Authors

Aarynn L. Carter, University of California, Santa Cruz
Sasha Hinkley, University of Exeter
Jens Kammerer, Space Telescope Science Institute
Andrew Skemer, University of California, Santa Cruz
Beth A. Biller, University of Edinburgh, Institute for Astronomy
Jarron M. Leisenring, The University of Arizona
Maxwell A. Millar-Blanchaer, University of California, Santa Barbara
Simon Petrus, Universidad de Valparaiso
Jordan M. Stone, U.S. Naval Research Laboratory
Kimberly Ward-Duong, Smith CollegeFollow
Jason J. Wang, Northwestern University
Julien H. Girard, Space Telescope Science Institute
Dean C. Hines, Space Telescope Science Institute
Marshall D. Perrin, Space Telescope Science Institute
Laurent Pueyo, Space Telescope Science Institute
William O. Balmer, Space Telescope Science Institute
Mariangela Bonavita, The Open University
Mickael Bonnefoy, Institut de Planétologie et d’Astrophysique de Grenoble (IPAG)
Gael Chauvin, Laboratoire Joseph-Louis Lagrange
Elodie Choquet, Laboratoire d'Astrophysique de Marseille
Valentin Christiaens, Université de Liège
Camilla Danielski, CSIC - Instituto de Astrofísica de Andalucía (IAA)
Grant M. Kennedy, Faculty of Science, Engineering and Medicine
Elisabeth C. Matthews, Max Planck Institute for Astronomy
Brittany E. Miles, University of California, Santa Cruz
Polychronis Patapis, ETH Zürich
Shrishmoy Ray, University of Exeter
Emily Rickman, European Space Agency - ESA
Steph Sallum, University of California, Irvine
Karl R. Stapelfeldt, California Institute of Technology
Niall Whiteford, American Museum of Natural History
Yifan Zhou, College of Natural Sciences

Author ORCID Identifier

Kimberly Ward-Duong: 0000-0002-4479-8291

Document Type

Article

Publication Date

7-1-2023

Publication Title

Astrophysical Journal Letters

Abstract

We present JWST Early Release Science coronagraphic observations of the super-Jupiter exoplanet, HIP 65426b, with the Near-Infrared Camera (NIRCam) from 2 to 5 μm, and with the Mid-Infrared Instrument (MIRI) from 11 to 16 μm. At a separation of ∼0.″82 (87 − 31 + 108 au), HIP 65426b is clearly detected in all seven of our observational filters, representing the first images of an exoplanet to be obtained by JWST, and the first-ever direct detection of an exoplanet beyond 5 μm. These observations demonstrate that JWST is exceeding its nominal predicted performance by up to a factor of 10, depending on separation and subtraction method, with measured 5σ contrast limits of ∼1 × 10−5 and ∼2 × 10−4 at 1″ for NIRCam at 4.4 μm and MIRI at 11.3 μm, respectively. These contrast limits provide sensitivity to sub-Jupiter companions with masses as low as 0.3M Jup beyond separations of ∼100 au. Together with existing ground-based near-infrared data, the JWST photometry are fit well by a BT-SETTL atmospheric model from 1 to 16 μm, and they span ∼97% of HIP 65426b's luminous range. Independent of the choice of model atmosphere, we measure an empirical bolometric luminosity that is tightly constrained between log L bol / L ⊙ = −4.31 and −4.14, which in turn provides a robust mass constraint of 7.1 ± 1.2 M Jup. In totality, these observations confirm that JWST presents a powerful and exciting opportunity to characterize the population of exoplanets amenable to high-contrast imaging in greater detail.

Volume

951

Issue

1

DOI

10.3847/2041-8213/acd93e

ISSN

20418205

Creative Commons License

Creative Commons Attribution 4.0 International License
This work is licensed under a Creative Commons Attribution 4.0 International License.

Rights

© 2023 The Authors

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