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Sigvartssøn MKK, Bak EN, Nørnberg P, Jensen SJK, Thøgersen J, Begnhøj M, Finster K. Investigation of the Cytotoxicity of Mars-Relevant Minerals upon Abrasion. ASTROBIOLOGY 2023; 23:1090-1098. [PMID: 37672600 DOI: 10.1089/ast.2023.0015] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 09/08/2023]
Abstract
Since the Viking Labeled Release experiments were carried out on Mars in the 1970s, it has been evident that the martian surface regolith has a strong oxidizing capacity that can convert organic compounds into CO2 and probably water. While H2O2 was suggested originally for being the oxidizing agent responsible for the outcome of the Viking experiments, recent analyses of the martian regolith by the Phoenix lander and by consecutive missions point toward radiation-mediated decomposition products of perchlorate salts as the primary oxidant. In a series of experiments, we have shown that abrasion and triboelectric charging of basalt by simulated saltation could be an additional way of activating regolith. We have also shown that abraded basalt with a chemical composition close to that of martian regolith is toxic to several bacterial species and thus may affect the habitability of the martian surface. In the present study, we investigated the effect of the quantitatively most important minerals (olivine, augite, and plagioclase) and iron oxides (hematite, magnetite, and maghemite) on the survival of bacterial cells to elucidate whether a specific mineral that constitutes basalt is responsible for our observations. We observed that suspensions of iron-containing minerals olivine and augite in phosphate-buffered saline (1 × PBS) significantly reduce the number of surviving cells of our model organism Pseudomonas putida after 24 h of incubation. In contrast, the iron-free mineral plagioclase showed no effect. We also observed that suspending abraded olivine and augite in 1 × PBS led to a dramatic increase in pH compared to the pH of 1 × PBS alone. The sudden increase in pH caused by the presence of these minerals may partly explain the observed cytotoxicity. The cytotoxic effect of augite could be relieved when a strong buffer (20 × PBS) was used. In contrast, olivine, despite the stronger buffer, maintained its cytotoxicity. Iron oxides per se have no negative effect on the survival of our test organism. Overall, our experiments confirm the cytotoxicity of basalt and show that no single constituent mineral of the basalt can account for its toxicity. We could show that abraded iron-containing minerals (olivine and augite) change the pH of water when brought into suspension and thereby could affect the habitability of martian regolith.
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Affiliation(s)
| | - Ebbe Norskov Bak
- Department of Biology, Microbiology section, Aarhus University, Aarhus C, Denmark
| | - Per Nørnberg
- Department of Biology, Microbiology section, Aarhus University, Aarhus C, Denmark
- Department of Geoscience, Aarhus University, Aarhus C, Denmark
| | | | - Jan Thøgersen
- Department of Chemistry, Aarhus University, Aarhus C, Denmark
| | - Mikkel Begnhøj
- Department of Biology, Microbiology section, Aarhus University, Aarhus C, Denmark
- Department of Chemistry, Aarhus University, Aarhus C, Denmark
| | - Kai Finster
- Department of Biology, Microbiology section, Aarhus University, Aarhus C, Denmark
- Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Aarhus C, Denmark
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Mao W, Fu X, Wu Z, Zhang J, Ling Z, Liu Y, Zhao YYS, Changela HG, Ni Y, Yan F, Zou Y. Solid-gas carbonate formation during dust events on Mars. Natl Sci Rev 2023; 10:nwac293. [PMID: 36960225 PMCID: PMC10029838 DOI: 10.1093/nsr/nwac293] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/27/2022] [Revised: 12/24/2022] [Accepted: 01/04/2023] [Indexed: 01/13/2023] Open
Abstract
Electrostatic discharge experiments under simulated martian atmospheric conditions indicate that atmospheric CO2 has been sequestered into carbonate by the Mars dust activities during the Amazonia era.
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Affiliation(s)
- Wenshuo Mao
- Shandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, School of Space Science and Physics, Institute of Space Sciences, Shandong University, China
| | - Xiaohui Fu
- Shandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, School of Space Science and Physics, Institute of Space Sciences, Shandong University, China
- CAS Center for Excellence in Comparative Planetology, China
| | - Zhongchen Wu
- Shandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, School of Space Science and Physics, Institute of Space Sciences, Shandong University, China
| | - Jiang Zhang
- Shandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, School of Space Science and Physics, Institute of Space Sciences, Shandong University, China
| | - Zongcheng Ling
- Shandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, School of Space Science and Physics, Institute of Space Sciences, Shandong University, China
- CAS Center for Excellence in Comparative Planetology, China
| | - Yang Liu
- State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, China
| | - Yu-Yan Sara Zhao
- International Center for Planetary Science, College of Earth Science, Chengdu University of Technology, China
- CAS Center for Excellence in Comparative Planetology, China
| | - Hitesh G Changela
- J’Heyrovski Institute of Physical Chemistry, Czech Academy of Sciences, Czech Republic
- Department of Earth & Planetary Science, University of New Mexico, USA
| | - Yuheng Ni
- Shandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, School of Space Science and Physics, Institute of Space Sciences, Shandong University, China
| | - Fabao Yan
- School of Mechanical, Electrical & Information Engineering, Shandong University, China
| | - Yongliao Zou
- State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, China
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Rodriguez JAP, Robertson DK, Kargel JS, Baker VR, Berman DC, Cohen J, Costard F, Komatsu G, Lopez A, Miyamoto H, Zarroca M. Evidence of an oceanic impact and megatsunami sedimentation in Chryse Planitia, Mars. Sci Rep 2022; 12:19589. [PMID: 36456647 PMCID: PMC9715952 DOI: 10.1038/s41598-022-18082-2] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/09/2021] [Accepted: 08/04/2022] [Indexed: 12/05/2022] Open
Abstract
In 1976, NASA's Viking 1 Lander (V1L) was the first spacecraft to operate successfully on the Martian surface. The V1L landed near the terminus of an enormous catastrophic flood channel, Maja Valles. However, instead of the expected megaflood record, its cameras imaged a boulder-strewn surface of elusive origin. We identified a 110-km-diameter impact crater (Pohl) ~ 900 km northeast of the landing site, stratigraphically positioned (a) above catastrophic flood-eroded surfaces formed ~ 3.4 Ga during a period of northern plains oceanic inundation and (b) below the younger of two previously hypothesized megatsunami deposits. These stratigraphic relationships suggest that a marine impact likely formed the crater. Our simulated impact-generated megatsunami run-ups closely match the mapped older megatsunami deposit's margins and predict fronts reaching the V1L site. The site's location along a highland-facing lobe aligned to erosional grooves supports a megatsunami origin. Our mapping also shows that Pohl's knobby rim regionally represents a broader history of megatsunami modification involving circum-oceanic glaciation and sedimentary extrusions extending beyond the recorded megatsunami emplacement in Chryse Planitia. Our findings allow that rocks and soil salts at the landing site are of marine origin, inviting the scientific reconsideration of information gathered from the first in-situ measurements on Mars.
