^1,5,6Seann J. MCKIBBIN,^1,7Lidia PITTARELLO,¹Christina MAKARONA,^2,3
Christopher HAMANN,^2,3Lutz HECHT,^4,8Stepan M. CHERNONOZHKIN,¹Steven GODERIS,¹Philippe CLAEYS
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13392]
¹Analytical, Environmental and Geo-Chemistry, Vrije Universiteit Brussel, Pleinlaan 2, Brussels 1050, Belgium
²Museum fur Naturkunde, Leibniz-Institut fur Evolutions- und Biodiversitatsforschung, Invalidenstraße 43,
10115 Berlin, Germany
³Institut fur Geologische Wissenschaften, Freie Universitat Berlin, Malteserstraße 74-100, 12249 Berlin, Germany
⁴GeoRessources, Faculte des Sciences et Technologies, Universite de Lorraine, Rue Jacques Callot, BP 70239, 54506,
Vandoeuvre-les-Nancy CEDEX, France
⁵Present address: Institut f€ur Erd- und Umweltwissenschaften, Universitat Potsdam, Haus 27, Karl-Liebknecht-Straße 24-25,
Potsdam-Golm 14476, Germany
⁶Present address: Geowissenschaftliches Zentrum, Abteilung Isotopengeologie, Georg-August-Universitat Göttingen,
Goldschmidtstraße 1, Göttingen 37073, Germany
⁷Present address: Department of Lithospheric Research, Universit€at Wien, UZA 2, Althanstraße 14, Vienna A-1090,Austria
⁸Department of Chemistry, Universiteit Gent, Krijgslaan 281-S12, Ghent 9000, BelgiumPresent address: Department of Chemistry, Universiteit Gent, Krijgslaan 281-S12, Ghent 9000, Belgium
Published by arrangement with John Wiley & Sons

Main group pallasite meteorites are samples of a single early magmatic planetesimal, dominated by metal and olivine but containing accessory chromite, sulfide, phosphide, phosphates, and rare phosphoran olivine. They represent mixtures of core and mantle materials, but the environment of formation is poorly understood, with a quiescent core–mantle boundary, violent core–mantle mixture, or surface mixture all recently suggested. Here, we review main group pallasite data sets and petrologic characteristics, and present new observations on the low‐MnO pallasite Brahin that contains abundant fragmental olivine, but also rounded and angular olivine and potential evidence of sulfide–phosphide liquid immiscibility. A reassessment of the literature shows that low‐MnO and high‐FeO subgroups preferentially host rounded olivine and low‐temperature P₂O₅‐rich phases such as the Mg‐phosphate farringtonite and phosphoran olivine. These phases form after metal and silicate reservoirs back‐react during decreasing temperature after initial separation, resulting in oxidation of phosphorus and chromium. Farringtonite and phosphoran olivine have not been found in the common subgroup PMG, which are mechanical mixtures of olivine, chromite with moderate Al₂O₃ contents, primitive solid metal, and evolved liquid metal. Lower concentrations of Mn in olivine of the low‐MnO PMG subgroup, and high concentrations of Mn in low‐Al₂O₃ chromites, trace the development and escape of sulfide‐rich melt in pallasites and the partially chalcophile behavior for Mn in this environment. Pallasites with rounded olivine indicate that the core–mantle boundary of their planetesimal may not be a simple interface but rather a volume in which interactions between metal, silicate, and other components occur.

¹Hoppe, P.,^2,4,5,6Pignatari, M.,³Amari, S.
Springer Proceedings in Physics 219, 373-376 Link to Article [DOI: 10.1007/978-3-030-13876-9_68]
¹Max Planck Institute for Chemistry, Hahn-Meitner-Weg 1, Mainz, 55128, Germany
²E. A. Milne Centre for Astrophysics, University of Hull, Hull, HU6 7RX, United Kingdom
³McDonnell Center for the Space Sciences and Physics Department, Washington University, St. Louis, MO 63130, United States
⁴NuGrid Collaboration, East Lansing, United States
⁵JINA-CEE, East Lansing, United States
⁶Konkoly Observatory, Konkoly Thege Miklos ut 15-17, Budapest, 1121, Hungary

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¹E. A. MacLagan,^1,2E. L. Walton,¹C. D. K. Herd,¹B. Rivard
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13388]
¹Department of Earth and Atmospheric Sciences, University of Alberta, 1-26 Earth Sciences Building, Edmonton, Alberta T6G 2E3, Canada
²Department of Physical Sciences, MacEwan University, City Centre Campus, 10700 104 Ave, Edmonton, Alberta T5J 4S2, Canada
Published by Arrangement with John Wiley and Sons

