Article in PDF |
"Peremennye Zvezdy", Prilozhenie, vol. 21, N 3 (2021) |
#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: 10.24412/2221-0474-2021-3 |
Received: 3.12.2016; accepted: 31.08.2021
(E-mail for contact: slovoktk@mail.ru)
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Comments:
1. MinII = 16m.21.
2. Possible DSCT type with P = 0.08506 d and JD0 = 2456928.241.
3. J = 11m.870, H = 11m.199, K = 10m.991 (2MASS).
7. MinII = 15m.26.
9. MinII = 15m.27.
11. J = 9m.384, H = 8m.392, K = 8m.079 (2MASS).
12. J = 8m.352, H = 7m.613, K = 7m.256 (2MASS).
13. EW type with twice longer period is possible (0.31671 d, JD0 = 2456934.179).
14. J = 12m.425, H = 11m.904, K = 11m.762 (2MASS).
15. J = 8m.256, H = 7m.217, K = 6m.809 (2MASS).
The object is in the NSVS database: ID 3468452.
17. J = 8m.819, H = 7m.774, K = 7m.414 (2MASS).
19. J = 11m.476, H = 11m.770, K = 11m.541 (2MASS).
23. MinII = 15m.36.
25. MinII = 15m.07.
26. J = 9m.648, H = 8m.659, K = 8m.387 (2MASS).
28. J = 10m.214, H = 8m.472, K = 7m.177 (2MASS).
29. J = 8m.760, H = 7m.695, K = 7m.241 (2MASS).
30. J = 6m.969, H = 5m.924, K = 5m.470 (2MASS).
The object is in the NSVS database: ID 3470780.
31. MinII = 13m.65.
32. J = 8m.588, H = 7m.616, K = 7m.219 (2MASS).
33. MinII = 16m.03.
35. J = 9m.788, H = 8m.713, K = 8m.385 (2MASS).
36. EW type with twice longer period (0.17079 d) is possible.
37. Twice longer period (0.572456 d) is possible.
42. MinII = 13m.90.
46. J = 8m.812, H = 7m.825, K = 7m.439 (2MASS).
48. J = 10m.510, H = 9m.486, K = 9m.074 (2MASS).Remarks:
We present the second part of new discoveries of variable stars in Lacerta: area of 2°.3×2°.3, center α=22h50m δ=54°00′(2000.0). Some of the objects are newly discovered, some are already known from massive surveys like ZTF and ASAS-SN.
Our observations of an area in Lacerta were performed in 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.
We obtained all unfiltered CCD observations 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). We used VaST software (Sokolovsky & Lebedev 2018) to search for variable stars. To perform periodogram analysis, we applied WinEfk software provided by V.P. Goranskij.
This work was supported by Ministry of Education and Science of Russian Federation within the framework of state contract 3.6822.2017/7.8.
Acknowledgements: The authors are grateful to 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., Girard, T. M. et al., 2013, Astron. J., 145, 44, The Fourth US Naval Observatory CCD Astrograph Catalog (UCAC4)