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Jakubek RS, Bhartia R, Uckert K, Asher SA, Czaja AD, Fries MD, Hand K, Haney NC, Razzell Hollis J, Minitti M, Sharma SK, Sharma S, Siljeström S. Calibration of Raman Bandwidths on the Scanning Habitable Environments with Raman and Luminescence for Organics and Chemicals (SHERLOC) Deep Ultraviolet Raman and Fluorescence Instrument Aboard the Perseverance Rover. Appl Spectrosc 2023:37028231210885. [PMID: 37964538 DOI: 10.1177/00037028231210885] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2023]
Abstract
In this work, we derive a simple method for calibrating Raman bandwidths for the Scanning Habitable Environments with Raman and Luminescence for Organics and Chemicals (SHERLOC) instrument onboard NASA's Perseverance rover. Raman bandwidths and shapes reported by an instrument contain contributions from both the intrinsic Raman band (IRB) and instrumental artifacts. To directly correlate bandwidth to sample properties and to compare bandwidths across instruments, the IRB width needs to be separated from instrumental effects. Here, we use the ubiquitous bandwidth calibration method of modeling the observed Raman bands as a convolution of a Lorentzian IRB and a Gaussian instrument slit function. Using calibration target data, we calculate that SHERLOC has a slit function width of 34.1 cm-1. With a measure of the instrument slit function, we can deconvolve the IRB from the observed band, providing the width of the Raman band unobscured by instrumental artifact. We present the correlation between observed Raman bandwidth and intrinsic Raman bandwidth in table form for the quick estimation of SHERLOC Raman intrinsic bandwidths. We discuss the limitations of using this model to calibrate Raman bandwidth and derive a quantitative method for calculating the errors associated with the calibration. We demonstrate the utility of this method of bandwidth calibration by examining the intrinsic bandwidths of SHERLOC sulfate spectra and by modeling the SHERLOC spectrum of olivine.
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Affiliation(s)
| | - Rohit Bhartia
- Photon Systems Incorporated, Covina, California, USA
| | - Kyle Uckert
- Jet Propulsion Laboratory, California Institution of Technology, Pasadena, California, USA
| | - Sanford A Asher
- Department of Chemistry, University of Pittsburgh, Pittsburgh, Pennsylvania, USA
| | - Andrew D Czaja
- Department of Geology, University of Cincinnati, Cincinnati, Ohio, USA
| | | | - Kevin Hand
- Jet Propulsion Laboratory, California Institution of Technology, Pasadena, California, USA
| | | | | | | | - Shiv K Sharma
- Hawaii Institute of Geophysics and Planetology, University of Hawaii, Honolulu, Hawaii, USA
| | - Sunanda Sharma
- Jet Propulsion Laboratory, California Institution of Technology, Pasadena, California, USA
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2
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Miner KR, Hollis JR, Miller CE, Uckert K, Douglas TA, Cardarelli E, Mackelprang R. Earth to Mars: A Protocol for Characterizing Permafrost in the Context of Climate Change as an Analog for Extraplanetary Exploration. Astrobiology 2023; 23:1006-1018. [PMID: 37566539 PMCID: PMC10510695 DOI: 10.1089/ast.2022.0155] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/08/2022] [Accepted: 07/02/2023] [Indexed: 08/13/2023]
Abstract
Abstract Permafrost is important from an exobiology and climate change perspective. It serves as an analog for extraplanetary exploration, and it threatens to emit globally significant amounts of greenhouse gases as it thaws due to climate change. Viable microbes survive in Earth's permafrost, slowly metabolizing and transforming organic matter through geologic time. Ancient permafrost microbial communities represent a crucial resource for gaining novel insights into survival strategies adopted by extremotolerant organisms in extraplanetary analogs. We present a proof-of-concept study on ∼22 Kya permafrost to determine the potential for coupling Raman and fluorescence biosignature detection technology from the NASA Mars Perseverance rover with microbial community characterization in frozen soils, which could be expanded to other Earth and off-Earth locations. Besides the well-known utility for biosignature detection and identification, our results indicate that spectral mapping of permafrost could be used to rapidly characterize organic carbon characteristics. Coupled with microbial community analyses, this method has the potential to enhance our understanding of carbon degradation and emissions in thawing permafrost. Further, spectroscopy can be accomplished in situ to mitigate sample transport challenges and in assessing and prioritizing frozen soils for further investigation. This method has broad-range applicability to understanding microbial communities and their associations with biosignatures and soil carbon and mineralogic characteristics relevant to climate science and astrobiology.
