(2) LATMOS-IPSL, Verrières-le-Buisson, France

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1 (2) LATMOS-IPSL, Verrières-le-Buisson, France
Photochimie en orbite : Amino/UVolution/Process – 1/6 H. Cottin (1), P. Coll (1), M. Cloix (1), D. Coscia (2), N. Fray (1), Y.Y. Guan (1), F. Macari (1), F. Raulin (1), F. Stalport (1), C. Szopa (2), D. Chaput (3), M. Viso (3), M. Bertrand (4), A. Chabin (4), F. Westall (4), A. Brack (4), J. Vergne (5), M.C. Maurel (5) (1) LISA, Université Paris 7 & Paris 12, UMR 7583 CNRS, Créteil, France (2) LATMOS-IPSL, Verrières-le-Buisson, France (3) CNES, France (4) CBM, CNRS, Orléans, France, (5) Anbiophy, UPMC, Paris, France

2 Photochimie en orbite : Amino/UVolution/Process – 2/6
First order decay t1/2 = ln 2 / J Photochimie en orbite : Amino/UVolution/Process – 2/6 absorption cross section (cm²) photons flux (photon.cm-2.s-1) Solar or lab. photolysis quantum yield

3 Photochimie en orbite : Amino/UVolution/Process – 3/6

4 PROCESS, AMINO : International Space Station
PROCESS – Expose-E (Columbus) : Fev – August 2009 AMINO - Expose-R (Zvezda) : Mars 2009 – Sept. 2010 UV-olution : FOTON-3M / BIOPAN 6 September 14-26, 2007 BIOPAN (FOTON) EXPOSE (ISS)

5 Stability of organic molecules at Mars surface
Photochimie en orbite : Amino/UVolution/Process – 5/6 Cycle of organic matter in Titan Origin of the distributed sources Exogenous delivery Stability of organic molecules at Mars surface ARN stability

6 Photochimie en orbite : Amino/UVolution/Process – 6/6
2010 : Analyse des échantillons PROCESS Retour des échantillons AMINO Réponse à l’AO ESA ILSRA 2009 Projet PSS : Photochemistry on the Space Station (LISA, LATMOS, CBM, Obs. Catania, Obs. Leiden, Nasa Ames) Projet VITRINE (LISA, LATMOS, CBM, IAS, PIIM, ECP, LERMA, Obs. Catania, Obs. Leiden, Nasa Ames) : suivi in situ en orbite et extension à basse température R&T CNES sur VITRINE

7 Conception of a very high mass resolution mass spectrometer
Exploration in situ : prospective ILMA (astéroïde) – 1/6 ILMA: Ion Laser Mass Analyser, in-situ analysis of a carbonaceous asteroid for the MARCO POLO spatial mission. Conception of a very high mass resolution mass spectrometer H. Cottin(1), J.J. Berthelier (6), A. Bouabdellah (6), C. Briois(2), N. Carrasco(6), P. Gilbert (6), C. Engrand(3), N. Grand(1), P. Zapf (1), M. Hilchenbach(7), H. Krüger(7), A. Makarov(8), P. Puget(5), B. Arezki (5), C. Szopa(6), L. Thirkell(2), A. Boukrara(2), and R. Thissen(4) (1) LISA, Universités Paris 12, Paris 7, UMR 7583 CNRS, Créteil cedex, (2) LPC2E - UMR-CNRS 6115 , Orléans, France, (3) CSNSM,  ORSAY Campus, France, (4) LPG, UMR 5109 CNRS - UJF, Grenoble, France, (5) LAOG, CNRS, Université Joseph Fourier, UMR 5571, BP 53, F Grenoble, France, (6) LATMOS, CNRS, UVSQ, UPMC, Verrières le  Buisson Cedex, France, (7) MPI für  Sonnensystemforschung,, D Katlenburg-Lindau, Germany, (8)Thermo Fisher Scientific, Hanna-Kunath Str 11, Bremen, Germany

8 Thanks to the high resolution
Exploration in situ : prospective ILMA (astéroïde) – 2/6 TECHNICAL REQUIREMENTS Mass: ~ 2.2 kg (with 20% margin) Volume: x15x5 cm3 Electronic unit : x10x3 cm3 Mean power: ~ 9 W Mass range: / amu Mass resolution: ,000 at 50% height at 400 amu Analyzed area: a few µm² to 1 mm² Data budget : 40 Mo per analysis (at least 2 analysis per sample). Thanks to the high resolution Analysis of Minerals & Organics Desorbed Ions Vacuum Solid Collision cascade Region of greatest damage Region of least damage LDIMS Process Laser shot

9 Exploration in situ : prospective ILMA (astéroïde) – 3/6
First publication Makarov, Anal Chem (2000)

10 Example : mixture of complex high molecular weight organic compounds
Exploration in situ : prospective ILMA (astéroïde) – 4/6 m/Dm = m/Dm = m/Dm = 3000 Example : mixture of complex high molecular weight organic compounds m/z = 262

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