HD 222237 b: a long-period super-Jupiter around a nearby star revealed by radial-velocity and Hipparcos-Gaia astrometry
Article
Article Title | HD 222237 b: a long-period super-Jupiter around a nearby star revealed by radial-velocity and Hipparcos-Gaia astrometry |
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ERA Journal ID | 1074 |
Article Category | Article |
Authors | Xiao, Guang-Yao, Feng, Fabo, Shectman, Stephen A., Tinney, C. G., Teske, Johanna K., Carter, B. D., Jones, H. R. A., Wittenmyer, Robert A., Diaz, Matias R., Crane, Jeffrey D., Wang, Sharon X., Bailey, J., O'Toole, S. J., Feinstein, Adina D., Rice, Malena, Essack, Zahra, Montet, Benjamin T., Shporer, Avi and Butler, R. Paul |
Journal Title | Monthly Notices of the Royal Astronomical Society |
Journal Citation | 534 (3), pp. 2858-2874 |
Article Number | United Kingdom |
Number of Pages | 17 |
Year | 2024 |
Publisher | Oxford University Press |
Place of Publication | United Kingdom |
ISSN | 0035-8711 |
1365-2966 | |
Digital Object Identifier (DOI) | https://doi.org/10.1093/mnras/stae2151 |
Web Address (URL) | https://academic.oup.com/mnras/article/534/3/2858/7778276 |
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 ± 0.002 pc away. By combining RV data, Hipparcos, and multi-epoch Gaia astrometry, we estimate the planetary massto be 5.19+0.58 −0.58 MJup, with an eccentricity of 0.56+0.03 −0.03 and a period of 40.8+5.8 −4.5 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 (15.50μm) is approximately 1.9 × 10−4, which is comparable with the measured limit of the MIRI coronagraphs. The relatively low metallicity of the host star (−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. |
Keywords | stars: individual: HD 222237; techniques: radial velocities; astrometry; planetary systems |
Contains Sensitive Content | Does not contain sensitive content |
ANZSRC Field of Research 2020 | 510199. Astronomical sciences not elsewhere classified |
Public Notes | This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2024 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. |
Byline Affiliations | Shanghai Jiao Tong University, China |
Carnegie Institution for Science, United States | |
University of New South Wales | |
Centre for Astrophysics | |
University of Hertfordshire, United Kingdom | |
Las Campanas Observatory, Chile | |
Tsinghua University, China | |
Macquarie University | |
University of Colorado Boulder, United States | |
Yale University, United States | |
University of New Mexico, United States | |
Massachusetts Institute of Technology, United States |
https://research.usq.edu.au/item/zv2v6/hd-222237-b-a-long-period-super-jupiter-around-a-nearby-star-revealed-by-radial-velocity-and-hipparcos-gaia-astrometry
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