INTERNATIONAL ASTRONOMICAL UNION COMMISSION 26 (DOUBLE STARS)
INFORMATION CIRCULAR No. 185 (FEBRUARY 2015)
NEW ORBITS
ADS Name P (yr) T e W(2000) 2014 Author
RA 2000 DEC n (deg) a (") i (deg) w (deg) Last ob. 2015
---------------------------------------------------------------------------------------------
32 STF3056AB 545. 2142.0 0.670 136.4 141.9 0.709 ZIRM
00047+3416 0.6606 0.623 99.4 119.6 2009.8 141.9 0.708
147 BU 255 245. 2067.2 0.960 166.1 66.3 0.445 ZIRM
00118+2825 1.4694 0.661 116.0 265.4 2008.8 65.9 0.442
285 AC 1 525. 1820.1 0.600 107.5 288.7 1.839 ZIRM
00209+3259 0.6857 1.234 84.0 26.8 2012.1 288.8 1.841
363 A 431AB 53.56 2003.58 0.644 25.5 329.5 0.172 SCARDIA
00271-0753 6.7214 0.364 109.0 293.0 2013.573 321.9 0.168 et al. (*)
1081 STF 113A,BC 650. 1686.0 0.640 87.2 20.4 1.637 ZIRM
01198-0031 0.5538 1.324 43.5 106.7 2013.9 20.6 1.638
- MCA 7 3.800 2010.280 0.017 145.0 47.8 0.030 DOCOBO
02366+1227 94.737 0.077 112.7 3.7 2010.718 322.9 0.078 et al. (**)
- FIN 333 83.73 1998.06 0.423 34.1 34.1 0.462 DOCOBO
02434-6643 4.300 0.509 90.0 269.2 2013.737 34.1 0.457 et al. (**)
2524 A 2909 11.345 2013.744 0.507 16.2 23.1 0.129 DOCOBO
03244-1539 31.732 0.172 71.3 283.0 2013.737 38.4 0.125 et al. (**)
2117 BU 9AB 616. 1952.0 0.100 174.0 214.8 0.937 ZIRM
02471+3533 0.5844 1.882 67.3 21.5 2009.1 215.7 0.926
2452 HU 1056 603. 2010.2 0.180 83.3 80.1 1.073 ZIRM
03196+6714 0.5970 1.386 99.2 15.4 2012.8 79.9 1.067
2628 BU 533AB 463. 1776.6 0.110 42.7 221.0 1.037 ZIRM
03356+3141 0.7775 0.992 94.8 15.3 2012.2 221.0 1.033
- KUI 15AB 871. 1909.3 0.660 28.6 206.6 0.790 ZIRM
03520+0632 0.4133 0.925 96.1 73.7 2012.1 206.6 0.793
3430 BU 186 729.6 1999.78 0.806 178.1 34.3 0.366 RICA
04460-0659 0.4934 1.53 55.6 150.2 2012.8986 37.1 0.369
3072 BU 547AB 479. 1816.6 0.910 52.9 339.5 1.263 ZIRM
04139+0916 0.7516 1.053 128.6 263.0 2009.1 339.4 1.263
4390 STF 795 1140. 2187.6 0.580 19.6 219.7 1.026 ZIRM
05480+0627 0.3158 1.237 61.0 340.7 2012.4 219.9 1.020
6263 STF1126AB 752. 2254.0 0.330 124.4 176.4 0.840 ZIRM
07401+0514 0.4787 1.054 55.4 208.7 2012.2 176.8 0.836
7039 A 2473 113.4 2018.01 0.972 115.0 94.6 0.195 DOCOBO
08507+1800 3.175 0.979 80.2 89.0 2009.265 98.2 0.171 et al. (**)
- HDO 207 400.0 1960.7 0.538 43.7 77.2 0.134 DOCOBO
09128-6055 0.900 0.548 76.4 149.0 2013.238 74.2 0.132 et al. (**)
8332 A 2579 236.3 1897.68 0.287 17.8 35.0 0.406 DOCOBO
11532-1540 1.524 0.321 147.9 160.6 2010.266 34.3 0.407 et al. (**)
8405 A 682 380.0 1999.48 0.270 143.5 178.2 0.191 RICA
12042+2407 0.9474 0.389 116.5 276.5 2013.033 176.6 0.196
8708 STT 256 605. 1749.7 0.900 143.6 100.4 1.061 ZIRM
12564-0057 0.5950 1.549 75.0 108.1 2013.3 100.5 1.064
8801 MCA 38Aa,Ab 695. 1935.3 0.720 126.8 351.7 0.406 ZIRM
13099-0532 0.5180 1.243 74.7 124.8 2009.3 352.6 0.404
8988 HU 897 531. 2076.2 0.360 88.0 55.1 0.365 ZIRM
13400+3759 0.6780 0.476 33.9 41.4 2008.3 56.0 0.364
- HWE 28AB 373.0 1958.57 0.775 112.3 314.6 1.008 DOCOBO
13535-3540 0.9652 1.519 74.2 90.7 2011.0401 315.0 1.009 & LING
9254 STF1837 1850. 2083.5 0.700 82.7 271.5 1.159 ZIRM
14247-1140 0.1946 2.712 115.7 239.0 2006.3 271.2 1.155
9312 STF1858AB 1750. 1758.9 0.900 30.7 37.9 3.029 ZIRM
14336+3535 0.2057 4.796 85.6 259.3 2011.5 37.9 3.030
9395 HU 141 173.9 1949.33 0.890 6.9 309.6 0.411 ZIRM
