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We report precise Doppler measurements of GJ317 (M3.5V) that reveal thepresence of a planet with a minimum mass Msini = 1.2 Mjup in an eccentric,692.9 day orbit. GJ317 is only the third M dwarf with a Doppler-detected Jovianplanet. The residuals to a single-Keplerian fit show evidence of a possiblesecond orbital companion. The inclusion of an additional Jupiter-mass planet (P= 2700 days, Msini = 0.83 Mjup) improves the quality of fit significantly,reducing the rms from 12.5 m/s to 6.32 m/s. A false-alarm test yields a 1.1%probability that the curvature in the residuals of the single-planet fit is dueto random fluctuations, lending additional credibility to the two-planet model.However, our data only marginally constrain a two-planet fit and furthermonitoring is necessary to fully characterize the properties of the secondplanet. To study the effect of stellar mass on Jovian planet occurrence wecombine our samples of M stars, Solar-mass dwarfs and intermediate-masssubgiants. We find a positive correlation between stellar mass and theoccurrence rate of Jovian planets within 2.5 AU; the former A-type stars in oursample are nearly 5 times more likely than the M dwarfs to harbor a giantplanet. Our analysis shows that the correlation between Jovian planetoccurrence and stellar mass remains even after accounting for the effects ofstellar metallicity.

A New Planet Around an M Dwarf: Revealing a Correlation Between Exoplanets and Stellar Mass