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1. Time-Sensitive Aspects of Mars Sample Return (MSR) Science

Author: Tosca, N. J., Agee, Carl, Cockell, C., Glavin, D P, Hutzler, Aurore, Marty, B., McCubbin, F. M., Regberg, Aaron, Velbel, Michael, Kminek, G., Meyer, M., Beaty, D.W., Carrier, B. L., Haltigin, T., Hays, Lindsay, Busemann, H., Cavalazzi, Barbara, Debaille, V, Grady, M., Hauber, Ernst, Pratt, Lisa, Smith, Alvin, Smith, C., Summons, R E, Swindle, T. D., Tait, Kimberly, Udry, Arya, Usui, Tomohiro, Wadhwa, M., Westall, F., Zorzano, M.-P., Tosca N. J., Beaty D. W., Carrier B. L., Agee C. B., Cockell C. S., Glavin D. P., Hutzler A., Marty B., McCubbin F. M., Regberg A. B., Velbel M. A., Kminek G., Meyer M. A., Haltigin T., Busemann H., Cavalazzi B., Debaille V., Grady M. M., Hauber E., Hays L. E., Pratt L. M., Smith A. L., Smith C. L., Summons R. E., Swindle T. D., Tait K. T., Udry A., Usui T., Wadhwa M., Westall F., Zorzano M. -P., University of Cambridge [UK] (CAM), The University of New Mexico [Albuquerque], University of Edinburgh, NASA Goddard Space Flight Center (GSFC), European Space Agency (ESA), Centre de Recherches Pétrographiques et Géochimiques (CRPG), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), NASA Johnson Space Center (JSC), NASA, Michigan State University [East Lansing], Michigan State University System, Smithsonian Institution, NASA Headquarters, California Institute of Technology (CALTECH), Canadian Space Agency (CSA), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Bologna, Université libre de Bruxelles (ULB), The Open University [Milton Keynes] (OU), German Aerospace Center (DLR), Indiana University [Bloomington], Indiana University System, The Natural History Museum [London] (NHM), University of Glasgow, Massachusetts Institute of Technology (MIT), University of Arizona, Royal Ontario Museum, University of Nevada [Las Vegas] (WGU Nevada), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Arizona State University [Tempe] (ASU), Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), University of Aberdeen, Tosca, Nicholas [0000-0003-4415-4231], and Apollo - University of Cambridge Repository
Subjects: Minerals, geology, Extraterrestrial Environment, laboratory experiments, Sulfates, [SDV]Life Sciences [q-bio], astrobiology, Mars, Space Flight, Mars Sample Return (MSR) Science, sample return, Agricultural and Biological Sciences (miscellaneous), Space and Planetary Science, Exobiology, Clay, Gases
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 <
Published: 2022
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2. Science and Curation Considerations for the Design of a Mars Sample Return (MSR) Sample Receiving Facility

Author: Carrier, B. L., Beaty, D., Hutzler, Aurore, Smith, Alvin, Kminek, G., Meyer, M., Haltigin, T., Hays, Lindsay, Agee, Carl, Busemann, H., Cavalazzi, B., Cockell, C., Debaille, V, Glavin, D P, Grady, M., Hauber, Ernst, Marty, B., McCubbin, F. M., Pratt, Lisa, Regberg, Aaron, Smith, C., Summons, R E, Swindle, T. D., Tait, Kimberly, Tosca, N. J., Udry, Arya, Usui, Tomohiro, Velbel, Michael, Wadhwa, M., Westall, F., Zorzano, M.-P., California Institute of Technology (CALTECH), European Space Agency (ESA), NASA Headquarters, Canadian Space Agency (CSA), The University of New Mexico [Albuquerque], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Bologna, University of Edinburgh, Université libre de Bruxelles (ULB), NASA Goddard Space Flight Center (GSFC), The Open University [Milton Keynes] (OU), German Aerospace Center (DLR), Centre de Recherches Pétrographiques et Géochimiques (CRPG), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), NASA Johnson Space Center (JSC), NASA, Indiana University [Bloomington], Indiana University System, The Natural History Museum [London] (NHM), University of Glasgow, Massachusetts Institute of Technology (MIT), University of Arizona, Royal Ontario Museum, University of Cambridge [UK] (CAM), University of Nevada [Las Vegas] (WGU Nevada), Japan Aerospace Exploration Agency [Tokyo] (JAXA), Michigan State University [East Lansing], Michigan State University System, Smithsonian Institution, Arizona State University [Tempe] (ASU), Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), University of Aberdeen, Agence Spatiale Européenne = European Space Agency (ESA), University of Bologna/Università di Bologna, Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Frapart, Isabelle, Carrier B. L., Beaty D. W., Hutzler A., Smith A. L., Kminek G., Meyer M. A., Haltigin T., Hays L. E., Agee C. B., Busemann H., Cavalazzi B., Cockell C. S., Debaille V., Glavin D. P., Grady M. M., and Hauber E., Marty B., McCubbin F. M., Pratt L. M., Regberg A. B., Smith C. L., Summons R. E., Swindle T. D., Tait K. T., Tosca N. J., Udry A., Usui T., Velbel M. A., Wadhwa M., Westall F., Zorzano M. -P.
Subjects: geology, Extraterrestrial Environment, laboratory experiments, Sample Safety Assessment Protocol (SSAP), Plant Extracts, astrobiology, Reproducibility of Results, Mars, intrumentation, Space Flight, sample return, Agricultural and Biological Sciences (miscellaneous), [SDU] Sciences of the Universe [physics], containment, contamination, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Sample Receiving Facility (SRF), Mars Sample Return (MSR) Campaign, Spacecraft
Abstract: The most important single element of the "ground system" portion of a Mars Sample Return (MSR) Campaign is a facility referred to as the Sample Receiving Facility (SRF), which would need to be designed and equipped to receive the returned spacecraft, extract and open the sealed sample container, extract the samples from the sample tubes, and implement a set of evaluations and analyses of the samples. One of the main findings of the first MSR Sample Planning Group (MSPG, 2019a) states that "The scientific community, for reasons of scientific quality, cost, and timeliness, strongly prefers that as many sample-related investigations as possible be performed in PI-led laboratories outside containment." There are many scientific and technical reasons for this preference, including the ability to utilize advanced and customized instrumentation that may be difficult to reproduce inside in a biocontained facility, and the ability to allow multiple science investigators in different labs to perform similar or complementary analyses to confirm the reproducibility and accuracy of results. It is also reasonable to assume that there will be a desire for the SRF to be as efficient and economical as possible, while still enabling the objectives of MSR to be achieved. For these reasons, MSPG concluded, and MSPG2 agrees, that the SRF should be designed to accommodate only those analytical activities that could not reasonably be done in outside laboratories because they are time- or sterilization-sensitive, are necessary for the Sample Safety Assessment Protocol (SSAP), or are necessary parts of the initial sample characterization process that would allow subsamples to be effectively allocated for investigation. All of this must be accommodated in an SRF, while preserving the scientific value of the samples through maintenance of strict environmental and contamination control standards. Executive Summary The most important single element of the "ground system" portion of a Mars Sample Return (MSR) Campaign is a facility referred to as the Sample Receiving Facility (SRF), which would need to be designed and equipped to enable receipt of the returned spacecraft, extraction and opening of the sealed sample container, extraction of the samples from the sample tubes, and a set of evaluations and analyses of the samples-all under strict protocols of biocontainment and contamination control. Some of the important constraints in the areas of cost and required performance have not yet been set by the necessary governmental sponsors, but it is reasonable to assume there will be a desire for the SRF to be as efficient and economical as is possible, while still enabling the objectives of MSR science to be achieved. Additionally, one of the main findings of MSR Sample Planning Group (MSPG, 2019a) states "The scientific community, for reasons of scientific quality, cost, and timeliness, strongly prefers that as many sample-related investigations as possible be performed in PI-led laboratories outside containment." There are many scientific and technical reasons for this preference, including the ability to utilize advanced and customized instrumentation that may be difficult to reproduce inside a biocontained facility. Another benefit is the ability to enable similar or complementary analyses by multiple science investigators in different laboratories, which would confirm the reproducibility and accuracy of results. For these reasons, the MSPG concluded-and the MSR Science Planning Group Phase 2 (MSPG2) agrees-that the SRF should be designed to accommodate only those analytical activities inside biocontainment that could
Published: 2021
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3. Preliminary Planning for Mars Sample Return (MSR) Curation Activities in a Sample Receiving Facility

