Cambridge University Press, UK. Lahav, N., White, D., and Chang, S. (1978). Peptide formation in the prebiotic era: thermal condensation of glycine

in fluctuating clay environments. Science, 201: 67–69. Ponnamperuma, C., Shimoyama, A., and Friebele, E. (1982). Clay and the origin of life. Orig. Life OICR-9429 nmr Evol. Biosph., 12: 9–40. E-mail: pdalai@uni-hohenheim.​de V.U.V. Irradiation of Interstellar Ice Analogs: A Potential Source for Prebiotic Molecules in Planetary Systems G. Danger1, P. de Marcellus1, Z. Djouadi1, J.B. Bossa2, T. Chiavassa2, L.d’Hendecourt1* 1 Astrochimie et Origines, Institut d’Astrophysique Spatiale, Orsay, France. 2Spectromatries et Dynamique Moléculaire, Physique des Interactions Ioniques et Moléculaires, Université de Provence, Marseille, France The study of astrophysical chemistry is an important task to understand matter evolutions in the Universe and notably evolution pathways from abiotic chemistry

in the interstellar medium (MIS) to prebiotic chemistry in planetary systems. In the dense interstellar medium, the major part of light elements (O,C,N) is adsorbed on interstellar grains. From a schematic point of view, these grains are formed with different layers which included ices of volatile compounds which surround residue of refractory carbon and a nucleus consisting of silicate compounds. The physical and chemical evolution Selleck AZD2281 of these grains is followed by parent body’s aggregation, the first step towards planetary formation. From experimental simulations of astrophysical environments in the laboratory, and particularly conditions see more of molecular ices formation, our aim is to understand the chemical evolution of these ices in order to retrace the chemical evolution toward complex molecule formation in the ISM (e.g. pathways for amino acid synthesis or their precursors). The first results obtained after ice analogs (e.g.

including H2O, CO, NH3, CH3OH…) irradiation have shown the formation of radicals and more complex molecules by infrared in situ analysis. The first step is thus to compare these data with astronomical observations in order to identify the importance of photochemical processes in astrophysical environments. After sample heating, radicals and molecules can rearrange to form a residue which includes complex organic molecules such as amino acids, detected after hydrolysis treatment of the samples (Bernstein et al., 2002; Muñoz-Caro et al., 2002; Nuevo et al., 2008). Without this treatment only very few amounts of amino acids are detected (Nuevo et al., 2008). This observation leads to the hypothesis that amino acids could be included in a complex structure which, after degradation, releases them during hydrolysis. Another possibility is that amino acids could come from precursors such as nitriles (Elesila et al, 2007). The last hypothesis is corroborated by the recent this website aminoacetonitrile detection in the ISM gas phase (Belloche et al., 2008).