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Affiliation(s)
- J. Alexis P. Rodriguez
- grid.423138.f0000 0004 0637 3991Planetary Science Institute, 1700 East Fort Lowell Road, Suite 106, Tucson, AZ 85719-2395 USA
| | - Darrel K. Robertson
- grid.419075.e0000 0001 1955 7990NASA Ames Research Center, Moffett Field, CA 94035 USA
| | - Jeffrey S. Kargel
- grid.423138.f0000 0004 0637 3991Planetary Science Institute, 1700 East Fort Lowell Road, Suite 106, Tucson, AZ 85719-2395 USA
| | - Victor R. Baker
- grid.134563.60000 0001 2168 186XDepartment of Hydrology and Atmospheric Sciences, University of Arizona, Tucson, AZ 85721 USA
| | - Daniel C. Berman
- grid.423138.f0000 0004 0637 3991Planetary Science Institute, 1700 East Fort Lowell Road, Suite 106, Tucson, AZ 85719-2395 USA
| | - Jacob Cohen
- grid.419075.e0000 0001 1955 7990NASA Ames Research Center, Moffett Field, CA 94035 USA
| | - Francois Costard
- grid.503243.3GEOPS-Géosciences Paris Sud, Université Paris-Sud, CNRS, Université Paris-Saclay, 91405 Orsay, France
| | - Goro Komatsu
- grid.412451.70000 0001 2181 4941International Research School of Planetary Sciences, Università D’Annunzio, Viale Pindaro 42, 65127 Pescara, Italy
| | - Anthony Lopez
- grid.423138.f0000 0004 0637 3991Planetary Science Institute, 1700 East Fort Lowell Road, Suite 106, Tucson, AZ 85719-2395 USA
| | - Hideaki Miyamoto
- grid.26999.3d0000 0001 2151 536XDepartment of Systems Innovation, University of Tokyo, Tokyo, 113-8656 Japan
| | - Mario Zarroca
- grid.7080.f0000 0001 2296 0625External Geodynamics and Hydrogeology Group, Department of Geology, Autonomous University of Barcelona, 08193 Bellaterra, Barcelona, Spain
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Cassaro A, Pacelli C, Onofri S. Survival, metabolic activity, and ultrastructural damages of Antarctic black fungus in perchlorates media. Front Microbiol 2022; 13:992077. [PMID: 36523839 PMCID: PMC9744811 DOI: 10.3389/fmicb.2022.992077] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/12/2022] [Accepted: 10/06/2022] [Indexed: 09/12/2023] Open
Abstract
Evidence from recent Mars landers identified the presence of perchlorates salts at 1 wt % in regolith and their widespread distribution on the Martian surface that has been hypothesized as a critical chemical hazard for putative life forms. However, the hypersaline environment may also potentially preserve life and its biomolecules over geological timescales. The high concentration of natural perchlorates is scarcely reported on Earth. The presence of perchlorates in soil and ice has been recorded in some extreme environments including the McMurdo Dry Valleys in Antarctica, one of the best terrestrial analogues for Mars. In the frame of "Life in space" Italian astrobiology project, the polyextremophilic black fungus Cryomyces antarcticus, a eukaryotic test organism isolated from the Antarctic cryptoendolithic communities, has been tested for its resistance, when grown on different hypersaline substrata. In addition, C. antarcticus was grown on Martian relevant perchlorate medium (0.4 wt% of Mg(ClO4)2 and 0.6 wt% of Ca(ClO4)2) to investigate the possibility for the fungus to survive in Martian environment. Here, the results indicate a good survivability and metabolic activity recovery of the black fungus when grown on four Martian relevant perchlorates. A low percentage of damaged cellular membranes have been found, confirming the ultrastructural investigation.
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Affiliation(s)
- Alessia Cassaro
- Department of Ecological and Biological Sciences, University of Tuscia, Largo dell’Università snc, Viterbo, Italy
| | - Claudia Pacelli
- Department of Ecological and Biological Sciences, University of Tuscia, Largo dell’Università snc, Viterbo, Italy
- Human Spaceflight and Scientific Research Unit, Italian Space Agency, via del Politecnico, Rome, Italy
| | - Silvano Onofri
- Department of Ecological and Biological Sciences, University of Tuscia, Largo dell’Università snc, Viterbo, Italy
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Abstract
To assess Mars’ potential for both harboring life and providing useable resources for future human exploration, it is of paramount importance to comprehend the water situation on the planet. Therefore, studies have been conducted to determine any evidence of past or present water existence on Mars. While the presence of abundant water on Mars very early in its history is widely accepted, on its modern form, only a fraction of this water can be found, as either ice or locked into the structure of Mars’ plentiful water-rich materials. Water on the planet is evaluated through various evidence such as rocks and minerals, Martian achondrites, low volume transient briny outflows (e.g., dune flows, reactivated gullies, slope streaks, etc.), diurnal shallow soil moisture (e.g., measurements by Curiosity and Phoenix Lander), geomorphic representation (possibly from lakes and river valleys), and groundwater, along with further evidence obtained by probe and rover discoveries. One of the most significant lines of evidence is for an ancient streambed in Gale Crater, implying ancient amounts of “vigorous” water on Mars. Long ago, hospitable conditions for microbial life existed on the surface of Mars, as it was likely periodically wet. However, its current dry surface makes it almost impossible as an appropriate environment for living organisms; therefore, scientists have recognized the planet’s subsurface environments as the best potential locations for exploring life on Mars. As a result, modern research has aimed towards discovering underground water, leading to the discovery of a large amount of underground ice in 2016 by NASA, and a subglacial lake in 2018 by Italian scientists. Nevertheless, the presence of life in Mars’ history is still an open question. In this unifying context, the current review summarizes results from a wide variety of studies and reports related to the history of water on Mars, as well as any related discussions on the possibility of living organism existence on the planet.
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Williams AJ, Eigenbrode J, Floyd M, Wilhelm MB, O'Reilly S, Johnson SS, Craft KL, Knudson CA, Andrejkovičová S, Lewis JM, Buch A, Glavin DP, Freissinet C, Williams RH, Szopa C, Millan M, Summons RE, McAdam A, Benison K, Navarro-González R, Malespin C, Mahaffy PR. Recovery of Fatty Acids from Mineralogic Mars Analogs by TMAH Thermochemolysis for the Sample Analysis at Mars Wet Chemistry Experiment on the Curiosity Rover. ASTROBIOLOGY 2019; 19:522-546. [PMID: 30869535 PMCID: PMC6459279 DOI: 10.1089/ast.2018.1819] [Citation(s) in RCA: 14] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/08/2018] [Accepted: 01/14/2019] [Indexed: 05/21/2023]
Abstract
The Mars Curiosity rover carries a diverse instrument payload to characterize habitable environments in the sedimentary layers of Aeolis Mons. One of these instruments is Sample Analysis at Mars (SAM), which contains a mass spectrometer that is capable of detecting organic compounds via pyrolysis gas chromatography mass spectrometry (py-GC-MS). To identify polar organic molecules, the SAM instrument carries the thermochemolysis reagent tetramethylammonium hydroxide (TMAH) in methanol (hereafter referred to as TMAH). TMAH can liberate fatty acids bound in macromolecules or chemically bound monomers associated with mineral phases and make these organics detectable via gas chromatography mass spectrometry (GC-MS) by methylation. Fatty acids, a type of carboxylic acid that contains a carboxyl functional group, are of particular interest given their presence in both biotic and abiotic materials. This work represents the first analyses of a suite of Mars-analog samples using the TMAH experiment under select SAM-like conditions. Samples analyzed include iron oxyhydroxides and iron oxyhydroxysulfates, a mixture of iron oxides/oxyhydroxides and clays, iron sulfide, siliceous sinter, carbonates, and shale. The TMAH experiments produced detectable signals under SAM-like pyrolysis conditions when organics were present either at high concentrations or in geologically modern systems. Although only a few analog samples exhibited a high abundance and variety of fatty acid methyl esters (FAMEs), FAMEs were detected in the majority of analog samples tested. When utilized, the TMAH thermochemolysis experiment on SAM could be an opportunity to detect organic molecules bound in macromolecules on Mars. The detection of a FAME profile is of great astrobiological interest, as it could provide information regarding the source of martian organic material detected by SAM.
