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vol. 7, N 25 (2007)
Received: 10.10.2007; accepted: 22.10.2007
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1. M-m = 0.36 P. J-H = 0.135 (2MASS).
2. M-m = 0.40 P. The color index B-V = 1.379 (Tycho2) is probably wrong (the star is at the faint limit for the Tycho2 catalog). J-H = 0.251 (2MASS) is in agreement with the RRC type.
3. M-m = 0.40 P. J-H = 0.214 (2MASS).
4. M-m = 0.48 P. B-V = 0.505 (Tycho2).
5. M-m = 0.18 P. J-H = 0.239 (2MASS). There is a companion star (15.7 R) in 10" to the NW. 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.
6. According to ROTSE-I data (Wozniak et al., 2004), GSC 4181-00046 is a high-amplitude double-mode Delta Scuti star. J-H = 0.128 (2MASS). The following light elements are used to plot the phased light curves: HJD(max) = 2451407.680 + 0.0944226 x E (fundamental mode) and HJD(max) = 2451407.688 + 0.0730446 x E (first overtone mode). The period ratio P1/P0=0.7736 is typical of high-amplitude double-mode Delta Scuti stars (Petersen and Christensen-Dalsgaard, 1996). In the phased light curves, top panels are NSVS data folded with the fundamental-mode and the first overtone periods. Bottom panels are the same curves after prewhitening the other oscillation. Small dots are the NSVS data with err. > 0.05 mag. These observations were removed from the bottom curves.
I present the discovery of 6 new short-period pulsating variables. A search for variables was carried out in the publicly available data of the Northern Sky Variability Survey (NSVS, Wozniak et al., 2004, also see http://skydot.lanl.gov/nsvs). 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.
Petersen, J.O., Christensen-Dalsgaard, J., 1996, Astron. and Astrophys., 312, 463
Wozniak, P.R., Vestrand, W.T., Akerlof, C.W. et al., 2004, Astron. J., 127, 2436