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Wu T, Zhang X, Chen X, Liu W, Han Y, Zhong Y, Zhao D, Fang Z, Pan L, Wang F, Xu H. Simulation Research and Analysis of Wavelength Modulation Off-Axis Integrated Cavity Output Spectrum Measurement System. SENSORS (BASEL, SWITZERLAND) 2025; 25:2478. [PMID: 40285167 PMCID: PMC12031079 DOI: 10.3390/s25082478] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 03/12/2025] [Revised: 04/09/2025] [Accepted: 04/12/2025] [Indexed: 04/29/2025]
Abstract
Wavelength modulation spectroscopy off-axis integrated cavity output spectroscopy (WMS-OA-ICOS) is an in situ detection technique suitable for analyzing trace gases in the atmospheres, characterized by its high sensitivity and ease of integration. However, in current practical applications, the design and optimization of WMS-OA-ICOS systems primarily rely on empirical knowledge, lacking systematic quantitative methodologies. To address this limitation, this study conducts comprehensive modeling and simulation research on WMS-OA-ICOS spectroscopy, proposing a novel modeling approach. The spot distribution simulation results obtained from the self-developed model are validated against those generated using Tracepro. Furthermore, based on the self-developed model, an in-depth investigation is conducted into the effects of cavity length tolerance, beam waist matching, modulation depth, and laser linewidth on signal quality. The findings provide valuable insights for designing and optimizing miniaturized systems with high signal-to-noise ratios.
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Affiliation(s)
- Tao Wu
- Deep Space Exploration Laboratory, Hefei 230000, China
- National Key Laboratory of Deep Space Exploration, Hefei 230000, China
| | - Xiao Zhang
- Deep Space Exploration Laboratory, Hefei 230000, China
- National Key Laboratory of Deep Space Exploration, Hefei 230000, China
| | - Xiao Chen
- Deep Space Exploration Laboratory, Hefei 230000, China
- National Key Laboratory of Deep Space Exploration, Hefei 230000, China
| | - Wangwang Liu
- Deep Space Exploration Laboratory, Hefei 230000, China
- National Key Laboratory of Deep Space Exploration, Hefei 230000, China
| | - Yan Han
- Deep Space Exploration Laboratory, Hefei 230000, China
- National Key Laboratory of Deep Space Exploration, Hefei 230000, China
| | - Yubin Zhong
- Deep Space Exploration Laboratory, Hefei 230000, China
- National Key Laboratory of Deep Space Exploration, Hefei 230000, China
| | - Dan Zhao
- Deep Space Exploration Laboratory, Hefei 230000, China
- National Key Laboratory of Deep Space Exploration, Hefei 230000, China
| | - Zhen Fang
- Deep Space Exploration Laboratory, Hefei 230000, China
- National Key Laboratory of Deep Space Exploration, Hefei 230000, China
| | - Linxin Pan
- Deep Space Exploration Laboratory, Hefei 230000, China
- National Key Laboratory of Deep Space Exploration, Hefei 230000, China
| | - Feiyang Wang
- Deep Space Exploration Laboratory, Hefei 230000, China
- National Key Laboratory of Deep Space Exploration, Hefei 230000, China
| | - Hang Xu
- Deep Space Exploration Laboratory, Hefei 230000, China
- National Key Laboratory of Deep Space Exploration, Hefei 230000, China
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Egea-González I, McKay CP, Hallsworth JE, Jiménez-Díaz A, Ruiz J. Ammonia or Methanol Would Enable Subsurface Liquid Water at the Martian South Pole. ASTROBIOLOGY 2025; 25:201-208. [PMID: 39960810 DOI: 10.1089/ast.2024.0075] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 03/21/2025]
Abstract
The notion of liquid water beneath the ice layer at the south polar layered deposits (SPLD) of Mars is an interesting possibility given the implications for astrobiology and possible human habitation. A body of liquid water located at a depth of 1.5 km has been inferred from radar data in the South Polar Cap. However, the high temperatures that would facilitate the existence of liquid water or brine at that depth are not consistent with estimations of heat flow that are based on the lithosphere's flexure. Attempts to reconcile both issues have been inconclusive or otherwise unsuccessful. Here, we analyze the possible role(s) of subsurface ammonia and/or methanol in maintaining water in a liquid state at subsurface temperatures that are compatible with the lithosphere strength. Our results indicate that the presence of these compounds at the base of the SPLD can reconcile the existence of liquid water with previous estimations of surface heat flow.
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Affiliation(s)
- Isabel Egea-González
- Departamento de Física Aplicada, Escuela Superior de Ingeniería, Universidad de Cádiz, Cádiz, Spain
| | - Christopher P McKay
- Space Science Division, NASA Ames Research Center, Moffett Field, California, USA
| | - John E Hallsworth
- Institute for Global Food Security, School of Biological Sciences, Medical Biology Centre, Queen's University Belfast, Belfast, UK
| | - Alberto Jiménez-Díaz
- Departamento de Biología y Geología, Física y Química Inorgánica, ESCET, Universidad Rey Juan Carlos, Madrid, Spain
| | - Javier Ruiz
- Departamento de Geodinámica, Estratigrafía y Paleontología; Facultad de Ciencias Geológicas, Universidad Complutense de Madrid, Madrid, Spain
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3
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Butturini A, Benaiges-Fernandez R, Fors O, García-Castellanos D. Potential Habitability of Present-Day Martian Subsurface for Earth-Like Methanogens. ASTROBIOLOGY 2025; 25:253-268. [PMID: 40047175 DOI: 10.1089/ast.2024.0100] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 03/21/2025]
Abstract
The intense debate about the presence of methane in the martian atmosphere has stimulated the study of methanogenic species that are adapted to terrestrial habitats that resemble martian environments. We examined the environmental conditions, energy sources, and ecology of terrestrial methanogens that thrive in deep crystalline fractures, subsea hypersaline lakes, and subglacial water bodies, considered analogs of a hypothetical habitable martian subsurface. We combined this information with recent data on the distribution of buried water/ice and radiogenic elements on Mars, and with models of the subsurface thermal regime of this planet, we identified a 4.3-8.8 km-deep regolith habitat at the midlatitude location of Acidalia Planitia that might fit the requirements for hosting putative martian methanogens analogous to the methanogenic families, Methanosarcinaceae and Methanomicrobiaceae.
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Affiliation(s)
- A Butturini
- Departament de Biologia Evolutiva, Ecologia y Ciències Ambientals, Universitat de Barcelona, Barcelona, Spain
| | - R Benaiges-Fernandez
- Departament de Genètica, Microbiologia i Estadística, Universitat de Barcelona, Barcelona, Spain
| | - O Fors
- Departament de Física Quàntica i Astrofísica, Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona, Barcelona, Spain
| | - D García-Castellanos
- Geosciences Barcelona (GEO3BCN), Consejo Superior de Investigaciones Científicas (CSIC), Barcelona, Spain
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4
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Harris RL, Schuerger AC. Hydrogenotrophic methanogenesis at 7-12 mbar by Methanosarcina barkeri under simulated martian atmospheric conditions. Sci Rep 2025; 15:2880. [PMID: 39843490 PMCID: PMC11754898 DOI: 10.1038/s41598-025-86145-1] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/01/2024] [Accepted: 01/08/2025] [Indexed: 01/24/2025] Open
Abstract
Mars, with its ancient history of long-lived habitable environments, continues to captivate researchers exploring the potential for extant life. This study investigates the biosignature potential of Martian methane by assessing the viability of hydrogenotrophic methanogenesis in Methanosarcina barkeri MS under simulated Martian surface conditions. We expose M. barkeri to sustained hypobaria (7-12 mbar), low temperature (0˚C), and a CO2-dominated gas mixture mimicking the Martian atmosphere. The results demonstrate statistically quantifiable CH4 production under all tested conditions, including at 7-12 mbar. Transcriptomics reveal that low total pressure and temperature did not significantly impact gene expression, highlighting the resilience of M. barkeri. However, atmospheric gas composition, specifically Mars gas with 2.9% pH2, led to significant down-regulation of methanogenesis genes, hindering growth over 14 days. Notably, CH4 production scaled with the partial pressure of H2, revealing that hydrogen uptake affinity is a stronger predictor of habitability and methanogenic potential than favorable Gibbs free energy of reaction. Our findings suggest that Mars' subsurface could harbor habitable refugia capable of supporting methanogenesis, sustaining microbial life at low metabolic steady states. These insights challenge assumptions about Martian habitability and have implications for astrobiological exploration, planetary protection, and in situ resource utilization for future human missions.
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Affiliation(s)
- Rachel L Harris
- Department of Organismic and Evolutionary Biology, Harvard University, Cambridge, MA, 02138, USA.
- NASA Postdoctoral Management Program Fellow, Astrobiology Program, NASA Headquarters, Washington, DC, 20546, USA.
| | - Andrew C Schuerger
- Department of Plant Pathology, Space Life Sciences Lab, University of Florida, 505 Odyssey Way, Exploration Park,, Merritt Island, FL, 32953, USA.
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5
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Grady MM. Constraining the history of water and climate on Mars through light element stable isotope analysis of volatiles in returned martian samples. Proc Natl Acad Sci U S A 2025; 122:e2404260121. [PMID: 39761390 PMCID: PMC11745331 DOI: 10.1073/pnas.2404260121] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/24/2024] [Accepted: 11/12/2024] [Indexed: 01/23/2025] Open
Abstract
Much has been learned about Mars through data returned from space missions and analyses of martian meteorites. There are, however, many questions still outstanding which cannot currently be answered-including the issue of whether there is, or was, life on Mars. The return of a cache of samples-including of the atmosphere-from separate locations in Jezero Crater and with differing petrogeneses will provide the international community with the opportunity to explore part of the evolutionary history of Mars in great detail. Specifically, measurements of the isotopic compositions of the light elements H, C, N, O, Cl, and S can be used to follow how volatile species cycle through the different martian volatile reservoirs (atmosphere, lithosphere, cryosphere, and hydrosphere). Measurement of isotopic fractionation enables inference of the environmental conditions (e.g., temperature, water/rock ratio) under which fractionation occurred. Knowing the contextual relationship of the materials to their geological settings, coupled with precise compositional measurements will enable a more thorough understanding of martian volatile history and allow a picture to be constructed of water and climate on Mars as represented at Jezero Crater.
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Affiliation(s)
- Monica M. Grady
- School of Physical Sciences, The Open University, Milton KeynesMK7 6AA, United Kingdom
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6
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Swindle TD, Pack A, Schwenzer SP, Young ED. The value of returning a sample of the Martian atmosphere. Proc Natl Acad Sci U S A 2025; 122:e2404258121. [PMID: 39761392 PMCID: PMC11745387 DOI: 10.1073/pnas.2404258121] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 01/23/2025] Open
Abstract
The elemental and isotopic abundances of major species in the Martian atmosphere have been determined, but analyses often lack sufficient precision, and those of minor and trace species are frequently not well known. Many important questions about the evolution and current state of Mars require the kind of knowledge that can be gained from analysis of a returned sample of the Martian atmosphere. Key target species include the noble gases, nitrogen, and various species containing carbon, hydrogen, and oxygen, such as methane. More detailed analyses will no doubt provide measurements of other species that will allow insights of their own. These volatiles can constrain the origin of the Martian atmosphere, exchange of volatiles between the surface and interior, polar processes, and (in the case of methane) the possibility of extant biology on Mars.
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Affiliation(s)
| | - Andreas Pack
- Georg-August-Universitāt, Geowissenschaftliches Zentrum, Department of Geochemistry and Isotope Geology, Goldschmidtstraße 1, GöttingenD-37073, Germany
| | - Susanne P. Schwenzer
- AstrobiologyOU, School of Environment, Earth & Ecosystem Sciences, Open University, Milton KeynesMK7 6AA, United Kingdom
| | - Edward D. Young
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, CA90095
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7
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Burtt DG, Stern JC, Webster CR, Hofmann AE, Franz HB, Sutter B, Thorpe MT, Kite ES, Eigenbrode JL, Pavlov AA, House CH, Tutolo BM, Des Marais DJ, Rampe EB, McAdam AC, Malespin CA. Highly enriched carbon and oxygen isotopes in carbonate-derived CO 2 at Gale crater, Mars. Proc Natl Acad Sci U S A 2024; 121:e2321342121. [PMID: 39374395 PMCID: PMC11494307 DOI: 10.1073/pnas.2321342121] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/08/2024] [Accepted: 08/07/2024] [Indexed: 10/09/2024] Open
Abstract
Carbonate minerals are of particular interest in paleoenvironmental research as they are an integral part of the carbon and water cycles, both of which are relevant to habitability. Given that these cycles are less constrained on Mars than they are on Earth, the identification of carbonates has been a point of emphasis for rover missions. Here, we present carbon (δ13C) and oxygen (δ18O) isotope data from four carbonates encountered by the Curiosity rover within the Gale crater. The carbon isotope values range from 72 ± 2‰ to 110 ± 3‰ Vienna Pee Dee Belemnite while the oxygen isotope values span from 59 ± 4‰ to 91 ± 4‰ Vienna Standard Mean Ocean Water (1 SE uncertainties). Notably, these values are isotopically heavy (13C- and 18O-enriched) relative to nearly every other Martian material. The extreme isotopic difference between the carbonates and other carbon- and oxygen-rich reservoirs on Mars cannot be reconciled by standard equilibrium carbonate-CO2 fractionation, thus requiring an alternative process during or prior to carbonate formation. This paper explores two processes capable of contributing to the isotopic enrichments: 1) evaporative-driven Rayleigh distillation and 2) kinetic isotope effects related to cryogenic precipitation. In isolation, each process cannot reproduce the observed carbonate isotope values; however, a combination of these processes represents the most likely source for the extreme isotopic enrichments.
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Affiliation(s)
- David G. Burtt
- NASA Postdoctoral Fellow, Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD20771
| | - Jennifer C. Stern
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD20771
| | | | - Amy E. Hofmann
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA91109
| | - Heather B. Franz
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD20771
| | - Brad Sutter
- Jacobs Technology, Houston, TX77058
- NASA Johnson Space Center, Houston, TX77058
| | - Michael T. Thorpe
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD20771
- University of Maryland/Goddard Space Flight/Center for Research and Exploration in Space and Science Technology (CRESST II), Greenbelt, MD20771
| | - Edwin S. Kite
- Department of Geophysical Sciences, University of Chicago, Chicago, IL60637
| | | | - Alexander A. Pavlov
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD20771
| | - Christopher H. House
- Department of Geosciences, Pennsylvania State University, University Park, PA16802
| | - Benjamin M. Tutolo
- Department of Geoscience, University of Calgary, Calgary, ABT2N 1N4, Canada
| | | | | | - Amy C. McAdam
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD20771
| | - Charles A. Malespin
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD20771
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8
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Cleaves HJ, Hystad G, Prabhu A, Wong ML, Cody GD, Economon S, Hazen RM. A robust, agnostic molecular biosignature based on machine learning. Proc Natl Acad Sci U S A 2023; 120:e2307149120. [PMID: 37748080 PMCID: PMC10576141 DOI: 10.1073/pnas.2307149120] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/29/2023] [Accepted: 07/17/2023] [Indexed: 09/27/2023] Open
Abstract
The search for definitive biosignatures-unambiguous markers of past or present life-is a central goal of paleobiology and astrobiology. We used pyrolysis-gas chromatography coupled to mass spectrometry to analyze chemically disparate samples, including living cells, geologically processed fossil organic material, carbon-rich meteorites, and laboratory-synthesized organic compounds and mixtures. Data from each sample were employed as training and test subsets for machine-learning methods, which resulted in a model that can identify the biogenicity of both contemporary and ancient geologically processed samples with ~90% accuracy. These machine-learning methods do not rely on precise compound identification: Rather, the relational aspects of chromatographic and mass peaks provide the needed information, which underscores this method's utility for detecting alien biology.
