New Elements for 34 NSV and GCVS Stars

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

Received:   17.03.2017;   accepted:   6.12.2017
(E-mail for contact: helene@inasan.ru, pastukhova@sai.msu.ru)

Comments:


1. Min II = 9.84 V, Min II–Min I = 0.61 P. The Hipparcos and Tycho Catalogues (1997) give a wrong period of 13^d.2714.

2. Variability of the star was discovered in the ASAS-3 survey. OV CMa enters their variable-star catalogue as a MISC-type star with a wrong period of 101^d.7.

4. R = 18.5 on the DSS2 image of 1986-12-09.

5. R = 15.5 on the DSS2 image of 1989-01-08.

6. NE companion of 9" pair. The ASAS range is for the combined brightness of the Mira and its neighbor.

7. Min II = 7.17 V. The Hipparcos and Tycho Catalogues (1997) give a wrong period of 6^d.1708.

8. Variability of the star was discovered in the ASAS-3 survey. V340 CMa enters their variable-star catalogue as a MISC-type star with a wrong period of 258^d.

12. POSS I (1951-07-07) B = 16.5, POSS II (1988-07-14) B = 20.0.

14. N companion of 3" pair. The NSVS range is for the combined brightness of the Mira and its neighbor. We proved our P = 188^d using the ASAS-3 data.

15. M–m = 0.44 P.

16. USNO-B1.0 magnitudes: R1 = 14.57, R2 = 17.89.

17. Min II = 13.3 V, Min II–Min I = 0.60 P.

18. HV 5465 was found, upon our request, by the late Dr. M. Hazen in Harvard Observatory's logbooks.

19. NW companion of 8" pair. The NSVS range is for the combined brightness of the Mira and its neighbor. POSS I (1951-07-07) R = 14.7.

20. We proved our P = 430^d using the NSVS data. POSS I (1953-08-13) R = 15.5.

21. Variability of the star was discovered in the ASAS-3 survey. NSV 12403 enters their variable-star catalogue as a MISC-type star with a wrong period of 85^d.3.

23. Superposed variations of 36^d.07. Variability of the star was discovered in the ASAS-3 survey. NSV 12471 enters their variable-star catalogue as a MISC-type star with a wrong period of 282^d.6.

24. Variability of the star was discovered in the ASAS-3 survey. NSV 12478 their variable-star catalogue as a MISC-type star with a wrong period of 149^d.8.

25. Min II = 14.18 CV. Probably misprint coordinates for this variable by Luyten (1937a): it should read 19^h 46^m.5 –23° 23' (1900) instead of 19^h 46^m.5 –23° 33' (1900).

26. P1 = 0^d.407886, P0 = 0^d.546995, P1/P0 = 0.7457. The variability was suspected by Luyten (1937b), recovered by us.

27. POSS I (1953-08-13) R = 16.2.

28. We proved our P = 227^d using the ASAS-3 data.

29. Period is strongly variable.

32. Min I is possible Min II.

33. M–m = 0.13P. The ASAS-3 data confirm P = 0^d.484400.

34. Min II = 7.35 V. Variability of the star was discovered in the Hipparcos and Tycho Catalogues (1997) with a wrong period of 0^d.8277234.

Remarks:
In the process of improving coordinates and data for variable stars in the new electronic version of NSV catalogue (Kholopov 1982) and our work on Version 5.1 of GCVS (Samus et al. 2017), we determined light elements and types of variability for 22 suspected and 12 GSVS variables. The study of the variables was made using the publicly available electronic archives of CCD observations of the ASAS-3 project (Pojmanski 2002), the Catalina Sky Survey photometric data (Drake et al. 2009) and the Northern Sky Variability Survey (NSVS) data (Woźniak et al. 2004). We measured minimal brightness for many Mira variables using Digitized Sky Survey images (R–band) of the STScI Archive.

References:
Drake, A.J., Djorgovski, S.G., Mahabal, A., et al., 2009, Astrophys. J., 696, 870
The Hipparcos and Tycho Catalogues (European Space Agency, 1997), ESA SP-1200
Kholopov, P.N. (editor), 1982, New Catalogue of Suspected Variable Stars, Moscow: Nauka
Luyten, W.J., 1937a, Astron. Nachr., 261, 451
Luyten, W.J., 1937b, Astron. Nachr., 264, 63
Pojmanski, G., 2002, Acta Astron., 52, 397
Samus, N.N., Kazarovets, E.V., Durlevich, O.V., Kireeva, N.N., Pastukhova, E.N., 2017, General Catalogue of Variable Stars: Version GCVS 5.1, Astronomy Reports, 61, No. 1, pp. 80–88
Woźniak, P. R., Vestrand, W. T., Akerlof, C. W., et al., 2004, Astron. J., 127, 2436