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 544Â 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 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 HD 27149 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 BAS 3 Hyad - Melotte 25 VA 201 = vB 34.
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
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
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
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