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Affiliation(s)
- Amy J. Williams
- Department of Physics, Astronomy, and Geosciences, Towson University, Towson, Maryland, USA
- Center for Research and Exploration in Space Sciences and Technology/University of Maryland Baltimore County, Baltimore, Maryland, USA
- Space Science Exploration Division (Code 690), NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
| | - Jennifer Eigenbrode
- Space Science Exploration Division (Code 690), NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
| | - Melissa Floyd
- Space Science Exploration Division (Code 690), NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
| | | | - Shane O'Reilly
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, Massachusetts, USA
- School of Earth Sciences, University College Dublin, Dublin, Ireland
| | | | - Kathleen L. Craft
- Johns Hopkins University Applied Physics Laboratory, Laurel, Maryland, USA
| | - Christine A. Knudson
- Space Science Exploration Division (Code 690), NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
- Center for Research and Exploration in Space Sciences and Technology/University of Maryland College Park, College Park, Maryland, USA
| | - Slavka Andrejkovičová
- Space Science Exploration Division (Code 690), NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
- Center for Research and Exploration in Space Sciences and Technology/University of Maryland College Park, College Park, Maryland, USA
| | - James M.T. Lewis
- Space Science Exploration Division (Code 690), NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
- Universities Space Research Association, Columbia, Maryland, USA
| | - Arnaud Buch
- Laboratoire de Génie des Procédés et Matériaux, CentraleSupelec, Gif sur Yvette, France
| | - Daniel P. Glavin
- Space Science Exploration Division (Code 690), NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
| | - Caroline Freissinet
- CNRS–UVSQ Laboratoire Atmosphères Milieux Observations Spatiales LATMOS, Guyancourt, France
| | - Ross H. Williams
- Space Science Exploration Division (Code 690), NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
- Center for Research and Exploration in Space Sciences and Technology/University of Maryland College Park, College Park, Maryland, USA
| | - Cyril Szopa
- CNRS–UVSQ Laboratoire Atmosphères Milieux Observations Spatiales LATMOS, Guyancourt, France
| | - Maëva Millan
- Space Science Exploration Division (Code 690), NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
- Department of Biology, Georgetown University, Washington, DC, USA
| | - Roger E. Summons
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, Massachusetts, USA
| | - Amy McAdam
- Space Science Exploration Division (Code 690), NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
| | - Kathleen Benison
- Department of Geology and Geography, West Virginia University, Morgantown, West Virginia, USA
| | - Rafael Navarro-González
- Instituto de Ciencias Nucleares, Universidad Nacional Autonoma de Mexico, Circuito Exterior, Ciudad Universitaria, Ciudad de Mexico, Mexico
| | - Charles Malespin
- Space Science Exploration Division (Code 690), NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
| | - Paul R. Mahaffy
- Space Science Exploration Division (Code 690), NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
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Bhardwaj A, Sam L, Martín-Torres FJ, Zorzano MP. Discovery of recurring slope lineae candidates in Mawrth Vallis, Mars. Sci Rep 2019; 9:2040. [PMID: 30765841 PMCID: PMC6376049 DOI: 10.1038/s41598-019-39599-z] [Citation(s) in RCA: 9] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/14/2018] [Accepted: 01/28/2019] [Indexed: 11/09/2022] Open
Abstract
Several interpretations of recurring slope lineae (RSL) have related RSL to the potential presence of transient liquid water on Mars. Such probable signs of liquid water have implications for Mars exploration in terms of rover safety, planetary protection during rover operations, and the current habitability of the planet. Mawrth Vallis has always been a prime target to be considered for Mars rover missions due to its rich mineralogy. Most recently, Mawrth Vallis was one of the two final candidates selected by the European Space Agency as a landing site for the ExoMars 2020 mission. Therefore, all surface features and landforms in Mawrth Vallis that may be of special interest in terms of scientific goals, rover safety, and operations must be scrutinised to better assess it for future Mars missions. Here, we report on the initial detection of RSL candidates in two craters of Mawrth Vallis. The new sightings were made outside of established RSL regions and further prompt the inclusion of a new geographical region within the RSL candidate group. Our inferences on the RSL candidates are based on several morphological and geophysical evidences and analogies: (i) the dimensions of the RSL candidates are consistent with confirmed mid-latitude RSL; (ii) albedo and thermal inertia values are comparable to those of other mid-latitude RSL sites; and (iii) features are found in a summer season image and on the steep and warmest slopes. These results denote the plausible presence of transient liquid brines close to the previously proposed landing ellipse of the ExoMars rover, rendering this site particularly relevant to the search of life. Further investigations of Mawrth Vallis carried out at higher spatial and temporal resolutions are needed to identify more of such features at local scales to maximize the scientific return from the future Mars rovers, to prevent probable biological contamination during rover operations, to evade damage to rover components as brines can be highly corrosive, and to quantify the ability of the regolith at mid-latitudes to capture atmospheric water which is relevant for in-situ-resource utilization.
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Affiliation(s)
- Anshuman Bhardwaj
- Division of Space Technology, Department of Computer Science, Electrical and Space Engineering, Luleå University of Technology, Luleå, Sweden.
| | - Lydia Sam
- Division of Space Technology, Department of Computer Science, Electrical and Space Engineering, Luleå University of Technology, Luleå, Sweden
- Institut für Kartographie, Technische Universität Dresden, Dresden, Germany
| | - F Javier Martín-Torres
- Division of Space Technology, Department of Computer Science, Electrical and Space Engineering, Luleå University of Technology, Luleå, Sweden
- Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Armilla, Granada, Spain
- UK Centre for Astrobiology, School of Physics and Astronomy, University of Edinburgh, Edinburgh, UK
| | - María-Paz Zorzano
- Division of Space Technology, Department of Computer Science, Electrical and Space Engineering, Luleå University of Technology, Luleå, Sweden
- Centro de Astrobiología (INTA-CSIC), 28850, Torrejón de Ardoz, Madrid, Spain
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Martian slope streaks as plausible indicators of transient water activity. Sci Rep 2017; 7:7074. [PMID: 28765566 PMCID: PMC5539097 DOI: 10.1038/s41598-017-07453-9] [Citation(s) in RCA: 33] [Impact Index Per Article: 4.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/13/2017] [Accepted: 06/27/2017] [Indexed: 12/05/2022] Open
Abstract
Slope streaks have been frequently observed in the equatorial, low thermal inertia and dusty regions of Mars. The reason behind their formation remains unclear with proposed hypotheses for both dry and wet mechanisms. Here, we report an up-to-date distribution and morphometric investigation of Martian slope streaks. We find: (i) a remarkable coexistence of the slope streak distribution with the regions on Mars with high abundances of water-equivalent hydrogen, chlorine, and iron; (ii) favourable thermodynamic conditions for transient deliquescence and brine development in the slope streak regions; (iii) a significant concurrence of slope streak distribution with the regions of enhanced atmospheric water vapour concentration, thus suggestive of a present-day regolith-atmosphere water cycle; and (iv) terrain preferences and flow patterns supporting a wet mechanism for slope streaks. These results suggest a strong local regolith-atmosphere water coupling in the slope streak regions that leads to the formation of these fluidised features. Our conclusions can have profound astrobiological, habitability, environmental, and planetary protection implications.
