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      A New Analysis of Mars “Special Regions”: Findings of the Second MEPAG Special Regions Science Analysis Group (SR-SAG2)

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          Abstract

          A committee of the Mars Exploration Program Analysis Group (MEPAG) has reviewed and updated the description of Special Regions on Mars as places where terrestrial organisms might replicate (per the COSPAR Planetary Protection Policy). This review and update was conducted by an international team (SR-SAG2) drawn from both the biological science and Mars exploration communities, focused on understanding when and where Special Regions could occur. The study applied recently available data about martian environments and about terrestrial organisms, building on a previous analysis of Mars Special Regions (2006) undertaken by a similar team. Since then, a new body of highly relevant information has been generated from the Mars Reconnaissance Orbiter (launched in 2005) and Phoenix (2007) and data from Mars Express and the twin Mars Exploration Rovers (all 2003). Results have also been gleaned from the Mars Science Laboratory (launched in 2011). In addition to Mars data, there is a considerable body of new data regarding the known environmental limits to life on Earth-including the potential for terrestrial microbial life to survive and replicate under martian environmental conditions. The SR-SAG2 analysis has included an examination of new Mars models relevant to natural environmental variation in water activity and temperature; a review and reconsideration of the current parameters used to define Special Regions; and updated maps and descriptions of the martian environments recommended for treatment as "Uncertain" or "Special" as natural features or those potentially formed by the influence of future landed spacecraft. Significant changes in our knowledge of the capabilities of terrestrial organisms and the existence of possibly habitable martian environments have led to a new appreciation of where Mars Special Regions may be identified and protected. The SR-SAG also considered the impact of Special Regions on potential future human missions to Mars, both as locations of potential resources and as places that should not be inadvertently contaminated by human activity.

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          A habitable fluvio-lacustrine environment at Yellowknife Bay, Gale crater, Mars.

          The Curiosity rover discovered fine-grained sedimentary rocks, which are inferred to represent an ancient lake and preserve evidence of an environment that would have been suited to support a martian biosphere founded on chemolithoautotrophy. This aqueous environment was characterized by neutral pH, low salinity, and variable redox states of both iron and sulfur species. Carbon, hydrogen, oxygen, sulfur, nitrogen, and phosphorus were measured directly as key biogenic elements; by inference, phosphorus is assumed to have been available. The environment probably had a minimum duration of hundreds to tens of thousands of years. These results highlight the biological viability of fluvial-lacustrine environments in the post-Noachian history of Mars.
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            Evidence for recent groundwater seepage and surface runoff on Mars.

            Relatively young landforms on Mars, seen in high-resolution images acquired by the Mars Global Surveyor Mars Orbiter Camera since March 1999, suggest the presence of sources of liquid water at shallow depths beneath the martian surface. Found at middle and high martian latitudes (particularly in the southern hemisphere), gullies within the walls of a very small number of impact craters, south polar pits, and two of the larger martian valleys display geomorphic features that can be explained by processes associated with groundwater seepage and surface runoff. The relative youth of the landforms is indicated by the superposition of the gullies on otherwise geologically young surfaces and by the absence of superimposed landforms or cross-cutting features, including impact craters, small polygons, and eolian dunes. The limited size and geographic distribution of the features argue for constrained source reservoirs.
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              Responses of soil microbial communities to water stress: results from a meta-analysis.

              Soil heterotrophic respiration and nutrient mineralization are strongly affected by environmental conditions, in particular by moisture fluctuations triggered by rainfall events. When soil moisture decreases, so does decomposers' activity, with microfauna generally undergoing stress sooner than bacteria and fungi. Despite differences in the responses of individual decomposer groups to moisture availability (e.g., bacteria are typically more sensitive than fungi to water stress), we show that responses of decomposers at the community level are different in soils and surface litter, but similar across biomes and climates. This results in a nearly constant soil-moisture threshold corresponding to the point when biological activity ceases, at a water potential of about -14 MPa in mineral soils and -36 MPa in surface litter. This threshold is shown to be comparable to the soil moisture value where solute diffusion becomes strongly inhibited in soil, while in litter it is dehydration rather than diffusion that likely limits biological activity around the stress point. Because of these intrinsic constraints and lack of adaptation to different hydro-climatic regimes, changes in rainfall patterns (primary drivers of the soil moisture balance) may have dramatic impacts on soil carbon and nutrient cycling.
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                Author and article information

                Journal
                Astrobiology
                Astrobiology
                Mary Ann Liebert Inc
                1531-1074
                1557-8070
                November 2014
                November 2014
                : 14
                : 11
                : 887-968
                Affiliations
                [1 ]Department of Biology, East Carolina University, Greenville, North Carolina, USA.
                [2 ]Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA.
                [3 ]Altoona College, Pennsylvania State University, Altoona, Pennsylvania, USA.
                [4 ]Department of Physics and Astronomy, Northern Arizona University, Flagstaff, Arizona, USA.
                [5 ]New Mexico Tech, Socorro, New Mexico, USA.
                [6 ]Arkansas Center for Space and Planetary Sciences, University of Arkansas, Fayetteville, Arkansas, USA.
                [7 ]Space Science Institute, Boulder, Colorado, USA.
                [8 ]German Aerospace Center, Institute of Planetary Research, Berlin, Germany.
                [9 ]Cooperative Institute for Research in Environmental Sciences, University of Colorado, Boulder, Colorado, USA.
                [10 ]Institute for Global Food Security, School of Biological Sciences, Queen's University Belfast, Belfast, UK.
                [11 ]Department of Earth, Environmental, and Planetary Sciences, Brown University, Providence, Rhode Island, USA.
                [12 ]Canadian Space Agency, Saint-Hubert, Quebec, Canada.
                [13 ]University of Arizona, Tucson, Arizona, USA.
                [14 ]Southwest Research Institute, Boulder, Colorado, USA.
                [15 ]Department of Microbiology, University of Tennessee, Knoxville, Tennessee, USA.
                [16 ]Department of Microbiology and Cell Science, University of Florida, Merritt Island, Florida, USA.
                [17 ]Department of Geological Sciences, The University of Texas at Austin, Austin, Texas, USA.
                [18 ]Queen's University, Kingston, Ontario, Canada.
                [19 ]Department of Geoscience and NASA Astrobiology Institute, University of Wisconsin, Madison, Wisconsin, USA.
                [20 ]University of Toronto, Toronto, Ontario, Canada.
                [21 ]U.S. Geological Survey, Flagstaff, Arizona, USA.
                [22 ]School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, Georgia, USA.
                Article
                10.1089/ast.2014.1227
                25401393
                3a4a8674-9f09-4340-83eb-31535d8e437e
                © 2014
                History

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