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SO2, silicate clouds, but no CH4 detected in a warm Neptune

Abstract

WASP-107b is a warm ( ~ 740 K) transiting planet with a Neptune-like mass of ~ 30.5 M⊕ and Jupiter-like radius of ~ 0.94 RJ 1,2 whose extended atmosphere is eroding 3. Previous observations showed evidence for water vapour and a thick high-altitude condensate layer in WASP-107b’s atmosphere 4,5. Recently, photochemically produced sulphur dioxide (SO2) was detected in the atmosphere of a hot ( ~ 1,200 K) Saturn-mass planet from transmission spectroscopy near 4.05 μm 6,7, but for temperatures below ~ 1,000 K sulphur is predicted to preferably form sulphur allotropes instead of SO2 8,9,10. Here we report the 9σ-detection of two fundamental vibration bands of SO2, at 7.35 μm and 8.69 μm, in the transmission spectrum of WASP-107b using the Mid-Infrared Instrument (MIRI) of the JWST. This discovery establishes WASP-107b as the second irradiated exoplanet with confirmed photochemistry, extending the temperature range of exoplanets exhibiting detected photochemistry from ~ 1,200 K down to ~ 740 K. Additionally, our spectral analysis reveals the presence of silicate clouds, which are strongly favoured ( ~ 7σ) over simpler cloud setups. Furthermore, water is detected ( ~ 12σ), but methane is not. These findings provide evidence of disequilibrium chemistry and indicate a dynamically active atmosphere with a super-solar metallicity.

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Author notes

  1. These authors contributed equally: Achrène Dyrek, Michiel Min and Leen Decin

Authors and Affiliations

  1. Université Paris Cité, Université Paris-Saclay, CEA, CNRS, AIM, Gif-sur-Yvette, France

    Achrène Dyrek

  2. SRON Netherlands Institute for Space Research, Leiden, the Netherlands

    Michiel Min, Rens Waters, Francisco Ardevol Martinez, Billy Edwards & Fred Lahuis

  3. Institute of Astronomy, KU Leuven, Leuven, Belgium

    Leen Decin, Thomas Konings, Bart Vandenbussche, Ioannis Argyriou, Linus Heinke & Pierre Royer

  4. Max-Planck-Institut für Astronomie (MPIA), Heidelberg, Germany

    Jeroen Bouwman, Paul Mollière, Manuel Güdel, Thomas Henning, Oliver Krause & Silvia Scheithauer

  5. Leiden Observatory, Leiden University, Leiden, the Netherlands

    Nicolas Crouzet & Ewine F. van Dishoeck

  6. Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, Gif-sur-Yvette, France

    Pierre-Olivier Lagage, Elsa Ducrot & Alain Coulais

  7. Université Paris-Saclay, UVSQ, CNRS, CEA, Maison de la Simulation, Gif-sur-Yvette, France

    Pascal Tremblin

  8. Department of Astrophysics, University of Vienna, Vienna, Austria

    Manuel Güdel & Gwenael Van Looveren

  9. ETH Zürich, Institute for Particle Physics and Astrophysics, Zürich, Switzerland

    Manuel Güdel, Adrian Glauser & Polychronis Patapis

  10. School of Physics & Astronomy, Space Research Centre, Space Park Leicester, University of Leicester, Leicester, UK

    John Pye

  11. Department of Astrophysics/IMAPP, Radboud University, Nijmegen, the Netherlands

    Rens Waters

  12. HFML – FELIX, Radboud University, Nijmegen, the Netherlands

    Rens Waters

  13. Kapteyn Institute of Astronomy, University of Groningen, Groningen, the Netherlands

    Francisco Ardevol Martinez & Michael Mueller

  14. Centre for Exoplanet Science, University of Edinburgh, Edinburgh, UK

    Francisco Ardevol Martinez & Linus Heinke

  15. School of GeoSciences, University of Edinburgh, Edinburgh, UK

    Francisco Ardevol Martinez & Linus Heinke

  16. STAR Institute, Université de Liège, Liège, Belgium

    Olivier Absil

  17. Centro de Astrobiología (CAB), CSIC-INTA, Madrid, Spain

    David Barrado, Daniel Rouan & Luis Colina

  18. LESIA, Observatoire de Paris, CNRS, Université Paris Diderot, Université Pierre et Marie Curie, Meudon, France

    Pierre Baudoz & Anthony Boccaletti

  19. Université Paris-Saclay, CEA, Département d’Electronique des Détecteurs et d’Informatique pour la Physique, Gif-sur-Yvette, France

    Christophe Cossou & René Gastaud

  20. LERMA, Observatoire de Paris, Université PSL, Sorbonne Université, CNRS, Paris, France

    Alain Coulais

  21. UK Astronomy Technology Centre, Royal Observatory, Edinburgh, UK

    Alistair Glasse

  22. Space Science and Astrobiology Division, NASA’s Ames Research Center, Moffett Field, California, USA

    Thomas P. Greene

  23. European Space Agency, Space Telescope Science Institute, Baltimore, Maryland, USA

    Sarah Kendrew

  24. Department of Astronomy, Stockholm University, AlbaNova University Center, Stockholm, Sweden

    Goran Olofsson

  25. Department of Physics and Astronomy, University College London, London, UK

    Ingo Waldmann

  26. Department of Astrophysics, American Museum of Natural History, New York, NY, USA

    Niall Whiteford

  27. Department of Astronomy, Oskar Klein Centre, Stockholm University, Stockholm, Sweden

    Göran Ostlin

  28. School of Cosmic Physics, Dublin Institute for Advanced Studies, Dublin, Ireland

    Tom P. Ray

  29. UK Astronomy Technology Centre, Royal Observatory Edinburgh, Edinburgh, UK

    Gillian Wright

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  1. Achrène Dyrek
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Corresponding author

Correspondence to
Achrène Dyrek.

Supplementary information

Supplementary Information

This file contains Supplementary Methods: a complete methodology of data reduction on both JWST and HST data, retrieval techniques and models with a peculiar emphasis on a specific non-linearity correction derived to reduce the JWST data. Included are Supplementary Figs. 1–15 and Supplementary Tables 1–3.

Peer Review File

Supplementary Data for Supplementary Fig. 13

Dataset describes the input stellar spectral energy distributions and photo-absorption cross sections of SO2, H2O, H2S, and CH4 used for the photochemical model.

Supplementary Data for Supplementary Fig. 14

Dataset that provides the model-predicted SO2 molar fractions when all photo-absorption cross sections are taken into account and when they are taken into account separately. Also provides the values of predicted SO2 molar fractions without vertical mixing, without photodissociation of H2O and without including the thermochemical reaction H2O + H⇌H2 + OH.

Supplementary Data for Supplementary Fig. 15

Dataset that provides the [OH]/[H] ratio for equilibrium and disequilibrium predictions through the [OH]/[H] proxy and the molar fraction of [OH]/[H] obtained with the model.

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Cite this article

Dyrek, A., Min, M., Decin, L. et al. SO2, silicate clouds, but no CH4 detected in a warm Neptune.
Nature (2023). https://doi.org/10.1038/s41586-023-06849-0

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  • Received: 23 June 2023

  • Accepted: 08 November 2023

  • Published: 15 November 2023

  • DOI: https://doi.org/10.1038/s41586-023-06849-0

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