A broadband thermal emission spectrum of the ultra-hot Jupiter WASP-18b.

Autor: Coulombe LP; Department of Physics, Université de Montréal, Montréal, Quebec, Canada. louis-philippe.coulombe@umontreal.ca.; Trottier Institute for Research on Exoplanets, Université de Montréal, Montréal, Quebec, Canada. louis-philippe.coulombe@umontreal.ca., Benneke B; Department of Physics, Université de Montréal, Montréal, Quebec, Canada.; Trottier Institute for Research on Exoplanets, Université de Montréal, Montréal, Quebec, Canada., Challener R; Department of Astronomy, University of Michigan, Ann Arbor, MI, USA., Piette AAA; Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, USA., Wiser LS; School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA., Mansfield M; Steward Observatory, University of Arizona, Tucson, AZ, USA., MacDonald RJ; Department of Astronomy, University of Michigan, Ann Arbor, MI, USA.; Department of Astronomy, Cornell University, Ithaca, NY, USA.; Carl Sagan Institute, Cornell University, Ithaca, NY, USA., Beltz H; Department of Astronomy, University of Michigan, Ann Arbor, MI, USA., Feinstein AD; Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL, USA., Radica M; Department of Physics, Université de Montréal, Montréal, Quebec, Canada.; Trottier Institute for Research on Exoplanets, Université de Montréal, Montréal, Quebec, Canada., Savel AB; Department of Astronomy, University of Maryland, College Park, MD, USA.; Center for Computational Astrophysics, Flatiron Institute, New York, NY, USA., Dos Santos LA; Space Telescope Science Institute, Baltimore, MD, USA., Bean JL; Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL, USA., Parmentier V; Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Nice, France., Wong I; NASA Goddard Space Flight Center, Greenbelt, MD, USA., Rauscher E; Department of Astronomy, University of Michigan, Ann Arbor, MI, USA., Komacek TD; Department of Astronomy, University of Maryland, College Park, MD, USA., Kempton EM; Department of Astronomy, University of Maryland, College Park, MD, USA., Tan X; Tsung-Dao Lee Institute, Shanghai Jiao Tong University, Shanghai, People's Republic of China.; School of Physics and Astronomy, Shanghai Jiao Tong University, Shanghai, People's Republic of China.; Atmospheric, Oceanic and Planetary Physics, Department of Physics, University of Oxford, Oxford, UK., Hammond M; Atmospheric, Oceanic and Planetary Physics, Department of Physics, University of Oxford, Oxford, UK., Lewis NT; Department of Mathematics and Statistics, Faculty of Environment, Science and Economy, University of Exeter, Exeter, UK., Line MR; School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA., Lee EKH; Center for Space and Habitability, University of Bern, Bern, Switzerland., Shivkumar H; Anton Pannekoek Institute for Astronomy, University of Amsterdam, Amsterdam, The Netherlands., Crossfield IJM; Department of Physics & Astronomy, University of Kansas, Lawrence, KS, USA., Nixon MC; Department of Astronomy, University of Maryland, College Park, MD, USA., Rackham BV; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA.; Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA., Wakeford HR; School of Physics, University of Bristol, Bristol, UK., Welbanks L; School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA., Zhang X; Department of Earth and Planetary Sciences, University of California, Santa Cruz, Santa Cruz, CA, USA., Batalha NM; Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA., Berta-Thompson ZK; Department of Astrophysical and Planetary Sciences, University of Colorado Boulder, Boulder, CO, USA., Changeat Q; European Space Agency, Space Telescope Science Institute, Baltimore, MD, USA.; Department of Physics and Astronomy, University College London, London, UK., Désert JM; Anton Pannekoek Institute for Astronomy, University of Amsterdam, Amsterdam, The Netherlands., Espinoza N; Space Telescope Science Institute, Baltimore, MD, USA., Goyal JM; School of Earth and Planetary Sciences (SEPS), National Institute of Science Education and Research (NISER), Homi Bhabha National Institute (HBNI), Jatni, India., Harrington J; Planetary Sciences Group, Department of Physics, University of Central Florida, Orlando, FL, USA.; Florida Space Institute, University of Central Florida, Orlando, FL, USA., Knutson HA; Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA., Kreidberg L; Max Planck Institute for Astronomy, Heidelberg, Germany., López-Morales M; Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA, USA., Shporer A; Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA., Sing DK; Department of Earth and Planetary Sciences, Johns Hopkins University, Baltimore, MD, USA.; Department of Physics & Astronomy, Johns Hopkins University, Baltimore, MD, USA., Stevenson KB; Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA., Aggarwal K; Indian Institute of Technology, Indore, India., Ahrer EM; Centre for Exoplanets and Habitability, University of Warwick, Coventry, UK.; Department of Physics, University of Warwick, Coventry, UK., Alam MK; Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, USA., Bell TJ; Bay Area Environmental