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Understanding the Chemistry of the Rocks at Jezero crater, Mars, through the Combined Use of SuperCam Spectroscopic and Optical Techniques
  • +23
  • Juan Manuel Madariaga,
  • Roger Wiens,
  • Gorka Arana,
  • Violaine Sautter,
  • Karim Benzerara,
  • Arya Udry,
  • Olivier Beyssac,
  • Lucia Mandon,
  • Olivier Gasnault,
  • Jeffrey Johnson,
  • Ann Ollila,
  • Kepa Castro,
  • Agnes Cousin,
  • Sylvestre Maurice,
  • Samuel Clegg,
  • Ryan Anderson,
  • Tanja Bosak,
  • Pierre Beck,
  • Thierry Fouchet,
  • Svetlana Shkolyar,
  • Edward Cloutis,
  • Cathy Quantin-Nataf,
  • Imanol Torre Fernandez,
  • Clément Royer,
  • Chip Legett,
  • Paolo Pilleri
Juan Manuel Madariaga
University of the Basque Country, University of the Basque Country, University of the Basque Country

Corresponding Author:[email protected]

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Roger Wiens
Los Alamos National Laboratory, Los Alamos National Laboratory, Los Alamos National Laboratory
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Gorka Arana
Universidad del País Vasco / Euskal Herriko Unibertsitatea, Universidad del País Vasco / Euskal Herriko Unibertsitatea, Universidad del País Vasco / Euskal Herriko Unibertsitatea
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Violaine Sautter
MNHN National Museum of Natural History Paris, MNHN National Museum of Natural History Paris, MNHN National Museum of Natural History Paris
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Karim Benzerara
Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, UPMC / CNRS / MNHN / IRD, Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, UPMC / CNRS / MNHN / IRD, Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, UPMC / CNRS / MNHN / IRD
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Arya Udry
University of Nevada Las Vegas, University of Nevada Las Vegas, University of Nevada Las Vegas
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Olivier Beyssac
IMPMC Institut de Minéralogie et de Physique des Milieux Condensés, IMPMC Institut de Minéralogie et de Physique des Milieux Condensés, IMPMC Institut de Minéralogie et de Physique des Milieux Condensés
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Lucia Mandon
LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris
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Olivier Gasnault
IRAP, CNRS, Université de Toulouse, UPS-OMP, IRAP, CNRS, Université de Toulouse, UPS-OMP, IRAP, CNRS, Université de Toulouse, UPS-OMP
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Jeffrey Johnson
Johns Hopkins University Applied Physics Laboratory, Johns Hopkins University Applied Physics Laboratory, Johns Hopkins University Applied Physics Laboratory
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Ann Ollila
Los Alamos National Laboratory, Los Alamos National Laboratory, Los Alamos National Laboratory
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Kepa Castro
Universidad del País Vasco / Euskal Herriko Unibertsitatea, Universidad del País Vasco / Euskal Herriko Unibertsitatea, Universidad del País Vasco / Euskal Herriko Unibertsitatea
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Agnes Cousin
Institut de Recherche en Astrophysique et Planétologie (IRAP), Institut de Recherche en Astrophysique et Planétologie (IRAP), Institut de Recherche en Astrophysique et Planétologie (IRAP)
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Sylvestre Maurice
IRAP, CNRS, Université de Toulouse, UPS-OMP, IRAP, CNRS, Université de Toulouse, UPS-OMP, IRAP, CNRS, Université de Toulouse, UPS-OMP
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Samuel Clegg
Los Alamos National Laboratory, Los Alamos National Laboratory, Los Alamos National Laboratory
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Ryan Anderson
United States Geological Survey, United States Geological Survey, United States Geological Survey
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Tanja Bosak
MIT, Earth, Atmospheric and Planetary Sciences, MIT, Earth, Atmospheric and Planetary Sciences, MIT, Earth, Atmospheric and Planetary Sciences
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Pierre Beck
University Joseph Fourier Grenoble, University Joseph Fourier Grenoble, University Joseph Fourier Grenoble
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Thierry Fouchet
LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris
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Svetlana Shkolyar
ASU, ASU, ASU
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Edward Cloutis
University of Winnipeg, University of Winnipeg, University of Winnipeg
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Cathy Quantin-Nataf
Université de Lyon, UCBL, ENSL, CNRS, LGL-TPE, Université de Lyon, UCBL, ENSL, CNRS, LGL-TPE, Université de Lyon, UCBL, ENSL, CNRS, LGL-TPE
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Imanol Torre Fernandez
Universidad del País Vasco / Euskal Herriko Unibertsitatea, Universidad del País Vasco / Euskal Herriko Unibertsitatea, Universidad del País Vasco / Euskal Herriko Unibertsitatea
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Clément Royer
LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris
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Chip Legett
Los Alamos National Laboratory, Los Alamos National Laboratory, Los Alamos National Laboratory
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Paolo Pilleri
IRAP, CNRS, Université de Toulouse, UPS-OMP, IRAP, CNRS, Université de Toulouse, UPS-OMP, IRAP, CNRS, Université de Toulouse, UPS-OMP
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Abstract

The SuperCam instrument onboard Perseverance rover has remote imaging (RMI), VISIR, LIBS, Raman and Time-Resolved Luminescence (TRL) capabilities. RMI images of the rocks at the Octavia Butler landing site have revealed important granular texture diversities. VISIR raster point observations have revealed important differences in the 2.10-2.50 µm infrared range (metal-hydroxides); many include water features at 1.40±0.04 and 1.92±0.02 µm [1]. LIBS observations on the same points analyzed by VISIR revealed important differences in the concentrations of major elements, suggesting mineral grain sizes larger than the laser beam (300-500 µm). LIBS and VISIR show coherent results in some rock surfaces that are consistent with an oxy-hydroxide (e.g., ferrihydrite) [1]. LIBS elemental compositions are consistent with pyroxenes, feldspars, and more often feldspar-like glass, often enriched in silica. Olivine compositions [1, 2] have been observed so far in LIBS data (up to Sol 140) exclusively in rounded regolith pebbles. They have not yet been observed in the rocks themselves, which are MgO-poor compared to regolith and are consistent with FeO bearing pyroxenes (e.g., hedenbergite, ferrosilite). A 3x3 LIBS and VISIR raster (9x9 mm) acquired on a low-standing rock on sol 90 exemplifies these finding. A dark L-shaped filled void sampled by points 1 and 2 with possible ferrihydrite (H seen in LIBS and VISIR spectra). Point 5 contains abundant silica and alkali elements but is Al-depleted relative to feldspars, consistent with dacitic glass composition. Point 7 has TiO2 content consistent with ilmenite. Comparisons to (igneous) Martian meteorites are potentially useful, e.g. [3], to explain the presence of several minerals, although most Martian meteorites are olivine-rich, e.g., more mafic than the rocks at the landing site. In summary, the bedrock at Octavia Butler landing site can be interpreted as showing evidence for relatively coarse-grained weathered pyroxenes, iron and titanium oxides and feldspars, while the local soil contains pebbles from a different source (richer in MgO) incorporating olivine grains. References: [1] Mandon et al. 2021 Fall AGU, New Orleans, LA, 13-17 Dec. ; [2] Beyssac et al. 2021 Fall AGU, New Orleans, LA, 13-17 Dec. ; [3] Garcia-Florentino et al.(2021), Talanta, 224, 121863.