|Article in PDF||
vol. 20, N 2 (2020)
|#1. Reshetnev Siberian State University of Science and Technology, 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: 10.24411/2221-0474-2020-10013|
Received: 3.12.2016; accepted: 15.12.2020
(E-mail for contact: email@example.com)
1. MinII = 15m.85.
4. MinII = 13m.23.
6. J=7m.843, H=7m.751, K=7m.327 (2MASS).
7. MinII = 12m.11.
8. MinII = 12m.75.
9. MinII = 16m.9:.
10. J=7m.843, H=6m.740, K=6m.294 (2MASS).
The object is in the NSVS database: NSVS ID 3463164.
14. J=11m.000, H=10m.375 K=10m.228 (2MASS).
15. J=10m.849, H=9m.860 K=9m.563 (2MASS).
16. J=10m.314, H=9m.238 K=8m.959 (2MASS).
20. J=9m.731, H=8m.734 K=8m.442 (2MASS).
23. MinII = 14m.98.
24. J=8m.770, H=7m.790 K=7m.479 (2MASS).
25. MinII = 15m.25.
26. MinII = 15m.08.
27. J=10m.515, H=9m.600 K=9m.321 (2MASS).
28. MinII = 15m.81.
29. MinII = 16m.75.
30. MinII = 15m.80.
31. MinII = 13m.41.
32. J=8m.851, H=7m.830 K=7m.499 (2MASS).
35. MinII = 17m.02.
37. MinII = 13m.96.
38. MinII = 12m.98.
40. MinII = 14m.74.
41. J=9m.763, H=8m.738 K=8m.434 (2MASS).
42. J=8m.887, H=7m.878 K=7m.494 (2MASS).
43. MinII = 15m.43.
44. J=9m.288, H=8m.341 K=8m.081 (2MASS).
45. MinII = 16m.30.
46. MinII = 14m.35.
47. MinII = 13m.17.
48. MinII = 13m.33.
49. MinII = 15m.66.
We present the first part of the list of variable stars in Lacerta: area of 2°.3×2°.3, centered at α=22h50m δ=54°00′ (2000.0). Some of objects are newly discovered, some are already known from massive surveys like ZTF and ASAS-SN. GW Lac was discovered by C. Hoffmeister (1967), but had no period.
Our observations of the field in Lacerta were performed at the observatory of 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 periods: August–October 2012 and September–October 2014.
The magnitudes were referred to unfiltered red band of comparison stars from the UCAC4 catalog (Zacharias et al. 2013). We used VaST software (Sokolovsky & Lebedev 2018) to search for variable stars. To search for periods, we applied WinEfk software provided by 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).
Hoffmeister, C., 1967, Astron. Nachr., 289, H.5, 205
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)