http://www.astrobiologia.pl/eana/

15 – 17 October 2012, AlbaNova University Center, Stockholm(EANA 2012)

Book of Abstracts

12th European Workshop on Astrobiology

2

Local Organizing Committee:

Engy Ahmed (Geological Sciences) <engy.ahmed@geo.su.se>

Clarisse Balland-Bolou-Bi (Geological Sciences) <ClarisseBolou-Bi@geo.su.se>

Axel Brandenburg (Nordita) <brandenb@nordita.org>

Gianni Cataldi (Astronomy) <gianni.cataldi@astro.su.se>

Chi-kwan Chan (Nordita) <ckch@nordita.org>

Pantea Fathi (Molecular Physics) <pantea.fathi@fysik.su.se>

Wolf Dietrich Geppert (Molecular Physics) <wgeppert@fysik.su.se>

Nils Holm (Geological Sciences) <nils.holm@geo.su.se>

Enrique Iniguez Pacheco (Geological Sciences) <enrique.iniguez@geo.su.se>

Hans Muhlen (Nordita) <hvzm@physto.se>

Anna Neubeck (Geological Sciences) <anna.neubeck@geo.su.se>

Britt-Marie Sjoberg (Molecular Biology) <bitte@molbio.su.se>

Fabio Del Sordo (Nordita) <fabio@nordita.org>

Elizabeth Yang (Nordita) <eyang@kth.se>

Scientific Organizing Committee:

Ricardo Amils (CAB, Madrid) <ricardo.amils@uam.es>

Andre Brack (CNRS, Paris) <brack@cnrs-orleans.fr>

Axel Brandenburg (Nordita, Stockholm) <brandenb@nordita.org>

John Brucato (INAF, Firenze) <jbrucato@arcetri.astro.it>

Charles Cockell (Edinburgh Univ.) <c.s.cockell@ed.ac.uk>

Pascale Ehrenfreund (Leiden Univ.) <p.ehrenfreund@chem.leidenuniv.nl>

Natalia Gontareva (Russian Academy of Sciences, St. Petersburg) <ngontar@mail.cytspb.rssi.ru>

John Lee Grenfell (DLR, Berlin) <Lee.Grenfell@dlr.de>

Nils Holm (Stockholm Univ.) <nils.holm@geo.su.se>

Gerda Horneck (DLR, Cologne) <Gerda.Horneck@dlr.de>

Helmut Lammer (IWF, Graz) <helmut.lammer@oeaw.ac.at>

Kirsi Lehto (Turku Univ.) <klehto@utu.fi>

Steen Rasmussen (Univ. Southern Denmark, Odense) <steen@ifk.sdu.dk>

Francois Raulin (CNRS, Paris) <francois.raulin@lisa.u-pec.fr>

Petra Rettberg (DLR, Cologne) <petra.rettberg@dlr.de>

Ewa Szuszkiewicz (Szczecin Univ.) <szusz@fermi.fiz.univ.szczecin.pl>

Frances Westall (CNRS, Paris) <westall@cnrs-orleans.fr>

Message from the EANA president

Dear participants:

Welcome to the 12th European Workshop on Astrobiology “EANA’12”. I heartily welcome two new associated non-European members to EANA:

- The Mexican Society of Astrobiology: SOMA, and - University of São Paulo (USP) Research Unit in Astrobiology (NAP-Astrobio).

With great sadness I announce that our member of the Executive Committee of EANA, David Gilichinsky, Head of the Geocryology Laboratory, Institute of Physico-chemical and Biological Problems of Soil Science, Russian Academy of Sciences, Pushchino, Russia, passed away on February 17, 2012. David was a great pioneer in permafrost ecology, an enthusiastic Mars explorer and an excellent organizer of our 10th European Workshop on Astrobiology in September 2010 in Pushchino. The abstracts of EANA’10 are published in Paleontological Journal, 2012, Vol. 46, No. 9, pp. 1–38, with David a guest editor. “See you on Mars” he wrote in his introduction.

The last years have bestowed us with 2 successful astrobiology missions on the International Space Station: The results of EXPOSE-E have been published in a special issue of Astrobiology (vol. 12, no. 5, May 2012) and those of EXPOSE-R are foreseen for a special issue of the Intern. J. Astrobiol. The follow-on mission EXPOSE-R2 will be launched in 2013. Selected papers of EANA’11 were published in a Special Issue of Origins Life Evol. Biosph. (vol. 42, no. 2–3, June 2012)

This month, the 4th series of our Astrobiology lecture course Network (ABC-Net) have started, a real time tele-teaching combining 9 European universities, which include ABC-Net as part of their university lecture plan and the ECTS-system. ABC-Net is jointly organized by EANA and ESA, with Francois Raulin (EANA) as scientific organizer and Nigel Savage (ESA) providing the technical management. The lectures – as well as those of previous series – are available on the ESA web: http://wsn.spaceflight.esa.int/?pg=page&id=11

EANA’12 is hosted by NORDITA (the Nordic Institute for Theoretical Physics) and the Swedish Astrobiology Network (SwAN), which is gratefully acknowledged. EANA’12 is sponsored by Stockholm University, KTH Royal Institute of Technology, the Swedish Research Council, the Swedish National Space Board, the Wenner-Gren Foundations, the City of Stockholm and ESA. Their support made it possible to provide travel grants to 28 students and young scientists from 12 countries for attending EANA’12.

I hope that you will enjoy EANA’12 that reflects the facets of astrobiology in Europe.

Gerda Horneck

President of EANA

European Astrobiology Network Association

The European Astrobiology Network Association (EANA) was created in 2001 with the purpose to bring together European researchers interested in astrobiology programs and to foster their cooperation; to attract young scientists to this interdisciplinary field of research; and to popularize astrobiology to the public and to students. The EANA website is: http://www.astrobiologia.pl/eana/EANA now combines representatives of 19 European nations active in astrobiology: Austria, Belgium, Czech Republic, Denmark, Finland, France, Germany, Greece, Hungary, Italy, Poland, Portugal, Romania, Russia, Spain, Sweden, Switzerland, The Netherlands, United Kingdom, and organizes annual workshops in one of the member countries. Astrobiology groups in Brazil, China, Japan, Mexico and USA are associated members. EANA is sponsored by the European Space Agency. The EANA Executive Council has a total of 36 members, of which 19 are national representatives and 17 are elected members. EANA Executive Council (2010-2013)President: Gerda HorneckHonorary President: André BrackVice-Presidents: Charles Cockell, Pascale Ehrenfreund, Juan Perez-MercaderSecretary: Helmut Lammer, Nigel MasonTreasurer: Beda HofmannNational representatives: Elected members:AT: Helmut Lammer Amils, Ricardo BE: Christian Muller Cottin Hervé CH: Beda Hofmann De la Torre, RosaCZ: Jan Jelička Direito, SusanaDE: Gerda Horneck Gilichinsky, David (†)DK: David Field Holm, NilsES: Juan Perez Mercader Javaux, EmmanuelleFI: Harry Lehto Jehlička, JanFR: François Raulin Josset Jean-LucGR: Elias Chatzitheodoridis Kobayashi KenseiHU: Györgyi Ronto Lehto, KirsiI :Cristiano Cosmovici Mason, NigelNL: Pascale Ehrenfreund Rettberg, PetraPL: Ewa Szuszkiewicz Schwartz, AlanPT: Maria Webb Stan-Lotter, HelgaRO: Marius-Ioan Piso Vago JorgeRU: Anatoli Pavlov Westall, FrancesSE: Axel BrandenburgUK: Charles Cockell

European Astrobiology Network Association

Welcome  to  Nordita  in  Stockholm   Nordita  is  the  Nordic  Institute  for  Theoretical  Physics,  and  its  purpose  is  to  carry  out  research  and  strengthen  the  Nordic  collaboration  within  the  basic  areas  of  theoretical  physics.    

 

Nordita  was  founded  as  the  Nordic  Institute  for  Theoretical  Atomic  Physics  in  Copenhagen,  Denmark  in  1957,  under  the  ownership  of  the  Nordic  Council  of  Ministers  and  located  at  the  premises  of  the  Niels  Bohr  Institute.  

After  the  move  to  Stockholm,  Sweden  in  2007,  Nordita  is  hosted  jointly  by  the  Royal  Institute  of  Technology  (KTH)  and  Stockholm  Uni–versity.  Nordita  is  located  at  the  AlbaNova  University  Center,  north  of  Stockholm  city.    

 

Nordita  is  located  in  two  of  the  yellow  houses  in  front  of  the  main  AlbaNova  building,  with  the  address  Roslagstullsbacken  23  (Nordita  main  building)  and  Roslagstullsbacken  17.    Nordita  events  are  usually  held  in  the  main  building.  

 

For  instructions  on  how  to  get  to  Nordita,  see  below,  or  visit  our  website  at:  

www.nordita.org/map  

   

 

 You  can  find  more  information  that  can  help  you  during  your  stay  at  Nordita  on  the  web  page  

 

www.nordita.org/guests    

Tips  on  Activities  in  Stockholm  

As  a  visitor  in  Sweden  you  can  find  lots  of  useful  information  about  cultural  events,  museums,  restaurants,  emergency  numbers  and  etc.  in  the  booklet  “What’s  On".    

Another  useful  resource  is  the  official  Stockholm  Visitors  Guide  at  www.visitstockholm.com/en.  

Taxi  

Taking  a  taxi  from  Arlanda  to  anywhere  in  central  Stockholm  will  cost  approximately  450-­‐500  SEK.  Make  sure  to  ask  for  the  fixed  Arlanda-­‐Stockholm  price!  Taking  a  taxi  anywhere  within  the  central  Stockholm  will  cost  approximately  150  SEK.  Taxis  accept  all  major  credit  cards.    

These  are  the  taxi  companies  we  recommend:    Taxi  Stockholm:  +46  8  15  00  00    Taxi  020:  +46  20  20  20  20  TaxiKurir:  +46  8  30  00  00  TopCab  +46  8  33  33  33  Stockholm  Transfer  +46  20  35  00  00  

Buses  and  Subway    

On  the  web  site  sl.se/en/Visitor  you  can  find  information  about  public  local  transportation,  such  as  tickets,  prices,  timetables  and  etc.  

You  can  buy  tickets  for  bus  and  subway  in  all  convenience  stores  called  "Pressbyrån"  which  are  usually  located  in  or  near  subway  stations.    

Notice  that  if  you  want  to  take  a  bus  you  have  to  buy  your  ticket  in  advance  since  the  buses  do  not  sell  tickets.  If  you  come  from  the  subway,  that  ticket  can  be  used  for  transfer.    

The  closest  subway  station  to  Nordita  is  "Tekniska  högskolan",  on  the  red  subway  line  towards  "Mörby  centrum".  Take  the  exit  "Körsbärsvägen",  and  the  staircase  to  your  right  after  the  entrance.    

From  here  to  Nordita  it  is  a  10-­‐15  minutes  of  walk  (see  the  directions  on  the  map).  When  you  come  up  to  the  street  level  from  the  sub–way,  you  will  have  the  main  street  Valhalla–vägen  on  your  left  side.  Follow  that  street  and  continue  slightly  downhill  until  you  reach  a  hot-­‐dog  stand  “Tullfritt”,  at  the  bottom  of  a  steep  street  Roslagstullsbacken.  Nordita  is  at  the  top  of  that  street,  across  the  roundabout.    

 Instead  of  walking,  you  can  take  the  buses  43  or  44  just  outside  the  subway  exit  (50  m  ahead,  along  the  sidewalk)  to  the  end  desti–nation  "Ruddammen".    

