   OL  222     OL  194.                                                                        
22102+6811   MLB 370     MLR 104.                                                                        
22102+0612   VSP  57     ten Peg = 26 Peg.                                                               
22102+0255   HJ  957     Aka BAL2063.                                                                    
22103+0137   HJ 5526     BAL 1597.                                                                       
22104+1925   BRT2527     J  2364.                                                                J__1962a
22104-0108   J  1727     BAL 628.                                                                        
22104-5158   TOK 216     Possibly triple. The 1".4 companion found with NICI cannot explain the          
                         RV variability and acceleration.                                        Tok2012a
22105+1228   BPM2433     [PM2000] 2567677 + [PM2000] 2567773.                                    Gvr2010 
22106+7008   STF2883     HJL 301.                                                                HJL1986 
                         H N 121.                                                                MEv2010 
22107+3322   GYL  73     TOB 226. No sign of a 5.9" pair, although AC2000 shows coordinates              
                         corresponding to this value. Apparently this is due to an error in the          
                         catalog coordinate, as the true declination of the B component is ~15"          
                         due north of the AC2000 coordinates for B.                                      
22108+2151   J  2365     BRT 2528.                                                                       
22109+5757   BU  436     Hough suspected a close companion, not confirmed.                               
22111+1624   BPM2434     [PM2000] 2568540 + [PM2000] 2568461.                                    Gvr2010 
22112+5049   HJ 1741     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
22115+5925   CIA  45     lam Cep.                                                                        
                         Radial velocities are also discussed by Gies & Bolton (1986) and        Gie1986 
                         Underhill (1995 ApJS 100, 433).                                         Msn1998a
22115+1806   CHR 119     Ross 270, G126-62.                                                              
             OSO 171     G126-062. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
22115+1731   HD210647    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin (1984).                                                         Grf1984b
22115-0114   BAL 629     Also known as STF2871.                                                          
22116+2716   HO  289     CD of ADS should probably read BD.                                              
22116+1803   OSO 172     G126-063. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates.                                                  Oso2004 
22116-3428   CHR 230     Aa,Ab: This new component to the visual pair Bu 769 has moved through           
                         more than 4 deg in about 10 months, implying a period of order 60 - 70          
                         years. The wide pair has shown essentially no change since its          Bu_1887 
                         discovery by Burnham in 1879, on the other hand.                        Hrt1996b
22117+0612   OSO 173     G018-035. AC is not a common proper motion pair, based on comparison            
                         with POSS2 red plates.                                                  Oso2004 
22117-5850   HJ 5317     B is CPD-59@7774.                                                               
22118+5944   STF2880     STT 466.                                                                        
                         H 1  49.                                                                MEv2010 
22118+5650   GIC 176     The C component is G233-002.                                                    
22119+6342   STI1097     Appears to be identical with 22122+6344 BU 1512. measures merged.               
                         Farman notes a 13th magnitude star in 355@.                             Frm1907 
22120+3739   STF2876     Same as STF2864.                                                                
22121+1245   BPM2435     [PM2000] 2569827 + [PM2000] 2569969.                                    Gvr2010 
22122+5909   MLR 439     No significant movement since first resolution.                         Drd2009 
22125+1749   BPMA255     [PM2000] 2570388 + [PM2000] 2570558.                                    Gvr2010 
22126+5253   ES  146     Identical with ROE 93. Heintz confirms the BD identity.                 Hei1983a
                         A measure 1902.89 is contained in a letter from Espin to Roe. The       Es_1903 
                         measure in BDS evidently belongs to another pair.                               
22129+7318   STF2893     Spectrum composite; K0II-III+A3V.                                               
                         H 4  82.                                                                MEv2010 
22129+4555   BUR   1     Measured by Burling (2005) on DSS plate and incorrectly identified as   Bur2005 
                         HJ 1723.                                                                        
22130-4733   CPO 630     LDS 775.                                                                        
22132+2148   HJ  958     HJL 302.                                                                HJL1986 
22132-1111   BU 1215     EPIC 206135267. Primary is eclipsing binary, period 2.533d.             SJR2016 
22133+2352   HJ 1744     POU 5668.                                                                       
22137+5636   SMA 162     Also known as STI2651.                                                          
22138+2445   POU5671     J   2705.                                                                       
22138-0627   LDS4949     NLTT 53254/53255                                                        Chm2004 
22139+3943   MCA  70     A is a spectroscopic binary. Uncertain whether MCA pair is the same.            
22139+1519   BPM2436     [PM2000] 2572221 + [PM2000] 2572211.                                    Gvr2010 
22143+1711   STF2877     AB: An optical pair. Measures of the BD                                 WFC1998 
                         pair from Urban et al., Burnham, Abetti,                                Bu_1913 
                         Opik, and 2MASS were originally                                         Abt1922 
                         erroneously labelled as measures of the                                 Opi1932 
                         BC pair.                                                                TMA2003 
22143-1109   BRT2792     J 3239.                                                                         
22143-2104   H N  56     41 Aqr. Spectrum composite; K0III+F2V.                                          
22144-0845   OSO 174     LHS 3780. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
22146+1728   BPM2437     [PM2000] 2573096 + [PM2000] 2573005.                                    Gvr2010 
22147+1249   BPM2438     [PM2000] 2573244 + [PM2000] 2573421.                                    Gvr2010 
22150+5703   ENG  84     23 Cep = eps Cep. A is a Delta Scuti-type variable.                             
                         B is BD+56@2744.                                                                
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             MWT   1     Aa,Ab: Candidate close companion to eps Cep is estimated to be of               
                         spectral type K8-M2, mass ~0.5 Msun, radius ~0.7 Rsun, temperature 3            
                         650K, age ~600 Myr. Distance from the primary >= 8.6au.                 Mwt2011 
22151+3500   RAO 476     pa error = 348 deg.                                                     RAO2020b
22152-0535   A  2599     The close pair previously cataloged as MSN   1 was an error. This was           
                         verified by the null detection of Hartkopf et al. and reinspection of   Hrt2009 
                         the original data.                                                      Msn1996b
22154+5104   ES 1113     Also known as WFC 239.                                                          
22155+3450   ES  214     Also known as J  3317.                                                          
22156+3811   ES 2530     Also known as ALI 700.                                                          
22156-4121   CHR 187     Abt & Biggs (1972) note variable RV.                                    AbH1972 
22157-1809   LDS4950     NLTT 53321/53320                                                        Chm2004 
22158+4354   POP  23     Erroneously listed as companions to 22156+4352COU1981 = BD+43 4164      Pal2005c
                         rather than +43 4165.                                                           
22159+5440   BU  377     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AQ = BU  377Ab.                                                                 
             GIC 177     AT = G232-061/G232-062 = GJ 4268A+4269B.                                        
             BU  377     AC, AD: Rectilinear solutions by Friedman et al. (2011).                USN2011a
22159+3125   BU  477     HJL 303.                                                                HJL1986 
22161+3521   J  1211     Van Biesbroeck corrects the position by reference to BD+34@4642.        VBs1954 
22161-0705   HDS3158     Cvetkovic et al. (2014) derive spectral types G4 and  K3, masses 1.07           
                         and 0.79 Msun. Dynamical parallax is 17.56 +/- 0.44 mas.                Cve2014 
                         A 111.1d spectroscopic solution for the B component has been found      Tok2018d
                         making this a triple system.                                                    
                         Synthetic Spectrum gives Bt mags of 12.19 & 14.02 for Ba,Bb and 11.12   Mda2019 
                         and 12.67 for Vt. The solution for the three components A, Ba and Bb            
                         Teff = 5836 +/- 80, 5115 +/- 80, and 4500 +/- 80, degrees Kelvin,               
                         R = 1.09 +/- 0.039, 0.596 +/- 0.05, and 0.49 +/- 0.06, \rsun,                   
                         L = 1.24 +/- 0.10, 0.22 +/- 0.09, and 0.09 +/- 0.05, \lsun,                     
                         M = 1.05 +/- 0.16, 0.83 +/- 0.16, and 0.67 +/- 0.16, \msun.                     
22162+4229   COU1830     TDT3433.                                                                        
22162+1145   BPM2439     [PM2000] 2575225 + [PM2000] 2575139.                                    Gvr2010 
22163+1736   BPM2440     [PM2000] 2575257 + [PM2000] 2575213.                                    Gvr2010 
22164+7321   LDS1975     NLTT 53440/53441.                                                               
22165+3708   SEI1561     ID uncertain - no sign of SEI pair, and ALADIN only indicates one               
                         Astrographic Catalog star in vicinity of Scheiner's coordinates.                
22166+0147   HJ 3102     BAL 1598.                                                                       
22166-5543   SYO   2     LDS 781. B is CPD-56@9854.                                                      
22168+1746   BPM2441     [PM2000] 2575955 + [PM2000] 2575968.                                    Gvr2010 
22169+1258   HJ  293     Also known as STF2888.                                                          
22172+1725   BRT1358     J  3350.                                                                Nsn2016 
22173-0042   STF2887     HJL 304.                                                                HJL1986 
22173-0847   LDS 782     AB: NLTT 53397/53398                                                    Chm2004 
                         This system counts as single in our statistics, even though it appears          
                         to be a triple system in reality. The reason for this is that the A             
                         component was the AstraLux target, and the BC pair at ~7.8" is outside          
                         of the completeness cut-off at 6". Since the BC pair is visible in the          
                         AstraLux images, we can nonetheless analyze it astrometrically. This            
                         pair was first reported by Beuzit et al. (2004) with rho = 0.978" and           
                         theta = 305.8deg. There are no error bars quoted, but if we assume              
                         that the quoted precision in decimal places corresponds to measurement          
                         precision, and adopt errors of 5 mas and 0.5deg, which should be                
                         conservative in that circumstance, we find that common proper motion            
                         can be confirmed at a 76 sigma confidence level. Hence, physical                
                         companionship can be confidently inferred, even if the errors should            
                         be substantially larger than what we have assumed.                      Jnn2012 
22174+1309   BPM2442     [PM2000] 2576735 + [PM2000] 2576704.                                    Gvr2010 
22174-0102   BAL 631     The secondary in the original measure appears to be either a                    
                         typographical error or a plate flaw.                                            
22175+2335   GIC 179     G127-013/G127-014.                                                              
22175-2342   HJ 5324     LDS4954.                                                                        
                         NLTT 53404/53403                                                        Chm2004 
                         WHC  27.                                                                        
22180-6249   I    20     Ling (2004) derived an orbital parallax 0".00741 and a  mass sum of     Lin2004a
                         3.68 +/- 5.03 Msun.                                                             
22181+1126   BPM2443     [PM2000] 2577549 + [PM2000] 2577478.                                    Gvr2010 
22181-0014   CHR 107     This system, first announced by McAlister and recalled in a later       McA1984b
                         McAlister paper after repeated attempts at confirmation, has been       McA1993 
                         restored. While perhaps still spurious, the subsequent confirmation or          
                         suspected duplicity (by another technique) makes the discovery                  
                         measurement somewhat more probable.                                             
22182+1414   BPM2444     [PM2000] 2577654 + [PM2000] 2577722.                                    Gvr2010 
22182-6300   LTT18565    Hipparcos astrometric solution assumes circular orbit (e = omega = 0).  HIP1997d
22185+6313   STF2896     B is BD+62@2060.                                                                
22186+0827   OSO 175     G018-039. Not a common proper motion pair, based on color and                   
                         comparison with POSS2 red plates.                                       Oso2004 
22186-6014   alp Tuc     Elements P, T, e in the astrometric solution of Alden (1939) were       Ald1939a
                         taken from the spectroscopic orbit by Spencer Jones.                            
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Alden (1939).                                                           Ald1939a
22187-4954   I   303     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
22189+3746   STF2894     AB: HJL 305.                                                            HJL1986 
                         AB: H 3  17.                                                            MEv2010 
22191+5607   A  1461     One component is the Beta Lyrae-type system GP Cep.                             
22193+6319   WGT   4     Only quadrants were listed in the paper; position angles were                   
                         estimated from their figure.                                                    
                         Components D, E, F, and G are IR point-like sources near the massive            
                         protostellar object S140 IRS1.                                          Wgt2002a
             BEI   2     A: SH 2-140 IRS 1. Includes monopolar nebula that extends towards the           
                         SE at a PA ~150 +/- 15deg.                                              Alv2004 
22193+0800   J   179     OL  147.                                                                        
22193-1047   STF2892     Probably a misprint in BDS Vol II: AD should read AB.                           
22195-6048   HJ 5323     B is CPD-61@6639.                                                               
                         Spectrum of system: K1/2III F2/3(IV).                                           
22199+0526   OSO 176     G018-040. Not a common proper motion pair, based on astrometry and              
                         color.                                                                  Oso2004 
22199-3642   HJ 5326     SWR 268. CPM pair                                                       Skf2004 
22202-1307   EPI  17     EPIC 206061524. Planet Hunter Object of Interest (PHOI-5b), period              
                         5.8797 +0.0018/-0.0015d.                                                SJR2016 
22204+4625   RAO  74     A is also a 765d spectroscopic binary.                                  Tok2019b
22204+0520   CBL 540     Aka CRB  19.                                                                    
22204-0847   LDS2941     LDS5248.                                                                        
22205+0547   HJ  962     30 Peg.                                                                         
22205-0041   SLP   1     Primary is the white dwarf PHL 5038; a model fit to its spectrum                
                         yields Teff = 8000 +/- 100K and log g = 8.2 +/0 0.2, implying a mass            
                         of 0.72 +/- 0.15 Msun and a distance of 64 +/- 10 pc.  The B                    
                         component is likely a brown dwarf, spectral type L8-L9.                 SlP2009 
22206+5349   BU  379     Bidelman classifies AB as composite gK+ early A.                                
22207+2457   STF2895     CD: Also known as POU5695.                                                      
22210+4632   HJ 1755     2 Lac. A is a spectroscopic binary.                                             
22211+5428   ES 2718     B is BD+53@2854.                                                                
22211+3744   BRT2235     Aka ES 2531.                                                                    
22211+3544   ES 2389     J  3318.                                                                        
22213+5109   VBS  36     Van Biesbroeck called this HJ 1757, BDS 11679, but it looks like        VBs1914 
                         another pair.                                                                   
22213+2820   HO  615     32 Peg.                                                                         
22214+6828   OSO 177     G241-004. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
22216+1207   BPM2445     [PM2000] 2581835 + [PM2000] 2581704.                                    Gvr2010 
22217-0123   HJ 3106     gam Aqr = 48 Aqr = Sadachbia. A is a spectroscopic binary.                      
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2014).                         USN2014b
22220-3431   SHY 805     AB: HIP 110419 + HIP 110433.                                                    
             SHY 802     BC: HIP 110433 + HIP 109306.                                                    
22225+3021   HO  474     CD measure of Bu_1906 was erroneously also labelled as BD.                      
22226+1829   BPM2446     [PM2000] 2583171 + [PM2000] 2583192.                                    Gvr2010 
22226+0956   STTA231     B is BD+09@5031.                                                                
                         PU Peg, Beta Lyr (EB) type eclipsing binary, P = 0.862011 d.            Zas2011 
22227+2849   KU   64     CD: J 1796.                                                                     
22227+1457   BPM2447     [PM2000] 2583245 + [PM2000] 2583248.                                    Gvr2010 
22227-4152   DON1030     Spectrum K1/2III/IV.                                                            
22227-4557   I   135     pi 1 Gru = 161 Gru. A is an irregular variable.                                 
22229+1619   BB Peg      Multiple system including contact binary. Pribulla & Rucinski (2006)    Pbl2006 
                         estimate the mass of the contact pair at 1.951 Msun and the minimum             
                         mass of the wider component at 0.19 Msun.                                       
22230+5533   BAR  58     D is the Mira-type variable SU Lac.                                             
22231-4556   I   382     pi 2 Gru                                                                        
22231-6509   HJ 5327     B is CPD-65@4028.                                                               
22233+3642   ES 2070     Aka J  3319.                                                            Dam2013 
22234+3912   HJ 1759     ALI 987.                                                                        
22234+3228   WOR  11     Also known as GJ 856, this is a well studied binary with several                
                         astrometric data points over a long baseline. In Table 4, we present            
                         the AstraLux data as well as one example data point from literature,            
                         and otherwise refer to Seymour et al. (2002) for more information on    USN2002 
                         the astrometric data and a preliminary orbit fit. Lopez-Santiago et al          
                         (2006 ApJ 643, 1160) classify the system as a member of subgroup B4,            
                         with an estimated age of ~100 Myr.                                      Jnn2012 
22236+5431   ES 1021     STI2741.                                                                        
22236+5214   CHR 108     bet Lac = 3 Lac                                                                 
                         NPOI Limb-darkened diameter 1.92 +/- 0.02 mas,                          NOI1999 
                         R = 10.7 +/- 0.3 \rsun.                                                         
                         NPOI Limb-darkened diameter 1.909 +/- 0.011 mas.                        NOI2001a
                         NPOI Limb-darkened diameter 1.957 +/- 0.037 mas, Sp = G8III,            NOI2018 
                         R = 10.96 +/- 0.23 \rsun, Teff = 4803 +/- 75 K, L = 57.7 +/- 3.0 \lsun,         
                         M = 0.97 +/- 0.21 \msun, Age = 6.76 +/- 3.59 Gyr.                               
22236+4521   STF2902     AB: H N  64.                                                            MEv2010 
22237+2051   STF2900     33 Peg.                                                                         
                         STTA233. STFB 12.                                                               
                         AB: Additional notes may be found in Couteau (1955).                    Cou1955c
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: H 5  99.                                                            MEv2010 
             COU 139     CD: This may be the pair observed by Kuiper in 1934 and "suspected of   Kui1961b
                         being a very close, equal pair of 0".1". Star was not retained in the           
                         lists of Kuiper, nor in the IDS.                                        Cou1967a
             STF2900     AB: Rectilinear solution by Hartkopf & Mason (2013).                    Hrt2013b
22237-7248   HJ 5325     B is CPD-73@2252.                                                               
22240+0612   TOK 350     Triple system consisting of a close binary Aa,Ab with a separation of           
                         0".09 detected by Riddle et al. (2015) and a CPM companion with a       RAO2015 
                         separation of 171". The Aa,Ab system is unresolved in the Ks images,            
                         but elongated in the J images. We were unable to extract astrometry             
                         from the data. The separation has decreased since it was discovered             
                         in 2012; Tokovinin et al. (2014) resolved it with visible speckle       Tok2014a
                         interferometry at the 4.1 m SOAR telescope on 2013.73 at 41 mas.        Rbr2015d
22241-0450   BU  172     51 Aqr.                                                                         
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 5.81 +/- 1.40, 4.96, and 2.24 Msun, respectively.  Mlk2012 
                         1976.6164: This epoch was incorrectly given as 1976.6146                McA1982b
                         AB,C: H 5  95.                                                          MEv2010 
22242+3831   BRT2236     ALI 988.                                                                        
22243-0138   GIC 180     LDS5249.  G027-026/G027-025.                                                    
                         NLTT 53754/53752                                                        Chm2004 
22246+1359   BPM2448     [PM2000] 2585544 + [PM2000] 2585676.                                    Gvr2010 
22246-4127   JC   19     B is CD-42@15902.                                                               
22246-7215   FIN 285     nu Ind. Measures uncertain, too close. Proper motion +1326 -690.                
                         Needs speckle to elicit the nature of the motion.                               
