Kavli Affiliate: Avi Shporer
| First 5 Authors: Guang-Yao Xiao, Fabo Feng, Stephen A. Shectman, C. G. Tinney, Johanna K. Teske
| Summary:
Giant planets on long period orbits around the nearest stars are among the
easiest to directly image. Unfortunately these planets are difficult to fully
constrain by indirect methods, e.g., transit and radial velocity (RV). In this
study, we present the discovery of a super-Jupiter, HD 222237 b, orbiting a
star located $11.445pm0.002$ pc away. By combining RV data, Hipparcos and
multi-epoch Gaia astrometry, we estimate the planetary mass to be
${5.19}_{-0.58}^{+0.58},M_{rm Jup}$, with an eccentricity of
${0.56}_{-0.03}^{+0.03}$ and a period of ${40.8}_{-4.5}^{+5.8}$ yr, making HD
222237 b a promising target for imaging using the Mid-Infrared Instrument
(MIRI) of JWST. A comparative analysis suggests that our method can break the
inclination degeneracy and thus differentiate between prograde and retrograde
orbits of a companion. We further find that the inferred contrast ratio between
the planet and the host star in the F1550C filter ($15.50,mu rm m$) is
approximately $1.9times10^{-4}$, which is comparable with the measured limit
of the MIRI coronagraphs. The relatively low metallicity of the host star
($rm-0.32,dex$) combined with the unique orbital architecture of this system
presents an excellent opportunity to probe the planet-metallicity correlation
and the formation scenarios of giant planets.
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