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Martín-Torres J, Zorzano MP. Should We Invest in Martian Brine Research to Reduce Mars Exploration Costs? ASTROBIOLOGY 2017; 17:3-7. [PMID: 28026989 PMCID: PMC5278815 DOI: 10.1089/ast.2016.1602] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/11/2023]
Affiliation(s)
- Javier Martín-Torres
- Division of Space Technology, Department of Computer Science, Electrical and Space Engineering, Luleå University of Technology, Kiruna, Sweden
- Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain
| | - María-Paz Zorzano
- Division of Space Technology, Department of Computer Science, Electrical and Space Engineering, Luleå University of Technology, Kiruna, Sweden
- Centro de Astrobiología (CSIC-INTA), Madrid, Spain
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Wilson EH, Atreya SK, Kaiser RI, Mahaffy PR. Perchlorate formation on Mars through surface radiolysis-initiated atmospheric chemistry: A potential mechanism. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2016; 121:1472-1487. [PMID: 27774369 PMCID: PMC5054826 DOI: 10.1002/2016je005078] [Citation(s) in RCA: 7] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/18/2016] [Revised: 08/02/2016] [Accepted: 08/03/2016] [Indexed: 05/31/2023]
Abstract
Recent observations of the Martian surface by the Phoenix lander and the Sample Analysis at Mars indicate the presence of perchlorate (ClO4-). The abundance and isotopic composition of these perchlorates suggest that the mechanisms responsible for their formation in the Martian environment may be unique in our solar system. With this in mind, we propose a potential mechanism for the production of Martian perchlorate: the radiolysis of the Martian surface by galactic cosmic rays, followed by the sublimation of chlorine oxides into the atmosphere and their subsequent synthesis to form perchloric acid (HClO4) in the atmosphere, and the surface deposition and subsequent mineralization of HClO4 in the regolith to form surface perchlorates. To evaluate the viability of this mechanism, we employ a one-dimensional chemical model, examining chlorine chemistry in the context of Martian atmospheric chemistry. Considering the chlorine oxide, OClO, we find that an OClO flux as low as 3.2 × 107 molecules cm-2 s-1 sublimated into the atmosphere from the surface could produce sufficient HClO4 to explain the perchlorate concentration on Mars, assuming an accumulation depth of 30 cm and integrated over the Amazonian period. Radiolysis provides an efficient pathway for the oxidation of chlorine, bypassing the efficient Cl/HCl recycling mechanism that characterizes HClO4 formation mechanisms proposed for the Earth but not Mars.
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Affiliation(s)
- Eric H. Wilson
- Department of Climate and Space Sciences and EngineeringUniversity of MichiganAnn ArborMichiganUSA
| | - Sushil K. Atreya
- Department of Climate and Space Sciences and EngineeringUniversity of MichiganAnn ArborMichiganUSA
| | - Ralf I. Kaiser
- Department of ChemistryUniversity of Hawai'i at MānoaHonoluluHawaiiUSA
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Freissinet C, Glavin DP, Mahaffy PR, Miller KE, Eigenbrode JL, Summons RE, Brunner AE, Buch A, Szopa C, Archer PD, Franz HB, Atreya SK, Brinckerhoff WB, Cabane M, Coll P, Conrad PG, Des Marais DJ, Dworkin JP, Fairén AG, François P, Grotzinger JP, Kashyap S, ten Kate IL, Leshin LA, Malespin CA, Martin MG, Martin-Torres FJ, McAdam AC, Ming DW, Navarro-González R, Pavlov AA, Prats BD, Squyres SW, Steele A, Stern JC, Sumner DY, Sutter B, Zorzano MP. Organic molecules in the Sheepbed Mudstone, Gale Crater, Mars. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2015; 120:495-514. [PMID: 26690960 PMCID: PMC4672966 DOI: 10.1002/2014je004737] [Citation(s) in RCA: 160] [Impact Index Per Article: 17.8] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/03/2014] [Revised: 01/12/2015] [Accepted: 02/13/2015] [Indexed: 05/04/2023]
Abstract
UNLABELLED The Sample Analysis at Mars (SAM) instrument on board the Mars Science Laboratory Curiosity rover is designed to conduct inorganic and organic chemical analyses of the atmosphere and the surface regolith and rocks to help evaluate the past and present habitability potential of Mars at Gale Crater. Central to this task is the development of an inventory of any organic molecules present to elucidate processes associated with their origin, diagenesis, concentration, and long-term preservation. This will guide the future search for biosignatures. Here we report the definitive identification of chlorobenzene (150-300 parts per billion by weight (ppbw)) and C2 to C4 dichloroalkanes (up to 70 ppbw) with the SAM gas chromatograph mass spectrometer (GCMS) and detection of chlorobenzene in the direct evolved gas analysis (EGA) mode, in multiple portions of the fines from the Cumberland drill hole in the Sheepbed mudstone at Yellowknife Bay. When combined with GCMS and EGA data from multiple scooped and drilled samples, blank runs, and supporting laboratory analog studies, the elevated levels of chlorobenzene and the dichloroalkanes cannot be solely explained by instrument background sources known to be present in SAM. We conclude that these chlorinated hydrocarbons are the reaction products of Martian chlorine and organic carbon derived from Martian sources (e.g., igneous, hydrothermal, atmospheric, or biological) or exogenous sources such as meteorites, comets, or interplanetary dust particles. KEY POINTS First in situ evidence of nonterrestrial organics in Martian surface sediments Chlorinated hydrocarbons identified in the Sheepbed mudstone by SAM Organics preserved in sample exposed to ionizing radiation and oxidative condition.
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Affiliation(s)
- C Freissinet
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
- NASA Postdoctoral Program, Oak Ridge Associated UniversitiesOak Ridge, Tennessee, USA
- Correspondence to:
C. Freissinet and P. R. Mahaffy,, ,
| | - D P Glavin
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - P R Mahaffy
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
- Correspondence to:
C. Freissinet and P. R. Mahaffy,, ,
| | - K E Miller
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of TechnologyCambridge, Massachusetts, USA
| | - J L Eigenbrode
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - R E Summons
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of TechnologyCambridge, Massachusetts, USA
| | - A E Brunner
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
- Center for Research and Exploration in Space Science & Technology, University of MarylandCollege Park, Maryland, USA
| | - A Buch
- Laboratoire de Génie des Procédés et Matériaux, Ecole Centrale ParisChâtenay-Malabry, France
| | - C Szopa
- Laboratoire Atmosphères, Milieux, Observations Spatiales, Pierre and Marie Curie University, Université de Versailles Saint-Quentin-en-Yvelines, and CNRSParis, France
| | - P D Archer
- Jacobs, NASA Johnson Space CenterHouston, Texas, USA
| | - H B Franz
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
- Center for Research and Exploration in Space Science & Technology, University of Maryland, Baltimore CountyBaltimore, Maryland, USA
| | - S K Atreya
- Department of Atmospheric, Oceanic and Space Sciences, University of MichiganAnn Arbor, Michigan, USA
| | - W B Brinckerhoff
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - M Cabane
- Laboratoire Atmosphères, Milieux, Observations Spatiales, Pierre and Marie Curie University, Université de Versailles Saint-Quentin-en-Yvelines, and CNRSParis, France
| | - P Coll
- Laboratoire Interuniversitaire des Systèmes Atmosphériques, Université Paris-Est Créteil, Paris VII–Denis Diderot University, and CNRSCréteil, France
| | - P G Conrad
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - D J Des Marais
- Exobiology Branch, NASA Ames Research CenterMoffett Field, California, USA
| | - J P Dworkin
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - A G Fairén
- Department of Astronomy, Cornell UniversityIthaca, New York, USA
- Centro de Astrobiología, INTA-CSICMadrid, Spain
| | - P François
- Department of Atmospheric, Oceanic and Space Sciences, University of MichiganAnn Arbor, Michigan, USA
| | - J P Grotzinger
- Division of Geological and Planetary Sciences, California Institute of TechnologyPasadena, California, USA
| | - S Kashyap
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
- Center for Research and Exploration in Space Science & Technology, University of Maryland, Baltimore CountyBaltimore, Maryland, USA
| | - I L ten Kate
- Earth Sciences Department, Utrecht UniversityUtrecht, Netherlands
| | - L A Leshin
- Department of Earth and Environmental Sciences and School of Science, Rensselaer Polytechnic InstituteTroy, New York, USA
| | - C A Malespin
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
- Goddard Earth Sciences and Technologies and Research, Universities Space Research AssociationColumbia, Maryland, USA
| | - M G Martin
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
- Department of Chemistry, Catholic University of AmericaWashington, District of Columbia, USA
| | - F J Martin-Torres
- Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR)Granada, Spain
- Division of Space Technology, Department of Computer Science, Electrical and Space Engineering, Luleå University of TechnologyKiruna, Sweden
| | - A C McAdam
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - D W Ming
- Astromaterials Research and Exploration Science Directorate, NASA Johnson Space CenterHouston, Texas, USA
