  The properties of a transiting planet's host star are written in its transit
light curve. The light curve can reveal the stellar density 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 TESS 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 stellar density, 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. 95 %
of our measured stellar densities are in 3-sigma or better agreement with
previously published literature values. We make posterior distributions for all
of our target KOIs available for online download.
