Investigation and New Light Elements of 15 Variable Stars

E. V. Kazarovets, E. N. Pastukhova
Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia

Received:   21.11.2018;   accepted:   28.12.2018
(E-mail for contact: helene@inasan.ru, pastukhova@sai.msu.ru)

Comments:


1. The star was independently discovered by us and by the ASAS-SN patrol patrol team. Our results from the Table were obtained using the CRTS archive data (SSS_J200226.6-415932) for interval JD 2453556–2456460. The ASAS-SN Catalog of Variable Stars (Jayasinghe et al. 2018) gives light elements HJD 2456912.61015 + 0.3354747d x E, range V = 14.77–15.10 for interval JD 2456790–2458187. Period strongly varies.

2. We discovered the star using the CRTS archive data (SSS_J200755.7-631916). M–m = 0.44 P.

3. The star was included in the ASAS-SN Catalog of Variable Stars with a wrong P, 155^d.0.

4. The star was included in the ASAS-SN Catalog of Variable Stars without period, type L.

6. M–m = 0.22 P.

7. M–m = 0.40 P.

8. The star was included in the ASAS-SN Catalog of Variable Stars without period, type L.

9. MinII = 12.84 V. The star was included in the ASAS-SN Catalog of Variable Stars with a wrong type RRAB and P, 0^d.6071846.

10. MinII = 10.94 V. Period from the International Variable Star Index according to Watson et al. (2007) is erroneous: P = 0^d.316057.

11. MinII = 12.46 V.

12. MinII = 14.46 V. A SuperWASP variable object 1SWASP J211625.31+251755.4 (Lohr et al. 2013) is at 30" NW from the real variable star.

13. MinII = 14.17 V, MinII–MinI = 0.55 P, D = 0.02 P. Lapukhin et al. (2015) published a wrong period of 5^d.756:.

15. MinII = 11.91 V. The International Variable Star Index gives a wrong type and an erroneous P, 0^d.62690100. The coordinates point 25" SE from the real variable star.

Remarks:
While working on compiling of the Name-List No. 82 for Version 5.1 of GCVS (Samus et al. 2017), we determined or improved light elements, types, and coordinates for 9 new variable stars and 6 stars from the NSV catalogue (Kukarkin et al. 1982). The study of the variables was made using the publicly available electronic archives of CCD observations of the ASAS-3 project (Pojmanski 2002), ASAS-SN project (Shappee et al. 2014, Kochanek et al. 2017) and the Catalina Sky Survey (CRTS) photometric data (Drake et al. 2009). To find periods we applied the WinEfk software provided by Dr. V.P. Goranskij.

References:
Drake, A.J., Djorgovski, S.G., Mahabal, A., et al., 2009, Astrophys. J., 696, 870
Jayasinghe, T., Kochanek, C. S., Stanek, K. Z., et al., 2018, Mon. Not. Royal Astron. Soc., 477, No. 3, 3145
Kochanek, C. S., Shappee, B. J., Stanek, K. Z., et al., 2017, Publ. Astron. Soc. Pacific, 129, No. 980, 104502
Kukarkin, B. V., Kholopov, P. N., et al., 1982, New catalogue of suspected variable stars. Moscow: "Nauka"
Lapukhin, E.G., Veselkov, S.A., Zubareva, A.M., 2015, Perem. Zvezdy Prilozh., 15, No. 8
Lohr, M. E., Norton, A. J., Kolb, U. C., et al., 2013, Astron. Astrophys., 549, 86
Pojmanski, G., 2002, Acta Astron., 52, 397
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