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Affiliation(s)
- Kimberley R. Miner
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | | | - Charles E. Miller
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | - Kyle Uckert
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | | | - Emily Cardarelli
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
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3
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Sharma S, Roppel RD, Murphy AE, Beegle LW, Bhartia R, Steele A, Hollis JR, Siljeström S, McCubbin FM, Asher SA, Abbey WJ, Allwood AC, Berger EL, Bleefeld BL, Burton AS, Bykov SV, Cardarelli EL, Conrad PG, Corpolongo A, Czaja AD, DeFlores LP, Edgett K, Farley KA, Fornaro T, Fox AC, Fries MD, Harker D, Hickman-Lewis K, Huggett J, Imbeah S, Jakubek RS, Kah LC, Lee C, Liu Y, Magee A, Minitti M, Moore KR, Pascuzzo A, Rodriguez Sanchez-Vahamonde C, Scheller EL, Shkolyar S, Stack KM, Steadman K, Tuite M, Uckert K, Werynski A, Wiens RC, Williams AJ, Winchell K, Kennedy MR, Yanchilina A. Diverse organic-mineral associations in Jezero crater, Mars. Nature 2023; 619:724-732. [PMID: 37438522 PMCID: PMC10371864 DOI: 10.1038/s41586-023-06143-z] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/07/2022] [Accepted: 04/27/2023] [Indexed: 07/14/2023]
Abstract
The presence and distribution of preserved organic matter on the surface of Mars can provide key information about the Martian carbon cycle and the potential of the planet to host life throughout its history. Several types of organic molecules have been previously detected in Martian meteorites1 and at Gale crater, Mars2-4. Evaluating the diversity and detectability of organic matter elsewhere on Mars is important for understanding the extent and diversity of Martian surface processes and the potential availability of carbon sources1,5,6. Here we report the detection of Raman and fluorescence spectra consistent with several species of aromatic organic molecules in the Máaz and Séítah formations within the Crater Floor sequences of Jezero crater, Mars. We report specific fluorescence-mineral associations consistent with many classes of organic molecules occurring in different spatial patterns within these compositionally distinct formations, potentially indicating different fates of carbon across environments. Our findings suggest there may be a diversity of aromatic molecules prevalent on the Martian surface, and these materials persist despite exposure to surface conditions. These potential organic molecules are largely found within minerals linked to aqueous processes, indicating that these processes may have had a key role in organic synthesis, transport or preservation.
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Affiliation(s)
- Sunanda Sharma
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA.
| | - Ryan D Roppel
- Department of Chemistry, University of Pittsburgh, Pittsburgh, PA, USA
| | | | | | | | - Andrew Steele
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, USA
| | | | - Sandra Siljeström
- Department of Methodology, Textiles and Medical Technology, RISE Research Institutes of Sweden, Stockholm, Sweden
| | - Francis M McCubbin
- Astromaterials Research and Exploration Science Division, NASA Johnson Space Center, Houston, TX, USA
| | - Sanford A Asher
- Department of Chemistry, University of Pittsburgh, Pittsburgh, PA, USA
| | - William J Abbey
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Abigail C Allwood
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Eve L Berger
- Astromaterials Research and Exploration Science Division, NASA Johnson Space Center, Houston, TX, USA
- Texas State University, Houston, TX, USA
- Jacobs JETS II, Houston, TX, USA
| | | | - Aaron S Burton
- Astromaterials Research and Exploration Science Division, NASA Johnson Space Center, Houston, TX, USA
| | - Sergei V Bykov
- Department of Chemistry, University of Pittsburgh, Pittsburgh, PA, USA
| | - Emily L Cardarelli
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Pamela G Conrad
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, USA
| | - Andrea Corpolongo
- Department of Geosciences, University of Cincinnati, Cincinnati, OH, USA