| | - R Navarro-González
- Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Ciudad UniversitariaMéxico City, Mexico
| | - A A Pavlov
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - B D Prats
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - S W Squyres
- Department of Astronomy, Cornell UniversityIthaca, New York, USA
| | - A Steele
- Geophysical Laboratory, Carnegie Institution of WashingtonWashington, District of Columbia, USA
| | - J C Stern
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - D Y Sumner
- Department of Earth and Planetary Sciences, University of CaliforniaDavis, California, USA
| | - B Sutter
- Jacobs, NASA Johnson Space CenterHouston, Texas, USA
| | - M-P Zorzano
- Centro de Astrobiologia (INTA-CSIC)Madrid, Spain
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12
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Freissinet C, Glavin DP, Mahaffy PR, Miller KE, Eigenbrode JL, Summons RE, Brunner AE, Buch A, Szopa C, Archer PD, Franz HB, Atreya SK, Brinckerhoff WB, Cabane M, Coll P, Conrad PG, Des Marais DJ, Dworkin JP, Fairén AG, François P, Grotzinger JP, Kashyap S, Ten Kate IL, Leshin LA, Malespin CA, Martin MG, Martin-Torres FJ, McAdam AC, Ming DW, Navarro-González R, Pavlov AA, Prats BD, Squyres SW, Steele A, Stern JC, Sumner DY, Sutter B, Zorzano MP. Organic molecules in the Sheepbed Mudstone, Gale Crater, Mars. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2015; 120:495-514. [PMID: 26690960 DOI: 10.1002/2015je004884.received] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Key Words] [Subscribe] [Scholar Register] [Received: 10/03/2014] [Revised: 01/12/2015] [Accepted: 02/13/2015] [Indexed: 05/25/2023]
Abstract
UNLABELLED The Sample Analysis at Mars (SAM) instrument on board the Mars Science Laboratory Curiosity rover is designed to conduct inorganic and organic chemical analyses of the atmosphere and the surface regolith and rocks to help evaluate the past and present habitability potential of Mars at Gale Crater. Central to this task is the development of an inventory of any organic molecules present to elucidate processes associated with their origin, diagenesis, concentration, and long-term preservation. This will guide the future search for biosignatures. Here we report the definitive identification of chlorobenzene (150-300 parts per billion by weight (ppbw)) and C2 to C4 dichloroalkanes (up to 70 ppbw) with the SAM gas chromatograph mass spectrometer (GCMS) and detection of chlorobenzene in the direct evolved gas analysis (EGA) mode, in multiple portions of the fines from the Cumberland drill hole in the Sheepbed mudstone at Yellowknife Bay. When combined with GCMS and EGA data from multiple scooped and drilled samples, blank runs, and supporting laboratory analog studies, the elevated levels of chlorobenzene and the dichloroalkanes cannot be solely explained by instrument background sources known to be present in SAM. We conclude that these chlorinated hydrocarbons are the reaction products of Martian chlorine and organic carbon derived from Martian sources (e.g., igneous, hydrothermal, atmospheric, or biological) or exogenous sources such as meteorites, comets, or interplanetary dust particles. KEY POINTS First in situ evidence of nonterrestrial organics in Martian surface sediments Chlorinated hydrocarbons identified in the Sheepbed mudstone by SAM Organics preserved in sample exposed to ionizing radiation and oxidative condition.
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Affiliation(s)
- C Freissinet
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA ; NASA Postdoctoral Program, Oak Ridge Associated Universities Oak Ridge, Tennessee, USA
| | - D P Glavin
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - P R Mahaffy
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - K E Miller
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology Cambridge, Massachusetts, USA
| | - J L Eigenbrode
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - R E Summons
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology Cambridge, Massachusetts, USA
| | - A E Brunner
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA ; Center for Research and Exploration in Space Science & Technology, University of Maryland College Park, Maryland, USA
| | - A Buch
- Laboratoire de Génie des Procédés et Matériaux, Ecole Centrale Paris Châtenay-Malabry, France
| | - C Szopa
- Laboratoire Atmosphères, Milieux, Observations Spatiales, Pierre and Marie Curie University, Université de Versailles Saint-Quentin-en-Yvelines, and CNRS Paris, France
| | - P D Archer
- Jacobs, NASA Johnson Space Center Houston, Texas, USA
| | - H B Franz
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA ; Center for Research and Exploration in Space Science & Technology, University of Maryland, Baltimore County Baltimore, Maryland, USA
| | - S K Atreya
- Department of Atmospheric, Oceanic and Space Sciences, University of Michigan Ann Arbor, Michigan, USA
| | - W B Brinckerhoff
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - M Cabane
- Laboratoire Atmosphères, Milieux, Observations Spatiales, Pierre and Marie Curie University, Université de Versailles Saint-Quentin-en-Yvelines, and CNRS Paris, France
| | - P Coll
- Laboratoire Interuniversitaire des Systèmes Atmosphériques, Université Paris-Est Créteil, Paris VII-Denis Diderot University, and CNRS Créteil, France
| | - P G Conrad
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - D J Des Marais
- Exobiology Branch, NASA Ames Research Center Moffett Field, California, USA
| | - J P Dworkin
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - A G Fairén
- Department of Astronomy, Cornell University Ithaca, New York, USA ; Centro de Astrobiología, INTA-CSIC Madrid, Spain
| | - P François
- Department of Atmospheric, Oceanic and Space Sciences, University of Michigan Ann Arbor, Michigan, USA
| | - J P Grotzinger
- Division of Geological and Planetary Sciences, California Institute of Technology Pasadena, California, USA
| | - S Kashyap
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA ; Center for Research and Exploration in Space Science & Technology, University of Maryland, Baltimore County Baltimore, Maryland, USA
| | - I L Ten Kate
- Earth Sciences Department, Utrecht University Utrecht, Netherlands
| | - L A Leshin
- Department of Earth and Environmental Sciences and School of Science, Rensselaer Polytechnic Institute Troy, New York, USA
| | - C A Malespin
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA ; Goddard Earth Sciences and Technologies and Research, Universities Space Research Association Columbia, Maryland, USA
| | - M G Martin
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA ; Department of Chemistry, Catholic University of America Washington, District of Columbia, USA
| | - F J Martin-Torres
- Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR) Granada, Spain ; Division of Space Technology, Department of Computer Science, Electrical and Space Engineering, Luleå University of Technology Kiruna, Sweden
| | - A C McAdam
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - D W Ming
- Astromaterials Research and Exploration Science Directorate, NASA Johnson Space Center Houston, Texas, USA
| | - R Navarro-González
- Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Ciudad Universitaria México City, Mexico
| | - A A Pavlov
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - B D Prats
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - S W Squyres
- Department of Astronomy, Cornell University Ithaca, New York, USA
| | - A Steele
- Geophysical Laboratory, Carnegie Institution of Washington Washington, District of Columbia, USA
| | - J C Stern
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - D Y Sumner
- Department of Earth and Planetary Sciences, University of California Davis, California, USA
| | - B Sutter
- Jacobs, NASA Johnson Space Center Houston, Texas, USA
| | - M-P Zorzano
- Centro de Astrobiologia (INTA-CSIC) Madrid, Spain
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13
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Li X, Danell RM, Brinckerhoff WB, Pinnick VT, van Amerom F, Arevalo RD, Getty SA, Mahaffy PR, Steininger H, Goesmann F. Detection of trace organics in Mars analog samples containing perchlorate by laser desorption/ionization mass spectrometry. ASTROBIOLOGY 2015; 15:104-110. [PMID: 25622133 DOI: 10.1089/ast.2014.1203] [Citation(s) in RCA: 19] [Impact Index Per Article: 2.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/04/2023]
Abstract
Evidence from recent Mars missions indicates the presence of perchlorate salts up to 1 wt % level in the near-surface materials. Mixed perchlorates and other oxychlorine species may complicate the detection of organic molecules in bulk martian samples when using pyrolysis techniques. To address this analytical challenge, we report here results of laboratory measurements with laser desorption mass spectrometry, including analyses performed on both commercial and Mars Organic Molecule Analyzer (MOMA) breadboard instruments. We demonstrate that the detection of nonvolatile organics in selected spiked mineral-matrix materials by laser desorption/ionization (LDI) mass spectrometry is not inhibited by the presence of up to 1 wt % perchlorate salt. The organics in the sample are not significantly degraded or combusted in the LDI process, and the parent molecular ion is retained in the mass spectrum. The LDI technique provides distinct potential benefits for the detection of organics in situ on the martian surface and has the potential to aid in the search for signs of life on Mars.
