Replication Data for: Halogen and Cl isotopic systematics in Martian phosphates: Implications for the Cl cycle and surface halogen reservoirs on Mars.

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Replication Data for: Halogen and Cl isotopic systematics in Martian phosphates: Implications for the Cl cycle and surface halogen reservoirs on Mars.
Bellucci, Jeremy J.; Whitehouse, M.J; John, Timm; Nemchin, A.A.; Snape, J.F., 2021, "Replication Data for: Halogen and Cl isotopic systematics in Martian phosphates: Implications for the Cl cycle and surface halogen reservoirs on Mars.", https://doi.org/10.35003/ZW5GXO, TRR170-DB, V1, UNF:6:fK1yjupGfONUkhKtIfun7Q== [fileUNF]
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Description
• In situ investigation of the Cl and halogen concentrations in Martian meteorites. • Cl compositions in Martian meteorites controlled by interactions with the surface halogens and perchlorate. • Evidence for early and widespread interaction between Martian meteorites, Martian hydrosphere, and Martian atmosphere. • Similar bulk initial Cl isotope composition between the Earth, Moon, and Mars. (2016-01-01)
Subject Chemistry; Other
Keyword Mars, halogen cycle, water cycle, photochemistry, Cl isotopes
Related Publication Bellucci J.J., Whitehouse M.J., John T., Nemchin A.A., Snape J.F., Bland P.A., Benedix G.K. (2017): Halogen and Cl isotopic systematics in Martian phosphates: Implications for the Cl cycle and surface halogen reservoirs on Mars. Earth Planet. Sci. Lett., 458, 192-202
Notes TRR 170 publication no. 07. NordSIMS publication no. 477.
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1-s2.0-S0012821X16305854-mmc01.tab
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11 Variables, 99 Observations UNF:6:fK1yjupGfONUkhKtIfun7Q==
MMC 1. Supplementary Tables: Raw Cl isotopic measurements for standards and unknowns over two analytical sessions.
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Fig. 6. Schematic diagram of the Cl cycle on Mars proposed here. Recent basalts erupt with phosphates with a δ37Cl of −0.6‰, which is representative of the bulk Martian mantle. When on or near the surface, these phosphates interact with halogen rich brines that have incorporated isotopically fractionated Cl, which occurred by photochemistry in the atmosphere (a minimum of −55 to a maximum of +5‰, Jackson et al., 2010) or the soil (which would have a similar composition). The perchlorate on the Martian surface that is likely incorporated into the Martian brines has a δ37Cl of −55 to −1‰ (Farley et al., 2016).
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Fig. 5. Standard mixing calculation with a 80 μg/g initial phosphate Cl concentration with an isotope composition of δ37Cl of −0.6, the average of SaU 005, NWA 4864, Zagami, and Tissint (Table 1) and a crustal Cl concentration of 5000 μg/g (Keller et al., 2006). Positive mixing end member δ37Cl is a hypothetical +5‰, which is seen as the maximum perchlorate δ37Cl value on Earth (Jackson et al., 2010) and negative δ37Cl of −14‰, the most negative perchlorate value on Earth (Jackson et al., 2010) and ranging to −51‰, which has been measured in Gale crater (Farley et al., 2016).
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Fig. 4. X-ray maps of Si, P, Cl, and Ca for a clast phosphate in NWA7533 indicating hydrothermal replacement of phosphate by silica rich veins.
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Fig. 3. Electron microprobe x-ray maps of P, Cl, and F in phosphates from LAR12011 (A, B), Tissint (C), NWA7533 (D), and ALH84001 (E). Scale bar units are counts. Clear zonation in the halogens is apparent in LAR12011 and NWA7533. This zone of enrichment in LAR12011 corresponds with increasingly negative δ37Cl (−3‰ vs. −6‰). Additional x-ray maps for other grains and for elements Si, Fe, and Ca available in Supplementary Materials.
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Fig. 2. Halogen ratios (Cl/I, Cl/Br, and ClF) vs. halogen concentrations (in μg/g). The gray field is defined by SaU 005, NWA 4864, Zagami, and Tissint, which show no secondary features in microprobe mapping or major element concentrations (McCubbin et al., 2016). The Nakhla veins field in Cl/Br vs. Br is from Rao et al., 2005, while the trend for Meridiani rocks measured by the Opportunity lander is from Rao et al., 2009. The bulk nakhlite measurements are from Cartwright et al., 2013.
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Fig. 1. Halogen concentrations in μg/g vs. δ37Cl. The box heights and widths represent both range in both halogen concentrations and δ37Cl, respectively. Uncertainties are smaller than the boxes. The gray band represents the Earth's mantle δ37Cl compositions (Sharp et al., 2007, Sharp et al., 2013) and the red band represents measurements of Martian meteorite δ37Cl isotopic compositions by previous workers (Sharp et al., 2016). The red and gray bands do not indicate ranges in halogen concentrations for the Martian or terrestrial mantle. (For interpretation of the references to color in this figure legend, the reader is referred to the web version of this article.)
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