HD 222237 b: a long period super-Jupiter around a nearby star revealed by radial-velocity and Hipparcos-Gaia astrometry

Guang-Yao Xiao, Fabo Feng, Stephen A. Shectman, C. G. Tinney, Johanna K. Teske, B. D. Carter, H. R. A. Jones, Robert A. Wittenmyer, Matías R. Díaz, Jeffrey D. Crane, Sharon X. Wang, J. Bailey, S. J. O'Toole, Adina D. Feinstein, Malena Rice, Zahra Essack, Benjamin T. Montet, Avi Shporer, R. Paul Butler
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Abstract

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 $11.445\pm0.002$ 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 $1.9\times10^{-4}$, 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.
HD 222237 b:通过径向速度和海马座-盖亚天体测量法揭示的一颗围绕附近恒星的长周期超级木星
围绕最近恒星的长周期轨道上的巨行星是最容易直接成像的。遗憾的是,这些行星很难用间接方法(如凌日和径向速度)来完全约束。在这项研究中,我们发现了一颗超级木星HD 222237 b,它围绕着距离我们11.445/pm0.002$ pc的恒星运行。通过结合RV数据、Hipparcos和多表位Gaia天体测量数据,我们估计这颗行星的质量为${5.19}_{-0.58}^{+0.58}\,M_{/rm Jup}$,偏心率为${0.56}_{-0.03}^{+0.03}$和周期为${40.8}_{-4.5}^{+5.8}$年,这使得HD222237 b很有希望成为利用JWST的中红外仪器(MIRI)进行成像的目标。对比分析表明,我们的方法可以打破倾角退化,从而区分伴星的顺行和逆行轨道。我们进一步发现,在F1550C滤光片($15.50\, \mu \rm m$)中,推断出的行星与主星之间的对比度约为1.9\times10^{-4}$,这与MIRI日冕仪的测量极限相当。宿主恒星相对较低的金属性($\rm-0.32\,dex$)与该系统独特的轨道结构相结合,为探测行星与金属性的相关性以及巨行星的形成情况提供了一个极好的机会。
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