Author: Tait, Kimberly, McCubbin, F. M., Smith, C., Agee, Carl, Busemann, H., Cavalazzi, B., Debaille, V, Hutzler, Aurore, Usui, Tomohiro, Kminek, G., Meyer, M., Beaty, D., Carrier, B. L., Haltigin, T., Hays, Lindsay, Cockell, C., Glavin, D. P., Grady, M., Hauber, Ernst, Marty, B., Pratt, Lisa, Regberg, Aaron, Smith, Alvin, Summons, R E, Swindle, T. D., Tosca, N. J., Udry, Arya, Velbel, Michael, Wadhwa, M., Westall, F., Zorzano, M.-P., Royal Ontario Museum, NASA Johnson Space Center (JSC), NASA, The Natural History Museum [London] (NHM), University of Glasgow, The University of New Mexico [Albuquerque], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Bologna, Université libre de Bruxelles (ULB), European Space Agency (ESA), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), NASA Headquarters, California Institute of Technology (CALTECH), Canadian Space Agency (CSA), University of Edinburgh, NASA Goddard Space Flight Center (GSFC), The Open University [Milton Keynes] (OU), German Aerospace Center (DLR), Centre de Recherches Pétrographiques et Géochimiques (CRPG), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Indiana University [Bloomington], Indiana University System, Massachusetts Institute of Technology (MIT), University of Arizona, University of Cambridge [UK] (CAM), University of Nevada [Las Vegas] (WGU Nevada), Michigan State University [East Lansing], Michigan State University System, Smithsonian Institution, Arizona State University [Tempe] (ASU), Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), University of Aberdeen, Tait K. T., McCubbin F. M., Smith C. L., Agee C. B., Busemann H., Cavalazzi B., Debaille V., Hutzler A., Usui T., Kminek G., Meyer M. A., Beaty D. W., Carrier B. L., Haltigin T., Hays L. E., Cockell C. S., Glavin D. P., Grady M. M., Hauber E., Marty B., Pratt L. M., Regberg A. B., Smith A. L., Summons R. E., Swindle T. D., and Tosca N. J.
Subjects: geology, laboratory experiments, Extraterrestrial Environment, Mars Sample Return Planning Group 2 (MSPG2), astrobiology, Mars, Dust, curation, sample return, Space Flight, exploration, Agricultural and Biological Sciences (miscellaneous), Space and Planetary Science, [SDU]Sciences of the Universe [physics], sample receiving facility, Exobiology, Gases
Abstract: The Mars Sample Return Planning Group 2 (MSPG2) was tasked with identifying the steps that encompass all the curation activities that would happen within the MSR Sample Receiving Facility (SRF) and any anticipated curation-related requirements. An area of specific interest is the necessary analytical instrumentation. The SRF would be a Biosafety Level-4 facility where the returned MSR flight hardware would be opened, the sample tubes accessed, and the martian sample material extracted from the tubes. Characterization of the essential attributes of each sample would be required to provide enough information to prepare a sample catalog used in guiding the preparation of sample-related proposals by the world's research community and informing decisions by the sample allocation committee. The sample catalog would be populated with data and information generated during all phases of activity, including data derived concurrent with Mars 2020 sample-collecting rover activity, sample transport to Earth, and initial sample characterization within the SRF. We conclude that initial sample characterization can best be planned as a set of three sequential phases, which we have called Pre-Basic Characterization (Pre-BC), Basic Characterization (BC), and Preliminary Examination (PE), each of which requires a certain amount of instrumentation. Data on specific samples and subsamples obtained during sample safety assessments and time-sensitive scientific investigations would also be added to the catalog. There are several areas where future work would be beneficial to prepare for the receipt of samples, which would include the design of a sample tube isolation chamber and a strategy for opening the sample tubes and removing dust from the tube exteriors. Executive Summary All material collected from Mars (gases, dust, rock, regolith) would need to be carefully handled, stored, and analyzed following Earth return to minimize the alteration or contamination that could occur on Earth and maximize the scientific information that can be attained from the samples now and into the future. A Sample Receiving Facility (SRF) is where the Earth Entry System (EES) would be opened and the sample tubes opened and processed after they land on Earth. Samples should be accessible for research in biocontainment for time-sensitive studies and eventually, when deemed safe for release after sterilization or biohazard assessment, should be transferred out of biocontainment for allocation to scientific investigators in outside laboratories. There are two main mechanisms for allocation of samples outside the SRF: 1) Wait until the implementation of the Sample Safety Assessment Protocol (Planetary Protection) results concludes that the samples are non-hazardous, 2) Render splits of the samples non-hazardous by means of sterilization. To make these samples accessible, a series of observations and analytical measurements need to be completed to produce a sample catalog for the scientific community. Specialist members of the Mars Sample Return Planning Group Phase 2 (MSPG2), referred to here as the Curation Focus Group, have identified four curation goals that encompass all of the activities within the SRF: 1.Documentation of the state of the sample tubes and their contents prior to opening, 2.Inventory and tracking of the mass of each sample, 3.Preliminary assessment of lithology and any macroscopic forms of heterogeneity (on all the samples, non-invasive, in pristine isolators), 4.Sufficient characterization of the essential attributes of each sample to prepare a sample catalog and respond to requests by the sample allocation committee (partial samples, invasive, outside of pristine isolators). The sample catalog will provide data for the scientific community to make informed requests for samples for scientific investigations and for the approval of allocations of appropriate samples to satisfy these requests. The sample catalog would be populated with data and information generated during all phases of activity, including data derived from the landed Mars 2020 mission, during sample collection and transport to Earth, and reception within the Sample Receiving Facility. Data on specific samples and subsamples would also be generated during curation activities carried out within the Sample Receiving Facility and during sample safety assessments, time-sensitive studies, and a series of initial sample characterization steps we refer to as Pre-Basic Characterization (Pre-BC), Basic Characterization (BC), and Preliminary Examination (PE) phases. A significant portion of the Curation Focus Group's efforts was to determine which instrumentation would be required to produce a sample catalog for the scientific community and how and when certain instrumentation should be used. The goal is to provide enough information for the PIs to request material for their studies but to avoid facilitating studies that target scientific research that is better left to peer-reviewed competitive processes. We reviewed the proposed scientific objectives of the International MSR Objectives and Samples Team (iMOST) (Beaty
Published: 2021
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4. Searching for Signs of Life on Other Planets: Mars a Case Study

Author: Vago J. L., Westall F., Cavalazzi B., Exo-Mars Science Working Team, Agence Spatiale Européenne (ESA), European Space Agency (ESA), Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), University of Bologna, Barbara Cavalazzi, Frances Westall, B. Cavalazzi, F. Westall, and Vago J.L., Westall F., Cavalazzi B., Exo-Mars Science Working Team
Subjects: COSMIC cancer database, 010504 meteorology & atmospheric sciences, Mars Exploration Program, 01 natural sciences, Exoplanet, Astrobiology, Orbit, Mar, 13. Climate action, Planet, [SDU]Sciences of the Universe [physics], Extraterrestrial life, 0103 physical sciences, Missions, ESA, [CHIM]Chemical Sciences, Biosignature, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: International audience; Demonstrating the existence of simple life forms (past or present) on a cosmic body other than Earth is exceedingly challenging: (1) A naturally sceptic scientific community expects the evidence to be convincing—for example, several independent lines of analyses performed on a feature where the results can only be explained by a biological process. (2) Most bodies are difficult to explore in situ, just about the only way to achieve the above goal, and even then, typically, several missions are required to understand where to go and what to study. (3) Planets and moons that can only be observed remotely (e.g. exoplanets) or from orbit can at best provide some indirect hints of life potential. The actual verification of life would require studying samples containing biosignatures. With the exception of some active moons where jets and plumes may provide the means for satellites to analyse surface sourced material, most other cases require landing, exploring, collecting samples, and analysing them in situ—or bringing them back to Earth.In this chapter we look at Mars as an example case and propose a scoring system for assigning a confidence value to a group of observations aiming to establish whether a location hosted (or still harbors) microbial life.Life-seeking missions to other planets should target as many biosignatures as possible. Their discoveries cannot be conclusive unless they include powerful analytical chemistry instruments able to study biosignatures of biomolecules and their degradation products.
Published: 2019
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5. Earth as a Tool for Astrobiology:A European Perspective

Author: Martins, Z., Cottin, H., Kotler, J.M., Carrasco, N., Cockell, C.S., delaTorreNoetzel, R., Demets, R., de Vera, J.-P., d’Hendecourt, L., Ehrenfreund, P., Elsaesser, A., Foing, B., Onofri, S., Quinn, R., Rabbow, E., Rettberg, P., Ricco, A.J., Slenzka, K., Stalport, F., tenKate, I.L., van Loon, J.J.W.A., Westall, F., Petrology, Department of Earth Science and Technology [Imperial College London], Imperial College London, Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS), Chemical Analysis Facility (CAF), University of Reading (UOR), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), SUPA School of Physics and Astronomy [Edinburgh], University of Edinburgh, INTA Departamento de Observación de la Tierra, Instituto Nacional de Técnica Aeroespacial (INTA), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Space Policy Institute [Washington], The George Washington University (GW), Experimental Molecular Biophysics [Berlin], Fachbereich Physik [Berlin], Freie Universität Berlin-Freie Universität Berlin, Università degli studi della Tuscia [Viterbo], NASA Ames Research Center (ARC), DLR Institut für Luft- und Raumfahrtmedizin, Deutsches Zentrum für Luft- und Raumfahrt [Köln] (DLR), OHB Systems AG, Department of Earth Sciences [Utrecht], Utrecht University [Utrecht], VU University Medical Center [Amsterdam], Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), ESA, CNES, ANR, CNRS (CNRS-MI-2014), European Project: 636829,H2020,ERC-2014-STG,PRIMCHEM(2015), European Project: 607297,EC:FP7:SPA,FP7-SPACE-2013-1,MASE(2014), Fachbereich Physik [Freie Univeristät Berlin] | Department of Physics [Freie Univeristät Berlin], Orbitale Hochtechnologie Bremen (OHB Systems AG), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Universiteit Leiden, Agence Spatiale Européenne = European Space Agency (ESA), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Cardon, Catherine, Primitive chemistry in planetary atmospheres: From the upper atmosphere down to the surface - PRIMCHEM - - H20202015-09-01 - 2020-09-01 - 636829 - VALID, Mars Analogues for Space Exploration - MASE - - EC:FP7:SPA2014-01-01 - 2018-01-01 - 607297 - VALID, Oral and Maxillofacial Surgery / Oral Pathology, Amsterdam Movement Sciences - Restoration and Development, The Royal Society, Petrology, MKA VUmc (ORM, ACTA), and Maxillofacial Surgery (VUmc)
Subjects: Engineering, Solar System, planetary field analogues, 010504 meteorology & atmospheric sciences, Exoplanetology, astrobiology, Field test campaigns, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astronomy & Astrophysics, 01 natural sciences, Astrobiology, Planet, 0103 physical sciences, Exobiology, Astrobiology Science and Technology for Exploring Planets, field test campaigns, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Astrochemistry, exobiology, business.industry, astrochemistry, Astronomy and Astrophysics, Laboratory analogues, Field (geography), EXPOSE, Outreach, laboratory analogues, 0201 Astronomical And Space Sciences, Planetary science, 13. Climate action, Space and Planetary Science, Planetary field analogues, business
Abstract: International audience; Scientists use the Earth as a tool for astrobiology by analyzing planetary field analogues (i.e. terrestrial samples and field sites that resemble planetary bodies in our Solar System). In addition, they expose the selected planetary field analogues in simulation chambers to conditions that mimic the ones of planets, moons and Low Earth Orbit (LEO) space conditions, as well as the chemistry occurring in interstellar and cometary ices. This paper reviews the ways the Earth is used by astrobiologists: (i) by conducting planetary field analogue studies to investigate extant life from extreme environments, its metabolisms, adaptation strategies and modern biosignatures; (ii) by conducting planetary field analogue studies to investigate extinct life from the oldest rocks on our planet and its biosignatures; (iii) by exposing terrestrial samples to simulated space or planetary environments and producing a sample analogue to investigate changes in minerals, biosignatures and microorganisms. The European Space Agency (ESA) created a topical team in 2011 to investigate recent activities using the Earth as a tool for astrobiology and to formulate recommendations and scientific needs to improve ground-based astrobiological research. Space is an important tool for astrobiology (see Horneck et al. in Astrobiology, 16:201–243, 2016; Cottin et al., 2017), but access to space is limited. Complementing research on Earth provides fast access, more replications and higher sample throughput. The major conclusions of the topical team and suggestions for the future include more scientifically qualified calls for field campaigns with planetary analogy, and a centralized point of contact at ESA or the EU for the organization of a survey of such expeditions. An improvement of the coordinated logistics, infrastructures and funding system supporting the combination of field work with planetary simulation investigations, as well as an optimization of the scientific return and data processing, data storage and data distribution is also needed. Finally, a coordinated EU or ESA education and outreach program would improve the participation of the public in the astrobiological activities.
Published: 2017
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6. MICROORGANISMS FROM MARS ANALOGUE ENVIRONMENTS IN EARTH - COULD THEY SURVIVE ON MARS?

