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Ancient Mars is now considered to have had an environment somewhat similar to that of Earth in terms of the existence of large bodies of water, a wide range of surface oxidation states, an active dynamo and associated magnetic field, magmatism and tectonism which includes mountain building and basin formation, and appearances of variety of chemical components potentially building blocks of life. Similar to habitable Earth, ancient Mars included hydrological cycling among the atmosphere, ocean, and landmass (southern cratered highlands), and plate tectonism cannot be ruled out. Endogenic activities have continued until even very recently, and recent water-related geological features indicate prolonged existence of aquifer systems, where habitable environments may exist for a significant period of time. Occasional releases of volatiles from such aquifer systems may ultimately account for the detection of methane by the Curiosity rover in the Gale crater and the inconclusive result (i.e., not unambiguous denial) of metabolism-detection instrument onboard Viking landers. Unequivocal evidence of the existence of subsurface aquifers or extant endogenic activity is, however, still lacking possibly due to the existence of homogeneous regolith materials covering the surface of Mars. Also, even if a habitable environment exists at depth, accessing the environment by a spacecraft (either a lander or a rover) has been considered to be challenging especially because such an environment has been generally thought to exist more than several kilometers below the Martian surface. Recent findings of a recurring slope lineae (RSL) point to traces of possible seasonal liquid water flows along slopes, findings of which will likely change the above prevailing view; some of these features might result from the partial discharges from an aquifer. In other words, RSLs might provide a natural bridge between a subsurface aquifer and the surface accessible by a rover. Thus, subsurface structures near such features become prime targets to be explored through future missions. Once the presence of ground water is confirmed, especially an aquifer, mapping and characterizing the distribution of subsurface water would significantly help address the 地学雑誌 Journal of Geography(Chigaku Zasshi) 125(1)171–184 2016 doi:10.5026/jgeography.125.171 * 東京大学総合研究博物館 ** ダヌンツィオ大学国際惑星科学研究大学院 *** 東京工業大学理工学研究科 **** 東京薬科大学生命科学部 * University Museum, University of Tokyo, Tokyo, 113-0033, Japan ** International Research School of Planetary Sciences, Università d'Annunzio, 65127 Pescara, Italy *** Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo, 152-8551, Japan **** Department of Applied Life Sciences, Tokyo University of Pharmacy and Life Sciences, Tokyo, 192-0392, Japan

Geomorphological View of the Environmental History of Mars and Candidate Habitable Environments