22247-0159   ALP  28     2MASSW J2224438-015852                                                          
                         Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
22248+2409   HJ 1763     52.5s p and 3' n of BD+23 4532.                                         Doo1915a
22257+1641   BPM2449     [PM2000] 2586892 + [PM2000] 2586810.                                    Gvr2010 
22259-7501   DUN 238     AB + KO    5AC + TOK 434Ba,Bb: HIP 110712 and 110719 form the 20".6             
                         pair DUN 238 AB. We observed both components. The A component has a             
                         variable RV according to the GCS, but not confirmed by Jones et al.             
                         (2002); it was unresolved. The newly found pair Ba,Bb has a period on   CPS2002b
                         the order of 10yr. Considering the distant companion                    Cab2012 
                         C found by Caballero (2012), the system contains at least 4 stars.      Tok2015c
22262+3606   BRT3254     ALI 230.                                                                        
22262-6157   HJ 5331     B is CPD-62@6336.                                                               
22263-1839   BHA  52     CPD-19@8232.                                                                    
22264+5714   STI2778     22265+5714SMA 164                                                               
22264+5534   HJ 1767     STI 2777.                                                                       
22266+0424   BU  290     34 Peg.                                                                         
                         This cannot be the close 931.3-d spectroscopic binary.                  Grf2010a
                         AB: A = 34 Peg is SB1, P=913.3d=2.55y (Griffin 2010). Also astrometric  Grf2010a
                         orbit, P=2.404y (Goldin & Makarov 2007).                                Gln2007 
22266-1645   SHJ 345     53 Aqr.                                                                         
                         AB: H N  41.                                                            MEv2010 
22267+1458   BPM2450     [PM2000] 2588140 + [PM2000] 2587991.                                    Gvr2010 
22268-5446   RST1132     CD-55@9094.                                                                     
22269+2653   COU 539     This cannot be the close 6.5-d spectroscopic binary.                    Grf2011 
22269-1152   LDS2943     NLTT 53864/53865                                                        Chm2004 
22272-0146   STF2904     BAL 269.                                                                        
22273-6458   CHR 188     del Tuc                                                                         
22274+4749   HJ 1768     B is BD+47@3801.                                                                
22274+3949   CHR 109     This system, first announced by McAlister and recalled in a later       McA1984b
                         McAlister paper after repeated attempts at confirmation, has been       McA1993 
                         restored. While perhaps still spurious, the subsequent confirmation or          
                         suspected duplicity (by another technique) makes the discovery                  
                         measurement somewhat more probable.                                             
22274-3411   LDS 785     Spectra DA and M?.                                                              
22274-5800   I   137     DK Tuc, Algol-type eclipsing binary, P = 5.33793 d.                     Zas2011 
22275-2630   LDS3388     DEA  24.                                                                        
22275-7743   MUG  18     Exoplanet host, P=2.24d. Companion listed by Roell et al. (2012) is     Rol2012 
                         confirmed by Mugrauer & Neuhauser (2009).                               Mug2009 
22276+5730   HJ 1771     STI 2784.                                                                       
22279+0442   ENG  85     35 Peg.                                                                         
22279-0517   OSO 178     G027-029.                                                                       
22280+5742   KR   60     B is the flare star DO Cep, which is fairly active with flares of small         
                         to moderate amplitudes.                                                         
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AC, AE, AF, and AI: Optical pair, based on study of relative motion of          
                         the components using the method of apparent motion parameters.          Kiy2008 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 0.43 +/- 0.06, 0.42, and 0.56 Msun, respectively.  Mlk2012 
             HZE   5     Heinze et al. (2010) determine the K component is a background object.  Hze2010 
             FYM 118     The EQ pair was initially listed incorrectly as CQ.  The CD pair was            
                         initially listed incorrectly as a new CT pair.                          FyM2014b
             KR   60     AD, AG: Rectilinear solutions by Mason & Hartkopf (2016).               Msn2016a
                         AF: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
             HEL   4     AJ: Rectilinear solution by Mason & Hartkopf (2016).                    Msn2016a
             FYM 118     AM, AO, AS: Rectilinear solutions by Mason & Hartkopf (2016).           Msn2016a
                         CE: Despite having an orbit, an optical pair based on parallax.         Mlk2022 
22284-2553   LDS2944     NLTT 53929/53928                                                        Chm2004 
22285+5110   OSO 179     G215-047. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
22286-6729   VIG  21     Optical/physical nature of the faint companion is undefined.            Vig2012 
22287+3514   POP  99     Possibly an identification problem with the Orlov et al. 2009 measure.  Orl2012 
22287+1333   BPM2451     [PM2000] 2590474 + [PM2000] 2590573.                                    Gvr2010 
22287-3908   SEE 473     nu Gru                                                                          
22288-0001   STF2909     A: zet 2 Aqr = 55 Aqr A                                                         
                         B: zet 1 Aqr = 55 Aqr B                                                         
                         AB: LDS4971.                                                                    
             EBE   1     The close pair has been resolved by infrared speckle interferometry             
                         (McCarthy 1983). Suspected variability of one of the components is      Mcy1983 
                         unconfirmed. Aa,Ab also known as TOK 201.                                       
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         A perturbation of the AB orbit (period ~25y) was first noted by Strand  Str1942 
                         (1942). The mass of the third star was subsequently estimated at 0.22           
                         Msun by Harrington (1968) and 0.4 Msun by Heintz (1984). Based on       Hrr1968 
                         parallax observations, Franz (1958) associated this third star with     Hei1984c
                         the B component, while Heintz favored the A component. Ebersberger &    Fnz1958 
                         Weigelt (1979) found a close visual companion to the A component,       Ebe1979 
                         while McCarthy et al. (1982) discovered a companion to B in the near    Mcy1982b
                         infrared. Scardia et al (2010) find the astrometry of the McCarthy      Sca2010c
                         companion to be in good agreement with predictions of the perturbation          
                         orbit, so assume this orbit is associated with B.                               
                         H 2   7.                                                                MEv2010 
22290-0956   STF2907     B is BD-10@5924.                                                                
22291+1212   BPM2452     [PM2000] 2590844 + [PM2000] 2590968.                                    Gvr2010 
22291-3658   RSS  38     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
22292+5825   BU  702     A: del Cep = 27 Cep. Prototype of the Cepheid variables, P = 5.36d.             
                         A: Gallene et al. (2016) searched for close companions to del Cep,              
                         using the CHARA Array. H-band magnitude limits for separation regimes           
                         r < 25 mas, 25 < r < 50 mas, and 50 < r < 100 mas of 6.17, 5.63, and            
                         5.26 mags correspond to spectral type limits for possible companions            
                         of F0V, A1V, and B9V, respectively,                                     CIA2016a
                         NPOI Limb-darkened diameter 1.52 +/- 0.02 mas,                          NOI1999 
                         R = 51.  +/- 9.  \rsun.                                                         
                         NPOI Limb-darkened diameter 1.520 +/- 0.014 mas.                        NOI2001a
             STFA 58     STTA235. C is variable and a spectroscopic binary.                              
                         AC: H 5   4.                                                            MEv2010 
                         C: Benedict et al. (2002) used the HST FGS3 to derive parallaxes for            
                         del Cep (3.66 +/- 0.15 mas) and its 40" companion HD 213307 = STFA 58C          
                         (3.65 +/- 0.15 mas). Residuals to the data for the C component showed           
                         long-term and non-linear trends, which they used to derive a                    
                         preliminary perturbation orbit with period 390d and a = 2.0 mas.        AST2002b
                         In addition to detecting the unresolved spectroscopic companion with            
                         P = 2202 +/- 6d a parallax of 4.09 +/- 0.16 is determined for the               
                         system from Hipparcos Intermediate Data.                                IRA2015 
                         Masses are 5.2 and 4. Msun. Estimated period = 345,000y,                        
                         a = 10,000au = 38.6".                                                   Evs2013 
22292+5451   MLR 613     Aa,Ab: TDT3541.                                                                 
22293-4330   I  1054     del 1 Gru. Variable?                                                            
22294-2840   SEE 474     AB: Duplicity doubtful, but should be tested by speckle.  Hipparcos             
                         suspected non-single.                                                           
22295+4742   MCA  71     5 Lac. A long-period (P = 41.95y) SB now resolved by interferometry.            
                         NPOI Limb-darkened diameter 5.881 +/- 0.022 mas, Sp = K4I,              NOI2018 
                         R = 319.2 +/- 29.3 \rsun, Teff = 3713 +/- 56 K,                                 
                         L = 17473 +/- 3344 \lsun, M = 5.11 +/- 0.18 \msun,                              
                         Age = 0.11 +/- 0.01 Gyr.                                                        
22296+3623   BRT3255     ALI 233.                                                                        
22296+0538   BU  844     BC: J 917.                                                              J__1957 
22298-4345   DUN 239     del 2 Gru. A is an irregular variable. B is CD-44@14934.                        
22299+5225   LEO  53     AB: Spectral type of B at Mt. Wilson is F5.                                     
22299+3912   MLB 905     ALI 991.                                                                        
22300+4851   JNN 294     Estimated age 30-300 Myr; masses 0.44 +/- 0.20 and 0.25 +/- 0.13 Msun;          
                         a ~42.7 au.                                                             Jnn2014 
22300+3234   CHR 110     38 Peg.                                                                         
                         This system, first announced by McAlister and recalled in a later       McA1984b
                         McAlister paper after repeated attempts at confirmation, has been       McA1993 
                         restored. While perhaps still spurious, the subsequent confirmed or             
                         suspected duplicity (by another technique) makes the discovery                  
                         measurement somewhat more probable.                                             
22300+0426   STF2912     The primary is a single-lined spectroscopic binary, P = 372.4 d.                
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.33 +/- 0.95, 3.00, and 1.35 Msun, respectively.             Mlk2012 
22301+4921   FRK  11     A is an eclipsing binary, V350 Lac. B is optical.                               
22302+2228   HU  388     Double never clearly resolved.                                          WRH1954b
                         BD +21 4772 , 4' distant, may have common proper motion (Eggen 1965).   Egg1965 
22303+5714   STT 473     Spectroscopic binary.                                                           
22303+0047   RST5485     Position corrected by Heintz.                                           Hei1980a
22305+2232   VOU  38     Many negative results make interpretation uncertain.                            
22305-0807   STF2913     H 2  59.                                                                MEv2010 
22308+5637   DOO  17     The distance to 22308+5630DOO  18 is 370.6 @ 351.5".                    Fox1925 
22308+5630   STI2805     AC: Also known as DOO  18AC.                                                    
22308+4007   A  1467     Rectilinear solution by Rica & Zirm (2012).                             FMR2012i
22308+1629   BPM2453     [PM2000] 2592687 + [PM2000] 2592741.                                    Gvr2010 
22310-4926   HDO 299     AB: Primary is exoplanet host, P=951d. Roell et al.(2012 A&A 542, A92)          
                         list C at 96" as physical. Aladin: color DSS2 confirms CPM?             Tok2014d
                         B and D are not co-moving with A, but AC is CM pair.                            
             MUG   5     Followup spectroscopy confirmed the C component is a dwarf; estimated           
                         mass is 0.146 +- 0.005 Msun.                                            Mug2005 
             HDO 299     AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
22311+4509   LEP 108     NI   45.                                                                        
22313+5017   BU  703     alp Lac = 7 Lac.                                                                
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         Rectilinear solution by Hurowitz et al. (2014).                         USN2014b
22313-0633   CHR 111     Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         Hipparcos astrometric solution assumes circular orbit (e = omega = 0).  HIP1997d
                         Proper quadrants determined by occultation (D. Herald, private comm.)           
                         Orbit determined by fitting revised Hipparcos intermediate astrometric          
                         data. Derived component masses 1.07 +/- 0.06 and 1.00 +/- 0.06 Msun.    Ren2010 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.02 +/- 0.13, 1.98, and 1.13 Msun, respectively.             Mlk2012 
22314-0925   GIC 181     AB = G156-012/G156-013.                                                         
                         AB: NLTT 54059/54058                                                    Chm2004 
22315-3221   EHR  18     Primary is bet PsA = 17 PsA. B component is background star.            Ehr2010 
             PZ    7     AC: C is CD-32@17127.                                                           
22317+5711   SMA 166     STI 2808.                                                                       
22317-1054   58 Aqr      Hipparcos astrometric solution assumes circular orbit (e = omega = 0).  HIP1997d
22318+2953   MLB 582     J 2372.                                                                         
22320+6311   MLR  18     Aa,Ab: TDT3573.                                                                 
22320+2847   BRT 228     Probably J  2371.                                                       Nsn2016 
22321-4244   I  1455     Appears to be in rapid retrograde motion.                                       
22324+6015   HJ 1782     AC: Also known as 22326+6014BU 1514AC.                                          
22324+1606   BPM2454     [PM2000] 2594481 + [PM2000] 2594442.                                    Gvr2010 
22324-1056   STF2914     Aa,Ab: BDS has this examined by several apertures (6-40") from          Bu_1906 
                         1875-1904. Never resolved. According to Burnham: "It is therefore               
                         certain that the H companion does not exist."                                   
22325+6229   HJ 1784     STI 1113.                                                                       
22326+4307   ES  539     SMA 168.                                                                        
22326+0725   STF2915     A has been connected with BD+06@5033.                                           
                         Statistically the same parallax within the errors would indicate the            
                         components are physical.                                                        
             SHY 353     BC: HIP 111276 + HIP 110341.                                                    
22328+4857   ES  540     Aka OL  176.                                                            Dam2018l
22328+1024   OSO 180     G018-055. Not a common proper motion pair                               Oso2004 
22328-0557   OSO 181     G027-033. Not a common proper motion pair, based on color               Oso2004 
22329+5348   KUI 112     Proper motion +1361 +105.  The identification of this pair with the             
                         star at the quoted precise coordinates is uncertain.                            
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 0.65 +/- 0.34, 1.18, and 0.65 Msun, respectively.  Mlk2012 
22329+4923   HU 1320     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.98 +/- 0.69, 2.65, and 1.25 Msun, respectively.             Mlk2012 
22329+0219   LDS4976     Noticeable difference of AB from NLTT data.                             Gel1987 
22330+6955   STF2924     Giant (A9 III) classification probably wrong.                                   
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 4.28 +/- 0.89, 2.72, and 1.79 Msun, respectively.  Mlk2012 
22332+1732   OL  223     a.k.a. COU 332. In his 1968 observation Couteau notes "This is          Cou1970a
                         probably the star observed by Olivier in 1927 but not found at the      Ol_1928 
                         approximate position in the Index Catalog."                             IDS1963A
22332-0046   J   291     J 1728.                                                                         
22333-3844   SEE 475     Probably not double. However, should be checked with speckle.                   
22333-6049   MLO   7     G8/K0II+F/G.                                                                    
22334+1249   BPM2456     [PM2000] 2595677 + [PM2000] 2595703.                                    Gvr2010 
22334+1122   BPM2455     [PM2000] 2595578 + [PM2000] 2595624.                                    Gvr2010 
22334-0937   MCT  13     GJ 4282 = Steph 2018                                                            
                         Daemgen et al. (2007) derive a distance of 26.7 +/- 4.1 pc, separation  Dae2007 
                         of 41.9 +/- 6.4 au, and a predicted orbital period of 382 +89/-90 yr.           
                         Spectral types for both stars are M3.0 +/- 0.5; masses for both are             
                         0.42 +0.05/-0.06 Msun.                                                          
22338+0352   GRV 587     B component is +03 4726.                                                        
22339+1537   BPM2457     [PM2000] 2596171 + [PM2000] 2596113.                                    Gvr2010 
22340-0134   BU 1515     60 Aqr.                                                                         
22341+3920   BAG  47     Primary is the alpha2 CVn type variable V362 Lac.                               
22343-3759   UC 4769     SKF1510.                                                                        
22345+1358   J   292     TDT3598.                                                                        
22347+4042   ALR   2     Allers et al. (2009) Estimate distance at 325 +72/-50 pc, giving a              
                         projected separation of 51 +11/-8 au. Based on composite optical and            
                         near-IR spectroscopy, spectral type for both components is M6.                  
                         Individual masses for both components, based on an age of ~1 Myr, are           
                         estimated at 0.10 +0.075/-0.04 Msun.                                    Alr2009 
22347-0336   GAA  24     LL Aqr                                                                          
22350-1229   GIC 182     G156-022/G156-023.                                                              
22354+3249   ES 2270     Aka COU 736.                                                                    
22355+0234   HLD  51     A has been connected with BD+01@4632.                                           
22357+5652   HJ 1791     AB: HJL 306.                                                            HJL1986 
22357+5312   A  1470     1985.8481: Autocorrelogram was remeasured; new results in catalog               
                         Tokovinin gives combined spectroscopic/visual orbit, also yielding              
                         orbital parallax and component masses and absolute magnitudes.          Tok1993 
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.95 +/- 0.40, 1.85, and 1.26 Msun, respectively.             Mlk2012 
                         For the Horch et al. (2015) combined solution, the spectroscopic                
                         elements are fixed to those of Pourbaix (2000). Assigned spectral       Pbx2000b
                         types are G2V and G3V; derived masses 1.00 and 0.97 Msun.               Hor2015 
22357+1705   BPM2458     [PM2000] 2598252 + [PM2000] 2598177.                                    Gvr2010 
22357-2808   SHY 352     AB: HIP 111520 + HIP 110084.                                                    
22359+3938   CHR 112     8 Lac. A shows variable velocity, possibly due to motion in the Aa,Ab           
                         system. Shell star.                                                             
             STF2922     AB: H 4  86.                                                            MEv2010 
22359-2056   H 5  96     H V 96. B is BD-21@6253.                                                        
                         HJ 3122.                                                                        
                         Place by description. Harding has no star corresponding.                H__1867 
22361+7253   BU 1092     AB: LDS1995.                                                                    
                         Autocorrelogram for 1984.7042 observation was remeasured; new results           
                         are given in the catalog.                                                       
                         AB,D: HJL 307.                                                          HJL1986 
                         AB,D: SHY 810. Bayesian analysis by Shaya & Olling (2011) indicates     Shy2011 
                         very high (near 100%) probability pair is physical.                             