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Affiliation(s)
- Xiang Li
- 1 Center for Space Science and Technology, University of Maryland , Baltimore County, Baltimore, Maryland, USA
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14
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Chloromethane release from carbonaceous meteorite affords new insight into Mars lander findings. Sci Rep 2014; 4:7010. [PMID: 25394222 PMCID: PMC4230006 DOI: 10.1038/srep07010] [Citation(s) in RCA: 12] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/18/2014] [Accepted: 10/13/2014] [Indexed: 11/08/2022] Open
Abstract
Controversy continues as to whether chloromethane (CH3Cl) detected during pyrolysis of Martian soils by the Viking and Curiosity Mars landers is indicative of organic matter indigenous to Mars. Here we demonstrate CH3Cl release (up to 8 μg/g) during low temperature (150–400°C) pyrolysis of the carbonaceous chondrite Murchison with chloride or perchlorate as chlorine source and confirm unequivocally by stable isotope analysis the extraterrestrial origin of the methyl group (δ2H +800 to +1100‰, δ13C −19.2 to +10‰,). In the terrestrial environment CH3Cl released during pyrolysis of organic matter derives from the methoxyl pool. The methoxyl pool in Murchison is consistent both in magnitude (0.044%) and isotope signature (δ2H +1054 ± 626‰, δ13C +43.2 ± 38.8‰,) with that of the CH3Cl released on pyrolysis. Thus CH3Cl emissions recorded by Mars lander experiments may be attributed to methoxyl groups in undegraded organic matter in meteoritic debris reaching the Martian surface being converted to CH3Cl with perchlorate or chloride in Martian soil. However we cannot discount emissions arising additionally from organic matter of indigenous origin. The stable isotope signatures of CH3Cl detected on Mars could potentially be utilized to determine its origin by distinguishing between terrestrial contamination, meteoritic infall and indigenous Martian sources.
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15
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Aerts JW, Röling WFM, Elsaesser A, Ehrenfreund P. Biota and biomolecules in extreme environments on Earth: implications for life detection on Mars. Life (Basel) 2014; 4:535-65. [PMID: 25370528 PMCID: PMC4284457 DOI: 10.3390/life4040535] [Citation(s) in RCA: 23] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/07/2014] [Revised: 09/08/2014] [Accepted: 09/16/2014] [Indexed: 11/24/2022] Open
Abstract
The three main requirements for life as we know it are the presence of organic compounds, liquid water, and free energy. Several groups of organic compounds (e.g., amino acids, nucleobases, lipids) occur in all life forms on Earth and are used as diagnostic molecules, i.e., biomarkers, for the characterization of extant or extinct life. Due to their indispensability for life on Earth, these biomarkers are also prime targets in the search for life on Mars. Biomarkers degrade over time; in situ environmental conditions influence the preservation of those molecules. Nonetheless, upon shielding (e.g., by mineral surfaces), particular biomarkers can persist for billions of years, making them of vital importance in answering questions about the origins and limits of life on early Earth and Mars. The search for organic material and biosignatures on Mars is particularly challenging due to the hostile environment and its effect on organic compounds near the surface. In support of life detection on Mars, it is crucial to investigate analogue environments on Earth that resemble best past and present Mars conditions. Terrestrial extreme environments offer a rich source of information allowing us to determine how extreme conditions affect life and molecules associated with it. Extremophilic organisms have adapted to the most stunning conditions on Earth in environments with often unique geological and chemical features. One challenge in detecting biomarkers is to optimize extraction, since organic molecules can be low in abundance and can strongly adsorb to mineral surfaces. Methods and analytical tools in the field of life science are continuously improving. Amplification methods are very useful for the detection of low concentrations of genomic material but most other organic molecules are not prone to amplification methods. Therefore, a great deal depends on the extraction efficiency. The questions “what to look for”, “where to look”, and “how to look for it” require more of our attention to ensure the success of future life detection missions on Mars.
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Affiliation(s)
- Joost W Aerts
- Molecular Cell Physiology, Faculty of Earth and Life Sciences, VU University Amsterdam, de Boelelaan 1085, 1081 HV Amsterdam, The Netherlands.
| | - Wilfred F M Röling
- Molecular Cell Physiology, Faculty of Earth and Life Sciences, VU University Amsterdam, de Boelelaan 1085, 1081 HV Amsterdam, The Netherlands.
| | - Andreas Elsaesser
- Leiden Observatory, Leiden University, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands.
| | - Pascale Ehrenfreund
- Leiden Observatory, Leiden University, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands.
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16
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Sephton MA, Carter JN. Statistics provide guidance for indigenous organic carbon detection on Mars missions. ASTROBIOLOGY 2014; 14:706-713. [PMID: 25061905 DOI: 10.1089/ast.2014.1161] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/03/2023]
Abstract
Data from the Viking and Mars Science Laboratory missions indicate the presence of organic compounds that are not definitively martian in origin. Both contamination and confounding mineralogies have been suggested as alternatives to indigenous organic carbon. Intuitive thought suggests that we are repeatedly obtaining data that confirms the same level of uncertainty. Bayesian statistics may suggest otherwise. If an organic detection method has a true positive to false positive ratio greater than one, then repeated organic matter detection progressively increases the probability of indigeneity. Bayesian statistics also reveal that methods with higher ratios of true positives to false positives give higher overall probabilities and that detection of organic matter in a sample with a higher prior probability of indigenous organic carbon produces greater confidence. Bayesian statistics, therefore, provide guidance for the planning and operation of organic carbon detection activities on Mars. Suggestions for future organic carbon detection missions and instruments are as follows: (i) On Earth, instruments should be tested with analog samples of known organic content to determine their true positive to false positive ratios. (ii) On the mission, for an instrument with a true positive to false positive ratio above one, it should be recognized that each positive detection of organic carbon will result in a progressive increase in the probability of indigenous organic carbon being present; repeated measurements, therefore, can overcome some of the deficiencies of a less-than-definitive test. (iii) For a fixed number of analyses, the highest true positive to false positive ratio method or instrument will provide the greatest probability that indigenous organic carbon is present. (iv) On Mars, analyses should concentrate on samples with highest prior probability of indigenous organic carbon; intuitive desires to contrast samples of high prior probability and low prior probability of indigenous organic carbon should be resisted.
