Detection and discrimination of sulfate minerals using reflectance spectroscopy

Cloutis, E. A.; Hawthorne, Frank C.; Mertzman, Stanley A.; Krenn, Kurt; Craig, M. A.; MARCINO, D; Méthot, Myriam; Strong, J.; Mustard, John F.; Blaney, D. L.

doi:10.1016/j.icarus.2006.04.003

Cited by 324 publications

(377 citation statements)

References 125 publications

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“…All of these whitish to yellowish soils exhibited distinctive reflectance maxima near 670 nm consistent with the presence of hydrated ferric sulfates (and distinct from jarosite and hematite; e.g., Morris et al, 1985;Crowley et al, 2003;Cloutis et al, 2006). Subtle absorptions and inflections near 480 nm and between 800-900 nm Figure 13.12) were also observed in some regions within these soils; these features are consistent with the presence of some Fe 3+ -bearing sulfate minerals.…”

Section: Whitish/yellowish Salty Soilsmentioning

confidence: 58%

Mars Exploration Rover Pancam multispectral imaging of rocks, soils, and dust at Gusev crater and Meridiani Planum

Bell

Calvin²,

Farrand³

et al. 2008

The Martian Surface

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Multispectral imaging from the Panoramic Camera (Pancam) instruments on the Mars Exploration Rovers Spirit and Opportunity has provided important new insights about the geology and geologic history of the rover landing sites and traverse locations in Gusev crater and Meridiani Planum. Pancam observations from near-UV to near-IR wavelengths provide limited compositional and mineralogic constraints on the presence abundance, and physical properties of ferric-and ferrous-iron bearing minerals in rocks, soils, and dust at both sites. High resolution and stereo morphologic observations have also helped to infer some aspects of the composition of these materials at both sites. Perhaps most importantly, Pancam observations were often efficiently and effectively used to discover and select the relatively small number of places where in situ measurements were performed by the rover instruments, thus supporting and enabling the much more quantitative mineralogic discoveries made using elemental chemistry and mineralogy data. This chapter summarizes the major compositionally-and mineralogicallyrelevant results at Gusev and Meridiani derived from Pancam observations. Classes of materials encountered in Gusev crater include outcrop rocks, float rocks, cobbles, clasts, soils, dust, rock grindings, rock coatings, windblown drift deposits, and exhumed whitish/yellowish salty soils. Materials studied in Meridiani Planum include sedimentary outcrop rocks, rock rinds, fracture fills, hematite spherules, cobbles, rock fragments, meteorites, soils, and windblown drift deposits. This chapter also previews the results of a number of coordinated observations between Pancam and other rover-based and Mars-orbital instruments that were designed to provide complementary new information and constraints on the mineralogy and physical properties of martian surface materials. 13

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Section: Whitish/yellowish Salty Soilsmentioning

confidence: 58%

Mars Exploration Rover Pancam multispectral imaging of rocks, soils, and dust at Gusev crater and Meridiani Planum

Bell

Calvin²,

Farrand³

et al. 2008

The Martian Surface

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“…All spectra contained common absorptions at approximately 1.4 and 1.9 µm indicating the presence of O-H and H2O bonds within minerals in every sample ( Figure 2). An absorption at approximately 2.22 µm is also observed in every sample, indicating the presence of either metal-O-H bonds or combination H2O and S-O bonds 22 . Shallow Fe 3+ electron transition absorptions in the 0.9 -1.0 µm range are also present in all samples indicating the presence of small amounts of iron-oxides, iron hydroxides or iron bearing silicates.…”

Section: Laboratory Vnir Reflectance Spectroscopymentioning

confidence: 84%

Spectral identification and quantification of salts in the Atacama Desert

Harris

Cousins

Claire

2016

Earth Resources and Environmental Remote Sensing/Gis Applications VII

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Salt minerals are an important natural resource. The ability to quickly and remotely identify and quantify salt deposits and salt contaminated soils and sands is therefore a priority goal for the various industries and agencies that utilise salts. The advent of global hyperspectral imagery from instruments such as Hyperion on NASA's Earth-Observing 1 satellite has opened up a new source of data that can potentially be used for just this task. This study aims to assess the ability of Visible and Near Infrared (VNIR) spectroscopy to identify and quantify salt minerals through the use of spectral mixture analysis. The surface and near-surface soils of the Atacama Desert in Chile contain a variety of well-studied salts, which together with low cloud coverage, and high aridity, makes this region an ideal testbed for this technique. Two forms of spectral data ranging 0.35 -2.5 μm were collected: laboratory spectra acquired using an ASD FieldSpec Pro instrument on samples from four locations in the Atacama desert known to have surface concentrations of sulfates, nitrates, chlorides and perchlorates; and images from the EO-1 satellite's Hyperion instrument taken over the same four locations. Mineral identifications and abundances were confirmed using quantitative XRD of the physical samples. Spectral endmembers were extracted from within the laboratory and Hyperion spectral datasets and together with additional spectral library endmembers fed into a linear mixture model. The resulting identification and abundances from both dataset types were verified against the sample XRD values. Issues of spectral scale, SNR and how different mineral spectra interact are considered, and the utility of VNIR spectroscopy and Hyperion in particular for mapping specific salt concentrations in desert environments is established. Overall, SMA was successful at estimating abundances of sulfate minerals, particularly calcium sulfate, from both hyperspectral image and laboratory sample spectra, while abundance estimation of other salt phase spectral end-members was achieved with a higher degree of error.

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“…Spectral signatures have been indicative of the presence of gypsum in the CRISM image frt00017ae0 (Fig 2a & b). Main absorption bands identified are triplet absorption between 1440-1540 nm, absorptions at 1900 nm, and small absorption at 2250 nm, all due to combinations and overtones of H 2 O vibrations and liberations (Hunt et al, 1971;Cloutis et al, 2006). One of the most prominent absorption bands is at 2400 nm, which has been assigned to polyhydrated sulphates (Bishop et al, 2007).…”

Section: Resultsmentioning

confidence: 99%

Mineralogical characterization of Juventae Chasma, Mars: evidences from MRO-CRISM

Singh

Rajesh

2014

Int. Arch. Photogramm. Remote Sens. Spatial Inf. Sci.

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Juventae Chasma is a long depression associated with Valles Marineris and this study discusses the spectral observation made after analysing the Mars Reconnaissance Orbiter (MRO) Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) Full Resolution targeted (FRT) Images in the wavelength region of 1000–2600 nm. Observations reveal the presence of hydrous sulphates, pyroxenes (mafic minerals) and silica rich minerals, more likely opaline silica or glass. Hydrous mineral identified shows the absorption bands, which are more consistent with gypsum. Absorption bands at 2300–2350 nm, and 2500–2550 nm, which are characteristics of carbonates, have been also identified in the region. Presence of this mineral assemblage, confirmed by the observed spectral signatures ranging from volcanic to sedimentary origin, implies a relatively geologically active area, and a significant region in terms of aqueous activity.

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Detection and discrimination of sulfate minerals using reflectance spectroscopy

Cited by 324 publications

References 125 publications

Mars Exploration Rover Pancam multispectral imaging of rocks, soils, and dust at Gusev crater and Meridiani Planum

Mars Exploration Rover Pancam multispectral imaging of rocks, soils, and dust at Gusev crater and Meridiani Planum

Spectral identification and quantification of salts in the Atacama Desert

Mineralogical characterization of Juventae Chasma, Mars: evidences from MRO-CRISM

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