| | - Andrew D Czaja
- Department of Geosciences, University of Cincinnati, Cincinnati, OH, USA
| | - Lauren P DeFlores
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | | | - Kenneth A Farley
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
| | - Teresa Fornaro
- Astrophysical Observatory of Arcetri, INAF, Florence, Italy
| | - Allison C Fox
- Astromaterials Research and Exploration Science Division, NASA Johnson Space Center, Houston, TX, USA
- Texas State University, Houston, TX, USA
- Jacobs JETS II, Houston, TX, USA
| | - Marc D Fries
- Astromaterials Research and Exploration Science Division, NASA Johnson Space Center, Houston, TX, USA
| | - David Harker
- Malin Space Science Systems, Inc., San Diego, CA, USA
| | | | | | - Samara Imbeah
- Malin Space Science Systems, Inc., San Diego, CA, USA
| | - Ryan S Jakubek
- Astromaterials Research and Exploration Science Division, NASA Johnson Space Center, Houston, TX, USA
- Jacobs JETS II, Houston, TX, USA
| | - Linda C Kah
- Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN, USA
| | - Carina Lee
- Astromaterials Research and Exploration Science Division, NASA Johnson Space Center, Houston, TX, USA
- Texas State University, Houston, TX, USA
- Jacobs JETS II, Houston, TX, USA
| | - Yang Liu
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Angela Magee
- Malin Space Science Systems, Inc., San Diego, CA, USA
| | | | - Kelsey R Moore
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
| | | | | | - Eva L Scheller
- Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - Svetlana Shkolyar
- Department of Astronomy, University of Maryland, College Park, MD, USA
- Planetary Geology, Geophysics and Geochemistry Lab, NASA Goddard Space Flight Center, Greenbelt, MD, USA
- Blue Marble Space Institute of Science, Seattle, WA, USA
| | - Kathryn M Stack
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Kim Steadman
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Michael Tuite
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Kyle Uckert
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | | | - Roger C Wiens
- Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, Lafayette, IN, USA
| | - Amy J Williams
- Department of Geological Sciences, University of Florida, Gainesville, FL, USA
| | - Katherine Winchell
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
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4
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Razzell Hollis J, Sharma S, Abbey W, Bhartia R, Beegle L, Fries M, Hein JD, Monacelli B, Nordman AD. A Deep Ultraviolet Raman and Fluorescence Spectral Library of 51 Organic Compounds for the SHERLOC Instrument Onboard Mars 2020. Astrobiology 2023; 23:1-23. [PMID: 36367974 PMCID: PMC9810352 DOI: 10.1089/ast.2022.0023] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 02/15/2022] [Accepted: 08/01/2022] [Indexed: 06/16/2023]
Abstract
We report deep ultraviolet (DUV) Raman and Fluorescence spectra obtained on a SHERLOC (Scanning Habitable Environments with Raman and Luminescence for Organics and Chemicals) analog instrument for 51 pure organic compounds, including 5 carboxylic acids, 10 polycyclic aromatic hydrocarbons, 24 amino acids, 6 nucleobases, and 6 different grades of macromolecular carbon from humic acid to graphite. Organic mixtures were not investigated. We discuss how the DUV fluorescence and Raman spectra exhibited by different organic compounds allow for detection, classification, and identification of organics by SHERLOC. We find that 1- and 2-ring aromatic compounds produce detectable fluorescence within SHERLOC's spectral range (250-355 nm), but fluorescence spectra are not unique enough to enable easy identification of particular compounds. However, both aromatic and aliphatic compounds can be identified by their Raman spectra, with the number of Raman peaks and their positions being highly specific to chemical structure, within SHERLOC's reported spectral uncertainty of ±5 cm-1. For compounds that are not in the Library, classification is possible by comparing the general number and position of dominant Raman peaks with trends for different kinds of organic compounds.
