Since the emergence of Exobiology, back to the 1960ties, this field drastically increased and, although differently named, is today a largely recognized scientific domain of wild interdisciplinarity. It includes not only the search for extraterrestrial living systems, in particular by direct exploration of planetary bodies and studies of extraterrestrial materials, but also the study on the origins of life on Earth and, in connection to this field, the study of extraterrestrial organic chemistry. The exobiology programmes currently developed at LISA are related to this last aspect. They include the study of prebiotic-like chemistry in the gas and solid phases, based on laboratory simulation experiments, theoretical modeling and future in situ measurements in Titan's atmosphere and in cometary nuclei. A national program of exobiology, coordinated by LISA is under development in France, it covers many of the various aspects of Exobiology, including the study of life in extreme environments, as a reference tool for extraterrestrial life, the study of the primitive environment of the Earth, of the organic chemistry in comets and on Titan, of Mars and Europa and even of extrasolar planets as potential niches for extraterrestrial living systems, associated to the determination of the electromagnetic signatures of life. In parallel to this general program, a proposal for a large simulation chamber to be used as a national facility in particular to simulate the organic chemistry in various planetary environments, and in the interstellar medium, is under preparation. International cooperations linked to these programmes, in particular in the frame of the development of an exobiology facility on the International Space Station, would be of crucial interest

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The crucial organic molecules associated with life are chiral. β irradiation on the causal origin for the great preference of biomolecules in life over their corresponding enantiomers has been extensively studied. The left helical β electrons, with spin and momentum antiparallel, should propagate with different velocities in the two enantiomers. Much effort has been done to investigate possible mechanism of inducing asymmetry, using longitudinally polarized β rays to decompose asymmetrically racemic mixtures of biomolecules, but the results were inconclusive and contradictory. In this paper we present our viewpoint that the direct inelastic scattering between polarized electrons and chiral molecules is the dominant one in producing the asymmetry of cross sections for both &beta⁺ and β^- irradiation. The inelastic cross section σ- (0 → n) is dependant on the dipole strength Dn, rotatory strength Rn of the molecule. According to the theoretical study, the asymmetry of cross section F is ∼ 10^-6 and it depends on the sign of Rn⁺(L type). When Rn⁺> 0, σ_D> σ_L, it favors L-amino acid surviving . When Rn⁺< 0, σ_D< σ_L, it favours D-amino acid surviving. Our results show that helical electrons do distinguish between molecules of opposite chirality, and the disputation and suspicion about the controversial experimental results between Garay¹ and Darge &Thiemann²can be explained.

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The atmosphere of Titan is constantly bombarded by galactic cosmic rays and Saturnian magnetospheric electrons causing the formation of free electrons and primary ions, which are then stabilized by ion cluster formation and charging of aerosols. These charged particles accumulate in drops in cloud regions of the troposphere. Their abundance can substantially increase by friction, fragmentation or collisions during convective activity. Charge separation occurs with help of convection and gravitational settling leading to development of electric fields within the cloud and between the cloud and the ground. Neutralization of these charged particles leads to corona discharges which are characterized by low current densities. We have therefore, experimentally studied the corona discharge of a simulated Titan's atmosphere (10% methane and 2% argon in nitrogen) at 500 Torr and 298 K by GC-FTIR-MS techniques. The main products have been identified as hydrocarbons (ethane, ethyne, ethene, propane, propene+propyne, cyclopropane, butane, 2-methylpropane, 2-methylpropene, n-butane, 2-butene, 2,2-dimethylpropane, 2-methylbutane, 2-methylbutene, n-pentane, 2,2-dimethylbutane, 2-methylpentane, 3-methylpentane, n-hexane, 2,2-dimethylhexane, 2,2-dimethylpentane, 2,2,3-trimethylbutane, 2,3-dimethylpentane and n-heptane), nitriles (hydrogen cyanide, cyanogen, ethanenitrile, propanenitrile, 2-methylpropanenitrile and butanenitrile) and a highly branched hydrocarbon deposit. We present the trends of hydrocarbons and nitriles formation as a function of discharge time in an ample interval and have derived their initial yields of formation. The results clearly demonstrate that a complex organic chemistry can be initiated by corona processes in the lower atmosphere. Although photochemistry and charged particle chemistry occurring in the stratosphere can account for many of the observed hydrocarbon species in Titan, the predicted abundance of ethene is too low by a factor of 10 to 40. While some ethene will be produced by charged-particle chemistry, the production of ethene by corona processes and its subsequent diffusion into the stratosphere appears to be an adequate source. Because little UV penetrates to the lower atmosphere to destroy the molecules formed there, the corona-produced species may be long-lived and contribute significantly to the composition of the lower atmosphere and surface.

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A large collection of micrometeorites has been recently extracted from Antarctic old blue ice. In the 50 to 100μm size range, the carbonaceous micrometeorites represent 80 % of the samples and contain 2 % of carbon. They might have brought more carbon to the surface of the primitive Earth than that involved in the present surficial biomass. Amino acids such as “-amino isobutyric acid have been identified in these Antarctic micrometeorites. Enantiomeric excesses of L-amino acids have been detected in the Murchison meteorite. A large fraction of homochiral amino acids might have been delivered to the primitive Earth via meteorites and micrometeorites. Space technology in Earth orbit offers a unique opportunity to study the behaviour of amino acids required for the development of primitive life when they are exposed to space conditions, either free or associated with tiny mineral grains mimicking the micrometeorites. Our objectives are to demonstrate that porous mineral material protects amino acids in space from photolysis and racemization (the conversion of L-amino acids into a mixture of L- and D-molecules) and to test whether photosensitive amino acids derivatives can polymerize in mineral grains under space conditions. The results obtained in BIOPAN-1 and BIOPAN-2 exposure experiments on board unmanned satellite FOTON are presented.