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Affiliation(s)
- H. James Cleaves
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC20015
- Earth Life Science Institute, Tokyo Institute of Technology, Tokyo152-8550, Japan
- Blue Marble Space Institute for Science, Seattle, WA98104
| | - Grethe Hystad
- Department of Mathematics and Statistics, Purdue University Northwest, Hammond, IN46323
| | - Anirudh Prabhu
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC20015
| | - Michael L. Wong
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC20015
- Sagan Fellow, NASA Hubble Fellowship Program, Space Telescope Science Institute, Baltimore, MD21218
| | - George D. Cody
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC20015
| | - Sophia Economon
- Department of Earth and Planetary Sciences, Johns Hopkins University, Baltimore, MD21218
| | - Robert M. Hazen
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC20015
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9
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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: 2] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Download PDF] [Figures] [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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10
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Zhou Y, Zhang Z, Li Y, Zhao G, Zhou X, Zhang B, Jiao K, Yan X, Li C, Axner O, Ma W. Self-calibrated NICE-OHMS based on an asymmetric signal: theoretical analysis and experimental validation. OPTICS EXPRESS 2023; 31:27830-27842. [PMID: 37710850 DOI: 10.1364/oe.497862] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/13/2023] [Accepted: 07/26/2023] [Indexed: 09/16/2023]
Abstract
As an ultra-sensitive detection technique, the noise-immune cavity enhanced optical heterodyne molecular spectroscopy (NICE-OHMS) technique has great potential for assessment of the concentration of trace gases. To determine gas concentrations at the ppt or lower level with high accuracy, it is desirable that the technique exhibits self-calibration (or calibration-free) capabilities. Although being sensitive, NICE-OHMS has so far not demonstrated any such ability. To remedy this, this paper provides a self-calibrated realization of NICE-OHMS that is based on a switching of the feedback target of the DeVoe-Brewer (DVB) locking procedure from the modulation frequency of the frequency modulation spectroscopy (FMS) to the cavity length, which creates an asymmetrical signal whose form and size can be used to unambiguously assess the gas concentration. A comprehensive theoretical model for self-calibrated NICE-OHMS is established by analyzing the shift of cavity modes caused by intracavity absorption, demonstrating that gas absorption information can be encoded in both the laser frequency and the NICE-OHMS signal. To experimentally verify the methodology, we measure a series of dispersion signals under different levels of absorbance using a built experimental setup. An instrument factor and the partial pressure are obtained by fitting the measured signal through theoretical expressions. Our results demonstrate that fitted values are more accurate for higher partial pressures than for lower. To improve on the accuracy at low partial pressures, it is shown that the instrument factor obtained by fitting the signal at large partial pressures (in this case, above 7.8 µTorr) can be set to a fixed value for all fits. By this, the partial pressures can be assessed with a relative error below 0.65%. This technique has the potential to enable calibration-free ultra-sensitive gas detection.
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11
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Touchette D, Maggiori C, Altshuler I, Tettenborn A, Bourdages LJ, Magnuson E, Blenner-Hassett O, Raymond-Bouchard I, Ellery A, Whyte LG. Microbial Characterization of Arctic Glacial Ice Cores with a Semiautomated Life Detection System. ASTROBIOLOGY 2023; 23:756-768. [PMID: 37126945 DOI: 10.1089/ast.2022.0130] [Citation(s) in RCA: 2] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/03/2023]
Abstract
The search for extant microbial life will be a major focus of future astrobiology missions; however, no direct extant life detection instrumentation is included in current missions to Mars. In this study, we developed the semiautomated MicroLife detection platform that collects and processes environmental samples, detects biosignatures, and characterizes microbial activity. This platform is composed of a drill for sample collection, a redox dye colorimetric system for microbial metabolic activity detection and assessment (μMAMA [microfluidics Microbial Activity MicroAssay]), and a MinION sequencer for biosignature detection and characterization of microbial communities. The MicroLife platform was field-tested on White Glacier on Axel Heiberg Island in the Canadian high Arctic, with two extracted ice cores. The μMAMA successfully detected microbial metabolism from the ice cores within 1 day of incubation. The MinION sequencing of the ice cores and the positive μMAMA card identified a microbial community consistent with cold and oligotrophic environments. Furthermore, isolation and identification of microbial isolates from the μMAMA card corroborated the MinION sequencing. Together, these analyses support the MicroLife platform's efficacy in identifying microbes natively present in cryoenvironments and detecting their metabolic activity. Given our MicroLife platform's size and low energy requirements, it could be incorporated into a future landed platform or rovers for life detection.
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Affiliation(s)
- David Touchette
- Department of Natural Resource Sciences, McGill University, Sainte-Anne-de-Bellevue, Canada
- McGill Space Institute, Montréal, Canada
- Environmental Engineering Institute, River Ecosystems Laboratory, School of Architecture, Civil and Environmental Engineering, École Polytechnique Fédérale de Lausanne, Lausanne, Switzerland
| | - Catherine Maggiori
- Department of Natural Resource Sciences, McGill University, Sainte-Anne-de-Bellevue, Canada
- McGill Space Institute, Montréal, Canada
| | - Ianina Altshuler
- Department of Natural Resource Sciences, McGill University, Sainte-Anne-de-Bellevue, Canada
- Environmental Engineering Institute, MACE Laboratory, School of Architecture, Civil and Environmental Engineering, École Polytechnique Fédérale de Lausanne, Lausanne, Switzerland
| | - Alex Tettenborn
- Department of Mechanical and Aerospace Engineering, Carleton University, Ottawa, Canada
| | - Louis-Jacques Bourdages
- Department of Natural Resource Sciences, McGill University, Sainte-Anne-de-Bellevue, Canada
- Department of Mechanical Engineering, Faculty of Engineering, McGill University, Montréal, Canada
| | - Elisse Magnuson
- Department of Natural Resource Sciences, McGill University, Sainte-Anne-de-Bellevue, Canada
| | - Olivia Blenner-Hassett
- Department of Natural Resource Sciences, McGill University, Sainte-Anne-de-Bellevue, Canada
- McGill Space Institute, Montréal, Canada
| | - Isabelle Raymond-Bouchard
- Department of Natural Resource Sciences, McGill University, Sainte-Anne-de-Bellevue, Canada
- McGill Space Institute, Montréal, Canada
| | - Alex Ellery
- Department of Mechanical and Aerospace Engineering, Carleton University, Ottawa, Canada
| | - Lyle G Whyte
- Department of Natural Resource Sciences, McGill University, Sainte-Anne-de-Bellevue, Canada
- McGill Space Institute, Montréal, Canada
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12
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O'Brien ÁC, Hallis LJ, Regnault C, Morrison D, Blackburn G, Steele A, Daly L, Tait A, Tremblay MM, Telenko DE, Gunn J, McKay E, Mari N, Salik MA, Ascough P, Toney J, Griffin S, Whitfield P, Lee M. Using Organic Contaminants to Constrain the Terrestrial Journey of the Martian Meteorite Lafayette. ASTROBIOLOGY 2022; 22:1351-1362. [PMID: 36264546 PMCID: PMC9618387 DOI: 10.1089/ast.2021.0180] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 11/04/2021] [Accepted: 09/07/2022] [Indexed: 06/16/2023]
Abstract
A key part of the search for extraterrestrial life is the detection of organic molecules since these molecules form the basis of all living things on Earth. Instrument suites such as SHERLOC (Scanning Habitable Environments with Raman and Luminescence for Organics and Chemicals) onboard the NASA Perseverance rover and the Mars Organic Molecule Analyzer onboard the future ExoMars Rosalind Franklin rover are designed to detect organic molecules at the martian surface. However, size, mass, and power limitations mean that these instrument suites cannot yet match the instrumental capabilities available in Earth-based laboratories. Until Mars Sample Return, the only martian samples available for study on Earth are martian meteorites. This is a collection of largely basaltic igneous rocks that have been exposed to varying degrees of terrestrial contamination. The low organic molecule abundance within igneous rocks and the expectation of terrestrial contamination make the identification of martian organics within these meteorites highly challenging. The Lafayette martian meteorite exhibits little evidence of terrestrial weathering, potentially making it a good candidate for the detection of martian organics despite uncertainties surrounding its fall history. In this study, we used ultrapure solvents to extract organic matter from triplicate samples of Lafayette and analyzed these extracts via hydrophilic interaction liquid chromatography-mass spectrometry (HILIC-MS). Two hundred twenty-four metabolites (organic molecules) were detected in Lafayette at concentrations more than twice those present in the procedural blanks. In addition, a large number of plant-derived metabolites were putatively identified, the presence of which supports the unconfirmed report that Lafayette fell in a semirural location in Indiana. Remarkably, the putative identification of the mycotoxin deoxynivalenol (or vomitoxin), alongside the report that the collector was possibly a student at Purdue University, can be used to identify the most likely fall year as 1919.
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Affiliation(s)
- Áine Clare O'Brien
- School of Geographical and Earth Sciences, University of Glasgow, Lilybank Gardens, Glasgow, UK
- SUERC, University of Glasgow, East Kilbride, UK
| | - Lydia Jane Hallis
- School of Geographical and Earth Sciences, University of Glasgow, Lilybank Gardens, Glasgow, UK
| | - Clement Regnault
- Polyomics, University of Glasgow, Wolfson Wohl Cancer Research Centre, Switchback Rd, Bearsden, Glasgow, UK
| | | | - Gavin Blackburn
- Polyomics, University of Glasgow, Wolfson Wohl Cancer Research Centre, Switchback Rd, Bearsden, Glasgow, UK
| | - Andrew Steele
- Carnegie Planets, Carnegie Science, Washington DC, USA
| | - Luke Daly
- School of Geographical and Earth Sciences, University of Glasgow, Lilybank Gardens, Glasgow, UK
- Australian Centre for Microscopy and Microanalysis, The University of Sydney, Sydney, Australia
- Department of Materials, University of Oxford, Oxford, UK
| | - Alastair Tait
- School of Earth, Atmosphere & Environment Monash University, Rainforest Walk Clayton, Victoria, Australia
| | - Marissa Marie Tremblay
- Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, Indiana, USA
| | - Darcy E.P. Telenko
- Department of Botany and Plant Pathology, Purdue University, West Lafayette, Indiana, USA
| | - Jacqueline Gunn
- School of Professional Services, Glasgow Caledonian University, Cowcaddens Road, Glasgow, UK
| | | | - Nicola Mari
- Dipartimento di Scienze della Terra e dell'Ambiente, University of Pavia, Pavia, Italy
| | - Mohammad Ali Salik
- School of Geographical and Earth Sciences, University of Glasgow, Lilybank Gardens, Glasgow, UK
| | | | - Jaime Toney
- School of Geographical and Earth Sciences, University of Glasgow, Lilybank Gardens, Glasgow, UK
| | - Sammy Griffin
- School of Geographical and Earth Sciences, University of Glasgow, Lilybank Gardens, Glasgow, UK
| | - Phil Whitfield
- Polyomics, University of Glasgow, Wolfson Wohl Cancer Research Centre, Switchback Rd, Bearsden, Glasgow, UK
| | - Martin Lee
- School of Geographical and Earth Sciences, University of Glasgow, Lilybank Gardens, Glasgow, UK
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13
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Taguchi K, Gilbert A, Sherwood Lollar B, Giunta T, Boreham CJ, Liu Q, Horita J, Ueno Y. Low 13C- 13C abundances in abiotic ethane. Nat Commun 2022; 13:5790. [PMID: 36184637 PMCID: PMC9527245 DOI: 10.1038/s41467-022-33538-9] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/24/2022] [Accepted: 09/22/2022] [Indexed: 11/09/2022] Open
Abstract
Distinguishing biotic compounds from abiotic ones is important in resource geology, biogeochemistry, and the search for life in the universe. Stable isotopes have traditionally been used to discriminate the origins of organic materials, with particular focus on hydrocarbons. However, despite extensive efforts, unequivocal distinction of abiotic hydrocarbons remains challenging. Recent development of clumped-isotope analysis provides more robust information because it is independent of the stable isotopic composition of the starting material. Here, we report data from a 13C-13C clumped-isotope analysis of ethane and demonstrate that the abiotically-synthesized ethane shows distinctively low 13C-13C abundances compared to thermogenic ethane. A collision frequency model predicts the observed low 13C-13C abundances (anti-clumping) in ethane produced from methyl radical recombination. In contrast, thermogenic ethane presumably exhibits near stochastic 13C-13C distribution inherited from the biological precursor, which undergoes C-C bond cleavage/recombination during metabolism. Further, we find an exceptionally high 13C-13C signature in ethane remaining after microbial oxidation. In summary, the approach distinguishes between thermogenic, microbially altered, and abiotic hydrocarbons. The 13C-13C signature can provide an important step forward for discrimination of the origin of organic molecules on Earth and in extra-terrestrial environments.
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Affiliation(s)
- Koudai Taguchi
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Meguro, Tokyo, 152-8551, Japan.
| | - Alexis Gilbert
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Meguro, Tokyo, 152-8551, Japan. .,Earth-Life Science Institute (WPI-ELSI), Tokyo Institute of Technology, Meguro, Tokyo, 152-8550, Japan.
| | - Barbara Sherwood Lollar
- Department of Earth Sciences, University of Toronto, Toronto, ON, M5S 3B1, Canada.,Institut de physique du globe de Paris (IPGP), Université Paris Cité, Paris, France
| | - Thomas Giunta
- Department of Earth Sciences, University of Toronto, Toronto, ON, M5S 3B1, Canada.,Univ Brest, CNRS, Ifremer, Geo-Ocean, F-29280, Plouzané, France
| | | | - Qi Liu
- State Key Laboratory of Ore Deposit Geochemistry, Institute of Geochemistry, Chinese Academy of Sciences, Guiyang, 550081, China
| | - Juske Horita
- Department of Geosciences, Texas Tech University, Lubbock, TX, 79409, USA
| | - Yuichiro Ueno
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Meguro, Tokyo, 152-8551, Japan. .,Earth-Life Science Institute (WPI-ELSI), Tokyo Institute of Technology, Meguro, Tokyo, 152-8550, Japan. .,Institute for Extra-cutting-edge Science and Technology Avant-garde Research (X-star), Japan Agency for Marine-Earth Science and Technology (JAMSTEC), Natsushima-cho, Yokosuka, 237-0061, Japan.