Author: Rettberg, Petra, Cockell, C.S., Beblo-Vranesevic, K., Bohmeier, M., Rabbow, E., Schwendner, P., Westall, F., Gaboyer, F., Walter, N., Moissl-Eichinger, C., Perras, A., Gomez, F., Amils, R., Garcia, L., Ehrenfreund, P., Monaghan, E., Marteinsson, V., Vannier, P., and Rettberg, P.
Subjects: Strahlenbiologie, Mars, MASE, Astrobiology
Abstract: Assessing the habitability of Mars and detecting life, if it was ever there, depends on knowledge of whether the combined environmental stresses experienced on Mars are compatible with life and whether a record of that life could ever be detected. Many combinations of Mars relevant stress factors, such as high radiation dose rates and high UV uences combined with high salt concentrations, and low water activity, have not been investigated. In particular, the response of anaerobic organisms to Mars-like stress factors and combinations thereof are not known. In the EC project MASE (Mars Analogues for Space Exploration) we address these limitations by characterising different Mars analogue environments on Earth, isolating microorganisms from these sites and exposing them to Mars relevant stress factors alone and in combination. We want to find out, if these bacteria respond in an additive or synergistic way and if they would be able to survive on Mars. So far, eight only distantly related microorganisms are under detailed investigation, e.g Yersinia sp., Halanaerobium sp., Acidiphilum sp. Desulfovibrio sp.. Unexpectedly, a Yersinia strain turned out to be quite resistant, especially against desicca- tion and oxidising compounds, whereas a Desulfovibrio sp. strain exhibit a relatively high radiation resistance. The future experiments aim at the identification of the underlying cellu- lar and molecular mechanisms and the comparison to other new isolates from Mars analogue environments on Earth in the MASE project.
Published: 2016

7. Assessing the habitability of the MASE Mars analogue sites

Author: Monaghan, E., Ehrenfreund, P., Cockell, C.S., Schwendner, P., Rettberg, Petra, Beblo-Vranesevic, Kristina, Bohmeier, M., Rabbow, E., Westall, F., Gaboyer, F., Walter, N., Moissl-Eichinger, C., Perras, A., Gomez, F., Amils, R., Garcia Descalzo, L., Marteinsson, V., and Vannier, P.
Subjects: Strahlenbiologie, Mars, Mars Analogues, Astrobiology
Abstract: The MASE (Mars Analogues for Space Exploration) [1] project is a four-year collaborative research project supported by the European Commission Seventh Framework Contract. The aim of the project is to understand how combined environmental stresses influence the habitability of a number of Mars analogue environments in Europe and beyond. Field sites sampled for MASE include deep subsurface salts at Boulby Mine in the UK, sulfidic springs In Germany and an acidic cold lake in lceland. Samples and isolates have also been provided to the project from acidic deep subsurface environments at the Rio Tinto in Spain as well as permafrost sites in Russian Siberia and northern Canada. Crucial to assessing the habitability of any environmental system to be used as an astrobiological analogue • whether for life in general or, as in this case, for anaerobic microorganisms • is a detailed understanding of their geological and physiochemical context [2, 3]. One of the key outcomes of the MASE project is a comparison and synthesis of just such a set of context data from a varied set of analogue sites, the core of which is presented here, and complemented by an analysis of field samples to detect and quantify amino acids, other organics as well as biologically relevant molecules. We show that anaerobic environments provide some of the best fidelity environments for examining the potential habitability of environments on Mars, which are also anaerobic, but that even these analogue environments show the signatures of Earth's very different geological history, such as high carbon abundance in some environments (from 0.1% in lcelandic lake sediments to 22. 7% in deep .permafrost environments).
Published: 2016

8. Mars Analogues for space exploration - from anaerobic field site to culture collection

Author: Cockell, Charles S. and the MASE team, Schwendner, P., Rettberg, Petra, Beblo-Vranesevic, Kristina, Bohmeier, M., Rabbow, E., Westall, F., Gaboyer, F., Walter, N., Cabezas, P., Moissl-Eichinger, C., Perras, A., Gomez, F., Amils, R., Garcia-Descalzo, L., Ehrenfreund, P., Monaghan, E., Riede, A., Marteinsson, V., and Vannier, P.
Subjects: Strahlenbiologie, Mars analogues, Mars, Astrobiology, culture collection
Abstract: Astrobiology seeks to understand the limits of life and to determine the physiology of organisms in order to be able to better assess the potential habitability of other worlds and improve our ability to assay them for the presence of life. To successfully achieve this we require representative microorganisms from environments on Earth that in physical and/or chemical conditions approximate to extraterrestrial environments. The most challenging of these environments with respect to the sample collection and follow on isolation and cultivation of microorganisms are anaerobic environments. Here we describe a systematic approach to this challenge and aim to provide a guideline for future fieldwork and sampling campaigns. We selected a number of anaerobic environments based on characteristics that make them analogous to past and present locations on Mars (Icelandic lakes, sulfidic springs, deep hypersaline environments, acidic iron-rich environments, and permafrost). We implemented a culturing approach to enrich organisms from these environments under anaerobic conditions using a defined medium that would allow for all organisms to be grown under identical culturing conditions m future physiological comparisons. We then isolated anaerobic microorganisms, carried out a study of their basic physiology and deposited these organisms in the DSMZ (Deutsche Sammlung von Mikroorganismen und Zellkulturen GmbH) culture collection to make them available to astrobiologists and microbiologists. This project represents the first attempt to implement a coordinated effort from the selection of extraterrestrial analog sites through to the isolation and the characterisation of organisms and their deposition within a culture collection.
Published: 2016

9. Biosignatures for Mars

Author: Westall, F., BARBARA CAVALAZZI, Foucher, F., Bost, N., Westall F, Cavalazzi B, Foucher F, and Bost N
Subjects: ASTROBIOLOGY, Biosignaure
Published: 2012

10. Fe-framboids from Devonian methane-related carbonate mounds: potential fossil analogues of MOA-SRB consortia and relationships with Martian astrobiology

Author: CAVALAZZI, BARBARA, BARBIERI, ROBERTO, GAMBERINI, FABIO, Westall F., Cady SL, Ori GG, Gennaro S, Lui A, Canteri R, Foucher F, Pepponi G, Kalender W, Karolczak M., Nunzia Stivaletta, Cavalazzi B, Barbieri R., Westall F., Cady SL, Ori GG, Gennaro S, Lui A, Canteri R, Foucher F, Gamberini F, Pepponi G, Kalender W, and Karolczak M
Subjects: Fe-framboid, Biosignature, Astrobiology
Published: 2009

