Experimental Astronomy

, Volume 40, Issue 2–3, pp 481–500 | Cite as

Unveiling the atmospheres of giant exoplanets with an EChO-class mission

  • Vivien Parmentier
  • Adam P. Showman
  • Julien de Wit
Original Article


More than a thousand exoplanets have been discovered over the last decade. Perhaps more excitingly, probing their atmospheres has become possible. With current data we have glimpsed the diversity of exoplanet atmospheres that will be revealed over the coming decade. However, numerous questions concerning their chemical composition, thermal structure, and atmospheric dynamics remain to be answered. More observations of higher quality are needed. In the next years, the selection of a space-based mission dedicated to the spectroscopic characterization of exoplanets would revolutionize our understanding of the physics of planetary atmospheres. Such a mission was proposed to the ESA cosmic vision program in 2014. Our paper is therefore based on the planned capabilities of the Exoplanet Characterization Observatory (EChO), but it should equally apply to any future mission with similar characteristics. With its large spectral coverage (0.4 − 16 μm), high spectral resolution (λλ > 300 below 5 μm and λλ > 30 above 5 μm) and 1.5m mirror, a future mission such as EChO will provide spectrally resolved transit lightcurves, secondary eclipses lightcurves, and full phase curves of numerous exoplanets with an unprecedented signal-to-noise ratio. In this paper, we review some of today’s main scientific questions about gas giant exoplanets atmospheres, for which a future mission such as EChO will bring a decisive contribution.


Exoplanet Atmosphere EChO 


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Copyright information

© Springer Science+Business Media Dordrecht 2014

Authors and Affiliations

  • Vivien Parmentier
    • 1
  • Adam P. Showman
    • 2
  • Julien de Wit
    • 3
  1. 1.Laboratoire Lagrange, UMR7293Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’AzurNiceFrance
  2. 2.Department of Planetary Sciences, Lunar and Planetary LaboratoryUniversity of ArizonaTucsonUSA
  3. 3.Department of EarthAtmospheric and Planetary Sciences, MITCambridgeUSA

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