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14
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Enya K, Yamagishi A, Kobayashi K, Yoshimura Y. Comparative study of methods for detecting extraterrestrial life in exploration mission of Mars and the solar system. LIFE SCIENCES IN SPACE RESEARCH 2022; 34:53-67. [PMID: 35940690 DOI: 10.1016/j.lssr.2022.07.001] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/12/2022] [Revised: 06/16/2022] [Accepted: 07/07/2022] [Indexed: 06/15/2023]
Abstract
The detection and analysis of extraterrestrial life are important issues of space science. Mars is among the most important planets to explore for extraterrestrial life, owing both to its physical properties and to its ancient and present environments as revealed by previous exploration missions. In this paper, we present a comparative study of methods for detecting extraterrestrial life and life-related substances. To this end, we have classified and summarized the characteristics targeted for the detection of extraterrestrial life in solar system exploration mission and the methods used to evaluate them. A summary table is presented. We conclude that at this moment (i) there is no realistic single detection method capable of concluding the discovery of extraterrestrial life, (ii) no single method has an advantage over the others in all respects, and (iii) there is no single method capable of distinguishing extraterrestrial life from terrestrial life. Therefore, a combination of complementary methods is essential. We emphasize the importance of endeavoring to detect extraterrestrial life without overlooking possible alien life forms, even at the cost of tolerating false positives. Summaries of both the targets and the detection methods should be updated continuously, and comparative studies of both should be pursued. Although this study assumes Mars to be a model site for the primary environment for life searches, both the targets and detection methods described herein will also be useful for searching for extraterrestrial life in any celestial environment and for the initial inspection of returned samples.
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Affiliation(s)
- Keigo Enya
- Institute of Space & Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuou, Sagamihara, Kanagawa 252-5210, Japan.
| | - Akihiko Yamagishi
- School of Life Science, Tokyo University of Pharmacy and Life Science, 1432-1 Horinouchi, Hachioji, Tokyo 192-0392, Japan
| | - Kensei Kobayashi
- Department of Chemistry, Yokohama National University, 79-5 Tokiwadai, Hodogaya, Yokohama 240-8501, Japan
| | - Yoshitaka Yoshimura
- Department of Life Science, Tamagawa University, 6-1-1 Tamagawagakuen, Machida, Tokyo 194-8610, Japan
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15
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Seaton KM, Cable ML, Stockton AM. Analytical Chemistry Throughout This Solar System. ANNUAL REVIEW OF ANALYTICAL CHEMISTRY (PALO ALTO, CALIF.) 2022; 15:197-219. [PMID: 35300527 DOI: 10.1146/annurev-anchem-061020-125416] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/14/2023]
Abstract
One of the greatest and most long-lived scientific pursuits of humankind has been to discover and study the planetary objects comprising our solar system. Information gained from solar system observations, via both remote sensing and in situ measurements, is inherently constrained by the analytical (often chemical) techniques we employ in these endeavors. The past 50 years of planetary science missions have resulted in immense discoveries within and beyond our solar system, enabled by state-of-the-art analytical chemical instrument suites on board these missions. In this review, we highlight and discuss some of the most impactful analytical chemical instruments flown on planetary science missions within the last 20 years, including analytical techniques ranging from remote spectroscopy to in situ chemical separations. We first highlight mission-based remote and in situ spectroscopic techniques, followed by in situ separation and mass spectrometry analyses. The results of these investigations are discussed, and their implications examined, from worlds as close as Venus and familiar as Mars to as far away and exotic as Titan. Instruments currently in development for planetary science missions in the near future are also discussed, as are the promises their capabilities bring. Analytical chemistry is critical to understanding what lies beyond Earth in our solar system, and this review seeks to highlight how questions, analytical tools, and answers have intersected over the past 20 years and their implications for the near future.
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Affiliation(s)
- Kenneth Marshall Seaton
- School of Chemistry and Biochemistry, Georgia Institute of Technology, Atlanta, Georgia, USA;
| | - Morgan Leigh Cable
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
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16
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Tosca NJ, Agee CB, Cockell CS, Glavin DP, Hutzler A, Marty B, McCubbin FM, Regberg AB, Velbel MA, Kminek G, Meyer MA, Beaty DW, Carrier BL, Haltigin T, Hays LE, Busemann H, Cavalazzi B, Debaille V, Grady MM, Hauber E, Pratt LM, Smith AL, Smith CL, Summons RE, Swindle TD, Tait KT, Udry A, Usui T, Wadhwa M, Westall F, Zorzano MP. Time-Sensitive Aspects of Mars Sample Return (MSR) Science. ASTROBIOLOGY 2022; 22:S81-S111. [PMID: 34904889 DOI: 10.1089/ast.2021.0115] [Citation(s) in RCA: 7] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/14/2023]
Abstract
Samples returned from Mars would be placed under quarantine at a Sample Receiving Facility (SRF) until they are considered safe to release to other laboratories for further study. The process of determining whether samples are safe for release, which may involve detailed analysis and/or sterilization, is expected to take several months. However, the process of breaking the sample tube seal and extracting the headspace gas will perturb local equilibrium conditions between gas and rock and set in motion irreversible processes that proceed as a function of time. Unless these time-sensitive processes are understood, planned for, and/or monitored during the quarantine period, scientific information expected from further analysis may be lost forever. At least four processes underpin the time-sensitivity of Mars returned sample science: (1) degradation of organic material of potential biological origin, (2) modification of sample headspace gas composition, (3) mineral-volatile exchange, and (4) oxidation/reduction of redox-sensitive materials. Available constraints on the timescales associated with these processes supports the conclusion that an SRF must have the capability to characterize attributes such as sample tube headspace gas composition, organic material of potential biological origin, as well as volatiles and their solid-phase hosts. Because most time-sensitive investigations are also sensitive to sterilization, these must be completed inside the SRF and on timescales of several months or less. To that end, we detail recommendations for how sample preparation and analysis could complete these investigations as efficiently as possible within an SRF. Finally, because constraints on characteristic timescales that define time-sensitivity for some processes are uncertain, future work should focus on: (1) quantifying the timescales of volatile exchange for core material physically and mineralogically similar to samples expected to be returned from Mars, and (2) identifying and developing stabilization or temporary storage strategies that mitigate volatile exchange until analysis can be completed. Executive Summary Any samples returned from Mars would be placed under quarantine at a Sample Receiving Facility (SRF) until it can be determined that they are safe to release to other laboratories for further study. The process of determining whether samples are safe for release, which may involve detailed analysis and/or sterilization, is expected to take several months. However, the process of breaking the sample tube seal and extracting the headspace gas would perturb local equilibrium conditions between gas and rock and set in motion irreversible processes that proceed as a function of time. Unless these processes are understood, planned for, and/or monitored during the quarantine period, scientific information expected from further analysis may be lost forever. Specialist members of the Mars Sample Return Planning Group Phase 2 (MSPG-2), referred to here as the Time-Sensitive Focus Group, have identified four processes that underpin the time-sensitivity of Mars returned sample science: (1) degradation of organic material of potential biological origin, (2) modification of sample headspace gas composition, (3) mineral-volatile exchange, and (4) oxidation/reduction of redox-sensitive materials (Figure 2). Consideration of the timescales and the degree to which these processes jeopardize scientific investigations of returned samples supports the conclusion that an SRF must have the capability to characterize: (1) sample tube headspace gas composition, (2) organic material of potential biological origin, (3) volatiles bound to or within minerals, and (4) minerals or other solids that host volatiles (Table 4). Most of the investigations classified as time-sensitive in this report are also sensitive to sterilization by either heat treatment and/or gamma irradiation (Velbel et al., 2022). Therefore, these investigations must be completed inside biocontainment and on timescales that minimize the irrecoverable loss of scientific information (i.e., several months or less; Section 5). To that end, the Time-Sensitive Focus Group has outlined a number of specific recommendations for sample preparation and instrumentation in order to complete these investigations as efficiently as possible within an SRF (Table 5). Constraints on the characteristic timescales that define time-sensitivity for different processes can range from relatively coarse to uncertain (Section 4). Thus, future work should focus on: (1) quantifying the timescales of volatile exchange for variably lithified core material physically and mineralogically similar to samples expected to be returned from Mars, and (2) identifying and developing stabilization strategies or temporary storage strategies that mitigate volatile exchange until analysis can be completed. List of Findings FINDING T-1: Aqueous phases, and oxidants liberated by exposure of the sample to aqueous phases, mediate and accelerate the degradation of critically important but sensitive organic compounds such as DNA. FINDING T-2: Warming samples increases reaction rates and destroys compounds making biological studies much more time-sensitive. MAJOR FINDING T-3: Given the potential for rapid degradation of biomolecules, (especially in the presence of aqueous phases and/or reactive O-containing compounds) Sample Safety Assessment Protocol (SSAP) and parallel biological analysis are time sensitive and must be carried out as soon as possible. FINDING T-4: If molecules or whole cells from either extant or extinct organisms have persisted under present-day martian conditions in the samples, then it follows that preserving sample aliquots under those same conditions (i.e., 6 mbar total pressure in a dominantly CO2 atmosphere and at an average temperature of -80°C) in a small isolation chamber is likely to allow for their continued persistence. FINDING T-5: Volatile compounds (e.g., HCN and formaldehyde) have been lost from Solar System materials stored under standard curation conditions. FINDING T-6: Reactive O-containing species have been identified in situ at the martian surface and so may be present in rock or regolith samples returned from Mars. These species rapidly degrade organic molecules and react more rapidly as temperature and humidity increase. FINDING T-7: Because the sample tubes would not be closed with perfect seals and because, after arrival on Earth, there will be a large pressure gradient across that seal such that the probability of contamination of the tube interiors by terrestrial gases increases with time, the as-received sample tubes are considered a poor choice for long-term gas sample storage. This is an important element of time sensitivity. MAJOR FINDING T-8: To determine how volatiles may have been exchanged with headspace gas during transit to Earth, the composition of martian atmosphere (in a separately sealed reservoir and/or extracted from the witness tubes), sample headspace gas composition, temperature/time history of the samples, and mineral composition (including mineral-bound volatiles) must all be quantified. When the sample tube seal is breached, mineral-bound volatile loss to the curation atmosphere jeopardizes robust determination of volatile exchange history between mineral and headspace. FINDING T-9: Previous experiments with mineral powders show that sulfate minerals are susceptible to H2O loss over timescales of hours to days. In addition to volatile loss, these processes are accompanied by mineralogical transformation. Thus, investigations targeting these minerals should be considered time-sensitive. FINDING T-10: Sulfate minerals may be stabilized by storage under fixed relative-humidity conditions, but only if the identity of the sulfate phase(s) is known a priori. In addition, other methods such as freezing may also stabilize these minerals against volatile loss. FINDING T-11: Hydrous perchlorate salts are likely to undergo phase transitions and volatile exchange with ambient surroundings in hours to days under temperature and relative humidity ranges typical of laboratory environments. However, the exact timescale over which these processes occur is likely a function of grain size, lithification, and/or cementation. FINDING T-12: Nanocrystalline or X-ray amorphous materials are typically stabilized by high proportions of surface adsorbed H2O. Because this surface adsorbed H2O is weakly bound compared to bulk materials, nanocrystalline materials are likely to undergo irreversible ripening reactions in response to volatile loss, which in turn results in decreases in specific surface area and increases in crystallinity. These reactions are expected to occur over the timescale of weeks to months under curation conditions. Therefore, the crystallinity and specific surface area of nanocrystalline materials should be characterized and monitored within a few months of opening the sample tubes. These are considered time-sensitive measurements that must be made as soon as possible. FINDING T-13: Volcanic and impact glasses, as well as opal-CT, are metastable in air and susceptible to alteration and volatile exchange with other solid phases and ambient headspace. However, available constraints indicate that these reactions are expected to proceed slowly under typical laboratory conditions (i.e., several years) and so analyses targeting these materials are not considered time sensitive. FINDING T-14: Surface adsorbed and interlayer-bound H2O in clay minerals is susceptible to exchange with ambient surroundings at timescales of hours to days, although the timescale may be modified depending on the degree of lithification or cementation. Even though structural properties of clay minerals remain unaffected during this process (with the exception of the interlayer spacing), investigations targeting H2O or other volatiles bound on or within clay minerals should be considered time sensitive upon opening the sample tube. FINDING T-15: Hydrated Mg-carbonates are susceptible to volatile loss and recrystallization and transformation over timespans of months or longer, though this timescale may be modified by the degree of lithification and cementation. Investigations targeting hydrated carbonate minerals (either the volatiles they host or their bulk mineralogical properties) should be considered time sensitive upon opening the sample tube. MAJOR FINDING T-16: Current understanding of mineral-volatile exchange rates and processes is largely derived from monomineralic experiments and systems with high surface area; lithified sedimentary rocks (accounting for some, but not all, of the samples in the cache) will behave differently in this regard and are likely to be associated with longer time constants controlled in part by grain boundary diffusion. Although insufficient information is available to quantify this at the present time, the timescale of mineral-volatile exchange in lithified samples is likely to overlap with the sample processing and curation workflow (i.e., 1-10 months; Table 4). This underscores the need to prioritize measurements targeting mineral-hosted volatiles within biocontainment. FINDING T-17: The liberation of reactive O-species through sample treatment or processing involving H2O (e.g., rinsing, solvent extraction, particle size separation in aqueous solution, or other chemical extraction or preparation protocols) is likely to result in oxidation of some component of redox-sensitive materials in a matter of hours. The presence of reactive O-species should be examined before sample processing steps that seek to preserve or target redox-sensitive minerals. Electron paramagnetic resonance spectroscopy (EPR) is one example of an effective analytical method capable of detecting and characterizing the presence of reactive O-species. FINDING T-18: Environments that maintain anoxia under inert gas containing <<1 ppm O2 are likely to stabilize redox-sensitive minerals over timescales of several years. MAJOR FINDING T-19: MSR investigations targeting organic macromolecular or cellular material, mineral-bound volatile compounds, redox sensitive minerals, and/or hydrous carbonate minerals can become compromised at the timescale of weeks (after opening the sample tube), and scientific information may be completely lost within a time timescale of a few months. Because current considerations indicate that completion of SSAP, sample sterilization, and distribution to investigator laboratories cannot be completed in this time, these investigations must be completed within the Sample Receiving Facility as soon as possible.
