Peremennye Zvezdy

Peremennye Zvezdy (Variable Stars) 27, No. 6, 2007

Received 3 September; accepted 26 October.

Article in PDF

New GCVS Versions for Three Southern Constellations

N.N Samus1,2, E.N. Pastukhova1, O.V. Durlevich2

  1. Institute of Astronomy, Russian Academy of Sciences, 48, Pyatnitskaya Str., Moscow 119017, Russia

  2. Sternberg Astronomical Institute, 13, University Ave., Moscow 119992, Russia


We are currently working on a version of the General Catalogue of Variable Stars (GCVS) revised taking into account the new data accumulated since the 4th GCVS edition. A draft new version will be released for each constellation as soon as the work for the constellation is finished. It will contain all stars of the 4th GCVS edition plus a complete catalogue of the stars added to the GCVS in the Name Lists of Variable Stars Nos. 67-78. Now we are ready for the first release, containing more than 1300 variable stars in the constellations of Antlia, Ara, and Telescopium. When preparing the release, we actively used modern data-mining possibilities to improve variability types and light elements. This paper introduces the first release of the new GCVS version and presents new results (types, light elements), based mainly on data mining, for 213 stars.

1. INTRODUCTION

The first three volumes of the 4th edition of the General Catalogue of Variable Stars (GCVS), containing information on our Galaxy's variable stars in all the 88 constellations, were published about 20 years ago (Kholopov, 1985ab; Kholopov, 1987). They contained more than 28000 variable stars. Since then, about 12000 variable stars have been added to the GCVS system via Name Lists of Variable Stars, regularly published in the Information Bulletin on Variable Stars. The electronic GCVS version available at the GCVS site (http://www.sai.msu.su/gcvs/gcvs/) contains all these stars, those of the 4th edition and those of the Name Lists published since (Nos. 67-78), but the data presented for the Name-List stars is incomplete. (It should be reminded that the coordinates of variable stars in the web GCVS version have been considerably improved compared to the original paper version; cf. Samus et al., 2006, and references therein.) For many GCVS stars of the main edition, new publications appeared, demanding changes in the astrophysical information provided by the GCVS.

At the recent General Assembly of the International Astronomical Union (IAU), the IAU Commission 27 "Variable Stars" and the IAU Division V "Variable Stars" discussed the future of variable-star catalogues. The variable-star community is facing serious problems because of the current flow of new automatic discoveries, usually not accompanied with a sufficiently thorough analysis of new results. Commission 27, on behalf of Division V, created an informal working group to discuss these problems and suggest a solution. Meanwhile, it was generally agreed that attempts to prepare a new GCVS version providing up-to-date information were desirable.

It is also obvious that the variable-star classification system used in the 4th GCVS edition should be revised for the new GCVS versions. One of us (N.N.S.) presented a draft new classification scheme to the IAU Commission 27 (see
http://www.sai.msu.su/gcvs/future/classif.htm). It was understood that we would tentatively use this draft scheme in our GCVS work, while the variable-star community would send us suggestions of its improvement.

2. RESULTS

As the first approach to the new GCVS version, we have looked into information available for the GCVS and Name-List stars in three southern constellations, Antlia, Ara, and Telescopium. Earlier, we already approached this task for the constellation of Telescopium and gained some experience in using data available online for improving the GCVS information; we published our results mainly for stars with no light elements in the 4th GCVS edition (Pastukhova et al., 2004). We also used data mining to derive light elements for 100 stars, most of them objects of the NSV catalogue (Kazarovets et al., 2005).

For the constellations of Antlia, Ara, and Telescopium, the most important source of online photometric information is the ASAS-3 survey (Pojmanski, 2002). Many stars in these constellations are contained in the ASAS-3 variable-star catalogue. We are not always satisfied with light curve solutions and period determinations of the ASAS-3 catalogue and sometimes attempted to improve these data. Moreover, for variable stars not in the ASAS-3 catalogue, it is often possible to derive data needed for the GCVS using ASAS-3 raw data. Unfortunately, during 2006, the ASAS-3 data were not completely accessible due to hardware problems in Poland. Additional information for some stars in Antlia could be found in the ROTSE1/NSVS data (Wozniak et al., 2004).

