Scientific and Technical Aerospace Reports Volume 39 April 6, 2001

This work will describe the Thermal Evolved Gas Analyser (TEGA) instrument as it was built for the Mars Polar Lander
mission, its applicability to future Mars missions, and modest modifications which can make it more valuable to the future exploration
of Mars.
Author
Mars Polar Lander; Mars Missions; Instrument Packages; Gas Analysis
20010023063 Centre National de la Recherche Scientifique, Centre de Biophysique Moleculaire, Orleans, France
Search for Organic Matter on Mars: Complementarity of In Situ Analyses and Laboratory Analyses of Martian Samples
Brack, A., Centre National de la Recherche Scientifique, France; Commeyras, A., Montpellier-2 Univ., France; Derenne, S., Ecole
Nationale Superieure de Chimie, France; Despois, D., Observatoire de Bordeaux, France; Dhamelincourt, P., Lille-1 Univ.,
France; Dobrijevic, M., Observatoire de Bordeaux, France; Engrand, C., Centre de Spectrometrie Nucleaire et de Spectrometrie
de Masse, France; Geffard, M., Ecole Practique des Hautes Etudes, France; Grenier-Loustalot, M. F., Centre National de la
Recherche Scientifique, France; Largeau, C., Ecole Nationale Superieure de Chimie, France; Concepts and Approaches for Mars
Exploration; July 2000, Part 1, pp. 42-43; In English; See also 20010023036; No Copyright; Avail: CASI; A01, Hardcopy; A03,
Microfiche
On Earth, the molecules which participated in the emergence of life about 4 Ga ago have been erased by plate tectonics, the
permanent presence of running water, unshielded solar ultraviolet radiation and by oxygen produced by life. Since the environment
of the early Mars about 3.5-4 Ga ago was probably very close to that of the early Earth, life might have emerged on Mars
as well and might give us some insight into the prebiotic chemistry that took place on Earth about 4 Ga ago. Furthermore, there
is a possibility that life still exists on Mars, protected from the harsh environment in some specific locales. In order to search for
life on Mars, one should look for potential biogenic markers such as organic matter and inorganic signatures (microfossils, biominerals,
biogenic etching, isotopic fingerprints...) which have different degrees of resistance to the Martian environment. As biomarkers
could be organic or inorganic in nature, complete organic and mineral analyses should therefore be conducted in parallel
on the same sets of samples, going from the least destructive to the most destructive technique of micro-analysis. Furthermore,
in situ analyses should be complemented by high precision and high sensitivity laboratory measurements of returned Martian samples.
Due to the very oxidized Martian environment, organic molecules should be searched for in protected sites, either surface
boulders or near sub-surface, in layers deep enough for avoiding the oxidizing effect of the atmosphere. Molecules that should
be looked for include low and high molecular weight organics (like alkanoic acids, peroxiacids, PAHs and amino acids, respectively),
and macromolecular com-pounds like kerogens or kerogen-like materials. Previous in situ analyses were performed using
pyrolysis systems which allow to detect organic compounds but do not always permit the identification of individual molecules.
New possible analytical solutions could include gas chromatography-based techniques coupled with a mass spectrometer using
multi GC columns systems, including columns able to separate enantiomers, chemical derivatization cells (using new derivatization
schemes in particular for amino acid analysis), high performance liquid chromatography and supercritical fluid chromatography.
Derived from text
Mars Surface Samples; Organic Materials; Gas Chromatography; Mass Spectrometers
20010023065 NASA Ames Research Center, Moffett Field, CA USA
Mars Exploration 2003 to 2013: An Integrated Perspective
Briggs, G., NASA Ames Research Center, USA; McKay, C., NASA Ames Research Center, USA; Concepts and Approaches for
Mars Exploration; July 2000, Part 1, pp. 45; In English; See also 20010023036; No Copyright; Abstract Only; Available from
CASI only as part of the entire parent document
The science goals for the Mars exploration program, together with the HEDS precursor environmental and technology needs,
have been carefully laid out over the last several years and serve as a solid starting point for re-planning the program in an orderly
way. Most recently, the science and HEDS communities have recognized the significance of subsurface sampling as a key component
in ”following the water”: 1) to achieve science goals related to the search for evidence of life and 2) to gain access to the most
valuable resource -- water. Accessing samples from hundreds and even thousands of meters beneath the surface is a challenge that
will call for technology development and for one or more demonstration missions. Recent mission failures and concerns about
the complexity of the previously planned MSR missions indicate that, before we are ready to undertake sample return and deep
sampling, the Mars exploration program needs to include 1) technology development missions and 2) basic landing site assessment
missions. These precursor missions should demonstrate the capability for reliable & accurate soft landing and in situ propellant
production. The precursor missions will need to carry out close-up site observations, ground-penetrating radar mapping from
orbit and conduct seismic surveys. The needs of the science and HEDS program requirements have much in common and clearly
the programs should be planned as a single, continuous exploration effort. (We note that, although we are not yet ready to carry
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