Peremennye Zvezdy


Peremennye Zvezdy (Variable Stars) 25, No. 2, 2005

Received 2005 December 20; accepted 2005 December 30.

Article in PDF

New Light Elements for 100 Variable Stars

E.V. Kazarovets1, E.N. Pastukhova1, N.N. Samus1, 2

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

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


Classifications and light elements, based on data mining in the ASAS-3 and ROTSE-I/NSVS data, are presented for 100 variable stars, 78 of them from the NSV catalog. Availability of online observations makes it possible to suggest all these stars for GCVS Name-Lists.

Introduction

In our work on improved coordinates for all stars in the database of the GCVS and the NSV catalog (Samus et al., 2002, 2003, 2006), it was very important to be able to "recover" many variables (especially those from the NSV catalog), which had no finding charts and only very rough coordinates published. Successful search became possible with publicly available electronic archives of CCD observations from large-scale automatic sky surveys, like ASAS-3 (Pojmanski, 2002) and ROTSE1/NSVS (Wozniak et al., 2004). Recovered variables can be effectively studied using these data. In some cases, additional insight into the lower brightness limit of red variable stars can be gained using the US Naval Observatory Image and Catalog Archive (http://www.nofs.navy.mil/data/fchpix/).

Usually we proceeded in the following way. We selected candidate stars by brightness, within a radius about around the position published by the discoverer. Then the candidates were tested for brightness variations using the CCD archives mentioned above. Alternatively, for fainter variability limits, we sometimes looked for variable stars comparing several images of the USNO Archive. For stars with CCD observations available, we searched for periodicity using the WINEFK code developed by Dr. V.P. Goranskii; usually the well-known Lafler-Kinman algorithm was applied.

In this way, we have already recovered several hundred "lost" variables. A part of them were earlier found by the author of the ASAS-3 survey in the cause of automatic reductions of the original observations and included into the catalog of ASAS-3 variable stars, which contains approximate coordinates, variability types, and parameters of the mean light curves. Note that, in most cases, the ASAS-3 cataloged light elements for stars with uncertain classification (the ASAS type MISC) are, in fact, fictitious.

Results

For this paper, we have selected 100 variable stars, mainly from the NSV catalog but also a number of recently discovered but insufficiently studied variables, for which we were able to derive significant information sufficient for the stars to be named in the GCVS system. The stars will be included in one of the Name-Lists of Variable Stars soon.