 

Dear  Participants,  

My  name  is  Elizabeth  Yang  and  I  am  responsible  for  visitor  arrangements  here  at  Nordita  together  with  the  event  organizers.  

If  you  have  any  questions,  please  feel  free  to  contact  me  and  I  would  be  glad  to  assist  you.  

My  phone  number  is  +46  8  5537  8754  and  my    e-­mail  is  eyang@kth.se.  

I  am  looking  forward  to  seeing  you  and  wish  you  a  pleasant  stay  at  Nordita!  

 

Yours  Sincerely,  

 Elizabeth  Yang  

Scienticfic  Program  Coordinator,  Economic  Officer  

 

 

12th European Workshop on Astrobiology EANA’12

AlbaNova, StockholmOctober 15-17, 2012

Date: 14 October 201217:00 - 20:00 Registration, with wine & cheese

Date: 15 October 2012

08:00 Registration

Opening Session09:30 Welcome

Vice-Rector of Stockholm University Anders KarlhedeDirector of AlbaNova Mats LarssonDirector of Nordita Larus Thorlacius President of EANA Gerda HorneckChair of Organizing Committee Axel BrandenburgWorkshop begin with music Gunnar Julin & Co.

10:30 Break.

Session 1: Extrasolar planets / AstrophysicsCo-Chair: René LiseauCo-Chair: Pascale EhrenfreundNo. Time

O1.1 11:00 Yamila Miguel, Lisa Kaltenegger:Exploring super-Earth atmospheres

O1.2 11:15 Ewa Szuszkiewicz, John C.B. Papaloizou, Edyta Podlewska-Gaca:Reversing the inward migration of super-Earths

O1.3 11:30 Jack O'Malley-James, John Raven, Charles Cockell, Jane Greaves:Life & Light: Exotic photosynthesis in binary and multiple star systems

O1.4 11:45 Jordi Gutiérrez:Metallicity effects on the extension of the stellar habitable zone

O1.5 12:00 Vassilissa Vinogradoff, Fabrice Duvernay, Albert Rimola, Gregoire Danger, Patrice Theulé, Fabien Borget, Jean-Claude Guillemin, Thierry Chiavassa:Specific chemistry in interstellar ice: Reactivity of formaldehyde

O1.6 12:15 Claudio Maccone:A mathematical model for SETI, evolution and human history

12:30 Lunch break

Session 2: Planetary Habitability Co-Chair: Rosa de la TorreCo-Chair: Helmut LammerNo. Time

O2.1 14:00 Jean-Pierre de Vera, Ernst Hauber, Nicole Schmitz, Ulrich Szewzyk:Habitability and exploration of Mars: A scientific and engineering evaluation concept of Antarctic and Arctic field sites as geo-biological analogues for the surface of Mars

O2.2 14:15 Pascale Ehrenfreund, Antonella Barucci, Patrick Michel, Hermann Böhnhardt, John R. Brucato, Elisabetta Dotto, Ian A. Franchi, Simon F. Green, Luisa-M. Lara, Bernard Marty, Detlef Koschny:MarcoPolo-R Asteroid Sample Return Mission: tracing origins

O2.3 14:30 Sean McMahon, John Parnell, Nigel Blamey:Analysis of volatiles in basalt, a possible source of Martian methane

O2.4 14:45 Fulvio Franchi, A. P. Rossi, M. Pondrelli, B. Cavalazzi, R. Barbieri:Ancient fluid escape and related features in the equatorial Arabia Terra (Mars)

O2.5 15:00 Nicolas Bost, Frances Westall, Marylène Bertrand, Barbara Cavalazzi, Frédéric Foucher:Martian exploration: Do not underestimate the volcanic rocks as a possible habitat

O2.6 15:15 Anatoliy Pavlov, Alexander A. Pavlov, Gennady Vasilyev, Valery Ostryakov, Maria A. Vdovina:Degradation of the "biomarkers" in the shallow subsurface of Mars due to irradiation by cosmic rays

15:30 Break

Session 3: Geochemical origin of lifeCo-Chair: Nils HolmCo-Chair: Anna NeubeckNo. TimeO3.1 16:00 William F. Martin:

Hydrogen, metals, electron bifurcation, and ion gradients: The early evolution of biological energy conservation

O3.2 16:15 Jean-François Lambert, Maguy Jaber, Thomas Georgelin, Houssein Bazzi:Formation of activated molecules by condensation on mineral surfaces: A contribution to prebioenergetics

O3.3 16:30 David E. Bryant, Barry Herschy, Richard Telford, Katie E. R. Marriott, Nichola E. Cosgrove, Karl Kaye, Matthew A. Pasek, Claire Cousins, Ian Crawford, Terence P. Kee:Pyrophosphite as a plausibly prebiotic energy currency molecule on the early earth

O3.4 16:45 Stefan Fox, Henry Strasdeit:Primordial island volcanoes as locations of prebiotic chemical evolution

O3.5 17:00 Axelle Hubert, Frances Westall, Claire Ramboz, Alexandre Simionovici, Laurence Lemelle, Barbara Cavalazzi:Investigating the geochemical composition of early life signatures and environment of deposition in highly silicified Archaean cherts - Analytical methods

O3.6 17:15 Kai Finster:Sulfur disproportionators as a model of a chemolithoautotrophic “LUCA”

17:30 Poster session20:00 WS Dinner at Pong Buffé on Drottninggatan 71C (city center; see map at end of booklet)

Date: 16 October 2012

Student contest (I)Co-Chair: Ralf MoellerCo-Chair: Oleg GusevJury: Nils Holm, Helmut Lammer, Natalia B. Gontareva, Kai FinsterNo. Time

SC 1 09:00 Siddharth Hegde, Lisa Kaltenegger:Colors of extreme exoEarth environments

SC 2 09:15 Jan Marie Andersen, Heidi Korhonen:M dwarfs as planet hosts: Consequences of stellar activity on exoplanet detection

SC 3 09:30 Aristodimos Vasileiadis, Åke Nordlund, Martin Bizzarro:Isotopic abundances in evolving, star-forming giant molecular clouds

SC 4 09:45 Arkadii V. Tarasevych, Jean-Claude Guillemin:Crystallization and sublimation of non-racemic mixtures of natural amino acids: A path towards homochirality

SC 5 10:00 Stefanie Lutz, Alexandre M. Anesio, Liane G. Benning:Cryo-life habitability on a polythermal glacier in Greenland

SC 6 10:15 Ebbe Norskov Bak, Svend Knak Jensen, Jon Merrison, Per Nørnberg, Kai Finster:Wind-driven erosion of silicates as a source of oxidants in Martian soil

10:30 Break

Student contest (II)No. time

SC 7 11:00 Gayathri Murukesan, Taina Laiho, Kirsi Lehto:Local Martian resources allow efficient cyanobacterial biomass and biohydrogen production

SC 8 11:15 Alfonso Delgado-Bonal, F.J. Martín-Torres, E. Simoncini:Accurate calculations of ozone and liquid water over Gale Crater

SC 9 11:30 Mickael Baqué, Daniela Billi, Jean-Pierre Paul de Vera:BIOMEX-desert cyanobacteria: Ground simulations of the EXPOSE-R2 mission

SC 10 11:45 Petra Schwendner, Simon Barczyk, Francesco Canganella, Viacheslav Ilyin, Reinhard Wirth, Harald Huber, Reinhard Rachel, Petra Rettberg:Monitoring of the microbial community during simulated flight to Mars

12:30 Lunch break

Session 4: Cryobiosphere, dedicated to David Gilichinsky Co-Chair: Charles CockellCo-Chair: Petra RettbergNo. Time

O4.1KN

14:00 Elizaveta Rivkina:Microbial life within Permafrost (In memory of David Gilichinsky)

O4.2 14:30 Sergey Bulat, Dominique Marie, Jean-Robert Petit:Assessing microbial life in extreme subglacial Lake Vostok, East Antarctica from accretion ice-lake water boundary samples

O4.3 14:45 Paloma Serrano, Antje Hermelink, Ute Boettger, Jean Pierre de Vera, Dirk Wagner:Methanogenic archaea from Siberian permafrost: survival in simulated Mars conditions and biosignature detection

O4.4 15:00 Lada Petrovskaya, Ksenia A. Novototskaya-Vlasova, Elizaveta M. Rivkina, Dmitry A. Dolgikh:Structure-functional study of "permafrost-adapted" proteins

O4.5 15:15 John Wettlaufer, Maya Bar-Dolev, Yeliz Celik, Peter L. Davies, Ido Braslavsky:Ice growth and melting modifications by antifreeze proteins

15:30 Break

Session 5: Homochirality Co-Chair: Steen RasmussenCo-Chair: Natalia GontarevaNo. Time

O5.1 16:00 Françoise Pauzat:Is it possible to enhance homochirality in space? A theoretical study of an enantio-selective adsorption process

O5.2 16:15 Axel Brandenburg, Alfio Bonanno, Fabio Del Sordo, Dhrubaditya Mitra:Spatial competition of opposing chiralities: Similarities between biochemical and magnetohydrodynamic processes

O5.3 16:30 Søren Toxvaerd:The role of carbohydrates at the origin of homochirality in biosystems

O5.4 16:45 Coryn Bailer-Jones, F. Feng:Assessing the influence of the solar Galactic orbit on terrestrial biodiversity variations

17:10 Departure to City hall (busses are waiting outside)18:00 City hall reception hosted by the City of Stockholm

Date: 17 October 2012

Session 6: Life’s evolution / Extremophiles

Co-Chair: Oleg GusevCo-Chair: Jana KviderovaNo. Time

O6.1 9:00 Lynn Rothschild, Kosuke Fujishima, Ivan Paulino Lima, Diana Gentry, Samson Phan, Jesica Navarette, Jesse Palmer, André Burnier:From extremophiles to Star Trek, the use of Synthetic Biology in Astrobiology

O6.2 9:30 Anthony Poole:Evaluating RNA world relics with comparative genomics

O6.3 9:45 John Parnell, Sean McMahon:Targeting the Deep Biosphere in the Search for Life

O6.4 10:00 Ricardo Amils, Víctor Parro, David Fernández-Remolar, José A. Manfredi, Kenneth Timmis, Monika Oggerin, Enoma Omoregie, Francisco J. López de Saro, Jose P. Fernández Rodríguez, Mónica Sánchez-Román, Carlos Briones Llorente, Felipe Gómez Gómez, Miriam García Villadangos, Nuria Rodríguez, David Gómez-Ortiz, José L. Sanz and the IPBSL Team:Iberian Pyrite Belt Subsurface Life (IPBSL), a drilling project of astrobiological interest

O6.5 10:15 Helga Stan-Lotter, Sergiu Fendrihan,Marion Dornmayr-Pfaffenhuemer, Friedrich W. Gerbl:Exposure to low water activity converts Halobacterium rods into small viable spheres - implications for microbial survival in ancient halite

10:30 Break

Session 7: Astrobiology on the ISSCo-Chair: Nigel MasonCo-Chair: Kensei Kobayashi

No. Time

O7.1 11:00 Kafila Saiagh, N. Fray, Y.Y. Guan, M. Cloix, D. Chaput, H. Cottin:Photostability of prebiotioc organic compounds from Low Earth Orbit experiments, ground laboratory photolysis, and from measurements of absorption vacuum UV (VUV) spectra

O7.2 11:15 Ralf Moeller, Petra Rettberg, Gerda Horneck, Günther Reitz, Wayne L. Nicholson:Bacillus subtilis spores in space: What can we learn from gene expression data?