We prepared a complete new GCVS version for 1317 stars in the three constellations, "old" GCVS (4th edition) stars as well as stars named in the Name Lists Nos. 67-78 (the number 1317 does not include non-existing stars; stars having several GCVS names are counted once, in accordance with their main designations). For purposes of evaluation of the new classification system, a subversion using the new draft classification is available at the GCVS Internet site (http://www.sai.msu.su/gcvs/future/). In this subversion, two types are given for each star, according to the old and new classification system. Another subversion, with GCVS information revised but based on the GCVS (4th edition) classification scheme, has been introduced in the main online GCVS version, including data provided by the GCVS search engine.

The Table below contains those stars of the new-classification subversion where information (types, light elements) was significantly revised by us, primarily by means of data mining. The columns are traditional for the GCVS (with the exception that, for eclipsing binaries, the brightness in the secondary minimum is given in the Table rather than in Remarks). Asterisks after GCVS names refer to the short, most important Remarks given after the Table. More detailed remarks, with additional references, can be found at the GCVS site. Like in our earlier catalogues, an asterisk in the " or " column means "".


Table. Revised Catalogue Data


Name
Type Magnitude Range MinII Epoch, JD 24... Period or

S
Ant EC 6.27 6.83 V 6.80 52627.7968 0.6483489
Z Ant Lb 8.5 10.5 V
RS Ant M 11.4 15.0 V 52105 324
RT Ant RR0 13.2 14.2 V 53870.597 0.552956 25
RX Ant M 10.6 14.5 V 52643 234 60
RY Ant SR 10.1 11.1 V 72
RZ Ant SR 12.4 14.6 V 53503 232
SS Ant RR0 12.8 14.2 V 53154.540 0.483725 25
SU Ant M 12.3 14.8 V 53145 335
SV Ant M 11.8 14.6 V 53169 298
TT Ant SR 12.7 13.6 V 90
TY Ant SR 11.3 12.0 V 103
TZ Ant SR 10.9 11.7 V 53431 99
UU Ant EA 11.94 12.4 V 12.1 53474.6407 1.36411 14
UV Ant L: 12.2 13.1 V
UW Ant SR 12.1 13.6 V 126
UY Ant M 10.4 14.5 V 53432 297
UZ Ant RR0 13.1 14.4 p 53965.8348 0.60032 28
VZ Ant M 11.1 14.4 V 53453 424
WX Ant EA 11.25 12.95 V 11.6 51964.6801 3.8171 16
XZ Ant EA 9.65 10.75 V 53036.7096 7.150737 13
YY Ant Lb 8.74 9.4 V
YZ Ant EA 10.48 11.54 V 10.56 52988.815 2.152391 14
ZZ Ant M 10.3 12.0 V 53433 221
AB Ant Lb 6.6 7.1 V
AD Ant M 10.4 14.7 V 53459 316
AE Ant SR 8.8 10.7 V 258
AH Ant SRd 8.40 8.8 V 53492 75
AN Ant EC 8.21 8.34 V 8.26 52974.8389 3.681309
AT Ant SR 8.1 8.6 V 53497 45.3
AV Ant SR 7.5 8.3 V 84
AW Ant SRd: 8.6 9.5 V 700 :
AY Ant SRd 9.64 10.06 V 53.5
BB Ant SR 8.1 9.0 V 122
BD Ant M 11.1 15.0 V 53474 283
BE Ant M 11.2 14.6 V 53476 201
S Ara * RR0 9.92 11.24 V 52764.738 0.4518587 12
U Ara M 7.7 14.1 V 51981 224.6 44
RR Ara M 11.5 15.8 B 52542 204
RS Ara M 10.1 12.2 V 52928 204.4
RT Ara RV 10.2 11.3 V 51983.8 76.69
RU Ara M 8.6 13.0 V 52868 256.8
RW Ara * EA 8.85 11.45 V 8.91 52740.796 4.3674535 13
SS Ara Cst: 9.28 V
SW Ara EA 12.5 15.9 p 53124.984 6.23796 13
SY Ara EA 10.50 12.11 V 10.60 53230.692 1.8566643 13 *
SZ Ara * SR 9.0 11.5 V 53097 221.8
TU Ara M 10.4 13.7 V 53037 353
UW Ara EA 9.48 10.40 V 9.53 52740.812 3.297015 11 *
UX Ara M 9.9 12.8 V 250 :
UY Ara RV 10.5 11.4 V 52080.6 57.95
UZ Ara EA 11.4 12.4 p 51955.840 1.5999079 11 *
WY Ara M 12.5 14.3 V 52889
AH Ara EA 13.0 14.5 p 53191.746 1.00503 15 *
AS Ara SR 14.5 16.5 p 52753 257
BD Ara M 12.7 15.0 V 52922 269
BK Ara M 11.6 14.6 V 52192 206.1 45
BM Ara M 11.7 14.1 V 52082 231.2
BS Ara M: 15.0 16.5 p 52846 256 :
CC Ara M 12.1 15.0 V 52548 312


