Article in PDF |
"Peremennye Zvezdy", Prilozhenie, vol. 17, N 4 (2017) |
#1. Sternberg Astronomical Institute, Lomonosov Moscow State University, Moscow, Russia;
#2. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia. |
ISSN 2221–0474 |
Received: 21.02.2014; accepted: 26.12.2017
(E-mail for contact: khruslov@bk.ru)
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Comments:
1. The twice longer period is not excluded. A bright close companion, variable CSS_J085842.7+173936 (type RRC, Drake et al. 2014), is in 12''.
2. J–K = 0.496 (2MASS). From 1SWASP data, 14m.35 – 14m.6; from ROTSE-I/NSVS data, 14m.2 – 14m.6 in the R band. According to NSVS data, the light elements are: JD(max) = 2451504.2 + 13d.2×E. Combined brightness of three stars, GSC 2986-00338 and fainter ones, USNO-A2.0 1275-07437120 and USNO-A2.0 1275-07437162, was measured in the NSVS and 1SWASP, the tabulated amplitudes are considerably underestimated. The ROTSE data with photometric correction flags were kept for the analysis.
3. MinII = 11.76 (WASP). From CSS data, 11m.6 – 11m.85 (CV); from ROTSE-I/NSVS data, 11m.74 – 11m.93, MinII = 11m.91 in the R band.
4. X-ray sources 1WGA J0907.4+4228, 1RXP J090728+4227.8 and 2RXP J090729.3+422723. From 1SWASP data, 12m.05 – 12m.15. According to 1SWASP data, the light elements are: JD(min) = 2454535. + 25d.8×E. The light curve shape and period vary. J–K = 0.616 (2MASS).
5. X-ray sources 1WGA J0908.7+4229, 1RXP J090847+4229.1 and 2RXP J090847.8+422904. From ROTSE-I/NSVS data, 10m.75 – 10m.87 in the R band. B–V = 0.718 (Tycho2), J–K = 0.411 (2MASS). A star with a considerable proper motion (in the Tycho-2 catalog, pmRA(mas/yr) = –65.8; pmDE(mas/yr) = –37.6 ).
6. From 1SWASP data, 12m.73 – 12m.83, MinII = 12.82; from ROTSE-I/NSVS data, 12m.9 – 13m.0 in the R band. Combined brightness of two stars, GSC 3424-01547 and GSC 3424-00988, was measured in NSVS and 1SWASP, the tabulated amplitudes are possibly slightly underestimated. According to CSS data GSC 3424-00988 is constant star and GSC 3424-01547 is the variable star. Because of the large uncertainties the CSS data were rejected.
7. From ROTSE-I/NSVS data, 12m.35 – 12m.45 in the R band. According to NSVS data, the light elements are: JD(max) = 2451453.65 + 3d.427×E. J–K = 0.401 (2MASS). The star has a faint close companion USNO-B1.0 1304-0198089.
8. MinII = 12m.48 (WASP). From ROTSE-I/NSVS data, 12m.35 – 12m.6, MinII = 12m.45 in the R band.
9. From ROTSE-I/NSVS data, 10m.5 – 10m.7 in the R band. The ROTSE data with photometric correction flags were kept for the analysis. Probably can be identified with IRAS F09148+5120. B–V = 1.887 (Tycho2), J–K = 1.163 (2MASS). Type SR is also not excluded.
10. MinII = 11.94 (WASP). From ROTSE-I/NSVS data, 12m.29 – 12m.43, MinII = 12m.38 in the R band. The ROTSE data with photometric correction flags were kept for the analysis.
11. X-ray sources 1WGA J0935.4+4938, 1RXP J093525+4938.5, 2RXP J093525.3+493830 and 1RXS J093521.9+493822. D = 0.14 P. From 1SWASP data, 12m.2 – 12m.45. B–V = 0.328 (Tycho2), J–K = 0.554 (2MASS). According to WASP data, shape of the light curve and the depth of minima are possibly subject to changes.
12. X-ray sources 1WGA J0942.0+4722, 1RXP J094206+4722.2, 2RXP J094205.6+472203. B–V = 1.255 (Tycho2), J–K = 0.731 (2MASS).