Hyperspectral imaging can be used to rapidly identify and map the spatial
distributions of many minerals. Here, hyperspectral mapping in three wavelength regions(visible and near-infrared, shortwave infrared, and thermal infrared) was applied to drill cores (ST001, ST002, and ST003) penetrating a continuous sequence of crater-fill breccias from the Steen River impact structure in Alberta, Canada. The combined data sets reveal distinct mineralogical layering, with breccias derived predominantly from sedimentary rocks overlying those derived from granitic basement. This stratigraphy demonstrates that the
breccias were not appreciably disturbed following deposition, which is inconsistent with formation models of similar breccias (suevites) by explosive impact melt–fluid interaction. At Steen River, volatiles from sedimentary target rocks were an inherent part of forming these enigmatic breccias. Approximately three quarters of terrestrial impact structures contain sedimentary target rocks; therefore, the role of volatiles in producing so-called
suevitic breccias may be more widespread than previously realized. The hyperspectral maps, specifically within the SWIR wavelength region, also delineate minerals associated with postimpact hydrothermal activity, including ammoniated clay and feldspar minerals not detectable using traditional techniques. These nitrogen-bearing minerals may have originated from microbial processes, associated with oil- and gas-producing units in the
crater vicinity. Such minerals may have important implications for the production of habitable environments by impact-induced hydrothermal activity on Earth and Mars.

¹B.L. Carrier,¹W.J. Abbey,¹L.W. Beegle,¹R. Bhartia,¹Y. Liu
Journal of Geophysical Research, Planets (in Press) Link to Article [https://doi.org/10.1029/2018JE005758]
¹Jet Propulsion Laboratory, California Institute of Technology
Published by arrangement with John Wiley & Sons

The effects of radiation on the survivability of key biosignatures are a driving factor in exploration strategies throughout the solar system. Ultraviolet (UV) radiation, especially shorter wavelength UVC radiation, is known to be damaging to organisms and to potential organic biosignatures; however the interaction of UV radiation with minerals and rocks is not well understood. Constraining the survivability of organics and generation of habitable zones requires assessment of physical parameters such as penetration depth of UV photons. This type of information helps to identify to what extent rocks and minerals can provide effective shielding against UV radiation and is especially important on Mars where the surface chemistry is more oxidizing and the radiation environment is more extreme than on Earth. Using pressed pellets of natural gypsum, kaolinite, Mars simulant basalt and welded tuff, we measured the spectral transmittance of each in the wavelength range of 220‐400 nm. Although transmittance drops off quickly with depth, detectable levels of UV can penetrate >500 μm in each material. Each substrate allowed higher transmittance of UVC radiation than of longer wavelength UVA/B radiation, possibly as a result of surface reflectance and internal scattering properties. This could result in increased subsurface photolysis of organic compounds and biosignatures. We have used the transmittance data collected herein to constrain the lifetimes of several organic molecules in the Martian subsurface. These results will also have implications for organic analyses to be conducted by Mars 2020, and could be used to better constrain the SHERLOC/Mars 2020 interrogation volume.

¹Makino, Y.,²Kuroki, Y.,¹Hirata, T.
Journal of Analytical Atomic Spectroscopy 34, 1794-1799 Link to Article [DOI: 10.1039/c9ja00181f]
¹Geochemistry Research Center, School of Science, University of Tokyo Hongo, Tokyo, 113-0033, Japan
²Thermo Fisher Scientific K.K., Tokyo, 108-0023, Japan

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¹McLoughlin, N.,¹Grosch, E.G.,^2,3Vullum, P.E., ⁴Guagliardo, P.,^4,5Saunders, M.,⁴Wacey, D.
Geobiology (in Press) Link to Article [DOI: 10.1111/gbi.12361]
¹Department of Geology, Rhodes University, Grahamstown, South Africa
²SINTEF Materials and Chemistry, Trondheim, Norway
³Department of Physics, Norwegian University of Science and Technology (NTNU), Trondheim, Norway
⁴Centre for Microscopy Characterisation and Analysis, The University of Western Australia, Perth, WA, Australia
⁵School of Molecular Sciences, The University of Western Australia, Perth, WA, Australia

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¹Bramble, M.S.,^1,2Yang, Y.,³Patterson, W.R., III,¹Milliken, R.E.,¹Mustard, J.F.,^4,5Donaldson Hanna, K.L.
Review of Scientific Instruments 90, 093101 Link to Article [DOI: 10.1063/1.5096363]
¹Department of Earth, Environmental, and Planetary Sciences, Brown University, Providence, RI 02912, United States
²Planetary Science Institute, School of Earth Sciences, China University of Geosciences, Wuhan, 430074, China
³School of Engineering, Brown University, Providence, RI 02912, United States
⁴Atmospheric, Oceanic, and Planetary Physics, University of Oxford, Oxford, OX1 3PU, United Kingdom
⁵Department of Physics, University of Central Florida, Orlando, FL 32816, United States