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Affiliation(s)
- Nicholas J Tosca
- University of Cambridge, Department of Earth Sciences, Cambridge, UK
| | - Carl B Agee
- University of New Mexico, Institute of Meteoritics, Albuquerque, New Mexico, USA
| | - Charles S Cockell
- University of Edinburgh, Centre for Astrobiology, School of Physics and Astronomy, Edinburgh, UK
| | - Daniel P Glavin
- NASA Goddard Space Flight Center, Solar System Exploration Division, Greenbelt, Maryland, USA
| | | | | | - Francis M McCubbin
- NASA Johnson Space Center, Astromaterials Research and Exploration Science Division, Houston, Texas, USA
| | - Aaron B Regberg
- NASA Johnson Space Center, Astromaterials Research and Exploration Science Division, Houston, Texas, USA
| | - Michael A Velbel
- Michigan State University, Earth and Environmental Sciences, East Lansing, Michigan, USA
- Smithsonian Institution, Department of Mineral Sciences, National Museum of Natural History, Washington, DC, USA
| | | | - Michael A Meyer
- NASA Headquarters, Mars Sample Return Program, Washington, DC, USA
| | - David W Beaty
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | - Brandi L Carrier
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | | | - Lindsay E Hays
- NASA Headquarters, Mars Sample Return Program, Washington, DC, USA
| | - Henner Busemann
- ETH Zürich, Institute of Geochemistry and Petrology, Zürich, Switzerland
| | - Barbara Cavalazzi
- Università di Bologna, Dipartimento di Scienze Biologiche, Geologiche e Ambientali, Bologna, Italy
| | | | | | - Ernst Hauber
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - Lisa M Pratt
- Indiana University Bloomington, Earth and Atmospheric Sciences, Bloomington, Indiana, USA
| | - Alvin L Smith
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | - Caroline L Smith
- Natural History Museum, Department of Earth Sciences, London, UK
- University of Glasgow, School of Geographical and Earth Sciences, Glasgow, UK
| | - Roger E Summons
- Massachusetts Institute of Technology, Earth, Atmospheric and Planetary Sciences, Cambridge, Massachusetts, USA
| | - Timothy D Swindle
- University of Arizona, Lunar and Planetary Laboratory, Tucson, Arizona, USA
| | - Kimberly T Tait
- Royal Ontario Museum, Department of Natural History, Toronto, Ontario, Canada
| | - Arya Udry
- University of Nevada Las Vegas, Las Vegas, Nevada, USA
| | - Tomohiro Usui
- Japan Aerospace Exploration Agency (JAXA), Institute of Space and Astronautical Science (ISAS), Chofu, Tokyo, Japan
| | - Meenakshi Wadhwa
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
- Arizona State University, Tempe, Arizona, USA
| | - Frances Westall
- Centre National de la Recherche Scientifique (CNRS), Centre de Biophysique Moléculaire, Orléans, France
| | - Maria-Paz Zorzano
- Centro de Astrobiologia (CSIC-INTA), Torrejon de Ardoz, Spain
- University of Aberdeen, Department of Planetary Sciences, School of Geosciences, King's College, Aberdeen, UK
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17
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Swindle TD, Atreya S, Busemann H, Cartwright JA, Mahaffy P, Marty B, Pack A, Schwenzer SP. Scientific Value of Including an Atmospheric Sample as Part of Mars Sample Return (MSR). ASTROBIOLOGY 2022; 22:S165-S175. [PMID: 34904893 DOI: 10.1089/ast.2021.0107] [Citation(s) in RCA: 8] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/14/2023]
Abstract
The Perseverance rover is meant to collect samples of the martian surface for eventual return to Earth. The headspace gas present over the solid samples within the sample tubes will be of significant scientific interest for what it reveals about the interactions of the solid samples with the trapped atmosphere and for what it will reveal about the martian atmosphere itself. However, establishing the composition of the martian atmosphere will require other dedicated samples. The headspace gas as the sole atmospheric sample is problematic for many reasons. The quantity of gas present within the sample tube volume is insufficient for many investigations, and there will be exchange between solid samples, headspace gas, and tube walls. Importantly, the sample tube materials and preparation were not designed for optimal Mars atmospheric gas collection and storage as they were not sent to Mars in a degassed evacuated state and have been exposed to both Earth's and Mars' atmospheres. Additionally, there is a risk of unconstrained seal leakage in transit back to Earth, which would allow fractionation of the sample (leak-out) and contamination (leak-in). The science return can be improved significantly (and, in some cases, dramatically) by adding one or more of several strategies listed here in increasing order of effectiveness and difficulty of implementation: (1) Having Perseverance collect a gas sample in an empty sample tube, (2) Collecting gas in a newly-designed, valved, sample-tube-sized vessel that is flown on either the Sample Fetch Rover (SFR) or the Sample Retrieval Lander (SRL), (3) Adding a larger (50-100 cc) dedicated gas sampling volume to the Orbiting Sample container (OS), (4) Adding a larger (50-100 cc) dedicated gas sampling volume to the OS that can be filled with compressed martian atmosphere.
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Affiliation(s)
- Timothy D Swindle
- University of Arizona, Lunar and Planetary Laboratory, Tucson, Arizona, USA
| | | | - Henner Busemann
- ETH Zürich, Institute of Geochemistry and Petrology, Zürich, Switzerland
| | | | - Paul Mahaffy
- NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
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18
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Thompson MA, Krissansen-Totton J, Wogan N, Telus M, Fortney JJ. The case and context for atmospheric methane as an exoplanet biosignature. Proc Natl Acad Sci U S A 2022; 119:e2117933119. [PMID: 35353627 PMCID: PMC9168929 DOI: 10.1073/pnas.2117933119] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/08/2021] [Accepted: 01/31/2022] [Indexed: 11/24/2022] Open
Abstract
Methane has been proposed as an exoplanet biosignature. Imminent observations with the James Webb Space Telescope may enable methane detections on potentially habitable exoplanets, so it is essential to assess in what planetary contexts methane is a compelling biosignature. Methane’s short photochemical lifetime in terrestrial planet atmospheres implies that abundant methane requires large replenishment fluxes. While methane can be produced by a variety of abiotic mechanisms such as outgassing, serpentinizing reactions, and impacts, we argue that—in contrast to an Earth-like biosphere—known abiotic processes cannot easily generate atmospheres rich in CH4 and CO2 with limited CO due to the strong redox disequilibrium between CH4 and CO2. Methane is thus more likely to be biogenic for planets with 1) a terrestrial bulk density, high mean-molecular-weight and anoxic atmosphere, and an old host star; 2) an abundance of CH4 that implies surface fluxes exceeding what could be supplied by abiotic processes; and 3) atmospheric CO2 with comparatively little CO.
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Affiliation(s)
- Maggie A. Thompson
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064
| | | | - Nicholas Wogan
- Department of Earth and Space Sciences, University of Washington, Seattle, WA 98195
| | - Myriam Telus
- Department of Earth and Planetary Sciences, University of California, Santa Cruz, CA 95064
| | - Jonathan J. Fortney
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064
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19
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From Atmospheric Evolution to the Search of Species of Astrobiological Interest in the Solar System—Case Studies Using the Planetary Spectrum Generator. ATMOSPHERE 2022. [DOI: 10.3390/atmos13030461] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
Abstract
The study of minor chemical species in terrestrial planets’ atmospheres can teach us about the chemistry, dynamics and evolution of the atmospheres through time. Phosphine or methane on terrestrial planets are potential biosignatures, such that their detection may signify the presence of life on a planet. Therefore, the search for these species in the solar system is an important step for the subsequent application of the same techniques to exoplanetary atmospheres. To study atmospheric depletion and the evolution of water abundance in the atmospheres of terrestrial planets, the estimation of the D/H ratio and its spatial and temporal variability is used. We used the Planetary Spectrum Generator (PSG), a radiative transfer suite, with the goal of simulating spectra from observations of Venus, Mars and Jupiter, searching for minor chemical species. The present study contributes to highlight that the PSG is an efficient tool for studying minor chemical species and compounds of astrobiological interest in planetary atmospheres, allowing to perform the detection and retrieval of the relevant molecular species. Regarding detection, it is effective in disentangling different molecular opacities affecting observations. In order to contribute to the scientific community that is focused on the study of minor chemical species in the solar system’s atmospheres, using this tool, in this work, we present the results from an analysis of observations of Venus, Mars and Jupiter, by comparison of observations with simulations in the infrared (IR). The first step was to clearly identify the position of molecular features using our model simulations, since the molecular absorption/emission features of different molecules tend to overlap. For this step, we used the method of the variation of abundances. The second step was to determine the molecular abundances and compare them with values from the literature using the retrieval method and the line depth ratio method. For Venus, our study of SO2-related observations by the Texas Echelon Cross Echelle Spectrograph (TEXES) at 7.4 μm enabled the identification of absorption lines due to sulphur dioxide and carbon dioxide as well as constrain the abundance of SO2 at the cloud top. Phosphine was not detected in the comparison between the simulation and TEXES IR observations around 10.5 μm. For Mars, both a positive and a non-detection of methane were studied using PSG simulations. The related spectra observations in the IR, at approximately 3.3 μm, correspond, respectively, to the Mars Express (MEx) and ExoMars space probes. Moreover, an estimate of the deuterium-to-hydrogen ratio (D/H ratio) was obtained by comparing the simulations with observations by the Echelon Cross Echelle Spectrograph (EXES) onboard the Stratospheric Observatory for Infrared Astronomy (SOFIA) at approximately 7.19–7.23 μm. For Jupiter, the detection of ammonia, phosphine, deuterated methane and methane was studied, by comparing the simulations with IR observations by the Infrared Space Observatory (ISO) at approximately 7–12 μm. Moreover, the retrieval of the profiles of ammonia and phosphine was performed.
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Huidobro J, Aramendia J, Arana G, Madariaga JM. Reviewing in situ analytical techniques used to research Martian geochemistry: From the Viking Project to the MMX future mission. Anal Chim Acta 2022; 1197:339499. [DOI: 10.1016/j.aca.2022.339499] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/04/2021] [Revised: 01/11/2022] [Accepted: 01/12/2022] [Indexed: 11/01/2022]
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Laboratory experiment of ATP measurement using Mars soil simulant: as a method for extraterrestrial life detection. ANAL SCI 2022; 38:725-730. [PMID: 35286642 PMCID: PMC9013681 DOI: 10.1007/s44211-022-00081-y] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/13/2021] [Accepted: 01/06/2022] [Indexed: 12/04/2022]
Abstract
We present a laboratory experiment of ATP measurement using Mars soil simulant and Escherichia coli (E. coli) with a point of view for future application to searching extraterrestrial life. We used Mars Global Simulant MGS-1 (Exolith Lab) as soil simulant, added E. coli suspension to it, then the soil simulant with E. coli was dried. Various configurations of samples with different E. coli density, 1.75 × 102, 1.75 × 103, 1.75 × 104, 1.75 × 105, and 1.75 × 106 cells (g soil)−1, were prepared together with controls. ATP extraction reagent and luminescence reagent were added to the sample, and bioluminescence measurement was performed. The result suggests significant detection of ATP for samples with E. coli density used in this work. Similar experiments but without the soil simulant were carried out, and results with and without the soil simulant are compared. Based on the ATP measurement studied in this work, we discussed extraterrestrial life search, planetary protection, relation with the panspermia hypothesis, and also other applications.
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Depleted carbon isotope compositions observed at Gale crater, Mars. Proc Natl Acad Sci U S A 2022; 119:2115651119. [PMID: 35042808 PMCID: PMC8795525 DOI: 10.1073/pnas.2115651119] [Citation(s) in RCA: 13] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Accepted: 12/01/2021] [Indexed: 11/20/2022] Open
Abstract
Carbon isotopic analysis is among the most pervasive geochemical approaches because the fractionation of carbon isotopes produces a natural tracer of biological and chemical processes. Rover-based carbon isotopic analyses of sedimentary rocks on Mars have the potential to reveal modes of Martian carbon cycling. We report carbon isotopic values of the methane released during pyrolysis of samples obtained at Gale crater. The values show remarkable variation indicating different origins for the carbon evolved from different samples. Samples from multiple locations within Gale crater evolved methane with highly fractionated carbon isotopes. We suggest three routes by which highly fractionated carbon could be deposited on Mars, with each suggesting that Martian carbon cycling is quite distinct from that of the present Earth. Obtaining carbon isotopic information for organic carbon from Martian sediments has long been a goal of planetary science, as it has the potential to elucidate the origin of such carbon and aspects of Martian carbon cycling. Carbon isotopic values (δ13CVPDB) of the methane released during pyrolysis of 24 powder samples at Gale crater, Mars, show a high degree of variation (−137 ± 8‰ to +22 ± 10‰) when measured by the tunable laser spectrometer portion of the Sample Analysis at Mars instrument suite during evolved gas analysis. Included in these data are 10 measured δ13C values less than −70‰ found for six different sampling locations, all potentially associated with a possible paleosurface. There are multiple plausible explanations for the anomalously depleted 13C observed in evolved methane, but no single explanation can be accepted without further research. Three possible explanations are the photolysis of biological methane released from the subsurface, photoreduction of atmospheric CO2, and deposition of cosmic dust during passage through a galactic molecular cloud. All three of these scenarios are unconventional, unlike processes common on Earth.
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Luo Y, Mischna MA, Lin JC, Fasoli B, Cai X, Yung YL. Mars Methane Sources in Northwestern Gale Crater Inferred From Back Trajectory Modeling. EARTH AND SPACE SCIENCE (HOBOKEN, N.J.) 2021; 8:e2021EA001915. [PMID: 35860450 PMCID: PMC9285602 DOI: 10.1029/2021ea001915] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 07/11/2021] [Revised: 10/26/2021] [Accepted: 10/27/2021] [Indexed: 06/15/2023]
Abstract
During its first seven years of operation, the Sample Analysis at Mars Tunable Laser Spectrometer (TLS) on board the Curiosity rover has detected seven methane spikes above a low background abundance in Gale crater. The methane spikes are likely sourced by surface emission within or around Gale crater. Here, we use inverse Lagrangian modeling techniques to identify upstream emission regions on the Martian surface for these methane spikes at an unprecedented spatial resolution. Inside Gale crater, the northwestern crater floor casts the strongest influence on the detections. Outside Gale crater, the upstream regions common to all the methane spikes extend toward the north. The contrasting results from two consecutive TLS methane measurements performed on the same sol point to an active emission site to the west or the southwest of the Curiosity rover on the northwestern crater floor. The observed spike magnitude and frequency also favor emission sites on the northwestern crater floor, unless there are fast methane removal mechanisms at work, or either the methane spikes of TLS or the non-detections of ExoMars Trace Gas Orbiter cannot be trusted.
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Affiliation(s)
- Y. Luo
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | - M. A. Mischna
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - J. C. Lin
- Department of Atmospheric SciencesUniversity of UtahSalt Lake CityUTUSA
| | - B. Fasoli
- Department of Atmospheric SciencesUniversity of UtahSalt Lake CityUTUSA
| | - X. Cai
- Columbia UniversityNew YorkNYUSA
| | - Y. L. Yung
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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McMahon S, Ivarsson M, Wacey D, Saunders M, Belivanova V, Muirhead D, Knoll P, Steinbock O, Frost DA. Dubiofossils from a Mars-analogue subsurface palaeoenvironment: The limits of biogenicity criteria. GEOBIOLOGY 2021; 19:473-488. [PMID: 33951268 DOI: 10.1111/gbi.12445] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/11/2020] [Revised: 03/12/2021] [Accepted: 03/30/2021] [Indexed: 06/12/2023]
Abstract
The search for a fossil record of Earth's deep biosphere, partly motivated by potential analogies with subsurface habitats on Mars, has uncovered numerous assemblages of inorganic microfilaments and tubules inside ancient pores and fractures. Although these enigmatic objects are morphologically similar to mineralized microorganisms (and some contain organic carbon), they also resemble some abiotic structures. Palaeobiologists have responded to this ambiguity by evaluating problematic filaments against checklists of "biogenicity criteria". Here, we describe material that tests the limits of this approach. We sampled Jurassic calcite veins formed through subseafloor serpentinization, a water-rock reaction that can fuel the deep biosphere and is known to have occurred widely on Mars. At two localities ~4 km apart, veins contained curving, branched microfilaments composed of Mg-silicate and Fe-oxide minerals. Using a wide range of analytical techniques including synchrotron X-ray microtomography and scanning transmission electron microscopy, we show that these features meet many published criteria for biogenicity and are comparable to fossilized cryptoendolithic fungi or bacteria. However, we argue that abiotic processes driven by serpentinization could account for the same set of lifelike features, and report a chemical garden experiment that supports this view. These filaments are, therefore, most objectively described as dubiofossils, a designation we here defend from criticism and recommend over alternative approaches, but which nevertheless signifies an impasse. Similar impasses can be anticipated in the future exploration of subsurface palaeo-habitats on Earth and Mars. To avoid them, further studies are required in biomimetic geochemical self-organization, microbial taphonomy and micro-analytical techniques, with a focus on subsurface habitats.
