| Article in PDF |
"Peremennye Zvezdy", Prilozhenie, vol. 8, N 26 (2008) |
| #1. Astrotel Observatory, Karachay-Cherkessia, Russia;
#2. Surgut, Russia; #3. Tula, Russia. |
| ISSN 2221–0474 |
Received: 28.05.2008; accepted: 26.06.2008
(E-mail for contact: bredfild@mail.ru, sav@surgut.ru, bs25@mail.ru, khruslov@bk.ru)
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Comments:
1. From NSVS data (Wozniak et al., 2004), one of the authors (A. Khruslov) detected RR Lyrae-type variability of NSVS 525525, but the ROTSE-I angular resolution was insufficient to determine which of the two stars, GSC 4329-01772 or GSC 4329-01832, varied. We were able to solve this problem from our CCD observations. Blazhko effect. Four observed maxima: HJD 2454460.5698, 2454497.2770, 2454499.3176, 2454533.3152.
2. Discovered by Khruslov (2006). Four observed primary minima: HJD 2454460.4769, 2454506.3610, 2454510.3807, 2454533.3238. MinII = 13.37.
3. Discovered by Khruslov (2006). Four observed primary minima: 2454460.6114, 2454502.2318, 2454507.2884, 2454533.3498. MinII = 14.27.
4. Unknown type, possibly a Cepheid.
5. We observed one primary minimum, HJD 2454460.4247. MinII = 15.34.
6. We observed five primary minima, HJD 2454497.2280, 2454499.2192, 2454506.3782, 2454510.3548, 2454524.2739. MinII = 16.13.
7. We observed four primary minima, HJD 2454502.1929, 2454507.3100, 2454509.3562, 2454510.3763. MinII = 16.10.
8. We observed two primary minima, HJD 2454460.4309, 2454499.1830. MinII = 15.03.
9. We observed five primary minima, HJD 2454497.2937, 2454499.3856, 2454504.2529, 2454506.3435, 2454507.3925. MinII = 16.48.Remarks:
During observations of the variable object NSVS 525525, a close pair of the stars GSC 4329-01772 and GSC 4329-01832 (37" angular separation), we determined which star was variable, discovered six new variable stars, and observed two variable stars discovered earlier. Our observations were carried out in Astrotel-Caucasus observatory using the 300-mm Ritchey-Chretien telescope, equipped with an unfiltered SBIG STL-11000 CCD camera. In total, we obtained 520 5-minute images on JD 2454460-54537. We used the MaxIm DL software for basic reductions for dark current, flat fields, and bias. For search for new variable stars, we applied VaST software by Sokolovsky and Lebedev (2005), and for photometry, CCD Soft V.5 (http://www.bisque.com/Products/CCDSoft/). The comparison star was GSC 4329-02360 (USNO-B1 1585-0074036; 04:29:26.47, +68:33:49.4 (J2000), R1 = 13.96, R2 = 14.26) assuming Rcomp = 14.11. The check star was GSC 4329-02690.References:
Khruslov, A.V., 2006, PZP, 6, No. 11
Sokolovsky, K., Lebedev, A., 2005, in 12th Young Scientists' Conference on Astronomy and Space Physics, Kyiv, Ukraine, April 19-23, 2005, eds.: Simon, A.; Golovin, A., p.79
Wozniak, P.R., Vestrand, W.T., Akerlof, C.W. et al., 2004, Astron. J., 127, 2436
