Article in PDF |
"Peremennye Zvezdy", Prilozhenie, vol. 14, N 12 (2014) |
#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 |
ISSN 2221–0474 |
Received: 24.03.2012; accepted: 16.12.2014
(E-mail for contact: slovoktk@mail.ru)
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Comments:
1. MinII = 16m.82.
2. MinII = 15m.78.
3. MinII = 15m.30.
4. MinII = 14m.63.
5. MinII = 14m.22.
6. J = 9.701, H = 8.762, K = 8.431 (2MASS).
7. MinII = 12m.08.
8. J = 9.257, H = 8.282, K = 7.954 (2MASS).
10. MinII = 14m.21.
11. J = 11.879, H = 11.296, K = 11.174 (2MASS).
15. J = 10.952, H = 10.464, K = 10.308 (2MASS).
16. MinII = 16m.02.
17. MinII = 15m.69. O'Connell effect.
18. MinII = 15m.06:.
19. MinII = 15m.80.
20. MinII = 16m.47.
21. MinII = 17m.1.
22. MinII = 14m.40. A twice shorter period with RRC type is possible.
24. MinII = 13m.14.
25. MinII = 15m.55.
26. J = 13.765, H = 13.145, K = 13.000 (2MASS).
27. MinII = 14m.72.
28. J = 12.185, H = 11.573, K = 11.452 (2MASS).
29. MinII = 15m.6.
30. MinII = 14m.53.
31. MinII = 14m.45.
32. MinII = 12m.64.
33. J = 12.526, H = 12.266, K = 12.168 (2MASS).
34. MinII = 14m.02.
35. MinII = 17m.1.
36. MinII = 12m.53.
37. MinII = 16m.15.
38. MinII = 13m.49.
GSC 03630-00738. Bakos et al. (2002) found P = 0d.18.
39. MinII = 15m.08.
40. MinII = 15m.17.
41. MinII = 12m.65.
42. MinII = 15m.00.
44. MinII = 15m.66.
45. J = 9.803, H = 8.853, K = 8.565 (2MASS).
46. MinII = 14m.35.
47. MinII = 17m.8.
48. J = 11.999, H = 11.369, K = 11.237 (2MASS).
49. MinII = 13m.20.
50. MinII = 17m.3.
51. J = 12.827, H = 12.200, K = 12.035 (2MASS).
52. MinII = 12m.65:.
53. MinII = 16m.6.
54. MinII = 16m.48.
55. J = 8.940, H = 7.999, K = 7.739 (2MASS).
56. MinII = 13m.80. O'Connell effect.
57. MinII = 12m.31.
GSC 03630-00750. Bakos et al. (2002) found P = 0d.43.
58. MinII = 16m.5.
59. A twice longer period with EW type is possible.
60. MinII = 15m.61.
61. MinII = 17m.6.
62. MinII = 14m.62.Remarks:
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 has the coordinates α = 22h50m , δ = +50°00′ and size 2.3°×2.3°. Here the third part of our results is presented.
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 MaxIm DL 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 new variable stars, we applied VaST software (developed by K. Sokolovsky and A. Lebedev, described by Kolesnikova et al. 2008). Some of the variable stars were found with C-Munipack package. To search for periods, we applied WinEfk software provided by V.P. Goranskij.
We also determined types and periods for two known variable stars (GSC 03630-00738 and GSC 03630-00750).
Acknowledgements: The authors wish to thank Dr. V.P. Goranskij for providing WinEfk software and Dr. K. Sokolovsky and A. Lebedev for VaST software.References:
Bakos, G.A., Lazar, J., Papp, I., et al., 2002, Publ. Astron. Soc. Pacific, 114, 974
Kolesnikova, D.M., Sat, L.A., Sokolovsky, K.V., et al., 2008, Acta Astron., 58, 279
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