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Affiliation(s)
- Sean McMahon
- UK Centre for Astrobiology, School of Physics and Astronomy, University of Edinburgh, Edinburgh, UK
- School of Geosciences, Grant Institute, University of Edinburgh, Edinburgh, UK
| | - Magnus Ivarsson
- Department of Paleobiology, Swedish Museum of Natural History, Stockholm, Sweden
| | - David Wacey
- Centre for Microscopy Characterisation and Analysis, The University of Western Australia, Perth, WA, Australia
| | - Martin Saunders
- Centre for Microscopy Characterisation and Analysis, The University of Western Australia, Perth, WA, Australia
| | - Veneta Belivanova
- Department of Paleobiology, Swedish Museum of Natural History, Stockholm, Sweden
| | - David Muirhead
- School of Geosciences, King's College, University of Aberdeen, Aberdeen, UK
| | - Pamela Knoll
- Department of Chemistry and Biochemistry, Florida State University, Tallahassee, FL, USA
| | - Oliver Steinbock
- Department of Chemistry and Biochemistry, Florida State University, Tallahassee, FL, USA
| | - Daniel A Frost
- Department of Earth & Planetary Science, University of California, Berkeley, CA, USA
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Rizzo V, Armstrong R, Hua H, Cantasano N, Nicolò T, Bianciardi G. Life on Mars: Clues, Evidence or Proof? SOLAR SYSTEM PLANETS AND EXOPLANETS 2021. [DOI: 10.5772/intechopen.95531] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/23/2023]
Abstract
The search for life on Mars is one of the main objectives of space missions. At “Pahrump Hills Field Site” (Gale Crater, Mojave target), inside the mudstones of the Murray lacustrine sequence, Curiosity rover found organic materials and lozenge shaped laths considered by NASA as pseudomorphic crystals. Besides it detected mineral assemblages suggesting both oxidizing (hematite) and reducing (magnetite) environments, as well as acidic (diagenetic and/or authigenic jarosite) and neutral (apatite) conditions, that might suggest bacterially mediated reactions. Our morphological and morphometrical investigations show that such diagenetic microstructures are unlikely to be lozenge shapes and, in addition to several converging features, they suggest the presence of remnants of complex algal-like biota, similar to terrestrial procaryotes and/or eukaryotes; possible microorganisms that, on the base of absolute dating criteria used by other scholars, lived on Mars about 2.12 +/−0.36 Ga ago.
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Harris RL, Schuerger AC, Wang W, Tamama Y, Garvin ZK, Onstott TC. Transcriptional response to prolonged perchlorate exposure in the methanogen Methanosarcina barkeri and implications for Martian habitability. Sci Rep 2021; 11:12336. [PMID: 34117335 PMCID: PMC8196204 DOI: 10.1038/s41598-021-91882-0] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/16/2021] [Accepted: 05/28/2021] [Indexed: 02/05/2023] Open
Abstract
Observations of trace methane (CH4) in the Martian atmosphere are significant to the astrobiology community given the overwhelming contribution of biological methanogenesis to atmospheric CH4 on Earth. Previous studies have shown that methanogenic Archaea can generate CH4 when incubated with perchlorates, highly oxidizing chaotropic salts which have been found across the Martian surface. However, the regulatory mechanisms behind this remain completely unexplored. In this study we performed comparative transcriptomics on the methanogen Methanosarcina barkeri, which was incubated at 30˚C and 0˚C with 10-20 mM calcium-, magnesium-, or sodium perchlorate. Consistent with prior studies, we observed decreased CH4 production and apparent perchlorate reduction, with the latter process proceeding by heretofore essentially unknown mechanisms. Transcriptomic responses of M. barkeri to perchlorates include up-regulation of osmoprotectant transporters and selection against redox-sensitive amino acids. Increased expression of methylamine methanogenesis genes suggest competition for H2 with perchlorate reduction, which we propose is catalyzed by up-regulated molybdenum-containing enzymes and maintained by siphoning diffused H2 from energy-conserving hydrogenases. Methanogenesis regulatory patterns suggest Mars' freezing temperatures alone pose greater constraints to CH4 production than perchlorates. These findings increase our understanding of methanogen survival in extreme environments and confers continued consideration of a potential biological contribution to Martian CH4.
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Affiliation(s)
- Rachel L Harris
- Department of Geosciences, Princeton University, Princeton, NJ, USA.
- Department of Organismic and Evolutionary Biology, Harvard University, Cambridge, MA, USA.
| | - Andrew C Schuerger
- Department of Plant Pathology, University of Florida, Gainesville, FL, USA
| | - Wei Wang
- Lewis-Sigler Institute for Integrative Genomics, Department of Molecular Biology, Princeton University, Princeton, NJ, USA
| | - Yuri Tamama
- Department of Geosciences, Princeton University, Princeton, NJ, USA
| | - Zachary K Garvin
- Department of Geosciences, Princeton University, Princeton, NJ, USA
| | - Tullis C Onstott
- Department of Geosciences, Princeton University, Princeton, NJ, USA
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YOSHIMURA Y, ENYA K, KOBAYASHI K, SASAKI S, YAMAGISHI A. Life Explorations for Biosignatures in Space. BUNSEKI KAGAKU 2021. [DOI: 10.2116/bunsekikagaku.70.309] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/23/2022]
Affiliation(s)
- Yoshitaka YOSHIMURA
- Department of Advanced Food Sciences, College of Agriculture, Tamagawa University
| | - Keigo ENYA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency
| | - Kensei KOBAYASHI
- Graduate School of Engineering Science, Yokohama National University
| | - Satoshi SASAKI
- School of Bioscience and Biotechnology, Tokyo University of Technology
| | - Akihiko YAMAGISHI
- Department of Applied Life Sciences, School of Life Sciences, Tokyo University of Pharmacy and Life Sciences
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Abstract
This Feature introduces and discusses the findings of key analytical techniques used to study planetary bodies in our solar system in the search for life beyond Earth, future missions planned for high-priority astrobiology targets in our solar system, and the challenges we face in performing these investigations.
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Affiliation(s)
- Kenneth Marshall Seaton
- School of Chemistry & Biochemistry, Georgia Institute of Technology, North Avenue NW, Atlanta, Georgia 30332, United States
| | - Morgan Leigh Cable
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California 91109, United States
| | - Amanda Michelle Stockton
- School of Chemistry & Biochemistry, Georgia Institute of Technology, North Avenue NW, Atlanta, Georgia 30332, United States
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Surmick DM, Taleh L, Melikechi N. Effects of Laser Beam Focusing Characteristics on Laser-Induced Breakdown Spectra. APPLIED SPECTROSCOPY 2021; 75:127-136. [PMID: 33016770 DOI: 10.1177/0003702820961437] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/11/2023]
Abstract
The impact of altering laser focusing conditions on laser-induced breakdown spectroscopy experiments is investigated under ambient Earth laboratory and simulated Martian atmospheres. Experiments were performed in which the focal spot size was varied on a sample by altering the lens to sample distance with respect to targets of interest. Samples investigated include aluminum, copper, and steel. Specific neutral and ionic transitions of each sample were monitored. Atomic and ionic emissions show different intensity peak distributions along the varying lens to sample distance. Ionic species have peak emissions when laser plasma is initiated with a focused spot within the sample in ambient Earth laboratory air, while atomic emissions have peak intensities several millimeters deeper into a sample. In simulated Martian atmospheres, atomic emissions are observed to peak when the laser is focused within the sample, while ionic emissions have peak intensities when the laser is focused near the surface of a sample.
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Affiliation(s)
- David M Surmick
- Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts, Lowell, MA, USA
| | | | - Noureddine Melikechi
- Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts, Lowell, MA, USA
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Ng CY, Xu Y, Chang YC, Wannenmacher A, Parziale M, Armentrout PB. Quantum electronic control on chemical activation of methane by collision with spin–orbit state selected vanadium cation. Phys Chem Chem Phys 2021; 23:273-286. [DOI: 10.1039/d0cp04333h] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/21/2022]
Abstract
A detailed investigation of absolute integral cross sections (σ's) for the reactions, V+[a5DJ (J = 0, 2), a5FJ (J = 1, 2), and a3FJ (J = 2, 3)] + CH4, can be interpreted using a weak spin crossing mechanism.
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Affiliation(s)
- Cheuk-Yiu Ng
- Department of Chemistry
- University of California
- Davis
- USA
| | - Yuntao Xu
- Department of Chemistry
- University of California
- Davis
- USA
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31
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McMahon S, Parnell J, Reekie PBR. Mars-Analog Calcium Sulfate Veins Record Evidence of Ancient Subsurface Life. ASTROBIOLOGY 2020; 20:1212-1223. [PMID: 32985907 DOI: 10.1089/ast.2019.2172] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/11/2023]
Abstract
Ancient veins of calcium sulfate minerals (anhydrite, bassanite, and gypsum) deposited by subsurface aqueous fluids crosscut fluviolacustrine sedimentary rocks at multiple localities on Mars. Although these veins have been considered an attractive target for astrobiological investigation, their potential to preserve biosignatures is poorly understood. Here, we report the presence of biogenic authigenic pyrite in a fibrous gypsum vein of probable Cenozoic emplacement age from Permian lacustrine rocks in Northwest England. Pyrite occurs at the vein margins and displays a complex interfingering boundary with the surrounding gypsum suggestive of replacive authigenic growth. Gypsum-entombed carbonaceous material of probable organic origin was also identified by Raman spectroscopic microscopy in close proximity to the pyrite. Spatially resolved ion microprobe (SIMS) measurements reveal that the pyrite sulfur isotope composition is consistently very light (δ34SVCDT = -30.7‰). Comparison with the sulfate in the vein gypsum (δ34SVCDT = +8.5‰) indicates a fractionation too large to be explained by nonbiological (thermochemical) sulfate reduction. We infer that the pyrite was precipitated by microorganisms coupling the reduction of vein-derived sulfate with the oxidation of wall-derived organic matter. This is the first evidence that such veins can incorporate biosignatures that remain stable over geological time, which could be detected in samples returned from Mars.
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Affiliation(s)
- S McMahon
- UK Centre for Astrobiology, School of Physics and Astronomy, University of Edinburgh, Edinburgh, UK
- School of Geosciences, Grant Institute, University of Edinburgh, Edinburgh, UK
| | - J Parnell
- School of Geosciences, University of Aberdeen, King's College, Aberdeen, UK
| | - P B R Reekie
- UK Centre for Astrobiology, School of Physics and Astronomy, University of Edinburgh, Edinburgh, UK
- School of Geosciences, Grant Institute, University of Edinburgh, Edinburgh, UK
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Vance SD, Melwani Daswani M. Serpentinite and the search for life beyond Earth. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2020; 378:20180421. [PMID: 31902342 DOI: 10.1098/rsta.2018.0421] [Citation(s) in RCA: 12] [Impact Index Per Article: 2.4] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 11/27/2019] [Indexed: 06/10/2023]
Abstract
Hydrogen from serpentinization is a source of chemical energy for some life forms on Earth. It is a potential fuel for life in the subsurface of Mars and in the icy ocean worlds in the outer solar system. Serpentinization is also implicated in life's origin. Planetary exploration offers a way to investigate such theories by characterizing and ultimately searching for life in geochemical settings that no longer exist on Earth. At present, much of the current context of serpentinization on other worlds relies on inference from modelling and studies on Earth. While there is evidence from orbital spectral imaging and martian meteorites that serpentinization has occurred on Mars, the extent and duration of that activity has not been constrained. Similarly, ongoing serpentinization might explain hydrogen found in the ocean of Saturn's tiny moon Enceladus, but this raises questions about how long such activity has persisted. Titan's hydrocarbon-rich atmosphere may derive from ancient or present-day serpentinization at the bottom of its ocean. In Europa, volcanism or serpentinization may provide hydrogen as a redox couple to oxygen generated at the moon's surface. We assess the potential extent of serpentinization in the solar system's wet and rocky worlds, assuming that microfracturing from thermal expansion anisotropy sets an upper limit on the percolation depth of surface water into the rocky interiors. In this bulk geophysical model, planetary cooling from radiogenic decay implies the infiltration of water to greater depths through time, continuing to the present. The serpentinization of this newly exposed rock is assessed as a significant source of global hydrogen. Comparing the computed hydrogen and surface-generated oxygen delivered to Europa's ocean reveals redox fluxes similar to Earth's. Planned robotic exploration missions to other worlds can aid in understanding the planetary context of serpentinization, testing the predictions herein. This article is part of a discussion meeting issue 'Serpentinite in the Earth System'.
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Affiliation(s)
- S D Vance
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8001, USA
| | - M Melwani Daswani
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8001, USA
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33
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Szopa C, Freissinet C, Glavin DP, Millan M, Buch A, Franz HB, Summons RE, Sumner DY, Sutter B, Eigenbrode JL, Williams RH, Navarro-González R, Guzman M, Malespin C, Teinturier S, Mahaffy PR, Cabane M. First Detections of Dichlorobenzene Isomers and Trichloromethylpropane from Organic Matter Indigenous to Mars Mudstone in Gale Crater, Mars: Results from the Sample Analysis at Mars Instrument Onboard the Curiosity Rover. ASTROBIOLOGY 2020; 20:292-306. [PMID: 31880468 DOI: 10.1089/ast.2018.1908] [Citation(s) in RCA: 20] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Abstract
Chromatographic analysis of the Cumberland mudstone in Gale crater by the Sample Analysis at Mars (SAM) instrument revealed the detection of two to three isomers of dichlorobenzene. Their individual concentrations were estimated to be in the 0.5-17 ppbw range relative to the sample mass. We also report the first detection of trichloromethylpropane and the confirmation of the detection of chlorobenzene previously reported. Supporting laboratory experiments excluded the SAM internal background as the source of those compounds, thus confirming the organic carbon and chlorine of the newly detected chlorohydrocarbons are indigenous to the mudstone sample. Laboratory experiments also demonstrated that the chlorohydrocarbons were mainly produced from chemical reactions occurring in the SAM ovens between organic molecules and oxychlorines contained in the sample. The results we obtained show that meteoritic organics and tested chemical species (a polycyclic aromatic hydrocarbon, an amino acid, and a carboxylic acid) were plausible organic precursors of the chlorinated aromatic molecules detected with SAM, thus suggesting that they could be among the organic molecules present in the mudstone. Results from this study coupled with previously reported detections of chlorinated aromatics (<300 ppbw) indigenous to the same mudstone highlight that organics can be preserved from the harsh surface conditions even at shallow depth. The detection of new chlorohydrocarbons with SAM confirms that organic molecules should have been available in an environment favorable to life forms, strengthening the habitability aspect of Gale crater.