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A scheme is presented for an analog investigation of long term irradiation of ices and organics following the cyclic evolution of interstellar dust. The irradiation is proposed to be performed at cryogenic temperatures on a space platform, and with an enhancement of the solar ultraviolet flux using a concave mirror, grating combination which eliminates the visual and infrared from the sample surface.

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Simulation experiments on ground have shown that “amino acid precursors”, which give amino acids after acid-hydrolysis, can be formed when an ice mixture simulating ice mantles of interstellar dust particles (ISDs) is irradiated with high energy particles or UV light. It is strongly suggested that such bioorganic compounds were delivered by comets for the first biosphere on the Earth. It is of great interest to confirme this hypothesis in actual space conditions, such as in an exposed facility of JEM. Fundamental designs for such exobiology experiments in earth orbit (EEEO) will be discussed.

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A conceptual design was developed for a cosmo-biology experiment. It is intended to expose simulated interstellar ice materials deposited on dust grains to the space environment. The experimental system consists of a cryogenic system to keep solidified gas sample, and an optical device to select and amplify the ultraviolet part of the solar light for irradiation. By this approach, the long lasting chemical evolution of icy species could be examined in a much shorter time of exposure by amplification of light intensity. The removal of light at longer wavelength, which is ineffective to induce photochemical reactions, reduces the heat load to the cryogenic system that holds solidified reactants including CO as a constituent species of interstellar materials. Other major hardware components were also defined in order to achieve the scientific objectives of this experiment. Those are a cold trap maintained at liquid nitrogen temperature to prevent the contamination of the sample during the exposure, a mechanism to exchange multiple samples, and a system to perform bake-out of the sample exposure chamber. This experiment system is proposed as a candidate payload implemented on the exposed facility of Japanese Experiment Module on International Space Station.

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Ecological cultivation capsules (ECC), that is a materially sealed microcosm, composed of primary producers, consumers and bacteria as a decomposer were developed in order to cultivate bacteria without any artificial operation for long duration more than 10 years in space. It is planned to be left on the space station to study the process that bacteria in MIR space station had acquired their resistance to cosmic ray radiation as well as ultra-violet light. As contrasted with the space experiment, bacteria are cultivating in the ECC on the ground to trace the changes of bacteria under the simulated radiation dose in Earth orbit.

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A materially-closed aquatic ecosystem (microcosm) was developed. The microcosm contained two families of green algae and blue-green alga as primary producers, protozoa, two species of rotifers and oligochaetes as consumers, and bacteria as decomposers. The microcosm could be readily replicated. It was confirmed the population densities of each organism were almost constant for 365 days without artificial operation except temperature and light. The population dynamics and the spatial patterns of the organisms were simulated by mathematical models. This hermetically-sealed microcosm could be a useful subject to investigate ecology under space environment.

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A multi-user integrated suite of instruments designed to optimize the search for evidence of life on Mars is described. The package includes: - Surface inspection and surface environment analysis to identify the potential Mars landing sites, to inspect the surface geology and mineralogy, to search for visible surficial microbial macrofossils, to study the surface radiation budget and surface oxidation processes, to search for niches for extant life. - Subsurface sample acquisition by core drilling- Analysis of surface and subsurface minerals and organics to characterize the surface mineralogy, to analyse the surface and subsurface oxidants, to analyse the mineralogy of subsurface aliquots, to analyse the organics present in the subsurface aliquots (elemental and molecular composition, isotopes, chirality). - Macroscopic and microscopic inspection of subsurface aliquots to search for life's indicators (paleontological, biological, mineralogical) and to characterize the mineralogy of the subsurface aliquots. The study is led by ESA Manned Spaceflight and Microgravity Directorate.

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Liquid water, underwater volcanoes and possibly life forms have been suggested to be present beneath the estimated 10 km-thick ice shell of Europa, the Jovian satellite J2. Europa's possible ocean is estimated to be 100-200 km deep. Despite the great depth of the Europa's ocean, hydrostatic pressure at the seafloor would be 130-260 MPa, corresponding to 13-26 km depth of a theoretical Earth's ocean. The hydrostatic pressure is not beyond the edge of existing deep-sea technology. Here we propose exploration of Europa's deep-sea by the use of current technologies, taking a symbolic example of a deep submergence vehicle Shinkai 6500 which dives to a depth of 6.5 km deep (50 km depth of Europa's ocean). Shinkai 6500 is embarkable in the payload bay of the Space Shuttles in terms of size and weight for the transportation to a Low Earth Orbit (LEO). Secondary boost is needed for interplanetary flight from the LEO.On-orbit assembly of the secondary booster is a technological challenge. The International Space Station (ISS) and ISS-related technologies will facilitate the secondary boost. Also, ice shell drilling is a challenge and is needed before the dive into Europa's ocean. These challenges should be overcome during a certain leading time for matured experience in the ISS operation.

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It has been eagerly requested to develop a highly-sensitive method to characterize extremely minute amounts of natural organic materials occluded in meteorites and/or space dusts in order to confirm the existence of life in the extraterrestrial space. In this article, the reactive pyrolysis-gas chromatography (Py-GC) applied to the analysis of the lipid components contained in every zooplankter individual is introduced for the sake of its potential extension to the characterization of trace amounts of the extraterrestrial organic materials. Here, Py-GC was applied to 1) the discriminative analysis among zooplankter individuals cultured in different food concentrations, and 2) the correlation analysis between the distributions of fatty acid components in the lipids of zooplankter individuals and ingested algae phytoplankton.

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