New Light Elements and Types for 29 NSV Stars

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

Received:   21.05.2007;   accepted:   28.05.2007
(E-mail for contact: elena_k@sai.msu.ru, pastukhova@sai.msu.ru)

Comments:


1. Reported as a confirmed variable in Greaves (2006a).

2. Reported as a confirmed variable in Greaves (2006a).

3. M-m = 0.25. Classified as a DCEP/EC star in the ASAS-3 catalogue, with a spurious period, P = 0.85095d.

4. The ASAS-3 range is for the combined brightness of the variable and its neighbor, which has B = 14.7. Reported as a confirmed variable in Greaves (2006a).

5. MinII = 14.5:.

6. M-m = 0.25.

7. MinII = 14.4. The star was found by M. Hazen on Harvard plates.

8. MinII = 12.92.

9. The star was studied by Koen and Eyer (2002) on the base of Hipparcos photometry, they found a period close to 5 days. The light curve for Hipparcos photometry is not good for any of the suggested periods, the ASAS-3 data gives a much better light curve with the period given in the table.

11. D = 0.10:. Due to the period being close to an integer number of days, the phase coverage is poor. A twice longer or a twice shorter period is possible; a secondary minimum of any depth might be present.

14. M-m = 0.2.

15. The ASAS-3 range is for the combined brightness of the Mira and its neighbor, which has B = 14.0.

18. M-m = 0.38.

21. D = 0.20:. A blend of several stars influences ASAS-3 photometry, the identification of the particular variable component is based on sky survey images. The period can also be twice longer.

22. M-m = 0.30:. A one-day alias, P = 0.41454d, is also possible.

23. M-m = 0.17.

25. M-m = 0.09.

28. Type MISC in the ASAS-3 catalogue, with a period of 222d (apparently wrong). Also reported as a confirmed variable in Greaves (2006a).

29. Reported as a confirmed variable in Greaves (2006b).

Remarks:
In our work on the improvement of the coordinates for all stars in the NSV catalogue, we succeeded in studying 29 variable stars. We could study the variables thanks to the publicly available electronic archives of CCD observations of the ASAS-3 (Pojmanski, 2002) and ROTSE1/NSVS (Wozniak et al., 2004) surveys. We recovered the variables NSV5922, NSV6118, NSV6256, NSV6360 suspected by Luyten (1935), NSV6132, NSV6240, NSV6241 suspected by Luyten (1934), NSV6159, NSV6221, NSV6222, NSV6334 suspected by Luyten (1933), NSV6227 suspected by Balanovsky (1918), NSV6234, NSV6294, NSV6318, NSV6338 and NSV6344 suspected by Shapley (1954). The candidates were found using the US Naval Observatory Image Archive (http://www.nofs.navy.mil/data/fchpix/). Our studies are supported by grants from the Russian Foundation for Basic Research (grant No. 05-02-16289), from the Program "Origin and Evolution of Stars and Galaxies" of the Presidium of Russian Academy of Science, and from the Program of Support for Leading Scientific Schools of Russia (grant No. NSh 5290.2006.2).

References:
Balanovsky, J., 1918, AN, 208, 33
Greaves, J., 2006a, OEJV, 33, 1
Greaves, J., 2006b, OEJV, 36, 1
Koen, C., Eyer, L., 2002, MNRAS, 331, 45
Luyten, W.J., 1933, AN 249, 395
Luyten, W.J., 1934, AN 253, 135
Luyten, W.J., 1935, AN 256, 325
Pojmanski, G., 2002, Acta Astronomica, 52, 397
Shapley, H., Allen, L.B., Greenstein, N., 1954, Astron.J, 59, 270
Wozniak, P.R., Vestrand, W.T., Akerlof, C.W. et al., 2004, Astron.J., 127, 2436