14492-1050 2.0702 0.374 57.4 114.8 2008.5 310.0 0.414
9396 BU 106AB 614. 1655.0 0.650 46.5 6.1 1.946 ZIRM
14493-1409 0.5863 1.587 52.9 116.5 2008.1 6.3 1.948
- HJ 4753AB 772. 2048.0 0.430 137.4 117.9 0.824 ZIRM
15185-4753 0.4663 1.657 114.6 80.9 2010.3 117.2 0.811
9600 HU 146 627. 2174.7 0.300 113.3 123.7 0.717 ZIRM
15210+2104 0.5742 0.839 102.8 84.1 2010.4 123.5 0.719
9628 HU 149 770. 1979.4 0.170 90.7 270.7 0.652 ZIRM
15246+5413 0.4675 0.776 96.8 156.0 2010.4 270.7 0.652
9647 STF1944 1030. 2089.3 0.500 142.6 295.2 0.633 ZIRM
15277+0606 0.3495 1.131 126.6 294.8 2010.5 294.6 0.626
9834 HU 1274 361. 1974.3 0.000 124.4 114.5 0.444 ZIRM
15550-1923 0.9972 0.576 101.7 0.0 2009.3 114.2 0.438
9880 STT 303AB 1460. 1475.0 0.000 11.0 173.6 1.587 ZIRM
16009+1316 0.2466 2.214 72.9 0.0 2012.5 173.8 1.593
10659 A 1156 195.22 2000.00 0.260 168.3 345.8 0.204 DOCOBO
17366+0723 1.8441 0.281 95.5 156.8 2009.2659 345.5 0.201 & LING
- CHR 63 20.911 2013.189 0.027 62.9 268.9 0.068 DOCOBO
17375+2419 17.216 0.096 114.8 97.9 2008.467 257.2 0.083 et al. (**)
- CHR 63 10.420 2005.929 0.753 72.4 269.4 0.068 DOCOBO
17375+2419 34.549 0.127 100.6 259.8 2008.467 253.8 0.053 et al. (**)
10728 STF2218 2130. 2108.0 0.790 85.9 309.7 1.446 ZIRM
17403+6341 0.1690 3.575 133.5 234.1 2013.6 309.2 1.439
10796 HU 1288 765. 2005.0 0.160 159.5 160.2 0.436 ZIRM
17472+1502 0.4706 0.519 64.5 355.1 2010.6 160.5 0.436
11098 HU 314 1075. 1885.7 0.200 170.0 72.9 0.290 ZIRM
18086+1838 0.3349 0.602 123.1 31.7 2010.6 72.1 0.291
12447 STF2525AB 882.9 1887.72 0.958 155.3 289.5 2.163 SCARDIA
19266+2719 0.4077 1.870 150.7 62.5 2014.740 289.5 2.172 et al. (*)
12623 STT 375 682. 2271.2 0.200 177.7 187.3 0.602 ZIRM
19346+1808 0.5279 0.521 24.0 159.4 2011.7 187.7 0.601
13196 STF 2606AB 455. 1745.7 0.690 127.4 146.4 0.675 ZIRM
19585+3317 0.7912 1.081 82.4 240.5 2012.8 146.6 0.669
14880 BU 838 1280. 2050.0 0.200 12.9 154.5 1.661 ZIRM
21209+0307 0.2813 2.342 40.8 148.7 2007.7 154.9 1.664
16011 HU 981 934. 1904.6 0.650 53.0 214.3 0.295 ZIRM
22305+6137 0.3854 0.612 102.0 116.9 2008.8 214.0 0.294
- KUI 114 54.57 1969.38 0.005 128.9 126.3 0.252 DOCOBO
22408-0333 6.597 0.367 87.5 12.9 2012.705 126.8 0.280 et al. (**)
16317 STF2950AB 804. 2083.5 0.520 116.2 274.8 1.182 ZIRM
22514+6142 0.4478 1.854 128.3 298.1 2011.9 274.2 1.169
(*) SCARDIA, PRIEUR, PANSECCHI, ARGYLE & ZANUTTA
(**) DOCOBO, TAMAZIAN, CAMPO, MALKOV & CHULKOV
==========================================================================================
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NEW COMBINED SPECTROSCOPIC/ASTROMETRIC ORBITS
In the article "Are the orbital poles of binary stars in the solar neighbourhood
anisotropically distributed?" (2015 A&A 574, A6), the authors reported the fact that, of
the 95 systems that are closer than 18 pc from the Sun and have an orbit in the 6th
Catalogue of Orbits of Visual Binaries, the pole ambiguity could be resolved for 51
systems using radial velocity measurements. Also, it was possible to correct the erroneous
nodes and determine new combined spectroscopic/astrometric orbits for the following
systems: WDS 01083+5455 Aa,Ab; 01418+4237 AB; 02278+0426 AB (SB2); 09006+4147 AB (SB2);
16413+3136 AB; 17121+4540 AB; 18070+3034 AB.