Research Institute, NASA Ames Research Center, Moffett Field, CA, USA., Blecic J; Department of Physics, New York University Abu Dhabi, Abu Dhabi, United Arab Emirates.; Center for Astro, Particle, and Planetary Physics (CAP3), New York University Abu Dhabi, Abu Dhabi, United Arab Emirates., Caceres C; Instituto de Astrofisica, Universidad Andrés Bello, Santiago, Chile.; Núcleo Milenio de Formación Planetaria (NPF), Valparaíso, Chile.; Centro de Astrofisica y Tecnologias Afines (CATA), Santiago, Chile., Carter AL; Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA., Casewell SL; School of Physics and Astronomy, University of Leicester, Leicester, UK., Crouzet N; Leiden Observatory, University of Leiden, Leiden, The Netherlands., Cubillos PE; INAF - Osservatorio Astrofisico di Torino, Pino Torinese, Italy.; Space Research Institute, Austrian Academy of Sciences, Graz, Austria., Decin L; Institute of Astronomy, Department of Physics and Astronomy, KU Leuven, Leuven, Belgium., Fortney JJ; Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA., Gibson NP; School of Physics, Trinity College Dublin, Dublin, Ireland., Heng K; Department of Physics, University of Warwick, Coventry, UK.; Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, München, Germany.; ARTORG Center for Biomedical Engineering Research, University of Bern, Bern, Switzerland., Henning T; Max Planck Institute for Astronomy, Heidelberg, Germany., Iro N; Institute of Planetary Research (PF), German Aerospace Center (DLR), Berlin, Germany., Kendrew S; European Space Agency, Space Telescope Science Institute, Baltimore, MD, USA., Lagage PO; Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, Gif-sur-Yvette, France., Leconte J; Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, Pessac, France., Lendl M; Département d'Astronomie, Université de Genève, Sauverny, Switzerland., Lothringer JD; Department of Physics, Utah Valley University, Orem, UT, USA., Mancini L; Max Planck Institute for Astronomy, Heidelberg, Germany.; INAF - Osservatorio Astrofisico di Torino, Pino Torinese, Italy.; Department of Physics, University of Rome 'Tor Vergata', Rome, Italy., Mikal-Evans T; Max Planck Institute for Astronomy, Heidelberg, Germany., Molaverdikhani K; Max Planck Institute for Astronomy, Heidelberg, Germany.; Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, München, Germany.; Exzellenzcluster Origins, Garching, Germany., Nikolov NK; Space Telescope Science Institute, Baltimore, MD, USA., Ohno K; Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA., Palle E; Instituto de Astrofísica de Canarias (IAC), Tenerife, Spain., Piaulet C; Department of Physics, Université de Montréal, Montréal, Quebec, Canada.; Trottier Institute for Research on Exoplanets, Université de Montréal, Montréal, Quebec, Canada., Redfield S; Astronomy Department, Van Vleck Observatory, Wesleyan University, Middletown, CT, USA., Roy PA; Department of Physics, Université de Montréal, Montréal, Quebec, Canada.; Trottier Institute for Research on Exoplanets, Université de Montréal, Montréal, Quebec, Canada., Tsai SM; Department of Earth and Planetary Sciences, University of California, Riverside, Riverside, CA, USA., Venot O; Université Paris Cité and Université Paris-Est Creteil, CNRS, LISA, Paris, France., Wheatley PJ; Centre for Exoplanets and Habitability, University of Warwick, Coventry, UK.; Department of Physics, University of Warwick, Coventry, UK.
Jazyk: angličtina
Zdroj: Nature [Nature] 2023 Aug; Vol. 620 (7973), pp. 292-298. Date of Electronic Publication: 2023 May 31.
DOI: 10.1038/s41586-023-06230-1
Abstrakt: Close-in giant exoplanets with temperatures greater than 2,000 K ('ultra-hot Jupiters') have been the subject of extensive efforts to determine their atmospheric properties using thermal emission measurements from the Hubble Space Telescope (HST) and Spitzer Space Telescope 1-3 . However, previous studies have yielded inconsistent results because the small sizes of the spectral features and the limited information content of the data resulted in high sensitivity to the varying assumptions made in the treatment of instrument systematics and the atmospheric retrieval analysis 3-12 . Here we present a dayside thermal emission spectrum of the ultra-hot Jupiter WASP-18b obtained with the NIRISS 13 instrument on the JWST. The data span 0.85 to 2.85 μm in wavelength at an average resolving power of 400 and exhibit minimal systematics. The spectrum shows three water emission features (at >6σ confidence) and evidence for optical opacity, possibly attributable to H - , TiO and VO (combined significance of 3.8σ). Models that fit the data require a thermal inversion, molecular dissociation as predicted by chemical equilibrium, a solar heavy-element abundance ('metallicity', [Formula: see text] times solar) and a carbon-to-oxygen (C/O) ratio less than unity. The data also yield a dayside brightness temperature map, which shows a peak in temperature near the substellar point that decreases steeply and symmetrically with longitude towards the terminators.
(© 2023. The Author(s).)
Databáze: MEDLINE
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