Recovery of Harvard Variables: Light Elements for 41 Mira Type Stars

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

Received:   26.11.2015;   accepted:   15.04.2016
(E-mail for contact: helene@inasan.ru, pastukhova@sai.msu.ru)

Comments:


2. Variability of the star was discovered in the ASAS-3 survey. It enters their variable-star catalog as a MISC-type star with a wrong period of 210^d.3. The ASAS-3 range is for the combined brightness of the Mira and its neighbor.

4. The ASAS-3 range is for the combined brightness of the Mira and its neighbor. HV 9231 was found, upon our request, by D. Williams on Harvard plates.

5. The ASAS-3 range is for the combined brightness of the Mira and its neighbor.

6. Variability of the star was discovered in the ASAS-3 survey. It enters their variable-star catalog as a MISC-type star with a wrong period of 150^d.6.

8. The ASAS-3 range is for the combined brightness of the Mira and its neighbor.

10. Variability of the star was discovered in the ASAS-3 survey. It enters their variable-star catalog as a Mira-type star with a wrong period of 354^d.2.

13. The ASAS-3 range is for the combined brightness of the Mira and its neighbor.

15. We have found only one maximum of the star in ASAS-3, on HJD 2452760:. Provisionally, we suggest P = 480:^d.

21. Note from the editors: the star's light elements were independently determined in the AAVSO Variable Star Index (VSX), but, as of April 15, 2016, the AAVSO coordinates were wrong by 3' in declination.

22. Note from the editors: S.A. Otero solved the star independently on March 25, 2016 (see VSX).

23. Sitek & Pojmanski (2014) solved the star independently using I-band observations. Our V-band light curve based on ASAS-3 data covers a larger number of maxima.

26. The ASAS-3 range is for the combined brightness of the Mira and its neighbor.

28. The Mira type, with a wrong period (157^d.8), was announced for this variable in the VSX (March 23, 2012) by S.A. Otero.

29. The ASAS-3 range is for the combined brightness of the Mira and its neighbor.

39. The star was discovered by Woźniak et al. (2004b). The VSX mentions it as an SRA variable with the period of 129^d.

Remarks:
In the process of improving coordinates of variable stars in the NSV catalog (Samus et al. 2007–2015), we determined light elements for 41 Mira type stars. We recovered the following variables suspected by W.J. Luyten: HV 9298 (Luyten 1933a); HV 9203, 9204, 9220, 9244, 9256, 9257, 9260, 9285, 9288, 9336, 9351, 9362, 9369, 9390 (Luyten 1933b); HV 9540 (Luyten 1935); HV 9228, 9247, 9252, 9259, 9276, 9279, 9357, 9446 (Luyten 1936); HV 9306, 9365 (Luyten 1937a); HV 9286, 9304, 9353, 9368, 9386, 9391 (Luyten 1937b). Finding charts for these variables have never been published before. We measured minimal brightness for many Mira variables using Digitized Sky Survey images (R-band). The study of the variables was made using the publicly available electronic archives of CCD observations of the ASAS-3 project (Pojmanski 2002) and images of the STScI and US Naval Observatory Image and Catalog Archive. We studied the variability of NSV 10306 in the Northern Sky Variability Survey (NSVS) data (Woźniak et al. 2004a).

Acknowledgments: Our studies are supported by a grant from the Program "Transition and explosive processes in the Universe" of the Presidium of Russian Academy of Sciences.

References:
Luyten, W.J., 1933a, Astron. Nachr., 249, 395
Luyten, W.J., 1933b, Astron. Nachr., 250, 259
Luyten, W.J., 1935, Astron. Nachr., 256, 325
Luyten, W.J., 1936, Astron. Nachr., 258, 121
Luyten, W.J., 1937a, Astron. Nachr., 263, 181
Luyten, W.J., 1937b, Astron. Nachr., 264, 63
Pojmanski, G., 2002, Acta Astron., 52, 397
Samus, N.N., Durlevich, O.V., Goranskij, V.P., Kazarovets, E V., Kireeva, N.N., Pastukhova, E.N., Zharova, A.V., 2007–2015, General Catalogue of Variable Stars, Centre de Données Astronomiques de Strasbourg, B/gcvs
Sitek, M., Pojmanski G., 2014, Acta Astron., 64, 115
Woźniak, P. R., Vestrand, W. T., Akerlof, C. W., et al., 2004a, Astron. J., 127, 2436
Woźniak, P.R., Williams, S.J., Vestrand, W.T. et al., 2004b, Astron. J., 128, 2965