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Report of the COSPAR mars special regions colloquium
Authors:G Kminek  JD Rummel  CS Cockell  R Atlas  N Barlow  D Beaty  W Boynton  M Carr  S Clifford  CA Conley  AF Davila  A Debus  P Doran  M Hecht  J Heldmann  J Helbert  V Hipkin  G Horneck  TL Kieft  G Klingelhoefer  M Meyer  H Newsom  GG Ori  J Parnell  D Prieur  F Raulin  D Schulze-Makuch  JA Spry  PE Stabekis  E Stackebrandt  J Vago  M Viso  M Voytek  L Wells  F Westall
Institution:1. ESA-ESTEC, Keplerlaan 1, 2200 Noordwijk, The Netherlands;2. East Carolina University, East Fifth Street, Greenville, NC 27858-4353, USA;3. Open University, Milton Keynes, MK7 6AA, UK;4. University of Louisville, Louiseville, KY 40292, USA;5. Northern Arizona University, Flagstaff, AZ 86011-6010, USA;6. NASA Jet Propulsion Laboratory, Pasadena, 4800 Oak Grove Drive, CA 91109-8001, USA;g Lunar and Planetary Lab, University of Arizona, Tucson, AZ 85721, USA;h United States Geological Survey Pacific Science Center, 400 Natural, Bridges Drive, Santa Cruz, CA 95060, USA;i Lunar and Planetary Institute, 3600 Bay Area Blvd, Houston, TX 77058, USA;j NASA Headquarters, Washington, DC 20546-0001, USA;k NASA Ames Research Center, Mountain View, CA 94043, USA;l CNES, Agence Française de l’Espace, 18, Avenue Edouard Belin 31 401 Toulouse Cedex 9, France;m University of Illinois in Chicago, 845 West Taylor Street, Chicago, IL 60607, USA;n DLR, Inst. fuer Planetenforschung, Berlin, Germany;o Canadian Space Agency, 6767 Route de l’Aéroport, Saint-Hubert, Quebec, Canada J3Y 8Y9;p DLR, Linder Höhe, 51147 Köln, Germany;q New Mexico Tech, 801 Leroy Pl., Socorro, NM 87801, USA;r University of Mainz, 55131 Mainz, Germany;s University of New Mexico, Albuquerque, NM 87131-0001, USA;t IRSPS, Universita d’Annunzio, 65127 Pescara, Italy;u University of Aberdeen, Aberdeen, AB24 3UE, UK;v University of Brest, Brest, France;w CNRS and Universités Paris, 61 Avenue du Général de Gaulle, F-94010 Créteil Cedex, France;x Washington State University, Pullman, WA 99164-6376, USA;y DSMZ, Inhoffenstrasse 7B, 38124 Braunschweig, Germany;z University of Pennsylvania, Philadelphia, PA 19014, USA;aa CNRS, 45100 Orléans, France
Abstract:In this paper we present the findings of a COSPAR Mars Special Regions Colloquium held in Rome in 2007. We review and discuss the definition of Mars Special Regions, the physical parameters used to define Mars Special Regions, and physical features on Mars that can be interpreted as Mars Special Regions. We conclude that any region experiencing temperatures > −25 °C for a few hours a year and a water activity > 0.5 can potentially allow the replication of terrestrial microorganisms. Physical features on Mars that can be interpreted as meeting these conditions constitute a Mars Special Region. Based on current knowledge of the martian environment and the conservative nature of planetary protection, the following features constitute Mars Special regions: Gullies and bright streaks associated with them, pasted-on terrain, deep subsurface, dark streaks only on a case-by-case basis, others to be determined. The parameter definition and the associated list of physical features should be re-evaluated on a regular basis.
Keywords:Special regions  Mars  Planetary protection  Forward contamination  Low temperature  Water activity
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