Adam and gaia duplicates9/20/2023 ( 2013) for Earth-sized planets around solar-type stars with orbital periods between 5 and 100 days. Dressing & Charbonneau ( 2013) found that for the M dwarf stars in the Kepler sample, the Earth-sized (0.5–1.4 R ⊕) planetary occurrence rate is 0.51 planets per star for orbital periods less than 50 days, significantly higher than the 0.26 planetary occurrence rate found by Petigura et al. 2012), a population that is absent in our own solar system. For example, many planets observed around Kepler host stars have been found to have sizes between Earth and Neptune (Howard et al. ![]() One of the biggest breakthroughs enabled by Kepler was our understanding of exoplanet occurrence rates as a function of planet size, orbital period, and stellar type. 2010), officially retired in 2018, has left behind a legacy data set for stellar astrophysics and exoplanet science. We furthermore use the Gaia proper motions to show that the Kepler selection function was unbiased with respect to kinematics. We find that the Kepler target selection is nearly complete for stars brighter than Kp 1.2) RUWE values at ∼ σ significance, suggesting that the Kepler target selection shows some bias against either close or wide binaries. ![]() Here we use Gaia DR2 to reconstruct the Kepler selection function and explore possible biases with respect to evolutionary state, stellar multiplicity, and kinematics. ![]() A critical piece of information to exploit Kepler data is its selection function, since all targets had to be selected from a sample of half a million stars on the Kepler CCDs using limited information. The Kepler Mission revolutionized exoplanet science and stellar astrophysics by obtaining highly precise photometry of over 200,000 stars over 4 yr.
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