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Characterization of potentially habitable planets: Retrieval of atmospheric and planetary properties from emission spectra

hal.structure.identifierSSE 2013
dc.contributor.authorVON PARIS, P.
hal.structure.identifierSSE 2013
dc.contributor.authorHEDELT, P.
hal.structure.identifierSSE 2013
dc.contributor.authorSELSIS, Franck
dc.contributor.authorSCHREIER, F.
hal.structure.identifierDLR Institut für Methodik der Fernerkundung / DLR Remote Sensing Technology Institute [IMF]
dc.contributor.authorTRAUTMANN, T.
dc.date.created2013-01-02
dc.date.issued2013-03
dc.identifier.issn0004-6361
dc.description.abstractEnContext. An increasing number of potentially habitable terrestrial planets and planet candidates are found by ongoing planet search programs. The search for atmospheric signatures to establish planetary habitability and the presence of life might be possible in the future. Aims: We want to quantify the accuracy of retrieved atmospheric parameters (composition, temperature, pressure) that might be obtained from infrared emission spectroscopy. Methods: We use synthetic observations of the atmospheres of hypothetical potentially habitable planets. These were constructed with a parametrized atmosphere model, a high-resolution radiative transfer model and a simplified noise model. The simulated observations were used to fit the model parameters. Furthermore, classic statistical tools such as χ2 statistics and least-square fits were used to analyze the simulated observations. Results: When adopting the design of currently planned or proposed exoplanet characterization missions, we find that emission spectroscopy could provide weak limits on the surface conditions of terrestrial planets, hence their potential habitability. However, these mission designs are unlikely to allow the composition of the atmosphere of a habitable planet to be characterized, even though CO2 is detected. Upon increasing the signal-to-noise ratios by about a factor of 2-5 (depending on spectral resolution) compared to current mission designs, the CO2 content could be characterized to within two orders of magnitude. The detection of the O3 biosignature remains marginal. The atmospheric temperature structure could not be constrained. Therefore, a full atmospheric characterization seems to be beyond the capabilities of such missions when using only emission spectroscopy during secondary eclipse or target visits. Other methods such as transmission spectroscopy or orbital photometry are probably needed in order to give additional constraints and break degeneracies.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enplanets and satellites: atmospheres
dc.subject.entechniques: spectroscopic
dc.subject.enmethods: data analysis
dc.title.enCharacterization of potentially habitable planets: Retrieval of atmospheric and planetary properties from emission spectra
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201220009
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.identifier.arxiv1301.0217
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.page120
bordeaux.volume551
bordeaux.peerReviewedoui
hal.identifierhal-00824609
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00824609v1
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