Table (Continued)


Name
Type Magnitude Range MinII Epoch, JD 24... Period or

CH
Ara M 9.7 13.4 V 52821 247.5
CL Ara EC: 12.9 13.7 V 13.6 52129.544 0.414584
DR Ara SR 10.8 12.7 V 196
DU Ara * CW 11.73 12.46 V 52105.572 1.6406576 33
DZ Ara M 12.5 16.5 p 51968 161.8
EP Ara M 13.5 16.5 p 52733 251
ES Ara M 12.0 15.0 V 53133 289
EU Ara SR 11.1 12.0 V 235
EV Ara M 12.4 14.7 V 52713 260
FO Ara RR0 12.7 13.7 V 52725.838 0.600222 16
FR Ara EA 11.8 12.6 V 12.0 52071.672 1.66864 16
FT Ara RR0 13.5 14.5 V 53144.852 0.78432 15
FZ Ara SR 13.1 15.0 V 168
HH Ara M 11.4 14.5 V 52164 290
HX Ara RR1 11.85 12.22 V 52699.869 0.219408 39
II Ara M 12.1 14.5 V 51843 223
IN Ara RR0 12.32 13.6 V 52802.840 0.631489 17
IV Ara Lb: 12.9 14.1 V
KM Ara SR 11.9 12.4 V 97 :
KN Ara Lb: 11.4 12.0 V
KP Ara SR 12.4 13.2 V 53129 277 50
KQ Ara Lb 13.2 14.1 V
KR Ara SR 11.6 13.6 V 52907 204
KS Ara Lb 12.2 12.8 V
KT Ara M 12.5 16.1 p 53220 259
KX Ara Lb 12.5 13.5 V
LM Ara M 13.7 17.7 p 51954 250
LN Ara M 11.8 14.6 V 52152 122.5
LP Ara EC 10.0 11.0 V 10.4 51965.813 8.533069
MM Ara EA 11.25 11.89 V 11.85 52102.592 2.556502
MS Ara RR0 11.52 12.48 V 52918.610 0.5249875 25
NN Ara SR 11.9 12.8 V 53133 121.2 50
OW Ara EA 12.8 14.0 V 53067.894 2.7301 11
PQ Ara M 10.9 13.5 V 52038 329
QV Ara RR 13.7 14.8 p 0.3180 :
QY Ara M: 10.7 12.8 V 51970 261 :
QZ Ara M 11.5 14.2 V 51963 390 :
V341 Ara * CV: 10.47 11.04 V
V344 Ara M 12.0 14.6 : V 52753 245 :
V357 Ara M 14.0 16.5 p 52566 277
V380 Ara M 15.2 19.0 p 53242 228
V382 Ara SR: 12.5 14.2 V 99 :
V388 Ara M 13.0 16.3 p 52511 233 :
V389 Ara M 14.0 16.3 p 52461 455
V404 Ara M 12.5 16.3 p 53117 320
V430 Ara RR0 12.6 14.1 p 52820.551 0.528406 15
V432 Ara M 12.7 15.0 V 53176 253.3
V447 Ara * EA 12.7 13.9 V 52027.729 1.35225 :
V451 Ara M 12.7 16.0 p 52854 350
V454 Ara EC 13.2 13.9 V 13.6 52088.600 0.81082
V471 Ara M 11.3 16.1 V 52416 279.7 20
V479 Ara RR0 13.5 14.8 p 52736.761 0.55821 15
V482 Ara E 12.9 13.9 V 13.2 53032.874 5.0864
V491 Ara EC 12.2 13.4 V 12.8 52732.844 0.940097
V497 Ara EA 13.3 14.8 V 13.4 : 52094.584 1.14086 12
V498 Ara M: 13.1 14.9 V 53139 215 :
V509 Ara M 12.4 16.0 p 52743 500 :
V511 Ara M: 15.2 16.2 p 53139 290 :
V514 Ara SRd 13.5 14.6 : V 52550 119
V523 Ara M 11.9 14.3 V 52403 201.2 25


