Water in the Martian regolith from OMEGA/Mars Express

Audouard, J.; Poulet, F.; Vincendon, M.; Milliken, R. E.; Jouglet, D.; Bibring, Jean‐Pierre; Gondet, B.; Langevin, Y.

doi:10.1002/2014je004649

Cited by 45 publications

(56 citation statements)

References 93 publications

(233 reference statements)

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“…The atmospheric 3‐

normalμ

m IBD can be used to obtain a quick look at water ice clouds in our data set. It is also of interest in itself as orbital observations of Mars surface have to account for atmospheric 3‐

normalμ

m contribution to deliver information about surface hydration (Audouard et al, ; Jouglet et al, ). As illustrated in Figure , the 3‐

normalμ

m IBD matches at first order the more elaborated water ice detection scheme presented in section .…”

Section: Resultsmentioning

confidence: 99%

Martian Water Ice Clouds During the 2018 Global Dust Storm as Observed by the ACS‐MIR Channel Onboard the Trace Gas Orbiter

et al. 2020

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The Atmospheric Chemistry Suite (ACS) instrument onboard the ExoMars Trace Gas Orbiter (TGO) European Space Agency‐Roscosmos mission began science operations in March 2018. ACS Mid‐InfraRed (MIR) channel notably provides solar occultation observations of the Martian atmosphere in the 2.3‐ to 4.2‐ normalμ m spectral range. Here, we use these observations to characterize water ice clouds before and during the MY 34 Global Dust Storm (GDS). We developed a method to detect water ice clouds with mean particle size ≤ 2 normalμ m and applied it to observations gathered between Ls=165∘ and Ls=243∘. We observe a shift in water ice cloud maximum altitudes from about 60 km before the GDS to above 90 km during the storm. These very high altitude, small‐sized ( reff≤0.3.3emnormalμ m) water ice clouds are more frequent during MY 34 compared to non‐GDS years at the same season. Particle size frequently decreases with altitude, both locally within a given profile and globally in the whole data set. We observe that the maximum altitude at which a given size is observed can increase during the GDS by several tens of kilometers for certain sizes. We notably notice some large water ice particles ( reff≥1.5.3emnormalμ m) at surprisingly high altitudes during the GDS (50–70 km). These results suggest that GDS can significantly impact the formation and properties of high‐altitude water ice clouds as compared to the usual perihelion dust activity.

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“…The atmospheric 3‐

normalμ

m IBD can be used to obtain a quick look at water ice clouds in our data set. It is also of interest in itself as orbital observations of Mars surface have to account for atmospheric 3‐

normalμ

m contribution to deliver information about surface hydration (Audouard et al, ; Jouglet et al, ). As illustrated in Figure , the 3‐

normalμ

m IBD matches at first order the more elaborated water ice detection scheme presented in section .…”

Section: Resultsmentioning

confidence: 99%

Martian Water Ice Clouds During the 2018 Global Dust Storm as Observed by the ACS‐MIR Channel Onboard the Trace Gas Orbiter

et al. 2020

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“…Wang et al ., ]. Recent analyses of visible/near‐infrared reflectance spectra globally across Mars also support a negligible role for H 2 O adsorption in the Martian surface compared to chemically bound H 2 O [ Audouard et al ., ].…”

Section: Resultsmentioning

confidence: 99%

Sulfates hydrating bulk soil in the Martian low and middle latitudes

Karunatillake

Wray

Gasnault

et al. 2014

Geophysical Research Letters

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The evidence for sulfate-bearing strata, across Late-Noachian to Amazonian eons, suggests a central role for sulfates in acidity and salinity of Martian paleofluids and the planet's habitability. However, details remain unclear owing to shallow sampling and the limited ability of visible/near-infrared spectroscopy to distinguish among some sulfates. Using chemical data from the Mars Odyssey gamma ray spectrometer, including the sulfur map of Mars, we confirm the possibility of hydrous sulfates acting as key hydrates throughout the southern midlatitudinal soil at decimeter depths. An H 2 O:S molar ratio between 2.4 and 4.0 for 80% of the midlatitudes is also consistent with hydrous sulfate phases, including the many Fe sulfates hydrated in this range or mixtures of Ca and Mg sulfates. Nevertheless, hydrous Fe sulfates could explain our observations in a simpler manner relative to Ca/Mg mixtures. Furthermore, phyllosilicates, zeolites, amorphous phases, and H 2 O(s) do not seem to be strong candidates to explain the H-S variations. Consequently, we speculate that sulfates, as the primary contributor of H 2 O in bulk soil, may influence modern aqueous processes including warm-season slope lineae in the southern hemisphere.

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“…32 This hydrated dust cover measured in situ is consistent with the global infrared water absorption band seen in orbital data. 67 …”

Section: Aeolian Dust Analysismentioning

confidence: 99%

ChemCam activities and discoveries during the nominal mission of the Mars Science Laboratory in Gale crater, Mars

Maurice

Clegg

Wiens

et al. 2016

J. Anal. At. Spectrom.

151

111

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At Gale crater, Mars, ChemCam acquired its first laser-induced breakdown spectroscopy (LIBS) target on Sol 13 of the landed portion of the mission (a Sol is a Mars day). Up to Sol 800, more than 188 000 LIBS spectra were acquired on more than 5800 points distributed over about 650 individual targets. We present a comprehensive review of ChemCam scientific accomplishments during that period, together with a focus on the lessons learned from the first use of LIBS in space. For data processing, we describe new tools that had to be developed to account for the uniqueness of Mars data. With regard to chemistry, we present a summary of the composition range measured on Mars for major-element oxides (SiO 2 , TiO 2 , Al 2 O 3 , FeO T , MgO, CaO, Na 2 O, K 2 O) based on various multivariate models, with associated precisions.ChemCam also observed H, and the non-metallic elements C, O, P, and S, which are usually difficult to quantify with LIBS. F and Cl are observed through their molecular lines. We discuss the most relevant LIBS lines for detection of minor and trace elements (Li, Rb, Sr, Ba, Cr, Mn, Ni, and Zn). These results were obtained thanks to comprehensive ground reference datasets, which are set to mimic the expected mineralogy and chemistry on Mars. With regard to the first use of LIBS in space, we analyze and quantify, often for the first time, each of the advantages of using stand-off LIBS in space: no sample preparation, analysis within its petrological context, dust removal, sub-millimeter scale investigation, multi-point analysis, the ability to carry out statistical surveys and whole-rock analyses, and rapid data acquisition.We conclude with a discussion of ChemCam performance to survey the geochemistry of Mars, and its valuable support of decisions about selecting where and whether to make observations with more time and resource-intensive tools in the rover's instrument suite. In the end, we present a bird's-eye view of Cite this:

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Water in the Martian regolith from OMEGA/Mars Express

Cited by 45 publications

References 93 publications

Martian Water Ice Clouds During the 2018 Global Dust Storm as Observed by the ACS‐MIR Channel Onboard the Trace Gas Orbiter

Martian Water Ice Clouds During the 2018 Global Dust Storm as Observed by the ACS‐MIR Channel Onboard the Trace Gas Orbiter

Sulfates hydrating bulk soil in the Martian low and middle latitudes

ChemCam activities and discoveries during the nominal mission of the Mars Science Laboratory in Gale crater, Mars

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