Exoplanet atmospheres

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EPICS: direct imaging of exoplanets with the E-ELT

GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY III 7735 (2010) ARTN 77352E

Authors:

Markus Kasper, Jean-Luc Beuzit, Christophe Verinaud, Raffaele G Gratton, Florian Kerber, Natalia Yaitskova, Anthony Boccaletti, Niranjan Thatte, Hans Martin Schmid, Christoph Keller, Pierre Baudoz, Lyu Abe, Emmanuel Aller-Carpentier, Jacopo Antichi, Mariangela Bonavita, Kjetil Dohlen, Enrico Fedrigo, Hiddo Hanenburg, Norbert Hubin, Rieks Jager, Visa Korkiakoski, Patrice Martinez, Dino Mesa, Olivier Preis, Patrick Rabou, Ronald Roelfsema, Graeme Salter, Mattias Tecza, Lars Venema
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Element cycling and the evolution of the Earth System

GEOCHIMICA ET COSMOCHIMICA ACTA 74:12 (2010) A339-A339

Authors:

Y Godderis, Y Donnadieu, JZ Williams, C Roelandt, J Schott, D Pollard, RT Pierrehumbert, S Brantley
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KMOS: Assembly, integration and testing of three 0.8-2.5 micron spectrographs

GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY III 7735 (2010) ARTN 773551

Authors:

Richard J Masters, Ian J Lewis, Ian AJ Tosh, Matthias Tecza, James Lynn, Robert EJ Watkins, Andrew Clack, Roger L Davies, Niranjan A Thatte, Mike Tacon, Rick Makin, Jon Temple, Alan Pearce
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Mapping Titan's HCN in the far infra-red: implications for photochemistry.

Faraday Discuss 147 (2010) 51-64

Authors:

NA Teanby, PGJ Irwin, R de Kok, CA Nixon

Abstract:

Observations of Titan's far infra-red spectra by the Cassini orbiter's Composite InfraRed Spectrometer have been used to determine the latitude distribution of HCN at 1 mbar by fitting the HCN and CO rotational lines in the 18-60 cm(-1) (160-550 microm) spectral range. Results confirm the north polar HCN enrichment previously observed using mid-IR data and support the conclusion that Titan's nitrile species are significantly more enriched than hydrocarbons species with similar predicted photochemical lifetimes. This suggests Titan's photochemical cycle includes an additional sink for nitrogen bearing species. The abundance of CO was also determined, and had a mean value of 55 +/- 6 ppm at 20 mbar. However, it was not possible to reliably determine the CO latitude variation due to unconstrained temperatures in the north polar lower stratosphere.
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Martian atmosphere as observed by VIRTIS-M on Rosetta spacecraft

JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS 115 (2010) ARTN E04004

Authors:

A Coradini, D Grassi, F Capaccioni, G Filacchione, F Tosi, E Ammannito, MC De Sanctis, V Formisano, P Wolkenberg, G Rinaldi, G Arnold, MA Barucci, G Bellucci, J Benkhoff, JP Bibring, A Blanco, D Bockelee-Morvan, MT Capria, R Carlson, U Carsenty, P Cerroni, L Colangeli, M Combes, M Combi, J Crovisier, P Drossart, T Encrenaz, S Erard, C Federico, U Fink, S Fonti, W-H Ip, PGJ Irwin, R Jaumann, E Kuehrt, Y Langevin, G Magni, T McCord, V Mennella, S Mottola, G Neukum, V Orofino, P Palumbo, G Piccioni, H Rauer, B Schmitt, D Tiphene, FW Taylor, GP Tozzi
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