O7.3 11:30 Yuko Kawaguchi, Yinjie Yang, Narutoshi Kawashiri, Keisuke Shiraishi, Yasuyuki Simizu, Tomohiro Sugino, Yuta Takahashi, Yoshiaki Tanigawa, Issay Narumi, Katsuya Satoh, Hirofumi Hashimoto, Satoshi Yoshida, Kensei Kobayashi, Kazumichi Nakagawa, Shin-ichi Yokobori, Akihiko Yamagishi and theTanpopo WG:Resistance of Deinococcus sp. to environmental factors of International Space Station (ISS) orbit - Microbes exposure experiment at ISS in the mission “Tanpopo”

O7.4 11:45 Daniela Billi, Mickael Baqué, Giuliano Scalzi, Elke Rabbow, Petra Rettberg:BOSS-Cyanobacteria: Subcellular integrities of Chroococcidiopsis biofilms after space and Martian simulations

O7.5 12:00 Michel Viso, Hervé Cottin, Pascale Chazalnoel, Michel Villenave, Didier Chaput:VITRINE: A new orbital facility for Astrobiology, Astrochemistry and Planetology

O7.6 12:15 Gerda Horneck:Forty years of astrobiology experimentation in space

12:30 Lunch break

14:00 Panel: Pan-European Projects related to astrobiologyCo-Chair: Axel BrandenburgCo-Chair: Gerda HorneckNo.

PA.1 Felipe Gómez, Nicolas Walter, Gerda Horneck, Christian Muller, Petra Rettberg, Maria T. Capria:AstRoMap, Astrobiology and Space Missions Road Mapping, a FP7 project

PA.2 Nigel Mason:The Chemical Cosmos, Understanding Chemistry in Astronomical Environments, a COST project

PA.3 Helmut Lammer:EuroPlanet, European Planetology Network, a FP7 project

PA.4 Jean-Pierre Bibring:From Mars Express to ExoMars: ESA contribution to Mars astrobiological exploration

PA.5 Christian Muller and the ULISSE consortium:ULISSE, USOCs knowledge integration and dissemination for space science experimentation

PA 6 Martin Zell:ESA Human exploration and ELIPS program: activities related to astrobiology

PA 7 Hervé Cottin, Julia M. Kotler, topical team members & guests:Astrobiology, an ESA Topical Team

PA 8 Petra Rettberg, Gerda Horneck, André Brack, Charles Cockell, Cristiano Cosmovici, Pascale Ehrenfreund, Nils G. Holm, Jan Jehlicka, Kensei Kobayashi, Helmut Lammer, Harry Lehto, Kirsti Lehto, Nigel J. Mason, Christian Muller, François Raulin, Alan Schwarz, Helga Stan-Lotter, Ewa Szuszkiewicz:EANA, European Astrobiology Network Association, an ESA Topical Team

PA 9 Charles Cockell:Geo-microbiology, an ESA Topical Team

PA 10 Dag Linnarsson, James Carpenter, Bice Fubini, Per Gerde, Lars L. Karlsson, David J. Loftus, G. Kim Prisk, Urs Staufer, Erin M. Tranfield, Wim van Westrenen:Toxicity of Lunar dust, an ESA Topical Team

Closing Session15:30 Closing Session with poster awards, student contest awards and announcement of next

European Workshop on Astrobiology EANA 13

16:30 Farewell coffee and tea17:30 End of 12th European Workshop on Astrobiology EANA 12

14

Poster session: Monday 15 October, 2012, 17:30 - 19:00Posters will be on display during the whole workshop

Part 1: Extrasolar Planets

Co-chair: Ewa SzuszkiewiczCo-chair: Claudio Maccone

P1.01 Rene Liseau :Space Missions Relevant to Astrobiology

P1.02 Eva Plavalova :Taxonomy of extrasolar planet: constancy of the classes

P1.03 Lisa Nortmann, Stefan Dreizler :Ground-based Spectroscopy of Exoplanet Atmospheres

P1.04 Helmut Lammer, Kristina G. Kislyakova, Petra Odert, Nikolai V. Erkaev, Manuel Gudel,Arnold Hanslmeier :Origin and atmosphere evolution scenarios of Venus, Earth and Mars: Implicationsfor super-Earths

P1.05 Kristina G. Kislyakova, Helmut Lammer, Mats Holmstroem, Nikolai V. Erkaev, Maxim L.Khodachenko:Characterizing exoplanet upper atmosphere-plasma environments around hot Jupitersand terrestrial exoplanets

P1.06 Fadil Inceoglu, Mads Faurschou Knudsen, Christoffer Karoff, Jan Heinemeier, Margit Schwikowski,Pierre-Alain Herren, Anna Sturevik Storm, Ala Aldahan, Goran Possnert :Reconstruction of solar variability during the Holocene based on 10Be record

P1.07 Mats Holmstrom :Energetic Neutral Atoms in Planetary Systems

P1.08 Siddharth Hegde, Lisa Kaltenegger :Colors of extreme exoEarth environments

P1.09 Jan Marie Andersen, Heidi Korhonen:M dwarfs as planet hosts: consequences of stellar activity on exoplanet detection

P1.10 Gianni Cataldi, Alexis Brandeker :Where is the carbon gas in the debris disk around β Pictoris located?

P1.11 Samuel Regandell, Susanne Hofner, Wladimir Lyra, Nikolai Piskunov :Spectral Synthesis for Protoplanetary disk models

P1.12 Kateryna Frantseva, Nadia M. Kostogryz, Taras M. Yakobchuk :Polarimetric effects simulation for HD189733

P1.13 Aris Vasileiadis, Ake Nordlund, Martin Bizzarro:Isotopic Abundances in Evolving, Star-forming Giant Molecular Clouds

P1.14 Eduardo Penteado, Herma M Cuppen, Helio J Rocha-Pinto:Modeling the evolution of molecular clouds as a function of metallicity

P1.15 Eamonn Ansbro:SETV: A new frontier for SETI

15

Part 2: Geochemical origin of life

Co-chair: Nils HolmCo-chair: Alan Schwartz

P2.01 Laura Barge :Pyrophosphate Synthesis in a Proton Gradient Across Iron Sulfide Membranes Sim-ulating Hadean Submarine Hydrothermal Systems

P2.02 Barry Herschy, Tasnim Munshi, Ian Scowen, David Greenfield, Matthew A. Pasek, Claire Cousins,Ian Crawford, Terence P. Kee :Low pH Geothermal Chemistry on the Vatnajokull Glacier. Provision of ActivatedPhosphorus on the Early Earth

P2.03 Jose Enrique Iniguez-Pacheco, Nils G. Holm:On the ferrobrucite role as reactive intermediate of serpentines in pyrophosphateproduction, and its potential role in the phosphorylation reactions in hydrothermalsystems on early Earth

P2.04 Yves Ellinger, Mathias Toulouze, Julien Pilme, Francoise Pauzat :About the presence of arsenic in prebiotic species: a quantum chemical view

P2.05 Marie-Paule Bassez, Yoshinori Takano, Kensei Kobayashi :Prebiotic Organic Microstructures

P2.06 Hiroshi Kanamaru, Hikaru Koda, Kyoko Yokomizo, Yuta Hatae, Shoichi Nakamura, MamiTuruyama, Hajime Mita:Characterization of proteinoid microspheres on their formation and degradation

P2.07 Kensei Kobayashi, Hironari Kurihara, Yukinori Kawamoto, Takuto Okabe, Midori Eto, Yu-miko Obayashi, Takeo Kaneko, Hikaru Yabuta, Hajime Mita, Kazuhiro Kanda:Possible Scenario of the Prebiotic Formation of Organic Aggregates by High-EnergyRadiation and Hydrothermal Processes

P2.08 Franz Leissing, Stefan Fox, Henry Strasdeit :The Thermal Stability of Tetrapyrroles: Exploring the Limits

P2.09 Alexey Novoselov, Paloma Serrano, Mırian Liza Alves Forancelli Pacheco, Michael Scott Chaf-fin, Jack Thomas O’Malley-James, Susan Carla Moreno, Filipe Batista Ribeiro, Carlos Roberto deSouza Filho:From Cytoplasm to Environment: the Inorganic Ingredients for the Origin of Life

P2.10 Robert Bywater :Chemoinformatics and chemical evolution

P2.11 Vladimir Kompanichenko:Inversion concept of the origin of life, its consequences and the experimental verifi-cation program

P2.12 Georg Hildenbrand, Michael Hausmann:Categories of Life

16

Part 3: Origin and evolution of the biosphere

Co-chair: Bill MartinCo-chair: Kirsi Lehto

P3.01 Coryn Bailer-Jones, Fabo Feng :Assessing the influence of the solar Galactic orbit on terrestrial biodiversity variations

P3.02 Veronika Grosz, Gergely Goldschmidt, Attila Berces:Continuous, in situ measurement of the altitude-dependent change of UV radiationand its effects on biological systems

P3.03 Barbara Cavalazzi, Ian R. McLachlan, Nicholas J. Beukes:Glendonite minerals from Late Carboniferous glaciomarine Dwyka Group, SouthAfrica - palaeoenvironmental implication and astrobiological potential

P3.04 Barbara Cavalazzi, Nicholas J. Beukes, Frikkie C. de Beer, Jakobus W. Hoffman, Ian R.McLachlan, Roberto Barbieri :X-Ray tomography and Raman characterization of water expulsion-related microfrac-tures in glendonite nodules: an example from Late Carboniferous glaciomarine DwykaGroup, South Africa

P3.05 Philipp M.G. Loffler, Anders Albertsen, Rafal Wieczorek, Michael Wamberg, Mark Dorr, PernilleL. Pedersen, Carsten Svaneborg, Harold Fellermann, Joseph B. Edson, Jonathan L. Cape, MartinHanczyc, Hans Ziock, James M. Boncella, Pierre-Alain Monnard, Steen Rasmussen :Integration of protocellular components

P3.06 Lauri Nikkanen, Kirsi Lehto:Origin of cellular life: The earliest genome was of eukaryotic type?