Table (Continued)


Name
Type Magnitude Range MinII Epoch, JD 24... Period or

V524
Ara SR 13.9 15.1 p 112
V529 Ara EA 13.0 13.7 V 13.2 52929.526 0.951954 14
V533 Ara RR0 13.0 14.1 p 52406.737 0.567861 12
V536 Ara EA 11.7 13.0 V 11.8 52923.570 2.374084 13
V537 Ara EA 8.64 8.94 V 8.91 52861.711 1.874351
V538 Ara CW 12.3 13.9 V 52177.50 15.8612 28
V544 Ara EA 13.3 14.0 V 13.8 53141.814 1.81635 :
V561 Ara M 12.5 15.0 V 52907 300
V593 Ara SR 11.6 13.6 V 53110 156.5 50 :
V609 Ara SR 12.6 13.8 V 53163 162
V617 Ara * CW 11.49 11.97 V 52755.74 2.52203 30
V624 Ara * SR 11.65 12.2 V 53043 294
V625 Ara Lb 12.0 12.3 V
V630 Ara SR 12.0 13.6 V 98
V631 Ara SR 11.4 12.6 V 53224 208
V633 Ara M 11.0 14.5 V 52907 223.3
V638 Ara M: 11.5 13.2 V 52097 194
V639 Ara * M 12.3 17.6 p 52792 312.5
V643 Ara M: 12.5 14.1 V 52716 249.3 :
V644 Ara Lb 12.8 14.4 V
V649 Ara SR 13.2 14.4 V 52157 172 :
V662 Ara RV: 11.5 12.5 V 52879.5 92.80
V675 Ara M 11.4 13.2 V 52795 193.6
V684 Ara SR 12.8 14.4 V 52785 132.6 45 :
V686 Ara RV 12.7 14.1 V 52178.5 36.30
V689 Ara Lb 13.0 14.6 V
V691 Ara RV 11.3 11.9 V 53081 130.6
V694 Ara SR 13.0 14.0 V 164.5
V696 Ara SR 13.0 14.3 V 53159 127.8 50
V701 Ara RR0 12.7 14.0 V 52821.568 0.55585 18
V706 Ara Lb 13.0 14.0 V
V708 Ara SR 13.3 14.3 V 56.7
V710 Ara * SR 8.5 10.0 V 94.6
V712 Ara SR 12.5 13.3 V 52813 123
V713 Ara Lb 7.86 8.82 V
V719 Ara SR 12.8 14.0 V 77.0
V725 Ara SR 12.7 13.5 V 117
V728 Ara EC 13.0 13.6 V 13.5 52719.824 0.73464
V729 Ara * SR 10.0 11.5 V 52753 38.0
V733 Ara SR 12.3 13.7 V 52441 183
V734 Ara M 13.0 15.4 V 52758 314
V738 Ara Lb: 13.0 13.7 p
V740 Ara EC: 12.9 13.7 V 13.5 52751.696 0.37935
V769 Ara M 12.3 14.7 V 53278 307
V771 Ara M 10.8 14.2 V 52418 185 :
V773 Ara M 11.8 14.2 V 52548 275
V776 Ara M 12.6 15.0 V 52437 206
V779 Ara M 11.7 14.4 V 53125 188.1
V786 Ara RV: 12.6 13.7 V 52129 187
V798 Ara M 10.4 13.5 V 52415 273
V810 Ara SR 11.3 13.0 V 120 :
V813 Ara SR: 13.2 14.2 V 180 :
V815 Ara SR 12.1 12.9 V 55.2
V836 Ara E 7.47 7.65 V 53250.579 7.0337 :
V865 Ara SR 7.55 7.70 V 27.8
V867 Ara EC 7.40 7.60 V 7.57 52764.7376 0.4937123
V870 Ara EC 9.00 9.40 Hp 9.40 52031.780 0.399773
V874 Ara M 11.0 14.2 V 52475 265
R Tel M 7.6 14.8 V 52979 467 43
V Tel SR 9.1 10.2 V 373


Table (Continued)


