Article in PDF |
"Peremennye Zvezdy", Prilozhenie, vol. 22, N 2 (2022) |
#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; #4. Samarkand State University, Samarkand, Republic of Uzbekistan. |
ISSN 2221–0474 | DOI: 10.24412/2221-0474-2022-2 |
Received: 3.12.2016; accepted: 1.11.2022
(E-mail for contact: slovoktk@mail.ru)
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Comments:
1. MinII = 15m.05. D = 0.1 P.
2. MinII = 12m.37.
3. J = 8m.425, H = 7m.401, K = 7m.055 (2MASS). NSVS catalog entry: Object ID 3472469.
4. MinII = 16m.7.
5. J = 8m.328, H = 7m.257, K = 6m.849 (2MASS). NSVS catalog entry: Object ID 3471820.
6. J = 9m.743, H = 8m.733, K = 8m.433 (2MASS).
7. MinII = 14m.82. O'Connell effect.
9. MinII = 14m.55.
10. MinII = 14m.8. D = 0.16 P.
11. MinII = 15m.75.
12. MinII = 14m.61.
13. MinII = 13m.14. D = 0.12 P.
14. MinII = 16m.8.
15. J = 11m.655, H = 11m.341, K = 11m.258 (2MASS).
16. MinII = 15m.55:. D = 0.18 P.
17. J = 10m.889, H = 10m.256, K = 10m.108 (2MASS).
18. J = 11m.772, H = 11m.502, K = 11m.438 (2MASS).
20. J = 8m.587, H = 8m.588, K = 7m.125 (2MASS). NSVS catalog entry: Object ID 3473769.
21. MinII = 12m.92. O'Connell effect.
22. MinII = 15m.46. D = 0.16 P.
24. MinII = 14m.80.
25. MinII = 13m.94.
26. MinII = 15m.63.
27. J = 9m.232, H = 8m.059, K = 7m.667 (2MASS).
29. J = 9m.671, H = 5m.549, K = 8m.167 (2MASS).
30. Twice shorter period (1.2339 d) is possible.
31. D = 0.16: P. Twice longer period is possible.
32. MinII = 15m.2. D = 0.16 P.
33. MinII = 15m.68. D = 0.10: P.
34. D = 0.16: P. Twice longer period is possible.
36. MinII = 16m.8:.
37. Twice longer period is possible.
38. MinII = 15m.93.
39. MinII = 15m.44.
40. MinII = 15m.04. D = 0.17 P.
41. MinII = 14m.88. D = 0.18 P.
46. The star became brighter by 0m.06 between 2012 and 2014. The magnitude ranges within the observational seasons are: 13m.31–13m.36 in 2012, 13m.36–13m.46 in 2014.
47. MinII = 15m.53.
48. MinII = 15m.04.Remarks:
We present the third part of our discoveries of variable stars in Lacerta: area of 2°.3×2°.3, centered at α=22h50m δ=54°00′. Some of the objects are newly discoveries, some are already known from large scale surveys like ZTF and ASAS-SN.
Our observations of an area in Lacerta were performed at the observatory of the Reshetnev Siberian State University of Science and Technology with a Hamilton telescope (D = 400 mm, F = 915 mm), equipped with an FLI ML9000 CCD chip (3056×3056 pixels, pixel size 12 μm). Exposures of all frames were 30 seconds. A CCD image covers 2°.3×2°.3 of the sky.
All unfiltered CCD observations were obtained during two time intervals: August–October 2012 and September–October 2014.
The magnitudes were referred to those of comparison stars (in unfiltered red band) from the UCAC4 catalog (Zacharias et al. 2013) using VaST software(Sokolovsky and Lebedev 2018). We also used VaST to search for new variable stars. To define periods, we applied WinEfk software provided by Dr. V. P. Goranskij.
This work was supported by Ministry of Education and Science of Russian Federation within limits of state contract 3.6822.2017/7.8.
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).References:
Sokolovsky, K. V., Lebedev, A. A., 2018, Astron. and Computing, 22, 28
Zacharias, N., Finch, C. T., et al., 2013, The Fourth US Naval Observatory CCD Astrograph Catalog (UCAC4)