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

Bibring, Jean‐Pierre; Langevin, Y.; Gendrin, A.; Gondet, B.; Poulet, F.; Berthé, Michel; Soufflot, A.; Arvidson, R. E.; Mangold, N.; Mustard, John F.; Drossart, P.

doi:10.1126/science.1108806

Cited by 879 publications

(703 citation statements)

References 21 publications

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“…An example is the hydrothermal alteration of the country rock related to intrusive activity observed in France (e.g., Merceron et al, 1992). The CRISM-based identification of Fe/Mg-rich hydrated phyllosilicates, as part of the suite of potential rock materials that form the Claritas rise, is consistent with MEX OMEGA-based spectroscopic investigations that show mineralogic evidence of ancient (Noachian) aqueous activity elsewhere in the geologic record of Mars (e.g., Bibring et al, 2005;Poulet et al, 2005). Thus, the CRISM signature may be consistent with a geologic environment influenced by the interaction of magma, tectonism, and water at Claritas rise, as indicated by the stratigraphic, geomorphic, and paleotectonic information presented earlier.…”

Section: Crism Analysis Of the Claritas Rise-forming Rock Materialssupporting

confidence: 53%

New evidence for a magmatic influence on the origin of Valles Marineris, Mars

Dohm

Williams

Anderson

et al. 2009

Journal of Volcanology and Geothermal Research

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Section: Crism Analysis Of the Claritas Rise-forming Rock Materialssupporting

confidence: 53%

New evidence for a magmatic influence on the origin of Valles Marineris, Mars

Dohm

Williams

Anderson

et al. 2009

Journal of Volcanology and Geothermal Research

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“…Observations from the OMEGA imaging spectrometer aboard Mars Express (Bibring et al 2004;Chicarro et al 2004) have revealed a rich diversity of mineralogy on the surface of Mars, including the hydrated clay mineral nontronite in older cratered terrains (Bibring et al 2005), along with montmorillonite and other clay minerals (Poulet et al 2005). Recent observations of hydrated silicate minerals by the CRISM instrument on Mars Reconnaissance Orbiter have validated these observations and provided an even more detailed picture of the distribution of hydrous phyllosilicates on the Martian surface Bishop et al 2008).…”

Section: Phyllosilicate Mineralsmentioning

confidence: 90%

Characterization and Calibration of the CheMin Mineralogical Instrument on Mars Science Laboratory

Blake¹,

Vaniman²,

Achilles³

et al. 2012

Mars Science Laboratory

120

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A principal goal of the Mars Science Laboratory (MSL) rover Curiosity is to identify and characterize past habitable environments on Mars. Determination of the mineralogical and chemical composition of Martian rocks and soils constrains their formation and alteration pathways, providing information on climate and habitability through time. The CheMin X-ray diffraction (XRD) and X-ray fluorescence (XRF) instrument on MSL will return accurate mineralogical identifications and quantitative phase abundances for scooped soil samples and drilled rock powders collected at Gale Crater during Curiosity's 1-Marsyear nominal mission. The instrument has a Co X-ray source and a cooled charge-coupled device (CCD) detector arranged in transmission geometry with the sample. CheMin's angular range of 5 • to 50 • 2θ with < 0.35 • 2θ resolution is sufficient to identify and quantify virtually all minerals. CheMin's XRF requirement was descoped for technical and budgetary reasons. However, X-ray energy discrimination is still required to separate Co Kα from Co Kβ and Fe Kα photons. The X-ray energy-dispersive histograms (EDH) returned along with XRD for instrument evaluation should be useful in identifying elements Z > 13 that are contained in the sample. The CheMin XRD is equipped with internal chemical and mineralogical standards and 27 reusable sample cells with either Mylar ® or Kapton ® windows to accommodate acidic-to-basic environmental conditions. The CheMin flight model (FM) instrument will be calibrated utilizing analyses of common samples against a demonstrationmodel (DM) instrument and CheMin-like laboratory instruments. The samples include phyllosilicate and sulfate minerals that are expected at Gale crater on the basis of remote sensing observations.

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“…Such secondary alteration products have been identified by thermal emission spectroscopy from orbit (Bandfield et al 2003;Bibring et al 2005). All the most recent missions to Mars have carried spectrometers capable of analysing the planet's surface at a variety of resolutions, and across a range of wavelengths, mainly from the near to mid-IR.…”

Section: Water On Mars : Evidence From Spectroscopic Analysismentioning

confidence: 99%

WatSen: searching for clues for water (and life) on Mars

Grady

2006

International Journal of Astrobiology

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: There is plenty of evidence for fluid on Mars : large-scale (planet-wide) features have been captured over four decades by a procession of orbiting satellites equipped with cameras with increasingly higher spatial resolutions. Imagery of the surface shows channels, valleys, ice-caps, etc. Small-scale, more local evidence for fluid has come from images obtained by rovers on the Martian surface. Images that water produced many of the features are supported by spectroscopic measurements (again both planet-wide and local) over a range of wavelengths, which show the presence of minerals generally only produced in the presence of water (haemetite, jarosite, etc.). Results from meteorites continue this picture of fluid activity taking place over significant periods of Mars' history. Despite all these indicators of water, direct detection of water has never been performed. We have reviewed the evidence for water on Mars' surface, and have described WatSen, a combined humidity sensor and infrared IR detector, which can be employed to search for water at and below Mars' surface. WatSen is designed to be part of the suite of instruments on the mole that will be deployed as part of the Geophysics and Environment Package on ExoMars. The objectives of the package are as follows : (i) to detect water within Martian soil by measuring humidity and IR spectral characteristics of the substrate at surface and at depth ; (ii) to determine the mineralogy and mineral chemistry of surface soils (this measurement will provide the mineralogical context for the elemental results that come from other instruments mounted on the landing platform); (iii) to determine how mineralogy changes with depth. The utility of WatSen is that it will not only detect the presence of water, but will also be able to record which minerals are present and their chemistry ; it is also sensitive to many organic species. WatSen is a new instrument concept specifically designed to search for clues of the presence of water, and to look for evidence of life on Mars.

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

Cited by 879 publications

References 21 publications

New evidence for a magmatic influence on the origin of Valles Marineris, Mars

New evidence for a magmatic influence on the origin of Valles Marineris, Mars

Characterization and Calibration of the CheMin Mineralogical Instrument on Mars Science Laboratory

WatSen: searching for clues for water (and life) on Mars

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