11. Abundance and isotopic composition of gases in the martian atmosphere from the Curiosity rover

Author: Mahaffy, P. R., Webster, C. R., Atreya, S. K., Franz, H., Wong, M., Conrad, P. G., Harpold, D., Jones, J. J., Leshin, L. A., Manning, H., Owen, T., Pepin, R. O., Squyres, S., Trainer, M., Kemppinen, O., Bridges, N., Johnson, J. R., Minitti, M., Cremers, D., Bell, J. F., 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., Grotzinger, J., Miller, H., Newcombe, M., Pilorget, C., Rice, M., Siebach, K., Stack, K., Stolper, E., Brunet, C., Hipkin, V., Leveille, R., Marchand, G., Sanchez, P. S., Favot, L., Cody, G., Steele, A., 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, J. C., Blazquez, I. C., Gomez, F. G., Gomez-Elvira, J., Hettrich, S., Malvitte, A. L., Jimenez, M. M., Martinez-Frias, J., Martin-Soler, J., Martin-Torres, F. J., Jurado, A. M., Mora-Sotomayor, L., Caro, G. M., Lopez, S. N., Peinado-Gonzalez, V., Pla-Garcia, J., Manfredi, J. A. R., Romeral-Planello, J. J., Fuentes, S. A. S., Martinez, E. S., Redondo, J. T., Urqui-O'Callaghan, R., Mier, M.-P. Z., Chipera, S., Lacour, J.-L., Mauchien, P., Sirven, J.-B., 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, A.-M., Haukka, H., Kahanpaa, H., Kauhanen, J., Paton, M., Polkko, J., Schmidt, W., Siili, T., Fabre, C., Wray, J., Wilhelm, M. B., 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, Q.-M., Maurice, S., Meslin, P.-Y., Pallier, E., Parot, Y., Pinet, P., Schroder, S., Toplis, M., Lewin, E., Brunner, W., Heydari, E., Achilles, C., Oehler, D., Sutter, B., Cabane, M., Coscia, D., Szopa, C., Dromart, G., Robert, F., Sautter, V., Le Mouelic, S., Mangold, N., Nachon, M., Buch, A., Stalport, F., Coll, P., Francois, P., Raulin, F., Teinturier, S., Cameron, J., Clegg, S., Cousin, A., DeLapp, D., Dingler, R., Jackson, R. S., Johnstone, S., Lanza, N., Little, C., Nelson, T., Wiens, R. C., Williams, R. B., 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, M. R., 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, K. L., Iagnemma, K., Miller, K., Summons, R., Goesmann, F., Goetz, W., Hviid, S., Johnson, M., Lefavor, M., Lyness, E., Breves, E., Dyar, M. D., Fassett, C., Blake, D. F., Bristow, T., DesMarais, D., Edwards, L., Haberle, R., Hoehler, T., Hollingsworth, J., Kahre, M., Keely, L., McKay, C., Bleacher, L., Brinckerhoff, W., Choi, D., Dworkin, J. P., Eigenbrode, J., Floyd, M., Freissinet, C., Garvin, J., Glavin, D., Martin, D. K., McAdam, A., Pavlov, A., Raaen, E., Smith, M. D., Stern, J., Tan, F., Meyer, M., Posner, A., Voytek, M., Anderson, R. C., Aubrey, A., Beegle, L. W., Behar, A., Blaney, D., Brinza, D., Calef, F., Christensen, L., Crisp, J. A., DeFlores, L., Feldman, J., Feldman, S., Flesch, G., Hurowitz, J., Jun, I., Keymeulen, D., Maki, J., Mischna, M., Morookian, J. M., Parker, T., Pavri, B., Schoppers, M., Sengstacken, A., Simmonds, J. J., Spanovich, N., Juarez, M. d. l. T., Vasavada, A. R., Yen, A., Archer, P. D., Cucinotta, F., Ming, D., Morris, R. V., Niles, P., Rampe, E., Nolan, T., Fisk, M., Radziemski, L., Barraclough, B., Bender, S., Berman, D., Dobrea, E. N., Tokar, R., Vaniman, D., Williams, R. M. E., Yingst, A., Lewis, K., Cleghorn, T., Huntress, W., Manhes, G., Hudgins, J., Olson, T., Stewart, N., Sarrazin, P., Grant, J., Vicenzi, E., Wilson, S. A., 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, S. P., Anderson, R. B., Herkenhoff, K., Lee, E. M., Sucharski, R., Hernandez, M. A. d. P., Avalos, J. J. B., Ramos, M., Kim, M.-H., Malespin, C., Plante, I., Muller, J.-P., Navarro-Gonzalez, R., Ewing, R., Boynton, W., Downs, R., Fitzgibbon, M., Harshman, K., Morrison, S., Dietrich, W., Kortmann, O., Palucis, M., Sumner, D. Y., Williams, A., Lugmair, G., Wilson, M. A., Rubin, D., Jakosky, B., Balic-Zunic, T., Frydenvang, J., Jensen, J. K., Kinch, K., Koefoed, A., Madsen, M. B., Stipp, S. L. S., Boyd, N., Campbell, J. L., Gellert, R., Perrett, G., Pradler, I., VanBommel, S., Jacob, S., Rowland, S., Savijarvi, H., Boehm, E., Bottcher, S., Burmeister, S., Guo, J., Kohler, J., Garcia, C. M., Mueller-Mellin, R., Wimmer-Schweingruber, R., Bridges, J. C., McConnochie, T., Benna, M., Bower, H., Brunner, A., Blau, H., Boucher, T., Carmosino, M., Elliott, H., Halleaux, D., Renno, N., Elliott, B., Spray, J., Thompson, L., Gordon, S., Newsom, H., Ollila, A., Williams, J., Vasconcelos, P., Bentz, J., Nealson, K., Popa, R., Kah, L. C., Moersch, J., Tate, C., Day, M., Kocurek, G., Hallet, B., Sletten, R., Francis, R., McCullough, E., Cloutis, E., ten Kate, I. L., Arvidson, R., Fraeman, A., Scholes, D., Slavney, S., Stein, T., Ward, J., Berger, J., Moores, J. E., GeoRessources, Institut national des sciences de l'Univers (INSU - CNRS)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), MSL Science Team, NWO-NSO: The role of perchlorates in the preservation of organic compounds on Mars, and Petrology
Subjects: 010504 meteorology & atmospheric sciences, Curiosity rover, chemistry.chemical_element, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Mars, MSL Mars Atmosphere Isotopis Composition, martian atmosphere, 01 natural sciences, Astrobiology, Isotopic signature, chemistry.chemical_compound, 0103 physical sciences, MSL, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Martian, Multidisciplinary, δ13C, Atmosphere of Mars, Nitrogen, chemistry, 13. Climate action, Sample Analysis at Mars, Carbon dioxide, Environmental science, Carbon monoxide
Abstract: Mars' Atmosphere from Curiosity The Sample Analysis at Mars (SAM) instrument on the Curiosity rover that landed on Mars in August last year is designed to study the chemical and isotopic composition of the martian atmosphere. Mahaffy et al. (p. 263 ) present volume-mixing ratios of Mars' five major atmospheric constituents (CO 2 , Ar, N 2 , O 2 , and CO) and isotope measurements of 40 Ar/ 36 Ar and C and O in CO 2 , based on data from one of SAM's instruments, obtained between 31 August and 21 November 2012. Webster et al. (p. 260 ) used data from another of SAM's instruments obtained around the same period to determine isotope ratios of H, C, and O in atmospheric CO 2 and H 2 O. Agreement between the isotopic ratios measured by SAM with those of martian meteorites, measured in laboratories on Earth, confirms the origin of these meteorites and implies that the current atmospheric reservoirs of CO 2 and H 2 O were largely established after the period of early atmospheric loss some 4 billion years ago.
Published: 2013
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12. Curiosity at Gale Crater, Mars: Characterization and analysis of the rocknest sand shadow