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¹Lees, T.C.,²Murphy, F.C.,³Tomkins, A.G.,⁴ O’Donohue, D.
Economic Geology 114, 427-439 Link to Article [DOI: 10.5382/econgeo.4639]
¹Fathom Geological Consulting Pty Ltd., 999 Nepean Highway, Melbourne, VIC 3189, Australia
²Fractore Pty Ltd., 2/2 Brinsley Road, Melbourne, VIC 3124, Australia
³School of Earth, Atmosphere and Environment, Monash University, Melbourne, VIC 3800, Australia
⁴New Century Resources Ltd., Level 4, 360 Collins Street, Melbourne, VIC 3000, Australia

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¹d’Ischia, M.,²Manini, P.,^3,4Moracci, M.,⁵Saladino, R.,^6,7Ball, V.,⁸Thissen, H.,⁸Evans, R.A.,⁹Puzzarini, C.,¹⁰Barone, V.
International Journal of Molecular Sciences 20 Link to Article [DOI: 10.3390/ijms20174079]
¹Department of Chemical Sciences, University of Naples “Federico II”, Complesso Universitario di Monte S. Angelo ,Via Cupa Nuova Cinthia 21, Naples, 80126, Italy
²Department of Chemical Sciences, University of Naples “Federico II”, Complesso Universitario di Monte S. Angelo ,Via Cupa Nuova Cinthia 21, Naples, 80126, Italy
³Department of Biology, University of Naples “Federico II”, Complesso Universitario di Monte S. Angelo ,Via Cupa Nuova Cinthia 21, Naples, 80126, Italy
⁴Institute of Biosciences and BioResources, National Research Council of Italy, Via P. Castellino 111, Naples, 80131, Italy
⁵Department of Ecological and Biological Sciences, University of Tuscia, Via S. Camillo de Lellis, Viterbo, 01100, Italy
⁶Institut National de la Santé et de la RechercheMédicale, 11 rue Humann, France
⁷Faculté de Chirurgie Dentaire, Université de Strasbourg, 1 Place de l’Hôpital, Strasbourg, 67000, France
⁸Commonwealth Scientific and Industrial Research Organisation (CSIRO) Manufacturing, Clayton, VIC 3168, Australia
⁹Department of Chemistry “Giacomo Ciamician”, University of Bologna, Via F. Selmi 2, Bologna, I-40126, Italy
¹⁰Scuola Normale Superiore, Piazza dei Cavalieri 7, Pisa, I-56126, Italy

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¹Christian VOLLMER,²Jan LEITNER,^3,4Demie KEPAPTSOGLOU,^3,5Quentin M. RAMASSE,⁶Henner BUSEMANN,¹Peter HOPPE
Meteoritics and Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13389]
¹Institut für Mineralogie, Westfalische Wilhelms-Universität, Corrensstr. 24, 48149 Münster, Germany
²Particle Chemistry Department, Max Planck Institute for Chemistry, Hahn-Meitner-Weg 1, 55128 Mainz, Germany
³SuperSTEM Laboratory, Keckwick Lane, Daresbury, UK
⁴Department of Physics, Jeol Nanocentre, University of York, Heslington YO 10 50D, UK
⁵School of Chemical and Process Engineering, Scbool of Physics, University of Leeds, Leeds LS2 9JT, UK
⁶Institut für Geochemie und Petrologie, ETH Zürich, Clausiusstr. 25, Zürich, Switzerland
Copyright Elsevier

Organic matter (OM) was widespread in the early solar nebula and might have played an important role for the delivery of prebiotic molecules to the early Earth. We investigated the textures, isotopic compositions, and functional chemistries of organic grains in the Renazzo carbonaceous chondrite by combined high spatial resolution techniques (electron microscopy–secondary ion mass spectrometry). Morphologies are complex on a submicrometer scale, and some organics exhibit a distinct texture with alternating layers of OM and minerals. These layered organics are also characterized by heterogeneous 15N isotopic abundances. Functional chemistry investigations of five focused ion beam‐extracted lamellae by electron energy loss spectroscopy reveal a chemical complexity on a nanometer scale. Grains show absorption at the C‐K edge at 285, 286.6, 287, and 288.6 eV due to polyaromatic hydrocarbons, different carbon‐oxygen, and aliphatic bonding environments with varying intensity. The nitrogen K‐edge functional chemistry of three grains is shown to be highly complex, and we see indications of amine (C‐NHx) or amide (CO‐NR2) chemistry as well as possible N‐heterocycles and nitro groups. We also performed low‐loss vibrational spectroscopy with high energy resolution and identified possible D‐ and G‐bands known from Raman spectroscopy and/or absorption from C=C and C‐O stretch modes known from infrared spectroscopy at around 0.17 and 0.2 eV energy loss. The observation of multiglobular layered organic aggregates, heterogeneous 15N‐anomalous compositions, and indication of NHx‐(amine) functional chemistry lends support to recent ideas that 15N‐enriched ammonia (NH3) was a powerful agent to synthesize more complex organics in aqueous asteroidal environments.