HAT Variability Survey in the High Stellar Density "Kepler Field" with Millimagnitude Image Subtraction Photometry

Details HAT Variability Survey in the High Stellar Density "Kepler Field" with Millimagnitude Image Subtraction Photometry HAT Variability Survey in the High Stellar Density "Kepler Field" with Millimagnitude Image Subtraction Photometry

2004-05-29

arxiv.org/abs/astro-ph/0405597v2

Astron.J. 128 (2004) 1761

Astronomy and Astrophysics

Astrophysics

44 pages, 19 figures. Accepted for publication in the Astronomical Journal. Revised version, including updated matches to exis

Scientific paper

10.1086/423920

The Hungarian-made Automated Telescope network (HATnet) is an ongoing project to detect transiting extra-solar planets using small aperture (11 cm diameter), robotic telescopes. In this paper we present the results from using image subtraction photometry to reduce a crowded stellar field observed with one of the HATnet telescopes (HAT-5). This field was chosen to overlap with the planned Kepler mission. We obtained I-band light curves for 98,000 objects in a 8.3x8.3 square degree field of view, near the Galactic plane in the constellations Cygnus and Lyra. These observations include 788 5-minute exposures over 30 days. For the brightest stars (I~8.0) we achieved a precision of 3.5 millimagnitudes, falling to 0.1 magnitudes at the faint end (I~14). From these light curves we identify 1617 variable stars, of which 1439 are newly discovered. The fact that nearly 90% of the variables were previously undetected further demonstrates the vast number of variables yet to be discovered even among fairly bright stars in our Galaxy. We also discuss some of the most interesting cases. These include: V1171 Cyg, a triple system with the inner two stars in P=1.462 day period eclipsing orbit and the outer star a P=4.86 day Cepheid; HD227269, an eccentric eclipsing system with a P=4.86 day period that also shows P=2.907 day pulsations; WW Cyg, a well studied eclipsing binary; V482 Cyg, an RCB star; and V546 Cyg, a PV Tel Variable. We also detect a number of small amplitude variables, in some cases with full amplitude as low as 10 mmag.

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