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Affiliation(s)
- Joseph Razzell Hollis
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
- Department of Life Sciences, The Natural History Museum, London, United Kingdom
| | - Sunanda Sharma
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | - William Abbey
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | | | - Luther Beegle
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | - Marc Fries
- NASA Johnson Space Center, Houston, Texas, USA
| | - Jeffrey D. Hein
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | - Brian Monacelli
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | - Austin D. Nordman
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
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5
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Scheller EL, Razzell Hollis J, Cardarelli EL, Steele A, Beegle LW, Bhartia R, Conrad P, Uckert K, Sharma S, Ehlmann BL, Abbey WJ, Asher SA, Benison KC, Berger EL, Beyssac O, Bleefeld BL, Bosak T, Brown AJ, Burton AS, Bykov SV, Cloutis E, Fairén AG, DeFlores L, Farley KA, Fey DM, Fornaro T, Fox AC, Fries M, Hickman-Lewis K, Hug WF, Huggett JE, Imbeah S, Jakubek RS, Kah LC, Kelemen P, Kennedy MR, Kizovski T, Lee C, Liu Y, Mandon L, McCubbin FM, Moore KR, Nixon BE, Núñez JI, Rodriguez Sanchez-Vahamonde C, Roppel RD, Schulte M, Sephton MA, Sharma SK, Siljeström S, Shkolyar S, Shuster DL, Simon JI, Smith RJ, Stack KM, Steadman K, Weiss BP, Werynski A, Williams AJ, Wiens RC, Williford KH, Winchell K, Wogsland B, Yanchilina A, Yingling R, Zorzano MP. Aqueous alteration processes in Jezero crater, Mars-implications for organic geochemistry. Science 2022; 378:1105-1110. [PMID: 36417498 DOI: 10.1126/science.abo5204] [Citation(s) in RCA: 9] [Impact Index Per Article: 4.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/24/2022]
Abstract
The Perseverance rover landed in Jezero crater, Mars, in February 2021. We used the Scanning Habitable Environments with Raman and Luminescence for Organics and Chemicals (SHERLOC) instrument to perform deep-ultraviolet Raman and fluorescence spectroscopy of three rocks within the crater. We identify evidence for two distinct ancient aqueous environments at different times. Reactions with liquid water formed carbonates in an olivine-rich igneous rock. A sulfate-perchlorate mixture is present in the rocks, which probably formed by later modifications of the rocks by brine. Fluorescence signatures consistent with aromatic organic compounds occur throughout these rocks and are preserved in minerals related to both aqueous environments.
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Affiliation(s)
- Eva L Scheller
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA.,Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - Joseph Razzell Hollis
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA.,The Natural History Museum, London, UK
| | - Emily L Cardarelli
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Andrew Steele
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, USA
| | - Luther W Beegle
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | | | - Pamela Conrad
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, USA
| | - Kyle Uckert
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Sunanda Sharma
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Bethany L Ehlmann
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA.,NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - William J Abbey
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Sanford A Asher
- Department of Chemistry, University of Pittsburgh, Pittsburgh, PA, USA
| | - Kathleen C Benison
- Department of Geology and Geography, West Virginia University, Morgantown, WV, USA
| | - Eve L Berger
- Texas State University, San Marcos, TX, USA.,Jacobs Johnson Space Center Engineering, Technology and Science Contract, Houston, TX, USA.,NASA Johnson Space Center, Houston, TX, USA
| | - Olivier Beyssac
- Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, Centre National de la Recherche Scientifique, Sorbonne Université, Muséum National d'Histoire Naturelle, 75005 Paris, France
| | | | - Tanja Bosak
- Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA
| | | | | | - Sergei V Bykov
- Department of Chemistry, University of Pittsburgh, Pittsburgh, PA, USA
| | - Ed Cloutis
- Geography, The University of Winnipeg, Winnipeg, MB, Canada
| | - Alberto G Fairén
- Centro de Astrobiología, Consejo Superior de Investigaciones Cientificas-Instituto Nacional de Tecnica Aeroespacial, Madrid, Spain.,Department of Astronomy, Cornell University, Ithaca, NY, USA
| | - Lauren DeFlores
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Kenneth A Farley
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