Table 1. Coordinates of the studied NSV-catalog stars


NSV

 NSV


NSV 0917

 0246211 -361336 NSV 4944 1041132 -713315
NSV 1773 04 55 30.3 +03 04 28 NSV 4974 10 47 46.5 -46 10 00
NSV 3245 06 50 54.9 -37 29 23 NSV 4984 10 48 46.4 -69 17 50
NSV 3552 07 21 14.8 -29 18 00 NSV 4989 10 50 36.3 -52 30 40
NSV 3967 08 19 47.2 +77 44 32 NSV 4993 10 51 05.6 -55 47 35
NSV 3981 08 17 01.9 -15 00 43 NSV 5010 10 53 23.8 -59 35 12
NSV 4081 08 26 04.2 -30 06 41 NSV 5026 10 57 00.1 -53 45 58
NSV 4114 08 31 02.3 -10 58 04 NSV 5029 10 57 19.2 -55 35 25
NSV 4229 08 43 45.4 -55 01 52 NSV 5046 10 59 25.4 -58 12 18
NSV 4342 08 59 25.8 -55 58 50 NSV 5065 11 00 54.5 -84 05 27
NSV 4378 08 56 35.7 -83 05 11 NSV 5052 11 00 55.4 -48 00 56
NSV 4353 09 01 00.9 -54 57 00 NSV 5061 11 01 48.0 -56 10 31
NSV 4358 09 02 42.4 -30 32 43 NSV 5095 11 07 25.4 -52 48 00
NSV 4381 09 05 18.0 -67 08 24 NSV 5130 11 11 39.7 -54 11 25
NSV 4388 09 07 15.3 -53 25 19 NSV 5135 11 12 32.6 -47 33 41
NSV 4403 09 10 14.7 -37 55 23 NSV 5142 11 13 28.9 -67 35 29
NSV 4424 09 12 57.9 -57 48 28 NSV 5145 11 14 22.4 -42 40 20
NSV 4467 09 21 08.9 -61 56 22 NSV 5148 11 14 59.9 -42 28 27
NSV 4468 09 22 04.5 -36 42 09 NSV 5162 11 17 35.4 -51 37 40
NSV 4487 09 23 08.1 -78 36 41 NSV 5168 11 18 42.7 +27 31 50
NSV 4483 09 23 32.2 -72 22 49 NSV 5176 11 21 58.3 -49 28 55
NSV 4481 09 24 07.0 -36 05 50 NSV 5186 11 23 32.0 -71 36 12
NSV 4535 09 33 14.2 -64 21 07 NSV 5187 11 23 58.3 -33 08 23
NSV 4639 09 49 11.2 -40 41 36 NSV 5191 11 24 05.9 -75 54 49
NSV 4655 09 51 08.6 -57 08 45 NSV 5207 11 26 46.2 -50 47 14
NSV 4708 10 00 19.4 -69 13 40 NSV 5215 11 28 18.5 -49 15 00
NSV 4719 10 03 09.5 -47 24 03 NSV 5216 11 28 21.4 -70 24 06
NSV 4728 10 04 57.7 -60 04 56 NSV 5236 11 30 57.0 -69 34 44
NSV 4735 10 05 27.8 -67 36 59 NSV 5275 11 37 38.9 -72 11 10
NSV 4754 10 07 34.1 -63 09 49 NSV 5292 11 39 25.2 -87 09 26
NSV 4760 10 09 14.3 -62 42 23 NSV 5288 11 40 14.8 -30 15 49
NSV 4780 10 11 50.9 -48 51 19 NSV 5295 11 41 19.5 -72 30 39
NSV 4783 10 12 46.3 -57 49 51 NSV 5301 11 42 33.4 -67 52 09
NSV 4795 10 14 12.1 -66 08 19 NSV 5340 11 47 53.8 -63 44 59
NSV 4805 10 16 16.1 -51 29 25 NSV 5342 11 48 24.1 -67 53 47
NSV 4830 10 21 23.9 -68 50 23 NSV 5406 11 59 19.1 -27 09 03
NSV 4853 10 24 54.1 -63 52 14 NSV 5480 12 10 06.8 -53 25 40
NSV 4900 10 35 03.9 -44 25 32 NSV 5541 12 18 37.0 -53 08 12
NSV 4932 10 40 13.8 -44 19 45 NSV 8470 17 18 10.9 -24 30 05

Remark to Table 1. NSV 5162 has the alternative name NSV 5164; the two entries of the NSV catalog turned out to be the same star.

Table 2. Coordinates of the new variables


Name

 Ref.


Mis V1246

 02 03 21.1 +46 23 48 1
Mis V1190 02 09 46.9 +46 43 17 1
Mis V1250 04 00 39.7 +51 21 02 1
Toa V20 08 25 40.3 -22 10 34 2
GSC 8586-00290 09 00 58.1 -54 55 55 3
GSC 3010-01290 11 13 06.0 +40 21 38 4
GSC 3015-00374 11 21 41.1 +43 36 53 4
GSC 3453-01714 11 32 20.9 +49 44 10 4
GSC 3015-01522 11 33 34.7 +42 58 29 4
GSC 3013-01988 11 35 36.7 +38 45 58 4
Mis V0038 16 51 24.6 -28 21 54 1
GSC 7872-02362 16 56 43.3 -40 36 25 5
Mis V0005 16 59 28.1 -13 23 14 1
Mis V0483 17 59 09.3 -26 38 00 1
Mis V0111 18 57 29.9 +20 05 28 1
Mis V0213 18 57 40.7 -13 13 35 1
Mis V0033 18 57 42.3 -10 49 04 1
Mis V0110 18 59 38.6 +19 59 00 1
Mis V0168 19 02 53.7 -10 26 43 1
Had V107 19 43 21.5 +00 30 35 6
IRAS 19582-0613 20 00 56.8 -06 05 13 7
Brh V124 21 25 44.1 +16 02 11 8

References.
1. http://www.aerith.net/misao; 2. Takao (2003); 3. ASAS-3 (Pojmanski, 2002); 4. Kehoe et al. (2002); 5. Fu et al. (2003); 6. Haseda (2002); 7. Wils (2003a); 8. http://mitglied.lycos.de/KlausBernhard.


Tables 1 presents coordinates for the NSV stars studied by us, Table 2 contains coordinates for newly-discovered variables and references to their discovery announcements.

