Gas Giant and Brown Dwarf Companions: Mass Ratio and Orbital Distributions From A stars to M dwarfs

Understanding demographic properties of planet populations and multiple star systems constrains theories of planet and star formation. Surveys for very low-mass companions to M-A type stars detect brown dwarfs from multiple star formation and planets from circumstellar disks. We fit a composite model describing both very low-mass brown dwarf companions from "multiple-like processes" and gas giants from "planet-like processes" as functions of orbital separation and host star mass. We assemble a database of companion frequency estimates for masses from $< 1$ to $> 75$ Jupiter masses, separations from $< 0.3$ to $> 300$ AU, and host masses from $< 0.3$ to $> 2 M_{\odot}$. Using multinest, we fit these data to various models, performing model selection and deriving probability density functions. We assume companion mass ratio distributions are independent of orbital separation and fit a common log-normal orbital distribution to gas giant populations around M dwarfs, FGK, and A stars. A six-parameter model based on companion mass ratio distributions for planets and brown dwarfs is preferred. The planet CMRD slope is consistent with previous studies ($dN/dq \sim q^{-1.3} \pm 0.03$). Gas giant planets around stars from $< 0.3$ to $> 2.0 M_{\odot}$ follow a log-normal distribution peaking at ln(a) = 1.30 $\pm$ 0.03 (3.8 AU) with dispersion 0.22 $\pm$ 0.04. M dwarf distributions peak at smaller orbital radii than A stars, consistent with iceline considerations. Brown dwarf companion distributions extend stellar binary patterns, with the brown dwarf desert explained by flat-in-q mass functions and limited mass ratios below 0.1.