Agati J-L., Bonneau D., Jorissen A., Souli E., Udry S., Verhas P., and Dommanget J.
==========================================================================================
NOTE: ON THE DESIGNATION OF MULTIPLE STARS
On the designation of multiple stars
Back in 2003, the IAU GA XXV recognized the need of a unified and computer-friendly system
for designating components of binary and multiple stars (http://adsabs.harvard.edu/abs/
2005HiA....13.1011M). The naming system adopted in the WDS is not satisfactory because the
discoverer codes are not recognized or used by the majority of astronomers. Sometimes, but
not always, component identifiers are appended to the discoverer codes. Both codes and
component identifiers in the WDS change with time. As a result, a given binary has a
changing name in the WDS and in the orbit catalogs and cannot be associated with a unique
string of characters for automated searches. The WDS nomenclature is also poorly suited
for hierarchical systems.
In my work, I follow the rule formulated by Hartkopf & Mason (http://adsabs.harvard.edu/
abs/2005HiA....13..981H): \A comma will be used as the delimiter between components in a
system, with the full component identifier before and after the comma (e.g. Aa,Ab)." There
must be no exceptions to this rule when dealing with triples. When needed, hierarchy is
coded by adding the name of the parent component in a separate field or with another comma
(see e.g. http://www.ctio.noao.edu/~atokovin/stars/index.php). For example, in a triple
system consisting of a close pair A,B and a wider component C, the outer pair is named
AB,C,* (where * means no parent) and the inner pair as A,B,AB. Here AB refers to the
center of mass of the inner binary - a composite "component" with such properties as
position, mass, and ux, while A,B refers to the orbit of the inner pair with its period,
eccentricity, mass ratio, etc. Obviously, the component AB and the system A,B are
different entities, not to be confused. Each component must be designated by a unique,
fixed sequence of letters and numbers (a string). A system is then designated by its two
components joined with comma. Strict adherence to this rule will allow automated searches
in the double-star catalogs, easy designation of newly discovered components, and
consistent description of hierarchy.
Once the fixed component designations are adopted (changing designations are not
acceptable anyway), each system will be uniquely defined by its two components, so the
discoverer codes become redundant. They are the old, complementary way to name visual
binaries. The historical reasons behind these codes (individual observers) are no longer
valid. Modern authors do not assign their codes to the new systems, while such codes
invented later by the WDS are arbitrary and essentially meaningless. Discoverer codes are
not used for eclipsing and spectroscopic binaries or exoplanets.
The messy designations in the current WDS arise from the old restrictions on the number of
characters in the computer records and from the desire to reflect the hierarchy in the
component's names themselves. As the knowledge of hierarchy changes, so do the component
letters in the WDS. To serve as component designations, these letters must be fixed. In
contrast, the hierarchy can be described flexibly by parent components and can be changed
as needed without affecting the component's names.
To implement the IAU recommendation, I propose the following:
1. Freeze the component designations existing currently in the WDS. Explicitly assign A
and B to those that are missing.
2. Enforce the use of comma in the system designation.
3. Separate the component-based system designations such as A,B from the discoverer codes,
never concatenate them in one string.
4. Discontinue assigning discoverer codes to new systems.
Andrei Tokovinin
******************************************************************************************
The deadline for contributions to Information Circular No. 186 is:
June 15th 2015
J. A. Docobo (joseangel.docobo@usc.es)
J. F. Ling (josefinaf.ling@usc.es)
Tel: +34 981592747
Fax: +34 981597054
Observatorio Astronomico "R. M. Aller"
P. O. Box 197
Universidade de Santiago de Compostela
SPAIN
ISSN: 1024-7769
INTERNATIONAL ASTRONOMICAL UNION COMMISSION 26 (DOUBLE STARS)
INFORMATION CIRCULAR No. 186 (JUNE 2015)
NEW ORBITS
ADS Name P (yr) T e W(2000) 2015 Author
RA 2000 DEC n (deg) a (") i (deg) w (deg) Last ob. 2016
---------------------------------------------------------------------------------------------
- GJ 1005 4.55 2018.08 0.361 56.3 286.9 0.333 PEREZ
00152-1607 79.1209 0.305 145.2 338.5 2014.8535 247.8 0.409 et al. (*) ^1
363 A 431 49.10 2003.90 0.606 206.9 323.4 0.168 PEREZ
00270-0752 7.3320 0.349 110.7 116.1 2014.8535 314.4 0.166 et al. (*) ^2
671 STF 60 AB 479.27 1889.93 0.497 278.0 324.1 13.266 SCARDIA
00491+5749 0.7511 12.040 35.6 269.8 2014.641 324.6 13.295 et al. (**)