Author: Blake, D. F., Morris, R. V., Kocurek, G., Morrison, S. M., Downs, R. T., Bish, D., Ming, D. W., Edgett, K. S., Rubin, D., Goetz, W., Madsen, M. B., Sullivan, R., Gellert, R., Campbell, I., Treiman, A. H., McLennan, S. M., Yen, A. S., Grotzinger, J., Vaniman, D. T., Chipera, S. J., Achilles, C. N., Rampe, E. B., Sumner, D., Meslin, P.- Y., Maurice, S., Forni, O., Gasnault, O., Fisk, M., Schmidt, M., Mahaffy, P., Leshin, L. A., Glavin, D., Steele, A., Freissinet, C., Navarro-Gonzalez, R., Yingst, R. A., Kah, L. C., Bridges, N., Lewis, K. W., Bristow, T. F., Farmer, J. D., Crisp, J. A., Stolper, E. M., Des Marais, D. J., Sarrazin, P., Agard, C., Alves Verdasca, J. A., Anderson, R., Archer, D., Armiens-Aparicio, C., Arvidson, R., Atlaskin, E., Atreya, S., Aubrey, A., Baker, B., Baker, M., Balic-Zunic, T., Baratoux, D., Baroukh, J., Barraclough, B., Bean, K., Beegle, L., Behar, A., Bell, J., Bender, S., Benna, M., Bentz, J., Berger, G., Berger, J., Berman, D., Blanco Avalos, J. J., Blaney, D., Blank, J., Blau, H., Bleacher, L., Boehm, E., Botta, O., Bottcher, S., Boucher, T., Bower, H., Boyd, N., Boynton, B., Breves, E., Bridges, J., Brinckerhoff, W., Brinza, D., Brunet, C., Brunner, A., Brunner, W., Buch, A., Bullock, M., Burmeister, S., Cabane, M., Calef, F., Cameron, J., Cantor, B., Caplinger, M., Rodriguez, J. C., Carmosino, M., Blazquez, I. C., Charpentier, A., Choi, D., Clark, B., Clegg, S., Cleghorn, T., Cloutis, E., Cody, G., Coll, P., Conrad, P., Coscia, D., Cousin, A., Cremers, D., Cros, A., Cucinotta, F., d'Uston, C., Davis, S., Day, M., Juarez, M. d. l. T., DeFlores, L., DeLapp, D., DeMarines, J., Dietrich, W., Dingler, R., Donny, C., Drake, D., Dromart, G., Dupont, A., Duston, B., Dworkin, J., Dyar, M. D., Edgar, L., Edwards, C., Edwards, L., Ehlmann, B., Ehresmann, B., Eigenbrode, J., Elliott, B., Elliott, H., Ewing, R., Fabre, C., Fairen, A., Farley, K., Fassett, C., Favot, L., Fay, D., Fedosov, F., Feldman, J., Feldman, S., Fitzgibbon, M., Flesch, G., Floyd, M., Fluckiger, L., Fraeman, A., Francis, R., Francois, P., Franz, H., French, K. L., Frydenvang, J., Gaboriaud, A., Gailhanou, M., Garvin, J., Geffroy, C., Genzer, M., Godber, A., Goesmann, F., Golovin, D., Gomez, F. G., Gomez-Elvira, J., Gondet, B., Gordon, S., Gorevan, S., Grant, J., Griffes, J., Grinspoon, D., Guillemot, P., Guo, J., Gupta, S., Guzewich, S., Haberle, R., Halleaux, D., Hallet, B., Hamilton, V., Hardgrove, C., Harker, D., Harpold, D., Harri, A.-M., Harshman, K., Hassler, D., Haukka, H., Hayes, A., Herkenhoff, K., Herrera, P., Hettrich, S., Heydari, E., Hipkin, V., Hoehler, T., Hollingsworth, J., Hudgins, J., Huntress, W., Hurowitz, J., Hviid, S., Iagnemma, K., Indyk, S., Israel, G., Jackson, R., Jacob, S., Jakosky, B., Jensen, E., Jensen, J. K., Johnson, J., Johnson, M., Johnstone, S., Jones, A., Jones, J., Joseph, J., Jun, I., Kahanpaa, H., Kahre, M., Karpushkina, N., Kasprzak, W., Kauhanen, J., Keely, L., Kemppinen, O., Keymeulen, D., Kim, M.-H., Kinch, K., King, P., Kirkland, L., Koefoed, A., Kohler, J., Kortmann, O., Kozyrev, A., Krezoski, J., Krysak, D., Kuzmin, R., Lacour, J. L., Lafaille, V., Langevin, Y., Lanza, N., Lasue, J., Le Mouelic, S., Lee, E. M., Lee, Q.-M., Lees, D., Lefavor, M., Lemmon, M., Lepinette Malvitte, A., Leveille, R., Lewin-Carpintier, E., Li, S., Lipkaman, L., Little, C., Litvak, M., Lorigny, E., Lugmair, G., Lundberg, A., Lyness, E., Maki, J., Malakhov, A., Malespin, C., Malin, M., Mangold, N., Manning, H., Marchand, G., Marin Jimenez, M., Martin Garcia, C., Martin, D., Martin, M., Martinez-Frias, J., Martin-Soler, J., Martin-Torres, F. J., Mauchien, P., McAdam, A., McCartney, E., McConnochie, T., McCullough, E., McEwan, I., McKay, C., McNair, S., Melikechi, N., Meyer, M., Mezzacappa, A., Miller, H., Miller, K., Milliken, R., Minitti, M., Mischna, M., Mitrofanov, I., Moersch, J., Mokrousov, M., Molina Jurado, A., Moores, J., Mora-Sotomayor, L., Morookian, J. M., Mueller-Mellin, R., Muller, J.-P., Munoz Caro, G., Nachon, M., Navarro Lopez, S., Nealson, K., Nefian, A., Nelson, T., Newcombe, M., Newman, C., Newsom, H., Nikiforov, S., Niles, P., Nixon, B., Dobrea, E. N., Nolan, T., Oehler, D., Ollila, A., Olson, T., Owen, T., Pablo, H., Paillet, A., Pallier, E., Palucis, M., Parker, T., Parot, Y., Patel, K., Paton, M., Paulsen, G., Pavlov, A., Pavri, B., Peinado-Gonzalez, V., Pepin, R., Peret, L., Perez, R., Perrett, G., Peterson, J., Pilorget, C., Pinet, P., Pla-Garcia, J., Plante, I., Poitrasson, F., Polkko, J., Popa, R., Posiolova, L., Pradler, I., Prats, B., Prokhorov, V., Purdy, S. W., Raaen, E., Radziemski, L., Rafkin, S., Ramos, M., Raulin, F., Ravine, M., Reitz, G., Renno, N., Rice, M., Richardson, M., Robert, F., Rodriguez Manfredi, J. A., Romeral-Planello, J. J., Rowland, S., Saccoccio, M., Salamon, A., Sandoval, J., Sanin, A., Sans Fuentes, S. A., Saper, L., Sautter, V., Savijarvi, H., Schieber, J., Schmidt, W., Scholes, D., Schoppers, M., Schroder, S., Sebastian Martinez, E., Sengstacken, A., Shterts, R., Siebach, K., Siili, T., Simmonds, J., Sirven, J.-B., Slavney, S., Sletten, R., Smith, M., Sobron Sanchez, P., Spanovich, N., Spray, J., Squyres, S., Stack, K., Stalport, F., Stein, T., Stern, J., Stewart, N., Stipp, S. L. S., Stoiber, K., Sucharski, B., Summons, R., Sun, V., Supulver, K., Sutter, B., Szopa, C., Tate, C., Teinturier, S., ten Kate, I. L., Thomas, P., Thompson, L., Tokar, R., Toplis, M., Torres Redondo, J., Trainer, M., Tretyakov, V., Urqui-O'Callaghan, R., Van Beek, J., Van Beek, T., VanBommel, S., Varenikov, A., Vasavada, A., Vasconcelos, P., Vicenzi, E., Vostrukhin, A., Voytek, M., Wadhwa, M., Ward, J., Webster, C., Weigle, E., Wellington, D., Westall, F., Wiens, R. C., Wilhelm, M. B., Williams, A., Williams, J., Williams, R., Williams, R. B., Wilson, M., Wimmer-Schweingruber, R., Wolff, M., Wong, M., Wray, J., Wu, M., Yana, C., Zeitlin, C., Zimdar, R., Zorzano Mier, M.-P., GeoRessources, Institut national des sciences de l'Univers (INSU - CNRS)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), NASA Ames Research Center (ARC), NASA Johnson Space Center (JSC), NASA, Department of Geological Sciences [Austin], Jackson School of Geosciences (JSG), University of Texas at Austin [Austin]-University of Texas at Austin [Austin], Department of Geology [Tucson], University of Arizona, Department of Geological Sciences [Bloomington], Indiana University [Bloomington], Indiana University System-Indiana University System, Malin Space Science Systems (MSSS), NASA Goddard Space Flight Center (GSFC), NWO-NSO: The role of perchlorates in the preservation of organic compounds on Mars, and Petrology
Subjects: Basalt, Meridiani Planum, Multidisciplinary, 010504 meteorology & atmospheric sciences, Curiosity rover, Geochemistry, Mars, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Mars Exploration Program, Exploration of Mars, 01 natural sciences, Astrobiology, Impact crater, 13. Climate action, MSL Mars Gale Crater Rocknest, Rocknest, 0103 physical sciences, Sample Analysis at Mars, Aeolian processes, MSL, Rocknest aeolian deposit, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences
Abstract: The Rocknest aeolian deposit is similar to aeolian features analyzed by the Mars Exploration Rovers (MERs) Spirit and Opportunity. The fraction of sand
Published: 2013
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13. Volatile, Isotope, and Organic Analysis of Martian Fines with the Mars Curiosity Rover

