Post-landing major element quantification using SuperCam laser induced breakdown spectroscopy
- Creators
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Anderson, Ryan B.
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Forni, Olivier
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Cousin, Agnes
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Wiens, Roger C.
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Clegg, Samuel M.
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Frydenvang, Jens
- Gabriel, Travis S. J.
- Ollila, Ann
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Schröder, Susanne
- Beyssac, Olivier
- Gibbons, Erin
- Vogt, David S.
- Clavé, Elise
- Manrique, Jose-Antonio
- Legett, Carey
- Pilleri, Paolo
- Newell, Raymond T.
- Sarrao, Joseph
- Maurice, Sylvestre
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Arana, Gorka
- Benzerara, Karim
- Bernardi, Pernelle
- Bernard, Sylvain
- Bousquet, Bruno
- Brown, Adrian J.
- Alvarez-Llamas, César
- Chide, Baptiste
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Cloutis, Edward
- Comellas, Jade
- Connell, Stephanie
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Dehouck, Erwin
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Delapp, Dorothea M.
- Essunfeld, Ari
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Fabre, Cécile
- Fouchet, Thierry
- Garcia-Florentino, Cristina
- García-Gómez, Laura
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Gasda, Patrick J.
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Gasnault, Olivier
- Hausrath, Elisabeth M.
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Lanza, Nina L.
- Laserna, Javier
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Lasue, Jeremie
- Lopez, Guillermo
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Madariaga, Juan Manuel
- Mandon, Lucia
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Mangold, Nicolas
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Meslin, Pierre-Yves
- Nelson, Anthony E.
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Newsom, Horton
- Reyes-Newell, Adriana L.
- Robinson, Scott
- Rull, Fernando
- Sharma, Shiv
- Simon, Justin I.
- Sobron, Pablo
- Torre Fernandez, Imanol
- Udry, Arya
- Venhaus, Dawn
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McLennan, Scott M.
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Morris, Richard V.
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Ehlmann, Bethany
Abstract
The SuperCam instrument on the Perseverance Mars 2020 rover uses a pulsed 1064 nm laser to ablate targets at a distance and conduct laser induced breakdown spectroscopy (LIBS) by analyzing the light from the resulting plasma. SuperCam LIBS spectra are preprocessed to remove ambient light, noise, and the continuum signal present in LIBS observations. Prior to quantification, spectra are masked to remove noisier spectrometer regions and spectra are normalized to minimize signal fluctuations and effects of target distance. In some cases, the spectra are also standardized or binned prior to quantification. To determine quantitative elemental compositions of diverse geologic materials at Jezero crater, Mars, we use a suite of 1198 laboratory spectra of 334 well-characterized reference samples. The samples were selected to span a wide range of compositions and include typical silicate rocks, pure minerals (e.g., silicates, sulfates, carbonates, oxides), more unusual compositions (e.g., Mn ore and sodalite), and replicates of the sintered SuperCam calibration targets (SCCTs) onboard the rover. For each major element (SiO₂, TiO₂, Al₂O₃, FeO_T, MgO, CaO, Na₂O, K₂O), the database was subdivided into five "folds" with similar distributions of the element of interest. One fold was held out as an independent test set, and the remaining four folds were used to optimize multivariate regression models relating the spectrum to the composition. We considered a variety of models, and selected several for further investigation for each element, based primarily on the root mean squared error of prediction (RMSEP) on the test set, when analyzed at 3 m. In cases with several models of comparable performance at 3 m, we incorporated the SCCT performance at different distances to choose the preferred model. Shortly after landing on Mars and collecting initial spectra of geologic targets, we selected one model per element. Subsequently, with additional data from geologic targets, some models were revised to ensure results that are more consistent with geochemical constraints. The calibration discussed here is a snapshot of an ongoing effort to deliver the most accurate chemical compositions with SuperCam LIBS.
Additional Information
Published by Elsevier. Received 12 November 2021, Revised 14 December 2021, Accepted 15 December 2021, Available online 24 December 2021, Version of Record 21 January 2022. This project was supported in the United States by the NASA Mars Exploration Program and in France by CNES, CNRS, and local universities. Support in Spain was provided by the Ministerio de Ciencia e Innovación. Support in Germany was provided by DLR. SuperCam benefitted from LANL laboratory-directed research and development funding which provided early prototypes of the new technologies incorporated in the SuperCam BU. JF acknowledges the support from the Carlsberg Foundation. EC acknowledges funding from the Canadian Space Agency, the Natural Sciences and Engineering Research Council of Canada, the Canada Foundation for Innovation, the Manitoba Research Innovation Fund and the University of Winnipeg. Any use of trade, firm, or product names is for descriptive purposes only and does not imply endorsement by the U.S. Government. We have no known conflicts of interest to report.Attached Files
Published - 1-s2.0-S0584854721003049-main.pdf
Supplemental Material - 1-s2.0-S0584854721003049-mmc1.csv
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Additional details
- Eprint ID
- 115331
- Resolver ID
- CaltechAUTHORS:20220705-346579000
- NASA
- Centre National d'Études Spatiales (CNES)
- Centre National de la Recherche Scientifique (CNRS)
- Ministerio de Ciencia e Innovación (MICINN)
- Deutsches Zentrum für Luft- und Raumfahrt (DLR)
- Los Alamos National Laboratory
- Carlsberg Foundation
- Canadian Space Agency (CSA)
- Natural Sciences and Engineering Research Council of Canada (NSERC)
- Canada Foundation for Innovation
- Manitoba Research and Innovation Fund
- University of Winnipeg
- Created
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2022-07-08Created from EPrint's datestamp field
- Updated
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2022-07-25Created from EPrint's last_modified field
- Caltech groups
- Division of Geological and Planetary Sciences