A temperate super-Jupiter imaged with JWST in the mid-infrared

E. C. Matthews (), A. L. Carter, P. Pathak, C. V. Morley, M. W. Phillips, S. Krishanth P. M., F. Feng, M. J. Bonse, L. A. Boogaard, J. A. Burt, I. J. M. Crossfield, E. S. Douglas, Th. Henning, J. Hom, C.-L. Ko, M. Kasper, A.-M. Lagrange, D. Petit dit de la Roche and F. Philipot
Additional contact information
E. C. Matthews: Max Planck Institute for Astronomy
A. L. Carter: Space Telescope Science Institute
P. Pathak: Indian Institute of Technology Kanpur
C. V. Morley: University of Texas at Austin
M. W. Phillips: University of Edinburgh, Royal Observatory
S. Krishanth P. M.: Steward Observatory and Department of Astronomy
F. Feng: Shanghai Jiao Tong University
M. J. Bonse: Institute for Particle Physics & Astrophysics
L. A. Boogaard: Max Planck Institute for Astronomy
J. A. Burt: California Institute of Technology
I. J. M. Crossfield: University of Kansas
E. S. Douglas: Steward Observatory and Department of Astronomy
Th. Henning: Max Planck Institute for Astronomy
J. Hom: Steward Observatory and Department of Astronomy
C.-L. Ko: Steward Observatory and Department of Astronomy
M. Kasper: European Southern Observatory
A.-M. Lagrange: Université PSL, CNRS
D. Petit dit de la Roche: University of Geneva
F. Philipot: Université PSL, CNRS

Nature, 2024, vol. 633, issue 8031, 789-792

Abstract: Abstract Of the approximately 25 directly imaged planets to date, all are younger than 500 Myr, and all but six are younger than 100 Myr (ref. 1). Eps Ind A (HD209100, HIP108870) is a K5V star of roughly solar age (recently derived as 3.7–5.7 Gyr (ref. 2) and $${3.5}_{-1.3}^{+0.8}$$ 3.5 − 1.3 + 0.8 Gyr (ref. 3)). A long-term radial-velocity trend4,5 and an astrometric acceleration6,7 led to claims of a giant planet2,8,9 orbiting the nearby star (3.6384 ± 0.0013 pc; ref. 10). Here we report JWST coronagraphic images which reveal a giant exoplanet that is consistent with these radial and astrometric measurements but inconsistent with the previously claimed planet properties. The new planet has a temperature of approximately 275 K and is remarkably bright at 10.65 and 15.50 µm. Non-detections between 3.5 and 5.0 µm indicate an unknown opacity source in the atmosphere, possibly suggesting a high-metallicity, high carbon-to-oxygen ratio planet. The best-fitting temperature of the planet is consistent with theoretical thermal evolution models, which were previously untested at this temperature range. The data indicate that this is probably the only giant planet in the system, and therefore we refer to it as b, despite it having significantly different orbital properties than the previously claimed planet b.

Date: 2024
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DOI: 10.1038/s41586-024-07837-8

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