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We present the validation and characterization of Kepler-61b: a 2.15 R_Earthplanet orbiting near the inner edge of the habitable zone of a low-mass star.Our characterization of the host star Kepler-61 is based upon a comparison withthe set of spectroscopically similar stars with directly-measured radii andtemperatures. We apply a stellar prior drawn from the weighted mean of theseproperties, in tandem with the Kepler photometry, to infer a planetary radiusfor Kepler-61b of 2.15+/-0.13 R_Earth and an equilibrium temperature of273+/-13 K (given its period of 59.87756+/-0.00020 days and assuming aplanetary albedo of 0.3). The technique of leveraging the physical propertiesof nearby "proxy" stars allows for an independent check on stellarcharacterization via the traditional measurements with stellar spectra andevolutionary models. In this case, such a check had implications for theputative habitability of Kepler-61b: the planet is 10% warmer and larger thaninferred from K-band spectral characterization. From the Kepler photometry, weestimate a stellar rotation period of 36 days, which implies a stellar age of>1 Gyr. We summarize the evidence for the planetary nature of the Kepler-61transit signal, which we conclude is 30,000 times more likely to be due to aplanet than a blend scenario. Finally, we discuss possible compositions forKepler-61b with a comparison to theoretical models as well as to knownexoplanets with similar radii and dynamically measured masses.

Exoplanet Characterization by Proxy: a Transiting 2.15 R_Earth Planet Near the Habitable Zone of the Late K dwarf Kepler-61