The variability data for the program stars are collected in Table 3. Its contents is typical of the GCVS. Epochs of maxima for pulsating stars (except the RVA variable) and of minima for the RVA star and eclipsing variables are given. An asterisk in the "Remarks" column means that the star appears in the ASAS-3 variable-star online catalog (Pojmanski, 2002), but our solution differs considerably from that in the cited catalog. Asterisks instead of the photometric system mean CCD unfiltered observations (usually related to -band magnitudes of comparison stars). Remarks concerning several stars follow the table.

Table 3. Variability data


Name

 Rem. Max Min   Type Epoch, 24... Period, d


NSV 0917

   10.2 11.2 M 52886 304
NSV 1773   12.0 14.6 M 51565 396
NSV 3245 1 12.4 15.5 M 53466 299
NSV 3552 2,* 11.3 13.0 SR   290
NSV 3967   9.1 9.6 * SR 51630 56
NSV 3981   12.6 15 M 53054 254
NSV 4081 * 11.0 13.4 RVA 53077.7 58.1
NSV 4114   10.5 15.0 M 53364 315
NSV 4229   11.2 14.0 M 53455 180
NSV 4342   12.4 14.5 SR 53421 460
NSV 4378   12.0 14.8 M 53119 266
NSV 4353   11.7 14.0 M 52903 370
NSV 4358   11.3 15.0 M 53356 326
NSV 4381 * 11.0 12.6 SRA: 52624 252
NSV 4388   11.9 13.8 M 53117 489
NSV 4403 * 12.0 14.4 SRA 53644 261
NSV 4424 * 10.9 15.0 M 53463 301
NSV 4467   11.0 14.2 M 52971 406
NSV 4468 * 10.6 14.3 M 52945 333
NSV 4487   12.4 15.2 M 53133 228
NSV 4483   12.6 15.0 M 53500 245
NSV 4481 * 12.5 14.3 SRA 53070 287
NSV 4535 * 10.8 14.3 M 52174 386
NSV 4639   12.3 16.2 M 52468 236
NSV 4655 * 11.6 12.8 SRA: 52950 346
NSV 4708   13.2 15.0 SR: 53472 344:
NSV 4719   13.7 16.7 EA 52949.8504 4.414288
NSV 4728   12.0 14.2 M 53159 203
NSV 4735   12.6 13.8 SRA: 51939 275:
NSV 4754 * 11. 16.5 M 53455 350
NSV 4760   12.7 16.2: M 52984 304:
NSV 4780 * 11.4 14.0 M 53391 215
NSV 4783   11.8 14.6 M 53443 288
NSV 4795   12.6 15.8 M 52999 328
NSV 4805 * 11. 14.5 M 51941 345
NSV 4830   12.7 15.0 M 52999 290
NSV 4853   12.0 13.8 SRA 52105 376
NSV 4900   10.5 14.0 M 53504 165
NSV 4932 * 12.0 14.5 M 53385 365
NSV 4944   13.0 16.2 M 52566 336
NSV 4974 * 11.1 12.7 SRA 53407 265
NSV 4984 * 10.5 15.8 M 51940 269
NSV 4989   10.8 13.9 M 52952 380
NSV 4993   12.6 14.4 M 53159 270
NSV 5010   12.0 13.1 SRA: 52969 290
NSV 5026   12.2 14.2: SRA: 53512 256