13. MinII = 14m.10 (CV). From ROTSE-I/NSVS data, 14m.0 – 14m.3 in the R band. Combined brightness of two stars, GSC 2999-01120 (=var) and USNO-A2.0 1275-07588822, was measured in the NSVS, the tabulated amplitudes are possibly slightly underestimated.
14. From 1SWASP data, 13m.9 – 14m.1; from ROTSE-I/NSVS data, 13m.6 – 13m.85 in the R band. According to NSVS data, the light elements are: JD(max) = 2451507.3 + 19d.2×E; double wave in NSVS. J–K = 0.718 (2MASS).
15. From 1SWASP data, 11m.55 – 11m.7. B–V = 1.652 (Tycho2), J–K = 0.984 (2MASS).
16. From ROTSE-I/NSVS data, 13m.6 – 13m.95 in the R band. P = 1.1858 days is not excluded. J–K = 0.700 (2MASS).
17. MinII = 13m.76 (CV). From ROTSE-I/NSVS data, 13m.7 – 13m.9 in the R band. The star has a faint close companion USNO-B1.0 1409-0212238.
18. D = 0.07 P. From ROTSE-I/NSVS data, 12m.1 – 12m.6 in the R band.
19. D = 0.08 P. From ROTSE-I/NSVS data, 12m.2 – 12m.55 in the R band. The light elements of the distortion wave: JD(max) = 2451451.6 + 3d.697×E. The ROTSE data with photometric correction flags were kept for the analysis.
20. From 1SWASP data, 12m.56 – 12m.64. According to 1SWASP data, the light elements are: JD(max) = 2454150.570 + 0d.27185×E. J–K = 0.618 (2MASS).
21. The ROTSE data with photometric correction flags were kept for the analysis. The star's mean brightness variations were subtracted in the 1SWASP light curve. The star was independently discovered by Ivan Sergey.
22. MinII = 13m.66 (CV). From ROTSE-I/NSVS data, 13m.5 – 13m.9 in the R band. In CSS data mean brightness varies. The star was independently discovered by Ivan Sergey, Sergei Dubrovski, and Astrobloknot Team.
23. MinII = 12m.84 (WASP). From ROTSE-I/NSVS data, 12m.7 – 12m.85 in the R band.
24. MinII = 14m.25 (WASP). From ROTSE-I/NSVS data, 13m.4 – 14m.0 in the R band. The ROTSE data with photometric correction flags were kept for the analysis.
25. MinII = 15.52 (CV); D = 0.11 P. A close companion, variable CSS_J215508.0+134117 (type RRC, Drake et al. 2014), is in 12'' from the star.Remarks:
I present a discovery of 25 new variable stars. My search for variables was carried out in the publicly available data of the Northern Sky Variability Survey (NSVS, Woźniak et al. 2004). Besides, to improve classification and light elements, I analyzed all available observations of these stars from the Catalina Surveys (Drake et al. 2009) and SuperWASP (Butters et al. 2010). The sky area with RA between 08h 45m and 10h 20m, Dec between +40° and +52° was searched. Three stars (No. 1, 24, 25) are not in the mentioned field. I discovered the variability of No. 1 and No. 25 while investigating stars of RRC type from Catalina Surveys catalog (Drake et al. 2014).
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 from the 2MASS catalogs.
The SuperWASP observations are available as FITS tables, which were converted into ASCII tables using the OMC2ASCII program as described by Sokolovsky (2007).
Acknowledgements: Thanks are due to Dr. K.V. Sokolovsky for his advice concerning data retrieving. The author wishes to thank Dr. V.P. Goranskij for providing his software. This study was supported by the Program "Non-stationary Phenomena of Objects in the Universe" of the Presidium of Russian Academy of Sciences.References:
Butters, O.W., West, R.G., Anderson, D.R., et al., 2010, Astron. and Astrophys., 520, L10
Drake, A.J., Djorgovski, S.G., Mahabal, A., et al., 2009, Astrophys. J., 696, 870
Drake, A.J., Graham, M.J., Djorgovski, S.G., et al., 2014, Astrophys. J. Suppl., 213, 9
Sokolovsky, K.V., 2007, Perem. Zvezdy Prilozh., 7, No. 30
Woźniak, P.R., Vestrand, W.T., Akerlof, C.W., et al., 2004, Astron. J., 127, 2436