                         H 5  94.                                                                        
             HJ 3133     AB,C: Rectilinear solution by Hurowitz et al. (2014).                   USN2014b
22361+6053   MLB  97     Also known as STI6328.                                                          
22362+0010   STF2921     BAL 936.                                                                        
22366-3140   DUN 241     B is CD-32@17162.                                                               
                         Identified as optical and linear solution also published.               LRR2022c
22368+1551   HEI  85     BD+15 4680, formerly assigned to HJ  1790, now assigned here.           Hei1980a
22368+1550   HJ 1790     Much fainter than advertised. BD+15 4680 belongs with HEI   85          Hei1980a
22370+3716   J  2706     ALI 457. J 3176.                                                                
22370-4035   BU  771     sig 2 Gru                                                                       
             SHY 811     AC: HIP 111643 + HIP 111594.                                                    
22375+3923   HDS3211     A is also a 6177d spectroscopic binary.                                 Tok2019b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 0.95 +/- 0.10, 1.19, and 1.00 Msun, respectively.             Mlk2012 
             KIR   5     AC: Data from 2MASS. Kirkpatrick et al. (2001) derive spectral types    Kir2001b
                         M0V+M0V and M9.5V, conclude the C component is a CPM pair with                  
                         separation 635 au.                                                              
22375-6706   SHY 356     AC: HIP 111686 + HIP 111566.                                                    
22376-2805   LDS 789     B is CD-28@17852.                                                               
22378-0414   HJ 5529     kap Aqr = 63 Aqr = Situla                                                       
                         The pair observed by Burnham and others is not the Herschel pair, but           
                         was incorrectly assigned to that designation. According to Burnham,             
                         "No other measures. At one time Herschel suspected a very small                 
                         companion (= H 5529) but this has never been seen since, and certainly          
                         does not exist."                                                        Bu_1913 
22380+7305   LDS1996     NLTT 54455/54454.                                                               
22381+2601   OSO 182     GD 239. Not a common proper motion pair, based on comparison with               
                         POSS2 red plates                                                        Oso2004 
22383+4511   CHR 114     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 11.95 +/- 2.82, 5.02, and 4.04 Msun, respectively.            Mlk2012 
22384-0754   A  2695     One component is variable.                                                      
                         Malkov et al. (2012) derive dynamical and spectroscopic masses                  
                         1.83 +/- 1.07 and 4.47 Msun, respectively.                              Mlk2012 
22385+1559   BPM2459     [PM2000] 2601424 + [PM2000] 2601331.                                    Gvr2010 
22385+0218   HO  479     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
22385-1519   BLA  10     L 789-6. GJ 866. One of the nearest stars, proper motion +2340 +2270.           
                         Leinert et al. (1990) derive a combined spectroscopic/interferometric/  Lei1990 
                         photometric solution, yielding masses and temperatures, etc.                    
                          Adopted magnitude differences are as follows:                                  
                              0.20 +/- 0.13 mag    845 nm                                                
                              0.63 +/- 0.08 mag   1250 nm                                                
                              0.63 +/- 0.06 mag   1650 nm                                                
                              0.63 +/- 0.06 mag   2250 nm                                                
                              0.63 +/- 0.10 mag   3800 nm                                                
                              0.55 +/- 0.36 mag   4800 nm                                                
                         Very low mass triple. AC pair is 3.8-day SB orbiting B component.               
                         Combined spectroscopic/interferometric/parallax orbit given for AC,B            
                         by Delfosse et al. (1999). Resulting masses are placed on M-L diagram.  Del1999b
                         Combined solution from astrometry, spectroscopy, and parallax derived           
                         by Segransan et al. (2000). Solution yields mass and orbital parallax   Sgr2000 
                         determination.                                                                  
22386+5648   HJ 1796     Rectilinear solution by Friedman et al. (2012).                         USN2012a
22388+4419   HO  295     Slight variability is reported.                                                 
                         Visual sec. is 552d SB2.                                                Duq1987 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.26 +/- 0.16, 2.14, and 1.07 Msun, respectively.  Mlk2012 
                         AB: For the Horch et al. (2015) combined solution, the spectroscopic    Hor2015 
                         elements are fixed to those of Duquennoy (1987).                        Duq1987 
             BAG  15     Ba,Bb: There is some confusion in the literature as to whether the              
                         close Balega pair is Aa,Ab or Ba,Bb. However, Duquennoy (1987) says     Duq1987 
                         the secondary is a 552d SB2 and Horch et al. (2015) have clearly        Hor2015 
                         resolved the fainter star into a close pair and derive an orbit using           
                         the Duquennoy SB elements. The components of the close pair have                
                         therefore been changed to Ba,Bb accordingly.                                    
                         Ba,Bb: For the Horch et al. (2015) combined solution, all elements are          
                         calculated from the speckle data, but a double-lined orbit exists due           
                         to Duquennoy (1987). This orbit has similar elements to the orbit here  Duq1987 
                         except for the time of periastron passage.  Assigned spectral types             
                         for A, Ba, and Bb are F9V, G5V, and K1V; derived masses are 1.12, 0.92          
                         and 0.77 Msun.                                                          Hor2015 
22388-2037   HJ 3126     LDS4984.  A is a BY Dra-type variable, and B is a flare star. The A             
                         component is FK Aqr, a 4.1d SB2. The HJ pair has an estimated period of Tok2006 
                         2800y. The B component is a 1.8d SB1. The companion to B may be a Brown DCL2014 
                         Dwarf.                                                                          
22389+3010   CHE 331     Chevalier made an error in applying the RA offset.                      Che1908 
                         See Hartkopf (2012).                                                    Hrt2012b
22389+1931   KUI 113     40 Peg.                                                                         
22389-3527   BRT1826     Spectrum: K1/2III/IV.                                                           
22390+1850   HU  392     A 1923 measure of 16394-0306 BU 820 by Gauchet was inadvertently        Gau1925 
                         attributed to 22390+1850 and listed as new companion GAU 19AC. Error            
                         noted by Thorel (2012).                                                 Thr2012 
22390+1037   BRT3369     Originally published as BRT1959.                                        Brt1936b
                         J  3351.                                                                Nsn2016 
22391+3723   STT 475     A is a spectroscopic binary.                                                    
22392+2014   HU  393     Last position given in IDS appears to be in error. Angular motion has           
                         actually been some 10deg less than indicated.                           Wor1967b
22393+3903   S   813     10 Lac.                                                                         
             TRN  36     AC: The image rotator was in an unknown state, so two possible theta            
                         values are listed for the 2001.7339 observation - one for zenith up             
                         and one for north up.                                                   Trn2008 
             S   813     AB: H 5  97.                                                            MEv2010 
                         Uniform disk diameter  0.11  +/- 0.02  mas,                                     
                         Limb darkened diameter 0.121 +/- 0.005 mas,                                     
                         Teff = 40,000 +/- 1300 K, Radius is 6.7 +/- 1.4 \rsun.                  CIA2018e
22396+3736   HO  187     Spectrum G3Ib-IICN-1CH2Fe-1 in Bright Star Catalogue.                           
22396+1121   OSO 183     G067-009. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
             LEP 110AD   Aka CRB  21.                                                                    
22397-2820   H 6 119     AB: H VI 119 = DUN 242.                                                         
                         HJ 5356  H N 117. Star seen (by HJ) as close double (distance 2")               
                         and registered as No. 5356: pos 59.2deg, dist. 2", mags 8 and 10,               
                         with this description: "Elegant; has a * 6m, 2.5s p, and about                  
                         100" n, which with this constitutes the coarse double star D 242.       H__1867 
22399+6143   OSO 184     G233-026. Neither is a common proper motion pair.                       Oso2004 
22402+3732   HO  188     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.13 +/- 2.71, 2.83, and 1.10 Msun, respectively.             Mlk2012 
22405-5750   HJ 5354     B is CPD-58@7983.                                                               
22407+2959   STF3134     Chevalier made a reduction error in converting from (dx,dy) to          Che1908 
                         (rho,theta).                                                            Hrt2012b
22407+1547   BPM2460     [PM2000] 2604048 + [PM2000] 2604027.                                    Gvr2010 
22408-0333   KUI 114     Long-period (circular) orbit preferred, but strangely low mass-sum,             
                         probably still underestimated a.                                        Sod1999 
                         Occultations indicate a third body?                                     Grf1987 
                         Equinox-1900 position was incorrectly given as 22356+0404               McA1978b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 0.80 +/- 0.22, 2.16, and 1.17 Msun, respectively.             Mlk2012 
22409+1433   HO  296     Primary giant according to isochrone fit.                                       
                         Combined spectroscopic/astrometric solution of SB2. Calculated masses           
                         1.075 +/- 0.058 and 1.171 +/- 0.047 Msun, distance 34.43 +/- 0.34 pc.   Mut2010b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.17 +/- 0.33, 2.47, and 0.97 Msun, respectively.  Mlk2012 
22412+7546   LDS2000     LDS2001.                                                                        
22412+1155   BPM2461     [PM2000] 2604556 + [PM2000] 2604626.                                    Gvr2010 
22413-1045   LDS6386     NLTT 54554/54555                                                        Chm2004 
22414+5626   KRV  43     Classical Cepheid RR Lac.                                                       
22415+4014   S   815     A is the Beta CMa-type variable DD Lac.                                         
                         H 6 121.                                                                MEv2010 
22415+3256   J  2376     AB: Rectilinear solution by Cvetkovic et al. (2019).                    Cve2019b
22415+1050   BU 1516     zet Peg = 42 Peg = Homam                                                        
22417+3059   CHE 368     Chevalier made a trigonometric error in deriving theta; the correct     Che1908 
                         value is 180deg - theta.                                                Hrt2012b
22418+3041   CHE 370     AC: Chevalier made a reduction error in converting from (dx,dy) to      Che1908 
                         (rho,theta).                                                            Hrt2012b
22419+2126   STF2934     One component has an unseen companion with P = 82y. It is not known             
                         with which component the probable subsystem is associated; thus,                
                         assignment to A is arbitrary.                                                   
22420+1513   HU  781     V415 Peg, Algol-type eclipsing binary, P = 11.4456 d.                   Zas2011 
22424+5436   HJ 3138     STI 2845.                                                                       
22424+3025   CHE 380     Possibly an error in transcribing or in precessing to generate WDS              
                         designation? The pair was at the location predicted by precessing       Hrt2012b
                         Chevalier's coordinates.                                                Che1908 
22425+4110   COU2710     AC: No closer pair seen.                                                B__1963b
                         AC: A was single in 1957, and not seen double by Heintz, who concluded  Cou1958a
                         who concluded that Espin measured another star (GCB 64). Hence the      Hei1983a
                         pair ES 1699 probably does not exist.                                           
22426-4713   COO 252     A is variable.                                                                  
                         AB: Primary is possible astrometric pair.  Jones et al. (2002)          CPS2002b
                         do not detect SB with precise RV                                        Tok2014d
22428+1100   STF2933     J  3352.                                                                Nsn2016 
22428-5751   HJ 5357     Spectral type of A may be K0.                                                   
22430+3013   BLA  11     Aa,Ab: eta Peg = 44 Peg = Matar. Spectroscopic binary resolved by               
                         speckle interferometry. Spectrum of Aa,Ab is composite; G2II-III+F0IV.          
                         Hence a quadruple system.                                                       
                         The elements P, T, e in the astrometric solution by van de Kamp &               
                         Damkoehler (1957) have been taken from the spectroscopic orbit by       Kam1957 
                         Crawford. The astrometric amplitude is marginal and not certainly real          
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Crawford (1901).                                                        Crw1901 
                         Aa,Ab: Malkov et al. (2012) derive dynamical and spectroscopic masses           
                         5.17 +/- 0.72 and 3.35 Msun, respectively.                              Mlk2012 
                         Aa,Ab: Ren & Fu (2013) calculated an astrometric orbit, combining       Ren2013 
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Massarotti et al. (2008).                                               Msr2008 
                         NPOI Limb-darkened diameter 3.471 +/- 0.027 mas, Sp = G2III,            NOI2018 
                         R = 24.51 +/- 1.16 \rsun, Teff = 4970 +/- 65 K,                                 
                         L = 330.8 +/- 35.0 \lsun, M = 3.51 +/- 0.13 \msun,                              
                         Age = 0.27 +/- 0.03 Gyr.                                                        
             BU 1144     The pair BC (mags. 10.1-10.1, 0.3") is 91" distant and probably                 
                         physical; B is BD+29@4740.                                                      
                         Aka H 6  21 = S   816.                                                          
22431+4710   STT 476     B has been called a spectroscopic binary. No positive speckle results.          
                         A,BC: Additional notes may be found in Markowitz (1956).                Mrz1956 
22431+3149   CHE 338     Due to a typographical error in Che1911, the WDS designation for this           
                         pair was originally listed as 20401+3149.                                       
22431+1714   BPM2462     [PM2000] 2606650 + [PM2000] 2606719.                                    Gvr2010 
22431-0819   STF2935     AB: H 1  50 = H N 133.                                                  MEv2010 
                         Aka H N 128 = SHJ 349.                                                  Dam2011 
22432-0326   RST4710     J 1415.                                                                         
22433+4222   PAR   3     A is the Mira-type variable R Lac.                                              
22434+6744   HJ 1807     AB: HJL 308.                                                            HJL1986 
22435+3645   ALI 460     J 2405.                                                                         
22435-4125   I  1457     rho Gru                                                                         
22436+3811   ES 1997     J 3177.                                                                         
22438+1750   J   209     Pair is indeed BD+17 4798, but brighter than 9.5 magnitude listed in            
                         that catalog.                                                           J__1949a
22439-2846   BRT3106     A likely plate flaw.                                                    Grv2021b
22441+4149   STT 479     13 Lac.                                                                         
                         H N  42.                                                                MEv2010 
22441+3928   STF2942     A spectroscopic binary. Spectrum composite; K5III+K2III.                        
                         AB: STT 478.                                                                    
22441+1405   BPM2463     [PM2000] 2607642 + [PM2000] 2607682.                                    Gvr2010 
22441+1120   BPM2464     [PM2000] 2607673 + [PM2000] 2607764.                                    Gvr2010 
22442+2937   CHE 406     Originally listed with incorrect DM designation BD+28 4444, leading to          
                         poor WDS coordinates.                                                           
22444+1419   LDS1063     NLTT 54708/54709                                                        Chm2004 
22447-6007   HJ 5358     B is CPD-60@7595.                                                               
22448-0359   HJ 5359     B is BD-04@5748. Also known as STF2937.                                         
22449-0221   OSO 185     G027-045. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
22449-0654   CHR 207     First detected as an occultation binary by Edwards et al.               Evn1980 
22450+6808   STT 529     A is the Algol-type system ZZ Cep (B7+F0V). B is A2p. C is A5V.                 
22450-3314   LDS 793     Also known as LP 984-91 and LP 984-92. Part of Beta Pic Moving Group.           
                         Parallax of A component = 42.84 +/- 3.61 mas.                           VlF1997 
                         Parallax of B component = 47.84 +/- 2.34 mas.                           JLB2017 
22451-0240   A  2696     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
22452-4535   SHY 814     HIP 112330 + HIP 112337.                                                        
22453-0939   STF2939     H 3  69.                                                                MEv2010 
22455+1112   SHY 358     AD: HIP 112354 + HIP 112222.                                                    
22456+4524   LDS4995     AB: NLTT 54776/54777                                                    Chm2004 
22456-7952   HJ 5353     TOB 351.                                                                        
22457+4112   LEP 111     NI   46.                                                                        
22458+3006   CHE 421     This pair was not found at Chevalier's predicted location, nor was any  Che1908 
                         likely pair seen at other locations resulting from transposing x and y          
                         offsets from the plate center, or possibly sign errors in x and/or y.           
                         It remains the only one of his doubles from this paper not recovered.   Hrt2012b
22458+2940   CHE 423     Chevalier made  a reduction error in converting from (dx,dy) to         Che1908 
                         (rho,theta).                                                            Hrt2012b
22459+3252   CHE 425     Chevalier noted a large magnitude difference for this pair (5 mags).    Che1911 
                         The bright primary has a large proper motion along approximately the            
                         same direction as the position angle. The elongated image seen in               
                         Aladin suggests that the pair has closed in separation and the                  
                         secondary is currently lost in the primary’s glare.                     Hrt201
22461+6518   BLL  57     B is BD+64@1711.                                                                
22461+5804   STT 480     B is BD+57@2602.                                                                
22462+8138   LDS2009     NLTT 54931/54942.                                                               
22467+3226   CHE 430     The double measured by Berko (2010) is about 3' from Chevalier's        Che1911 
                         coordinates, but appears to be the correct pair.                        Bko2010b
                         See Hartkopf (2012).                                                    Hrt2012b
22467+1210   HJ  301     xi Peg = 46 Peg, high-PM star.. Mt. Wilson spectral classes F3s, dM0.           
                         CHARA Array Limb-darkened diameter  1.091 +/- 0.008 mas,                CIA2012e
                         R =  1.912 +/- 0.016 \rsun, L =  4.722 +/-0.087 \lsun,                          
                         Teff = 6167 +/-  36 K, M = 1.192 +/- 0.011 \msun,                               
                         Age =  4.8 +/- 0.2 Gyr.                                                         
                         AB: NLTT 54819/54820                                                    Chm2004 
                         AC: Rectilinear solution by Friedman et al. (2011).                     USN2011a
22467-4656   HJ 5362     A is a spectroscopic binary.                                                    
22468+4420   HER   5     A,BC: The flare star EV Lac.                                                    
22468+1901   LEP 112     NI   47.                                                                        
22469+5805   HJ 1810     DH Cep. The classification of the primary is from the UV tomographic    Pny1997 
                         analysis of Penny et al. (1997).                                        Msn1998a
22470+4446   A   189     Mt. Wilson spectral classes B8, B9.                                             
22471+1447   GRV 605     B component is +14 4870.                                                        
22473+2507   J  1357     POU 5750.                                                                       
22473-1609   HU  291     A=SB1, P=420d.                                                          Tok2014d
22474+1559   BPM2465     [PM2000] 2611249 + [PM2000] 2611308.                                    Gvr2010 
22474+0322   FAR  21     Primary is white dwarf WD 2244+031.                                     Far2005b
                         Originally listed as 22470+0325 with incorrect coordinates.                     
22476-2310   SHY 815     AC: HIP 112537 + HIP 111596.                                                    
22477-1403   STF2943     AB: tau 1 Aqr = 69 Aqr. A is a spectroscopic binary.                            
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
             GUI  38     AC: Aitken notes that Guillaume gives another measure to this system,   A__1932a
                         but neither the pair nor the original reference is found. The measure   Gui1932A
                         is assumed to be an error.                                                      
             STF2943     AB: H 5  80.                                                            MEv2010 
22478+6614   MLR  85     No significant movement since first resolution.                         Drd2009 
                         Assumed to be equivalent with the former DJU   8.                       Cgl2024a
22478-0414   STF2944     STFB 13.                                                                        
                         AB: NLTT 54867/54868                                                    Chm2004 
                         Both A and C are classed at Mt. Wilson as G2.                                   
                         AC and BC: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB: H 2  57.                                                            MEv2010 
22479+1259   HU  985     BU 1037.                                                                        
                         Pair has other discoverer's names and numbers in the literature due to          
                         duplicate discovery.                                                            
22479+0336   UC  278     Aka CBL 191.                                                                    
22479-5705   B  2059     Retrograde motion.                                                              
22481-1430   LIG   1     Ligi et al. (2018) determine the following parameters for                       
                         EPIC 206011496A:                                                                
                         R:    0.92 +/- 0.2 Rsun                                                         
                         age:  77.91 +1.11/-0.46 Myr (young)    2.42 +3.76/-1.47 Gyr (old)               
                         mass: 0.995 +/- 0.056 Msun  (young)    0.974 +/- 0.044 Msun (old)       Lig2018 
22481-2422   WSI 138     First associated with the C component of 22577-2937, the pair was       Msn2018a
                         closely examined and found single and an optical alignment has been     Mam2013 
                         ruled out as well. The working assumption is that the pointing was      Tok2015c
                         incorrect and an unknown pair was measured.                                     