P3.07 Clarisse Balland-Bolou-Bi, Sara J. M. Holmstrom, Sabina Hoppe, Nils G. Holm:Role of fungi in the weathering of different iron-bearing minerals

P3.08 Oleksandr Potashko:Comet Hazard to the Earth

P3.09 Arkadii V. Tarasevych, Jean-Claude Guillemin:Crystallization and sublimation of non-racemic mixtures of natural amino acids: apath towards homochirality

P3.10 Eugenio Simoncini, Alfonso Delgado-Bonal, Francisco J. Martin-Torres:Accounting the effect of life on Earth using Amospheric Chemical Disequilibrium.Impact on the definition of Habitable Zone

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Part 4: Planetary habitability & exploration (Mars, Titan, Europa,. . . )

Co-chair: Helmut LammerCo-chair: Wolf Geppert

P4.01 Antonella Barucci, Pascale Ehrenfreund, Patrick Michel, Hermann Bohnhardt, John R. Bru-cato, Elisabetta Dotto, Ian A. Franchi, Simon F. Green, Luisa-M. Lara, Bernard Marty, DetlefKoschny :MarcoPolo-R Asteroid Sample Return Mission: tracing origins

P4.02 Khawaja Nozair Ashraf, Harry Lehto, Johan Silen, Kirsi Lehto, Tuomo Lonnberg, HaraldKruger, Martin Hilchenbach and the COSIMA team:COSIMA-Cometary Secondary Ion Mass Analyzer

P4.03 Paula Lindgren :The history of liquid water in the early solar system: clues from carbonate mineralsin carbonaceous chondrite meteorites

P4.04 Arnold Gucsik, Ulrich Ott, Hirotsugu Nishido, Kiyotaka Ninagawa:Cathodoluminescence microcharacterization of apatite and calcite in the Martianmeteorites: An Implication for Astrobiology

P4.05 Pauli Laine :Habitability in the Solar System and new planetary missions

P4.06 Anna Neubeck, Magnus Ivarsson:Exploring Martian Habitability

P4.07 Frances Westall, Marylene Bertrand, Frederic Foucher, Nicolas Bost :Habitability and early life on Mars

P4.08 Sophie L. Nixon, Charles Cockell, Martyn Tranter :Limitations to a biological iron cycle on Mars

P4.09 Damhnait Gleeson, David Fernandez-Remolar, P. Martin, V. Ruiz :Scale-integrated spectral characterisation of mineralogical analogues to Mars at RioTinto

P4.10 Nicolas Bost, Frances Westall, Claire Ramboz, Frederic Foucher (presented by Marylene Bertrand):The International Space Analogue Rock Store (ISAR): A key tool for future planetaryand astrobiologicaly exploration

P4.11 Nicolas Bost, Frances Westall, Claire Ramboz, Frederic Foucher (presented by Marylene Bertrand):Hydrothermal, deuteritic and acidic basalt alteration at the Skouriotissa mine, Cyprus:relevance for Mars and astrobiological implications

P4.12 Anatoliy K. Pavlov, Maria A. Vdovina, Alexander A. Pavlov :Variation of the modern Martian atmospheric composition as a result of cometaryand asteroidal impacts

P4.13 Euan Monaghan, Manish R. Patel, Karen Olsson-Francis:Determining the extent of the martian water table using a simple lithospheric model

P4.14 Gayathri Murukesan, Taina Laiho, Kirsi Lehto:Local Martian resources allow ecient cyanobacterial biomass and biohydrogen pro-duction

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P4.15 Christine Moissl-Eichinger, Alexander Probst, Anna Auerbach, Petra Rettberg :

Microbial community shifts within a spacecraft associated clean room complex

P4.16 Petra Rettberg, Simon Barczyk, Hubertus Thomas, Satoshi Shimizu, Tetsuji Shimizu, TobiasKlampfl, Gregor Morfill :

The application of Cold Atmospheric Plasma (CAP) for the sterilisation of spacecraftmaterials

P4.17 Nicolas Walter (on behalf of the ESF Study Group):

MSR backward contamination - Considering the required contraints

P4.18 Petra Schwendner, Simon Barczyk, Francesco Canganella, Viacheslav Ilyin, Reinhard Wirth,Harald Huber, Reinhard Rachel, Petra Rettberg :

Monitoring of the microbial community during simulated flight to Mars

P4.19 Christian Muller, Nadia This, Didier Gillotay, Cedrik Depiesse, Didier Moreau:

New technology developments in exploration techniques: what they mean for astro-biology

P4.20 Jaqueline K. Jensen, Asmus Koefoed, Morten Bo Madsen:

Dust investigation on NASA’s Mars Science Laboratory

P4.21 Ebbe Norskov Bak, Svend Knak Jensen, Jon Merrison, Per Nørnberg, Kai W. Finster :

Wind-driven erosion of silicates as a source of oxidants in Martian soil

P4.22 Mikhail Gerasimov :

The Moon polar volatiles: what they can tell us

P4.23 Frederic Foucher, Frances Westall :

Raman mapping of silicied biological remains

P4.24 Bettina Bodeker, Ute Bottger, Heinz-Wilhelm Hubers, Jean-Pierre deVera, Stefan Fox, HenryStrasdeit :

Infrared and Raman Study of the Thermal Degradation of Biomolecules

P4.25 Joachim Meeßen, Ute Bottger, Dana Grunow, Heinz-Wilhelm Hubers, Jean-Pierre de Vera,Francisco Javier Sanchez, Jorg Fritz, Rosa de la Torre, Elke Rabbow, Sieglinde Ott :

Raman Laser Spectroscopy – a valid tool to detect biogenic substances in Mars Re-golith Simulants as well as bio-minerals and organic substances produced by lichens

P4.26 Rodrigo Nascimento, Marcelo M. Sant’anna, Ginette Jalbert, Luiz F. Coelho, N. V. de CastroFaria:

Electron detachment for collisions of carbon based molecular negative ions withmolecular nitrogen

P4.27 Hans Nilsson, Masatoshi Yamauchi, Stas Barabash:

Does a strong magnetic field protect a planetary atmosphere from stellar winds?

P4.28 Katherine Wright, Charles Williamson, Stephen E. Grasby, John R. Spear, Alexis S. Templeton:

”Following the Energy” in an arctic analogue for icy, sulphur-rich sites on Mars andEuropa

P4.29 Masatoshi Yamauchi, Iannis Dandouras and the NITRO proposal team (presented by H. Nilsson):

Understanding the Earth-Venus-Mars difference in Nitrogen

19

P4.30 Leonid Ksanfomality :Possible signs of life on Venus

P4.31 Jun Kawai, Seema Jagota, Kensei Kobayashi, Takeo Kaneko, Yumiko Obayashi, YoshitakaYoshimura, Bishun N. Khare, David W. Deamer, Christopher P. McKay :Self-assembly of Titan tholins in environments simulating Titan liquidospheres anditsimplication to formation of primitive membrane in Titan

P4.32 Alfonso Delgado-Bonal, Francicso .J. Martın-Torres, Eugenio Simoncini :Accurate calculations of Ozone and liquid water over Gale Crater

P4.33 Vivi Vajda, Erik Persson, Dag Ahren, Anna Cabak Redei, Dainis Dravins, David Duner, SofiaFeltzing, Gustav Holmberg, Arthur Holmer, Petter Persson:Signatures of Life on Earth and in Cosmos

20

Part 5: Extremophiles and early life

Co-chair: Daniela BilliCo-chair: Ricardo Amils

P5.01 Armando Azua-Bustos:Present time extreme environments as drivers of convergent evolution

P5.02 Natuschka M. Lee, Olexandra Ganzenko, Andreas Beck, Edwin Gnosq, Florian J. Zurfluhy,Beda Hofmann:Meteorites as habitats for lichens and microorganisms in hot deserts

P5.03 Magnus Ivarsson, Curt Broman, Erik Sturkell, Jens Ormo:Impact-induced hydrothermal systems as habitats for microbial life

P5.04 Petr Vıtek, Jacek Wierzchos, Beatriz Camara-Gallego, Jan Jehlicka, Carmen Ascaso, IanHutchinson, Howell G. M. Edwards:Microbial colonization of halite and gypsum crusts from the Atacama Desert studiedby combination of Raman spectroscopy and microscopic imaging

P5.05 Karen Olsson-Francis, Jon Watson, Charles S. Cockell :Cyanobacteria isolated from the high intertidal zone: a model for studying the phys-iological prerequisites for survival in extraterrestrial environments

P5.06 Engy Ahmed, Sara J. M. Holmstrom, Volker Bruchert, Nils G. Holm:Soil Microorganisms and Mineral Weathering: Mechanics of Biotite Dissolution

P5.07 Jan Frosler, Hans-Curt Flemming, Jost Wingender :The influence of extracellular polymeric substances on the desiccation tolerance ofDeinococcus geothermalis biofilms

P5.08 Oleg Gusev, K. Mukae, M. Sugimoto, T. Kikawada, T. Sakashita, T. Okuda:Surviving rules: wide overlap in gene expression response to desiccation and ionizingradiation in an anhydrobiotic midge

P5.09 Jana Kviderova, Linda Nedbalova, Lenka Prochazkova, Marie Drızhalova:Growth and photochemical activity of snow algae in crossed gradients of temperatureand irradiance

P5.10 Kirill Krivushin, David Gilichinsky, Andrew C. Schuerger, Wayne L. Nicholson:Permafrost microorganisms under Mars-simulated pressure

P5.11 Stefanie Lutz, Alexandre M. Anesio, Liane G. Benning :Cryo-life habitability on a polythermal glacier in Greenland

P5.12 Elena S. Bulat, V. A. Tselmovich, Jean-Robert Petit, L. M. Gindilis, Sergey A. Bulat :Snow cover of Central East Antarctica (Vostok station) as an ideal natural spot forcollecting Cosmic Dust: preliminary results on recovery of chondritic micrometeorites

P5.13 Tina Santl Temkiv, Kai Finster, Ulrich Gosewinkel Karlson:The application of a decontamination technique within the study of low bacterialdensity environments

P5.14 Tina Santl Temkiv, Kai Finster, Thorsten Dittmar, Bjarne Munk Hansen, Runar Thyrhaug,Niels Woetmann Nielsen, Ulrich Gosewinkel Karlson:Hailstones: a window into microbial life in storm clouds

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P5.15 Cleber Pereira Calca, Thomas R. Fairchild, Barbara Cavalazzi, Jorge Hachiro:A Permian hypersaline microbial community (Assistencia Formation, Irati Subgroup- Permian, Brazil) as a potential analogue for early Martian life

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Part 6: Astrobiology on the International Space Station

Co-chair: Herve CottinCo-chair: Helga Stan-Lotter

P6.01 Marylene Bertrand, Annie Chabin, Andre Brack, Herve Cottin, Frances Westall :

The PROCESS and AMINO Experiments: Effects of VUV Photochemistry on AminoAcids on the International Space Station and in Laboratory Simulations

P6.02 Andreas Elsaesser, Richard Quinn, Pascale Ehrenfreund, Alexander Kros, Andrew Mattioda,Antonio Ricco, Farid Salama, Orlando Santos, Herve Cottin, Emmanuel Dartois, Louis d’Hendecourt,Rene Demets, Bernard Foing, Zita Martins, Mark Sephton, Marco Spaans:

OREOcube: ORganics Exposure in Orbit

P6.03 Michael Simakov, Natalia Gontareva, Eugenia Kuzicheva:

Abiogenic synthesis of biologically important compounds in open space conditions

P6.04 Sohan Jheeta, Nigel J. Mason, Radmila Panajotovic, Maria E. Palumbo, Giovanni Strazzulla,Daniele Fulvio, Alicja Domaracka, Elisabeta Burean, Anne Lafosse, Bhalamurugan Sivaraman,Slywia Ptasinska:

Photostability of prebiotioc organic compounds from Low Earth Orbit experiments,ground laboratory photolysis, and from measurements of absorption vacuum UV(VUV) spectra

P6.05 Yukinori Kawamoto, Midori Eto, Takuto Okabe, Yumiko Obayashi, Takeo Kaneko, Jun-ichiTakahashi, Hajime Mita, Kazuhiro Kanda, Kensei Kobayashi :

Stability and alteration of amino acids and related compounds against soft X-raysin interplanetary space

P6.06 Shin-ichi Yokobori, Hirofumi Hashimoto, Nobuhiro Hayashi, Eiichi Imai, Hideyuki Kawai,Kensei Kobayashi, Hajime Mita, Kazumichi Nakagawa, Issay Narumi, Kyoko Okudaira, MakotoTabata, Sumitaka Tachikawa, Yuichi Takahashi, Kaori Tomita-Yokotani, Hikaru Yabuta, MasamichiYamashita, Hajime Yano, Akihiko Yamagishi and the Tanpopo WG :

TANPOPO: Astrobiology exposure and micrometeoroid capture experiments - Pro-posed experiments using the Exposure Facility on ISS-JEM

