A ground-based near-infrared emission spectrum of the exoplanet HD 189733b

Mark R. Swain (), Pieter Deroo, Caitlin A. Griffith, Giovanna Tinetti, Azam Thatte, Gautam Vasisht, Pin Chen, Jeroen Bouwman, Ian J. Crossfield, Daniel Angerhausen, Cristina Afonso and Thomas Henning
Additional contact information
Mark R. Swain: Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California 91109-8099, USA
Pieter Deroo: Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California 91109-8099, USA
Caitlin A. Griffith: University of Arizona, Lunar and Planetary Laboratory, Space Science Building Room 525, 1629 East University Boulevard, Tucson, Arizona 85721, USA
Giovanna Tinetti: University College London, Gower Street, WC1E 6BT, London, UK
Azam Thatte: Woodruff School of Mechanical Engineering, MRDC Building, Room 4111, Georgia Institute of Technology, Atlanta, Georgia 30332-0405, USA
Gautam Vasisht: Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California 91109-8099, USA
Pin Chen: Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California 91109-8099, USA
Jeroen Bouwman: Max-Planck Institute for Astronomy, Koenigstuhl 17, D-69117, Heidelberg, Germany
Ian J. Crossfield: 475 Portola Plaza, Los Angeles, California 90034, USA
Daniel Angerhausen: German SOFIA Institute, Institute for Space Systems, Pfaffenwaldring 3170569, Stuttgart, Germany
Cristina Afonso: Max-Planck Institute for Astronomy, Koenigstuhl 17, D-69117, Heidelberg, Germany
Thomas Henning: Max-Planck Institute for Astronomy, Koenigstuhl 17, D-69117, Heidelberg, Germany

Nature, 2010, vol. 463, issue 7281, 637-639

Abstract: Exoplanet atmospheres Space-based infrared spectroscopy has successfully identified various molecules — H2O, CH4, CO2 and CO — in the atmospheres of 'hot Jupiter' extrasolar planets. Swain et al. now report ground-based observations of the dayside emission spectrum of the hot Jupiter HD 189733b at near-infrared wavelengths not available to space-based telescopes. They find a bright emission feature at ∼3.25 μm which is unexpected and difficult to explain using current models that assume local thermodynamic equilibrium conditions. Fluorescence emission from methane, similar to that seen in the atmospheres of Solar System planets, seems a likely explanation. This work suggests that atmospheric chemistry on exoplanets is more complex than was thought, and opens the field of exoplanet molecular spectroscopy to ground-based telescopes.

Date: 2010
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DOI: 10.1038/nature08775

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