Know the Planet, Know the Star: Precise Stellar Densities from Kepler Transit Light Curves

被引：20

作者：

Sandford, Emily ^{[1
]}

Kipping, David ^{[1
]}

机构：

[1] Columbia Univ, Dept Astron, 550 West 120th St, New York, NY 10027 USA

来源：

ASTRONOMICAL JOURNAL | 2017年 / 154卷 / 06期

基金：

美国国家航空航天局;

关键词：

eclipses; planetary systems; planets and satellites: general; methods: data analysis; LIMB-DARKENING COEFFICIENTS; SYSTEMS; ECCENTRICITY; PARAMETERS; PHOTOMETRY; MODELS; TRES-2; !text type='PYTHON']PYTHON[!/text; ORBITS; BIASES;

D O I：

10.3847/1538-3881/aa94bf

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The properties of a transiting planet's host star are written in its transit light curve. The light curve can reveal the stellar density (rho(*)) and the limb-darkening profile in addition to the characteristics of the planet and its orbit. For planets with strong prior constraints on orbital eccentricity, we may measure these stellar properties directly from the light curve; this method promises to aid greatly in the characterization of transiting planet host stars targeted by the upcoming NASA Transiting Exoplanet Survey Satellite mission and any long-period, singly transiting planets discovered in the same systems. Using Bayesian inference, we fit a transit model, including a nonlinear limb-darkening law, to 66 Kepler transiting planet hosts to measure their stellar properties. We present posterior distributions of rho(*), limb-darkening coefficients, and other system parameters for these stars. We measure densities to within 5% for the majority of our target stars, with the dominant precision-limiting factor being the signal-to-noise ratio of the transits. Of our measured stellar densities, 95% are in 3 sigma or better agreement with previously published literature values. We make posterior distributions for all of our target Kepler objects of interest available online at 10.5281/zenodo.1028515.

引用

页数：15

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