HD 202206 : A Circumbinary Brown Dwarf System

Abstract

With Hubble Space Telescope Fine Guidance Sensor astrometry and previously published radial velocity measures we explore the exoplanetary system HD 202206. Our modeling results in a parallax, ${\pi }_{abs}=21.96\pm 0.12$ milliseconds of arc, a mass for HD 202206 B of M${}_B=0.089_{-0.006}^{+0.007}$ Msun, and a mass for HD 202206 c of M${}_c=17.9_{-1.8}^{+2.9}$ MJup. HD 202206 is a nearly face-on G+M binary orbited by a brown dwarf. The system architecture we determine supports past assertions that stability requires a 5:1 mean motion resonance (we find a period ratio, $P_c/P_B=4.92\pm 0.04$) and coplanarity (we find a mutual inclination, Phi = 6 \arcdeg \pm 2 \arcdeg).

Accepted by The Astronomical Journal, April 12, 2017. arXiv admin note: text overlap with arXiv:1003.0421. Revised to include Gaia acknowledgement

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