|#1. Siberian State Aerospace University, Krasnoyarsk, Russia;
#2. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia;
#3. Sternberg Astronomical Institute, Lomonosov Moscow State University, Moscow, Russia
Received: 5.06.2013; accepted: 24.04.2014
(E-mail for contact: email@example.com)
7. Combined brightness of two close stars, 2MASS J22431530+5028249 (J = 13.413, H = 13.470, K = 13.470) and 2MASS J22431499+5028244 (J = 13.907, H = 13.582, K = 13.487), was measured. The second one probably varies.
8. J = 8.182, H = 7.206, K = 6.851 (2MASS).
9. Combined brightness of two close stars, 2MASS J22433052+5000002 (J = 14.922, H = 14.580, K = 14.514) and 2MASS J22433029+4959576 (J = 14.906, H = 14.551, K = 14.323), was measured.
12. P = 0d.19176 is also possible with DSCT type.
16. J = 10.550, H = 9.639, K = 9.390 (2MASS).
17. MinII = 15m.88.
20. Twice shorter period is also possible.
26. O'Connell effect.
32. J = 13.408, H = 12.793, K = 12.616 (2MASS).
33. O'Connell effect.
35. J = 9.655, H = 9.081, K = 8.900 (2MASS).
37. J = 9.613, H = 8.622, K = 8.358 (2MASS).
40. J = 9.189, H = 8.198, K = 7.897 (2MASS).
43. Combined brightness of two close stars, 2MASS J22451536+4904507 (J = 11.902, H = 11.554, K = 11.459) and 2MASS J22451517+4904573 (J = 13.525, H = 13.325, K = 13.276), was measured. The first one probably varies.
45. Combined brightness of two close stars, 2MASS J22452406+4935318 (J = 13.393, H = 13.038, K = 13.028) and 2MASS J22451517+4904573 (J = 13.525, H = 13.325, K = 13.276), was measured.
50. MinII = 13m.74.
51. MinII = 14m.07.
Combined brightness of two close stars, 2MASS J22453398+4906590 (J = 14.300, H = 13.834, K = 13.785) and 2MASS J22453405+4907033 (J = 13.100, H = 12.910, K = 12.819), was measured. The first one probably varies.
52. J = 10.539, H = 9.570, K = 9.166 (2MASS).
53. MinII = 13m.77.
Combined brightness of two close stars, 2MASS J22454829+4916265 (J = 12.929, H = 12.761, K = 12.716) and 2MASS J22454858+4916322 (J = 14.979, H = 14.552, K = 14.433), was measured. The second one probably varies.
58. J = 9.417, H = 8.478, K = 8.213 (2MASS).
62. Only one minimum was observed.
On August 16 – October 30, 2011, we obtained about 1600 images with 30-second exposures of a field in Lacerta for discovery and investigation of new variables stars.
The field center has the coordinates α = 22h50m, δ = +50°00′, and the size of our frames is 2°.3 × 2°.3. In this paper, we present the first part of our results.
Our observations were performed in the city of Krasnoyarsk with a Hamilton telescope (D = 400 mm, F = 915 mm) equipped with an unfiltered FLI ML-9000 CCD camera (3056 × 3056 pixels, pixel size 12 μm).
For basic reductions for dark current, flat fields, bias, and for removing cosmic-ray hits, we used MaxImDL software.
The magnitudes were referred to red magnitudes of comparison stars from the USNO-A2.0 catalog (Monet et al. 1998).
For search and photometry of the majority of the new variable stars, we applied VaST software (developed by K. Sokolovsky and A. Lebedev, described by Kolesnikova et al. 2008). Several variable stars were found with the C-Munipack package.
To search for periods, we applied WinEfk software provided by Dr. V.P. Goranskij.
Acknowledgements: The authors wish to thank Dr. V.P. Goranskij for providing his efficient period-search software, Dr. K. Sokolovsky and A. Lebedev for their fine VaST software.
Monet, D., Bird, A., Canzian, B., et al., 1998, USNO-A2.0, A Catalog of Astrometric Standards (U.S. Naval Observatory, Washington, DC), Centre de Données Astronomiques de Strasbourg, I/252
Kolesnikova, D.M., Sat, L.A., Sokolovsky, K.V., et al., 2008, Acta Astron., 58, 279