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Affiliation(s)
- Cyril Szopa
- LATMOS/IPSL, UVSQ Université Paris-Saclay, UPMC Univ. Paris 06, CNRS, Guyancourt, France
- Institut Universitaire de France, Paris, France
| | - Caroline Freissinet
- LATMOS/IPSL, UVSQ Université Paris-Saclay, UPMC Univ. Paris 06, CNRS, Guyancourt, France
| | - Daniel P Glavin
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, Maryland
| | - Maeva Millan
- LATMOS/IPSL, UVSQ Université Paris-Saclay, UPMC Univ. Paris 06, CNRS, Guyancourt, France
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, Maryland
- Department of Biology, Georgetown University, Washington, District of Columbia
| | - Arnaud Buch
- Laboratoire de Génie des Procédés et Matériaux (LGPM), EA 4038, Centrale-Supelec, Rue Joliot Curie, Gif-sur-Yvette, France
| | - Heather B Franz
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, Maryland
| | - Roger E Summons
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, Massachusetts
| | - Dawn Y Sumner
- Department of Earth and Planetary Sciences, University of California, Davis, California
| | - Brad Sutter
- Jacobs Technology, Inc., Johnson Space Center, National Aeronautics and Space Administration, Houston, Texas
| | - Jennifer L Eigenbrode
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, Maryland
| | - Ross H Williams
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, Maryland
- Department of Astronomy and CRESST II, University of Maryland, College Park, Maryland
| | - Rafael Navarro-González
- Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Ciudad Universitaria, México, Distrito Federal, México
| | - Melissa Guzman
- LATMOS/IPSL, UVSQ Université Paris-Saclay, UPMC Univ. Paris 06, CNRS, Guyancourt, France
| | - Charles Malespin
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, Maryland
| | - Samuel Teinturier
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, Maryland
- Universities Space Research Association, Goddard Earth Sciences Technology and Research Studies and Investigations, Greenbelt, Maryland
| | - Paul R Mahaffy
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, Maryland
| | - Michel Cabane
- LATMOS/IPSL, UVSQ Université Paris-Saclay, UPMC Univ. Paris 06, CNRS, Guyancourt, France
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34
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Sterczewski LA, Bagheri M, Frez C, Canedy CL, Vurgaftman I, Kim M, Kim CS, Merritt CD, Bewley WW, Meyer JR. Near-infrared frequency comb generation in mid-infrared interband cascade lasers. OPTICS LETTERS 2019; 44:5828-5831. [PMID: 31774790 DOI: 10.1364/ol.44.005828] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/06/2019] [Accepted: 10/11/2019] [Indexed: 06/10/2023]
Abstract
The interband cascade laser (ICL) is an ideal candidate for low-power mid-infrared frequency comb spectroscopy. In this work, we demonstrate that its intracavity second-order optical nonlinearity induces a coherent up-conversion of the generated mid-infrared light to the near-infrared through second-harmonic and sum-frequency generation. At 1.8 µm, 10 mW of light at 3.6 µm convert into sub-nanowatt levels of optical power, spread across 30 nm of spectral coverage. The observed linear-to-nonlinear conversion efficiency exceeds ${3\;{\unicode{x00B5} {\rm W/W}}^2}$3µW/W2 in continuous wave operation. We use a dual-band ICL frequency comb source to characterize water vapor absorption in both spectral bands.
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35
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Drake H, Roberts NMW, Heim C, Whitehouse MJ, Siljeström S, Kooijman E, Broman C, Ivarsson M, Åström ME. Timing and origin of natural gas accumulation in the Siljan impact structure, Sweden. Nat Commun 2019; 10:4736. [PMID: 31628335 PMCID: PMC6802084 DOI: 10.1038/s41467-019-12728-y] [Citation(s) in RCA: 25] [Impact Index Per Article: 4.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/30/2019] [Accepted: 09/27/2019] [Indexed: 11/29/2022] Open
Abstract
Fractured rocks of impact craters may be suitable hosts for deep microbial communities on Earth and potentially other terrestrial planets, yet direct evidence remains elusive. Here, we present a study of the largest crater of Europe, the Devonian Siljan structure, showing that impact structures can be important unexplored hosts for long-term deep microbial activity. Secondary carbonate minerals dated to 80 ± 5 to 22 ± 3 million years, and thus postdating the impact by more than 300 million years, have isotopic signatures revealing both microbial methanogenesis and anaerobic oxidation of methane in the bedrock. Hydrocarbons mobilized from matured shale source rocks were utilized by subsurface microorganisms, leading to accumulation of microbial methane mixed with a thermogenic and possibly a minor abiotic gas fraction beneath a sedimentary cap rock at the crater rim. These new insights into crater hosted gas accumulation and microbial activity have implications for understanding the astrobiological consequences of impacts. Fractured rocks of impact craters have been suggested to be suitable hosts for deep microbial communities on Earth, and potentially other terrestrial planets, yet direct evidence remains elusive. Here, the authors show that the Siljan impact structure is host to long-term deep methane-cycling microbial activity.
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Affiliation(s)
- Henrik Drake
- Linnæus University, Department of Biology and Environmental Science, 39182, Kalmar, Sweden.
| | - Nick M W Roberts
- Geochronology and Tracers Facility, British Geological Survey, Nottingham, NG12 5GG, UK
| | - Christine Heim
- Department of Geobiology, Geoscience Centre Göttingen of the Georg-August University, Goldschmidtstr. 3, 37077, Göttingen, Germany
| | - Martin J Whitehouse
- Swedish Museum of Natural History, P.O. Box 50 007, 10405, Stockholm, Sweden
| | - Sandra Siljeström
- Bioscience and Materials/Chemistry and Materials, RISE Research Institutes of Sweden, Box 5607, 114 86, Stockholm, Sweden
| | - Ellen Kooijman
- Swedish Museum of Natural History, P.O. Box 50 007, 10405, Stockholm, Sweden
| | - Curt Broman
- Department of Geological Sciences, Stockholm University, 106 91, Stockholm, Sweden
| | - Magnus Ivarsson
- Swedish Museum of Natural History, P.O. Box 50 007, 10405, Stockholm, Sweden.,Department of Biology, University of Southern Denmark, Campusvej 55, 5230, Odense, Denmark
| | - Mats E Åström
- Linnæus University, Department of Biology and Environmental Science, 39182, Kalmar, Sweden
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36
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Seto M, Noguchi K, Cappellen PV. Potential for Aerobic Methanotrophic Metabolism on Mars. ASTROBIOLOGY 2019; 19:1187-1195. [PMID: 31173512 PMCID: PMC6785171 DOI: 10.1089/ast.2018.1943] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 08/20/2018] [Accepted: 05/07/2019] [Indexed: 06/09/2023]
Abstract
Observational evidence supports the presence of methane (CH4) in the martian atmosphere on the order of parts per billion by volume (ppbv). Here, we assess whether aerobic methanotrophy is a potentially viable metabolism in the martian upper regolith, by calculating metabolic energy gain rates under assumed conditions of martian surface temperature, pressure, and atmospheric composition. Using kinetic parameters for 19 terrestrial aerobic methanotrophic strains, we show that even under the imposed low temperature and pressure extremes (180-280 K and 6-11 hPa), methane oxidation by oxygen (O2) should in principle be able to generate the minimum energy production rate required to support endogenous metabolism (i.e., cellular maintenance). Our results further indicate that the corresponding metabolic activity would be extremely low, with cell doubling times in excess of 4000 Earth years at the present-day ppbv-level CH4 mixing ratios in the atmosphere of Mars. Thus, while aerobic methanotrophic microorganisms similar to those found on Earth could theoretically maintain their vital functions, they are unlikely to constitute prolific members of hypothetical martian soil communities.
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Affiliation(s)
- Mayumi Seto
- Department of Chemistry, Biology, and Environmental Sciences, Faculty of Science, Nara Women's University, Nara, Japan
| | - Katsuyuki Noguchi
- Department of Chemistry, Biology, and Environmental Sciences, Faculty of Science, Nara Women's University, Nara, Japan
| | - Philippe Van Cappellen
- Ecohydrology Research Group, Department of Earth and Environmental Sciences, Water Institute, University of Waterloo, Waterloo, Canada
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37
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Klein F, Grozeva NG, Seewald JS. Abiotic methane synthesis and serpentinization in olivine-hosted fluid inclusions. Proc Natl Acad Sci U S A 2019; 116:17666-17672. [PMID: 31427518 PMCID: PMC6731755 DOI: 10.1073/pnas.1907871116] [Citation(s) in RCA: 30] [Impact Index Per Article: 5.0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
The conditions of methane (CH4) formation in olivine-hosted secondary fluid inclusions and their prevalence in peridotite and gabbroic rocks from a wide range of geological settings were assessed using confocal Raman spectroscopy, optical and scanning electron microscopy, electron microprobe analysis, and thermodynamic modeling. Detailed examination of 160 samples from ultraslow- to fast-spreading midocean ridges, subduction zones, and ophiolites revealed that hydrogen (H2) and CH4 formation linked to serpentinization within olivine-hosted secondary fluid inclusions is a widespread process. Fluid inclusion contents are dominated by serpentine, brucite, and magnetite, as well as CH4(g) and H2(g) in varying proportions, consistent with serpentinization under strongly reducing, closed-system conditions. Thermodynamic constraints indicate that aqueous fluids entering the upper mantle or lower oceanic crust are trapped in olivine as secondary fluid inclusions at temperatures higher than ∼400 °C. When temperatures decrease below ∼340 °C, serpentinization of olivine lining the walls of the fluid inclusions leads to a near-quantitative consumption of trapped liquid H2O. The generation of molecular H2 through precipitation of Fe(III)-rich daughter minerals results in conditions that are conducive to the reduction of inorganic carbon and the formation of CH4 Once formed, CH4(g) and H2(g) can be stored over geological timescales until extracted by dissolution or fracturing of the olivine host. Fluid inclusions represent a widespread and significant source of abiotic CH4 and H2 in submarine and subaerial vent systems on Earth, and possibly elsewhere in the solar system.
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Affiliation(s)
- Frieder Klein
- Department of Marine Chemistry and Geochemistry, Woods Hole Oceanographic Institution, Woods Hole, MA 02543;
| | - Niya G Grozeva
- Massachusetts Institute of Technology-Woods Hole Oceanographic Institution Joint Program in Oceanography, Cambridge, MA 02139
| | - Jeffrey S Seewald
- Department of Marine Chemistry and Geochemistry, Woods Hole Oceanographic Institution, Woods Hole, MA 02543
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38
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Rennó NO, Backhus R, Cooper C, Flatico JM, Fischer E, Greer LC, Krasowski MJ, Kremic T, Martínez GM, Prokop NF, Sweeney D, Vicente-Retortillo A. A Simple Instrument Suite for Characterizing Habitability and Weathering: The Modern Aqueous Habitat Reconnaissance Suite (MAHRS). ASTROBIOLOGY 2019; 19:849-866. [PMID: 30964330 DOI: 10.1089/ast.2018.1945] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/09/2023]
Abstract
The shallow subsurface of Mars is extremely interesting as a possible microbial habitat because it becomes temporarily wet, it is shielded from radiation, and mixing by aeolian processes could provide the sources of energy and nutrients necessary for sustaining microbial life in it. The Modern Aqueous Habitat Reconnaissance Suite (MAHRS) was developed primarily to search for potentially habitable environments in the shallow subsurface of Mars and to study weathering, but it can also be used to search for potentially habitable environments in the shallow subsurface of other planetary bodies such as the Icy Worlds. MAHRS includes an instrument developed to measure regolith wetness and search for brine in the shallow subsurface of Mars, where it is most likely to be found. The detection of brine can aid in our understanding not only of habitability but also of geochemistry and aqueous weathering processes. Besides the regolith wetness sensor, MAHRS includes an electric field sensor, an optical microscope, and a radiometer developed to characterize the near-surface environment and study mixing by aeolian processes. MAHRS was designed to aid in the selection of optimum areas for sample collection for return to Earth.
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Affiliation(s)
- N O Rennó
- 1Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan
| | - R Backhus
- 2Space Physics Research Laboratory, University of Michigan, Ann Arbor, Michigan
| | - C Cooper
- 2Space Physics Research Laboratory, University of Michigan, Ann Arbor, Michigan
| | | | - E Fischer
- 1Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan
| | - L C Greer
- 4NASA Glenn Research Center, Cleveland, Ohio
| | | | - T Kremic
- 3Ohio Aerospace Institute, Cleveland, Ohio
| | - G M Martínez
- 1Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan
| | - N F Prokop
- 4NASA Glenn Research Center, Cleveland, Ohio
| | - David Sweeney
- 1Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan
| | - A Vicente-Retortillo
- 1Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan
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39
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Aeolian abrasion of rocks as a mechanism to produce methane in the Martian atmosphere. Sci Rep 2019; 9:8229. [PMID: 31160623 PMCID: PMC6546745 DOI: 10.1038/s41598-019-44616-2] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/24/2018] [Accepted: 05/16/2019] [Indexed: 11/08/2022] Open
Abstract
Seasonal changes in methane background levels and methane spikes have been detected in situ a metre above the Martian surface, and larger methane plumes detected via ground-based remote sensing, however their origin have not yet been adequately explained. Proposed methane sources include the UV irradiation of meteoritic-derived organic matter, hydrothermal reactions with olivine, organic breakdown via meteoroid impact, release from gas hydrates, biological production, or the release of methane from fluid inclusions in basalt during aeolian erosion. Here we quantify for the first time the potential importance of aeolian abrasion as a mechanism for releasing trapped methane from within rocks, by coupling estimates of present day surface wind abrasion with the methane contents of a variety of Martian meteorites, analogue terrestrial basalts and analogue terrestrial sedimentary rocks. We demonstrate that the abrasion of basalt under present day Martian rates of aeolian erosion is highly unlikely to produce detectable changes in methane concentrations in the atmosphere. We further show that, although there is a greater potential for methane production from the aeolian abrasion of certain sedimentary rocks, to produce the magnitude of methane concentrations analysed by the Curiosity rover they would have to contain methane in similar concentrations as economic reserved of biogenic/thermogenic deposits on Earth. Therefore we suggest that aeolian abrasion is an unlikely origin of the methane detected in the Martian atmosphere, and that other methane sources are required.
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40
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Ward LM, Stamenković V, Hand K, Fischer WW. Follow the Oxygen: Comparative Histories of Planetary Oxygenation and Opportunities for Aerobic Life. ASTROBIOLOGY 2019; 19:811-824. [PMID: 31188035 DOI: 10.1089/ast.2017.1779] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/09/2023]
Abstract
Aerobic respiration-the reduction of molecular oxygen (O2) coupled to the oxidation of reduced compounds such as organic carbon, ferrous iron, reduced sulfur compounds, or molecular hydrogen while conserving energy to drive cellular processes-is the most widespread and bioenergetically favorable metabolism on Earth today. Aerobic respiration is essential for the development of complex multicellular life; thus the presence of abundant O2 is an important metric for planetary habitability. O2 on Earth is supplied by oxygenic photosynthesis, but it is becoming more widely understood that abiotic processes may supply meaningful amounts of O2 on other worlds. The modern atmosphere and rock record of Mars suggest a history of relatively high O2 as a result of photochemical processes, potentially overlapping with the range of O2 concentrations used by biology. Europa may have accumulated high O2 concentrations in its subsurface ocean due to the radiolysis of water ice at its surface. Recent modeling efforts suggest that coexisting water and O2 may be common on exoplanets, with confirmation from measurements of exoplanet atmospheres potentially coming soon. In all these cases, O2 accumulates through abiotic processes-independent of water-oxidizing photosynthesis. We hypothesize that abiogenic O2 may enhance the habitability of some planetary environments, allowing highly energetic aerobic respiration and potentially even the development of complex multicellular life which depends on it, without the need to first evolve oxygenic photosynthesis. This hypothesis is testable with further exploration and life-detection efforts on O2-rich worlds such as Mars and Europa, and comparison to O2-poor worlds such as Enceladus. This hypothesis further suggests a new dimension to planetary habitability: "Follow the Oxygen," in which environments with opportunities for energy-rich metabolisms such as aerobic respiration are preferentially targeted for investigation and life detection.
