A new planet around an M dwarf: Revealing a correlation between exoplanets and stellar mass

We report precise Doppler measurements of GJ 317 ( M3.5 V) that reveal the presence of a planet with a minimum mass M-P sin i = 1.2 M-Jup in an eccentric, 692.9 day orbit. GJ 317 is only the third M dwarf with a Doppler- detected Jovian planet. The residuals to a single- Keplerian fit show evidence of a possible second orbital companion. The inclusion of a second Jupiter- mass planet ( P approximate to 2700 days, M-P sin i = 0: 83 M-Jup) decreases root X-u(2) similar to p from2.02 to 1.23, and reduces the rms from12.5 to 6.32ms(-1). A false- alarmtest yields a 1.1% probability that the curvature in the residuals of the single-planet fit is due to random fluctuations, lending additional credibility to the two- planet model. However, our data only marginally constrain a two- planet fit, and further monitoring is necessary to fully characterize the properties of the second companion. To study the effect of stellarmass on giant planet occurrence, wemeasure the fraction of starswith planets in threemass bins comprised of our samples ofMDwarfs, solar- mass stars, and intermediate- mass subgiants. We find a positive correlation between stellarmass and the occurrence rate of Jovian planetswithin 2.5AU. Low- mass K and M stars have a 1.8% +/- 1.0% planet occurrence rate compared to 4.2% +/- 0.7% for solar- mass stars and 8.9% +/- 2.9% for the higher mass subgiants. This result indicates that the former F- and A- type stars with M-* >= 1.3 M-circle dot in our sample are nearly 5 times more likely than the M dwarfs to harbor a giant planet. Our analysis shows that the correlation between Jovian planet occurrence and stellar mass exists even after correcting for the effects of stellar metallicity.