- BD+04 27.55 2030.23 0.663 90.3 75.3 0.741 PEREZ
01022+0503 13.0672 0.457 144.0 203.6 2014.7633 72.3 0.741 et al. (*) ^3
- GJ 54 1.78 2016.41 0.100 67.7 265.4 0.131 PEREZ
01102-6726 202.2472 0.139 136.2 70.6 2015.0284 85.6 0.133 et al. (*) ^4
- GJ 60 4.56 2019.26 0.302 76.9 152.3 0.122 PEREZ
01350-2954 78.9474 0.167 13.8 31.0 2015.0283 241.0 0.190 et al. (*) ^5
- DUN 5 475.2 1811.90 0.513 13.7 187.0 11.604 SCARDIA
01398-5612 0.7576 7.826 140.5 18.6 2013.710 186.7 11.610 et al. (**)
1615 STF 202 AB 3267.4 2188.58 0.465 3.7 263.3 1.832 SCARDIA
02020+0246 0.1102 7.400 113.4 147.9 2015.112 262.7 1.833 et al. (**)
1709 STF 228 145.41 1899.07 0.263 99.1 299.0 0.721 SCARDIA
02140+4729 2.4758 0.885 63.8 322.7 2015.113 300.7 0.695 et al. (**)
5447 STT 156 205.3 2017.76 0.605 10.1 139.1 0.166 SCARDIA
06474+1812 1.7535 0.445 150.5 258.9 2014.239 130.1 0.160 et al. (**)
- SEE 119 16.651 2019.562 0.726 37.2 254.1 0.424 DOCOBO
10373-4814 21.6203 0.361 128.5 288.9 2014.060 247.0 0.399 & CAMPO
8639 A 1602 699.4 1913.05 0.914 5.3 27.0 0.591 DOCOBO
12429+0516 0.5147 1.567 96.9 125.8 2014.30 26.8 0.598 & LING
- SEE 170 27.432 2021.872 0.687 98.2 126.8 0.183 DOCOBO
13123-5955 13.1234 0.167 57.7 199.3 2013.1291 131.6 0.160 & CAMPO
10075 STF2052 AB 230.06 1921.12 0.758 93.9 119.2 2.365 SCARDIA
16289+1825 1.5648 2.245 108.4 130.8 2014.511 119.0 2.386 et al. (**)
(*) PEREZ, MENDEZ & HORCH
(**) SCARDIA, PRIEUR, PANSECCHI, ARGYLE & ZANUTTA
Comments from web editor:
1: 00152-1607 GJ 1005 --> 00155-1608 HEI 299 AB
2: 00270-0752 A 431 --> 00270-0753 A 431 AB
3: 01022+0503 BD+04 --> 01024+0504 HDS 135
4: 01102-6726 GJ 54 --> 01104-6727 GKI 3
5: 01350-2954 GJ 60 --> 01350-2955 DAW 31 AB
==========================================================================================
NOTE
Response to Andrei Tokovinin's note (IAUDS Circular No. 185)
We'd like to thank our colleague and frequent collaborator for his many considered
comments and suggestions to improve the double star database. There is indeed a recognized
need for a unified and computer friendly system designating components of binary and
multiple stars (2005HiA....13.1011M); that same citation "... recommends that a uniform
designation scheme, based on expansion of the Washington Multiplicity Catalog (WMC)
system, be developed during the next three years ..." The rules of this scheme were rather
explicitly spelled out at a double star meeting hosted by the former president of the
commission (2004RMxAC..21...83H). Although a half-hour RA slice of the WDS, reformatted
and augmented with binaries disovered by other techniques, was used to generate a test
version of the new catalog, staffng reductions prevented our desire to fully implement the
WMC.
Alteration of WDS designations is kept to an absolute minimum to avoid confusion with
published data; however, there are a couple reasons why a designation may occasionally
require changing:
1. when a pair in the WDS is found to have an error in position so great that it adversely
affects its selection for observation, and
2. when an entry is determined to be physically associated with a pair at another WDS
coordinate.
An example of the former case (uncovered by WDS contributor Friederich Damm) would be
HJ 74 (= BDS 4376), first resolved in 1836MmRAS...9..193H. The pair was inadvertently
added at the wrong declination, and this error propagated through several double star
catalogs, including the WDS. Much later, Roe announced ROE 32 (1910PA.....18..354R).
Herschel's correct 1825 coordinates, when precessed to 2000, matched those of the ROE pair
already in the WDS. While Herschel's first measure was off in separation his second
measure, predating Roe's "discovery" by almost 80 years, was a very good match. Roe's
measure was subsequently merged with those of Herschel under a corrected WDS designation,
and an explanation was added to the WDS notes file.
The precise position is a datum* that is flexible depending on our knowledge of the
system. For example, for a wide AB pair the precise position is the 0".1-precise J2000
position of the A component. The precise position for the BC pair in that same system would
be the J2000 coordinates of the B component. However, all components of a multiple star
system have the same ten digit WDS designator to identify the family. Therefore, an
example of the latter reason for changing WDS designations would be the case of STF2576
and STF2580. STF2576 (= ADS 12889) and STF2580 (= ADS 12913) had different WDS
designations in earlier (up to the 2006.5) versions of the WDS (19456+3337 and 19464+3344,
respectively). However, upon closer analysis these pairs were found to be members of the
same wide multiple system (the "F" component of one pair was the same star as the "A"
component of the other). They are all currently found under the WDS designation
19464+3344, with STF2576 now designated as the "FG" components.
