An Intermediate-orbit Brown Dwarf Confirmed with Astrometry+Radial Velocity Joint Analysis, and The Eccentricity Distribution of Brown Dwarfs Across Different Locations

Intermediate-orbit (∼1 au) brown dwarfs with absolute mass measurements are essential for understanding the evolution of substellar objects. Although such systems remain rare, their number is now being enlarged thanks to astrometry. Here, we present the absolute mass measurements for HD 203771B, a massive brown dwarf orbiting a K dwarf ( M * = 0.79 ± 0.08 M ⊙ ) with a period of 1140 days on an eccentric ( e ≈ 0.5) and inclined ( i ≈ 130 ∘ ) orbit. Through joint analysis of (1) radial velocities and Gaia two-body solution, as well as (2) radial velocities, Hipparcos Intermediate Astrometric Data and two-epoch Gaia astrometry, we obtain true companion masses of 74.2 0 − 3.64 + 3.46 M J and 69.0 3 − 4.95 + 4.99 M J , respectively, agreeing with each other within 1 σ . Taking a sample of 159 brown dwarfs with absolute mass measurements from different detection techniques, we investigate their eccentricity distributions across different semimajor axis ranges by fitting a Beta distribution. We find that the peak of eccentricity distribution tends to gradually shift toward lower values from wide orbits ( a > 20 au) to intermediate (1 < a < 20 au) and inner (0.1 < a < 1 au) regions. Such trend is plausibly due to disk friction during orbital evolution. Together with obliquity studies showing that brown dwarfs are mostly aligned, our result suggests that brown dwarfs may migrate inward through quiescent coplanar disk-driven processes.