|#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
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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.
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.
Kolesnikova, D.M., Sat, L.A., Sokolovsky, K.V., et al., 2008, Acta Astronomica, 58, 279
Pojmanski G., 2002, Acta Astronomica, 52, 397