(* incorrect term "designation" changed by web editor)
To continue addressing Andrei's first point, assigning the component designator "AB" to
simple binaries would represent a loss of information. The presence of "AB" implies
additional components, whereas the absence of "AB" means it is a simple double.
In his second point, he considers the comma as delimiter. In the WMC (and therefore, WDS)
designation, approved by IAU resolution, a comma is indeed used as the delimiter between
components in a system, with the full component identifier before and after the comma
(e.g., Aa,Ab). The only exception is if only two characters are provided the delimiter is
assumed (e.g., WAK 8CD = WAK 8C,D). Further, the comma defines what is being measured
relative to what. For example, in the case of the well-known multiple system STF1196 the
component designation "AB,C" means the C component is measured relative to the photocenter
of AB. This is useful when a technique/instrument incapable of resolving AB is utilized.
When a higher resolution technique/instrument is used the component identifiers "AC" and
"BC" are used instead.
As the WDS is ingested by many users (CDS and NASA to name two), and used in its current
format, we try to make any format changes on an infrequent basis. Nevertheless, since
Charles Worley left the USNO in 1998 we have made significant changes which, we think,
provide a better product. In addition to improving the magnitudes, cross-references and
spectral types in a piecemeal basis we added the precise position to aid in finding pairs,
added the secondary proper motion to aid in identifying physicality, and added new column
notes indicating physical/optical codes based on various criteria. In the last version of
the WDS Charles prepared (WDS 1996.0; 1997A&AS..125..523W) the WDS contained 78,100 pairs
from 451,546 mean positions. The only measure of physicality was the online visual orbit
catalog, an update of Worley & Heintz (1983PUSNO..24g...1W), which contained 928 orbits of
847 systems. The known physicality total was thus 1.1%. The current version of the WDS
contains 132,231 systems based on 1,268,765 mean positions, increases of 69% and 181%,
respectively. The current orbit catalog contains 2518 orbits of 2413 systems (improvements
of 171% and 185%, respectively) as described above; this and other indicators identify
20,468 pairs (15%) as physical, 4623 (3%) as optical and the remainder (107,140) as
unknown.
Maintenance and improvement of the WDS has been taken very seriously ever since the double
star database was turned over to the US Naval Observatory half a century ago
(1966IAUTB..12..267V). While the catalog is offcially under the aegis of the IAU
(Commission 26 and after the forthcoming General Assembly Commission C.G1), it is for the
user that the WDS is provided. We are considering many other format changes to make the
WDS a better product, but to minimize disruption we are doing this with due deliberation
and seek to make many changes at once for the user (after ample warning, of course). Among
the changes we are currently considering implementing within the next three years are:
* expanding the WDS designation, as the current arcminute identification is not adequate
in crowded fields;
* expanding the multiplicity field, which is currently not adequate for nested
hierarchies;
* increasing the separation precision in the summary catalog, which is inadequate for
current techniques;
* adding a separation code for much closer and wider separations (arcminute,
milliarcseconds, microarcseconds); and
* adding additional flags for magnitudes in other filters (V,B,R,K ...).
Additional questions:
* Should proper motion unit (currently mas/yr) be expanded to 0.1 mas/yr precision?
* Should we include pm errors?
* We currently still use the long out-of-date DM (BD, CD, or CpD depending on declination)
as a cross-reference. What catalog should we use? Are precise coordinates sufficient
without a cross-reference name?
* Is more space needed for spectral type?
* Is more space for fractional year needed for fast moving systems?
* Should we move away from our own eight-character reference code to the 19-character
bibcode? However, note that 7-8% of the references in the WDS have no bibcode at this
time.
Regarding Andrei's third and fourth point, we have no objection to separating the
component field from the discovery designation field; this will be a trivial change to
make during the next major reformat of the WDS summary line. We likewise have no objection
if people wish to discontinue use of the discovery designation. The field is specified in
the WDS and will continue to be populated nonetheless. Inclusion of the DD does have some
advantages; knowledge of the discoverer often provides an indication whether a pair will
likely be close or wide, bright or faint, visible mainly in the infrared, have a small or
large magnitude difference. From a cataloging point of view, the main advantage of doing
away with discovery designations is that it eliminates people "stamp collecting" new
pairs. It is a waste of our time to catalog large numbers of new optical doubles which
only serve to appease someone's vanity.
The plethora of all-sky astrometric catalogs and the computer acumen of users has
exacerbated the issue of which pairs to add to the WDS. Formerly, a pair would
automatically be added when its components fell within some angular separation limit, such
as 10". We now encourage users to only measure (or data mine) pairs which have some
indication of physicality. An example of this would be our recent mining of the final UCAC
catalog (2013AJ....146...76H). Of the more than 113 million entries in UCAC4, and despite
the many close pairings we only added the 4082 pairs we determined to be likely physical.