P6.07 Corinna Panitz, Gerda Horneck, Katja Neuberger, Ralf Moeller, Elke Rabbow, Petra Rettberg,Astrid Lux-Endrich, B. Hock, D. P. Hader, T. Dachev, Gunther Reitz :

Experiment SPORES of the EXPOSE-R mission: Survival of bacterial and fungalspores after nearly 2 years in low Earth orbit

P6.08 Eckehardt Unruh, Peter-Diedrich Hansen :

Altered gravity conditions and its effect on the phagocytosis related ROS-productionof Blue Mussel hemocytes Results of the 56th ESA parabolic flight campaign

P6.09 Mickael Baque, Daniela Billi, Jean-Pierre Paul de Vera:

BIOMEX-Desert Cyanobacteria: ground simulations of the EXPOSE-R2 mission

P6.10 Casey Bryce, Sophie Nixon, Howell Edwards, Gerda Horneck, Charles Cockell :

Survival of Chroococcidiopsis and its biosignatures in Low Earth Orbit

P6.11 Francisco J. Sanchez Inigo, Rosa de la Torre Noetzel, Leopoldo Ga. Sancho, Gerda Horneck :

UV resistance properties of the space-tested lichens species Rhizocarpon geographicumand Circinaria gyrosa: role of the cortex/screening substances and hydration stateof the thalli

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P6.12 Rosa de la Torre Noetzel, Francisco J. Sanchez Inigo, Elke Rabbow, Gerda Horneck, Jean-Pierre de Vera, Leopoldo Ga. Sancho:Survival of lichens to simulated Mars conditions

P6.13 Annette Brandt, Jean-Pierre P. de Vera, Joachim Meeßen, Sieglinde Ott :Lichens as a model-system for survival of eukaryotic symbiotic associations exposedto space conditions

P6.14 Ximena C. Abrevaya, Pablo J.D. Mauas, Eduardo Corton:Microbial Fuel Cells in Life Support Systems

P6.15 Elke Rabbow, Petra Rettberg, Rainer Willnecker, Gunther Reitz :EXPOSE-R2 - the upcoming astrobiological exposure mission

P6.16 Joachim Meeßen, Francisco Javier Sanchez, Annette Brandt, Eva-Maria Balzer, Kai Lyhme,Paul Wieners, Jean-Pierre de Vera, Rosa de la Torre, Sieglinde Ott :Comparative studies on the morphological-anatomical, chemical, and physiologicalproperties of four space-relevant lichen species to assess their high potential in re-sisting extreme environmental conditions

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Abstracts oral presentations

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26

Session 1:Extrasolar planets / Astrophysics

Monday, 15 October 2012:

11:00 Yamila Miguel: Exploring super-Earth Atmospheres

11:15 Ewa Szuszkiewicz: Reversing the inward migration of super-Earths

11:30 Jack O’Malley-James: Life & Light: Exotic photosynthesis in binary and multiple star systems

11:45 Jordi Gutierrez: Metallicity effects on the extension of the stellar habitable zone

12:00 Vassilissa Vinogradoff: Specific chemistry in interstellar ice: reactivity of formaldehyde

12:15 Claudio Maccone: A Mathematical Model for SETI, Evolution and Human History

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28

O1.1 Exploring super-Earth Atmospheres

Yamila Miguel1, Lisa Kaltenegger1,2

1Max Planck Institut fuer Astronomie, Germany; miguel@mpia-hd.mpg.de2Harvard Smithsonian Center for Astrophysics, USA∗E-mail of corresponding author: miguel@mpia-hd.mpg.de

The search for extrasolar planets has resulted in the discovery of super-Earths, with masses between1 and 10 Earth masses. Interior models suggest that some of these exoplanets might be potentially rockyin nature, with outgassed atmospheres. Since no such planets exist in our solar system, the atmosphericcomposition and structure of these potentially rocky super-Earths remains largely unknown. Have abetter knowledge of the formation of rocky planets atmospheres is crucial for astrobiology, since this isa key factor when trying to find out their potential habitability. Our aim is to model the outgassingfrom the surface of the recently formed planet, studying specially the composition and structure of theoutgassed atmosphere, to get a better understanding and characterization of extrasolar rocky planets.With this aim, we explore the possible atmospheric structure of super-Earths with outgassed atmospheresand how this structure changes according to the planetary observable data: mass or radius, semimajoraxis and stellar type.

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O1.2 Reversing the inward migration of super-Earths

Ewa Szuszkiewicz1∗, John C.B. Papaloizou2, Edyta Podlewska-Gaca1

1CASA* and Institute of Physics, University of Szczecin, Poland2DAMTP, University of Cambridge, UK∗E-mail of corresponding author: szusz@fermi.fiz.univ.szczecin.pl

In this talk, I would like to present a new mechanism for stopping the inward migration of a low-massplanet (super-Earth) embedded in a gaseous protoplanetary disc. It operates when a low-mass planetencounters outgoing density waves excited by another source in the disc. This source could be a gasgiant in an orbit interior to that of the low-mass-planet. As a super-Earth passes through the wave field,angular momentum is transferred to the disc material and then communicated to the planet throughco-orbital dynamics, with the consequence that its inward migration can be halted or even reversed. Ourfindings have been published in April 2012 in the Monthly Notices of the Royal Astronomical Society.

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O1.3 Life & Light: Exotic photosynthesis in binary and multiplestar systems

Jack O’Malley-James1∗, John Raven2, Charles Cockell3, Jane Greaves4

1University of St Andrews, St Andrews, UK2University of Dundee at The James Hutton Institute, Dundee, UK3UK Centre for Astrobiology, University of Edinburgh, Edinburgh, UK4University of St Andrews, St Andrews, UK∗E-mail of corresponding author: jto5@st-andrews.ac.uk

The potential for Earth-like planets within binary and multiple star systems to host photosyntheticlife was evaluated by modelling the levels of photosynthetically active radiation (PAR) such planets re-ceive[1]. While previous work in this field has investigated the radiation environments for photosyntheticlife on planets orbiting stars with spectral characteristics that are different to those of the Sun, the influ-ence of two (or more) very different radiation regimes within the same stellar system has not previouslybeen investigated. With the discovery of exoplanets in binary systems, most recently Kepler 16b and,more notably low-mass planets such as 55 Cnc e and GJ 667C b, assessing the habitability of binary andmultiple star systems is becoming increasingly important in the field of astrobiology. In this investigation,G dwarf (sun-like) stars and M dwarf stars (low mass, cool stars) were of particular interest. The formerare known to host a number of exoplanets while the latter are the most abundant stars in the galaxy[2] and Kepler planetary candidate data suggests that terrestrial planets are more abundant around coolstars[3]. Orbital and radiation simulations of such systems were used, including double star systems inwhich the two stars are either very close together (< 0.5 AU), or more widely separated (> 3 AU) andthree-star systems (essentially a combination of the previous two cases). A range of stable radiation envi-ronments were found to be possible. Using what we currently know about photosynthetic life on Earth asa guide, these environmental conditions allow for the possibility of familiar, but also more exotic, formsof photosynthetic life. The possibilities explored include the likely dominant vegetation cover in thesedifferent scenarios, photosynthetic life that uses infrared radiation for photosynthesis and organisms thatare specialized for specific spectral niches in cases where a planet with two suns has two very distinctradiation environments on its surface.

References:

1. J.T. OMalley-James , J.A. Raven, C.S. Cockell and J.S. Greaves, Astrobiology, 12, 115 (2012)

2. J.C. Tarter, P.R. Backus, R.L. Mancinelli et al., Astrobiology, 7, 30 (2007)

3. A.W. Howard, G.W. Marcy, S.T. Bryson, et al., arXiv:1103.2541v1 (2011)

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O1.4 Metallicity effects on the extension of the stellar habitablezone

Jordi L. Gutierrez∗

Escola d’Enginyeria de Telecomunicacions i Aeroespacial de Castelldefels, Universitat Politecnica deCatalunya, Castelldefels, Spain∗E-mail of corresponding author: jordi.gutierrez@upc.edu

In its classical definition, the habitable zone stands for the region of a planetary system where watercan be maintained in its liquid state for extended periods of time (compatible with biological evolution)on the surface of an Earth–like planet. This definition has been challenged by the discovery of subsur-face oceans in Europa and other satellites, and by the overwhelming amount of hot Jupiters, with itspotentially habitable exomoons. Even so, we will stick to the classical definition due to the uncertaintiesrelated with these extensions of the habitable zone, which would seriously complicate its determination.Very recently, Buchhave et al. (2012) have presented strong evidence that small exoplanets do not showa marked metallicity dependence. Thus, them can have formed at rather small metallicities, openingthe possibility that the location and width of their habitable zones have been modified by metallicityeffects on the evolution of their central stars. Usually, stars of the same metallicity as our Sun have beenused to determine the boundaries of the classical habitable zone. In this regard it is interesting to notethat the actual metallicity of the sun is still somewhat uncertain, and that in the solar vicinity there isa considerable spread on metallicity. Taking everything together, it seems relevant to compute stellarevolution models of low mass stars (0.25–2.0 M�) with different initial metallicities (Z=0.001, 0.005, 0.01,0.015, 0.02, 0.03, 0.04), and determine the extension of the associated habitable zones using the modelby Jones et al. (2006).

References:

1. Buchhave, L. R. et al., ”An abundance of small exoplanets around stars with a wide range ofmetallicities” Nature 486, 375–377 (2012).

2. Jones, B. W., Sleep, P. N., Underwood, D. R., ”Habitability of Known Exoplanetary Systems Basedon Measured Stellar Properties”, Ap. J. 649, 1010–1019 (2006)

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O1.5 Specific chemistry in interstellar ice: reactivity of formalde-hyde

Vassilissa Vinogradoff1, Fabrice Duvernay1, Albert Rimola2, Gregoire Danger1, Patrice Theule1, FabienBorget1, Jean-Claude Guillemin3, Thierry Chiavassa1

1Aix Marseille University, Marseille, France2University Autonoma of Barcelona, Barcelona(UAB), Spain3ENSCR, Rennes, France∗E-mail of corresponding author: vass vino@yahoo.fr

Dust grains in the interstellar medium (ISM) play an important role in dense molecular clouds chem-istry of providing a surface (catalyst) upon which atoms and molecules can freeze out, forming icy mantles.Dense molecular clouds are characterized by low temperature (10–50 K) and represent the birth sites ofstars. After a gravitational breakdown, a part of the dense molecular cloud collapses toward the forma-tion of star and subsequently a protoplanetary disk from which planets, asteroids and comets will appear.During this evolution, interstellar organic material inside ices undergoes different range of chemical al-terations (thermal cycling process, ultraviolet photons, electron scattering and cosmic rays irradiation)hence increasing the molecular complexity before their incorporation inside precometary ices. We de-velop a new laboratory approach to understand the evolution in interstellar ices by separating thermalprocessing from VUV processing. Infrared spectroscopy and mass spectroscopy are used to monitor theexperiments. We were interested in the formation and mechanism, in interstellar conditions, of complexorganic molecules from a simple molecule: the formaldehyde (H2CO). We put in evidence a complexnetwork of reactions. Among these complex formed organic molecules, we were particularly interestedby the mechanism for HMT formation. HMT (hexamethylenetetramine) is a very interesting molecule,because it composes most part of the complex organic residue stable at room temperature, obtained fromVUV irradiation and warming of CH3OH, NH3 and H2O ice mixture. This residue is presumed to be aclose analog of dust organic mantles in molecular clouds, or in the mantle of comets and meteorites. Weput in evidence in our work that HMT can be easily formed only by the warming of an ice mixture offormaldehyde ammonia and formic acid, three interstellar molecules contained in icy-grains of molecularclouds, or comets mantle. Our study intend to better understand the complex chemistry which occur insuch astrophysical environments, by working with specific and simplified ice mixture in solid state andsimulate one energetic process at time. We put in evidence the importance of the mechanism which canhappen in solid phase chemistry and lead to complex organic molecules. Moreover, we show that theonly warming of specific molecule can lead to complex molecule organic, as VUV irradiation processes do.

