Article in PDF |
"Peremennye Zvezdy", Prilozhenie, vol. 12, N 4 (2012) |
ISSN 2221–0474 |
Received: 27.11.2011; accepted: 23.03.2012
(E-mail for contact: khruslov@bk.ru)
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Comments:
1. IRAS 23589+6406. J–H = 1.201 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
2. J–H = 1.120 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
3. IRAS Z00110+6800. J–H = 1.431 (2MASS). CGCS 22 (Alksnis et al. 2001). Type SR with the period 130 d is not excluded. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
4. IRAS Z00256+6758. J–H = 1.135 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
5. IRAS 00274+6930. J–H = 1.251 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
6. IRAS Z00351+6716. J–H = 1.164 (2MASS). Faint close companion USNO-B1.0 1575-0014023. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
7. IRAS 00363+6759. J–H = 1.171 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
8. IRAS Z00447+6704. J–H = 1.252 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
9. IRAS 00466+7106. J–H = 1.045 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
10. IRAS Z00477+7123. J–H = 1.137 (2MASS). CGCS 122 (Alksnis et al. 2001). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
11. IRAS Z00522+6944. J–H = 1.111 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
12. IRAS 00551+6812. J–H = 1.016 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
13. IRAS 00568+6721. J–H = 1.350 (2MASS). CGCS 152 (Alksnis et al. 2001). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
14. IRAS 00578+6647. J–H = 1.154 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
15. IRAS Z03525+5506. J–H = 1.097 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
16. IRAS 04119+4911. B–V = 2.606 (Tycho2), J–H = 0.828 (2MASS).
17. IRAS 04136+5035. J–H = 1.316 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis. Three red images from the Digitized Sky Survey show that the variability amplitude is considerable:
1954-10-05: R = 18.6;
1988-11-05: R = 14.1;
1993-10-20: R = 19.0.
Delta mag = 4.7 mag, indicating that the variable is a Mira star (the comparison star magnitudes were taken from the USNO-B1.0 catalog).
18. Probably can be identified with IRAS 04182+5010. J–H = 1.264 (2MASS). Type SR is not excluded. Faint close companion 2MASS 04220533+5017418.
19. Probably can be identified with IRAS 04187+5058. J–H = 1.167 (2MASS).
20. IRAS 04208+4922. J–H = 1.231 (2MASS).
21. J–H = 1.171 (2MASS).
22. IRAS Z04222+5021. J–H = 1.309 (2MASS). Type SR with the period of 71 d is not excluded.
23. IRAS 04240+4724. J–H = 1.547 (2MASS). CGCS 688 (Alksnis et al. 2001). Type SR with the period of 160 d is not excluded.
24. IRAS Z04274+4656 . J–H = 1.475 (2MASS). Close companion USNO-B1.0 1370-0121185, the NSVS amplitude is slightly underestimated. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
25. Probably can be identified with IRAS F04298+6653. J–H = 0.955 (2MASS).
26. IRAS 04346+4646. J–H = 1.347 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
27. J–H = 0.901 (2MASS).
28. IRAS Z04444+4440. J–H = 1.072 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
29. J–H = 0.838 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
30. Probably can be identified with IRAS Z04481+4418. J–H = 1.026 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
31. IRAS F05038+7245. J–H = 0.909 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
32. J–H = 1.078 (2MASS). Period 70 d and type SR are possible.
33. IRAS 05275+3650. J–H = 1.211 (2MASS).
34. IRAS 05280+3208. J–H = 1.252 (2MASS). Type SR with the period of 100 d is not excluded.
35. IRAS F05291+7059. J–H = 0.944 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
36. IRAS Z05404+3840. J–H = 1.001 (2MASS).
37. IRAS 05415+3838. J–H = 1.069 (2MASS).
38. IRAS 05417+3821. J–H = 1.000 (2MASS).
39. IRAS Z05446+3807. J–H = 1.192 (2MASS). CGCS 1055 (Alksnis et al. 2001). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
40. IRAS 06001+3814. J–H = 0.980 (2MASS), B–V = 1.455 (Tycho2). Type SR is not excluded. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
41. J–H = 0.950 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
42. Probably can be identified with IRAS Z06052+6856. J–H = 0.924 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
43. IRAS F06222+7259. J–H = 0.880 (2MASS). Type SR is not excluded. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
44. IRAS 13482+4755. B–V = 1.650 (Tycho2), J–H = 0.839 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
45. BD+25 2788, IRAS 14288+2452. B–V = 1.812 (Tycho2), J–H = 0.843 (2MASS). According to ASAS-3 data, the most probable period is 40.8 d; other possible periods are 36.7 and 29.2 days. According to ROTSE-I/NSVS data, the most probable period is 45.6 d, a 39.3-day period is also possible. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
46. IRAS Z14365-7019. J–H = 1.030 (2MASS).
47. IRAS 15401+4456. B–V = 1.360 (Tycho2), J–H = 0.863 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
48. IRAS F17348+6831. J–H = 0.887 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
49. IRAS 17500+7230. B–V = 1.631 (Tycho2), J–H = 0.849 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
50. IRAS F18141+3009. B–V = 2.226 (Tycho2), J–H = 0.874(2MASS). Type SR is not excluded. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
51. B–V = 0.855 (Tycho2), J–H = 0.590 (2MASS). Faint close companion GSC 2740-01090, J–H = 0.245 (2MASS), the NSVS amplitude is slightly underestimated. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
52. IRAS 23536+7043. J–H = 1.003 (2MASS). Type SR is not excluded. Faint close companion GSC 4483-01506 the NSVS amplitude is slightly underestimated. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
53. IRAS 23551+6844. J–H = 1.674 (2MASS). The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.Remarks:
I present the discovery of 53 new semiregular (SR, SRB, SRD) and irregular (LB) pulsating variable stars. A search for variables was carried out in the publicly available data of the Northern Sky Variability Survey (NSVS; Wozniak et al. 2004) and The All Sky Automated Survey (ASAS-3; Pojmanski 2002). These observations were analyzed using the period-search software developed by Dr. V.P. Goranskij for Windows environment. The coordinates were drawn either from the Tycho-2 or 2MASS catalogs.
In several cases, the ROTSE data with photometric correction flags (usually rejected) were kept for the analysis. The use of these data considerably increases the number of available observations without deteriorating quality and allows us to determine the period more accurately.
The sources of spectral types in the Table are: Abramyan and Gigoyan (1995), Alksnis et al. (2001), Lee et al. (1947), Mickaelian and Gigoyan (2000), Stephenson (1986).References:
Abramyan, G.V., Gigoyan, K.S., 1995, Astrophysics, 38, 115
Alksnis, A., Balklavs, A., Dzervitis, U., et al., 2001, Baltic Astronomy, 10, 1
Lee, O.J., Baldwin, R.J., Hamlin, D.W., 1947, Ann. Dearborn Obs., part No 1, 5
Mickaelian, A.M., Gigoyan, K.S, 2000, Astrophysics, 43, 55
Pojmanski, G., 2002, Acta Astronomica, 52, 397
Stephenson, C.B., 1986, Astrophys. J., 301, 927
Wozniak, P.R., Vestrand, W.T., Akerlof, C.W., et al., 2004, Astron. J., 127, 2436