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Affiliation(s)
- Mark A Sephton
- Impacts and Astromaterials Research Centre , Department of Earth Science and Engineering, Imperial College London, London, UK
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17
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Shelor CP, Dasgupta PK, Aubrey A, Davila AF, Lee MC, McKay CP, Liu Y, Noell AC. What can in situ ion chromatography offer for Mars exploration? ASTROBIOLOGY 2014; 14:577-588. [PMID: 24963874 DOI: 10.1089/ast.2013.1131] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/03/2023]
Abstract
The successes of the Mars exploration program have led to our unprecedented knowledge of the geological, mineralogical, and elemental composition of the martian surface. To date, however, only one mission, the Phoenix lander, has specifically set out to determine the soluble chemistry of the martian surface. The surprising results, including the detection of perchlorate, demonstrated both the importance of performing soluble ion measurements and the need for improved instrumentation to unambiguously identify all the species present. Ion chromatography (IC) is the state-of-the-art technique for soluble ion analysis on Earth and would therefore be the ideal instrument to send to Mars. A flight IC system must necessarily be small, lightweight, low-power, and have low eluent consumption. We demonstrate here a breadboard system that addresses these issues by using capillary IC at low flow rates with an optimized eluent generator and suppressor. A mix of 12 ions known or plausible for the martian soil, including 4 (oxy)chlorine species, has been separated at flow rates ranging from 1 to 10 μL/min, requiring as little as 200 psi at 1.0 μL/min. This allowed the use of pneumatic displacement pumping from a pressurized aluminum eluent reservoir and the elimination of the high-pressure pump entirely (the single heaviest and most energy-intensive component). All ions could be separated and detected effectively from 0.5 to 100 μM, even when millimolar concentrations of perchlorate were present in the same mixtures.
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Affiliation(s)
- C Phillip Shelor
- 1 Department of Chemistry and Biochemistry, The University of Texas at Arlington , Arlington, Texas
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18
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Atreya SK, Trainer MG, Franz HB, Wong MH, Manning HLK, Malespin CA, Mahaffy PR, Conrad PG, Brunner AE, Leshin LA, Jones JH, Webster CR, Owen TC, Pepin RO, Navarro-González R. Primordial argon isotope fractionation in the atmosphere of Mars measured by the SAM instrument on Curiosity and implications for atmospheric loss. GEOPHYSICAL RESEARCH LETTERS 2013; 40:5605-5609. [PMID: 25821261 PMCID: PMC4373143 DOI: 10.1002/2013gl057763] [Citation(s) in RCA: 8] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/04/2013] [Revised: 10/03/2013] [Accepted: 10/07/2013] [Indexed: 05/30/2023]
Abstract
[1] The quadrupole mass spectrometer of the Sample Analysis at Mars (SAM) instrument on Curiosity rover has made the first high-precision measurement of the nonradiogenic argon isotope ratio in the atmosphere of Mars. The resulting value of 36Ar/38Ar = 4.2 ± 0.1 is highly significant for it provides excellent evidence that "Mars" meteorites are indeed of Martian origin, and it points to a significant loss of argon of at least 50% and perhaps as high as 85-95% from the atmosphere of Mars in the past 4 billion years. Taken together with the isotopic fractionations in N, C, H, and O measured by SAM, these results imply a substantial loss of atmosphere from Mars in the posthydrodynamic escape phase.
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Affiliation(s)
- Sushil K Atreya
- Department of Atmospheric, Oceanic and Space Sciences, University of Michigan Ann Arbor, Michigan, USA
| | | | | | - Michael H Wong
- Department of Atmospheric, Oceanic and Space Sciences, University of Michigan Ann Arbor, Michigan, USA
| | | | | | | | | | | | - Laurie A Leshin
- School of Science, Rensselaer Polytechnic Institute Troy, New York, USA
| | | | - Christopher R Webster
- Jet Propulsion Laboratory, California Institute of Technology Pasadena, California, USA
| | - Tobias C Owen
- University of Hawai'i at Mānoa Honolulu, Hawaii, USA
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Leshin LA, Mahaffy PR, Webster CR, Cabane M, Coll P, Conrad PG, Archer PD, Atreya SK, Brunner AE, Buch A, Eigenbrode JL, Flesch GJ, Franz HB, Freissinet C, Glavin DP, McAdam AC, Miller KE, Ming DW, Morris RV, Navarro-Gonzalez R, Niles PB, Owen T, Pepin RO, Squyres S, Steele A, Stern JC, Summons RE, Sumner DY, Sutter B, Szopa C, Teinturier S, Trainer MG, Wray JJ, Grotzinger JP, Kemppinen O, Bridges N, Johnson JR, Minitti M, Cremers D, Bell JF, Edgar L, Farmer J, Godber A, Wadhwa M, Wellington D, McEwan I, Newman C, Richardson M, Charpentier A, Peret L, King P, Blank J, Weigle G, Schmidt M, Li S, Milliken R, Robertson K, Sun V, Baker M, Edwards C, Ehlmann B, Farley K, Griffes J, Miller H, Newcombe M, Pilorget C, Rice M, Siebach K, Stack K, Stolper E, Brunet C, Hipkin V, Leveille R, Marchand G, Sanchez PS, Favot L, Cody G, Fluckiger L, Lees D, Nefian A, Martin M, Gailhanou M, Westall F, Israel G, Agard C, Baroukh J, Donny C, Gaboriaud A, Guillemot P, Lafaille V, Lorigny E, Paillet A, Perez R, Saccoccio M, Yana C, Armiens-Aparicio C, Rodriguez JC, Blazquez IC, Gomez FG, Gomez-Elvira J, Hettrich S, Malvitte AL, Jimenez MM, Martinez-Frias J, Martin-Soler J, Martin-Torres FJ, Jurado AM, Mora-Sotomayor L, Caro GM, Lopez SN, Peinado-Gonzalez V, Pla-Garcia J, Manfredi JAR, Romeral-Planello JJ, Fuentes SAS, Martinez ES, Redondo JT, Urqui-O'Callaghan R, Mier MPZ, Chipera S, Lacour JL, Mauchien P, Sirven JB, Manning H, Fairen A, Hayes A, Joseph J, Sullivan R, Thomas P, Dupont A, Lundberg A, Melikechi N, Mezzacappa A, DeMarines J, Grinspoon D, Reitz G, Prats B, Atlaskin E, Genzer M, Harri AM, Haukka H, Kahanpaa H, Kauhanen J, Kemppinen O, Paton M, Polkko J, Schmidt W, Siili T, Fabre C, Wilhelm MB, Poitrasson F, Patel K, Gorevan S, Indyk S, Paulsen G, Gupta S, Bish D, Schieber J, Gondet B, Langevin Y, Geffroy C, Baratoux D, Berger G, Cros A, d'Uston C, Forni O, Gasnault O, Lasue J, Lee QM, Maurice S, Meslin PY, Pallier E, Parot Y, Pinet P, Schroder S, Toplis M, Lewin E, Brunner W, Heydari E, Achilles C, Oehler D, Coscia D, Israel G, Dromart G, Robert F, Sautter V, Le Mouelic S, Mangold N, Nachon M, Stalport F, Francois P, Raulin F, Cameron J, Clegg S, Cousin A, DeLapp D, Dingler R, Jackson RS, Johnstone S, Lanza N, Little C, Nelson T, Wiens RC, Williams RB, Jones A, Kirkland L, Treiman A, Baker B, Cantor B, Caplinger M, Davis S, Duston B, Edgett K, Fay D, Hardgrove C, Harker D, Herrera P, Jensen E, Kennedy MR, Krezoski G, Krysak D, Lipkaman L, Malin M, McCartney E, McNair S, Nixon B, Posiolova L, Ravine M, Salamon A, Saper