Biology
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p13b1394g&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #P13B-1394
Biology
[0448] Biogeosciences / Geomicrobiology, [0456] Biogeosciences / Life In Extreme Environments, [6225] Planetary Sciences: Solar System Objects / Mars
Scientific paper
The first astrobiological mission specially designed to detect life on Mars, the Viking missions, thought life unlikely, considering the amount of UV radiation bathing the surface of the planet, the resulting oxidative conditions, and the lack of adequate atmospheric protection. The necessity of the Europa surface exploration comes from the idea of a water ocean existence in its interior. Life needs several requirements for its establishment but, the only sine qua nom elements is the water, taking into account our experience on Earth extreme ecosystems The discovery of extremophiles on Earth widened the window of possibilities for life to develop in the universe, and as a consequence on Mars. The compilation of data produced by the ongoing missions (Mars Global Surveyor, Mars Odyssey, Mars Express and Mars Exploration Rover Opportunity) offers a completely different view: signs of an early wet Mars and rather recent volcanic activity. The discovery of important accumulations of sulfates, and the existence of iron minerals like jarosite, goethite and hematite in rocks of sedimentary origin has allowed specific terrestrial models related with this type of mineralogy to come into focus. Río Tinto (Southwestern Spain, Iberian Pyritic Belt) is an extreme acidic environment, product of the chemolithotrophic activity of microorganisms that thrive in the massive pyrite-rich deposits of the Iberian Pyritic Belt. The high concentrations of ferric iron and sulfates, products of the metabolism of pyrite, generate a collection of minerals, mainly gypsum, jarosite, goethite and hematites, all of which have been detected in different regions of Mars (Fernández-Remolar et al., 2004). But, where to look for life in other planetary bodies? Planet`s or Icy Moon`s surface are adverse for life. Some particular protective environments or elements should house the organic molecules and the first bacterial life forms (Gómez F. et al., 2007). Terrestrial analogues work could help us to afford its comprehension (Gómez F. et al., 2010). We are reporting here some preliminary studies about endolithic niches inside salt deposits used by phototrophs for taking advantage of sheltering particular light wavelengths. These acidic salts deposits located in Río Tinto shelter life forms which are difficult to localize by eye. Molecular ecology techniques are needed for its localization and study. We also are reporting here some results about bacterial survivability in Mars simulation conditions (Gómez F. et al., 2010). Final objective of this work is the development of the Habitability Index. Bibliography Fernández-Remolar, D. et al., Planetary and Space Science 52 (2004) 239 - 248 Gómez, F. et al., Icarus 191 (2007) 352-359. Gómez, F. et al. Icarus (2010), doi:10.1016/j.icarus.2010.05.027 Acknowledgments This study was funded by the project ESP2006-06640 from Spanish Ministry of Education and Science and FEDER funds from European Community.
Amils Ricardo
Gomez Facundo
Gomez-Elvira Javier
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