La planète Mars a connu une période où l'eau liquide était durablement stable. Outre les vestiges morphologiques d'une activité hydrologique en surface, l'interaction chimique de l'eau avec la croûte basaltique s'est traduite par la formation d'argiles et de sels hydratés en surface et en profondeur. Ces minéraux hydratés ont été détectés à la surface de Mars en 2004 grâce à l'instrument OMEGA, l'imageur hyperspectral infrarouge proche embarqué sur la sonde européenne Mars Express. Leur étude permet de reconstruire l'histoire de l'activité aqueuse sur Mars et de caractériser une période ancienne où l'environnement a pu être favorable à l'apparition d'une chimie pré-biotique. Ce travail de thèse s'intéresse aux environnements aqueux de Mars en couplant les données minéralogiques des imageurs hyperspectraux embarqués OMEGA/Mars Express et CRISM/Mars Reconnaissance Orbiter avec la morphologie. De nouveaux outils de traitement et d'analyse des données sont développés et ont permis la détection et la caractérisation spectrale de plus d'un millier de dépôts de minéraux hydratés sur Mars, fournissant une vue d'ensemble de l'altération. Celle-ci a eu lieu principalement dans la première partie du Noachien et a surtout formé des phyllosilicates ferro-magnésiens de la famille des vermiculites et smectites. Une importante diversité minérale est par ailleurs constatée avec une dizaine de familles minérales différentes, traçants des conditions géo-chimiques variées. Placés dans leur contexte géologique, certaines détections permettent de proposer l'existence passée d'un système hydrologique sur l'ensemble de la planète qui a donné naissance à un cycle des argiles similaire au cycle terrestre. Il apparait par ailleurs que les cratères d'impact sont le contexte privilégié des minéraux hydratés, mais le lien entre ces derniers et les processus d'impact demeure ambigu. La découverte d'un cycle des argiles est compatible avec l'hypothèse d'une planète potentiellement habitable au Noachien mais qui devra être vérifiée par l'exploration in-situ. / The planet Mars has experienced an era during which water was stable in its liquid state. In addition to morphological evidence for aqueous activity, the chemical interaction of water with the basaltic crust has led to the formation of hydrated clays and salts both on the surface and at depth. These hydrated minerals were first detected on the surface of Mars in 2004 with the OMEGA near infrared imaging spectrometer, onboard European probe Mars Express. Their study allows us to piece together the aqueous activity on Mars and to better understand an early era when the environment may have been conducive to prebiotic chemistry. This work focuses on the aqueous environments on Mars by coupling mineralogy data from the spaceborne imaging spectrometers OMEGA/Mars Express and CRISM/Mars Reconnaissance Orbiter to the surface morphology. The development of new data processing and analysis tools have led to the detection and spectral inquiry of over a thousand hydrated mineral exposures on Mars, thus providing a broad view of the aqueous alteration. The latter mostly took place during the Noachian era and formed primarily iron-magnesium bearing phyllosilicates of the vermiculite and smectite groups. In addition, great mineral diversity is found, implying varied geo-chemical formation conditions. Placed in their geological context, these detections show the likely existence of a past hydrological cycle on Mars which sustained a clay cycle similar to Earth's. It was also found that impact craters are the most common morphological context for these minerals, although the link between them remains unclear. The discovery of a clay cycle on Mars bodes well for the past habitability potential on Mars, but will need to be verified through in-situ exploration.

We investigate the spectra of asteroids at near- and mid-infrared wavelengths. In 2010 and 2011 we reported the detection of 3 ?m and 3.2-3.6 ?m signatures on (24) Themis and (65) Cybele indicative of water-ice and complex organics [1] [2] [3]. We further probed other primitive asteroids in the Cybele dynamical group and Themis family, finding diversity in the shape of their 3 ?m [4] [5] [6] and 10 ?m spectral features [4]. These differences indicated mineralogical and compositional variations within these asteroid populations. Also in the mid-infrared region we studied a larger population of asteroids belonging to the Bus C, D, and S taxanomic classes to understand the relationship between any mineralogy and hydration inferred in the visible and near- infrared with the shape, strength, and slope of the 10 ?m emission. We have discovered that at least 3 of the main Bus taxanomic groups (Cs, Ds, and Ss as defined by their visible spectra) clearly cluster into 3 statistically distinct groups based on their 8-13 ?m spectra. Additionally we have attempted to simulate in a laboratory the possible organic compounds we have detected on two asteroids, using various mixtures containing aromatic and aliphatic hydrocarbons. We find that asteroid (24) Themis and (65) Cybele have ?CH2/?CH3 and NCH2/NCH3 ratios similar to our 3- methylpentane, propane, and hexane residues, suggesting that the organics on these asteroids may be short chained and/or highly branched. The ?CH2/?CH3 and NCH2/NCH3 for asteroid(24)Themis are most consistent with the DISM, and some carbonaceous chondrites. The band centers of the C-H stretch absorptions indicate that both asteroids may have aliphatic carriers chemically bonded to electronegative groups (i.e. aromatics), and some that are not. We also detect a 3.45 ?m feature in the spectra of both asteroids that is present in several dense molecular clouds. Our results suggest an interstellar origin for the organics on (24) Themis, and likely (65) Cybele. The differences in the organics of Themis and Cybele are likely related to variations in thermal processing, irradiation and/or formation region in the solar nebula.

Triple oxygen and hydrogen isotope analysis of the structurally-bound water in gypsum can provide a direct measure of past hydrologic variability. This thesis presents the development of the water extraction and isotopic measurement procedures, the calculation of the gypsum-water isotope fractionation factors, and the application of the method to constrain the palaeohydrologic conditions in two temporally and geographically disparate sites. Measurement of the isotopic composition of gypsum hydration water is used to examine the hydrological changes that occurred during the Terminal Classic Drought of the Maya lowlands (~800-1000 CE), coincident with the period when the Classic Maya Civilization of Mesoamerica collapsed. The data provide a complete and direct archive of hydrological conditions that have previously been limited to ice core records. Mean annual rainfall is shown to have decreased by between 41% and 54%, with intervals of up to 70%, compared to present-day conditions. This study has also shown for the first time that relative humidity was 2%-7% lower during the Terminal Classic Drought compared to today. The methodology is also applied to the massive gypsum deposits in the marginal and deep basins of the Mediterranean to interpret the chemical evolution of parent water bodies during the Messinian Salinity Crisis (5.97-5.3 Ma). By combining the measurement of gypsum hydration water with other traditional (e.g. strontium) and novel (e.g. calcium and barium) isotope tracers, the hydrological changes during the deposition of Primary Lower Gypsum units of the Sorbas Basin in southeastern Spain, the Upper Gypsum units of Sicily, and deep basin deposits have been constrained. The results indicate that all deposits experienced a significant freshwater contribution to the mother fluids from which they formed. It is proposed that obliquity-controlled sea level and eccentricity-modulated precession, superimposed on longer-term tectonic restriction of the Mediterranean-Atlantic exchange, together controlled the varying depositional environments during the formation of the Messinian Salt Giant. This thesis demonstrates that the analysis of gypsum hydration water is a powerful tool for palaeoclimate reconstruction. The methodology can be applied to gypsum (and other hydrated minerals) in a wide range of settings across geological space and time, providing a rich source of information about the environmental conditions under which they formed.