L, Stoiber K, Supulver K, Van Beek J, Van Beek T, Zimdar R, French KL, Iagnemma K, Goesmann F, Goetz W, Hviid S, Johnson M, Lefavor M, Lyness E, Breves E, Dyar MD, Fassett C, Blake DF, Bristow T, DesMarais D, Edwards L, Haberle R, Hoehler T, Hollingsworth J, Kahre M, Keely L, McKay C, Wilhelm MB, Bleacher L, Brinckerhoff W, Choi D, Dworkin JP, Floyd M, Garvin J, Harpold D, Jones A, Martin DK, Pavlov A, Raaen E, Smith MD, Tan F, Meyer M, Posner A, Voytek M, Anderson RC, Aubrey A, Beegle LW, Behar A, Blaney D, Brinza D, Calef F, Christensen L, Crisp JA, DeFlores L, Ehlmann B, Feldman J, Feldman S, Hurowitz J, Jun I, Keymeulen D, Maki J, Mischna M, Morookian JM, Parker T, Pavri B, Schoppers M, Sengstacken A, Simmonds JJ, Spanovich N, Juarez MDLT, Vasavada AR, Yen A, Cucinotta F, Jones JH, Rampe E, Nolan T, Fisk M, Radziemski L, Barraclough B, Bender S, Berman D, Dobrea EN, Tokar R, Vaniman D, Williams RME, Yingst A, Lewis K, Cleghorn T, Huntress W, Manhes G, Hudgins J, Olson T, Stewart N, Sarrazin P, Grant J, Vicenzi E, Wilson SA, Bullock M, Ehresmann B, Hamilton V, Hassler D, Peterson J, Rafkin S, Zeitlin C, Fedosov F, Golovin D, Karpushkina N, Kozyrev A, Litvak M, Malakhov A, Mitrofanov I, Mokrousov M, Nikiforov S, Prokhorov V, Sanin A, Tretyakov V, Varenikov A, Vostrukhin A, Kuzmin R, Clark B, Wolff M, McLennan S, Botta O, Drake D, Bean K, Lemmon M, Schwenzer SP, Anderson RB, Herkenhoff K, Lee EM, Sucharski R, Hernandez MADP, Avalos JJB, Ramos M, Kim MH, Malespin C, Plante I, Muller JP, Ewing R, Boynton W, Downs R, Fitzgibbon M, Harshman K, Morrison S, Dietrich W, Kortmann O, Palucis M, Williams A, Lugmair G, Wilson MA, Rubin D, Jakosky B, Balic-Zunic T, Frydenvang J, Jensen JK, Kinch K, Koefoed A, Madsen MB, Stipp SLS, Boyd N, Campbell JL, Gellert R, Perrett G, Pradler I, VanBommel S, Jacob S, Rowland S, Atlaskin E, Savijarvi H, Boehm E, Bottcher S, Burmeister S, Guo J, Kohler J, Garcia CM, Mueller-Mellin R, Wimmer-Schweingruber R, Bridges JC, McConnochie T, Benna M, Bower H, Blau H, Boucher T, Carmosino M, Elliott H, Halleaux D, Renno N, Wong M, Elliott B, Spray J, Thompson L, Gordon S, Newsom H, Ollila A, Williams J, Vasconcelos P, Bentz J, Nealson K, Popa R, Kah LC, Moersch J, Tate C, Day M, Kocurek G, Hallet B, Sletten R, Francis R, McCullough E, Cloutis E, ten Kate IL, Kuzmin R, Arvidson R, Fraeman A, Scholes D, Slavney S, Stein T, Ward J, Berger J, Moores JE. Volatile, Isotope, and Organic Analysis of Martian Fines with the Mars Curiosity Rover. Science 2013; 341:1238937. [DOI: 10.1126/science.1238937] [Citation(s) in RCA: 327] [Impact Index Per Article: 29.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
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McKay CP, Stoker CR, Glass BJ, Davé AI, Davila AF, Heldmann JL, Marinova MM, Fairen AG, Quinn RC, Zacny KA, Paulsen G, Smith PH, Parro V, Andersen DT, Hecht MH, Lacelle D, Pollard WH. The Icebreaker Life Mission to Mars: a search for biomolecular evidence for life. ASTROBIOLOGY 2013; 13:334-53. [PMID: 23560417 DOI: 10.1089/ast.2012.0878] [Citation(s) in RCA: 56] [Impact Index Per Article: 5.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/22/2023]
Abstract
The search for evidence of life on Mars is the primary motivation for the exploration of that planet. The results from previous missions, and the Phoenix mission in particular, indicate that the ice-cemented ground in the north polar plains is likely to be the most recently habitable place that is currently known on Mars. The near-surface ice likely provided adequate water activity during periods of high obliquity, ≈ 5 Myr ago. Carbon dioxide and nitrogen are present in the atmosphere, and nitrates may be present in the soil. Perchlorate in the soil together with iron in basaltic rock provides a possible energy source for life. Furthermore, the presence of organics must once again be considered, as the results of the Viking GCMS are now suspect given the discovery of the thermally reactive perchlorate. Ground ice may provide a way to preserve organic molecules for extended periods of time, especially organic biomarkers. The Mars Icebreaker Life mission focuses on the following science goals: (1) Search for specific biomolecules that would be conclusive evidence of life. (2) Perform a general search for organic molecules in the ground ice. (3) Determine the processes of ground ice formation and the role of liquid water. (4) Understand the mechanical properties of the martian polar ice-cemented soil. (5) Assess the recent habitability of the environment with respect to required elements to support life, energy sources, and possible toxic elements. (6) Compare the elemental composition of the northern plains with midlatitude sites. The Icebreaker Life payload has been designed around the Phoenix spacecraft and is targeted to a site near the Phoenix landing site. However, the Icebreaker payload could be supported on other Mars landing systems. Preliminary studies of the SpaceX Dragon lander show that it could support the Icebreaker payload for a landing either at the Phoenix site or at midlatitudes. Duplicate samples could be cached as a target for possible return by a Mars Sample Return mission. If the samples were shown to contain organic biomarkers, interest in returning them to Earth would be high.
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Boynton WV, Taylor GJ, Evans LG, Reedy RC, Starr R, Janes DM, Kerry KE, Drake DM, Kim KJ, Williams RMS, Crombie MK, Dohm JM, Baker V, Metzger AE, Karunatillake S, Keller JM, Newsom HE, Arnold JR, Brückner J, Englert PAJ, Gasnault O, Sprague AL, Mitrofanov I, Squyres SW, Trombka JI, d'Uston L, Wänke H, Hamara DK. Concentration of H, Si, Cl, K, Fe, and Th in the low- and mid-latitude regions of Mars. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2007je002887] [Citation(s) in RCA: 234] [Impact Index Per Article: 13.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Karunatillake S, Keller JM, Squyres SW, Boynton WV, Brückner J, Janes DM, Gasnault O, Newsom HE. Chemical compositions at Mars landing sites subject to Mars Odyssey Gamma Ray Spectrometer constraints. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002859] [Citation(s) in RCA: 14] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
| | - John M. Keller
- Physics Department; California Polytechnic State University; San Luis Obispo California USA
| | | | - William V. Boynton
- Lunar and Planetary Laboratory; University of Arizona; Tucson Arizona USA
| | | | - Daniel M. Janes
- Lunar and Planetary Laboratory; University of Arizona; Tucson Arizona USA
| | - Olivier Gasnault
- Centre d'Etude Spatiale des Rayonnements/Centre National de la Recherche Scientifique/Université Paul Sabatier Toulouse; Toulouse France
| | - Horton E. Newsom
- Institute of Meteoritics and Department of Earth and Planetary Sciences; University of New Mexico; Albuquerque New Mexico USA
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