Identification of hydrated silicate minerals on Mars using MRO-CRISM: Geologic context near Nili Fossae and implications for aqueous alteration

The Noachian terrain west of the Isidis basin hosts a diverse collection of alteration minerals in rocks comprising varied geomorphic units within a 100,000 km2 region in and near the Nili Fossae. Prior investigations in this region by the Observatoire pour l'Minéralogie, l'Eau, les Glaces, et l'Activité (OMEGA) instrument on Mars Express revealed large exposures of both mafic minerals and iron magnesium phyllosilicates in stratigraphic context. Expanding on the discoveries of OMEGA, the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) aboard the Mars Reconnaissance Orbiter (MRO) has found more spatially widespread and mineralogically diverse alteration minerals than previously realized, which represent multiple aqueous environments. Using CRISM near-infrared spectral data, we detail the basis for identification of iron and magnesium smectites (including both nontronite and more Mg-rich varieties), chlorite, prehnite, serpentine, kaolinite, potassium mica (illite or muscovite), hydrated (opaline) silica, the sodium zeolite analcime, and magnesium carbonate. The detection of serpentine and analcime on Mars is reported here for the first time. We detail the geomorphic context of these minerals using data from high-resolution imagers onboard MRO in conjunction with CRISM. We find that the distribution of alteration minerals is not homogeneous; rather, they occur in provinces with distinctive assemblages of alteration minerals. Key findings are (1) a distinctive stratigraphy, in and around the Nili Fossae, of kaolinite and magnesium carbonate in bedrock units always overlying Fe/Mg smectites and (2) evidence for mineral phases and assemblages indicative of low-grade metamorphic or hydrothermal aqueous alteration in cratered terrains. The alteration minerals around the Nili Fossae are more typical of those resulting from neutral to alkaline conditions rather than acidic conditions, which appear to have dominated much of Mars. Moreover, the mineralogic diversity and geologic context of alteration minerals found in the region around the Nili Fossae indicates several episodes of aqueous activity in multiple distinct environments

Characterizing the Mineralogy of Potential Lunar Landing Sites

Many processes active on the early Moon are common to most terrestrial planets, including the record of early and late impact bombardment. The Moon's surface provides a record of the earliest era of terrestrial planet evolution, and the type and composition of minerals that comprise a planetary surface are a direct result of the initial composition and subsequent thermal and physical processing. Lunar mineralogy seen today is thus a direct record of the early evolution of the lunar crust and subsequent geologic processes. Specifically, the distribution and concentration of specific minerals is closely tied to magma ocean products, lenses of intruded or remelted plutons, basaltic volcanism and fire-fountaining, and any process (e.g. cratering) that might redistribute or transform primary and secondary lunar crustal materials. The association of several lunar minerals with key geologic processes is illustrated in Figure 1. The geologic history of potential landing sites on the Moon can be read from the character and context of local mineralogy

A synthesis of Martian aqueous mineralogy after 1 Mars year of observations from the Mars Reconnaissance Orbiter

Martian aqueous mineral deposits have been examined and characterized using data acquired during Mars Reconnaissance Orbiter's (MRO) primary science phase, including Compact Reconnaissance Imaging Spectrometer for Mars hyperspectral images covering the 0.4–3.9 μm wavelength range, coordinated with higher–spatial resolution HiRISE and Context Imager images. MRO's new high-resolution measurements, combined with earlier data from Thermal Emission Spectrometer; Thermal Emission Imaging System; and Observatoire pour la Minéralogie, L'Eau, les Glaces et l'Activitié on Mars Express, indicate that aqueous minerals are both diverse and widespread on the Martian surface. The aqueous minerals occur in 9–10 classes of deposits characterized by distinct mineral assemblages, morphologies, and geologic settings. Phyllosilicates occur in several settings: in compositionally layered blankets hundreds of meters thick, superposed on eroded Noachian terrains; in lower layers of intracrater depositional fans; in layers with potential chlorides in sediments on intercrater plains; and as thousands of deep exposures in craters and escarpments. Carbonate-bearing rocks form a thin unit surrounding the Isidis basin. Hydrated silica occurs with hydrated sulfates in thin stratified deposits surrounding Valles Marineris. Hydrated sulfates also occur together with crystalline ferric minerals in thick, layered deposits in Terra Meridiani and in Valles Marineris and together with kaolinite in deposits that partially infill some highland craters. In this paper we describe each of the classes of deposits, review hypotheses for their origins, identify new questions posed by existing measurements, and consider their implications for ancient habitable environments. On the basis of current data, two to five classes of Noachian-aged deposits containing phyllosilicates and carbonates may have formed in aqueous environments with pH and water activities suitable for life