Author: Leshin, L. A., Mahaffy, P. R., Webster, C. R., Cabane, M., Coll, P., Conrad, P. G., Archer, P. D., Atreya, S. K., Brunner, A. E., Buch, A., Eigenbrode, J. L., Flesch, G. J., Franz, H. B., Freissinet, C., Glavin, D. P., McAdam, A. C., Miller, K. E., Ming, D. W., Morris, R. V., Navarro-Gonzalez, R., Niles, P. B., Owen, T., Pepin, R. O., Squyres, S., Steele, A., Stern, J. C., Summons, R. E., Sumner, D. Y., Sutter, B., Szopa, C., Teinturier, S., Trainer, M. G., Wray, J. J., Grotzinger, J. P., Kemppinen, O., Bridges, N., Johnson, J. R., Minitti, M., Cremers, D., Bell, J. F., 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, P. S., 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, J. C., Blazquez, I. C., Gomez, F. G., Gomez-Elvira, J., Hettrich, S., Malvitte, A. L., Jimenez, M. M., Martinez-Frias, J., Martin-Soler, J., Martin-Torres, F. J., Jurado, A. M., Mora-Sotomayor, L., Caro, G. M., Lopez, S. N., Peinado-Gonzalez, V., Pla-Garcia, J., Manfredi, J. A. R., Romeral-Planello, J. J., Fuentes, S. A. S., Martinez, E. S., Redondo, J. T., Urqui-O'Callaghan, R., Mier, M.-P. Z., Chipera, S., Lacour, J.-L., Mauchien, P., Sirven, J.-B., 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, A.-M., Haukka, H., Kahanpaa, H., Kauhanen, J., Paton, M., Polkko, J., Schmidt, W., Siili, T., Fabre, C., Wilhelm, M. B., 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, Q.-M., Maurice, S., Meslin, P.-Y., Pallier, E., Parot, Y., Pinet, P., Schroder, S., Toplis, M., Lewin, E., Brunner, W., Heydari, E., Achilles, C., Oehler, D., Coscia, D., 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, R. S., Johnstone, S., Lanza, N., Little, C., Nelson, T., Wiens, R. C., Williams, R. B., 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, M. R., 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, K. L., Iagnemma, K., Goesmann, F., Goetz, W., Hviid, S., Johnson, M., Lefavor, M., Lyness, E., Breves, E., Dyar, M. D., Fassett, C., Blake, D. F., Bristow, T., DesMarais, D., Edwards, L., Haberle, R., Hoehler, T., Hollingsworth, J., Kahre, M., Keely, L., McKay, C., Bleacher, L., Brinckerhoff, W., Choi, D., Dworkin, J. P., Floyd, M., Garvin, J., Harpold, D., Martin, D. K., Pavlov, A., Raaen, E., Smith, M. D., Tan, F., Meyer, M., Posner, A., Voytek, M., Anderson, R. C., Aubrey, A., Beegle, L. W., Behar, A., Blaney, D., Brinza, D., Calef, F., Christensen, L., Crisp, J. A., DeFlores, L., Feldman, J., Feldman, S., Hurowitz, J., Jun, I., Keymeulen, D., Maki, J., Mischna, M., Morookian, J. M., Parker, T., Pavri, B., Schoppers, M., Sengstacken, A., Simmonds, J. J., Spanovich, N., Juarez, M. d. l. T., Vasavada, A. R., Yen, A., Cucinotta, F., Jones, J. H., Rampe, E., Nolan, T., Fisk, M., Radziemski, L., Barraclough, B., Bender, S., Berman, D., Dobrea, E. N., Tokar, R., Vaniman, D., Williams, R. M. E., Yingst, A., Lewis, K., Cleghorn, T., Huntress, W., Manhes, G., Hudgins, J., Olson, T., Stewart, N., Sarrazin, P., Grant, J., Vicenzi, E., Wilson, S. A., 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, S. P., Anderson, R. B., Herkenhoff, K., Lee, E. M., Sucharski, R., Hernandez, M. A. d. P., Avalos, J. J. B., Ramos, M., Kim, M.-H., Malespin, C., Plante, I., Muller, J.-P., Ewing, R., Boynton, W., Downs, R., Fitzgibbon, M., Harshman, K., Morrison, S., Dietrich, W., Kortmann, O., Palucis, M., Williams, A., Lugmair, G., Wilson, M. A., Rubin, D., Jakosky, B., Balic-Zunic, T., Frydenvang, J., Jensen, J. K., Kinch, K., Koefoed, A., Madsen, M. B., Stipp, S. L. S., Boyd, N., Campbell, J. L., Gellert, R., Perrett, G., Pradler, I., VanBommel, S., Jacob, S., Rowland, S., Savijarvi, H., Boehm, E., Bottcher, S., Burmeister, S., Guo, J., Kohler, J., Garcia, C. M., Mueller-Mellin, R., Wimmer-Schweingruber, R., Bridges, J. C., 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, L. C., Moersch, J., Tate, C., Day, M., Kocurek, G., Hallet, B., Sletten, R., Francis, R., McCullough, E., Cloutis, E., ten Kate, I. L., Arvidson, R., Fraeman, A., Scholes, D., Slavney, S., Stein, T., Ward, J., Berger, J., Moores, J. E., Department of Earth and Environmental Sciences [Troy, NY], Rensselaer Polytechnic Institute (RPI), NASA Goddard Space Flight Center (GSFC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS), Astromaterials Research and Exploration Science (ARES), NASA Johnson Space Center (JSC), NASA-NASA, Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Laboratoire de Génie des Procédés et Matériaux - EA 4038 (LGPM), CentraleSupélec, Center for Research and Exploration in Space Science and Technology [GSFC] (CRESST), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Laboratorio de Química de Plasmas y Estudios Planetarios [Mexico], Instituto de Ciencias Nucleares [Mexico], Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM)-Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), School of Physics and Astronomy [Minneapolis], University of Minnesota [Twin Cities] (UMN), University of Minnesota System-University of Minnesota System, Cornell University [New York], Geophysical Laboratory [Carnegie Institution], Carnegie Institution for Science, University of California [Davis] (UC Davis), University of California (UC), Jacobs Technology ESCG, Institut Pierre-Simon-Laplace (IPSL), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), School of Earth and Atmospheric Sciences [Atlanta], Georgia Institute of Technology [Atlanta], Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), NWO-NSO: The role of perchlorates in the preservation of organic compounds on Mars, Petrology, California Institute of Technology (CALTECH)-NASA, Universidad Nacional Autónoma de México (UNAM)-Universidad Nacional Autónoma de México (UNAM), Carnegie Institution for Science [Washington], University of California, École normale supérieure - Paris (ENS Paris), IMPEC - LATMOS, Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), University of Minnesota [Twin Cities], Cornell University, and École normale supérieure - Paris (ENS Paris)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National d'Études Spatiales [Toulouse] (CNES)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)
Subjects: Martian, Multidisciplinary, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Thermal decomposition, Curiosity rover, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], chemistry.chemical_element, Mars, organic analysis, Mars Exploration Program, 01 natural sciences, Astrobiology, chemistry.chemical_compound, chemistry, 13. Climate action, Isotopes of carbon, Rocknest, 0103 physical sciences, Sample Analysis at Mars, Carbonate, MSL Mars Volatiles Isotopes Organics Soil Gale Crater, 010303 astronomy & astrophysics, Carbon, 0105 earth and related environmental sciences
Abstract: Samples from the Rocknest aeolian deposit were heated to ~835°C under helium flow and evolved gases analyzed by Curiosity’s Sample Analysis at Mars instrument suite. H 2 O, SO 2 , CO 2 , and O 2 were the major gases released. Water abundance (1.5 to 3 weight percent) and release temperature suggest that H 2 O is bound within an amorphous component of the sample. Decomposition of fine-grained Fe or Mg carbonate is the likely source of much of the evolved CO 2 . Evolved O 2 is coincident with the release of Cl, suggesting that oxygen is produced from thermal decomposition of an oxychloride compound. Elevated δD values are consistent with recent atmospheric exchange. Carbon isotopes indicate multiple carbon sources in the fines. Several simple organic compounds were detected, but they are not definitively martian in origin.
Published: 2013
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14. Investigating the Oldest Traces of Life by AFM/Confocal Raman Spectroscopy: Applications for the Analysis of Martian Rocks.

Author: Foucher, F. and Westall, F.
Subjects: *MARS (Planet), *RAMAN spectroscopy, *SPACE biology, *ASTROBIOLOGY
Abstract: The next European mission to Mars, ExoMars (2016), is dedicated to the search for past and/or present traces of life. This is one of the primary goals of exo/astrobiology. Similarities in the environmental conditions of early Mars and the early Earth mean that life forms on the early Earth are good analogues for potential martian life. However, the oldest traces of terrestrial life are extremely small and highly sophisticated scientific equipment is required to reveal their subtle traces. Instruments that could observe biosignatures on in situ missions are, however, limited in resolution. In this study, various techniques are used to analyse martian analogue rocks containing traces of life. These rocks are 3.5-3.3 billion-years old volcanic sediments from the Pilbara in Australia and Barberton in South Africa. High magnification instruments were used to demonstrate the biogenicity of the fossilised structures. Space-adaptable techniques were then used in order to investigate larger scale biosignatures. Special emphasis was placed on Raman spectroscopy. This technique is extremely promising in the search for traces of life in situ on Mars. [ABSTRACT FROM AUTHOR]
Published: 2009
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15. The Geology and Habitability of Terrestrial Planets: Fundamental Requirements for Life.

Author: Fishbaugh, Kathryn E., Lognonné, Philippe, Raulin, François, Des Marais, David J., Korablev, Oleg, Southam, G., Rothschild, L. J., and Westall, F.
Abstract: The current approach to the study of the origin of life and to the search for life elsewhere is based on two assumptions. First, life is a purely physical phenomenon closely linked to specific environmental conditions. From this, we hypothesise that when these environmental conditions are met, life will arise and evolve. If these assumptions are valid, the search for life elsewhere should be a matter of mapping what we know about the range of environments in which life can exist, and then simply trying to find these environments elsewhere. Second, life can be clearly distinguished from the non-living world. While a single feature of a living organism left in the rock record is not always sufficient to determine unequivocally whether life was present, life often leaves multiple structural, mineralogical and chemical biomarkers that, in sum, support a conclusion that life was present. Our understanding of the habitats that can sustain or have sustained life has grown tremendously with the characterisation of extremophiles. In this chapter, we highlight the range of environments that are known to harbour life on Earth, describe the environments that existed during the period of time when life originated on Earth, and compare these habitats to the suitable environments that are found elsewhere in our solar system, where life could have arisen and evolved. [ABSTRACT FROM AUTHOR]
Published: 2007
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16. The Geology and Habitability of Terrestrial Planets: Fundamental Requirements for Life.

