Hydrogen Variability in the Murray Formation, Gale Crater, Mars

Thomas, N.; Ehlmann, B. L.; Rapin, W.; Rivera‐Hernández, F.; Stein, N.; Frydenvang, J.; Gabriel, T. S. J.; Meslin, Pierre‐Yves; Maurice, S.; Wiens, Roger C.

doi:10.1029/2019je006289

Cited by 18 publications

(26 citation statements)

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“…The ridge does not preserve a redox interface. Campaign Goal 3: Document additional primary and secondary geochemical environments that are preserved in the ridge. There is abundant textural, mineralogical, and chemical evidence of diagenetic overprinting across multiple spatial scales on VRR (Bennett et al, 2018; Das et al, 2020; David et al, 2020; Frydenvang et al, 2020; Horgan, 2020; L'Haridon et al, 2020; McAdam et al, 2020; Rampe et al, 2020; Thomas et al, 2020; Thompson et al, 2020; Turner et al, 2020; Wong et al, 2020). The ridge experienced a complex diagenetic history after sediments were initially deposited, and various hypotheses about geochemistry of diagenetic fluids are presented throughout this special issue (David et al, 2020; Frydenvang et al, 2020; L'Haridon et al, 2020; McAdam et al, 2020; Rampe et al, 2020; Turner et al, 2020; Wong et al, 2020).…”

Section: Discussionmentioning

confidence: 99%

Evidence for a Diagenetic Origin of Vera Rubin Ridge, Gale Crater, Mars: Summary and Synthesis of Curiosity's Exploration Campaign

et al. 2020

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This paper provides an overview of the Curiosity rover's exploration at Vera Rubin ridge (VRR) and summarizes the science results. VRR is a distinct geomorphic feature on lower Aeolis Mons (informally known as Mount Sharp) that was identified in orbital data based on its distinct texture, topographic expression, and association with a hematite spectral signature. Curiosity conducted extensive remote sensing observations, acquired data on dozens of contact science targets, and drilled three outcrop samples from the ridge, as well as one outcrop sample immediately below the ridge. Our observations indicate that strata composing VRR were deposited in a predominantly lacustrine setting and are part of the Murray formation. The rocks within the ridge are chemically in family with underlying Murray formation strata. Red hematite is dispersed throughout much of the VRR bedrock, and this is the source of the orbital spectral detection. Gray hematite is also present in isolated, gray-colored patches concentrated toward the upper elevations of VRR, and these gray patches also contain small, dark Fe-rich nodules. We propose that VRR formed when diagenetic event(s) preferentially hardened rocks, which were subsequently eroded into a ridge by wind. Diagenesis also led to enhanced crystallization and/or cementation that deepened the ferric-related spectral absorptions on the ridge, which helped make them readily distinguishable from orbit. Results add to existing evidence

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Section: Discussionmentioning

confidence: 99%

Evidence for a Diagenetic Origin of Vera Rubin Ridge, Gale Crater, Mars: Summary and Synthesis of Curiosity's Exploration Campaign

et al. 2020

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“… 2016 , 2018 , 2019 ; Thomas et al. 2020 ). ChemCam’s chemistry is complemented by visible-range (“VIS”) reflectance spectroscopy to that allowed Johnson et al.…”

Section: Introductionmentioning

confidence: 99%

The SuperCam Instrument Suite on the NASA Mars 2020 Rover: Body Unit and Combined System Tests

et al. 2020

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The SuperCam instrument suite provides the Mars 2020 rover, Perseverance, with a number of versatile remote-sensing techniques that can be used at long distance as well as within the robotic-arm workspace. These include laser-induced breakdown spectroscopy (LIBS), remote time-resolved Raman and luminescence spectroscopies, and visible and infrared (VISIR; separately referred to as VIS and IR) reflectance spectroscopy. A remote micro-imager (RMI) provides high-resolution color context imaging, and a microphone can be used as a stand-alone tool for environmental studies or to determine physical properties of rocks and soils from shock waves of laser-produced plasmas. SuperCam is built in three parts: The mast unit (MU), consisting of the laser, telescope, RMI, IR spectrometer, and associated electronics, is described in a companion paper. The on-board calibration targets are described in another companion paper. Here we describe SuperCam’s body unit (BU) and testing of the integrated instrument.The BU, mounted inside the rover body, receives light from the MU via a 5.8 m optical fiber. The light is split into three wavelength bands by a demultiplexer, and is routed via fiber bundles to three optical spectrometers, two of which (UV and violet; 245–340 and 385–465 nm) are crossed Czerny-Turner reflection spectrometers, nearly identical to their counterparts on ChemCam. The third is a high-efficiency transmission spectrometer containing an optical intensifier capable of gating exposures to 100 ns or longer, with variable delay times relative to the laser pulse. This spectrometer covers 535–853 nm ($105\text{--}7070~\text{cm}^{-1}$ 105 – 7070 cm − 1 Raman shift relative to the 532 nm green laser beam) with $12~\text{cm}^{-1}$ 12 cm − 1 full-width at half-maximum peak resolution in the Raman fingerprint region. The BU electronics boards interface with the rover and control the instrument, returning data to the rover. Thermal systems maintain a warm temperature during cruise to Mars to avoid contamination on the optics, and cool the detectors during operations on Mars.Results obtained with the integrated instrument demonstrate its capabilities for LIBS, for which a library of 332 standards was developed. Examples of Raman and VISIR spectroscopy are shown, demonstrating clear mineral identification with both techniques. Luminescence spectra demonstrate the utility of having both spectral and temporal dimensions. Finally, RMI and microphone tests on the rover demonstrate the capabilities of these subsystems as well.