                         The non-detections listed with this pair apply to the original                  
                         identification of LP 876-10.                                                    
22484-2206   LEO  54     CD-22@16058.                                                                    
22489+1307   HJ 1811     HJL 309.                                                                HJL1986 
22489+0137   HJ  970     BAL 1599.                                                                       
22489-2850   LDS4999     NLTT 54912/54933                                                        Chm2004 
                         A also known as LTT 9210, B as LP 932-83.                                       
                         Parallax of A component = 24.91 +/- 2.19 mas.                           VlF1997 
                         Parallax of B component = 29.79 +/- 2.09 mas.                           JLB2017 
22490+6834   STF2947     Mt. Wilson spectral classes F5s and F4s.                                        
                         AB: H 1  51.                                                            MEv2010 
22490-0320   LDS5000     NLTT 54927/54930                                                        Chm2004 
22494-1045   EPI  18     EPIC 206152015. Primary is eclipsing binary candidate, period 0.809d.   SJR2016 
22494-8457   GLI 277     Also known as TOB 354.                                                          
22496-1336   H 6  97     H VI 97. tau 2 Aqr = 71 Aqr. Variable?  B is BD-14@6351.                        
22497+6612   SHY 359     HIP 112724 + HIP 112324.                                                        
22498+1210   GIC 183     LDS1065. G067-024/G067-025.                                                     
                         NLTT 54980/54983                                                        Chm2004 
22498-1104   BU 1219     AC: AC is actually a measure from the Nebula h 2180 to a star. Kept X   Dam2013 
                         X coded.                                                                        
22499+8807   LDS2019     Aka WIS 372.                                                                    
22499+4620   HJ 1816     LDS5982.                                                                        
22499+0044   ALR   1     Allers et al. derive spectral types L3 +/- 0.5 and L5 +/- 1 for the     Alr2010 
                         primary and secondary, respectively; age of the system is roughly               
                         100 Myr. Based on luminosities and age, masses are expected to be               
                         roughly 0.029 +/- 0.006 and 0.021 +0.006/-0.009 Msun. Distance is               
                         about 56 +/- 16pc, and the orbital period is estimated at ~400 years.           
22500+5716   TOR  30     Formerly known as PAN  27.                                                      
22500-3248   HDO 301     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.67 +/- 1.11, 3.00, and 2.74 Msun, respectively.             Mlk2012 
22504+4157   HDS3244     A 0.9 arcsecond binary was published in 1985 and given the designation  McA1987a
                         CHR 115. This pair was subsequently deemed spurious after numerous              
                         failed confirmations. Reinspection of the 1985 data, post Hipparcos,    McA1993 
                         yielded a weak measure in good agreement with the Hipparcos                     
                         observation and subsequent speckle observations (see Mason et al.       Msn1999b
                         1999). This binary was incorrectly still listed as CHR 115 in Mason     Msn1997c
                         et al. (1997), however.                                                         
                         Primary is V360 Lac, Beta Lyr-type eclipsing binary, period 10.075d.    Zas2013 
22504-1744   DON1038     Gomez et al. (2016) derive dynamical parallax and component masses:             
                         16.10 +/- 0.89 mas, 0.644 +/- 0.017 Msun, 0.644 +/- 0.017 Msun.         Doc2016i
22505+5728   STI2873     STI2874???   The original STI2874 measure was likely of a plate flaw            
                         and it was not found in GSC.                                            Bko2009d
22506-5630   HJ 5364     LDS 796.                                                                        
22507+5535   ES 1031     VBS suspects a misprint in Espin discovery measure:                     VBs1954 
                         1910.74, 251.7@, 2.12".                                                 Es_1911 
22507+5107   HLD  54     On all 4 nights north following component looked the fainter to me.     B__1963b
22512+5712   HJ 1824     B is BD+56@2881.                                                                
22514+6142   STF2950     Spectrum composite; G8III-IV+G2IV.                                              
22514+2623   HO  482     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.72 +/- 1.72, 3.57, and 1.51 Msun, respectively.  Mlk2012 
                         AB: Prieur et al. (2014) derive a dynamical parallax of 6.5 mas and a           
                         total mass of 3.6 +/- 2.9 Msun (based on the original Hipparcos         HIP1997a
                         parallax) or 2.7 +/- 1.4 Msun (based on the revised Hipparcos parallax  VlF2007 
                         of van Leeuwen 2007).                                                   Pru2014 
22516-1104   GIC 184     Aa,Ab = LDS2958 = G156-054/G156-053.                                            
             LDS 423     AB = LDS6387.                                                                   
22518+4119   HJ 1823     STTA237.                                                                        
22518+3943   HO  298     Companion not seen 1944-1946, 1969.                                             
22519+5304   HJ 3150     B is BD+52@3314. Also known as STF2951.                                         
22519-1016   LDS5009     FAR  22. Secondary is white dwarf WD 2249-105.                          Far2005b
22520+5743   A   632     Giant (K5III) classification probably wrong.                                    
                         Possible triple?                                                        Dom1953b
                         Malkov et al. (2012) derive dynamical and spectroscopic masses                  
                         1.69 +/- 0.47 and 2.34 Msun, respectively.                              Mlk2012 
22520+4319   BU  451     15 Lac.                                                                         
22521-1257   HU   93     A is the Beta Lyrae-type system SU Aqr.                                         
                         Principal component is variable star SU Aqr; it was discovered as               
                         such by Miss Leavitt (Harv. Circ. 142, 2, 1908) but character of                
                         light curve is still somewhat doubtful.                                 VBs1927a
22522+3845   RAO 522     V364 Lac.                                                                       
22522+3527   BRG  35     HAT-P-8. Bergfors et al. (2013) estimate spectral types F5-F8V and              
                         M1-M3.5V.                                                               Brg2013 
             BEC   2     BC: Bechter et al. (2014) resolved the 1" companion to HAT-P-8 into 2           
                         stars, separated by 65 mas. Both components appear to be physically             
                         associated with the primary. Spectral types of the B and C components           
                         are ~M5V and ~M6V; masses are 0.22 +/- 0.03 and 0.18 +/- 0.02 Msun.     Bec2014 
22522-1730   RED  12     2MASS J22521073-1730134                                                         
                         A component spectral type probably L6 +/- 1, B component T2/T3; masses          
                         are about 0.07 and 0.06 Msun. Estimated distance is 13.6 pc.            Red2006a
22524+0950   EHR  19     Primary is sig Peg A. Called an SB in the Bright Star Catalogue.                
                         B and C components are background stars.                                Ehr2010 
22524-2142   BU  177     HDO 173                                                                         
22525+5717   TOR  31     Formerly known as PAN  28.                                                      
22525-3253   HJ 5367     gam PsA = 22 PsA. Variable? The historical data favor the Hipparcos             
                         magnitude over that of Tycho.                                                   
22525-4247   HJ 5366     B is CD-43@15179.                                                               
22525-8814   R   337     Also known as R   338 and TOB 355.                                              
22526-0735   SAO   1     Lam Aqr.                                                                        
             lam Aqr     1975.802: Probably unresolved (poor seeing).                            Bla1977a
22527+6759   STTA238     AB: HJL 310.                                                            HJL1986 
                         AB: SHY 819. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AB: H 6 100.                                                            MEv2010 
22527+6055   STF2953     MLR 511 misidentified and identical                                     Hei1987a
                         Primary is V453 Cep, an Algol-type eclipsing binary, P = 1.18475d.      Zas2012 
22527+3459   CRB  12     Due to typographical error, entered in WDS as 20527+3459.                       
22528+2926   COU2711     AB: AGK2+29 2849. BD+28 4475. Pair not in IDS or Carte de Ciel.                 
                         Proper motion of primary should allow determination in a few years of           
                         whether the pair is physical.                                           Cou1972a
22530+3140   HJ  972     Rectilinear solution by Friedman et al. (2012).                         USN2012a
22533+6209   ES  142     A is the Beta Lyrae-type system IL Cep.                                         
22533-1416   Gl 876      IL Aqr = Ross 780 = BD-15 6290. Star+planet pair. P, T, e, and                  
                         omega in Benedict et al. (2002) solution are constrained by RV          AST2002 
                         measurements; other elements from HST FGS data. Derived parallax =              
                         214.6 +/- 0.2 mas. Assuming mass of primary is 0.32 Msun, the planet            
                         mass = 1.89 +/- 0.34 Mjup.                                                      
22535-1137   MCA  73     74 Aqr. A spectroscopic, occultation, and interferometric system. The           
                         interferometric pair is not the spectroscopic pair, so the system is            
                         at least triple.                                                        Msn1997a
                         1977.4874: Theta incorrectly given as 92.8 degrees                      McA1979b
                         First detected as an occultation binary by Blow et al.                  Blw1982a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 23.11 +/- 7.09, 6.98, and 3.09 Msun, respectively.            Mlk2012 
22535-3054   LDS2960     NLTT 55142/55140                                                        Chm2004 
22536+3756   RUC  15     Multiple system including contact binary SW Lac. Pribulla & Rucinski            
                         (2006) estimate the mass of the contact pair at 2.196 Msun and the      Pbl2006 
                         minimum masses of the wider components at 1.89 and 0.54 Msun.                   
                         Spectral type of resolved companion estimated at K9-M0V.                Ruc2007 
22536+1647   BPM2466     [PM2000] 2617719 + [PM2000] 2617755.                                    Gvr2010 
22537+4445   BU  382     The RV of the primary is probably variable; identification of the               
                         ascending node from observations near periastron is thus tentative.     Mlr1954b
                         The visual primary is a 24d single-lined spectroscopic binary (#1406    Bte1989 
                         in Batten et al., 1989).                                                Sod1999 
22541+3527   HJ  973     ALI 10.                                                                         
22541-1152   HJ 3151     J 1418.                                                                         
22542-1323   LDS2962     LDS5987.                                                                        
22544+5538   HJ 1830     The 1917.81 Vatican Observatory measure of AC was originally            Vat1926 
                         attributed to DC.                                                               
22545+1517   LAU   5     AB,C: LDS 5016.                                                                 
22548+1511   STF2954     Delta from A to BD+14@4889 is 70.1". The motion seems to belong to B.           
22549+2415   GRV 620     This star has a probable wide companion at about 73" as noted in the            
                         WDS. It is however single in the separation range covered by the                
                         AstraLux data.                                                          Jnn2012 
22549-0922   HJ 3152     A is the irregular variable TT Aqr. Pair not found by Burnham.          Bu_1879 
22550+5132   HU  785     A premature orbit has been computed.                                            
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 8.68 +/- 8.02, 3.01, and 1.35 Msun, respectively.             Mlk2012 
22552-0459   BU  178     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
22553-4828   I    22     AB: Direct motion, with nearly a complete revolution.                   B__1956a
                         AB,CD: SHY 362. Bayesian  analysis by Shaya & Olling (2011) indicates   Shy2011 
                         very high (near 100%) probability pair is physical.                             
             B  2506     CD: Direct motion.                                                              
22553-5713   RED  19     Spectral type L6 +/- 1, distance 10.8 +/- 3.0 pc                        Red2008a
22555+3640   ES 2721     ALI 466.                                                                        
22557+3621   HJ  975     STTA239.  B is BD+35@4916.                                                      
22557-3023   LDS5017     NLTT 55271/55272                                                        Chm2004 
22557-3119   HUE   2     Companion detected in Ks band at 1.3", and marginally detected in H             
                         band. If bound, the companion candidate would be at a distance of               
                         13pc; spectral types estimated at T8 and T9.5.                          Hue2015 
22558-0749   GIC 185     G156-065/G156-064 = GJ 9803AB.                                                  
                         HIP 113231. See Allen et al. (2000) for information on metallicity,     AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 55287/55288                                                        Chm2004 
                         B is WD, DA7.4, mass 0.52 Msun (Holberg et al. 2013)                    Hbg2013 
22559-3232   HWE  91     del PsA = 23 PsA.  BU  772.                                                     
22562+7250   STT 484     AB,C same as STF2966.                                                           
             S   820     AB,D: BDS 11988 same star.                                                      
             STF2965     DE : This is also known as BU 1520. BU  1520DE is ADS 16393.                    
                         STF2965 is ADS 16384. These are the same system.                                
22564+4136   STF2960     STTA240. A is the Beta Cep-type variable EN Lac.                                
                         AB: H 4  85.                                                            MEv2010 
22564+1727   STF2957     HIP 113280. See Allen et al. (2000) for information on metallicity,     AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AB: NLTT 55326/55327                                                    Chm2004 
22565+6252   STF2961     One component is the Beta Cep-type variable KZ Cep.                             
22567+7830   STF2971     LDS2016.                                                                        
22570+2441   COU 542     Aa,Ab is also an SB, P = 118.48d.                                               
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 4.31 +/- 1.46, 2.15, and 0.85 Msun, respectively.  Mlk2012 
22570+1318   BPM2467     [PM2000] 2621102 + [PM2000] 2621111.                                    Gvr2010 
22570-0030   J  1419     BAL 634.                                                                        
22571-0315   STF2959     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: H N  15.                                                            MEv2010 
22574+1827   BPM2468     [PM2000] 2621541 + [PM2000] 2621534.                                    Gvr2010 
22575+5421   VBS  37     Also known as HJ 3157, BDS 12087.                                               
22575+2046   RBR  21     51 Peg = Helvetios.                                                             
                         2001.7340: PA is measured in zenith mode. If data collected in                  
                         equatorial mode, PA = 244.9. Confirmation of the pair should establish          
                         the correct theta value.                                                Rbr2011d
                         Based on van Leeuwen (2007) parallax, the candidate companion           VlF2007 
                         would have a separation of 45 au. Due to its relatively high proper             
                         motion, as additional observation will be able to determine whether             
                         the star shares common proper motion or is a background star.           Rbr2011d
                         CHARA Array Limb-darkened diameter  0.748 +/- 0.027 mas,                CIA2008c
                         R =  1.266 +/- 0.046 \rsun.                                                     
                         CHARA Array Limb-darkened diameter of A :                               CIA2013c
                         R =  1.1501 +/- 0.0195 \rsun, L =   1.2962 +/-0.0156 \lsun,                     
                         Teff = 5750 +/-  46 K, M = 1.064 \msun, Age = 5.6 Gyr.                          
22577-2937   KAL   1     Aa,Ab: Primary is alp PsA = Fomalhaut. Ab component is an exoplanet             
                         ~119 au from the star and ~18 au from the inner edge of the dust belt           
                         surrounding the star. Orbital motion is detected by HST observations            
                         separated by 1.73 years; the planet's mass if thought to be <3 Mjup.    Kal2008 
                         Intensity Interferometer Limb-darkened diameter 2.10 +/- 0.14 mas.      HBr1974 
             SHY 106     AB: HIP 113368 + HIP 113283                                                     
                         The pair may have first been noted as a cpm pair by Luyten.             Luy1938 
                         VLTI uniform disk diameter of B:       0.750 +/- 0.066 mas,             LTI2009 
                         VLTI limb-darkened disk diameter of B: 0.769 +/- 0.067 mas,                     
                         R = 0.629 +/- 0.051 \rsun, Teff = 4711 +/- 134 K,                               
                         M = 0.505 +/- 0.025 \msun.                                                      
             MAM   1AC   Full precision on relative position: PA = 337.9005206265515 and Sep =   Mam2013b
                         20410.120108318326" based on UCAC4 ICRS positions undated from the      Mam2013 
                         published value.                                                                
                         Parallax of A component = 129.81 +/- 0.47 mas.                          VlF1997 
                         Parallax of C component = 129.57 +/- 0.31 mas.                          XXX2016b
                         Parallax of C component = 132.07 +/- 1.19 mas.                          JLB2017 
22578+3840   HJ 1832     HJL 311.                                                                HJL1986 
22578-0222   LDS5028     NLTT 55402/55403                                                        Chm2004 
22578-2606   HJ 5371     LDS5027.                                                                        
                         NLTT 55389/55388                                                        Chm2004 
22578-3312   RSS  39     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
                         SHY 822. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
             SHY 823     AC: HIP 113381 + HIP 113532.                                                    
22579+1337   HU  989     Magnitude difference for this easy pair much less than given by Hussey  B__1963a
22583+5831   MLB  99     STI2914.                                                                        
22583+3717   J  3185     ALI 467.                                                                        
22583-0224   CHR 116     An occultation binary.                                                          
                         CHARA Array Limb-darkened diameter  0.704 +/- 0.013 mas.                CIA2009a
                         R =  1.50 +/- 0.03 \rsun, L =   1.2 +/-  0.0 \lsun,                             
                         Teff = 4895 +/-  57 K.                                                          
22583-6111   HJ 5370     B is CPD-61@6702. Spectral type of A may be F8.                                 
22586+1203   STTA241     B is BD+11@4911.                                                                
                         HJL 312.                                                                HJL1986 
22586+1122   BPM2469     [PM2000] 2622659 + [PM2000] 2622680.                                    Gvr2010 
22586+0921   STT 536     One component is variable or eclipsing.                                 Bu_1894 
                         Most speckle observations appear to be in `wrong' quadrant.                     
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.19 +/- 0.31, 2.23, and 1.97 Msun, respectively.  Mlk2012 
22586-4531   HU 1335     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.81 +/- 0.56, 1.98, and 0.98 Msun, respectively.             Mlk2012 
22587+6305   HDS3271     NY Cep, eclipsing binary of Algol-type, period 15.2756d.                Zas2016 
22587-2914   LDS5030     NLTT 55437/55435                                                        Chm2004 
22589+6902   GIC 186     G241-033/G241-032.                                                              
22590-0813   STF2962     Guillaume measures 1922.58, 223.8@, 14.3".  Archer believed the 1959    Gui1931 
                         observation was of AB,C component of ADS 16418 = STN 58. However, the   Arc1960 
                         Stone pair was determined to actually be ADS 16208 = STF2935AB.         Stn1878 
22591+1600   BPM2470     [PM2000] 2623184 + [PM2000] 2623078.                                    Gvr2010 
22592+1144   STT 483     52 Peg. Alternative spectrum: A8V+F6V.                                          
                         Period error +27.8/-22.7y. The Hipparcos parallax (12.26 +/- 0.94 mas)          
                         plus these elements yields a mass sum of 3.07; given the errors in              
                         parallax and period, however, the mass sum could be well over 4. The            
                         primary is spectral type A8V; the secondary may be a main-sequence F            
                         star. (Element errors and additional information from Alzner (private           
                         communication).                                                         Alz2007 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.84 +/- 1.37, 3.14, and 1.89 Msun, respectively.             Mlk2012 
22592-0052   JMS   6     AB: 2MASS J22590929-0051556 + 2MASS J22591388-0051581.                          
                         The C component is 2MASS J22590491-0052407.                             Jms2008 
22592-1034   AOT 120     WDS designation corrupted - should be 22592-0830                                
22592-1736   LEO  30     The 1923 measure by Przbyllok belongs to another pair.                          
