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Peremennye Zvezdy (Variable Stars) 33, No. 1, 2013 Received 23 January; accepted 6 February.
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Article in PDF |
GSC 1374-01131, a High-Amplitude Delta Scuti Star with an Eclipsing Component
A. V. Khruslov
- Institute of Astronomy, Russian Academy of Sciences,
Pyatnitskaya Str. 48, 119017 Moscow, Russia;
e-mail: khruslov@bk.ru
| I present the discovery of an eclipsing component in light variations of the known High-Amplitude Delta Scuti star GSC 1374-01131 based on the Catalina Surveys publicly available data. |
1. Introduction
The variability of GSC 1374-01131 = VSX J074722.4+220414
(
,
,
J2000, UCAC4) was reported in 2011 by S. Roland, N. Martinez, and
S. Bruzzone in the AAVSO Variable Star Index (VSX;
www.aavso.org/vsx/). From a single night of their observations,
the variable was classified as a HADS (High-Amplitude Delta Scuti)
star, with the light elements:
I reinvestigated the star using the currently available Catalina Surveys data (Drake et al. 2009; CSS J074722.5+220413). The observations I used are available online in the html version of this paper.
2. Results
According to my study, the variable is a HADS star with an eclipsing component (EA or EB type). The light elements of the pulsating and eclipsing components of the light variations are the following:
and
The light curves of GSC 1374-01131 are displayed in Fig. 1.
 |
Fig. 1. The light curves of GSC 1374-01131 based on Catalina data, folded with periods of pulsations and eclipses. Upper panels: raw data; lower panels: the folded light curves with the other variation pre-whitened. |
Brightness measurements of GSC 1374-01131 are also available in
other electronic archives, but they are not usable for several
reasons. The NSVS (Wozniak et al. 2004) and SuperWASP (Butters
et al. 2010) surveys contain photometry for the combined
brightness of the variable and its two brighter neighbors (TYC
1374 1314 1, 
and TYC 1374 1358 1, 
; Fig. 2).
Nevertheless, a weak short-period signal can be detected in the
1SWASP data, but large photometric errors make its analysis
impossible. In the ASAS-3 (Pojmanski 2002) data, the brightness
measurements do refer to GSC 1374-01131, but uncertainties and
data scattering are also very large.
3. Discussion
Eclipsing 
Scuti stars, EA+DSCTC, are well known. For
these stars, pulsation amplitudes are low (within 0
1) and
eclipse amplitudes are large. The only case of an EA+HADS (EA+DSCT
in the GCVS designations of variability types) contained in the
AAVSO Variable Star Index is V1264 Cen. The total amplitude of its
pulsation component is as large as 02, the eclipse amplitude
being 175 (GCVS, Samus et al. 2007-2012). In the case of
GSC 1374-01131, the pulsation and eclipsing variability
components have comparable amplitudes. The observed eclipse is
probably partial.
Acknowledgments: The author is grateful to Dr. V.P. Goranskij for providing software for the light-curve analysis. Thanks are due to Drs. S.V. Antipin and N.N. Samus for helpful discussions. This study was supported by the Russian Foundation for Basic Research through grant No. 11-02-00495.
References:
Butters, O.W., West, R.G., Anderson, D.R., et al., 2010, Astron. Astrophys., 520, L10
Drake, A.J., Djorgovski, S.G., Mahabal, A., et al., 2009, Astrophys. J., 696, 870
Pojmanski, G., 2002, Acta Astronomica, 52, 397
Samus, N.N., Durlevich, O.V., Kazarovets, E V., et al., 2007-2012, General Catalogue of Variable Stars, Centre de Donnees Astronomiques de Strasbourg, B/gcvs
Wozniak, P.R., Vestrand, W.T., Akerlof, C.W. et al., 2004, Astron. J., 127, 2436