|#1. Siberian State Aerospace University, Krasnoyarsk, Russia;
#2. Sternberg Astronomical Institute, Lomonosov Moscow State University, Moscow, Russia;
#3. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia
Received: 12.07.2012; accepted: 5.12.2012
(E-mail for contact: firstname.lastname@example.org)
3. P = 0d.3409505 is also possible.
4. MinII = 13m.15. B = 13.8, R = 13.1 (USNO-A2.0). DSCT type with P = 0d.132695 is possible.
6. MinII = 16m.3. P = 0d.362922 is also possible.
8. MinII = 14m.54.
9. The one-day alias, P = 0d.086921, is also possible.
10. MinII = 15m.77.
11. MinII = 14m.42.
12. MinII = 16m.2.
13. The one-day alias, P = 0d.195018, is also possible.
14. B = 17.0, R = 14.0 (USNO-A2.0). J = 7.249, H = 6.149, K = 5.660 (2MASS).
15. B = 15.7, R = 13.5 (USNO-A2.0). J = 11.737, H = 11.124, K = 10.877 (2MASS).
17. MinII = 12m.93.
18. The star in the NSVS database: NSVS ID 7023650 and NSVS ID 7008698. The NSVS data confirm the star's type.
B = 17.5, R = 14.4 (USNO-A2.0). J = 8.456, H = 7.391, K = 6.934 (2MASS).
20. MinII = 13m.46.
21. MinII = 15m.85.
22. The star in the NSVS database: NSVS ID 7075110. The NSVS data confirm the star's type and period.
25. MinII = 14m.2.
27. P = 2d.20781 is one of several possible periods. Additional CCD observations are needed to choose the true period.
28. B = 16.4, R = 13.9 (USNO-A2.0). J = 9.155, H = 8.111, K = 7.676 (2MASS).
29. X-ray source 1RXS J060210.7+282821, HR1 = 1.0, HR2 = 0.57, distan˝e 3".53.
B = 14.6, R = 13.4 (USNO-A2.0). J = 12.231, H = 11.222, K = 10.140 (2MASS).
31. MinII = 14m.52.
32. MinII = 15m.9.
35. B = 14.0, R = 12.2 (USNO-A2.0). J = 10.265, H = 9.144, K = 8.783 (2MASS).
36. The star in the NSVS database: NSVS ID 7014088. The NSVS data confirm the star's type.
B = 15.1, R = 12.6 (USNO-A2.0). J = 8.741, H = 7.615, K = 7.250 (2MASS).
37. MinII = 12m.91.
38. MinII = 14m.06, slight O'Connell effect.
39. The twice longer period with EW type is also not excluded.
40. J = 10.405, H = 9.466, K = 9.220 (2MASS).
42. MinII = 15m.07.
43. MinII = 16m.45.
44. B = 17.2, R = 14.3 (USNO-A2.0). J = 10.042, H = 8.827, K = 8.444 (2MASS).
Our observations of an area in Auriga were performed in the observatory of the Siberian State Aerospace University with a Hamilton telescope (D = 400 mm, F = 915 mm) equipped with an FLI ML9000 CCD chip (3056x3056 pixels, pixel size 12 μm). We obtained all unfiltered CCD observations during two time intervals: January 2011 – March 2011 and October 2011. Exposure times were 30 seconds for all frames. The size of the field is 2°.3 × 2°.3. The magnitudes were referred to red magnitudes of comparison stars from the USNO-A2.0 catalog (Monet et al. 1998). We used VaST (Sokolovsky & Lebedev 2005) software to search for new variable stars. To find periods, we applied WinEfk software provided by Dr. V.P. Goranskij. Observations for several stars can also be found in the ROTSE-I/NSVS survey (Wozniak et al. 2004).
Acknowledgements: The authors wish to thanks Dr. V.P. Goranskij for providing his efficient period-search software and Dr. K.V. Sokolovsky for providing VaST (a software package for detection of variable objects on a series of astronomical images). This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the UMass/IPAC-Caltech, funded by the NASA and the NSF, and the Aladin interactive sky atlas, operated at CDS, Strasbourg, France.
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
Sokolovsky, K., Lebedev, A., 2005, in 12th Young Scientists' Conference on Astronomy and Space Physics, Kyiv, Ukraine, April 19-23, 2005, eds.: Simon, A.; Golovin, A., p.79
Wozniak, P.R., Vestrand, W.T., Akerlof, C.W., et al., 2004, Astron. J., 127, 2436