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NOTE ADDED BY JPL WEBMASTER: This content has not been approved or adopted by, NASA, JPL, or the California Institute of Technology. This document is being made available for information purposes only, and any views and opinions expressed herein do not necessarily state or reflect those of NASA, JPL, or the California Institute of Technology.

H. Clenet, C. Quantin, M. Andreani and P. Allemand 29/02/2012, Washington CARBONATE-BEARING CRUSTAL EXPOSURE IN AN IMPACT CRATER ASSOCIATED WITH AN OUTFLOW CHANNEL CONTEXT

Map from Edwards et al., 2008, JGR Proposed landing site Olivine layer in Eos Chasma

R : LCPINDEX [ ] G: HPCINDEX [ ] B: OLINDEX [ ]

From Ehlmann et al., 2008

« Direct » carbonation reactions High P CO 2 Serpentinization of olivine (fayalite + aqueous silica = serpentine) Carbonation of serpentine (serpentine + CO 2 = talc + magnésite) Serpentine and carbonation reactions Low P CO 2 Circulation of fluids enriched in CO 2 High P CO 2 then

© IPGP (CNRS, Univ Paris Diderot)/Università di Modena e Reggio Emilia Menez et al., Nature Geoscience 2012 Blue=hydrogarnet (Ca 3 Al 2 (SiO 4 ) 3-x (OH) 4x ) Green=serpentinized pyroxene Red=Ferric oxyde Yellow=organic molecules Serpentinization of olivine (forsterite + H 2 O = serpentine + brucite + magnetite) Carbonation of serpentine (serpentine + CO 2 = talc + magnésite) Serpentine and carbonation reactions Low P CO 2 High P CO 2 then Habitability?

Circulation of fluids enriched in CO 2 Hydrothermal systemHesperian aqueous activity Emplacement of the mafic unit Post-impact process ? Paleolake induced deposits High T° Low T°

Elevation Slope

-Primitive martian crust -Putative hydrothermal system and its exobiological niches -Outflow channel context