22593+1212   OSO 186     G067-038. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
22593+0807   BFR  13     HD 217246 + 2MASS J22591631+0806556. Baron et al. (2015) estimate               
                         spectral types G5 and M6.5 +/- 0.5, distances 68 +70/-32 and                    
                         121 +20/-51 pc, masses 0.821-0.930 and 0.096-0.113 Msun.                BFr2015 
22595+1825   BPM2471     [PM2000] 2623619 + [PM2000] 2623629.                                    Gvr2010 
22595+0058   BAR  18     2 Psc.                                                                          
22596-0702   DEA   2     A,BC: The primary is a late-K star, while the secondary is a pair of            
                         M4.5 +/- 0.5 dwarfs, separated by 1-2" in SDSS images.                  Dea2013 
22597+7539   OSO 187     G242-019. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
22597+2553   MLB 727     Not found by Heintz at IDS position.                                    Hei1990b
22597-0422   STF2964     H N  90.                                                                MEv2010 
22598-1624   TOK 374     First resolution at 0".21 is secure and hints at a 30y period, but the          
                         preliminary SB orbit from CfA has a 9y period and corresponds to a              
                         0".09 semimajor axis.                                                   Tok2013b
22599+1822   BPM2472     [PM2000] 2623960 + [PM2000] 2623968.                                    Gvr2010 
23003+6755   GIC 187     G241-034/G241-035.                                                              
23004+0353   J  1797     BAL 2575.                                                                       
23005-2619   RST1154     AB: B is PMS star. Member of AB Dor moving group (see Lopez-Santiago            
                         et al. 2006 ApJ, 643, 1160)                                             Tok2014d
             SHY 364     AC: HIP 113597 + HIP 113579.                                                    
             CVN  67     CD: Originally 23003-2609 CVN  67, but primary was found to be the C            
                         component of 23005-2619 SHY 364AC.                                              
                         This is the more massive component of the WDS 23005-2619 system.        Skf2013 
23005-3345   B   582     A = TZ PsA, var. RS CVn type. Strassmeier (1993 A&AS 100, 173) gives            
                         P=1.642d.                                                               Tok2014d
23006-0704   RST4712     The B component is an unresolved composite spectrum binary harbouring           
                         the close hot white dwarf WD 2253-073. Spectral types of A, Ba, and Bb          
                         are G3V, K0V, and DA1.4, respectively; masses are 0.96, 0.79, and               
                         0.58 +/- 0.02 Msun; Teff 5670, 5236, and 37200 +/- 300K.                Hbg2014 
23006-2358   LDS5035     NLTT 9310 + NLTT 9315. CPM pair.                                        Mkr2008 
23008+7453   HJ 3162     H N  35.                                                                MEv2010 
23009-2216   BU  179     CD-22@16154.                                                                    
23005-2619   SHY 364     The more massive component of this multiple system is 23003-2609.       Skf2013 
23010+2646   STF2969     V416 Peg - Algol-type eclipsing binary, P = 1.424797 d.                 Zas2011 
23015+1658   BPMA256     [PM2000] 2625556 + [PM2000] 2625433.                                    Gvr2010 
23015+1202   BPM2473     [PM2000] 2625580 + [PM2000] 2625480.                                    Gvr2010 
23016+6912   OL  224     Also known as MLB 435.                                                          
23018-0351   GC 32089    Hipparcos astrometric solution assumes circular orbit (e = omega = 0).  HIP1997d
23019+4220   BLA  12     Aa,Ab: omi And = 1 And. Spectrum composite: B6IIIpe+A2p.                        
                         There appear to be both short and long period light variations.                 
                         Zhuchkov et al. (2010) generated a new orbital solution based on        Zhu2010 
                         published astrometry and new spectroscopic data.                                
             WRH  37     AB: P = 68.6y, a = 0.277", motion retrograde. B has been reported               
                         to be a double-lined spectroscopic binary, P = 33.01d.                          
                         Orbital elements by Olevic & Cvetkovic (2006) for SB:                   Ole2006a
                         P = 33.01 +/- 0.02 d, Tper = 2446925.3 +/- 0.2, e = 0.24 +/- 0.01,              
                         omega = 226.2 +/- 2.3deg, a sin i = 0.161 +/- 0.003 and                         
                         0.211 +/- 0.002 au, M sin3i  = 3.74 +/- 0.05 and 2.86 +/- 0.05 Msun.            
                         This component was first reported in McAlister & Hendry (1982) for      McA1982b
                         1976.61, after which earlier French data were reprocessed to yield the          
                         1975 measures.                                                                  
                         Zhuchkov et al. (2010) generated a new orbital solution based on        Zhu2010 
                         published astrometry, new 6m speckle data, and new radial velocities.           
                         LSC 104.                                                                        
23020+4800   A   194     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.24 +/- 2.37, 3.50, and 2.24 Msun, respectively.             Mlk2012 
23020-2151   B  1018     HDO 174                                                                         
23021+1026   J   294     J 1731.                                                                         
23023-6418   DUN 244     B is CPD-64@4310.                                                               
23024-1119   STF2970     H N 135.                                                                MEv2010 
23026+4946   ES 1185     LDS5999.                                                                        
23026+4245   BU 1147     2 And. The RV of the primary is probably variable.                              
                         Observations seem to confirm suspicion of van den Bos that the B                
                         component is variable.                                                  Baz1972 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         The equinox-1900 position was incorrectly given as 22590+4213 in                
                         McAlister & Hendry (1982).                                              McA1982b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 4.49 +/- 1.11, 5.85, and 2.00 Msun, respectively.  Mlk2012 
                         The physical nature of star C (mag. about 13, 90") unknown.                     
23028+5718   HJ 1843     STI 2929.                                                                       
23028+4404   STF2973     A variable, LN And.                                                             
23032+1558   BPM2474     [PM2000] 2627151 + [PM2000] 2627137.                                    Gvr2010 
23034+6027   STT 486     A is a spectroscopic binary. B is BD+59@2630.                                   
23035-3445   pi PsA      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Bopp et al. (1970).                                                     Evn1970 
23036-5618   HJ 5379     B is CPD-56@9990.                                                               
23037+5119   DBR  40     DBR  45.                                                                        
23038+2805   HJ 1842     bet Peg = 53 Peg = Scheat. A is an irregular variable, spectrum                 
                         M2.5II-III.                                                                     
                         AB and AC: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
23039+5123   DBR  44     DBR  54.                                                                        
23039+0056   J  1798     BAL 1247.                                                                       
23040-0233   OSO 188     G028-031. Not a common proper motion pair, based on color and                   
                         comparison with POSS2 red plates.                                       Oso2004 
23042+5121   DBR  52     DBR  76.                                                                        
23045+5126   DBR  53     DBR  65.                                                                        
23045+5125   DBR  46     DBR  66.                                                                        
23045+3123   ES  396     BRT 293.                                                                Brt1929b
23046-2611   B   587     Measures uncertain, too close. Needs speckle.                                   
23047+2355   POU5775     J 1898.                                                                         
23049+1539   WRH   2     BRT 1363 is probably identical.                                         Hei1983a
23051+5118   HJ 1846     Secondary is about 0.09 mag brighter than primary                       Los2005 
23052+6323   KR   62     The B component is V711 Cep, an Algol-type eclipsing binary with                
                         period 1.30436d.                                                        Zas2011 
23052-0742   A   417     83 Aqr. Alternative spectral type: F2IV+F0V.                                    
                         1977.9134: Rho was incorrectly given as 0".211                          McA1982b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 4.62 +/- 0.55, 2.86, and 1.79 Msun, respectively.  Mlk2012 
23054+5825   HJ 1847     Also known as STI2935.                                                          
23054+5453   HJ 3172     STI2934.                                                                        
23054-0911   LDS2965     NLTT 55790/55791                                                        Chm2004 
23056-3006   LDS6003     Not a double star. This is the galaxy LEDA 719617.                      Grv2020g
23060+1323   BPM2475     [PM2000] 2629594 + [PM2000] 2629619.                                    Gvr2010 
23061+6356   LAF  71     Due to the large number of components (exceeding the number of upper-           
                         case letters), a non-standard component designation was necessary,              
                         hence the pairings A,Za; A,Zb; etc. For this pair, as well as LAF  59           
                         and LAF  62, the lower-case designations (such as Za and Zb) do not             
                         refer to components of a close pair.                                            
23064+1235   GIC 188     AB = G029-001/G067-047.                                                         
                         AB: NLTT 55834/55835                                                    Chm2004 
             HDS3291     In addition to the previously known binary companion seen in the                
                         AstraLux images, 2MASS J23062378+1236269 is also a spectroscopic                
                         binary with a semi-major axis smaller than 0.31 au (Shkolnik et al.             
                         2010 ApJ 716, 1522), and has the additional wide companion 2MASS                
                         J23062530+1236570 (also in the sample, a single star in the AstraLux            
                         images) at 37.6" with confirmed proper motion (Lepine & Bongiorno       Lep2007 
                         2007), hence the system is likely quadruple in reality.                 Jnn2012 
23064-2152   HJ 3166     CD-22@16189.                                                                    
23065+4655   STTA242     B is BD+46@3933.                                                                
23067+3302   STF2975     Statistically the same parallax within the errors would indicate the            
                         components are physical.                                                        
23067-0412   HJ  978     Also known as CHE 435.                                                          
23068+1448   BPM2476     [PM2000] 2630304 + [PM2000] 2630364.                                    Gvr2010 
23069-4331   JC   20     the Gru. Spectrum F5m delta Del.                                                
                         AB: Additional notes may be found in van den Bos (1956).                B__1956a
                         AC: SHY 366. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
23071-2310   LDS5047     NLTT 55857/55860                                                        Chm2004 
23072-5041   DUN 246     B is CD-51@13470.                                                               
                         A comp is possible astrometric pair; however, no SB orbit for A. No             
                         acceleration in original HIP.                                           Tok2014d
23073-3216   PRO 238     B companion is a non-existing star but is scattered light from a                
                         nearby bright star.                                                             
23075+3250   STF2978     H N  11.                                                                MEv2010 
23075+2108   LWR  19     V342 Peg.  Based on the proper motion of A and change in relative               
                         position, Close et al. (2010) conclude B and C are background objects.  Clo2010 
                         AD: Found in SDSS data. Position angle estimated by catalog editor              
                         based on Aladin image.                                                          
             MAR   1     The Ab, Ac, and Ad components are Jovian-mass planets in orbit around           
                         HR 8799. Projected separations are 68, 38, and 24 au; orbital periods           
                         (assuming pole-view circular orbits) are estimated at 460, 190, and             
                         100 years.  Masses are 5-11, 7-13, and 7-13 Mjup, respectively.         Mar2008 
                         The Aa, Ab, Ac, and Ad components all appear to be co-moving.           Vig2012 
                         CHARA Array Limb-darkened diameter  0.342 +/- 0.008 mas.                CIA2012d
                         R = 1.44 +/- 0.06 \rsun, Teff = 7193 +/- 87K, L = 5.05 +/- 0.29 \lsun.          
23077+4623   HJ 1849     4 And.                                                                          
23077+0636   STF2976     AB: HJL 313.                                                            HJL1986 
23078+6338   HU  994     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 98.34 +/- 19.03, 12.26, and 6.92 Msun, respectively.          Mlk2012 
23078-2042   HJ 3169     Durchmusterung identification not certain.                                      
                         Aka ARA1595.                                                                    
23079+7523   STT 489     pi Cep = 33 Cep. Visual primary (G2 III) is 557d SB1 (#1425 in Batten   Bte1989 
                         n et al.). A spectroscopic orbit was published by Scarfe et al.         Scf1983 
                         AB: Additional notes may be found in Dembowski (1883) and               D__1883 
                         Muller (1950).                                                          Mlr1950b
             pi Cep      Aa,Ab: Astrometric orbit by Gatewood et al. (2001) found by combining   Gat2001b
                         Hipparcos and Multichannel Astrometric Photometer data with the                 
                         spectroscopic elements of Scarfe et al. (1983). The photographic        Scf1983 
                         semimajor axis estimated at 39.0 +/- 3.9 mas. Masses are determined             
                         for all three components of this triple.                                        
                         This object was misidentified as HR 8815 by McAlister (1978).           McA1978c
                         Aa,Ab: Ren & Fu (2013) calculated an astrometric orbit, combining       Ren2013 
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Scarfe et al. (1983).                                                   Scf1983 
23079-5938   NZO 104     Spectral type G0?                                                               
23080+4151   OSO 189     G190-010. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
23082+4038   COU1344     TDT3897.                                                                        
23083+0439   GIC 189     G029-006/G029-007.                                                              
23083-1525   TSN 207     HK Aqr.                                                                         
23086-6352   B   590     No certain elongation.                                                  B__1951a
23087+0208   5 Psc       Hipparcos astrometric solution assumes circular orbit (e = omega = 0).  HIP1997d
23088+1058   A  1238     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 4.89 +/- 1.95, 2.96, and 1.17 Msun, respectively.  Mlk2012 
                         AB: Prieur et al. (2014) derive a dynamical parallax of 9.8 mas and a           
                         total mass of 3.7 +/- 1.7 Msun (based on the original Hipparcos         HIP1997a
                         parallax) or 5.0 +/- 1.9 Msun (based on the revised Hipparcos parallax  VlF2007 
                         of van Leeuwen 2007).                                                   Pru2014 
23091-0233   HIP 114313  SB1 with P = 3.1 yr, estimated q > 0.15. The orbital axis is 31 mas,            
                         too close for NICI. Large acceleration.                                 Tok2012a
23092-0719   STF2980     H N  88.                                                                MEv2010 
23093+4939   HDS3296     1996.5352: Very weak detection, possibly an artifact.                   Msn1999b
23093-8224   HJ 5378     B is CPD-83@745.                                                                
23094+1350   BPM2477     [PM2000] 2632370 + [PM2000] 2632371.                                    Gvr2010 
23094+0701   OSO 190     G028-042. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
23095+0841   STF2982     57 Peg. A is an irregular variable, GZ Peg. Spectrum composite;                 
                         M4IIIs+A2V.                                                                     
                         AB: H N  16.                                                            MEv2010 
23096+0045   GAU  20     ZoSe 13964-13965. Proper motion -210 -1270.                                     
                         We do not confirm it using our data and images from the Digitized Sky           
                         Surveys                                                                 Oso2004 
23097+5920   KUI 115     2 Cas.                                                                          
             S   823     AC: H 6  55.                                                            Dam2011 
23099-2057   LDS5052     NLTT 55994/55997                                                        Chm2004 
23099-2227   RST3320     89 Aqr.                                                                         
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 7.05 +/- 2.92, 5.61, and 3.35 Msun, respectively.             Mlk2012 
23100+4758   STF2985     B is BD+47@4058.   AB has a period of ~6300y.                           Tok2006 
                         HJL 314.                                                                HJL1986 
                         AB: B is KZ And, var. of BY Dra type.  B is SB2, P=3.033d               Tok2014d
23100+3651   S   825     STTA243. B is BD+36@5011.                                                       
23100+1426   STF2986     LDS1066.                                                                        
                         Significantly different proper motion and parallax for components, so   Jao2017 
                         non physical.                                                                   
                         A comp is SB1, P=3.632d (Griffin, 2001 Obs 121, 221)                    Tok2014d
23104+4901   STF2987     NLTT 56040/56041                                                        Chm2004 
23104-4515   iot Gru     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Jones (1928).                                                           Jon1928e
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Pourbaix et al. (2004).                                                 Pbx2004 
23105+1502   BPM2478     [PM2000] 2633240 + [PM2000] 2633157.                                    Gvr2010 
23106-0550   LDS2970     NLTT 56037/56038                                                        Chm2004 
23108+6315   MLR 181     Aka MLR  71.                                                                    
23110+6555   AG  290     B is BD+65@1855.                                                                
23111+5304   HD 218915   Aslanov et al. (1984 SvAL 10, 278) discuss the radial velocities and            
                         the possibility of a low-mass companion.  We found a possible binary            
                         companion at a separation of 0".08 which needs confirmation.            Msn1998a
23112+0500   HJ  980BC   Aka BAL2988.                                                                    
23114+3924   MLB1102     ALI 1003.                                                                       
23114+3813   HO  197     Star C (BD +37 4784, mag. 9, 40") may be physical.                              
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 11.98 +/- 6.99, 3.26, and 1.20 Msun, respectively. Mlk2012 
23114-4259   B   594     A premature orbit has been calculated. Needs speckle.                           
                         Likely a spurious pair. Last measured 1963 and unresolved by SOAR on 3          
                         occasions 2008-2012.                                                    Tok2010 
                                                                                                 Tok2012d
                                                                                                 Tok2014a
                                                                                                 Tok2015c
                                                                                                 Tok2016a
                                                                                                 Tok2018c
                                                                                                 Tok2022f
23116+3654   RUC  26     Multiple system including contact binary AB And. Pribulla & Rucinski            
                         (2006) estimate the mass of the contact pair at 1.656 Msun and the      Pbl2006 
                         minimum mass of the wider component at 0.40 Msun.                               
23118+2651   BUP 234     60 Peg.                                                                         
23121+4517   BU 1528     See star at 23108+4531. Burnham thinks this star more likely to be      Bu_1913 
                         HJ 1853.                                                                        
23121+2656   LEP 113     AC: As noted in Lepine & Bongiorno (2007), 2MASS J23120603+2655579      Lep2007 
                         forms a probable wide (14") pair with HIP 114543, which is itself a 1"          
                         binary. Hence, with the additional component seen in the AstraLux               
                         images, the system is likely quadruple.                                 Jnn2012 
23126+0241   A  2298     Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.43 +/- 0.64, 2.39, and 0.95 Msun, respectively.  Mlk2012 
23128+1526   BPM2479     [PM2000] 2635121 + [PM2000] 2635106.                                    Gvr2010 
23128-5240   TOK 682     2MASS has 3 point sources within 10" of A.                              Tok2014d
23129+1233   HJ 3176     BDS 12223, HJ 3177 same star.                                                   
23131+4000   STF2992     Same as STF2994.                                                                
                         AB: HJL 315.                                                            HJL1986 
23133+5710   STT 599     A is variable. Proper motion +2075 +296.                                        
                         B is BD+56@2967. Proper motion of B +009 +006.                                  
                         CHARA Array Limb-darkened diameter of A :                               CIA2012f
                         R =  0.7784 +/- 0.0053 \rsun, L =  0.26499 +/-0.00152 \lsun,                    
                         Teff = 4699 +/-  16 K, M = 0.763 \msun.                                         
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
23133+2205   STF2990AB   Despite the linear solution, proper motion and parallax favor a         Grv2020a
                         physical connection. Long period and/or high eccentricity possible.             
23134+0241   SCA 144     AB: Eclipsing binary of Algol-type, SZ Psc.                                     
             TOK  37     AC has estimated period 50,000y; Evolved primary is 4d eclipsing SB2.           
                         G-solution in Hipparcos. The K1III subgiant primary likely transfers            
                         mass to the MS secondary. Kalimeris et al. (A&A 293, 371, 1995) find            
                         period changes, apparently explained by the mass transfer and magnetic          
                         fields. Any potential tertiary period should be longer than 56y.        Tok2006 
23137+0212   STT 491     ADS notes that the A component (= STT 491 rej) was excluded as single   A__1932a
                         in the 2nd edition of the Pulkova Catalog.                              Stt1878 
23141-0855   STF2993     LDS 802.                                                                        
                         AB: NLTT 56207/56208                                                    Chm2004 
                         B component is 7.1d SB1; period of AB estimated at 18,000y.             Tok2006 
                         B possibly close pair, sep 0.053"?                                      Tok2014d
             S   826     AC and BC: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
23142-1938   LDS5060     NLTT 56210/56211                                                        Chm2004 
23144+2946   ARN  26     AC: C component = primary of 23144+2943 HJ 1858.                                
23144+2943   HJ 1858     Primary = C component of 23144+2946 ARN  26AC.                                  
23146+2555   COU 335     TDT3949.                                                                        
23147-1041   BU  715     The Cincinnati observers in 1877 measured the large star as a close             
                         pair, 1.5deg, :0".32. This was carefully looked for in the 36inch and           
                         there was no trace of any elongation at any time.                       Bu_1894 
23149+4320   MRZ   2     Aka HDS3309.                                                                    
23150-6334   LDS 803     Spectral type K0?                                                               
23151+8327   STF3003     B is BD+82@712.                                                                 
23152+6027   DOO  21     STI 1158. The fainter component is a Wolf-Rayet star.                           