Finally, it is possible that Gaia (or later Gaia data-miners) may identify large numbers
of pairs that are preferentially optical. In order to address this we could construct a
"Faint Object Supplement" to the WDS. Only those Gaia pairs subsequently identified as
physical could then potentially "graduate" to the WDS.
We welcome any and all suggestions to improve the double star database for the user.
Changes will, and should be, deliberate. However, if the user needs them to make a better
product for the community we will strive to make those changes.
Brian D. Mason and William I. Hartkopf
U.S. Naval Observatory
==========================================================================================
RENE MANTE (1922-2014)
Rene Mante was born in Toulon on September 9, 1922 and passed away on June 14, 2014 in
Marsella. After completing High School, Rene Mante studied at the University of
Montpellier and became a Chemical Engineer. He worked in the Pennaroya Chemical Society.
Later, he searched for work in Marsella and enrolled in courses of Electronics and
Computer Science. For several years, he worked in a company that manufactured tartaric
acid until it closed. At that point, he and some friends established a laboratory that
analyzed food and chemical products. He retired in 1987 and dedicated himself to
Astronomy, a field about which he was very passionate. After having used a refractor
telescope, Mante ordered a reflector from a manufacturer in Trans-en-Provence (Department
of Vart) but that company committed an error in the focal longitude and then went out of
business. R. Mante, an amateur astronomer, was disappointed but he persevered and bought a
second, and then a third telescope. His great love for Mathematics served him in his
training that was necessary to carry out calculations associated with double stars. He
presented his research at numerous meetings of the Double Star Commission of the
Astronomical Society of France. Between 1998 and 2006, Mante published 49 preliminary
orbits for visual double stars: four in the journal, Observations et Travaux, and
forty-five in the Information Circulars of Commission 26 (Double and Multiple Stars) of
the IAU.
In 2005, along with D. Bonneau, he published an article in the journal, L'Astronomie,
entitled "Dans la chaleur des forges de Vulcain : le systme multiple omicron Andromede".
A cerebro-vascular accident and a fracture of the femur sadly ended his activities as an
astronomer.
Edgar Soulie and Suzanne Mante
******************************************************************************************
The deadline for contributions to Information Circular No. 187 is:
October 15th 2015
J. A. Docobo (joseangel.docobo@usc.es)
J. F. Ling (josefinaf.ling@usc.es)
Tel: +34 981592747
Fax: +34 981597054
Observatorio Astronomico "R. M. Aller"
P. O. Box 197
Universidade de Santiago de Compostela
SPAIN
ISSN: 1024-7769
INTERNATIONAL ASTRONOMICAL UNION COMMISSION G1 (BINARY AND MULTIPLE STAR SYSTEMS)
INFORMATION CIRCULAR No. 187 (OCTOBER 2015)
NEW ORBITS
ADS Name P (yr) T e W(2000) 2015 Author
RA 2000 DEC n (deg) a (") i (deg) w (deg) Last ob. 2016
---------------------------------------------------------------------------------------------
9 BU 281AB 1117. 2077.5 0.639 149.9 160.2 1.560 LING
00028+0208 0.3223 3.140 108.5 55.7 2014.8561 159.9 1.558
- HDS 101 24.809 2010.380 0.700 33.8 4.2 0.110 CVETKOVIC
00463-0634 14.5108 0.102 43.8 177.3 2010.7172 9.9 0.125
1458 A 2602 1606. 1976.2 0.868 4.5 181.1 0.795 DOCOBO
01500-0408 0.2242 2.455 82.4 45.3 2015.7382 181.2 0.814 et al. (*)
- DON 43 108.42 1972.75 0.362 29.6 274.1 0.208 DOCOBO
02514-2139 3.3204 0.242 52.1 94.1 2015.7383 276.7 0.207 et al. (*)
- HDS 430 54.70 2021.61 0.091 54.4 314.0 0.194 CVETKOVIC
03264+3520 6.5820 0.273 41.2 313.4 2010.8923 323.9 0.191
- HDS 441 18.964 2007.281 0.500 17.8 164.7 0.122 CVETKOVIC
03307-1926 18.9830 0.218 102.7 84.4 2014.7635 149.7 0.095
- HDS 510 35.44 2010.30 0.366 102.0 338.6 0.067 CVETKOVIC
04025+0638 10.1577 0.159 64.9 166.1 2008.6996 3.3 0.063