Name
Type Magnitude Range MinII Epoch, JD 24... Period or

Y
Tel SR 8.6 9.8 V 258
RT Tel Lb 9.3 9.8 V
RU Tel M 9.5 15.0 V 53866 273.3
RV Tel * EA 10.3 12.0 p 51953.664 8.328119 10
SS Tel M 9.1 13.3 V 52566 416.5 45
SW Tel M 10.4 14.3 V 48719 228.2
TY Tel M 10.5 16.0 p 52205 397
UY Tel SR 13.3 14.7 V 133
WZ Tel M 14.4 17.4 p 52032 394
XZ Tel UG: 15.2 19 : p
AA Tel SR 12.5 12.9 V 105
BO Tel CW 12.01 13.4 V 52102.6 14.81659 42
CC Tel M 11.8 15.0 V 53081 425 :
CU Tel SR 12.0 12.5 V 255
FF Tel E: 13.4 14.6 V 52922.570 0.3896
FY Tel RR0 13.1 14.0 V 52751.756 0.67969 30
GQ Tel RR0 14.0 14.8 V 52909.648 0.65107 : 30 :
HO Tel EA 8.22 8.73 V 8.67 52202.506 1.613101 12
IS Tel EA 9.67 10.40 V 9.82 52985.526 1.152800 17
IT Tel RR0 13.5 14.6 V 53819.907 0.68769 20
IY Tel RR0 13.4 14.3 V 52548.646 0.55592 25 :
KL Tel EA 13.4 14.4 V 52884.771 1.6306 15 *
MV Tel RR1 13.5 14.3 V 52874.797 0.30330 50 :
MY Tel EC 13.2 14.1 V 13.5 : 52057.7643 0.55252
NO Tel RR0 13.6 14.5 V 52053.798 0.61392 10
NV Tel EA 9.70 10.35 V 9.83 52179.524 3.544966 07
NX Tel SR 11.5 13.7 p 52924 277
QW Tel EC 7.55 7.69 V 7.67 52445.656 0.411930
QX Tel SRd: 8.62 8.78 Hp 28.3
QZ Tel * EC 8.07 8.27 V 8.27 52831.746 1.0309913
V339 Tel SR 6.80 7.02 V 24.20
V346 Tel Lb 8.96 9.55 V

Remarks. S Ara. Period varies, the given current elements are valid after JD 2441000. RW Ara. Changes of the shape of the light curve due to gaseous streams or to a hot spot are possible. SZ Ara. Period varies. DU Ara. Period varies. V341 Ara. The X-ray source 1RXS J165743.7-631237. Several periods were reported, they satisfy observations only during some time intervals. V447 Ara. A different solution of the ASAS-3 data was suggested in the literature. V617 Ara. Table 1 gives combined magnitudes with a nearby companion. V624 Ara. MaxII 11.9 at the phase 0.4. V639 Ara. V1 (NGC 6397). Cluster non-member. V710 Ara. Individual cycles have amplitudes from to , the secondary cycle is about . V729 Ara. Type RV with a twice longer period is possible. RV Tel. . QZ Tel. A visual double with separation. According to Hipparcos data, the variability is probably due to the fainter, north-eastern (B) component. The variability range in Table 1 is for combined light.

ACKNOWLEDGEMENTS

Thanks are due to V.P. Goranskii whose period-search software is extensively used in our GCVS work. The GCVS studies are supported, in part, by grants from the Russian Foundation for Basic Research (05-02-16289), from the Program "Origin and Evolution of Stars and Galaxies" of the Presidium of Russian Academy of Sciences, and from the Program of Support for Leading Scientific Schools of Russia (NSh 5290.2006.2). We acknowledge our use of ASAS-3 and ROTSE1/NSVS data. The authors are grateful to S.V. Antipin for helpful suggestions.

References:

Kazarovets, E.V., Pastukhova, E.N., Samus, N.N., 2005, Perem. Zvezdy, 25, No. 2

Kholopov, P.N. (ed.), 1985a, General Catalogue of Variable Stars, 4th edition, Volume I, Moscow: Nauka

Kholopov, P.N. (ed.), 1985b, General Catalogue of Variable Stars, 4th edition, Volume II, Moscow: Nauka

Kholopov, P.N. (ed.), 1987, General Catalogue of Variable Stars, 4th edition, Volume III, Moscow: Nauka

Pastukhova, E.N., Antipin, S.V., Samus, N.N., 2004, Inform. Bul. Var. Stars, No. 5522

Pojmanski, G., 2002, Acta Astronomica, 52, 397

Samus, N.N., Durlevich, O.V., Zharova, A.V. et al., 2006, Astronomy Letters, 32, 263

Wozniak, P.R., Vestrand, W.T., Akerlof, C.W. et al., 2004, Astron. J., 127, 2436





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