References:

1. New insight into the formation of Hexamethylenetetramine (HMT) in interstellar and cometary iceanalogs. V. Vinogradoff, F. Duvernay, G. Danger, P. Theul, and T. Chiavassa. A&A 530, A128(2011)

2. Acetaldehyde Solid State Reactivity at Low Temperature: Formation of the Acetaldehyde AmmoniaTrimer, V. Vinogradoff, F. Duvernay, M. Farabet, G. Danger, P. Theul, F. Borget, J.C. Guilleminand T. Chiavassa. J.Phys. Chem A, 116 (9), pp 2225–2233 (2012)

3. Aminoacetonitrile characterization in astrophysical-like conditions, F. Borget, G. Danger, F. Du-vernay, M. Chomat, V. Vinogradoff, P. Theul, and T. Chiavassa, A&A 541, A114 (2012)

4. Mechanism of Hexamethylentetramine (HMT) formation in interstellar conditions, Vinogradoff V.Rimola A. Duvernay F., Danger G., Theule P., Chiavassa T. JACS 2012, submitted

33

O1.6 A Mathematical Model for SETI, Evolution and HumanHistory

Claudio Maccone1,2

1Technical Director, International Academy of Astronautics (IAA), Paris, France2IASF-INAF Associate, Milan, Italy∗E-mail of corresponding author: clmaccon@libero.it

We present a mathematical theory unifying Darwinian Evolution and Human History into a single,new mathematical vision. If extrapolated into the future, this model might also enable us to estimatehow much more advanced than Humanity an Alien Civilization will be when SETI succeeds.

Our estimate of ‘evolution amount’ is achieved by mastering mathematically the only life example weknow for sure – i.e. ourselves. Therefore, the past of life on Earth is regarded as made up by two parts:Darwinian Evolution as it unfolded over the last 3.5 billion years and Human History as it unfolded overthe last 13 thousand years.

The mathematical tools used to merge them into a single mathematical vision are:

1. b-lognormals, i.e. lognormal probability density functions (pdf) starting at a given instant b > 0(standing for ‘birth’) rather than just at the at the origin, as it is usually done.

2. A new mathematical mechanism discovered by the author typical of all b-lognormals having theirpeak lying on an exponential function of the time (‘running b-lognormals’). Since the area undereach b-lognormal always equals to 1 (normalization condition), for small values of the peak timethe running b-lognormal is rather flat, whereas for higher values of the peak time the runningb-lognormal is much more peaked. Please see Figure 1.

3. Shannon’s entropy of the running b-lognormals is then the measure of the “evolution amount”achieved by the corresponding living organism or civilization. This result is important, inasmuch asthe mathematical apparatus of Information Theory may now be invoked to characterize the amountof evolution reached by each living organism or by each historic civilization. In other words, wehave discovered a way to quantify the amount of evolution, rather than just using words.

As for Darwinian Evolution, in a recent paper [1] this author proposed that:

1. The exponential growth of the number of species typical of Darwinian Evolution may be regardedas the geometric locus of the peaks of the b-lognormals constrained between the time axis and theexponential growth curve.

2. Cladograms are made up by arches of exponential curves for each species considered. These ex-ponentials may be either increasing (growing species) or decreasing (extinct species) or horizontallines in time (surviving species since their start up to now).

Abstract Sample: 12th European Workshop on Astrobiology (EANA) 2012 A Mathematical Model for SETI, Evolution and Human History

Claudio Maccone1, 2

1Technical Director, International Academy of Astronautics (IAA), Paris, France 2IASF-INAF Associate, Milan, Italy

We present a mathematical theory unifying Darwinian Evolution and Human History into a single, new mathematical vision. If extrapolated into the future, this model might also enable us to estimate how much more advanced than Humanity an Alien Civilization will be when SETI succeeds. Our estimate of “evolution amount” is achieved by mastering mathematically the only life example we know for sure – i.e. ourselves. Therefore, the past of life on Earth is regarded as made up by two parts: Darwinian Evolution as it unfolded over the last 3.5 billion years and Human History as it unfolded over the last 13 thousand years. The mathematical tools used to merge them into a single mathematical vision are: 1) b-lognormals, i.e. lognormal probability density functions (pdf) starting at a given instant

b>0 (standing for “birth”) rather than just at the at the origin, as it is usually done. 2) A new mathematical mechanism discovered by the author typical of all b-lognormals

having their peak lying on an exponential function of the time (“running b-lognormals”). Since the area under each b-lognormal always equals to 1 (normalization condition), for small values of the peak time the running b-lognormal is rather flat, whereas for higher values of the peak time the running b-lognormal is much more peaked. Please see Figure 1.

3) Shannon’s entropy of the running b-lognormals is then the measure of the “evolution

amount” achieved by the corresponding living organism or civilization. This result is important, inasmuch as the mathematical apparatus of Information Theory may now

Fig. 1 Example of three running b-lognormals, all having their peaks on the exponential above, but having each a different entropy. Figure 1: Example of three running b-lognormals, all having their peaks on the exponential above, but

having each a different entropy.

34

As for Human History, in [2] and [3] we extended these ideas to encompass Human History (AncientGreece to USA) and derive the relevant exponential growth trend. See Figure 2.

In conclusion, we believe that this unified new mathematical vision of Evolution and History maygreatly simplify our understanding of the past, and open up new prospects for the future.

References:

1. C. Maccone, Origins of Life and Evolutionary Biospheres (OLEB), 41, 609 (2011),

2. C. Maccone, SETI, Evolution and Human History merged into a Mathematical Model, submittedin May 2012 for publication in the journal Astrobiology.

3. C. Maccone, Mathematical SETI, a 700-pages book, Praxis-Springer, 2012, ISBN 978-3-642-27436-7.

Abstract Sample: 12th European Workshop on Astrobiology (EANA) 2012

be invoked to characterize the AMOUNT OF EVOLUTION reached by each living organism or by each historic civilization. In other words, we have discovered a way to QUANTIFY THE AMOUNT OF EVOLUTION, rather than just using words.

As for Darwinian Evolution, in a recent paper [1] this author proposed that: 1) The exponential growth of the number of species typical of Darwinian Evolution may be

regarded as the geometric locus of the peaks of the b-lognormals constrained between the time axis and the exponential growth curve.

2) Cladograms are made up by arches of exponential curves for each species considered. These exponentials may be either increasing (growing species) or decreasing (extinct species) or horizontal lines in time (surviving species since their start up to now).

As for Human History, in [2] and [3] we extended these ideas to encompass Human History (Ancient Greece to USA) and derive the relevant exponential growth trend. See Figure 2.

In conclusion, we believe that this unified new mathematical vision of Evolution and History may greatly simplify our understanding of the past, and open up new prospects for the future.

REFERENCES

[1] C. Maccone, Origins of Life and Evolutionary Biospheres (OLEB), 41, 609 (2011), [2] C. Maccone, SETI, Evolution and Human History merged into a Mathematical Model, submitted in May

2012 for publication in the journal Astrobiology. [3] C. Maccone, Mathematical SETI, a 700-pages book, Praxis-Springer, 2012, ISBN 978-3-642-27436-7.

Figure 2: Example of three running b-lognormals, all having their peaks on the exponential above, buthaving each a different entropy.

Session 2:Planetary Habitability

Monday, 15 October 2012:

14:00 Jean-Pierre De Vera: Habitability and Exploration of Mars: a scientific and engineering evaluationconcept of Antarctic and Arctic field sites as geo-biological analogues for the surface of Mars

14:15 Pascale Ehrenfreund: MarcoPolo-R Asteroid Sample Return Mission: tracing origins

14:30 Sean McMahon: Analysis of volatiles in basalt, a possible source of Martian methane

14:45 Fulvio Franchi: Ancient fluid escape and related features in the equatorial Arabia Terra (Mars)

15:00 Barbara Cavalazzi: Martian Exploration: Do not underestimate the volcanic rocks as a possiblehabitat

15:15 Anatoliy Pavlov: Degradation of the ”biomarkers” in the shallow subsurface of Mars due to irradi-ation by cosmic rays

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36

O2.1 Habitability and Exploration of Mars: a scientific and en-gineering evaluation concept of Antarctic and Arctic field sitesas geo-biological analogues for the surface of Mars

Jean-Pierre de Vera1, Ernst Hauber1, Nicole Schmitz1, Ulrich Szewzyk2

1German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany2Institut fur Technischen Umweltschutz, Umweltmikrobiologie, Technische Universitat Berlin, Germany∗E-mail of corresponding author: jean-pierre.devera@dlr.de

An evaluation project for classification of Antarctic field sites to be geo-biological relevant for Marsanalogues is planned to be done on the next German North Victorialand Expedition (GANOVEX 11).The aim is to work out an interdisciplinary topic, which will connect the expertise of the geo-sciences,the life sciences and the engineering sciences. The goal is to conduct comparing studies on field sites andin the laboratories, answering the question, which locations are relevant in the geological and climaticcontext to similar cartographic characterized locations on the planet Mars and which of them are alsoable to show niches for the survival and active life processes of microorganisms and may be classifiedas biological Mars relevant. On one hand the question will be addressed in this proposed comparativestudy, which criteria will classify niches on Mars as potential habitats for microorganisms and on the otherhand a complete inventory of biodiversity in the Antarctic niches with Mars relevance will be studiedby adding climatic and mineralogical characterization to topographic and cartographic localization ofthe Mars-like habitats. A collection of soil and rock samples colonized by organisms will be carried outafter characterization of the Antarctic habitats and their bio-diversity will be analyzed and determinedby classic and molecular biological methods. After the expedition the bio-samples will be investigated ontheir activity before, after and during Mars simulation experiments in a Mars simulation chamber, testingthe collected terrestrial life forms from polar habitats on their ability to adapt to Mars-like environmentalconditions. Finally comparing studies with data from arctic expeditions like data from expeditions inthe AMASE-program on Svalbard combined to extensive image material from the surface of Mars willbe studied. This might be relevant to find out if both investigated polar locations have similar analogueproperties with Mars relevance and if both of them are harboring life with similar retreat strategiesallowing a characterization of bio-relevant Mars analogue habitat. Tests with instrumentation whichmight be important for the next space missions to Mars will be done in parallel. The use of a PanCamsystem as well as different spectroscopy and sensor devices will be checked on their ability to detect lifeand to characterize the environment of probable habitable niches.

