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: http://www.astronet.ru/db/varstars/msg/1235170
Дата изменения: Fri Jun 19 15:33:44 2009 Дата индексирования: Fri Jan 8 11:29:32 2010 Кодировка: Поисковые слова: rho ophiuchi |
#1. Sternberg Astronomical Institute, Moscow, Russia;
#2. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia; #3. Max Planck Institute for Radio Astronomy, Bonn, Germany; #4. Astro Space Center of Lebedev Physical Institute, Moscow, Russia |
Received: 19.06.2009; accepted: 19.06.2009
(E-mail for contact: antipin@sai.msu.ru)
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Comments:
1. The star No. 8 on Fig. 1 in Kolesnikova et al. (2008). The comparison star is GSC 00429-02187 (17:52:32.65, +07:03:52.5, J2000), V = 12.991. Bpg = 15.2-15.9 on the digitized plates.
2. The comparison star is GSC 00429-00217 (17:54:39.65, +07:11:56.4, J2000), V = 12.613. Bpg = 16.0-16.55 on the digitized plates.
3. Our CCD observations do not cover all phases. The variability type is uncertain. The comparison star is USNO-A2.0 0975-10127960 (17:58:58.75, +09:28:25.3, J2000), V = 14.151. Bpg = 15.65-16.25 on the digitized plates.
4. MinII = 16.35V. The comparison star is GSC 00442-00675 (18:04:01.13, +06:21:42.4, J2000), V = 13.551. Bpg = 15.9-16.8 on the digitized plates.Remarks:
Kolesnikova et al. (2008) used digitized plates of the Moscow stacks to discover 274 new variable stars in a 5x10 degrees field in Ophiuchus. Besides, they suspected 30 stars to be variable. To confirm or disprove their variability, we undertook additional CCD observations using a Pictor 416XTE camera and the 50-cm reflector of the Crimean Laboratory, Sternberg Astronomical Institute, in July-August, 2008. Here we present an investigation of four stars from the list of suspects that we were able to confirm. The comparison and check stars are marked on the finding charts. V magnitudes of the comparison stars were taken from the ASAS-3 online photometry (Pojmanski 2002, http://www.astrouw.edu.pl/asas/?page=aasc). We have averaged the third of five columns of ASAS-3 data and rejected the observations that differed from the mean magnitude by more than 3σ.References:
Kolesnikova, D.M., Sat, L.A., Sokolovsky, K.V., et al., 2008, Acta Astronomica, 58, 279
Pojmanski G., 2002, Acta Astronomica, 52, 397