¹Michael S. Phillips,¹Scott L. Murchie,¹Frank P. Seelos,¹Katie M. Hancock,^1,2Christina Selby,¹Ryan T. Poffenbarger,¹David C. Stephens,^1,3Maia Kawamura
Icarus (in Press) Link to Article [https://doi.org/10.1016/j.icarus.2023.115712]
¹The Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
²MAXAR Technologies, Arlington, VA, USA
³Department of Physics and Astronomy, Dartmouth College, Hanover, NH, USA
Copyright Elsevier

The CRISM instrument on MRO collected visible-infrared hyperspectral mapping data (HSP; 180 m/pixel, 262 spectral channels covering 365 to 3937 nm) that covered ∼39% of Mars. Here we present results from a new processing pipeline for these data that produces 5° x 5° hyperspectral mapping tiled mosaics that overlap the coverage of recently released multispectral map tile products (version 4 Multispectral Reduced Data Records, MRDRs; 180 m/pixel, 72 spectral channels). These data enable regional investigations into compositional variations that require high spectral resolution or wavelengths not included in MRDRs. In addition to standard processing techniques available in the CRISM Analysis Toolkit (CAT), the pipeline includes a new correction for systematic discrepancies in radiometric calibration between CRISM observing modes, an improved filtering algorithm to remediate noise, and a technique to correct for differences in radiometry among data strips that arise from differences in photometric and atmospheric conditions. Demonstration hyperspectral mapping tiles covering the Mawrth Vallis region were developed and compared with MRDRs and high spatial resolution hyperspectral targeted observations. The new processing pipeline shows an improvement in data quality over standard processing using CAT utilities. Compared to targeted observations (18 or 36 m/pixel, 545 spectral channels), hyperspectral mapping tile mosaics reveal compositional information across a much greater spatial extent at the expense of 5–10 times coarser spatial resolution. In addition, the hyperspectral mapping tile mosaics reveal greater compositional detail in both the spatial and spectral dimensions compared to MRDRs, but with sparser spatial coverage. Sample hyperspectral mapping tile mosaics over the Mawrth Vallis region reveal hydrated silica, Al-bearing smectite, Fe/Mg-bearing smectite, and mixed clays, consistent with compositions previously reported in the literature.

^1,2Piers Koefoed,³Jean-Alix Barrat,^1,4Olga Pravdivtseva,⁵Conel M. O’D. Alexander,^1,2Katharina Lodders,^1,4Ryan Ogliore,^1,2Kun Wang 王昆
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2023.07.025]
¹McDonnell Center for the Space Sciences, Washington University in St. Louis, St. Louis, Missouri, 63130, USA
²Department of Earth and Planetary Sciences, Washington University in St. Louis, St. Louis, Missouri, 63130, USA
³Institut Universitaire Européen de la Mer, Université de Bretagne Occidentale, CNRS UMS 3113, F-29280 Plouzané, France
⁴Department of Physics, Washington University in St. Louis, St. Louis, Missouri, 63130, USA
⁵Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
Copyright Elsevier

The isotopic analysis of moderately volatile elements such as K have gained significant interest in recent years as they possess the potential to help us better understand solar system formation. Even so, the precise K isotopic composition of CI chondrites, the most chemically primitive chondrite, has remained elusive. As the K elemental composition of CI chondrites matches well with the solar photosphere, it is possible that their K isotopic composition represents the solar system initial value. Here, we investigate the CI chondrite K isotopic composition in order to determine the precise CI chondrite, and thus possibly solar system initial, δ41K value. In addition, we investigate the K isotope compositions of several other chondrite groups, evaluate all available chondrite K isotope data together, and use these data along with data from a range of other isotope systems to assess if nucleosynthetic variations, volatility related processes, or parent body processes can best explain the range of isotope variations. The δ41K composition of all nine CI chondrite pieces analyzed in this study show limited variation, ranging from −0.29‰ to −0.17‰. When combined with the previous CI analysis, an overall mean CI δ41K value of −0.21 ± 0.05‰ (2SE) is obtained. This K isotope composition is distinct from the Bulk Silicate Earth value of −0.43 ± 0.17‰ (2SD), heavier than almost all other chondrite groups, and may represent the solar system initial K isotope composition. When comparing all chondrites broadly, ordinary chondrites show the lightest mean K isotope composition of −0.76 ± 0.06‰ (H = −0.71 ± 0.12‰, L = −0.77 ± 0.04‰, LL = −0.81 ± 0.12‰), enstatite chondrites the middle composition of −0.39 ± 0.11‰ (EH = −0.34 ± 0.05‰, EL = −0.45 ± 0.20‰), and carbonaceous chondrites the heaviest composition of −0.31 ± 0.08‰. For the carbonaceous chondrite groups CK (−0.42 ± 0.11‰), CR (−0.46 ± 0.05‰), and CV (−0.38 ± 0.07‰) chondrites show lighter δ41K compositions compared to CO (−0.20 ± 0.10‰), CM (−0.23 ± 0.11‰), and CI (−0.21 ± 0.05‰) chondrites. When these K isotope group averages are compared against the averages for other mass-dependent moderately volatile element isotope systems (δ87Rb, δ66Zn, δ71Ga, δ128Te) and mass-independent isotope systems (ε54Cr, ε64Ni, ε50Ti, Δ17O, ε40K, and ε66Zn,), a range of correlations are observed. Across all chondrite groups δ41K shows correlations with δ87Rb, δ66Zn, and δ71Ga, and correlations with ε54Cr, ε64Ni, ε50Ti, ε40K, and ε66Zn. When comparing the CCs only, correlations are observed between δ41K and all four of the other moderately volatile elements assessed, while the mass-independent isotope systems show no strong correlations. Regarding the K isotope variations, these observations, along with other textural and chemical data, can be best explained by inherited isotopic variations form different precursor reservoirs (the cause of which is difficult to conclusively determine, though most likely related to the NC-CC dichotomy), and volatility related fractionation processes for the carbonaceous chondrite groups (most likely due to component mixing).