Author: Southam, G., Rothschild, L. J., and Westall, F.
Subjects: ORIGIN of life, PLANETS, EARTH (Planet), SUSTAINABLE development, ECOLOGY, COMPARATIVE studies, ASTROBIOLOGY, CONDUCT of life
Abstract: The current approach to the study of the origin of life and to the search for life elsewhere is based on two assumptions. First, life is a purely physical phenomenon closely linked to specific environmental conditions. From this, we hypothesise that when these environmental conditions are met, life will arise and evolve. If these assumptions are valid, the search for life elsewhere should be a matter of mapping what we know about the range of environments in which life can exist, and then simply trying to find these environments elsewhere. Second, life can be clearly distinguished from the non-living world. While a single feature of a living organism left in the rock record is not always sufficient to determine unequivocally whether life was present, life often leaves multiple structural, mineralogical and chemical biomarkers that, in sum, support a conclusion that life was present. Our understanding of the habitats that can sustain or have sustained life has grown tremendously with the characterisation of extremophiles. In this chapter, we highlight the range of environments that are known to harbour life on Earth, describe the environments that existed during the period of time when life originated on Earth, and compare these habitats to the suitable environments that are found elsewhere in our solar system, where life could have arisen and evolved. [ABSTRACT FROM AUTHOR]
Published: 2007
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17. ∼1.8 Ga iron-mineralized microbiota from the Gunflint Iron Formation, Ontario, Canada: implications for Mars

Author: Schelble, R.T., Westall, F., and Allen, C.C.
Subjects: *MICROBIOLOGY, *ELECTRON microscopy, *BIOLOGY
Abstract: A ∼1.8 Ga banded-iron stromatolite from the Mink Mountain locality (PPRG 336) of the Gunflint Iron Formation, Ontario, Canada was investigated as an analogue to Martian hematite deposits which have the potential to contain fossilized Martian life. The stromatolitic sample was primarily composed of quartz (SiO2) with fractional amounts of hematite (Fe2O3), greenalite ((Fe,Mg)3Si2O5(OH)2), and minor amounts of stilpnomelane (K(Fe2+,Mg,Fe3+, Al)8(Si,Al)12(O,OH)27 · 2H2O). Iron-bearing minerals were present within thin, discontinuous bands aligned roughly parallel. Octahedral pseudomorphs of hematite after magnetite occurred as localized elongate clusters, as well as on the outer rims of detrital oncolitic structures. Microcrystalline greenalite was present as a clay occurring in layers subparallel to the stromatolitic layering. Greenalite was observed in both the silica- and iron-rich layers, as well as within oncolitic structures. Irregular aggregates of radiating stilpnomelane needles extended into the silica matrix. Optical microscopy (OM) and scanning electron microscopy (SEM) revealed 5–10 μm diameter iron-mineralized or siliceous, concentrically laminated, ooid-like structures in localized patches. OM, SEM, and energy dispersive X-ray analyses (EDX) were used to characterize microfossils mineralized by iron-oxides in the stromatolite. The microfossils consisted of coccoidal and filamentous forms. The coccoids (∼0.5 to 2 μm diameter) were present both in chains and individually throughout the silica- and iron-rich bands, while the filamentous remnants (∼1–3 μm diameter, and up to 200 μm length) were localized and patchy in the sample. While the Gunflint Iron Formation does not provide us with a perfect analogue to the Martian hematite site, it does establish the potential for finding iron-mineralized microorganisms within Martian sediments. [Copyright &y& Elsevier]
Published: 2004
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18. ANCIENT BIOSIGNATURES IN ROCKS AND THEIR RELEVANCE IN THE SEARCH FOR EXTRATERRESTRIAL LIFE

Author: Westall, F., BARBARA CAVALAZZI, Foucher, F., Hubert, A., Westall F., Cavalazzi B., Foucher F., and Hubert A.
Subjects: ASTROBIOLOGY, BIOSIGNATURES

19. On biosignatures for Mars

Author: Frédéric Foucher, Barbara Cavalazzi, Jorge L. Vago, Laura Clodoré, Keyron Hickman-Lewis, Frances Westall, Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), University of Bologna/Università di Bologna, Agence Spatiale Européenne = European Space Agency (ESA), Frapart, Isabelle, and Westall F., Hickman-Lewis K., Cavalazzi B., Foucher F., Clodoré L., Vago J.L.
Subjects: ALH84001, Physics and Astronomy (miscellaneous), clay, Mars Exploration Program, biosignature, Astrobiology, [SDU] Sciences of the Universe [physics], Mar, carbonate, silica, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Earth and Planetary Sciences (miscellaneous), salt, Ecology, Evolution, Behavior and Systematics
Abstract: In this work, we address the difficulty of reliably identifying traces of life on Mars. Several independent lines of evidence are required to build a compelling body of proof. In particular, we underline the importance of correctly interpreting the geological and mineralogical context of the sites to be explored for the presence of biosignatures. We use as examples to illustrate this, ALH84001 (where knowledge of the geological context was very limited) and other terrestrial deposits, for which this could be properly established. We also discuss promising locations and formations to be explored by ongoing and future rover missions, including Oxia Planum, which, dated at 4.0 Ga, is the most ancient Mars location targeted for investigation yet.
Published: 2021
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20. Astrobiology of life on Earth

Author: Kathleen C. Benison, Hitesh Changela, Tiffany D. Dallas, Catharine A. Conley, Alfonso F. Davila, Rocco L. Mancinelli, Michael T. Madigan, John E. Hallsworth, Teresa Rinaldi, Ricardo Amils, Michail M. Yakimov, Alexander Rapoport, Laura Selbmann, Barbara Cavalazzi, Frances Westall, UAM. Departamento de Biología Molecular, Institute for Global Food Security [Belfast], Queen's University [Belfast] (QUB), Bay Area Environmental Research Institute (BAER), NASA Ames Research Center (ARC), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Department of Geology and Geography [Morgantown], West Virginia University [Morgantown], University of Latvia (LU), University of Bologna, Università degli studi della Tuscia [Viterbo], Institute of Geology and Geophysics [Beijing] (IGG), Chinese Academy of Sciences [Beijing] (CAS), The University of New Mexico [Albuquerque], Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), Institute for Biological Resources and Marine Biotechnology (IRBIM), Universidad Autonoma de Madrid (UAM), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Southern Illinois University [Carbondale] (SIU), Hallsworth J.E., Mancinelli R.L., Conley C.A., Dallas T.D., Rinaldi T., Davila A.F., Benison K.C., Rapoport A., Cavalazzi B., Selbmann L., Changela H., Westall F., Yakimov M.M., Amils R., Madigan M.T., Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), University of Bologna/Università di Bologna, Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Universidad Autónoma de Madrid (UAM), Frapart, Isabelle, Hallsworth, J. E. [0000-0001-6797-9362], Mancinelli, R. L. [0000-0002-8200-4878], Dallas, T. D. [0000-0002-5310-9857], Rinaldi, T. [0000-0001-6291-245X], Benison, K. C. [0000-0001-6104-2333], Rapoport, A. [0000-0002-6185-0039], Selbmann, L. [0000-0002-8967-3329], Amils, R. [0000-0002-7560-1033], and Biotechnology and Biological Sciences Research Council (BBSRC)
Subjects: Extraterrestrial Environment, Earth, Planet, terrestrial life, Biology, Microbiology, Astrobiology, [SDU] Sciences of the Universe [physics], 03 medical and health sciences, Microbial ecology, halophiles, Exobiology, Environmental Microbiology, Extremophile, Humans, SDG 14 - Life Below Water, Ecology, Evolution, Behavior and Systematics, Ecosystem, extremophiles, 030304 developmental biology, 2. Zero hunger, 0303 health sciences, Extremophile Viruses, 030306 microbiology, Biosphere, Mars Exploration Program, 15. Life on land, Mars exploration, Biología y Biomedicina / Biología, habitability, Habitat, 13. Climate action, [SDU]Sciences of the Universe [physics], planetary protection, Earth (chemistry), astrobiology, extremophile, halophile
Abstract: Astrobiology is mistakenly regarded by some as a field confined to studies of life beyond Earth. Here, we consider life on Earth through an astrobiological lens. Whereas classical studies of microbiology historically focused on various anthropocentric sub-fields (such as fermented foods or commensals and pathogens of crop plants, livestock and humans), addressing key biological questions via astrobiological approaches can further our understanding of all life on Earth. We highlight potential implications of this approach through the articles in this Environmental Microbiology special issue ‘Ecophysiology of Extremophiles’. They report on the microbiology of places/processes including low-temperature environments and chemically diverse saline- and hypersaline habitats; aspects of sulphur metabolism in hypersaline lakes, dysoxic marine waters, and thermal acidic springs; biology of extremophile viruses; the survival of terrestrial extremophiles on the surface of Mars; biological soils crusts and rock-associated microbes of deserts; subsurface and deep biosphere, including a salticle formed within Triassic halite; and interactions of microbes with igneous and sedimentary rocks. These studies, some of which we highlight here, contribute to our understanding of the spatiotemporal reach of Earth'sfunctional biosphere, and the tenacity of terrestrial life. Their findings will help set the stage for future work focused on the constraints for life, and how organisms adapt and evolve to circumvent these constraints. Funding was provided by the Biotechnology and Biological Sciences Research Council (BBSRC, United Kingdom) project BBF003471. Peerreview
Published: 2021
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21. Planning Implications Related to Sterilization-Sensitive Science Investigations Associated with Mars Sample Return (MSR)