7131 HU 225AB 125.94 1944.21 0.331 68.4 263.8 0.433 DOCOBO
09001-1228 2.8585 0.341 46.0 9.5 2011.0371 264.9 0.430 & LING
- HDS1353 93.92 1995.98 0.835 140.7 163.8 0.403 CVETKOVIC
09252+4606 3.8332 0.582 76.9 263.4 2010.0054 164.8 0.402
- CHR 176 21.724 2000.621 0.351 25.5 174.2 0.068 CVETKOVIC
09446+6459 16.5716 0.115 74.5 262.3 2005.2458 184.0 0.083
- HDS1507 23.361 2011.062 0.156 64.5 228.6 0.109 CVETKOVIC
10294+1211 15.4105 0.122 51.6 77.8 2007.3298 239.3 0.120
- HDS1568 16.244 2003.412 0.150 95.3 297.0 0.170 CVETKOVIC
10596+1800 22.1622 0.203 115.8 256.6 2010.3416 285.1 0.191
8092 A 1353 127.25 1962.00 0.644 44.4 209.1 0.561 DOCOBO
11136+5525 2.8291 0.390 117.6 39.2 2013.287 208.6 0.559 & LING
8727 CHR 39Aa,Ab 7.906 2011.562 0.363 21.6 5.5 0.105 DOCOBO
12597-0349 45.5350 0.078 19.3 174.9 2014.3003 27.3 0.105 & CAMPO
- CHR 180 219.2 2201.7 0.686 22.2 61.0 0.654 CVETKOVIC
13155+4051 1.6423 0.745 44.5 273.3 2010.4701 62.2 0.661
- HDS2108 37.53 2016.35 0.489 34.4 247.0 0.087 CVETKOVIC
14562+1745 9.5910 0.193 126.9 174.1 2008.4743 224.9 0.096
- HDS2163 130.91 1993.53 0.483 3.7 173.0 0.234 CVETKOVIC
15226+7254 2.7500 0.261 66.0 39.2 2010.4675 174.2 0.243
10828 STT 337 1000. 1787.0 0.613 134.1 164.7 0.573 DOCOBO
17506+0714 0.3600 1.389 100.1 141.7 2013.678 164.4 0.579 & LING
- B 398 74.37 2007.91 0.344 163.1 177.8 0.199 DOCOBO
18434-5546 4.8407 0.329 107.5 252.4 2015.7375 174.5 0.224 et al. (*)
- B 459BC 72.78 2044.56 0.229 64.6 194.7 0.279 DOCOBO
20002-5522 4.9464 0.292 44.9 278.7 2015.7377 198.3 0.283 et al. (*)
- RST2134 151.79 1977.23 0.258 22.2 234.8 0.238 DOCOBO
20081-3929 2.3717 0.259 133.1 18.9 2015.7377 233.0 0.244 et al. (*)
- I 1450 201.8 1961.8 0.780 10.2 349.3 0.775 DOCOBO
22007-5002 1.7844 0.599 58.4 162.8 2015.7378 349.7 0.785 et al. (*)
- DON1038 147.13 1972.27 0.556 9.9 238.7 0.356 DOCOBO
22504-1744 2.4468 0.488 64.2 97.6 2015.7379 240.4 0.354 et al. (*)
16850 SEE 492 77.75 1969.11 0.491 72.1 28.0 0.673 DOCOBO
23357-2729 4.6302 0.601 50.0 110.6 2014.7632 30.0 0.678 & CAMPO
(*) DOCOBO, GOMEZ & CAMPO
==========================================================================================
NEW LINEAR FITS
ADS Name X0 Xa rho_0 T0 2015 Author
RA 2000 DEC - Y0 Ya theta_0 Last ob. 2016
----------------------------------------------------------------------------------------
- STI2051AB 5.579910 0.042772 6.047 1939.9580 58.6 10.293 CVETKOVIC
04312+5858 - 2.330326 -0.102417 112.670 2013.7723 58.3 10.383
3527 HJ 3263 -3.459261 0.039617 4.066 1834.7860 375.0 14.184 CVETKOVIC
04556+1653 - -2.136124 -0.064157 301.700 2013.7749 375.1 14.256
- BRT2521 -1.248724 -0.076498 2.380 1940.8240 282.0 7.077 CVETKOVIC
05492+2941 - 2.026629 -0.047135 211.640 2013.7725 282.2 7.162
5423 AGC 1AD -16.490870 -0.182838 20.757 1994.900 248.1 21.539 MASON &
06451-1643 - 12.605517 -0.239193 232.61 1915.804 248.4 21.573 HARTKOPF
5423 HL 3AE 64.195206 0.550715 70.755 1877.958 46.5 191.705 MASON &
06451-1643 - 29.752087 -1.188261 114.87 2011.214 46.4 192.246 HARTKOPF
5423 BU 1411AF 67.216583 0.549349 74.047 1933.492 59.9 128.834 MASON &
06451-1643 - 31.062237 -1.188754 114.80 2011.214 59.8 129.264 HARTKOPF
6251 D 29AE 201.662064 0.692103 247.544 1676.174 67.0 473.087 MASON &
07393+0514 - 143.563950 -0.972186 125.45 2009.135 67.0 473.494 HARTKOPF
6251 SLE 439AF -123.079185 0.791689 156.630 1956.928 333.2 172.829 MASON &
07393+0514 - -96.874138 -1.005846 308.21 2012.237 333.4 173.049 HARTKOPF
6251 SMR 11AG -284.463531 0.741101 352.248 1977.242 313.6 355.263 MASON &
07393+0514 - -207.747711 -1.014771 306.14 2012.237 313.7 355.330 HARTKOPF
7472 J 78 0.562050 0.067989 3.088 1948.2240 113.3 5.555 CVETKOVIC
09388+0242 - 3.036883 -0.012583 169.510 2014.2542 112.9 5.612
- HJ 2804AB -2.604337 0.083382 5.534 2049.7729 238.8 6.436 CVETKOVIC
17046+3900 - 4.882575 0.044476 208.080 2014.6040 238.0 6.388
11711 STF2400AB -0.954074 0.029920 1.046 1869.0909 161.4 10.694 CVETKOVIC
18489+1615 - 0.429117 0.066523 245.780 2014.6100 161.4 10.767
11711 STF2400A,BC -1.225272 0.031637 1.366 1867.037 161.1 10.688 CVETKOVIC
