========================================================================== J/AJ/128/1761 HATNET variability survey (Hartman+, 2004) The following files can be converted to FITS (extension .fit .fgz or .fiZ) table1.dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/AJ/128/1761 ==========================================================================
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Beginning of ReadMe : J/AJ/128/1761 HATNET variability survey (Hartman+, 2004) ================================================================================ HATNET variability survey in the high stellar density "Kepler field" with millimagnitude image subtraction photometry. Hartman J.D., Bakos G., Stanek K.Z., Noyes R.W. <Astron. J., 128, 1761-1783 (2004)> =2004AJ....128.1761H ================================================================================ ADC_Keywords: Binaries, eclipsing ; Stars, variable ; Photometry, Cousins ; Photometry, infrared Keywords: binaries: eclipsing - catalogs - Cepheids - delta Scuti - stars: variables: other - techniques: photometric Abstract: The Hungarian-made Automated Telescope Network (HATnet) is an ongoing project to detect transiting extrasolar planets using small-aperture (11cm 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 67 square degree field of view centered at J2000 (alpha,delta)=(19h44m00.0s, +37deg32'00.0"), near the Galactic plane in the constellations Cygnus and Lyra. These observations include 788 exposures of 5' length over 30-days. For the brightest stars (I 8.0) we achieved a precision of 3.5mmag, falling to 0.1mag at the faint end (I 14). From these light curves we identify 1617 variable stars, of which 1439 are newly discovered. Description: The data were obtained in 2003 June and July using the HAT-5 telescope located at the Fred Lawrence Whipple Observatory (FLWO).
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