Variable Stars in Cygnus Discovered with Kourovka Planet Search. Part III: Pulsating variables of Delta Scuti type

A. A. Popov^#1, A. M. Zubareva^#2,3, A. Y. Burdanov^#4, V. V. Krushinsky^#1, E. A. Avvakumova^#1, K. Ivanov^#5

#1. Kourovka Astronomical Observatory of Ural Federal University, Ekaterinburg, Russia; #2. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia; #3. Sternberg Astronomical Institute, Lomonosov Moscow State University, Moscow, Russia; #4. Space sciences, Technologies and Astrophysics Research (STAR) Institute, Université de Liège, Liège, Belgium; #5. Irkutsk State University, Irkutsk, Russia.

Received:   11.12.2017;   accepted:   25.12.2017
(E-mail for contact: apopov66@gmail.com)

Comments:


2. There is a second periodicity P = 0^d.11972.

9. There is a second periodicity P = 0^d.12126.

10. There is a second periodicity P = 0^d.13658.

11. There are long-period changes of brightness.

15. There is a second periodicity P = 0^d.05356.

26. There is a second periodicity P = 0^d.15328.

Remarks:
In the current paper, we continue to announce new variable stars discovered in the frame of the KPS (Kourovka Planet Search). Detailed information about the project and about Algol-type eclipsing binaries we detected is provided in the first paper (Popov et al. 2015), and eclipsing binaries of β Lyrae and W Ursae Majoris- types are presented in the second paper (Popov et al. 2016).

This paper is dedicated to pulsating variables of the δ Scuti type. We discovered 27 such stars.

Each figure consist of three panels. In the upper part, we provide the power spectrum obtained using the on-line light curve analysis tool by Kirill Sokolovsky. The lower part of each figure has two panels. The star’s instrumental magnitude as a function of Julian Date is given in the left panel, and the phase-folded light curve is given in the right panel. We used red colour for R band, green colour for V band, and blue colour for B band data.

Acknowledgements:

This work has been supported by Russian Foundation for Basic Research grants 14-02-31338 and, partially, 14-02-31056.

The authors wish to thank Dr. Kirill Sokolovsky for providing the on-line lightcurve analysis tool.

This research made use of Aladin (Bonnarel et al., 2000), SIMBAD database (operated at the Centre de Données astronomiques de Strasbourg), the International Variable Star Index (VSX) database (operated at AAVSO, Massachusetts, USA), PyRAF (product of the Space Telescope Science Institute, operated by AURA for NASA), and the NASA/IPAC Extragalactic Database (NED) (operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration).

References:
Bonnarel, F., Fernique, P., Bienaymé, O., et al. 2000, Astron. and Astrophys. Suppl., 143, 33
Popov, A. A., Burdanov, A. Y., Zubareva, A. M., Krushinsky, V. V., Avvakumova, E. A., Ivanov, K. I., 2015, Perem. Zvezdy Prilozh., 15, No. 7
Popov, A. A., Burdanov, A. Y., Zubareva, A. M., Krushinsky, V. V., Avvakumova, E. A., Ivanov, K. I., 2016, Perem. Zvezdy Prilozh., 16, No. 5