18489+1615 - 0.603106 0.064275 243.79 2012.606 161.1 10.759
11711 STF2400AC -0.867775 0.016718 0.889 1862.1140 171.7 11.728 CVETKOVIC
18489+1615 - 0.194374 0.074637 257.370 2000.0000 171.7 11.804
- HDS2740 0.129807 0.009663 0.141 2016.6639 50.7 0.147 CVETKOVIC
19218+7708 - -0.055851 0.022458 66.720 2008.4750 60.2 0.142
12991 J 1336 AB -0.370453 0.047707 2.070 1904.8290 58.5 5.729 CVETKOVIC
19500+0637 - -2.036395 -0.008679 349.690 2013.5284 58.7 5.774
13421 J 1338 -0.230028 0.074518 1.557 1884.9110 72.5 9.924 CVETKOVIC
20087+1223 - -1.540130 -0.011130 351.510 2013.5366 72.5 9.999
==========================================================================================
ANNOUNCEMENTS
THE SPECKLE CAMERA PISCO IS NOW MOUNTED ON THE 104 CM "EPSILON" TELESCOPE OF THE
OBSERVATOIRE DE LA COTE D'AZUR, ON THE PLATEAU DE CALERN, FRANCE.
The speckle camera PISCO, originally built at the Observatoire Midi-Pyrnes for the Bernard
Lyot telescope of 2m aperture on the Pic du Midi, France, on November 2003 was transported
in Italy and mounted at the Cassegrain focus of the 102cm Zeiss telescope of the INAF -
Osservatorio Astronomico di Brera in Merate, where it became operational on 01 January
2004. From that date and until 04 June 2015 more than 3750 measures of visual binary stars
were performed. On 16 June 2015, PISCO was dismounted from the Zeiss telescope and placed
in the original boxes previously used for its transportation in Italy. Ten days later, it
was returned in France, at the Observatoire de la Cote d'Azur (OCA), on the Plateau de
Calern (~1270-m a.s.l.), near the town of Grasse, and transferred to the Group C2PU
(Centre Pedagogique Planete Univers), which manages the telescopes "Omicron" and
"Epsilon", both of 104cm aperture, of that observatory. Between August 3 and 7, after a
careful overhaul, and cleaning of the optics, PISCO was firmly mounted on the Epsilon
telescope. Then, the old ICCD Philips camera of 1992, used in Merate, technologically
obsolete, although still operational, was replaced with a modern, high-performance EMCCD
ANDOR Ixon Ultra 897 camera, belonging to the C2PU Group. At present, some necessary tests
are in progress, and the software for operating the camera ANDOR, the internal mechanisms
of PISCO, and for pointing the telescope is nearly completed. We foresee that the
Epsilon+PISCO unit will become operational before the end of the current year.
The PISCO Group (M. Scardia, J.-L. Prieur, L. Pansecchi, R.W. Argyle and E. Aristidi)
The C2PU Group (in alphabetical order: L. Abe, P. Bendjoya, C. Dimur, J.-P. Rivet, D.
Vernet and O. Suarez)
(Photographs: see pdf version of circular)
caption: The OCA Epsilon telescope at Calern with PISCO (black box with red button)
fastened alongside
caption: Detail of the mechanical connection of PISCO to the Epsilon telescope
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NEW BOOK
Jean-Claude Thorel announces the edition of the book:
Title: Robert JONCKHEERE l'astronome des etoiles doubles GENEALOGIE et complements a la
biographie "Le Ciel d'une Vie - Robert Jonckheere".
Editorial: Nice Imprim 794 071 316 R.C.S. Nice
Date: December 2014
==========================================================================================
Errata in Information Circular No. 186
- The entry 00152-1607 GJ 1005 should be 00155-1608 HEI 299 AB
- The entry 01022+0503 BD+04 should be 01024+0504 HDS 135
- The entry 01102-6726 GJ 54 should be 01104-6727 GKI 3
- The entry 01350-2954 GJ 60 should be 01350-2955 DAW 31 AB
- In the NOTE, the sentence\The precise position is a designation..." it should be
"The precise position is a datum..."
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The deadline for contributions to Information Circular No. 188 is:
February 15th 2016
J. A. Docobo (joseangel.docobo@usc.es)
J. F. Ling (josefinaf.ling@usc.es)
Tel: +34 981592747
Fax: +34 981597054
Observatorio Astronomico "R. M. Aller"
P. O. Box 197
Universidade de Santiago de Compostela
SPAIN
ISSN: 1024-7769