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"Peremennye Zvezdy", Prilozhenie, vol. 13, N 12 (2013) |
#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: 10.01.2013; accepted: 14.09.2013
(E-mail for contact: slovoktk@mail.ru)
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Comments:
2. MinII = 14m.62.
3. Jmag = 12.103, Hmag = 11.412, Kmag = 11.211 (2MASS).
5. MinII = 14m.95. Slight O'Connel effect.
9. Twice longer period is possible.
10. Jmag = 9.148, Hmag = 8.142, Kmag = 7.784 (2MASS).
The star in the NSVS database: NSVS ID 6070590. The NSVS data confirm the star's type.
13. MinII = 16m.51.
14. MinII = 15m.3.
16. Twice shorter period is also possible. O'Connel effect.
18. The star has at least two pulsation periods. One period is given in the table, the second is P = 0d.101399.
23. MinII = 14m.88.
24. Jmag = 12.848, Hmag = 12.445, Kmag = 12.359 (2MASS).
To determine period of this star we also used images obtained on August 16 and October 30, 2011.
25. MinII = 13m.58.
26. Jmag = 11.697, Hmag = 11.036, Kmag = 10.897 (2MASS).
27. Jmag = 11.253, Hmag = 10.618, Kmag = 10.466 (2MASS).
28. MinII = 13m.26.
29. Jmag = 13.443, Hmag = 12.859, Kmag = 12.679 (2MASS).
33. Jmag = 9.888, Hmag = 8.900, Kmag = 8.584 (2MASS).
34. Jmag = 10.171, Hmag = 9.189, Kmag = 8.846 (2MASS).
35. Jmag = 10.286, Hmag = 9.304, Kmag = 8.994 (2MASS).
36. MinII = 14m.93.
41. MinII = 16m.44.
47. Jmag = 8.887, Hmag = 7.878, Kmag = 7.494 (2MASS).
48. Jmag = 13.092, Hmag = 12.448, Kmag = 12.305 (2MASS).
49. Twice longer period is quite possible.
51. Jmag = 10.115, Hmag = 8.410, Kmag = 7.097 (2MASS).
55. MinII = 14m.54.
59. Jmag = 8.724, Hmag = 7.313, Kmag = 6.358 (2MASS).
60. P = 0d.12351 is possible.
63. MinII = 15m.84.
66. Jmag = 9.782, Hmag = 8.860, Kmag= 8.494 (2MASS).
To plot the light curve we also used images obtained on August 16 and October 30, 2011.
67. Jmag = 8.320, Hmag = 7.352, Kmag = 7.011 (2MASS).
The star in the NSVS database: NSVS ID 6176027. The NSVS data confirm the star's type.
68. Jmag = 12.304, Hmag = 11.636, Kmag = 11.503 (2MASS).
70. MinII = 15m.9.
75. MinII = 14m.65.
79. MinII = 15m.3.
80. MinII = 14m.39.
82. Jmag = 12.570, Hmag = 11.950, Kmag = 11.788 (2MASS).
To determine period of this star we also used images obtained on August 16 and October 30, 2011.
83. MinII = 16m.15.
85. MinII = 13m.54.
88. MinII = 14m.04.
92. MinII = 12m.78.
94. MinII = 14m.37.
99. Jmag = 9.675 Hmag = 8.679 Kmag = 8.319 (2MASS).
The star in the NSVS database: NSVS ID 6178264. The NSVS data confirm the star's type.
100. MinII = 15m.4.
101. MinII = 13m.31.
102. MinII = 14m.09.
104. Jmag = 12.905, Hmag = 12.270, Kmag = 12.175.
107. MinII = 14m.69.
112. Jmag = 9.142, Hmag = 8.121, Kmag = 7.803 (2MASS).
The star in the NSVS database: NSVS ID 6180054.
113. Jmag = 12.467, Hmag = 11.871, Kmag = 11.767 (2MASS).
117. MinII = 15m.3.
121. MinII = 14m.5.
122. MinII = 15m.15.
127. MinII = 14m.78.
128. MinII = 15m.34.
129. Jmag = 9.932, Hmag = 8.982, Kmag = 8.671 (2MASS).
The star in the NSVS database: NSVS ID 6181387.
To search for star's period we also used images obtained on August 16 and October 30, 2011.
130. Twice longer period is possible.
132. The star in the NSVS database: NSVS ID 6181268. The NSVS data confirm the star's type.
136. MinII = 13m.95.
138. Jmag = 13.266, Hmag = 12.822, Kmag = 12.721 (2MASS).
140. Jmag = 8.731, Hmag = 7.739, Kmag = 7.448 (2MASS).
The star in the NSVS database: NSVS ID 6182087.
141. P = 0d.4109221 is also possible: RRC type.
142. MinII = 16m.45.
143. MinII = 13m.24.
144. MinII = 14m.73Remarks:
Our observations of an area in Lacerta were performed in the observatory of the Siberian State Aerospace University with a Hamilton telescope (D = 400 mm, F = 915 mm) equipped with a FLI ML9000 CCD chip (3056x3056 pixels, pixel size 12 μm). We obtained all unfiltered CCD observations during time interval from August 2012 to November 2012. 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). For two previously known variables, EH Lac and V440 Lac, we present new light elements.
Acknowledgements: The authors wish to thank 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.References:
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