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“…Furthermore, Curiosity’s Dynamic Albedo of Neutron (DAN) instrument yields estimates between 1.5 and 3.3 wt% and up to ~5 wt% water locally within the upper 60 cm below the surface (Litvak et al, 2016; Mitrofanov et al, 2014). Measurements of bedrock in the Murray formation by ChemCam laser‐induced breakdown spectroscopy estimate a similar range of 2.3–3.1 wt% H 2 O (Thomas et al, 2020). The percentages for the Martian soil at Gale crater are likely derived from both adsorbed water molecules in the regolith and water structurally bound in minerals (Mitrofanov et al, 2014).…”

Section: Methodsmentioning

confidence: 90%

“…A similar near-surface water range of 2-7 wt% (Wernicke & Jakosky, 2021) was estimated based on data obtained by the Mars Odyssey Neutron Spectrometer (MONS; Feldman et al, 2004;Maurice et al, 2011) and the 3 µm absorption of the Observatoire pour la Min eralogie, l'Eau, les Glaces et l'Activit e (OMEGA; Audouard et al, 2014;Milliken et al, 2007). Furthermore, Curiosity's Dynamic Albedo of Neutron (DAN) instrument yields estimates between 1.5 and 3.3 wt% and up to ~5 wt% water locally within the upper 60 cm below the surface (Litvak et al, 2016 (Thomas et al, 2020). The percentages for the Martian soil at Gale crater are likely derived from both adsorbed water molecules in the regolith and water structurally bound in minerals (Mitrofanov et al, 2014).…”

Section: Fluid Content and Compositionmentioning

confidence: 99%

Constraints on the formation of carbonates and low‐grade metamorphic phases in the Martian crust as a function of H₂O‐CO₂ fluids

Semprich

Filiberto

Treiman

et al. 2021

Meteorit & Planetary Scien

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Low-grade metamorphic hydrous minerals and carbonates occur in various settings on Mars and in Martian meteorites. We present constraints on the stability of prehnite, zeolites, serpentine, and carbonates by modeling the influence of H 2 O-CO 2 fluids during low-grade metamorphism in the Martian crust using compositions of a Martian basalt and an ultramafic cumulate. In basaltic compositions with 5 wt% fluid, our models predict prehnite in less oxidized, CO 2 -poor conditions (≤0.44 mol kg À1 CO 2 ) on warmer geotherms of 20 °C km À1 . At fluid-saturated conditions, epidote and laumontite are replaced by quartz, calcite, chlorite, and muscovite. In ultramafic compositions with 5 wt% fluid, antigorite (serpentine) is stable at CO 2 -poor conditions of ≤0.33 mol kg À1 , while talc forms at 0.05-0.56 mol kg À1 CO 2 . At fluid-saturated conditions, antigorite is replaced by talc and chlorite, and at higher X(CO 2 ) by magnesite and quartz. Our models therefore suggest that prehnite, zeolites, and serpentine have formed in a CO 2 -poor environment on Mars implying that fluids during their formation either did not contain high amounts of CO 2 or had degassed CO 2 . Carbonates and potentially talc would have formed in the presence of a CO 2 -bearing fluid and therefore at different alteration stages than for prehnite, zeolites, and serpentine either in the same hydrothermal event during which the fluid composition changed gradually due to cooling and precipitation or by separate and successive alteration events with fluids of different compositions.

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Hydrogen Variability in the Murray Formation, Gale Crater, Mars

Cited by 18 publications

References 50 publications

Evidence for a Diagenetic Origin of Vera Rubin Ridge, Gale Crater, Mars: Summary and Synthesis of Curiosity's Exploration Campaign

Evidence for a Diagenetic Origin of Vera Rubin Ridge, Gale Crater, Mars: Summary and Synthesis of Curiosity's Exploration Campaign

The SuperCam Instrument Suite on the NASA Mars 2020 Rover: Body Unit and Combined System Tests

Constraints on the formation of carbonates and low‐grade metamorphic phases in the Martian crust as a function of H₂O‐CO₂ fluids

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Hydrogen Variability in the Murray Formation, Gale Crater, Mars

Cited by 18 publications

References 50 publications

Evidence for a Diagenetic Origin of Vera Rubin Ridge, Gale Crater, Mars: Summary and Synthesis of Curiosity's Exploration Campaign

Evidence for a Diagenetic Origin of Vera Rubin Ridge, Gale Crater, Mars: Summary and Synthesis of Curiosity's Exploration Campaign

The SuperCam Instrument Suite on the NASA Mars 2020 Rover: Body Unit and Combined System Tests

Constraints on the formation of carbonates and low‐grade metamorphic phases in the Martian crust as a function of H2O‐CO2 fluids

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Resources

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Constraints on the formation of carbonates and low‐grade metamorphic phases in the Martian crust as a function of H₂O‐CO₂ fluids