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J/ApJ/788/L9     Stellar parameters of KIC planet-host stars    (Bastien+, 2014)

Larger planet radii inferred from stellar "flicker" brightness variations of bright planet-host stars. Bastien F.A., Stassun K.G., Pepper J. <Astrophys. J., 788, L9 (2014)> =2014ApJ...788L...9B (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Effective temperatures ; Photometry Keywords: planets and satellites: fundamental parameters - stars: fundamental parameters - techniques: photometric Abstract: Most extrasolar planets have been detected by their influence on their parent star, typically either gravitationally (the Doppler method) or by the small dip in brightness as the planet blocks a portion of the star (the transit method). Therefore, the accuracy with which we know the masses and radii of extrasolar planets depends directly on how well we know those of the stars, the latter usually determined from the measured stellar surface gravity, log g. Recent work has demonstrated that the short-timescale brightness variations ("flicker") of stars can be used to measure log g to a high accuracy of ∼0.1-0.2 dex. Here, we use flicker measurements of 289 bright (Kepmag<13) candidate planet-hosting stars with Teff=4500-6650 K to re-assess the stellar parameters and determine the resulting impact on derived planet properties. This re-assessment reveals that for the brightest planet-host stars, Malmquist bias contaminates the stellar sample with evolved stars: nearly 50% of the bright planet-host stars are subgiants. As a result, the stellar radii, and hence the radii of the planets orbiting these stars, are on average 20%-30% larger than previous measurements had suggested. Description: We draw our bright KOI sample from the NASA Exoplanet Archive (NEA; Akeson et al. 2013PASP..125..989A) accessed on 2014 January 7. We restrict the sample to stars with 6650 K>Teff>4500 K, the Teff range for which F8 is calibrated. We exclude 28 stars with overall range of photometric variability >10 ppt (parts per thousand), as phenomena in the light curves of such chromospherically active stars can boost the measured F8 and thus result in an erroneous F8-based log g. These excluded stars (10% of the sample) are cooler than average for the overall sample, as expected given their large variability. Our sample after applying these cuts contains 289 stars (407 KOIs). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 38 289 Stellar parameters for study sample
See also: V/133 : Kepler Input Catalog (Kepler Mission Team, 2009) J/MNRAS/436/1883 : Properties of KOI host stars (Walkowicz+, 2013) J/ApJ/783/123 : Surface gravity for 220 Kepler stars (Campante+, 2014) J/ApJ/818/43 : Stellar surface gravity measures of KIC stars (Bastien+, 2016) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 9 I9 --- KIC Kepler Input Catalog identifier (KIC NNNNNNNN) 11- 15 F5.2 mag Kepmag Kepler magnitude 17- 20 I4 K Teff Effective temperature 22- 25 F4.2 [cm/s2] loggF8 Log surface gravity from 8-hr "flicker" 27- 30 F4.2 [cm/s2] loggNEA Log surface gravity from NASA Exoplanet Archive 32- 35 F4.2 ppm RVar Brightness variation range (in ppt unit) 38 I1 --- r_loggNEA [1/3] Reference for loggNEA (1)
Note (1): Reference as follows: 1 = asteroseismic (72 stars); 2 = spectroscopic (78 stars); 3 = photometric (139 stars).
History: From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 03-Jul-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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