New Variable Stars in Perseus

T. Kryachko^#1, A. Samokhvalov^#2, B. Satovskiy^#1

#1. Astrotel Observatory, Karachay-Cherkessia, Russia; #2. Surgut, Russia.

Received:   17.03.2013;   accepted:   8.04.2013
(E-mail for contact: bredfild@mail.ru, sav@surgut.ru, bs25@mail.ru)

Comments:


1. Type DSCT and period 0^d.1441 are also possible. Primary minima:

HJD(TT)	±
2455870.3295	0.0004
2455906.3605	0.0009

Min_II = 13^m.68.

2. Primary minima:

HJD(TT)	±
2455870.4074	0.0007
2455906.536	0.001

Min_II = 16^m.37.

3. Min_II = 18^m.24.

4. Primary minimum: HJD(TT) 2455906.453±0.005.

5. Primary minima:

HJD(TT)	±
2455870.4054	0.0003
2455906.4754	0.0007

Min_II = 15^m.85.

6. A close pair of two stars: USNO-A2.0 1200-02275043 and 2MASS 04274467+3215128, USNO-A2.0 1200-02275043 varies. Min_II = 16^m.10.

8. Primary minimum: HJD(TT) 2455906.3521±0.0004. Min_II = 12^m.95.

9. Maxima:

HJD(TT)	±
2455869.360	0.001
2455870.3700	0.0007
2455906.3718	0.0004
2455906.4655	0.0006

10. Primary minimum: HJD(TT) 2455869.3330±0.0009.

11. Min_II = 16^m.49.

12. Infrared colors J–H = 0.986, H–K = 0.423, J–K = 1.409 (2MASS) are consistent with the M spectral type (Bessell and Brett 1988) and SR: classification. Maximum: HJD(TT) 2455872.5±0.6.

Remarks:
During observations of a field in Perseus, we discovered 12 new variable stars. Our observations were carried out at the Astrotel-Caucasus observatory located at the Astronomical station of the Kazan Federal university using the 300-mm Ritchey-Chretien telescope, equipped with an unfiltered Apogee Alta U9000 CCD camera. A total of 256 images with 5-minute exposures were obtained on JD 2455826–2455906. For basic reductions for dark current, flat fields, bias and for removing cosmic-ray hits we used IRAF routines. For search and photometry of new variable stars, we applied VaST software by Sokolovsky and Lebedev (2005). The comparison star was USNO-A2.0 1200-02275475 = USNO-B1.0 1224-0079451 (α = 04^h27^m46^s.76, δ = +32°25′ 34″.2 (J2000, 2MASS)), R₁ = 13^m.97 R₂ = 13^m.60 (USNO-B1.0). Unfiltered magnitudes were calibrated using the comparison star, assuming R_comp = 13^m.785. The coordinates of the variable stars in the table were drawn from the 2MASS catalogue (Skrutskie et al. 2006) except for a star USNO-A2.0 1200-02287405; their coordinates were drawn from the USNO-A2.0 catalogue (Monet et al. 1998). For search for periods and epochs of extrema we use Peranso software.

Acknowledgements: We would like to thank S. V. Antipin and N. N. Samus for helpful discussion.

References:
Bessell, M.S., Brett, J.M., 1988, Publ. Astron. Soc. Pacific, 100, 1134
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 Donnees Astronomiques de Strasbourg, I/252
Skrutskie, M.F., Cutri, R.M., Stiening, R., et al., 2006, Astron. J., 131, 1163
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