Peremennye Zvezdy

"Peremennye Zvezdy",
Prilozhenie
,
vol. 9, N 21 (2009)

CCD Observations of Four Stars Suspected in Variability from Digitized Moscow Plates

S. V. Antipin#1,2, A. M. Zubareva#2, D. Kolesnikova#2, N. N. Samus#2,1, L. A. Sat#1, K. V. Sokolovsky#3,4
#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)


#NameOtherCoord (J2000)TypeMaxMinSystemPeriodEpoch (JD)typeSpCommentL.CurveFind.ChartData
1 MDV313, USNO-A2.0 0900-1077948517 52 28.67, +07 01 01.4EA15.0015.40V0.68131972454674.32min Comm. 1mdv313lc.jpgmdv313ch.jpgmdv313ccd.dat
2 MDV314, USNO-A2.0 0900-1088692417 54 37.74, +07 10 45.6HADS:15.9516.45V0.18338172454671.315max Comm. 2mdv314lc.jpgmdv314ch.jpgmdv314ccd.dat
3 MDV315, USNO-A2.0 0975-1012532817 58 54.93, +09 27 45.6EB:15.5215.81:V0.7028912442874.57min Comm. 3mdv315lc.jpgmdv315ch.jpgmdv315ccd.dat
4 MDV316, USNO-A2.0 0900-1142387718 03 58.96, +06 21 30.6EW15.7016.35V0.35553382454666.32min Comm. 4mdv316lc.jpgmdv316ch.jpgmdv316ccd.dat

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



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