23154+5937   STI9964     Erroneously identified as STI2964. This pair retained.                  Skf2017o
23154+5936   STI2964     Erroneously identified and here corrected.                              Skf2017o
23156+5829   MLR 365     Not the same as the nearby and similar J   860.                         Dam2013 
23156+5756   J   860     Not the same as the nearby and similar MLR 365.                         Dam2013 
23157+0118   CHR 141     Suspected occultation binary.                                                   
                         It has been speculated that the 468d companion is not the speckle       Grf2014d
                         companion. Only measured once.                                                  
23157-1221   LDS2977     NLTT 56270/56279                                                        Chm2004 
23159-0905   STFB 14     91 Aqr = psi 1 Aqr.  LDS 805.                                                   
                         NPOI Limb-darkened diameter 2.220 +/- 0.031 mas, Sp = K1III,            NOI2018 
                         R = 10.96 +/- 0.21 \rsun, Teff = 4730 +/- 68 K, L = 54.3 +/- 3.1 \lsun,         
                         M = 1.38 +/- 0.29 \msun, Age = 2.98 +/- 1.63 Gyr.                               
                         Burnham and Aitken both labelled this pair STFB 12; corrected by Weis   Bu_1906 
                         ("F.G.W. Struve's Double Stars").                                       A__1932a
                                                                                                 StF2002 
                         A,BC: NLTT 56282/56278                                                  Chm2004 
             STFB 12     A,BC: H 4  12.                                                          MEv2010 
             BU 1220     AD: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         BC: A pair in motion in a high-inclination orbit.                       Wor1967b
                         AD: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
23160-3309   B   596     Spectrum: Fm delta Del.                                                         
23161+4801   ES  694     ES 1186.                                                                        
23162-2823   LDS5062     NLTT 56294/56292                                                        Chm2004 
23162-5947   TOK 217     Tentatively resolved on 2011.85 at 147deg, 0".10, dK=2.5, but not               
                         confirmed here. As the RV is variable, we suppose the pair was                  
                         actually resolved last year but has closed in.                          Tok2013b
23163+1324   BRT1366     Aka ITF  92.                                                                    
23164+6407   BU  992     A premature orbit has been computed.                                            
23164+3739   ES 2537     J 3189.                                                                         
23165+6158   HDS3314     1991.9043: This observation confirms the Hipparcos solution at a                
                         similar epoch (1991.25). An elongated secondary peak yielded an                 
                         inaccurate value for rho, however.                                      Msn1999b
23166-0135   STF2995     LDS 808.                                                                        
23166-0558   OCC 731     BRT 561.                                                                Brt1931 
23167+3441   HDS3315     Cvetkovic et al. (2014) derive spectral types K1 and  K2, masses 0.85           
                         and 0.81 Msun. Dynamical parallax is 10.98 +/- 1.07 mas.                Cve2014 
23167+1937   HDS3316     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 0.78 +/- 0.19, 1.09, and 0.95 Msun, respectively.             Mlk2012 
23167-3635   HDS3317     A single star reported double due to a grid-step error according to             
                         Fabricius.                                                              Fab2000b
23170-6200   EHR  20     Companion appears to be a background star.                              Ehr2010 
23171+3144   OSO 191     G128-043. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
23171-1349   BU  182     Van Biesbroeck (1961) reports a companion with cpm (mag. 17, 15").      VBs1961 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.21 +/- 0.99, 1.83, and 1.29 Msun, respectively.  Mlk2012 
             LDS6393     G273-001. AB component not resolved in our data                         Oso2004 
                         HIP 114962. See Allen et al. (2000) for information on metallicity,     AlC2000 
                         age, galactic orbital parameters, etc.                                          
             BU  182     AB,C: Rectilinear solution by Mason & Hartkopf (2016).                  Msn2016a
23173-6655   LDS 807     B is CPD-67@3959.                                                               
                         HIP 114980. See Allen et al. (2000) for information on metallicity,     AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         SHY 368. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
23174+3813   HDS3319     Due to the large proper motion of the secondary, the 1929 measure was           
                         initially ascribed to a supposed AC pair in this system.                        
                         AB: Rectilinear solution by Hartkopf & Mason (2016).                    Hrt2016a
23174-5814   GAT  31     This is the C component of the wide CPM pair 23537-6557 = SHY 108AC             
23176+1818   HU  400     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 5.46 +/- 2.34, 3.74, and 1.45 Msun, respectively.             Mlk2012 
23176-0131   BU   79     HIP 115012. See Allen et al. (2000) for information on metallicity,     AlC2000 
                         age, galactic orbital parameters, etc.                                          
23177+4901   BU  717     8 And.                                                                          
23179-1112   LTT 9469    Hipparcos astrometric solution assuming circular orbit (e = omega = 0)  HIP1997d
23180+4006   MLB 505     ALI1185.                                                                        
23180+3132   OSO 192     G128-045. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
23180+0904   OSO 193     G029-020. Not a common proper motion pair, based on color and                   
                         comparison with POSS2 red plates.                                       Oso2004 
23180-6100   DUN 247     B is CPD-61@6734. B spectral type A5/7V.                                        
                         Statistically the same parallax within the errors would indicate the            
                         components are physical.                                                        
23181+6017   STI1165     B is called BD+59@2698 by Bacchus.                                              
23181-0721   LDS2978     LDS6023.                                                                        
23184-0015   GRV1144     Aka GWP3273.                                                                    
23184-0600   BRT 524     A likely plate flaw.                                                    Grv2021b
23185+7014   LDS2034     NLTT 56462/56463.                                                               
23185-0916   LDS 810     NLTT 56435/56436.                                                       Chm2004 
23186+6807   STF3001     omi Cep = 34 Cep. A premature orbit has been computed.                          
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         System mass 3.65 +-0.60 Msun. G8III spectral type of primary                    
                         confirmed.                                                              Doc2003d
23186-5818   HJ 5392     B is CPD-58@8063.                                                               
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
                         A 7.9d spectroscopic solution for the A component has been found        Tok2018d
                         making this binary since component B is non-physical.                           
23187+1324   HJ 1866     34s f and 1' s of BD+12 4966.                                           Doo1915a
23188+0510   STF2999     AB: H 6  61.                                                            MEv2010 
23189+0524   BU   80     Lewis and Leavenworth measures attributed to CE actually were of a new  L__1902a
                         pair, designated CF.                                                    Lv_1930 
                         AB: The Heintz (1996) orbit predicts a separation of 0.374"; however,   Hei1996c
                         the secondary may have been too faint for the CHARA camera.             Hrt2009 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.44 +/- 0.44, 1.71, and 0.85 Msun, respectively.  Mlk2012 
                         AE: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AE: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
23190-0937   HO  199     psi 3 Aqr = 95 Aqr                                                              
23191+4855   ES 2725     B is BD+48@3994.                                                                
23191-1328   MCA  74     94 Aqr. A is a long-period spectroscopic binary now resolved by                 
                         speckle interferometry.                                                         
                         Soderhjelm give triple solution with B (HIP 115125) instead of poor     Sod1999 
                         Hipparcos solution. The primary is overmassive, probably sp. bin.,              
                         cf. analysis of the spectroscopic/interferometric orbit by McAlister            
                         & Hendry (1982)                                                         McA1982c
                         Analysis of this observation by the techniques in use in 1985 was               
                         unable to yield a useable result.                                       Hrt1992b
                         1977.6350: This epoch was incorrectly given as 1977.6359.               McA1982b
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 1.55 +/- 0.87, 1.98, and 1.20 Msun, respectively.  Mlk2012 
             STF2998     AB: H 3  34.                                                            MEv2010 
23193+4343   SMA 188     J 2381.                                                                         
23194+7900   LDS2035     AB: Also known as MLR 271.                                                      
23194-0507   HJ 5394     96 Aqr. This cannot be the close 21.24-d spectroscopic binary.          Grf2009b
                         NLTT 56477/56476                                                        Chm2004 
23195+1325   HJ  308     15s f and 1' s of HJ  307.                                              Doo1915a
23195+1326   HJ  309     9s f and 3' s of HJ 307.                                                Doo1915a
23196+0322   SCA 152     We do not confirm it using our data and images from the Digitized Sky           
                         Surveys                                                                 Oso2004 
23197+4823   STTA244     B is BD+47@4111.                                                                
23198+1741   RBR  54     Suspected non-single.                                                   Hor2002b
23205+3037   GIC 190     G128-049/G128-050. The A component is Ross 243.                                 
                         NLTT 56545/56551                                                        Chm2004 
23205+1259   LDS5070     NLTT 56546/56548                                                        Chm2004 
23208+0227   STF3002     Despite the linear solution, proper motion and parallax favor a         Grv2020a
                         physical connection. Long period and/or high eccentricity possible.             
23208-5018   RST5560     Spectrum F5m Delta Del.                                                         
                         A is a close 3.4-d spectroscopic pair.                                  Tok2019a
23209+3811   ENG  86     12 And.                                                                         
23209+1643   HEI  88     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.93 +/- 0.65, 2.10, and 1.13 Msun, respectively.             Mlk2012 
23210-0148   DAE   7     NLTT 56566 LP 642-48                                                            
                         Daemgen et al. (2007) derive a distance of 22.6 +/- 6.7 pc, separation  Dae2007 
                         of 2.2 +/- 0.7 au, and predicted orbital period of 6 +/- 3 yr.                  
                         Spectral types for both stars are M4.0 +/- 0.5; masses are                      
                         0.25 +0.18/-0.11 and 0.21 +0.17/-0.09 Msun.                                     
                         Although the close binarity of 2MASS J23205766-0147373 was reported in          
                         Daemgen et al (2007) and our AstraLux data have a similar sensitivity,  Dae2007 
                         the star appears single in our images. Since the separation was only            
                         99 mas in 2005, it has presumably moved inward since then.              Jnn2012 
23212+6737   OSO 194     G241-052. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
23213+6926   LDS5078     Primary is white dwarf WD 2319+691  = GD 559.                           Far2005b
23214+0351   BAL2579     A likely plate flaw.                                                    Grv2021b
23215+3730   ES 2540     J 2407, ALI 469.                                                                
23217+0853   HJ 3185     Primary is galaxy NGC 7634.                                                     
23218-1217   HU   95     Combined magnitude from HD. Some visual observers report the pair               
                         to be brighter.                                                                 
23219+3149   BU  718     64 Peg. A is a spectroscopic binary, perhaps as a consequence of                
                         motion in the visual pair.                                                      
                         AB: Rectilinear solution by Rica & Zirm (2012).                         FMR2012i
23221+6120   B  2907     AC: The very faint companion C may have been a ghost, though it looked          
                         real on all three nights.                                               B__1963b
23224-4636   CPO 637     LDS 812.                                                                        
23226+1706   BPM2480     [PM2000] 2643200 + [PM2000] 2643193.                                    Gvr2010 
23227+6050   STI1171     SMA 189.                                                                        
23227-1502   HU  295     97 Aqr.                                                                         
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.54 +/- 0.93, 3.73, and 1.82 Msun, respectively.             Mlk2012 
23228+2208   GIC 191     G068-012/G068-007.                                                              
23228+2034   STF3007     AB: NLTT 56671/56672                                                    Chm2004 
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
23231+1219   HO  300     Removed from WDS as probably not real.                                          
23232+1226   BU 1529     CD: This measure is from the galaxy NGC 7671 near BU 1529 to            Dam2013 
                         BD+11 5002. Redesignated from AC (which was wrong) to CD and X coded.           
                         The measure of AC here is not this CD pairing.                          FyM2013 
23235+4548   STF3010     AB: NLTT 56707/56708                                                    Chm2004 
                         AB: HJL 316.                                                            HJL1986 
23237-1430   HJ 5397     B is BD-15@6411.                                                                
23238-0828   STF3008     An optical pair. A pair was measured by Harvard Observatory near        Pei1882 
                         ADS 16725: 1867.92, 194.4@, 34.09".                                             
                         H N 112.                                                                MEv2010 
23239-1747   TOK 218     dmu is explained by the newly resolved 0".5 pair. Triple, with                  
                         companion at 13".8 in 2MASS. This companion is measured with NICI as            
                         well at the same position, its colors matching a low-mass dwarf.                
                         Considering the low density of background stars, the companion is               
                         physical, although we cannot confirm it as CPM owing to the small PM            
                         of the main target.                                                     Tok2012a
23239-5349   DUN 249     B is CPD-54@10280.                                                              
23241-2146   I  1058     Reality of companion doubtful.                                                  
23244+1429   BU  719     There is an error in the declination in the original catalogue. The             
                         correct place is 231822+1349. HO 301 is identical with this pair.       Bu_1894 
                         A is a close 17.5-d spectroscopic pair.                                 Tok2019a
23244-0827   HDO9001     This is the pair described in the STF3008 note recovered.               Dam2010 
23246+4139   CHE 452     There are no obvious errors by Chevalier in applying the offset from    Che1911 
                         his plate center, but there are no pairs at Chevalier’s coordinates,    .     
                         nor coordinates found by reversing the sign of either or both offsets.  Hrt2012b
23246+0617   HJ 3190     13s f and 6' n of BD+05 5165.                                           Doo1915a
23248+6217   H 6  24     AB: H VI 24. 4 Cas.                                                             
                         CD: STI1174.                                                                    
23249+6137   STI1176     According to ADS, Stein also notes a close component (1905.79,          A__1932a
                         91.9deg, 1".2, magnitudes 10.5, 11.3)                                           
23249+4149   CHE 454     AC: A 10' error (23249+4139) in copying declination to catalog led              
                         to assigning a different designation to this companion of CHE 453.              
23250+2709   KPP3395     Reported by author that this is a bogus binary.                         Kpp2019p
23256+3326   AG  292     BDS: 11713, AG 282.                                                             
23259+4232   HJ 1877     C component is planetary nebula NGC 7662, "Copeland's Blue Snowball".           
23263+3311   OSO 195     Known companion (= 23263+3311LDS1067)                                   AlC2000 
                         at 4.33'                                                                Oso2004 
             LDS1067     G128-064. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AB: NLTT 56856/56847                                                    Chm2004 
23263+2752   JNN 139     A very close (~0.15") companion is detected, which is most likely               
                         physically bound, although this has yet to be confirmed with common             
                         proper motion.                                                          Jnn2012 
23263+0527   SCA 158     Aka BAL2991.                                                                    
23265+6038   OSO 196     G217-008. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
23266+5709   LEO  31     STI 2980.                                                                       
23266+4520   GIC 192     The pair HJ 1867 were improperly precessed before, so observers may             
                         have been looking in the wrong patch of sky. Component A of this                
                         optical triple has a very high proper motion. The proper motion of              
                         component B is quite small. The proper motion of component C is                 
                         unknown. At some point during the 20th century, the B and C components          
                         were in approximately the same position, which probably contributed to          
                         the lack of early epoch AC measures. It is possible that some of the            
                         early AB measures may have actually been measures of A,BC. A detailed           
                         analysis of this system is in Bur2003. AB = G216-044/G216-043.                  
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: NLTT 56881/56879                                                    Chm2004 
             YR   17     Aa,Ab: Rectilinear solution by Hartkopf & Mason (2013).                 Hrt2013b
23266+4520   GIC 192     AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
23266-5243   EHR  21     omi Gru. Pair appears to be comoving.                                   Ehr2010 
                         WDS designation initially corrupted to 23255-6243.                              
23269+0115   S   830     8 Psc = kap Psc. Spectrum A0pCrSi:Sr:.                                          
                         AB: H 6  62.                                                            MEv2010 
23270-0024   GRV1154     GRV1245.                                                                        
23272-5017   DUN 250     B is CD-50@13978.                                                               
                         Identified as optical and linear solution also published.               LRR2022c
23274+6027   SMA 198     A is an irregular variable.                                                     
23274+5016   OSO 197     G216-045. AF comprise the only common proper motion pair in this                
                         multiple system                                                         Oso2004 
23274+1623   BPMA257     [PM2000] 2647015 + [PM2000] 2647110.                                    Gvr2010 
23274-1736   HJ 3194     Aka ARA 511.                                                                    
23278+0451   DEA  65     NLTT 56936 + 2MASS J23274947+0450583. Primary is VZ Psc. Baron et al.           
                         (2015) estimate spectral types K2+K5 and M9 +/- 0.5, distances                  
                         64 +/-9 and 57 +3/-17 pc, masses 1.46 +/-0.09 and 0.079-0.085 Msun.     BFr2015 
23281-0228   CBL 194     AC: Originally 23281-0227 CBL 194, but secondary found to be primary            
                         of 23281-0228 RST4724. Systems merged, with quadrant flip.                      
23283+0604   H 5  48     H V 48. B is BD+05@5174.                                                        
23284+1432   BPM2481     [PM2000] 2647834 + [PM2000] 2647948.                                    Gvr2010 
23286+1301   BPM2482     [PM2000] 2647997 + [PM2000] 2647988.                                    Gvr2010 
23287+1157   A  1239     CHE, ADS 16834 is identical to A 1239 with a mistake in position.               
23287+0703   CRB  22     BC: Originally listed as separate pair 23288+0703, before its                   
                         affiliation with CBL 549 was noted.                                             
23289+1741   BPM2484     [PM2000] 2648224 + [PM2000] 2648201.                                    Gvr2010 
23289+1720   HJ  311     AC: The C component is n the galaxy NGC 7681.                           Dam2013 
23289+1626   BPM2483     [PM2000] 2648199 + [PM2000] 2648240.                                    Gvr2010 
23294+4128   GIC 193     G190-028/G190-027 =  GJ 4337A+4338B                                             
23297+5457   STI2987     V357 Cas. Primary is Beta Lyr type eclipsing binary, period1.58867d.    Zas2017b
23299-5213   BRT2104     CD-52@10438.                                                                    
                         A likely plate flaw.                                                    Grv2021b
23300+5833   STT 496     AC: BDS 12349. A is the Algol-type system AR Cas.                               
             DA    2     CD: Additional notes may be found in Worley (1967).                     Wor1967b
23300-5419   HJ 5401     B is CPD-55@10034.                                                              
23301+3557   J  3197     ALI 238.                                                                        
23304+3050   BU 1266     Triple-lined; both visual components are double-lined spectroscopic             
                         binaries, P = 1.92 and 13.04d resp. Suspected light variation of the            
                         system is unconfirmed.                                                          
             STF3018     Fekel (1986 private communication) reports that he has now detected             
                         four components in the spectrum of this star.                                   