| | | | - Teresa Fornaro
- Astrophysical Observatory of Arcetri, Istituto Nazionale di Astrofisica, Florence, Italy
| | | | - Marc Fries
- NASA Johnson Space Center, Houston, TX, USA
| | - Keyron Hickman-Lewis
- Department of Earth Sciences, The Natural History Museum, London, UK.,Dipartimento di Scienze Biologiche, Geologiche e Ambientali, Università di Bologna, Bologna, Italy
| | | | | | | | | | - Linda C Kah
- Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN, USA
| | - Peter Kelemen
- Lamont Doherty Earth Observatory, Columbia University, Palisades, NY, USA
| | | | - Tanya Kizovski
- Department of Earth Sciences, Brock University, St. Catharines, ON L2S 3A1, Canada
| | - Carina Lee
- Lunar and Planetary Institute, Universities Space Research Association, Houston, TX, USA
| | - Yang Liu
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Lucia Mandon
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, Centre National de la Recherche Scientifique, Sorbonne Université, Université Paris Diderot, 92195 Meudon, France
| | | | - Kelsey R Moore
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | | | - Jorge I Núñez
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | | | - Ryan D Roppel
- Department of Chemistry, University of Pittsburgh, Pittsburgh, PA, USA
| | - Mitchell Schulte
- Mars Exploration Program, NASA Headquarters, Washington, DC, USA
| | - Mark A Sephton
- Earth Science and Engineering, South Kensington Campus, Imperial College London, SW7 2AZ London, UK
| | - Shiv K Sharma
- Hawaii Institute of Geophysics and Planetology, University of Hawaii at Manoa, Honolulu, HI, USA
| | | | - Svetlana Shkolyar
- Department of Astronomy, University of Maryland, College Park, MD, USA.,NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - David L Shuster
- Earth and Planetary Science, University of California Berkeley, Berkeley, CA, USA
| | | | - Rebecca J Smith
- Department of Geosciences, Stony Brook University, Stony Brook, NY, USA
| | - Kathryn M Stack
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Kim Steadman
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Benjamin P Weiss
- Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA
| | | | - Amy J Williams
- Department of Geological Sciences, University of Florida, Gainesville, FL, USA
| | - Roger C Wiens
- Los Alamos National Laboratory, Los Alamos, NM, USA.,Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA
| | - Kenneth H Williford
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA.,Blue Marble Space Institute of Science, Seattle, WA, USA
| | | | - Brittan Wogsland
- Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN, USA
| | | | | | - Maria-Paz Zorzano
- Centro de Astrobiología, Consejo Superior de Investigaciones Cientificas-Instituto Nacional de Tecnica Aeroespacial, Madrid, Spain
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6
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Uckert K, Bhartia R, Beegle LW, Monacelli B, Asher SA, Burton AS, Bykov SV, Davis K, Fries MD, Jakubek RS, Hollis JR, Roppel RD, Wu YH. Calibration of the SHERLOC Deep Ultraviolet Fluorescence-Raman Spectrometer on the Perseverance Rover. Appl Spectrosc 2021; 75:763-773. [PMID: 33876994 DOI: 10.1177/00037028211013368] [Citation(s) in RCA: 6] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
We describe the wavelength calibration of the spectrometer for the scanning of habitable environments with Raman and luminescence for organics and chemicals (SHERLOC) instrument onboard NASA's Perseverance Rover. SHERLOC utilizes deep ultraviolet Raman and fluorescence (DUV R/F) spectroscopy to enable analysis of samples from the Martian surface. SHERLOC employs a 248.6 nm deep ultraviolet laser to generate Raman-scattered photons and native fluorescence emission photons from near-surface material to detect and classify chemical and mineralogical compositions. The collected photons are focused on a charge-coupled device and the data are returned to Earth for analysis. The compact DUV R/F spectrometer has a spectral range from 249.9 nm to 353.6 nm (∼200 cm-1 to 12 000 cm-1) (with a spectral resolution of 0.296 nm (∼40 cm-1)). The compact spectrometer uses a custom design to project a high-resolution Raman spectrum and a low-resolution fluorescence spectrum on a single charge-coupled device. The natural spectral separation enabled by deep ultraviolet excitation enables wavelength separation of the Raman/fluorescence spectra. The SHERLOC spectrometer was designed to optimize the resolution of the Raman spectral region and the wavelength range of the fluorescence region. The resulting illumination on the charge-coupled device is curved, requiring a segmented, nonlinear wavelength calibration in order to understand the mineralogy and chemistry of Martian materials.