Author: Michael A. Velbel, Charles S. Cockell, Daniel P. Glavin, Bernard Marty, Aaron B. Regberg, Alvin L. Smith, Nicholas J. Tosca, Meenakshi Wadhwa, Gerhard Kminek, Michael A. Meyer, David W. Beaty, Brandi Lee Carrier, Timothy Haltigin, Lindsay E. Hays, Carl B. Agee, Henner Busemann, Barbara Cavalazzi, Vinciane Debaille, Monica M. Grady, Ernst Hauber, Aurore Hutzler, Francis M. McCubbin, Lisa M. Pratt, Caroline L. Smith, Roger E. Summons, Timothy D. Swindle, Kimberly T. Tait, Arya Udry, Tomohiro Usui, Frances Westall, Maria-Paz Zorzano, and Velbel M.A., Beaty D.W., CarrierB.L., Cockell C.S., Glavin D.P., Marty B., Regberg A.B., Smith A.l., Tosca N.J., Wadhwa M., Kminek G., Meyer M.A., Haltigin T., Hays L.E., Agee C.B., Busemann H., Cavalazzi B., Debaille V., Grady M.M., Hauber E., Hutzler A., McCubbin F.M., Pratt L.M., Smith C.L., Summons R.E., Swindle T.D., Tait K.T., Udry A., Usui T., Westall F., Zorzano M.-P.
Subjects: geology, Extraterrestrial Environment, Nitrogen, Polymers, astrobiology, Mars, sample return, Hazardous Substances, Nucleic Acids, Exobiology, Minerals, Fatty Acids, Sterilization, Water, Phosphorus, DNA, Agricultural and Biological Sciences (miscellaneous), Carbon, Oxygen, Sterols, Space and Planetary Science, RNA, Gases, NASA/ESA Mars Sample Return (MSR), laboratory analysis, Hydrogen
Abstract: The NASA/ESA Mars Sample Return (MSR) Campaign seeks to establish whether life on Mars existed where and when environmental conditions allowed. Laboratory measurements on the returned samples are useful if what is measured is evidence of phenomena on Mars rather than of the effects of sterilization conditions. This report establishes that there are categories of measurements that can be fruitful despite sample sterilization and other categories that cannot. Sterilization kills living microorganisms and inactivates complex biological structures by breaking chemical bonds. Sterilization has similar effects on chemical bonds in non-biological compounds, including abiotic or pre-biotic reduced carbon compounds, hydrous minerals, and hydrous amorphous solids. We considered the sterilization effects of applying dry heat under two specific temperature-time regimes and the effects of γ-irradiation. Many measurements of volatile-rich materials are sterilization sensitive—they will be compromised by either dehydration or radiolysis upon sterilization. Dry-heat sterilization and γ-irradiation differ somewhat in their effects but affect the same chemical elements. Sterilization-sensitive measurements include the abundances and oxidation-reduction (redox) states of redox-sensitive elements, and isotope abundances and ratios of most of them. All organic molecules, and most minerals and naturally occurring amorphous materials that formed under habitable conditions, contain at least one redox-sensitive element. Thus, sterilization-sensitive evidence about ancient life on Mars and its relationship to its ancient environment will be severely compromised if the samples collected by Mars 2020 rover Perseverance cannot be analyzed in an unsterilized condition. To ensure that sterilization-sensitive measurements can be made even on samples deemed unsafe for unsterilized release from containment, contingency instruments in addition to those required for curation, time-sensitive science, and the Sample Safety Assessment Protocol would need to be added to the Sample Receiving Facility (SRF). Targeted investigations using analogs of MSR Campaign-relevant returned-sample types should be undertaken to fill knowledge gaps about sterilization effects on important scientific measurements, especially if the sterilization regimens eventually chosen are different from those considered in this report., Astrobiology, 22 (S1), ISSN:1531-1074, ISSN:1557-8070
Published: 2021

22. Biosignatures in Deep Time

Author: Barbara Cavalazzi, Frances Westall, Keyron Hickman-Lewis, B. Cavalazzi, F. Westall, Westall F., Hickman-Lewis K., Cavalazzi B., Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), University of Bologna, and Barbara Cavalazzi, Frances Westall
Subjects: early Earth, microfossil, 010504 meteorology & atmospheric sciences, Archean, Mars Exploration Program, 010502 geochemistry & geophysics, Early Earth, Geologic record, Life on Mars, 01 natural sciences, Astrobiology, 13. Climate action, Stage (stratigraphy), [CHIM]Chemical Sciences, biosignatures, Microbial mat, Deep time, 0105 earth and related environmental sciences, Archean life
Abstract: International audience; Life on the early Earth inhabited a planet whose environment was vastly different from the Earth of today. An anaerobic and hot early Earth was the birthplace of the first living cells but wide-spread small-scale physico-chemical diversity provided opportunities for a variety of specialists: alkalophiles, acidophiles, halophiles etc. The earliest record of life has been lost due to plate tectonic recycling and the oldest preserved terranes (~3.9–3.7 Ga) are heavily altered by metamorphism, although they may contain traces of fossil life. As of ~3.5 Ga, ancient sediments are so well-preserved that a broad diversity of micro-environments and fossil traces of life can be studied, providing a surprising window into communities of microbes that had already reached the evolutionary stage of photosynthesis. From the wide variety of traces of ancient life that have been reported from the Archaean geological record in Greenland, Canada, South Africa and Western Australia, we examine a few particularly pertinent examples. Biosignatures in the rock record include microfossils, microbial mats, stromatolites, microbially induced sedimentary structures, biominerals, biologically indicative isotopic ratios and fractionations, elemental distributions, organochemical patterns and other geochemical peculiarities best explained by biological mediation. Due to dynamic geological reprocessing over the billions of years since these fossils entered the rock record, identifications of very ancient traces of life have been subject to criticism, hence the often complex arguments regarding their biogenicity. We here highlight a range of unambiguously bona fide and widely supported examples of fossil biosignatures. Fossil biosignatures have great promise as analogues of life that might be detected on other planets. In this respect, the study of the early Earth is particularly pertinent to the search for life on Mars, given the planetary- and microbial-scale similarities that prevailed on both planets during their early histories, together with the lack of subsequent geological reprocessing on Mars, which may make it an ideal repository for a near-pristine fossil record.
Published: 2019
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23. Astrobiology, the Emergence of Life, and Planetary Exploration

Author: Sherry L. Cady, Barbara Cavalazzi, Roberto Orosei, Mihaela Glamoclija, Frances Westall, André Brack, Rossi A., van Gasselt S., Cavalazzi B., Glamoclija M., Brack A., Westall F., Orosei R., and Cady S.L.
Subjects: Martian, Solar System, Astrobiology, Biosignatures, Habitability, History, Meteorite, Planet, Abiogenesis, Astrobiology Science and Technology for Exploring Planets, Life on Mars, Astrobiology, Planetary exploration
Abstract: Astrobiology brings together scientific disciplines focused on deciphering the origin of life, its nature, evolution, and distribution in the universe. Exceptionally rapid progress in our understanding has been made over the past four decades, including new insights into how life could have emerged on Earth, the revelation that life can thrive in the most hostile terrestrial environments, evidence of the presence of liquid water throughout the universe, a controversial discovery of past life in a Martian meteorite that reinvigorated the search for life on Mars, and the discovery of Earth-like planets orbiting stars other than our Sun in the Milky Way. Although Earth is the only planet known to host life in our Solar System, continued advances in the field of astrobiology stimulate the search for life and its origin beyond our planet.
Published: 2018

24. Biosignatures in rocks

Author: Frances Westall, Barbara Cavalazzi, Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), Reitner, Joachim, Thiel, Volker, Frapart, Isabelle, Reitner, Joachim, Thiel, Volker, Reitner J., Thiel V., Fritz H. W., Kappler A., Konhauser K., Reid P., Zhang X., Reitner, J. V. Thiel, Westall F., and Cavalazzi B.
Subjects: 010504 meteorology & atmospheric sciences, Origin of Life, Geology, Biogeochemistry, 010502 geochemistry & geophysics, PALEOBIOLOGY, Astrobiology, 01 natural sciences, Microbiology, Geobiology, 13. Climate action, MICROFOSSILS, Biogeoscience, 0105 earth and related environmental sciences
Abstract: The interplay between Geology and Biology has shaped the Earth from the early Precambrian, 4 billion years ago. Moving beyond the borders of the classical core disciplines, Geobiology strives to identify cause-and-effect chains and synergisms between the geo- and the biospheres that have been driving evolution of life in modern and ancient environments. Combining modern methods, geobiological information can be extracted not only from visible remains of organisms, but also from organic molecules, rock fabrics, minerals, isotopes and other tracers. Exploring these processes and their signatures also creates enormous applied potentials with respect to issues of environment protection, public health, energy and resource management. The Encyclopedia of Geobiology is designed as a key reference for students, researchers, teachers, and the informed public to provide basic, but comprehensible knowledge on this rapidly expanding discipline at the interface between modern geo- and biosciences.
Published: 2011

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24 results on '"Westall, F"'

1. Time-Sensitive Aspects of Mars Sample Return (MSR) Science

2. Science and Curation Considerations for the Design of a Mars Sample Return (MSR) Sample Receiving Facility

3. Preliminary Planning for Mars Sample Return (MSR) Curation Activities in a Sample Receiving Facility

4. Searching for Signs of Life on Other Planets: Mars a Case Study

5. Earth as a Tool for Astrobiology:A European Perspective

6. MICROORGANISMS FROM MARS ANALOGUE ENVIRONMENTS IN EARTH - COULD THEY SURVIVE ON MARS?

7. Assessing the habitability of the MASE Mars analogue sites

8. Mars Analogues for space exploration - from anaerobic field site to culture collection

9. Biosignatures for Mars

10. Fe-framboids from Devonian methane-related carbonate mounds: potential fossil analogues of MOA-SRB consortia and relationships with Martian astrobiology

11. Abundance and isotopic composition of gases in the martian atmosphere from the Curiosity rover

12. Curiosity at Gale Crater, Mars: Characterization and analysis of the rocknest sand shadow

13. Volatile, Isotope, and Organic Analysis of Martian Fines with the Mars Curiosity Rover

14. Investigating the Oldest Traces of Life by AFM/Confocal Raman Spectroscopy: Applications for the Analysis of Martian Rocks.

15. The Geology and Habitability of Terrestrial Planets: Fundamental Requirements for Life.

16. The Geology and Habitability of Terrestrial Planets: Fundamental Requirements for Life.

17. ∼1.8 Ga iron-mineralized microbiota from the Gunflint Iron Formation, Ontario, Canada: implications for Mars

18. ANCIENT BIOSIGNATURES IN ROCKS AND THEIR RELEVANCE IN THE SEARCH FOR EXTRATERRESTRIAL LIFE

19. On biosignatures for Mars

20. Astrobiology of life on Earth

21. Planning Implications Related to Sterilization-Sensitive Science Investigations Associated with Mars Sample Return (MSR)

22. Biosignatures in Deep Time

23. Astrobiology, the Emergence of Life, and Planetary Exploration

24. Biosignatures in rocks

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