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
23305-2231   ARA2289     AC: Also known as AOT 123.                                                      
23306+1432   BPM2485     [PM2000] 2649501 + [PM2000] 2649488.                                    Gvr2010 
23307+0515   STF3019     H N 137.                                                                MEv2010 
23309+5825   STF3022     AB: H 4  65.                                                            MEv2010 
                         AB: Additional notes may be found in Burnham (1894).                    Bu_1894 
23309+2747   LDS5097     NLTT 57090/57088                                                        Chm2004 
23309-5807   SHY 833     AC: HIP 116056 + HIP 116387.                                                    
23310-6905   HJ 5402     B is CPD-69@3324.                                                               
                         Primary is PMS star, X-ray source.                                      Tok2014d
23311+0841   GIC 194     G029-039/G029-040.                                                              
23313+5225   STT 498     Aa,Ab: The Guillaume 1913 measure is supposed to refer to this object.  Gui1932A
23313+3914   WIS 387     = 14 And = Veritate.                                                            
                         CHARA Array Limb-darkened diameter  1.336 +/- 0.009 mas.                CIA2009a
                         R = 11.38 +/- 0.26 \rsun, L =  63.3 +/-  1.8 \lsun,                             
                         Teff = 4826 +/-  40 K.                                                          
23315-0405   KO    3     Triple, with wide pair a CPM pair. The primary is an F8 dwarf, the BC           
                         pair (CLO   4BC) comprised of an M8.0V+L3.0V. Data sources: Palomar             
                         Sky Survey red (1951.9), UK Schmidt blue (1982.8), UK Schmidt red               
                         (1988.8), UK Schmidt near-IR (1994.5), 2MASS (1998.8), DENIS I                  
                         (1999.8).  Mean separation of wide pair (1951-1999) 7.530 +/- 0.007             
                         arcmin. Masses of the three components estimated at 1.02 +0.07/-0.06,           
                         0.088 +/- 0.002, and 0.072 +/- 0.001 Msun, respectively                 Cab2007b
23315-2857   B   602     Measures uncertain, too close. Needs speckle.                                   
23317+1956   WIR   1     This is the flare star EQ Peg. Component B is suspected to be the               
                         source of the flares, although both components may be flare stars.              
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Additional notes may be found in Wilson (1954).                     WRH1954a
             LMP  24     AC: Rectilinear solution by Mason & Hartkopf (2016).                    Msn2016a
23317-0245   LWR  20     AF Psc                                                                          
                         There is a possible companion at 19" noted in Lowrance et al. (2005),   Lwr2005 
                         but it has not been checked for common proper motion.                   Jnn2012 
23319+5401   ES  109     A and B are 1mag below MS in (J,J-K). Parallax <16mas or subdwarfs?     Tok2014d
23320+4349   STF3024     H 2  94.                                                                MEv2010 
                         Primary is V389 And, an Algol-type eclipsing binary, P = 25.77827d.     Zas2012 
23322+1458   HDS3353     DI Peg.                                                                         
23322+0705   HU  298     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.47 +/- 0.60, 2.85, and 1.13 Msun, respectively.             Mlk2012 
23323+5111   OL   84     Aka TDT4088.                                                                    
23324-2155   LDS5098     NLTT 57164/57165                                                        Chm2004 
23325+2200   HLM  41     Aka GRV 670.                                                            Dam2010 
23328+2205   ELS   6     Aka DAM 252                                                                     
23328-1645   VOU  28     BC: The 1962 measure by van den Bos may not refer to this pair.         B__1963b
23328-1651   LDS 816     See BC (VOU 28) at 23328-1645                                           Kui1943 
                         A,BC: NLTT 57183/57180                                                  Chm2004 
             SHY 110     AE: HIP 116215 + HIP 116003.                                                    
23331+4556   OSO 198     G216-052. Neither AB nor AD is a common proper motion pair, based on            
                         comparison with POSS2 red plates                                        Oso2004 
23331-2127   HDO 177     BD-22@6147?                                                                     
23332+5724   STT 499     A,BC: HJL 317.                                                          HJL1986 
23333-2055   B  1900     101 Aqr.                                                                        
23334+4251   HDS3356     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.84 +/- 0.20, 1.83, and 1.05 Msun, respectively.             Mlk2012 
23334-1240   LDS2989     NLTT 57205/57204                                                        Chm2004 
23336+6028   STFA 60     AB: Pair appears in an appendix list, not part of the discoverer's              
                         regular numbering sequence.                                                     
23336+3234   OSO 199     G128-077. AB is a common proper motion pair, but AC is not, based on            
                         astrometry and color                                                    Oso2004 
23336+1749   LOS   1     Discovered while observing HO  655. A component is GSC 1723 2167.               
                         Magnitude of B estimated at 11.5.                                               
             HO  655     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
23339-3340   SEE 491     Jessup claims A is double, but gives no data.                           Jsp1964 
23340+3120   BU  720     Variable?                                                               Egg1947 
                         Only elements P and T have been amended by Starikova (1982) from the    Sta1982b
                         orbit of Baize (1976).                                                  Baz1976 
                         Elements published for this long-period system differ: Costa (1966              
                         Urania, Barcelona 51, 73) quotes P = 198.6 yr, while Tel'nyuk-Adamchuk  TkA1966 
                         gives P = 425 yr. The observed theta and rho for 1975.953 are in                
                         reasonable agreement with either uncertain orbit.                       BLM1978 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
23340+0334   BAL2581     2001 speckle measure actually a new pair, 23344+0331 = WSI 155.         WSI2015 
23341+5947   HJ 1892     KR   65.                                                                        
23341-3511   BRT3371     A likely plate flaw.                                                    Grv2021b
23342+0218   A  2499     Companion only seen in 1911, and not in 1921, 1933, and 1934.                   
23344+2739   LDS1069     This star has a possible wide companion at about 63" as noted in the            
                         WDS. It is however single in the separation range covered by the                
                         AstraLux data.                                                          Jnn2012 
23344+0331   WSI 155     2001 speckle measure of 23340+0334 = BAL2581 is actually this new pair. WSI2015 
23346-1647   LDS2990     NLTT 57262/57259                                                        Chm2004 
23347+3748   YSC 139     Data at hand suggest that this F8 pair with small magnitude difference          
                         is viewed nearly edge-on. The mass implied by the spectral type is              
                         perhaps 2-2.5 Msun, if the system were to have solar metallicity,               
                         again lower than that implied by the orbital elements. The metallicity          
                         of the system is -0.31 according to the Geneva-Copenhagen Catalog               
                         (Nordstrom et al. 2004), which would tend to lower the mass at a given  Nrd2004 
                         spectral type, thus making the discrepancy worse. Nonetheless, given            
                         the large uncertainty in dynamical mass, it is no worse than a 2 sigma          
                         difference at this point. The mass ratio in the Geneva-Copenhagen               
                         catalog is 0.9, so this at least is consistent with the small                   
                         magnitude difference obtained from speckle measures.                    Hor2015b
                         Orbit determined by fitting revised Hipparcos intermediate astrometric          
                         data. Derived component masses 1.64 +/- 0.29 and 0.90 +/- 0.15 Msun.    Ren2010 
                         Unclear if the SB2 orbit presented here is for this pair on another     Kie2018 
                         unresolved component.                                                           
                         A: Teff = 6227 +/- 68 K, B: Teff = 5915 +/- 10.                                 
23349+1124   BPM2486     [PM2000] 2652674 + [PM2000] 2652662.                                    Gvr2010 
23350+3302   OSO 200     G128-080. Not a common proper motion pair, based on color and                   
                         comparison with POSS2 red plates.                                       Oso2004 
23350+0136   MEL   9     GJ 900                                                                          
                         Malogolovets et al. (2007) combine all data to derive I-, K-, and       Mlg2007b
                         H-band absolute magnitudes for all three components, as well as                 
                         spectral types and masses:                                                      
                                 I  +/-     K  +/-    H   +/-   spec   mass (Msun)                       
                           A:  6.66 0.08  4.84 0.08  5.11 0.08  K5-K7  0.64 - 0.67                       
                           B:  9.15 0.11  6.76 0.20  6.85 0.09  M3-M4  0.28 - 0.34                       
                           C: 10.08 0.26  7.39 0.31  7.54 0.15  M5-M6  0.16 - 0.24                       
                         BC probably form inner short-period (~20y) pair moving with A around            
                         mass center; A,BC period ~80y. Observed configuration may be due to             
                         relative tilts of orbital planes. 2MASS images show faint objects ~12"          
                         northeast and 15" south of primary; stars are probably late M dwarfs            
                         and possibly members of the GJ 900 system.                                      
23351-4237   B   603     iot Phe. A variable of the Alpha CVn-type, spectrum A2VpSrCrEu.                 
             SHY 834     AC: HIP 116389 + HIP 116370.                                                    
23352+1240   BPM2487     [PM2000] 2652884 + [PM2000] 2652864.                                    Gvr2010 
23352-1135   BU   81     Spectrum: Fm Delta Del.                                                         
23352-6441   HJ 5403     B is CPD-65@4149.                                                               
23355+3101   LDS6405     HIP 116421. See Allen et al. (2000) for information on metallicity,     AlC2000 
                         age, galactic orbital parameters, etc.                                          
23355+0850   BRT3372     J 2408.                                                                         
23356+1524   BPM2488     [PM2000] 2653195 + [PM2000] 2653232.                                    Gvr2010 
23356+0823   VIG  22     The B component appears to be a faint background star.                  Vig2012 
23357+3425   ES 2273     ES 2397.                                                                        
23357-2729   SEE 492     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.03 +/- 0.32, 2.10, and 1.07 Msun, respectively.             Mlk2012 
23358+0027   OSO 201     G029-050.                                                                       
23358-5832   RST5174     CD-59@8165.                                                                     
23359+1440   GRV1246     SLW1327.                                                                        
23361-3237   B   604     CM Scl, Algol-type eclipsing binary, P = 10.28857 d.                    Zas2011 
23363-0707   BU  721     Elongations real, but too slight for reliable angles.                   B__1959a
23364+0206   THP   1     16 Psc                                                                          
                         SB, period 45d, according to Cayrel de Strobel (1974 A&A 37, 179).              
                         Observed during occultation by asteroid 7 Iris. Separation and                  
                         position angle for 2006.342 constrained to two possibilities, under             
                         assumption asteroid has circular silhouette.                            Thp2006 
23366+5958   OSO 202     G241-060. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
23370+0630   BRT2195     J 1730.                                                                         
23371+3927   A  1492     Closely sf BD+38@5037.                                                          
23373-2056   RSS 580     CPD-21@8282                                                                     
23375+4426   STT 500     A premature orbit has been computed.                                            
23375-4021   WG  289     BRT1133.                                                                Brt1933 
23376+5516   STI3010     SMA 202.                                                                        
23376+4627   STT 600     lam And = 16 And. A is a spectroscopic binary and light variable.               
                         NPOI Limb-darkened diameter    2.772 +/- 0.012 mas,                             
                         R =    7.72 (+/- 0.04   )  \rsun,  Teff = 4532 +/-  10 K,                       
                         L =   22.7 +/-   0.1 \lsun.                                             NOI2023 
23376+1236   HJ  315     HJL 318.                                                                HJL1986 
23377+1650   ENG  87     74 Peg. A is a spectroscopic binary.                                            
23377-1304   HJ  316     Aka H N  35 = BDS 12465.                                                Bu_1906 
             BU 1530     CD: This measure is from the galaxy NGC 7723 near BU 1530 to a nearby   Dam2013 
                         star. Redesignated from AC (which was wrong) to CD and X coded.                 
23379+1824   KUI 117     75 Peg. A is a spectroscopic binary.                                            
23382+5514   A  1493     A premature orbit has been computed.                                            
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.23 +/- 2.09, 3.30, and 2.24 Msun, respectively.             Mlk2012 
23386+1124   BPM2489     [PM2000] 2655505 + [PM2000] 2655562.                                    Gvr2010 
23387+1544   BPM2490     [PM2000] 2655551 + [PM2000] 2655564.                                    Gvr2010 
23388+4424   D    26     V392 And, Algol-type eclipsing binary, P = 4.046275 d.                  Zas2011 
23388-2816   B   608     Direct motion? Measures uncertain, too close. Needs speckle.                    
23389+2101   LDS5108     NLTT 57506/57507                                                        Chm2004 
23389-0310   BRT 525     Aka J  3354.                                                            Dam2016d
23389-4537   SHY 836     HIP 116602 + HIP 116699.                                                        
23390+3932   MLB 911     ALI 1004.                                                                       
23392-1831   BHA  55     J 1425.                                                                         
23393+7738   NHR   9     = Gam Cep = Errai.                                                              
                         Neuhauser et al. (2007)resolved the wide pair of the gam Cep triple             
                         system using the Subaru AO system. Their combined solution yielded              
                         masses for Aa and B of 1.40 +/- 0.12 and 0.409 +/- 0.018 Msun, plus a           
                         mass function for the planetary companion (M_Ab sin i) of 1.60 +/-              
                         0.13 Mjup. Physical separation for the AB pair is 20.18 +/- 0.66 au.    Nhr2007 
                         NPOI Limb-darkened diameter 3.24 +/- 0.03 mas,                          NOI1999 
                         R = 4.79 +/- 0.06 \rsun.                                                        
                         CHARA Array Limb-darkened diameter  3.302 +/- 0.029 mas.                CIA2009a
                         R =  5.01 +/- 0.05 \rsun, L =  11.4 +/-  0.0 \lsun,                             
                         Teff = 4744 +/-  21 K.                                                          
                         NPOI Limb-darkened diameter 3.254 +/- 0.020 mas, Sp = K1III,            NOI2018 
                         R = 4.93 +/- 0.04 \rsun, Teff = 4792 +/- 62 K, L = 11.6 +/- 0.6 \lsun,          
                         M = 1.41 +/- 0.08 \msun, Age = 3.25 +/- 0.63 Gyr.                               
23393+4543   CHR 149     1986.8914: This "prediscovery" confirmation was found by reexamination          
                         of archival data.                                                       McA1990 
                         Balega et al. (2004) notes that it is the B component of A   643, not   Bag2004 
                         the A component, which is comprised of the CHR 149 pair. The component          
                         designation has been changed from Aa,Ab to Ba,Bb accordingly.                   
                         Zhuchkov et al. (2008) give combined spectroscopic/astrometric orbits   Zhu2008 
                         for both wide and close pair.  Spectral types for A, Ba, and Bb are             
                         determined as G0III, F3III, and sdO-BVIII, respectively.  Magnitudes            
                         (assuming an integrated system magnitude of 7.63) are 8.53 +/- 0.03,            
                         8.66 +/- 0.04, and 9.51 +/- 0.05, while indiviual masses are estimated          
                         at 1.3 +/- 0.3, 1.3 +/- 0.3, and 0.7 +/- 0.4 Msun.                              
23395+6658   HJ 1897     Proper motion from Greenwich possibly reversed.                                 
23395-4638   DUN 251     the Phe                                                                         
                         RMK  27. Rectilinear solution by Letchford et al. (2018).               LRR2018a
                         Despite the linear solution, proper motion and parallax favor a         Grv2020a
                         physical connection. Long period and/or high eccentricity possible.             
23397+1153   BPM2491     [PM2000] 2656281 + [PM2000] 2656234.                                    Gvr2010 
23397+0331   BAL2069     HJL 319.                                                                HJL1986 
23398-0420   HWE  99     B is BD-05@6031.                                                                
23399+6419   ES  149     AB: HJL 320.                                                            HJL1986 
23399+5517   STI3015     SMA 203.                                                                        
23399+0538   BUP 240     iot Psc = 17 Psc.                                                               
                         AB: Rectilinear solution by Friedman et al. (2011).                     USN2011a
23400+5446   STI3016     Also known as SMA 204.                                                          
23404+4420   HJ 1898     kap And = 19 And.                                                               
             CSN   1     Aa,Ab: Carson et al. (2012) discovered a "super Jupiter" orbiting kap           
                         And. Spectral types are B9IV and L2-L8, masses 2.4-2.5 Msun and 12.8            
                         +2.0/-1.0 Mjup, assuming a system age 30 +20/-10 Myr (Marois et al.             
                         2010 Nature 468, 1080).                                                 Csn2013 
                         Aa,Ab: Hinkley et al. (2013) derive a spectral type L1 +/- 1, Teff =            
                         2040 +/- 60K, mass 50 +16/-13 Mjup, and age 220 +/- 100 Myr for the Ab          
                         companion of the B9IV star kap And. The primary has a mass of 2.8               
                         +0.1/-0.2 Msun, Teff 11361 +/- 66K, radius 2.29 +/- 0.06 Rsun, age              
                         the same as that of Ab. Results are based on spectroscopy obtained              
                         using a high-contrast imaging platform. They also conclude that the B           
                         and C stars in this system are not comoving with the A component.       Hnk2013 
                         Aa,Ab: Bonnefoy et al. (2014) derive spectral types B9IVn and M9-L3:,           
                         plus log luminosities 1.83 +/- 0.04and -3.76 +/- 0.06. The mass of the          
                         primary is estimated at 2.6 +/- 0.2 Msun; the secondary is 0.013                
                         +0.022/-0.001 Msun for a "hot-start" evolutionary model, >0.011 Msun            
                         for a "warm-start" model.                                               Bnf2014 
23406+5513   HJ 1899     BDS 12513, HJ 1901 same star.                                                   
23407-0023   STF3030     H N  91.                                                                MEv2010 
23409+2022   HO  303     Hough notes that STT 503 follows 1m13s and 3' S.                        Ho_1890 
                         AC: The C component measured by Burnham may be one of two stars in the  Bu_1913 
                         field. However, neither is in very good agreement with his measure,             
                         even after accounting for changes due to proper motion.                         
23411+4613   MLR   4     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.16 +/- 0.28, 2.61, and 1.13 Msun, respectively.             Mlk2012 
23412+7409   HJ 1905     AB: Rectilinear solution by Hurowitz et al. (2014).                     USN2014b
23412+1647   GRV 683     HJL 322.                                                                HJL1986 
23412+0616   STF3031     B is BD+05@5208.                                                                
                         HJL 321.                                                                HJL1986 
                         H N 136.                                                                MEv2010 
23413+4954   ES 2732     Also known as ES 2731.                                                          
23414+5925   OSO 203     G241-064. None is a common proper motion pair, based on comparison              
                         with POSS2 red plates.                                                  Oso2004 
23414-3205   LDS2992     NLTT 57627/57628                                                        Chm2004 
23415+5955   FOX  50AB   2MASS images seem to indicate this is a close 2" pair, but not          Skf2018f
                         measured yet.                                                                   
23418-1749   HJ 5413     104 Aqr. A spectroscopic binary. B is BD-18@6359.                               
23419-0559   LDS5112     NLTT 57682/57675                                                        Chm2004 
                         AB: Primary is exoplanet host, P=572d. A=SB?                            Tok2014d
             GC 32912    A: Combined solution, based on reduction of Hipparcos intermediate              
                         astrometric data together with spectroscopic elements from Vogt et al.  CPS2000c
                         (2000).                                                                 HaI2001 
23424+4956   HJ 1903     Herschel's 1828 measure than with Espin's in 1912.                      Es_1914 
23424-1357   LDS2995     NLTT 57711/57710                                                        Chm2004 
23427-1433   BU  279     ome 2 Aqr = 105 Aqr. A is a spectroscopic binary.                               
                         Uniform disk diameter  0.338 +/- 0.018 mas,                                     
                         Limb darkened diameter 0.348 +/- 0.018 mas,                                     
                         Teff = 11000 +/- 1300 K based on LDD.                                           
                         Radius is 1.82 +/- 0.10 \rsun.                                          CIA2019a
23430-2407   LDS 823     Proper motion +1270 -2200.                                                      
                         NLTT 57749/57756                                                        Chm2004 
23431+1150   A  1242     A premature orbit has been computed.                                    Baz1944a
23432+5455   ES 1048     DE: Also known as STI3022.                                                      
23432-0837   FOX 276     J 1426.                                                                         
23433-7049   HJ 5415     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
23434+0532   J   299     Jonckheere unable to recover.                                           J__1962a
23438-1517   HEG   2     R Aqr. Binary system consists of a Mira-type and a white dwarf                  
                         companion, estimated P=44yr (Willson, L.A., Garnavich, P., & Mattei,            
                         J.A. 1981 IBVS 1961, 1). Hollis et al. (1997) give preliminary orbital  HJM1997 
                         elements for the AB pair: P=44y, e=0.8, T=JD2442100.0, i=70deg,                 
                         Omega~90deg, omega = +/-90dega = 2.54e14cm for system mass 2.5 Msun,            
                         2.69e14cm for 3.0Msun.                                                          
23439+3232   LDS1070     Listed as double in ApJ 112, 214. L 1512-34a.                                   
