2014ApJ...791...91C

In contrast to radial velocity (RV) surveys, results from microlensing surveys indicate that giant planets with masses greater than the critical mass for core accretion (∼0.1 M_Jup) are relatively common around low-mass stars. Using the methodology developed in the first paper, we predict the sensitivity of M-dwarf RV surveys to analogs of the population of planets inferred by microlensing. We find that RV surveys should detect a handful of super-Jovian (>M_Jup) planets at the longest periods being probed. These planets are indeed found by RV surveys, implying that the demographic constraints inferred from these two methods are consistent. Finally, we combine the results from both methods to estimate planet frequencies spanning wide regions of parameter space. We find that the frequency of Jupiters and super-Jupiters (1 ≲ m_p sin i/M_Jup ≲ 13) with periods 1 ≤ P/days ≤ 10⁴ is f_J = 0.029_–0.015^+0.013, a median factor of 4.3 (1.5-14 at 95% confidence) smaller than the inferred frequency of such planets around FGK stars of 0.11±0.02. However, we find the frequency of all giant planets with 30 ≲ m_p sin i/M_⊕ ≲ 10⁴ and 1 ≤ P/days ≤ 10⁴ to be f_G = 0.15_–0.07^+0.06, only a median factor of 2.2 (0.73-5.9 at 95% confidence) smaller than the inferred frequency of such planets orbiting FGK stars of 0.31±0.07. For a more conservative definition of giant planets (50 ≲ m_psin i/M_⊕ ≲ 10⁴), we find f_G' = 0.11± 0.05, a median factor of 2.2 (0.73-6.7 at 95% confidence) smaller than that inferred for FGK stars of 0.25±0.05. Finally, we find the frequency of all planets with 1 ≤ m_psin i/M_⊕ ≤ 10⁴ and 1 ≤ P/days ≤ 10⁴ to be f_p= 1.9±0.5.