Mars Surface Diversity as Revealed by the OMEGA/Mars Express Observations

By B. Gondet, François Poulet, A. Soufflot, M. Combes, P. Drossart, T. Encrenaz, T. Fouchet, Riccardo Merchiorri, G. Belluci, F. Altieri and 23 more. Science, 2005

971 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Paleontology

View Paper: https://www.semanticscholar.org/paper/bed27441924ba101f5a1d083fb64c7530862f57a

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Citations in the corpus

The Sample Analysis at Mars Investigation and Instrument Suite (2012, positive): “At Gale crater, MSL will test the hypothesis that aqueous enviromnents on Mars evolved from phyllosilicate-forming to sulfate-forming (Bibring et al. 2006).”
Reflectance and emission spectroscopy study of four groups of phyllosilicates: smectites, kaolinite-serpentines, chlorites and micas (2008, methodology): “We focused on the visible/near-infrared (VNIR) region from 0.4 4.0 mm measured by Mars Express/OMEGA (Bibring et al., 2005), MRO/CRISM (Murchie et al., 2007) and partially covered by Mars Exploration Rover/Pancam (Bell et al., 2006), as well as the midIR region (5 50 mm) covered by MGS/TES…”
Outgassing History and Escape of the Martian Atmosphere and Water Inventory (2015, background): “Bibring et al. (2005) concluded that the non-detection of carbonates would indicate that no major surface sink of CO2 is present and the initial CO2, if it represented a much higher content, would then have been lost from Mars early rather than stored in surface reservoirs after having been…”
Atmospheric Escape and Evolution of Terrestrial Planets and Satellites (2008, background): “Bibring et al. (2005) concluded that the OMEGA observations are consistent with early strong escape of the most of the martian CO2 atmosphere.”
Mineralogy of a Mudstone at Yellowknife Bay, Gale Crater, Mars (2014, background): “The recent decade of orbiter- and rover-based studies of ancient sedimentary rocks on Mars has revealed a diverse mineralogy that constrains the nature and timing of early environments in the history of the planet (1, 2, 3) These studies provide a starting point for considering the habitability of M”
Scientific goals for the observation of Venus by VIRTIS on ESA/Venus Express mission (2007, background): “…of previous instruments which combine imaging and spectroscopy in the near infrared, like Galileo/NIMS (NIMS—near infrared mapping spectrometer) (Carlson et al., 1992), Cassini/ VIMS (VIMS—visible-infrared mapping spectrometer) (Brown et al., 2004) and Mars Express/OMEGA (Bibring et al., 2005).”
Near-infrared spectra of ferrous mineral mixtures and methods for their identification in planetary surface spectra (2014, neutral): “For example, iron oxides, iron-bearing clays, and ferric sulfates often exhibit absorption bands near 0.9 lm, along with other diagnostic absorptions in the visible, due to spin-forbidden transitions in Fe3+ (Morris et al., 1985; Bishop et al., 1993; Bishop and Murad, 1996; Cloutis et al., 2006).”
The Climate of Early Mars (2016, background): “The martian surface is sulfur-rich (Clark et al. 1976) and sulphates are abundant on Hesperian and Noachian terrain (Gendrin et al. 2005; Bibring et al. 2005; Ehlmann & Edwards 2014).”
Mineralogy and evolution of the surface of Mars: A review (2007, background): “The layered terrains containing the sulphates represent important deposits, tens of km wide, and with a thickness of a few km (Bibring et al., 2005; Gendrin et al., 2005).”
Hydration state of the Martian surface as seen by Mars Express OMEGA: 2. H2O content of the surface (2007, background): “This upper surface layer represents the boundary between the regolith and atmosphere; thus the amount of water stored in these two reservoirs and at this boundary is expected to vary spatially and temporally with changing equilibrium conditions.”