========================================================================== J/A+A/510/A21 CoRot and Kepler Stellar Limb-Darkening Coefficients (Sing, 2010) The following files can be converted to FITS (extension .fit or fit.gz) table1.dat table2.dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/A+A/510/A21 ==========================================================================
drwxr-xr-x 20 cats archive 4096 Jan 29 2012 [Up] drwxr-xr-x 2 cats archive 4096 Dec 15 2013 [TAR file] -rw-r--r-- 1 cats archive 477 Apr 23 2010 .message -r--r--r-- 1 cats archive 5283 Apr 23 2010 ReadMe -r--r--r-- 1 cats archive 229266 Jan 7 2010 table1.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 229594 Jan 7 2010 table2.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe : J/A+A/510/A21 Stellar Limb-Darkening Coefficients (Sing, 2010) ================================================================================ Stellar limb-darkening coefficients for CoRot and Kepler. Sing D.K. <Astron. Astrophys. 510, A21 (2010)> =2010A&A...510A..21S ================================================================================ ADC_Keywords: Models, atmosphere ; Binaries, eclipsing ; Planets Keywords: stars: atmospheres - planetary systems - binaries: eclipsing Abstract: Transiting exoplanets provide unparalleled access to the fundamental parameters of both extrasolar planets and their host stars. We present limb-darkening coefficients (LDCs) for the exoplanet hunting CoRot and Kepler missions. The LDCs are calculated with ATLAS stellar atmospheric model grids and span a wide range of T_eff_, logg, and metallically [M/H]. Both CoRot and Kepler use wide nonstandard photometric filters, and are producing a large inventory of high- quality transiting lightcurves, sensitive to stellar limb darkening. Comparing the stellar model limb darkening to results from the first seven CoRot planets, we find better fits are found when two model intensities at the limb are excluded in the coefficient calculations. This calculation method can help to avoid a major deficiency present at the limbs of the 1D stellar models. Description: These are calculations of limb-darkening coefficients used to describe the intensity profiles of stars for the CoRot and Kepler exoplanet missions. The full version of the tables can be also be found at http://vega.lpl.arizona.edu/~singd/ which also includes an IDL program to read and interpolate the tables.