37

O2.2 MarcoPolo-R Asteroid Sample Return Mission: tracingorigins

Pascale Ehrenfreund1∗, Antonella Barucci2, Patrick Michel3, Hermann Bohnhardt4, John R. Brucato5,Elisabetta Dotto6, Ian A. Franchi7, Simon F. Green7, Luisa-M. Lara8, Bernard Marty9, Detlef Koschny10

1Space Policy Institute, George Washington University, Washington DC, USA2LESIA-Observatoire de Paris, 92195 Meudon Principal Cedex, France3Univ. Nice, CNRS, OCA, France4MPS, Katlenburg-Lindau, Germany5INAF-Obs. of Arcetri, Italy6INAF-Obs. of Roma, Italy7Open Univ., Milton Keynes, UK8IAA-CSIC, Granada, Spain9CRPG, Nancy, France10ESTEC, ESA, Netherlands∗E-mail of corresponding author: pehren@gwu.edu

MarcoPolo-R is a sample return mission to a primitive Near-Earth Asteroid (NEA) selected for anassessment study at ESA in the framework of ESA Cosmic Vision program. MarcoPolo-R will rendezvouswith a primitive NEA, scientifically characterize the object at multiple scales, and return a unique sampleto Earth unaltered by the atmospheric entry process or terrestrial weathering. The baseline target is abinary asteroid (175706) 1996 FG3, which provides enhanced science return. MarcoPolo-R will returnbulk samples from an organic-rich binary asteroid to Earth for laboratory analyses, allowing us to:

• explore the origin of planetary materials and initial stages of habitable planet formation

• identify and characterize the organics and volatiles in a primitive asteroid

• understand the unique geophysics, dynamics and evolution of a binary NEA.

The baseline mission scenario of MarcoPolo-R to 1996 FG3 includes a single primary spacecraft, carryingthe Earth re-entry capsule and sample acquisition and transfer system, will be launched by a Soyuz-Fregatrocket from Kourou.The scientific payload includes state-of-the-art instruments, e.g. a camera systemfor high resolution imaging from orbit and on the surface, spectrometers covering visible, near-infraredand mid-infrared wavelengths, a neutral-particle analyser, a radio science experiment and optional laseraltimeter. The mission will answer to fundamental astrobiological questions “How does the Solar Systemwork?” and “What are the conditions for life and planetary formations?”.

38

O2.3 Analysis of volatiles in basalt, a possible source of Martianmethane

Sean McMahon1, John Parnell1, Nigel Blamey2,

1University of Aberdeen, UK2New Mexico Tech, USA∗E-mail of corresponding author: sean.mcmahon@abdn.ac.uk

If confirmed, the extremely low concentrations of methane (CH4) detected in the Martian atmo-sphere may represent reservoirs and emission processes that would normally be considered negligible onEarth. One such process is the release of ancient volatiles from fluid inclusions and interstitial sites inrocks and minerals during erosion or geothermal activity. Using a highly sensitive rock-crushing andmass-spectrometry technique previously shown to detect CH4 in serpentinites and hydrothermal mineraldeposits, we have demonstrated that CH4 and other ancient volatiles can be recovered from basalt, thedominant rock type on the Martian surface. Basalt and other mafic and ultramafic igneous rocks areknown to incorporate methane formed by both biological and geological processes, chiefly the serpentin-isation of olivine. Basalt samples from a wide range of ages and geological systems were tested, all ofwhich released CH4 when crushed. Samples analysed were Archean, Neoproterozoic, Ordovician, Ter-tiary and Recent and included vesicular, amygdaloidal and non-vesicular basalts; oxidatively weatheredbasalts; mineral veins cross-cutting basalt; subaerial and submarine basalts; and an olivine bomb (xeno-lith). Oxidative weathering was associated with lower quantities of CH4. Otherwise, CH4 recoverabilityshowed no relationship with age or geological context. Mineral veins cross-cutting one sample were foundto share the volatile composition of the basalt. In general, the results suggest that CH4-release fromancient basalts could be a significant process on Mars, which could be further investigated by Martianrovers using a similar rock-crushing and mass spectrometry technique in situ, perhaps supplemented byisotopic analysis.

39

O2.4 Ancient fluid escape and related features in the equatorialArabia Terra (Mars)

Fulvio Franchi1, A. P. Rossi2, M. Pondrelli3, B. Cavalazzi1, R. Barbieri1

1Dipartimento di Scienze Della Terra e Geologico, Ambientali, Universita di Bologna, Italy; fulvio.franchi2@unibo.it2Jacobs University, Bremen, Germany3IRSPS, Universita D’Annunzio, Pescara, Italy∗E-mail of corresponding author: fulvio.franchi2@unibo.it

In the last decades much energy was devoted to the research of fluid water evidences on Mars andother planetary bodies. Presence of past or present water is the strongest evidence of a living planetand an incentive for the astrobiological research looking for life signatures potentially preserved in thewater-related rocks. New models of Mars hydrology localized groundwater upwelling sites in the equa-torial lowlands where huge thickness of water-related sediments accompanied by peculiar structures wasdeposed. Upwelling of groundwater produced gullies, pitted cones, knobs, channels and many other fea-tures, throughout Mars in correspondence of evaporation-related sediments. A comparative approachof some of these morphologies identified in the Arabia Terra region provides insights into the geneticinteraction of water and Mars sediments. Arabia Terra, in the equatorial region of Mars, is long-timestudied area especially for the abundance of fluid related features. Detailed stratigraphic and morpholog-ical study of the succession exposed in the Crommelin and Firsoff craters, respectively centered at 4.9◦N– 349.5◦E and 2.6◦N – 350.8◦E, evidenced the occurrences of peculiar morphologies like flow structuresand conical mounds (see figure 3). All these morphologies occur within the Equatorial Layered Deposits(ELDs) described in literature as spring deposits [1]. Martian layered spring deposits are of considerableinterest for their supposed relationship with water and high potential of microbial signatures preserva-tion. Hence, their relation with fluids escape makes the Equatorial Layered Deposits attractive targetsfor future missions with astrobiological purposes on Mars. In this work we present the results of newelaborations of the remote sensing data base available in this region, coupled with the new theories ofa regional groundwater upwelling [2] and with a comparative study of other layered deposits describedelsewhere on Mars. This comparative study allowed us to assume that the described morphologies andspring deposits could be related to the presence of fluids escape in the Late Noachian which interestedthe ELDs during their deposition.

References:

1. M., Pondrelli, A.P., Rossi, G.G., Ori, S., van Gasselt, D., Praeg, S., Ceramicola, Earth and Plane-tary Science Letters, 304 (3-4), 511-519 (2011)

2. J.C., Andrews-Hanna, M.T., Zuber, R.E., Arvidson, S.M., Wiseman, Journal of Geophysical Re-search, 115, E06002 (2010)

40

Figure 3:

41

O2.5 Martian Exploration: Do not underestimate the volcanicrocks as a possible habitat.

Nicolas Bost1,2∗, Frances Westall1, Marylene Bertrand1, Barbara Cavalazzi3, Frederic Foucher1

1Centre de Biophysique Moleculaire, CNRS, Rue Charles Sadron, 45071 Orleans Cedex 22Institut des Sciences de la Terre d’Orleans, 1A rue de la Ferollerie, 45071 Orleans Cedex 23Department of Geology, University of Johannesburg, South Africa∗E-mail of corresponding author: nicolas.bost@cnrs-orleans.fr

Recent observations suggest Mars could have sustained life at least in some localities and during someperiods in the past. Perhaps the subsurface environment can support life today [1,2]. The surface of Marsis essentially composed by various types of basaltic rocks. The search for life on Mars has been concen-trated mainly on the search for sedimentary rocks, especially phyllosilicates and carbonates, thought tobe formed from aqueous processes. Although traces of life are more likely to be preserved in these kindsof rocks, volcanic rocks that were in direct association with water should not be neglected. Several of thesamples of volcanic rocks from the International Space Analogue Rockstore (ISAR, [3,4,5]) are volcanicrocks, such as komatiites from South Africa and Canada and artificial martian basalts showing spinifextextures [6]. These kinds of volcanic rocks are known to be favorable habitats for chemolithotrophicmicroorganisms [7], in particular along crystal boundaries or in cracks and vesicles. Furthermore, alter-ation of these rocks produces Fe-Mg clays, such as nontronite and chlorite-saponite, that could have beenimplicated in the concentration of prebiotic organics and, thus, in various scenarios for the origin of life[8]. Other volcanic samples in the ISAR collection include volcanogenic sediments, such as the 3.45 Gaold from from Kittys Gap in Australia, that were silicified. This sample contains evidence of traces ofthe early primitive life [1]. All the volcanic samples were investigated using Raman spectroscopy andGC-MS, revealing the presence of organic matter.

References:

1. Westall F. et al.,. Space Sci.59, 2011

2. Des Marais D. P. Am. Philos. Soc.154, 2010

3. Westall F. et al. LPI contribution 1608, 1346, 42nd LPSC, 2011

4. Bost N. et al. Icarus, in review

5. Bost N., et al. The International Space Analogue Rock Store (ISAR) : A key tool for futureplanetary and astrobiologicaly exploration, this conference

6. Bost N., et al. Meteorit. Planet. Sci. 45, 2012

7. Cavalazzi B. et al. Astrobiology 11, 2011

8. Meunier, A. Origins Life Evol. B. 40, 2010.

42

O2.6 Degradation of the ”biomarkers” in the shallow subsurfaceof Mars due to irradiation by cosmic rays

Anatoliy K.Pavlov1∗, Alexander A. Pavlov2, Gennady Vasilyev1, Valery Ostryakov3, Maria A. Vdovina1

1Ioffe Physical Technical Institute of RAS, Russia2NASA Goddard Space Flight Center, USA3Saint Petersburg Polytechnical State University, Russia∗E-mail of corresponding author: anatoli.pavlov@mail.ioffe.ru

Detection of the organic matter on Mars is one of the main goals of the future martian landing missions.Yet, the degradation of organic molecules by cosmic ray irradiation on Mars is often ignored. We calculatethe radiation dose accumulation rates from solar and galactic cosmic rays at various depths in the shallowMartian subsurface. We show that the preservation of ancient complex organic molecules in the shallow(∼ 10 cm depth) subsurface could be highly problematic if the exposure age of a geologic outcrop wouldexceed 300 Myr. We demonstrate that more simple organic molecules with masses ∼ 100 amu shouldhave a good chance to survive in the shallow subsurface. 13C/12C ratio is another type of ‘biomarkers’are shadowed by cosmic rays radiation accumulation of 13C producing by CR is able to significantlychange 13C/12C ratio in Martian soil with small carbon abundance. Time for 13C accumulation to ‘erase’biogenic isotope shift depends on the total carbon abundance in soil. It is 109 years for carbon abundance10−5 g/g and only 105 years for carbon abundance 10−9 g/g. Implications to the sampling strategy forthe oncoming martian missions are discussed.

Session 3:Geochemical origin of life

Monday, 15 October 2012:

16:00 William F. Martin: Hydrogen, metals, electron bifurcation, and ion gradients: The early evolutionof biological energy conservation

16:15 Jean-Francois Lambert: Formation of activated molecules by condensation on mineral surfaces

16:30 David Bryant: Pyrophosphite as a plausibly prebiotic energy currency molecule

16:45 Stefan Fox: Primordial island volcanoes as locations of prebiotic chemical evolution

17:00 Axelle Hubert: Investigating the geochemical composition of early life signatures and environmentof deposition in highly silicified Archaean cherts - Analytical methods

17:15 Kai Finster: Sulfur disproportionators as a model of a chemolithoautotrophic “LUCA”

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44

O3.1 Hydrogen, metals, electron bifurcation, and ion gradients:The early evolution of biological energy conservation

William F. Martin

Institute of Molecular Evolution, University of Dusseldorf, GermanyE-mail of corresponding author: bill@hhu.de

Life is a persistent, self-specified set of far from equilibrium chemical reactions. In modern microbes,core carbon and energy metabolism are what keep cells alive. In very early chemical evolution, theforerunners of carbon and energy metabolism were the processes of generating reduced carbon compoundsfrom CO2 and the mechanisms of harnessing energy as compounds capable of doing some chemical work.The process of serpentinization at alkaline hydrothermal vents holds promise as a model for the originof early reducing power, because Fe2+ in the Earth’s crust reduces water to H2 and inorganic carbonto methane. The overall geochemical process of serpentinization is similar to the biochemical processof methanogenesis, and methanogenesis is similar to acetogenesis in that both physiologies allow energyconservation from the reduction of CO2 with electrons from H2. Electron bifurcation is a newly recognizedcytosolic process involving soluble, not membrane associated proteins, that anaerobes use generate lowpotential electrons. It plays an important role in some forms of methanogenesis and, excitingly, also inacetogenesis. Electron bifurcation almost certainly figures into the early evolution of biological energyconservation. The question of how is the topic of the talk.