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Affiliation(s)
- Kyle Uckert
- Jet Propulsion Laboratory California Institution of Technology, Pasadena, CA, USA
| | | | - Luther W Beegle
- Jet Propulsion Laboratory California Institution of Technology, Pasadena, CA, USA
| | - Brian Monacelli
- Jet Propulsion Laboratory California Institution of Technology, Pasadena, CA, USA
| | - Sanford A Asher
- University of Pittsburgh Chemistry Department, Pittsburgh, PA, USA
| | | | - Sergei V Bykov
- University of Pittsburgh Chemistry Department, Pittsburgh, PA, USA
| | | | - Marc D Fries
- 43834NASA Johnson Space Center, Houston, TX, USA
| | | | | | - Ryan D Roppel
- University of Pittsburgh Chemistry Department, Pittsburgh, PA, USA
| | - Yen-Hung Wu
- Jet Propulsion Laboratory California Institution of Technology, Pasadena, CA, USA
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7
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Razzell Hollis J, Fornaro T, Rapin W, Wade J, Vicente-Retortillo Á, Steele A, Bhartia R, Beegle LW. Detection and Degradation of Adenosine Monophosphate in Perchlorate-Spiked Martian Regolith Analog, by Deep-Ultraviolet Spectroscopy. Astrobiology 2021; 21:511-525. [PMID: 33493410 DOI: 10.1089/ast.2020.2362] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
The search for organic biosignatures on Mars will depend on finding material protected from the destructive ambient radiation. Solar ultraviolet can induce photochemical degradation of organic compounds, but certain clays have been shown to preserve organic material. We examine how the SHERLOC instrument on the upcoming Mars 2020 mission will use deep-ultraviolet (UV) (248.6 nm) Raman and fluorescence spectroscopy to detect a plausible biosignature of adenosine 5'-monophosphate (AMP) adsorbed onto Ca-montmorillonite clay. We found that the spectral signature of AMP is not altered by adsorption in the clay matrix but does change with prolonged exposure to the UV laser over dosages equivalent to 0.2-6 sols of ambient martian UV. For pure AMP, UV exposure leads to breaking of the aromatic adenine unit, but in the presence of clay the degradation is limited to minor alteration with new Raman peaks and increased fluorescence consistent with formation of 2-hydroxyadenosine, while 1 wt % Mg perchlorate increases the rate of degradation. Our results confirm that clays are effective preservers of organic material and should be considered high-value targets, but that pristine biosignatures may be altered within 1 sol of martian UV exposure, with implications for Mars 2020 science operations and sample caching.
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Affiliation(s)
- Joseph Razzell Hollis
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | - Teresa Fornaro
- Carnegie Institution for Science, Washington, District of Columbia, USA
- INAF-Astrophysical Observatory of Arcetri, Florence, Italy
| | - William Rapin
- Department of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA
- Sorbonne Université, IMPMC, CNRS, Paris, France
| | - Jessica Wade
- Department of Physics, Imperial College London, London, United Kingdom
| | - Álvaro Vicente-Retortillo
- Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan, USA
- Centro de Astrobiología (CSIC-INTA), Torrejón de Ardoz, Spain
| | - Andrew Steele
- Carnegie Institution for Science, Washington, District of Columbia, USA
| | | | - Luther W Beegle
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
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8
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Abstract
Raman spectroscopy is an invaluable technique for identifying compounds by the unique pattern of their molecular vibrations and is capable of quantifying the individual concentrations of those compounds provided that certain parameters about the sample and instrument are known. We demonstrate the development of an optical model to describe the intensity distribution of incident laser photons as they pass through the sample volume, determine the limitations of that volume that may be detected by the spectrometer optics, and account for light absorption by molecules within the sample in order to predict the total Raman intensity that would be obtained from a given, uniform sample such as an aqueous solution. We show that the interplay between the shape and divergence of the laser beam, the position of the focal plane, and the dimensions of the spectrometer slit are essential to explaining experimentally observed trends in deep ultraviolet Raman intensities obtained from both planar and volumetric samples, including highly oriented pyrolytic graphite and binary mixtures of organic nucleotides. This model offers the capability to predict detection limits for organic compounds in different matrices based on the parameters of the spectrometer, and to define the upper/lower limits within which concentration can be reliably determined from Raman intensity for such samples. We discuss the potential to quantify more complex samples, including as solid phase mixtures of organics and minerals, that are investigated by the unique instrument parameters of the Scanning Habitable Environments with Raman and Luminescence for Organics and Chemicals (SHERLOC) investigation on the upcoming Mars 2020 rover mission.