Orbital Identification of Carbonate-Bearing Rocks on Mars

Geochemical models for Mars predict carbonate formation during aqueous alteration. Carbonate-bearing rocks had not previously been detected on Mars' surface, but Mars Reconnaissance Orbiter mapping reveals a regional rock layer with near-infrared spectral characteristics that are consistent with the presence of magnesium carbonate in the Nili Fossae region. The carbonate is closely associated with both phyllosilicate-bearing and olivine-rich rock units and probably formed during the Noachian or early Hesperian era from the alteration of olivine by either hydrothermal fluids or near-surface water. The presence of carbonate as well as accompanying clays suggests that waters were neutral to alkaline at the time of its formation and that acidic weathering, proposed to be characteristic of Hesperian Mars, did not destroy these carbonates and thus did not dominate all aqueous environments

Continued Use of Exogenic Materials found on Mars as Planetary Research Tools

Exogenic materials (meteorites, micrometeorites and chemical tracers) are encountered both serendipitously and as campaign targets during Mars rover terrain traverse and reconnaissance. We advocate the continued study of these materials in-situ when encountered and permitted by extended and new Mars surface missions in the 2023–2032 decade.Whitepaper submitted to the Planetary Science and Astrobiology Decadal Survey 2023-2032. Additional co-authors: Sara Motaghian, Brandi L. Carrier, William H. Farrand, Marc D. Fries, Peter Grindrod, Andrew Langedam, Jérémie Lasue

Granite-hosted gold mineralization at Timbarra, northern New South Wales, Australia

The Timbarra gold deposits, located in the southern New England Fold Belt of New South Wales, Australia, represent an economically significant and distinctive member of the intrusion-related class of gold deposits. The five known deposits possess a total identified mineral resource of 16.8 Mt at 0.73 g/t gold, for a total of 396,800 contained ounces. The granites in the Timbarra region form a texturally complex, zoned pluton. The gold deposits are found within the Stanthorpe leucomonzogranite (242 to 238 Ma), which intrudes and forms a core to the more mafic, barren, Bungulla monzogranite (248 to 243 Ma). Gold is disseminated in the roof zone (upper 240 m) of a fractionated, magnetite- and ilmenite-bearing, I-type leucomonzogranite phase of the Stanthorpe body. The entire gold resource occurs in the areally extensive main leucomonzogranite pluton and is hosted by a medium- to coarse-grained granite. Disseminated ore is present in all five deposits, comprises >95% of the overall resource at Timbarra, and occurs predominantly as gently dipping, tabular to lenticular bodies that are conformably constrained beneath a fine-grained aplite carapace and internal aplite layers. The disseminated ore consists of gold-bearing muscovite-chlorite-carbonate alteration and infill of primary miarolitic cavities within massive leucomonzogranite or microgranite, and contains no discernable vein, joint, or fracture control at the outcrop or hand specimen scale. Structurally controlled mineralization forms the remaining 5% of the Timbarra resource, and comprises minor, low-density (0.02 to 0.25 per meter), vein-dikes and quartz-molybdenite veins emplaced along steeply dipping east-southeast, east-northeast, and north-northeast striking cooling joints. Both mineralization styles and alteration share a common paragenetic sequence of mineral precipitation. Quartz, perthitic K-feldspar, minor biotite, and albite are the earliest and most abundant infill minerals and commonly line primary cavities and vein-dikes. Subsequent minerals include coeval arsenopyrite, pyrite, fluorite, and molybdenite. The latest minerals include muscovite, chlorite, gold, calcite, silver-bismuth telluride, lead-bismuth telluride, and rare galena and chalcopyrite. The gold ore has a low total sulfide mineral concentration (h1%). Ore contains elevated concentrations of Bi, Ag, Te, As, Mo, and Sb; gold is strongly correlated with Bi, Ag, and Te, but only weakly with Mo, As, and Sb. Gold grains are generally <1 to 50 µm in size, but rarer grains as large as 1 mm in diameter have been observed. Gold fineness ranges from 950 to 600, and varies both within and between individual grains for a given deposit. The moderately oxidized I-type host granite, low-sulfide (h1%) ores, Au-Bi-Ag-Te geochemical signature, muscovite-chlorite-carbonate alteration assemblage, and low-salinity aqueous and carbonic fluids suggest that Timbarra is part of the newly recognized intrusion-related gold deposit class. Timbarra is distinguished from other intrusion-related gold deposits by the disseminated mineralization style within pervasively altered granite, forming gently dipping, tabular to lenticular ore zones