                         AB: Secondary is white dwarf WD 2341+322.                               Far2005b
23440+2922   AGC  14     78 Peg.                                                                         
23441+6147   STI1204     A is a semiregular variable, PZ Cas. B is a Cepheid.                            
                         Also known as MLR 515.                                                          
23441-0254   BRT 526     A likely plate flaw.                                                    Grv2021b
23442+4923   LDS5116     NLTT 57825/57826                                                        Chm2004 
23444-1802   FEN  43     A likely plate flaw.                                                    Grv2021b
23445+4623   STF3034     Primary is V395 And, eclipsing binary of W UMa -type, period 0.6847 d.  Zas2012 
23448+5627   BAR  64     BC: STI3024                                                                     
23449+4831   ES  549     AB: Later measures were incorrectly added as the new pair ABH 179AD,            
                         due to the high proper motion of the primary and the long timespan              
                         between observations.                                                           
23449+1543   BPM2492     [PM2000] 2660049 + [PM2000] 2660092.                                    Gvr2010 
23450+3020   OSO 204     G130-007. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
23451+1459   JNN 140     G 68-39.                                                                        
                         Due to the compact configuration of the three components resolved by            
                         AstraLux, this is almost certainly a physically bound triple system.            
                         Only one epoch of images exist so far, hence common proper motion has           
                         not yet been demonstrated.                                              Jnn2012 
23454+1547   BPM2493     [PM2000] 2660398 + [PM2000] 2660323.                                    Gvr2010 
23456+1309   HJL1116     A combined interferometric/spectroscopic solution by Halbwachs et al.           
                         (2016) yields masses 1.686 +/- 0.021 and 1.390 +/- 0.034 Msun.          HJL2016 
                         Mass = 1.647  +/- 0.022 , 1.316   +/- 0.034   \msun for A and B.        HJL2020 
                         orbital parallax =  8.551 +/- 0.080 mas.                                        
23459+1941   GRV 691     HJL 323.                                                                HJL1986 
23460+4625   MCA  75     psi And = 20 And. R.H. Wilson reported a wide, faint companion.         WRH1950a
                         H. McAlister resolved the primary into a triple system.                 McA1978b
                         Aac: It is not established whether this third component belongs to Aa           
                         or Ab.                                                                          
                         Based on mean motion of Aa,Ac a period of ~300 years is postulated.     Tok2010b
                         Based on the separation of Aa,Ab relative to this dynamic stability             
                         is questioned, however Aa,Ab has only been measured four times while            
                         Aa,Ac has been measured 39. Is Aa,Ab of a larger delta-m and if not             
                         why is it so infrequently measured. Could it be spurious?                       
23460-1841   H 2  24     H II 24. 107 Aqr = i 2 Aqr. Alternative spectrum: F2III+F2V.                    
23461+6028   STF3037     E is BD+59@2769a.                                                               
23461+5040   STTA248     B is BD+49@4216.                                                                
23462+6240   STF3038     The John Herschel measure identified with this pair may go with         HJ_1831 
                         23463+6201STI1209 which it fits a little better. The measure is "T"             
                         coded with both systems.                                                        
23462+3515   OSO 205     G130-010. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
23463+6201   STI1209     The John Herschel measure identified with this pair may go with         HJ_1831 
                         23462+6240STF3038, which Herschel identified the measure with. It               
                         fits better here.                                                               
23464+1324   BPM2495     [PM2000] 2661188 + [PM2000] 2661265.                                    Gvr2010 
23464+1243   BPM2494     [PM2000] 2661128 + [PM2000] 2661130.                                    Gvr2010 
23464-2302   TOK 375     First resolution at 0".15; estimated period 12 y.                       Tok2013b
23465+1724   BPM2496     [PM2000] 2661247 + [PM2000] 2661243.                                    Gvr2010 
23465-4135   TOK 922     SX Phe.                                                                         
23465-7159   HJ 5419     B is CPD-72@2782.                                                               
23466-0900   TOK 220     Resolved on 2011.85 and found here at nearly the same position,                 
                         despite estimated period of 20yr. Seen in projection?                   Tok2013b
23467+6236   VBS  40     STI 1212.                                                                       
23469+2825   STF3039     AB: H 4 107.                                                            MEv2010 
23471-1921   DON1053     BHA 56.                                                                         
23472-2624   LDS5121     NLTT 57957/57958                                                        Chm2004 
23474-2217   I   696     CD-22@16450.                                                                    
23475+2535   BU  727     In my Tenth Catalogue where this pair originally appeared, the printed          
                         distance should be multiplied by two.                                   Bu_1894 
23476+4650   BU  995     A is a spectroscopic binary. One component is variable.                         
23476-6031   COO 261     RMK  28. Rectilinear solution by Letchford et al. (2018).               LRR2018a
23479+1703   STF3041     STTA249.                                                                        
23479+0624   GIC 195     G030-015/G029-067. The B component is variable star DO Psc.                     
23479-0246   S   835     20 Psc.                                                                         
23484-2141   ARA1950     Possibly = HDO 179, suspected binary of Win1882.                                
23485+2539   DSG   8     For the Horch et al. (2015) combined solution, spectroscopic elements           
                         are fixed to those of Griffin (2007). Assigned spectral types are       Grf2007 
                         F5V and F5.5V; derived masses 1.40 and 1.37 Msun.                       Hor2015 
23487+6453   STT 507     STTA250.                                                                        
23488+6213   STT 508     6 Cas. The variable V566 Cas.                                                   
                         Aitken notes that Guillaume gives his 1923 measure without              Gui1932A
                         identification and that the other Guillaume measure goes with           A__1932a
                         STT 508AC. The pair was assigned the designation GUI 39, but nothing            
                         matching his separation and angle can be found in the vicinity of STT           
                         508. The GUI 39 designation has therefore been removed, under the               
                         assumption that Guillaume's measure was of STT 508 but there was some           
                         typographical error in his original reference. This assumption is               
                         supported by the fact that his angle of 19.5 could instead be 195, in           
                         good agreement with contemporaneous measures of the Struve AB pair, as          
                         well as the match of his wider pair with the Struve AC pair.                    
23489-2509   SHY 839     HIP 117454 + HIP 117720.                                                        
23489-2808   BU 1013     del Scl                                                                         
23492+0459   TOK 376     First resolution at 0".20, dK=3.2.                                      Tok2013b
23496+6052   STI1222     B is BD+60@2625a.                                                               
23496-2212   B   619     CD-22@16466.                                                                    
23498+2741   A   424     Only elements P, T, and a have been amended from the orbit of           Sta1978c
                         Morel (1969).                                                           Mrl1969c
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 7.21 +/- 3.53, 5.19, and 1.40 Msun, respectively.             Mlk2012 
23500+4829   OSO 206     G171-023. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
23500+0843   OSO 207     G029-071. Not a common proper motion pair                               Oso2004 
23505+0807   CHE 505     Chevalier gave an incorrect Durchmusterung number for this pair,        Che1910 
                         leading to incorrect coordinates being added to the WDS.                Hrt2012b
23506+5412   SHY 840     AC: HIP 117573 + HIP 117733.                                                    
23506+4705   A   793     Often too close. Possible quadrant reversal about 1925.                         
23506-5142   SLR  14     High but rather imprecise mass-sum.                                     Sod1999 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.28 +/- 0.37, 1.92, and 0.95 Msun, respectively.             Mlk2012 
23509+4730   A   794     A is the semiregular variable TZ And.                                           
23509-7954   UC 5034     CPM candidate confirmed physical by photometry (2MASS and V mags).      Tok2013c
                         Primary is SB2                                                          Tok2014d
                         A is a close 4.4-d spectroscopic pair.                                  Tok2019a
23511+0214   HIP 117607  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Udry et al. (1998).                                                     Udr1998 
23512+5123   ALD   7     Not found by Heintz at IDS position.                                    Hei1990b
23513+1757   J   627     Aka COU  72.                                                            Dam2010 
23514+2344   BWL  61     AE:  Source appears spatially extended; probably a background galaxy.           
                         Primary is G 68-46.                                                     Bwl2015 
23515+2501   POU5863     J  1799.                                                                        
23516+3844   ES 2541     ALI1006.                                                                        
23516+3127   BWL   1     AB: Bowler et al. (2012) determined this pair shares CPM. At a          Bwl2012a
                         photometric distance of 50 +/- 10 pc, the projected separation is 119           
                         +/- 24 au. Spectral types are M2.0 +/- 0.5 and L0 +2/-1, masses 0.45            
                         +/- 0.05 Msun and 32 +/- 6 Mjup. Additional JHK photometry of both              
                         components was derived via synthetic photometry from spectrum                   
                         (calibrated to 2MASS), combined with NIRC2 differential photometry.     TMA2003 
                         AB: A comp is active M2.0 star. B is L0-L3, mass 32 +/- 3 Mjup.         Bwl2015 
23516+2502   POU5865     J  1800. Same as POU5866.                                                       
23516+0841   CHE 506     Chevalier gave an incorrect Durchmusterung number for this pair,        Che1910 
                         leading to incorrect coordinates being added to the WDS.                Hrt2012b
23518+1614   BPM2497     [PM2000] 2665067 + [PM2000] 2665069.                                    Gvr2010 
23518-0637   A  2700     Masses and bolometric magnitudes are derived for the two components             
                         of this system by Mason et al. (1999), based on assumed spectral types  Msn1999a
                         and available parallaxes.                                                       
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.82 +/- 0.51, 1.91, and 1.17 Msun, respectively.             Mlk2012 
23520+1252   A  1247     Linear solution first suggested and alternative linear solution in      Cve2022 
23522+6427   MLB 236     Aka STI1226.                                                                    
23524+7533   BU  996     A is a spectroscopic binary.                                                    
23525-0924   OSO 208     G273-152. Common proper motion pair.                                    Oso2004 
23527+6042   BU 1153     D component is primary of 23531+6042 STT 511.                                   
23527+2259   BU  859     The primary is the Zeta Aur binary V413 And. With a period of 50.1d             
                         this cannot be the apparently common proper motion binary BU  859.              
                         The spectral type of the primary is G7III+F2IIIm.                               
23527-0328   LDS3001     NLTT 58251/58250                                                        Chm2004 
23527-4254   I   144     DP Gru, Algol-type eclipsing binary, period 3.80343 d.                  Zas2018 
23528+5548   HJ 1914     STI3050.                                                                        
23529-0309   FIN 359     24 Psc.                                                                         
                         Mason et al. (1997) orbit includes mass determination.                  Msn1997a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.87 +/- 0.56, 2.69, and 2.75 Msun, respectively.             Mlk2012 
23530+4121   ARG 108     B is BD+40@5169.                                                                
23530+1155   STF3044     A purported FYM 5AC pair has been removed on request of the author.     FyM2014b
23532-0830   LDS3003     NLTT 58273/58274                                                        Chm2004 
23536+5131   STTA251     AB: Pair appears in an appendix list, not part of the discoverer's              
                         regular numbering sequence.                                                     
23537-0140   HJ 3223     B is BD-02@6055.                                                                
23537-4926   I  1476     Measures uncertain, too close.                                                  
23537-6557   HJ 5428     Pair bound. Near-IR colors indicate B component has a K9.5-M2.5                 
                         spectral type and a mass of 0.53 +/- 0.01 Msun.                         Egn2007 
             SHY 108     AC: HIP 117815 + HIP 114996. C component is gam Tuc.                            
                         The C component is the much closer double 23174-5814 = GAT  31.                 
23538-3729   LDS 825     LDS6407.                                                                        
23540+6522   LDS5135     Aka SLN 101.                                                                    
23541+3917   HO  205     V413 And. Primary is eclipsing binary of Algol-type, period 53.1d.      Zas2017b
23541-3317   LDS 826     AB: Primary is white dwarf WD 2351-335.                                 Far2005b
             SOZ   2     AC: CPM companion to red dwarf / white dwarf pair LHS 4039 / 4040 is            
                         an M8.5 dwarf; estimated distance 19.5 pc.                              Soz2004 
23542+3739   OL    7     ES 2004.                                                                        
23544-2703   LAL 192     phi Scl, a spectroscopic binary. Originally known as DUN 253 in         Dun1829 
                         Dunlop's original list and the ADS, the discovery designation of this   A__1932a
                         was changed at Lick for an unknown reason.                              IDS1963A
23545+2938   LEP 115     NI   50.                                                                        
23549+2929   STTA252     B is BD+28@4667.                                                                
23553+5144   ES 2735     AC: Measures in 1911 by Espin, and in 1919 by Olivier, disagree, as     Es_1912 
                         noted by Aitken. The Olivier measure was later assigned to              Ol_1920a
                         23562+5138 ALD 123.                                                     A__1932a
23554-5845   HJ 5432     B is CPD-59@7939.                                                               
23555+1755   BFR  14     TYC 1725 00344 1 + 2MASS J2355345 +175404. Baron et al. (2015)                  
                         estimate spectral types G5III and M9.0 +/- 0.5, distances 40 +28/-15            
                         and 103 +10/-37 pc, masses 1.91 +/-0.11 and 0.079-0.085 Msun.           BFr2015 
23555-7749   JSP 854     aka TDT4274.                                                            Dam2016f
23556+0042   LEP 116     NI   51.                                                                        
23558+1718   BPM2498     [PM2000] 2667910 + [PM2000] 2667843.                                    Gvr2010 
23561+2520   A   426     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.14 +/- 1.55, 2.44, and 1.05 Msun, respectively.             Mlk2012 
23562+5946   OSO 209     G217-024. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates.                                                  Oso2004 
             LEP 117     AD: CPM pair. D component is white dwarf candidate.                     Tok2014d
23564-0930   STF3046     AB: NLTT 58475/58476                                                    Chm2004 
23564-0930   STF3046AB   Despite the linear solution, proper motion and parallax favor a         Grv2020a
                         physical connection. Long period and/or high eccentricity possible.             
23565-0035   HJ  994     Aka WEI  44.                                                                    
23566+1855   BRT2518     Aka J  3355.                                                            Dam2016d
23566-5018   TOK 377     First resolution; estimated period 75 yr.                               Tok2013b
23568+0444   A  2100     This system has a Delta m of 0.9 +/- 0.4 in the blue, as determined             
                         from lunar occultation measures by Africano (1975).                     Afr1975 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.41 +/- 0.66, 3.38, and 1.45 Msun, respectively.             Mlk2012 
23568-4304   CPO 101     LDS 829.                                                                        
23570+2305   GIC 196     G129-045/G129-046.                                                              
23570-2836   LDS2065     NLTT 58501/58508                                                        Chm2004 
23571+5542   CIA  12     V1022 Cas.                                                              CIA2019b
                         A: M = 1.626+/-0.005 \msun, R = 2.65+/-0.21 \rsun, Teff = 6450+/-120 K, CIA2018c
                         B:   = 1.608+/-0.005          = 2.47+/-0.23               6590+/-110            
                         orbital parallax = 63.98+/-0.26 pc.                                             
23571-0147   BRT 528     A likely plate flaw.                                                    Grv2021b
23572-1631   LDS 831     NLTT 58517/58518                                                        Chm2004 
23573+6102   STT 512     CD: Also recorded as D 28, BDS 12659 and TDS1229.                               
23573-1259   LDS 830     NLTT 58528/58527                                                        Chm2004 
23575+1131   BPMA258     [PM2000] 2669134 + [PM2000] 2669021.                                    Gvr2010 
23576+6243   KRV  34     Classical Cepheid DD Cas.                                                       
23576-6418   EHR  22     Primary is eta Tuc.                                                     Ehr2010 
                         Ba,Bb: Physical/optical nature unknown.                                         
23578+2508   MCA  76     psi Peg = 84 Peg                                                                
23579+1557   RUC  16     U Peg. Spectral type of resolved companion later than M5V.              Ruc2007 
23579-1700   LDS5143     NLTT 58570/58571                                                        Chm2004 
23581+6112   LEO  55     Both components are Classical Cepheids: CE Cas A and CE Cas B.                  
23581+2840   HJ  995     Decided change; probably the measures of HO in 1893 belong to this.     Doo1915a
                         Rectilinear solution by Cvetkovic (2011).                               Cve2011c
                                                                                                         
23581+2420   STF3048     AB: NLTT 58582/58579                                                    Chm2004 
                         AB: HJL 324.                                                            HJL1986 
             GIC 197     DE: NLTT 58602/58601                                                    Chm2004 
23582-1725   DAE   8     NLTT 58589 = LP 746-40                                                          
                         Daemgen et al. (2007) derive a distance of 26.1 +/- 2.0 pc, separation  Dae2007 
                         of 49.7 +/- 3.8 au, and predicted orbital period of 477+/- 58 yr.               
                         Spectral types are M2.0 +/- 0.5 and M2.0 +/- 0.5; masses for both are           
                         0.45 +/- 0.05 Msun.                                                             
23582-2756   HJ 3228     LDS2067.                                                                        
23582-5712   GC 33239    Hipparcos astrometric solution assumes circular orbit (e = omega = 0).  HIP1997d
23584+5123   ES   37     R Cas                                                                           
23586-1408   RST4136     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 4.86 +/- 1.99, 3.15, and 1.35 Msun, respectively.  Mlk2012 
23587+4644   BAG  34     is also a spectroscopic binary with a P of 873d.                        Tok2019b
23587-0333   BU  730     27 Psc                                                                          
23588+3345   RAO  77     Triple system. The inner SB has P = 25.4 days (Latham et al. 2002),     Lat2002 
                         the Robo-AO companion at 5" is seen at a constant position despite              
                         PM(A) = 0".3/y, while its color places it on the MS.                    Rbr2015d
23588+3156   RAO  76     A is SB and astrometric binary.                                         Tok2014d
                         Previously thought to be a binary, but our observations reveal that             
                         it is actually a triple system. The outer component B at 4".8 was               
                         discovered by Robo-AO and confirmed by the 2MASS image and by the new           
                         data presented here. It is located near the low end of the MS. The              
                         main star with astrometric acceleration (Makarov & Kaplan 2005) is      Mkr2005 
                         now resolved at 0".4, corresponding to an orbital period of ~100 yr.            
                         The new component Ab is too faint for its detection in the i' band              
                         with Robo-AO.                                                           Rbr2015d
             RBR  55     Aa,Ab: incorrectly labelled RBR 30 in Table 1 of Roberts et al.         Rbr2015d
23590+5545   STF3049     AB: sig Cas = 8 Cas                                                             
                         AB: H 1   5.                                                            MEv2010 
23592+4112   HO  207     Aka COU 1500.                                                                   
             HJL1113     AC: SHY 376. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
23595+3343   STF3050     AB: H N  58.                                                            MEv2010 
                         AB: Additional notes may be found in Couteau (1952).                    Cou1952a
23597-3500   B  2511     BC: WSP   8.                                                                    
23598+1744   BPM2499     [PM2000] 2670806 + [PM2000] 2670809.                                    Gvr2010