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Affiliation(s)
| | - David Rheingold
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, USA
| | - Rohit Bhartia
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, USA
| | - Luther W Beegle
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, USA
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Sapers HM, Razzell Hollis J, Bhartia R, Beegle LW, Orphan VJ, Amend JP. The Cell and the Sum of Its Parts: Patterns of Complexity in Biosignatures as Revealed by Deep UV Raman Spectroscopy. Front Microbiol 2019; 10:679. [PMID: 31156562 PMCID: PMC6527968 DOI: 10.3389/fmicb.2019.00679] [Citation(s) in RCA: 10] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/18/2018] [Accepted: 03/18/2019] [Indexed: 01/27/2023] Open
Abstract
The next NASA-led Mars mission (Mars 2020) will carry a suite of instrumentation dedicated to investigating Martian history and the in situ detection of potential biosignatures. SHERLOC, a deep UV Raman/Fluorescence spectrometer has the ability to detect and map the distribution of many organic compounds, including the aromatic molecules that are fundamental building blocks of life on Earth, at concentrations down to 1 ppm. The mere presence of organic compounds is not a biosignature: there is widespread distribution of reduced organic molecules in the Solar System. Life utilizes a select few of these molecules creating conspicuous enrichments of specific molecules that deviate from the distribution expected from purely abiotic processes. The detection of far from equilibrium concentrations of a specific subset of organic molecules, such as those uniquely enriched by biological processes, would comprise a universal biosignature independent of specific terrestrial biochemistry. The detectability and suitability of a small subset of organic molecules to adequately describe a living system is explored using the bacterium Escherichia coli as a model organism. The DUV Raman spectra of E. coli cells are dominated by the vibrational modes of the nucleobases adenine, guanine, cytosine, and thymine, and the aromatic amino acids tyrosine, tryptophan, and phenylalanine. We demonstrate that not only does the deep ultraviolet (DUV) Raman spectrum of E. coli reflect a distinct concentration of specific organic molecules, but that a sufficient molecular complexity is required to deconvolute the cellular spectrum. Furthermore, a linear combination of the DUV resonant compounds is insufficient to fully describe the cellular spectrum. The residual in the cellular spectrum indicates that DUV Raman spectroscopy enables differentiating between the presence of biomolecules and the complex uniquely biological organization and arrangements of these molecules in living systems. This study demonstrates the ability of DUV Raman spectroscopy to interrogate a complex biological system represented in a living cell, and differentiate between organic detection and a series of Raman features that derive from the molecular complexity inherent to life constituting a biosignature.
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Affiliation(s)
- Haley M. Sapers
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, United States
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, United States
- Department of Earth Sciences, University of Southern California, Los Angeles, CA, United States
| | - Joseph Razzell Hollis
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, United States
| | - Rohit Bhartia
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, United States
| | - Luther W. Beegle
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, United States
| | - Victoria J. Orphan
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, United States
| | - Jan P. Amend
- Department of Earth Sciences, University of Southern California, Los Angeles, CA, United States
- Department of Biological Sciences, University of Southern California, Los Angeles, CA, United States
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Hellmann C, Treat ND, Scaccabarozzi AD, Razzell Hollis J, Fleischli FD, Bannock JH, de Mello J, Michels JJ, Kim JS, Stingelin N. Solution processing of polymer semiconductor: Insulator blends-Tailored optical properties through liquid-liquid phase separation control. ACTA ACUST UNITED AC 2014. [DOI: 10.1002/polb.23656] [Citation(s) in RCA: 23] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Affiliation(s)
- Christoph Hellmann
- Department of Materials and Centre for Plastic Electronics; Imperial College London; London SW7 2AZ United Kingdom
| | - Neil D. Treat
- Department of Materials and Centre for Plastic Electronics; Imperial College London; London SW7 2AZ United Kingdom
| | - Alberto D. Scaccabarozzi
- Department of Materials and Centre for Plastic Electronics; Imperial College London; London SW7 2AZ United Kingdom
| | - Joseph Razzell Hollis
- Department of Physics and Centre for Plastic Electronics; Imperial College London; London SW7 2AZ United Kingdom
| | - Franziska D. Fleischli
- Department of Materials and Centre for Plastic Electronics; Imperial College London; London SW7 2AZ United Kingdom
| | - James H. Bannock
- Department of Chemistry and Centre for Plastic Electronics; Imperial College London; London SW7 2AZ United Kingdom
| | - John de Mello
- Department of Chemistry and Centre for Plastic Electronics; Imperial College London; London SW7 2AZ United Kingdom
| | - Jasper J. Michels
- Max Planck Institute for Polymer Research; Ackermannweg 10 55128 Mainz Germany
| | - Ji-Seon Kim
- Department of Physics and Centre for Plastic Electronics; Imperial College London; London SW7 2AZ United Kingdom
| | - Natalie Stingelin
- Department of Materials and Centre for Plastic Electronics; Imperial College London; London SW7 2AZ United Kingdom
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