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Affiliation(s)
- Lewis M Ward
- 1 Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California
| | - Vlada Stamenković
- 2 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | - Kevin Hand
- 2 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | - Woodward W Fischer
- 1 Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California
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41
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Sholes SF, Krissansen-Totton J, Catling DC. A Maximum Subsurface Biomass on Mars from Untapped Free Energy: CO and H 2 as Potential Antibiosignatures. ASTROBIOLOGY 2019; 19:655-668. [PMID: 30950631 DOI: 10.1089/ast.2018.1835] [Citation(s) in RCA: 7] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/09/2023]
Abstract
Whether extant life exists in the martian subsurface is an open question. High concentrations of photochemically produced CO and H2 in the otherwise oxidizing martian atmosphere represent untapped sources of biologically useful free energy. These out-of-equilibrium species diffuse into the regolith, so subsurface microbes could use them as a source of energy and carbon. Indeed, CO oxidation and methanogenesis are relatively simple and evolutionarily ancient metabolisms on Earth. Consequently, assuming CO- or H2-consuming metabolisms would evolve on Mars, the persistence of CO and H2 in the martian atmosphere sets limits on subsurface metabolic activity. In this study, we constrain such maximum subsurface metabolic activity on Mars using a one-dimensional photochemical model with a hypothetical global biological sink on atmospheric CO and H2. We increase the biological sink until the modeled atmospheric composition diverges from observed abundances. We find maximum biological downward subsurface sinks of 1.5 × 108 molecules/(cm2·s) for CO and 1.9 × 108 molecules/(cm2·s1) for H2. These convert to a maximum metabolizing biomass of ≲1027 cells or ≤2 × 1011 kg, equivalent to ≤10-4-10-5 of Earth's biomass, depending on the terrestrial estimate. Diffusion calculations suggest that this upper biomass limit applies to the top few kilometers of the martian crust in communication with the atmosphere at low to mid-latitudes. This biomass limit is more robust than previous estimates because we test multiple possible chemoautotrophic ecosystems over a broad parameter space of tunable model variables using an updated photochemical model with precise atmospheric concentrations and uncertainties from Curiosity. Our results of sparse or absent life in the martian subsurface also demonstrate how the atmospheric redox pairs of CO-O2 and H2-O2 may constitute antibiosignatures, which may be relevant to excluding life on exoplanets.
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Affiliation(s)
- Steven F Sholes
- 1 Department of Earth and Space Sciences, University of Washington, Seattle, Washington
- 2 Astrobiology Program, University of Washington, Seattle, Washington
| | - Joshua Krissansen-Totton
- 1 Department of Earth and Space Sciences, University of Washington, Seattle, Washington
- 2 Astrobiology Program, University of Washington, Seattle, Washington
| | - David C Catling
- 1 Department of Earth and Space Sciences, University of Washington, Seattle, Washington
- 2 Astrobiology Program, University of Washington, Seattle, Washington
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42
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Sterczewski LA, Westberg J, Bagheri M, Frez C, Vurgaftman I, Canedy CL, Bewley WW, Merritt CD, Kim CS, Kim M, Meyer JR, Wysocki G. Mid-infrared dual-comb spectroscopy with interband cascade lasers. OPTICS LETTERS 2019; 44:2113-2116. [PMID: 30985824 DOI: 10.1364/ol.44.002113] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/08/2019] [Accepted: 03/19/2019] [Indexed: 06/09/2023]
Abstract
Two semiconductor optical frequency combs, consuming less than 1 W of electrical power, are used to demonstrate high-sensitivity mid-infrared dual-comb spectroscopy in the important 3-4 μm spectral region. The devices are 4 mm long by 4 μm wide, and each emits 8 mW of average optical power. The spectroscopic sensing performance is demonstrated by measurements of methane and hydrogen chloride with optical multi-pass cell sensitivity enhancement. The system provides a spectral coverage of 33 cm-1 (1 THz), 0.32 cm-1 (9.7 GHz) frequency sampling interval, and peak signal-to-noise ratio of ∼100 at 100 μs integration time. The monolithic design, low drive power, and direct generation of mid-infrared radiation are highly attractive for portable broadband spectroscopic instrumentation in future terrestrial and space applications.
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43
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Korablev O, Vandaele AC, Montmessin F, Fedorova AA, Trokhimovskiy A, Forget F, Lefèvre F, Daerden F, Thomas IR, Trompet L, Erwin JT, Aoki S, Robert S, Neary L, Viscardy S, Grigoriev AV, Ignatiev NI, Shakun A, Patrakeev A, Belyaev DA, Bertaux JL, Olsen KS, Baggio L, Alday J, Ivanov YS, Ristic B, Mason J, Willame Y, Depiesse C, Hetey L, Berkenbosch S, Clairquin R, Queirolo C, Beeckman B, Neefs E, Patel MR, Bellucci G, López-Moreno JJ, Wilson CF, Etiope G, Zelenyi L, Svedhem H, Vago JL. No detection of methane on Mars from early ExoMars Trace Gas Orbiter observations. Nature 2019; 568:517-520. [PMID: 30971829 DOI: 10.1038/s41586-019-1096-4] [Citation(s) in RCA: 88] [Impact Index Per Article: 14.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/18/2018] [Accepted: 03/14/2019] [Indexed: 11/09/2022]
Abstract
The detection of methane on Mars has been interpreted as indicating that geochemical or biotic activities could persist on Mars today1. A number of different measurements of methane show evidence of transient, locally elevated methane concentrations and seasonal variations in background methane concentrations2-5. These measurements, however, are difficult to reconcile with our current understanding of the chemistry and physics of the Martian atmosphere6,7, which-given methane's lifetime of several centuries-predicts an even, well mixed distribution of methane1,6,8. Here we report highly sensitive measurements of the atmosphere of Mars in an attempt to detect methane, using the ACS and NOMAD instruments onboard the ESA-Roscosmos ExoMars Trace Gas Orbiter from April to August 2018. We did not detect any methane over a range of latitudes in both hemispheres, obtaining an upper limit for methane of about 0.05 parts per billion by volume, which is 10 to 100 times lower than previously reported positive detections2,4. We suggest that reconciliation between the present findings and the background methane concentrations found in the Gale crater4 would require an unknown process that can rapidly remove or sequester methane from the lower atmosphere before it spreads globally.
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Affiliation(s)
- Oleg Korablev
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia.
| | | | - Franck Montmessin
- Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), UVSQ Université Paris-Saclay, Sorbonne Université, CNRS, Paris, France
| | - Anna A Fedorova
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia
| | | | - François Forget
- Laboratoire de Météorologie Dynamique (LMD), CNRS Jussieu, Paris, France
| | - Franck Lefèvre
- Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), UVSQ Université Paris-Saclay, Sorbonne Université, CNRS, Paris, France
| | - Frank Daerden
- Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Ian R Thomas
- Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Loïc Trompet
- Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Justin T Erwin
- Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Shohei Aoki
- Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Séverine Robert
- Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Lori Neary
- Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Sébastien Viscardy
- Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Alexey V Grigoriev
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia
| | - Nikolay I Ignatiev
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia
| | - Alexey Shakun
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia
| | - Andrey Patrakeev
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia
| | - Denis A Belyaev
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia
| | - Jean-Loup Bertaux
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia.,Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), UVSQ Université Paris-Saclay, Sorbonne Université, CNRS, Paris, France
| | - Kevin S Olsen
- Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), UVSQ Université Paris-Saclay, Sorbonne Université, CNRS, Paris, France
| | - Lucio Baggio
- Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), UVSQ Université Paris-Saclay, Sorbonne Université, CNRS, Paris, France
| | - Juan Alday
- Department of Physics, Oxford University, Oxford, UK
| | - Yuriy S Ivanov
- Main Astronomical Observatory (MAO), National Academy of Sciences of Ukraine, Kiev, Ukraine
| | - Bojan Ristic
- Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Jon Mason
- School of Physical Sciences, The Open University, Milton Keynes, UK
| | - Yannick Willame
- Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Cédric Depiesse
- Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Laszlo Hetey
- Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Sophie Berkenbosch
- Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Roland Clairquin
- Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Claudio Queirolo
- Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Bram Beeckman
- Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Eddy Neefs
- Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Manish R Patel
- School of Physical Sciences, The Open University, Milton Keynes, UK
| | | | - Jose-Juan López-Moreno
- Instituto de Astrofìsica de Andalucía, Consejo Superior de Investigaciones Científicas (CSIC), Granada, Spain
| | | | - Giuseppe Etiope
- Instituto de Astrofisica e Planetologia Spaziali, INAF, Rome, Italy.,Istituto Nazionale di Geofisica e Vulcanologia, Rome, Italy.,Faculty of Environmental Science and Engineering, Babes-Bolyai University, Cluj-Napoca, Romania
| | - Lev Zelenyi
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia
| | - Håkan Svedhem
- European Space Research and Technology Centre (ESTEC), ESA, Noordwijk, The Netherlands
| | - Jorge L Vago
- European Space Research and Technology Centre (ESTEC), ESA, Noordwijk, The Netherlands
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Gibson BM. Miniaturized ring-down spectrometer for CubeSat-based planetary science. APPLIED OPTICS 2019; 58:1941-1949. [PMID: 30874059 DOI: 10.1364/ao.58.001941] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/12/2018] [Accepted: 02/07/2019] [Indexed: 06/09/2023]
Abstract
A robust, miniaturized cavity ring-down spectrometer has been developed as a laboratory demonstration model for future CubeSat deployments of near- and mid-infrared spectrometers for in situ planetary science. The spectrometer is compact enough to ensure compatibility with standard CubeSat spacecraft buses, with a probed gas volume of less than 2.5 cc to ease mass, volume, and power requirements of sample gas handling subsystems. When operated at 1.39 μm for water vapor isotope measurements, a noise-equivalent absorption coefficient of 3.7×10-9 cm-1 Hz-1/2 is obtained. Oxygen isotope measurements were performed to demonstrate scanning performance. The spectrometer has been designed to use only components with functional equivalents throughout the 1-5 μm range to maintain flexibility across a wide array of planetary science targets. Preliminary results from a 3.27 μm implementation intended for methane measurements are also presented.
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45
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Serrano P, Alawi M, de Vera JP, Wagner D. Response of Methanogenic Archaea from Siberian Permafrost and Non-permafrost Environments to Simulated Mars-like Desiccation and the Presence of Perchlorate. ASTROBIOLOGY 2019; 19:197-208. [PMID: 30742498 DOI: 10.1089/ast.2018.1877] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/09/2023]
Abstract
Numerous preflight investigations were necessary prior to the exposure experiment BIOMEX on the International Space Station to test the basic potential of selected microorganisms to resist or even to be active under Mars-like conditions. In this study, methanogenic archaea, which are anaerobic chemolithotrophic microorganisms whose lifestyle would allow metabolism under the conditions on early and recent Mars, were analyzed. Some strains from Siberian permafrost environments have shown a particular resistance. In this investigation, we analyzed the response of three permafrost strains (Methanosarcina soligelidi SMA-21, Candidatus Methanosarcina SMA-17, Candidatus Methanobacterium SMA-27) and two related strains from non-permafrost environments (Methanosarcina mazei, Methanosarcina barkeri) to desiccation conditions (-80°C for 315 days, martian regolith analog simulants S-MRS and P-MRS, a 128-day period of simulated Mars-like atmosphere). Exposure of the different methanogenic strains to increasing concentrations of magnesium perchlorate allowed for the study of their metabolic shutdown in a Mars-relevant perchlorate environment. Survival and metabolic recovery were analyzed by quantitative PCR, gas chromatography, and a new DNA-extraction method from viable cells embedded in S-MRS and P-MRS. All strains survived the two Mars-like desiccating scenarios and recovered to different extents. The permafrost strain SMA-27 showed an increased methanogenic activity by at least 10-fold after deep-freezing conditions. The methanogenic rates of all strains did not decrease significantly after 128 days S-MRS exposure, except for SMA-27, which decreased 10-fold. The activity of strains SMA-17 and SMA-27 decreased after 16 and 60 days P-MRS exposure. Non-permafrost strains showed constant survival and methane production when exposed to both desiccating scenarios. All strains showed unaltered methane production when exposed to the perchlorate concentration reported at the Phoenix landing site (2.4 mM) or even higher concentrations. We conclude that methanogens from (non-)permafrost environments are suitable candidates for potential life in the martian subsurface and therefore are worthy of study after space exposure experiments that approach Mars-like surface conditions.
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Affiliation(s)
- Paloma Serrano
- 1 GFZ, German Research Centre for Geosciences, Helmholtz Centre Potsdam, Section Geomicrobiology, Potsdam, Germany
- 2 AWI, Alfred Wegener Institute, Helmholtz Centre for Polar and Marine Research, Potsdam, Germany
| | - Mashal Alawi
- 1 GFZ, German Research Centre for Geosciences, Helmholtz Centre Potsdam, Section Geomicrobiology, Potsdam, Germany
| | - Jean-Pierre de Vera
- 3 German Aerospace Center (DLR), Institute of Planetary Research, Management and Infrastructure, Research Group Astrobiological Laboratories, Berlin, Germany
| | - Dirk Wagner
- 1 GFZ, German Research Centre for Geosciences, Helmholtz Centre Potsdam, Section Geomicrobiology, Potsdam, Germany
- 4 University of Potsdam, Institute of Geosciences, Potsdam, Germany
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de Vera JP, Alawi M, Backhaus T, Baqué M, Billi D, Böttger U, Berger T, Bohmeier M, Cockell C, Demets R, de la Torre Noetzel R, Edwards H, Elsaesser A, Fagliarone C, Fiedler A, Foing B, Foucher F, Fritz J, Hanke F, Herzog T, Horneck G, Hübers HW, Huwe B, Joshi J, Kozyrovska N, Kruchten M, Lasch P, Lee N, Leuko S, Leya T, Lorek A, Martínez-Frías J, Meessen J, Moritz S, Moeller R, Olsson-Francis K, Onofri S, Ott S, Pacelli C, Podolich O, Rabbow E, Reitz G, Rettberg P, Reva O, Rothschild L, Sancho LG, Schulze-Makuch D, Selbmann L, Serrano P, Szewzyk U, Verseux C, Wadsworth J, Wagner D, Westall F, Wolter D, Zucconi L. Limits of Life and the Habitability of Mars: The ESA Space Experiment BIOMEX on the ISS. ASTROBIOLOGY 2019; 19:145-157. [PMID: 30742496 PMCID: PMC6383581 DOI: 10.1089/ast.2018.1897] [Citation(s) in RCA: 63] [Impact Index Per Article: 10.5] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 04/29/2018] [Accepted: 01/07/2019] [Indexed: 06/01/2023]
Abstract
BIOMEX (BIOlogy and Mars EXperiment) is an ESA/Roscosmos space exposure experiment housed within the exposure facility EXPOSE-R2 outside the Zvezda module on the International Space Station (ISS). The design of the multiuser facility supports-among others-the BIOMEX investigations into the stability and level of degradation of space-exposed biosignatures such as pigments, secondary metabolites, and cell surfaces in contact with a terrestrial and Mars analog mineral environment. In parallel, analysis on the viability of the investigated organisms has provided relevant data for evaluation of the habitability of Mars, for the limits of life, and for the likelihood of an interplanetary transfer of life (theory of lithopanspermia). In this project, lichens, archaea, bacteria, cyanobacteria, snow/permafrost algae, meristematic black fungi, and bryophytes from alpine and polar habitats were embedded, grown, and cultured on a mixture of martian and lunar regolith analogs or other terrestrial minerals. The organisms and regolith analogs and terrestrial mineral mixtures were then exposed to space and to simulated Mars-like conditions by way of the EXPOSE-R2 facility. In this special issue, we present the first set of data obtained in reference to our investigation into the habitability of Mars and limits of life. This project was initiated and implemented by the BIOMEX group, an international and interdisciplinary consortium of 30 institutes in 12 countries on 3 continents. Preflight tests for sample selection, results from ground-based simulation experiments, and the space experiments themselves are presented and include a complete overview of the scientific processes required for this space experiment and postflight analysis. The presented BIOMEX concept could be scaled up to future exposure experiments on the Moon and will serve as a pretest in low Earth orbit.