NSV 5029

   12.4 16.8 M 53383 379
NSV 5046   12.3 14.7 SRA: 53561 355
NSV 5065   11.6 14.5 M 53562 305
NSV 5052 * 11.2 14.8 M 53480 240
NSV 5061   10.7 13.0 M 52039 312
NSV 5095   12.6 15.2 M 52830 261
NSV 5130   12.9 14.8 SRA: 51927 281
NSV 5135   11.4 15.3 M 52056 340
NSV 5142   12.0 15.2 M 53541 131
NSV 5145 * 11.9 14.9 M 53539 318
NSV 5148   11.9 14.6 M 53391 273
NSV 5162   10.2 14.6 M 53423 278
NSV 5168   13.8 14.4 * EW 51286.7082 0.33770
NSV 5176   11.6 15.0 M 53466 276
NSV 5186 * 11.2: 13.9 M 52976 323
NSV 5187   13.1 14.3 EA 53499.6027 1.50944
NSV 5191 * 11.3 12.6: SRA 53541 234
NSV 5207   12.3 17.1: M 52963 360:
NSV 5215 3 11.2 13.2 SRA: 52835 145
NSV 5216 * 11.7 14.7 M 53564 268
NSV 5236 * 11.8 13.3 SRA 53476 196
NSV 5275   11.2 14.0 M 53075 334
NSV 5292   11.3 14.9 M 53597 193.4
NSV 5288 * 12.0 12.7 SRA: 52701 148
NSV 5295 4,* 11.0 14.4 M 52650 399
NSV 5301   12.0 14.2 M 53115 290
NSV 5340   11.7 14.6 M 53516 345
NSV 5342   11.0 14.2 M 53541 367
NSV 5406 * 11.7 15.4 M 53457 301
NSV 5480   12.8 15.0 M 53393 325
NSV 5541   13.2 15.0 M: 53141 241
NSV 8470   13.4 15.0 M 52157 261
Mis V1246   10.5 13.6 * M 51410 285:
Mis V1190   12.2 12.9 * EW 51370.877 0.33853
Mis V1250   11.7 13.9 * SRA: 51418 350
Toa V20   12.0 14.6 M 51418 350
GSC 8586-00290   10.6 11.2 SRB   93.3
GSC 3010-01290   11.66 12.04 * RRC 51306.702 0.31802
GSC 3015-00374   11.57 11.83 * EW 51312.8513 0.476058
GSC 3453-01714   11.97 12.60 * EW 51563.9502 0.410384
GSC 3015-01522   11.75 12.16 * EW 51330.7415 0.800632
GSC 3013-01988   11.8 12.3 * RRC 51305.7228 0.267946
Mis V0038   12.4 16.0 M 52483 555:
GSC 7872-02362 5 11.0 (0.22) EA 52468.5701 1.9083
Mis V0005   13.1 14.9 M 52821 210
Mis V0483   12.9 18.0 M 52465 585


Mis V0111

   11.8 15.2 M 53574 364:
Mis V0213   12.4 14.1 M 53469 288
Mis V0033   13.0 15.8 M 53240 291:
Mis V0110   11.0 13.3 * M 51375 365:
Mis V0168   10.5 13.2 * M 53275 370
Had V107   12.2 13.4 * SRA 51335 192
IRAS 19582-0613   12.1 14.6 M 53166 321
Brh V124   11.2 13.0 M 52952 223

Remarks to Table 3

  1. in Wils (2003b) is wrong.
  2. (P. Wils, vsnet-id No. 791, 2003) is worse.
  3. This is a wide double star, with a separation about 05. The ASAS-3 catalog contains the northern component as a variable. The infrared colors clearly indicate that the southern star must be the variable. Though it is formally possible to retrieve ASAS-3 observations separately for the northern and the southern component, the times of brightenings actually coincide. The ASAS-3 period (850) seems wrong.
  4. in Wils (2003b) is wrong.
  5. The star's period was first determined by Fu et al. (2005) as .

    Acknowledgements

    We wish to thank Dr. V.P. Goranskii for providing his excellent period-search software. Our GCVS studies are supported, in part, by grants from the Russian Foundation for Basic Research (05-02-16289) and from the Program of Support for Leading Scientific Schools of Russia (NSh-389-2003-2). We acknowledge with many thanks our use of excellent ASAS-3 and ROTSE1/NSVS data. This study made use of images from the Image and Catalog Archive of the Flagstaff Station of the US Naval Observatory.

    References:

    Fu, J.N., Bouzid, M.Y., Sterken, C., 2005, Astron. Nachr., 326, 349

    Fu, J.N., Sterken, C., Duerbeck, H.W., Mennickent, R.E., 2003, Astron. & Astrophys., 412, 97

    Haseda, K., 2002, vsnet-newvar 1520

    Kehoe, R., Akerlof, C., Balsano, R. et al., 2002, Astrophys. J., 577, 845

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

    Samus, N.N., Durlevich, O.V., Zharova, A.V. et al. 2006, Astron. Letters (accepted)

    Samus, N.N., Goranskii, V.P., Durlevich, O.V. et al. 2002, Astron. Letters, 28, 174

    Samus, N.N., Goranskii, V.P., Durlevich, O.V. et al. 2003, Astron. Letters, 29, 468

    Takao, A., 2003, vsnet-newvar 1805

    Wils, P., 2003a, Inform. Bul. Var. Stars, No. 5401

    Wils, P., 2003b, Inform. Bul. Var. Stars, No. 5457

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


Main Page | Search
Astronet | SAI | INASAN

Report problems