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We find that Kepler exoplanet candidate (EC) host stars are preferentiallymetal-rich, including the low-mass stellar hosts of small-radius ECs. The lastobservation confirms a tentative hint that there is a correlation between themetallicity of low-mass stars and the presence of low-mass and small-radiusexoplanets. In particular, we compare the J-H--g-r color-color distribution ofKepler EC host stars with a control sample of dwarf stars selected from the~150,000 stars observed during Q1 and Q2 of the Kepler mission but with nodetected planets. We find that at J-H = 0.30 characteristic of solar-typestars, the average g-r color of stars that host giant ECs is 4-sigma redderthan the average color of the stars in the control sample. At the same time,the average g-r color of solar-type stars that host small-radius ECs isindistinguishable from the average color of the stars in the control sample. Inaddition, we find that at J-H = 0.62 indicative of late K dwarfs, the averageg-r color of stars that host small-radius ECs is 4-sigma redder than theaverage color of the stars in the control sample. These offsets are unlikely tobe caused by differential reddening, age differences between the twopopulations, or the presence of giant stars in the control sample. Stellarmodels suggest that the first color offset is due to a 0.2 dex enhancement in[Fe/H] of the giant EC host population at M_star = 1 M_Sun, while Sloanphotometry of M 67 and NGC 6791 suggests that the second color offset is due toa similar [Fe/H] enhancement of the small-radius EC host population at M_star =0.7 M_Sun. These correlations are a natural consequence of the core-accretionmodel of planet formation.

Kepler Exoplanet Candidate Host Stars are Preferentially Metal Rich