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Affiliation(s)
- Jean-Pierre de Vera
- German Aerospace Center (DLR), Institute of Planetary Research, Management and Infrastructure, Research Group Astrobiological Laboratories, Berlin, Germany
| | - Mashal Alawi
- GFZ, German Research Centre for Geosciences, Helmholtz Centre Potsdam, Section 5.3 Geomicrobiology, Telegrafenberg, Potsdam, Germany
| | - Theresa Backhaus
- Institut für Botanik, Heinrich-Heine-Universität (HHU), Düsseldorf, Germany
| | - Mickael Baqué
- German Aerospace Center (DLR), Institute of Planetary Research, Management and Infrastructure, Research Group Astrobiological Laboratories, Berlin, Germany
| | - Daniela Billi
- University of Rome Tor Vergata, Department of Biology, Rome, Italy
| | - Ute Böttger
- German Aerospace Center (DLR), Institute for Optical Sensor Systems, Berlin, Germany
| | - Thomas Berger
- German Aerospace Center (DLR), Institute of Aerospace Medicine, Radiation Biology Department, Köln, Germany
| | - Maria Bohmeier
- German Aerospace Center (DLR), Institute of Aerospace Medicine, Radiation Biology Department, Köln, Germany
| | - Charles Cockell
- School of Physics and Astronomy, University of Edinburgh, Edinburgh, UK
| | - René Demets
- European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Noordwijk, the Netherlands
| | - Rosa de la Torre Noetzel
- Departamento de Observación de la Tierra, Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain
| | - Howell Edwards
- Raman Spectroscopy Group, University Analytical Centre, Division of Chemical and Forensic Sciences, University of Bradford, West Yorkshire, UK
| | - Andreas Elsaesser
- Institut für experimentelle Physik, Experimentelle Molekulare Biophysik, Frei Universität Berlin, Berlin, Germany
| | | | - Annelie Fiedler
- University of Potsdam, Biodiversity Research/Systematic Botany, Potsdam, Germany
| | - Bernard Foing
- European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Noordwijk, the Netherlands
| | - Frédéric Foucher
- CNRS, Centre de Biophysique Moléculaire, UPR 4301, Orléans, France
| | - Jörg Fritz
- Museum für Naturkunde - Leibniz Institute for Evolution and Biodiversity Science, Berlin, Germany
| | - Franziska Hanke
- German Aerospace Center (DLR), Institute for Optical Sensor Systems, Berlin, Germany
| | - Thomas Herzog
- TH Wildau (Technical University of Applied Sciences), Wildau, Germany
| | - Gerda Horneck
- German Aerospace Center (DLR), Institute of Aerospace Medicine, Radiation Biology Department, Köln, Germany
| | - Heinz-Wilhelm Hübers
- German Aerospace Center (DLR), Institute for Optical Sensor Systems, Berlin, Germany
| | - Björn Huwe
- University of Potsdam, Biodiversity Research/Systematic Botany, Potsdam, Germany
| | - Jasmin Joshi
- University of Potsdam, Biodiversity Research/Systematic Botany, Potsdam, Germany
- Hochschule für Technik HSR Rapperswil, Institute for Landscape and Open Space, Rapperswil, Switzerland
| | | | - Martha Kruchten
- Institut für Botanik, Heinrich-Heine-Universität (HHU), Düsseldorf, Germany
| | - Peter Lasch
- Robert Koch Institute, Centre for Biological Threats and Special Pathogens, Berlin, Germany
| | - Natuschka Lee
- Department of Ecology and Environmental Sciences, Umeå University, Umeå, Sweden
| | - Stefan Leuko
- German Aerospace Center (DLR), Institute of Aerospace Medicine, Radiation Biology Department, Köln, Germany
| | - Thomas Leya
- Extremophile Research & Biobank CCCryo, Fraunhofer Institute for Cell Therapy and Immunology, Branch Bioanalytics and Bioprocesses (IZI-BB), Potsdam, Germany
| | - Andreas Lorek
- German Aerospace Center (DLR), Institute of Planetary Research, Management and Infrastructure, Research Group Astrobiological Laboratories, Berlin, Germany
| | | | - Joachim Meessen
- Institut für Botanik, Heinrich-Heine-Universität (HHU), Düsseldorf, Germany
| | - Sophie Moritz
- University of Potsdam, Biodiversity Research/Systematic Botany, Potsdam, Germany
| | - Ralf Moeller
- German Aerospace Center (DLR), Institute of Aerospace Medicine, Radiation Biology Department, Köln, Germany
| | - Karen Olsson-Francis
- School of Environment, Earth and Ecosystem Sciences, The Open University, Milton Keynes, UK
| | - Silvano Onofri
- Department of Ecological and Biological Sciences, University of Tuscia, Viterbo, Italy
| | - Sieglinde Ott
- Institut für Botanik, Heinrich-Heine-Universität (HHU), Düsseldorf, Germany
| | - Claudia Pacelli
- Department of Ecological and Biological Sciences, University of Tuscia, Viterbo, Italy
| | - Olga Podolich
- Institute of Molecular Biology & Genetics of NASU, Kyiv, Ukraine
| | - Elke Rabbow
- German Aerospace Center (DLR), Institute of Aerospace Medicine, Radiation Biology Department, Köln, Germany
| | - Günther Reitz
- German Aerospace Center (DLR), Institute of Aerospace Medicine, Radiation Biology Department, Köln, Germany
| | - Petra Rettberg
- German Aerospace Center (DLR), Institute of Aerospace Medicine, Radiation Biology Department, Köln, Germany
| | - Oleg Reva
- Centre for Bioinformatics and Computational Biology, Department of Biochemistry, Genetics and Microbiology, University of Pretoria, Pretoria, South Africa
| | | | | | | | - Laura Selbmann
- Department of Ecological and Biological Sciences, University of Tuscia, Viterbo, Italy
- Italian National Antarctic Museum (MNA), Mycological Section, Genoa, Italy
| | - Paloma Serrano
- GFZ, German Research Centre for Geosciences, Helmholtz Centre Potsdam, Section 5.3 Geomicrobiology, Telegrafenberg, Potsdam, Germany
- AWI, Alfred Wegener Institute, Helmholtz Centre for Polar and Marine Research, Potsdam, Germany
| | - Ulrich Szewzyk
- TU Berlin, Institute of Environmental Technology, Environmental Microbiology, Berlin, Germany
| | - Cyprien Verseux
- University of Rome Tor Vergata, Department of Biology, Rome, Italy
| | | | - Dirk Wagner
- GFZ, German Research Centre for Geosciences, Helmholtz Centre Potsdam, Section 5.3 Geomicrobiology, Telegrafenberg, Potsdam, Germany
- University of Potsdam, Institute of Earth and Environmental Sciences, Potsdam, Germany
| | - Frances Westall
- CNRS, Centre de Biophysique Moléculaire, UPR 4301, Orléans, France
| | - David Wolter
- German Aerospace Center (DLR), Institute of Planetary Research, Management and Infrastructure, Research Group Astrobiological Laboratories, Berlin, Germany
| | - Laura Zucconi
- Department of Ecological and Biological Sciences, University of Tuscia, Viterbo, Italy
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Mars scientists edge closer to solving methane mystery. Nature 2018; 563:18-19. [DOI: 10.1038/d41586-018-07177-4] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/08/2022]
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Neveu M, Hays LE, Voytek MA, New MH, Schulte MD. The Ladder of Life Detection. ASTROBIOLOGY 2018; 18:1375-1402. [PMID: 29862836 PMCID: PMC6211372 DOI: 10.1089/ast.2017.1773] [Citation(s) in RCA: 96] [Impact Index Per Article: 13.7] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/06/2017] [Accepted: 03/23/2018] [Indexed: 05/04/2023]
Abstract
We describe the history and features of the Ladder of Life Detection, a tool intended to guide the design of investigations to detect microbial life within the practical constraints of robotic space missions. To build the Ladder, we have drawn from lessons learned from previous attempts at detecting life and derived criteria for a measurement (or suite of measurements) to constitute convincing evidence for indigenous life. We summarize features of life as we know it, how specific they are to life, and how they can be measured, and sort these features in a general sense based on their likelihood of indicating life. Because indigenous life is the hypothesis of last resort in interpreting life-detection measurements, we propose a small but expandable set of decision rules determining whether the abiotic hypothesis is disproved. In light of these rules, we evaluate past and upcoming attempts at life detection. The Ladder of Life Detection is not intended to endorse specific biosignatures or instruments for life-detection measurements, and is by no means a definitive, final product. It is intended as a starting point to stimulate discussion, debate, and further research on the characteristics of life, what constitutes a biosignature, and the means to measure them.
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Affiliation(s)
- Marc Neveu
- NASA Postdoctoral Management Program Fellow, Universities Space Research Association, Columbia, Maryland
- NASA Headquarters, Washington, DC
| | - Lindsay E. Hays
- NASA Headquarters, Washington, DC
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
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Yung YL, Chen P, Nealson K, Atreya S, Beckett P, Blank JG, Ehlmann B, Eiler J, Etiope G, Ferry JG, Forget F, Gao P, Hu R, Kleinböhl A, Klusman R, Lefèvre F, Miller C, Mischna M, Mumma M, Newman S, Oehler D, Okumura M, Oremland R, Orphan V, Popa R, Russell M, Shen L, Sherwood Lollar B, Staehle R, Stamenković V, Stolper D, Templeton A, Vandaele AC, Viscardy S, Webster CR, Wennberg PO, Wong ML, Worden J. Methane on Mars and Habitability: Challenges and Responses. ASTROBIOLOGY 2018; 18:1221-1242. [PMID: 30234380 PMCID: PMC6205098 DOI: 10.1089/ast.2018.1917] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/07/2018] [Accepted: 06/12/2018] [Indexed: 05/05/2023]
Abstract
Recent measurements of methane (CH4) by the Mars Science Laboratory (MSL) now confront us with robust data that demand interpretation. Thus far, the MSL data have revealed a baseline level of CH4 (∼0.4 parts per billion by volume [ppbv]), with seasonal variations, as well as greatly enhanced spikes of CH4 with peak abundances of ∼7 ppbv. What do these CH4 revelations with drastically different abundances and temporal signatures represent in terms of interior geochemical processes, or is martian CH4 a biosignature? Discerning how CH4 generation occurs on Mars may shed light on the potential habitability of Mars. There is no evidence of life on the surface of Mars today, but microbes might reside beneath the surface. In this case, the carbon flux represented by CH4 would serve as a link between a putative subterranean biosphere on Mars and what we can measure above the surface. Alternatively, CH4 records modern geochemical activity. Here we ask the fundamental question: how active is Mars, geochemically and/or biologically? In this article, we examine geological, geochemical, and biogeochemical processes related to our overarching question. The martian atmosphere and surface are an overwhelmingly oxidizing environment, and life requires pairing of electron donors and electron acceptors, that is, redox gradients, as an essential source of energy. Therefore, a fundamental and critical question regarding the possibility of life on Mars is, "Where can we find redox gradients as energy sources for life on Mars?" Hence, regardless of the pathway that generates CH4 on Mars, the presence of CH4, a reduced species in an oxidant-rich environment, suggests the possibility of redox gradients supporting life and habitability on Mars. Recent missions such as ExoMars Trace Gas Orbiter may provide mapping of the global distribution of CH4. To discriminate between abiotic and biotic sources of CH4 on Mars, future studies should use a series of diagnostic geochemical analyses, preferably performed below the ground or at the ground/atmosphere interface, including measurements of CH4 isotopes, methane/ethane ratios, H2 gas concentration, and species such as acetic acid. Advances in the fields of Mars exploration and instrumentation will be driven, augmented, and supported by an improved understanding of atmospheric chemistry and dynamics, deep subsurface biogeochemistry, astrobiology, planetary geology, and geophysics. Future Mars exploration programs will have to expand the integration of complementary areas of expertise to generate synergistic and innovative ideas to realize breakthroughs in advancing our understanding of the potential of life and habitable conditions having existed on Mars. In this spirit, we conducted a set of interdisciplinary workshops. From this series has emerged a vision of technological, theoretical, and methodological innovations to explore the martian subsurface and to enhance spatial tracking of key volatiles, such as CH4.
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Affiliation(s)
- Yuk L. Yung
- California Institute of Technology, Pasadena, California
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | - Pin Chen
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | | | | | | | - Jennifer G. Blank
- NASA Ames Research Center, Blue Marble Space Institute of Science, Mountain View, California
| | - Bethany Ehlmann
- California Institute of Technology, Pasadena, California
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | - John Eiler
- California Institute of Technology, Pasadena, California
| | - Giuseppe Etiope
- Istituto Nazionale di Geofisica e Vulcanologia, Rome, Italy
- Faculty of Environmental Science and Engineering, Babes-Bolyai University, Cluj-Napoca, Romania
| | - James G. Ferry
- The Pennsylvania State University, University Park, Pennsylvania
| | - Francois Forget
- Laboratoire de Météorologie Dynamique, Institut Pierre Simon Laplace, CNRS, Paris, France
| | - Peter Gao
- University of California, Berkeley, California
| | - Renyu Hu
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | - Armin Kleinböhl
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | | | - Franck Lefèvre
- Laboratoire Atmospheres, Milieux, Observations Spatiales (LATMOS), IPSL, Paris, France
| | - Charles Miller
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | - Michael Mischna
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | - Michael Mumma
- NASA Goddard Space Flight Center, Greenbelt, Maryland
| | - Sally Newman
- California Institute of Technology, Pasadena, California
| | | | | | | | | | - Radu Popa
- University of Southern California, Los Angeles, California
| | - Michael Russell
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | - Linhan Shen
- California Institute of Technology, Pasadena, California
| | | | - Robert Staehle
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | - Vlada Stamenković
- California Institute of Technology, Pasadena, California
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | | | | | - Ann C. Vandaele
- The Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Sébastien Viscardy
- The Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Christopher R. Webster
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | | | | | - John Worden
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
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