45

O3.2 Formation of activated molecules by condensation on min-eral surfaces - A contribution to prebioenergetics

Jean-Francois Lambert1,2∗, Maguy Jaber1,2, Thomas Georgelin1,2, Houssein Bazzi1,2

1UPMC Univ Paris 06, UMR 7197, Laboratoire de Reactivitde Surface, Tour 54-55, 2eme etage - Casier178, 4, Place Jussieu, F-75252 Paris CEDEX 05, France2CNRS, UMR 7197, Laboratoire de Reactivite de Surface∗E-mail of corresponding author: jean-francois.lambert@upmc.fr

The condensation of oligomers (amino acids, nucleotides) into the corresponding biopolymers on min-eral surfaces, with or without activators, is a part of many prebiotic scenarii [1,2]. While it has long beenevidenced experimentally, a satisfactory physico-chemical description is still lacking, and would consti-tute a prerequisite to determine the likelihood of “surface scenarii”. The corresponding polymerizationreactions in aqueous solutions are endergonic and therefore do not occur spontaneously.

What makes them thermodynamically allowed on surfaces is simply the possibility of working inconditions of very low water activity, as all reported successful instances of polymerization involve dryingsteps. Since these condensation reactions result in the production of one water molecule (R-COO− +R’-NH3+ = R-CO-NH-R’ + H2O), simple thermodynamic arguments (Lechatelier’s principle) ensure thatdecreasing water activity will favor condensation. This is of course not a catalytic effect since catalysiscannot change the thermodynamics.

The same argument holds for several reactions of fundamental importance in current bioenergetics,such as the formation of ATP (P-O-P from P-OH condensation) or various phosphorylations (C-O-P fromC-OH and P-OH).

Therefore we have compared on the same supports the dimerization of the simplest amino acid(glycine) with the formation of ATP from ADP and inorganic phosphate, and with the formation ofan inorganic activated molecule (pyro- and/or metaphosphates from orthophosphate). The investigatedsystems are characterized both macroscopically, from thermogravimetric analysis, and at the molecularlevel with 13C, 31P solid-state NMR, transmission IR and Raman spectroscopy of the dried powders inorder to unequivocally identify the formation of so-called high-energy bonds (P-O-P, C-O-P bust alsoamide bonds). The formation of these bonds upon drying is easily observed by TG, and thermal effectsare still endothermic, so that the entropic effect of removing water is fully responsible for condensation.

Not all mineral surfaces are efficient to promote endothermic condensations, although the thermo-dynamic argument should be the same for all of them. This is where catalysis comes into play. Somesurfaces, like those of divided silica (mesoporous or non-porous) and of calcium carbonate, provide an in-termediate strength interaction with the adsorbed biomolecules, probably by H-bonding, and in this wayopen new reaction pathways with lower activation energy, resulting in condensation at measurable ratesfor moderate temperatures (100–200◦C). In other situations (e.g. AAs intercalated within smectite claylayers), the activation is too weak to result in significant rates of condensation before the biomolecules arethermally degraded. In others still (e.g. glycine on alumina), the small biomolecules interact too stronglywith the surface and remain trapped in the adsorbed monomeric state.

References:

1. J.P. Ferris, A.R. Hill Jr, R. Liu, L.E. Orgel, Nature, 381, 59-61 (1996)

2. J-F. Lambert, Orig. Life Evol. Biosph., 38, 3, 211-242 (2008)

46

O3.3 Pyrophosphite as a plausibly prebiotic energy currencymolecule on the early earth

David E. Bryant1∗, Barry Herschy1, Richard Telford2, Katie E. R. Marriott1, Nichola E. Cosgrove1, KarlKaye1, Matthew A. Pasek3, Claire Cousins4, Ian Crawford4, Terence P. Kee1

1School of Chemistry, University of Leeds, Woodhouse Lane, Leeds, LS2 9JT, UK2School of Life Science, University of Bradford, Richmond Road, Bradford, BD7 1DP, UK3Department of Geology, University of South Florida, Tampa, FL 336204Department of Earth and Planetary Sciences, Birkbeck College, University of London, Gower Street,WC1E 6BT, UK∗E-mail of corresponding author: d.bryant@leeds.ac.uk

Amongst the most important and ubiquitous energy-currency molecules of contemporary biochem-istry are activated phosphorus (P) species such as phosphocreatine, phosphoenol pyruvate and adenosinetriphosphate (ATP). Activated-P based energy currencies in contemporary biochemistry (ATP, PEP &PC) along with plausibly prebiotic ancestors [PPi(V), cTMP, AcPi(V) & PPi(III)]. These moleculesare able to selectively discharge tranches of energy (ca. 40kJmol-1 for the hydrolysis of ATP to ADP)when coupled, mechanistically, to drive endergonic chemical reactions. Various mechanisms have emergedwithin prokaryotic & eukaryotic systems to re-charge their supply of ATP, with mitochondrial oxidativephosphorylation and substrate-level phosphorylation during glycolysis being central. One of the mostsignificant problems in the field of abiogenesis concerns the emergence of a global P-based system ofbioenergetics based on condensed phosphate energy currency molecules such as ATP. So firmly embed-ded is ATP in cellular bioenergetics that it is not unreasonable to propose it as being amongst the mostancient of biochemical machinery. The question of its emergence raises some challenging problems: (i)what simpler P-based systems could have preceded ATP as an energy currency, (ii) how could such sys-tems have emerged within early earth geological environments, (iii) what chemical processes could suchan energy currency have driven & (iv) how might such primitive P-based systems have evolved chem-ically into ATP-based contemporary biochemistry? Recently, there has been considerable support forpyrophosphate [PPi(V); P2O74-] as a logical ancestor of ATP, not least because of a firmly establishedrole in biology. Not only does PPi(V) retain the key [P-O-P] linkage central to energy transduction inATP but, divested of its adenosine cloak, its prebiotic plausibility becomes associated less with RNAworld chemistry and more focused on early earth geology. However, problems remain with PPi(V) asan effective pre-RNA world P-based energy currency, including inherent low solubility in salt-rich watersand low kinetic reactivity in the absence of suitable (enzyme) catalysts. Here we propose a new hypoth-esis in which the condensed oxyacid pyrophosphite [PPi(III); H2P2O52-] is envisaged to have precededthe condensed phosphates of contemporary biochemistry as a functional energy currency molecule. Inthis contribution we provide a geologically plausible provenance for PPi(III), evidence of its ability todrive chemistry of potential value to an emerging living system and also chart a prebiotically plausibleroute from PPi(III) to PPi(V). We report here that in situ field incubation of a fragment of Sikhote-Alinmeteorite, in geothermal fluid (pH 3.1; T = 93 − 94◦C) for 4 days in the Kverkfjll mountain region ofthe Vatnajokull glacier, south-east Iceland,followed by ambient temperature incubation in the same fluidfor a period of 4 weeks affords Pi(III) and that subsequent evaporation and dry-heating of this samegeological fluid sample to 85◦C in the open air affords PPi(III).

Laboratory experiments show the facile ambient temperature conversion of PPi(III) in the presenceof phosphate to the condensed oxyacid isohypophosphate [HP2O63-] with 45% yield. In the presenceof magnesium ions and an excess of phosphate at 80◦C, isohypophosphate can be further converted topyrophosphate [P2O74-] with a yield of ca. 35% after 5days. Pyrophosphite, PPi(III), activates aminoacids to form peptide bonds in aqueous solution at room temperature and pH 9-10 and can phosphonylateadenosine monophosphate (AMP) in either the 2’ or 5’ position under pH control.

47

O3.4 Primordial island volcanoes as locations of prebiotic chem-ical evolution

Stefan Fox∗, Henry Strasdeit

Department of Bioinorganic Chemistry, Institute of Chemistry, University of Hohenheim, 70599 Stuttgart,Germany∗E-mail of corresponding author: stefan.fox@uni-hohenheim.de

Prebiotic chemical complexity and eventually life on Earth must have evolved through a very largenumber of small steps. Therefore, one can assume that places where especially diverse geochemical andgeophysical conditions existed were beneficial to chemical evolution (Strasdeit, 2010). For example, pri-mordial volcanic islands could have provided several chemically interesting microenvironments where theformation of organic molecules and their self-assembly into protometabolic networks are conceivable: (i)hot lava fields (temperature gradients; thermal reactions; evaporation-condensation); (ii) coastal lavaflows (organic transformations; formation of salt crusts; release of HCl); (iii) acidic (e. g. HCl), neutraland basic locations (silicates; buffer effect of igneous rocks); (iv) eruption clouds (organic syntheses byvolcanic lightning) (Navarro-Gonzalez and Segura, 2004; Johnson et al., 2008); (v) rock pools (servingas reaction vessels of very different sizes); (vi) minerals (as mediators and catalysts); (vii) tidal zones(wetting-drying cycles). Volcanoes probably protruded already from the Earth’s early ocean. This issupported by the basaltic Coonterunah succession in Australia, which represents a record of volcanismand emergent continental crust from the early Archean ca. 3.5 Ga ago (Buik et al., 1995). It seemsplausible that Archean volcanoes were in many respects similar to modern ”hot-spot” islands. Today, apromising place to study a hot-spot volcano is La Reunion Island (Indian Ocean) with its shield volcanoPiton de la Fournaise. In April 2007, on the flank of the Piton de la Fournaise, 7 km away from thesummit in a region called Grand Brule, aa and pahoehoe lavas were released. The lava field resultingfrom this voluminous eruption covers an area of 3.8 square km with a thickness of up to 60 m (Staudacheret al., 2009). Some lava flows of this eruption reached the ocean. As a result of the explosive interactionof lava with seawater, an acidic steam plume was formed, which caused an acidic rainfall with pH valuesless than 2 over the southern part of La Reunion (Bhugwant et al., 2009). Today the lava field is a roughterrain dominated by lava tubes and hard and sharp clinkers, which often contain eye-catching olivineinclusions. These conditions make the Grand Brule a possible analogue site for island volcanoes on youngEarth-like planets and a guide for designing prebiotic simulation experiments.

References:

Bhugwant C, Sieja B, Bessafi M, Staudacher T, Ecormier J (2009) J Volcanol Geotherm Res 184:208-224

Buik R, Thornett JR, McNaughton NJ, Smith JB, Barley ME, Savage M. (1995) Nature 375:574-577

Johnson AP, Cleaves HJ, Dworkin JP, Glavin DP, Lazcano A, Bada JL (2008) Science 322:404

Navarro-Gonzalez R, Segura A (2004) in Origins: Genesis, Evolution and Diversity of Life. Seckbach J(Ed.), Kluwer, Dordrecht, pp. 137-152

Staudacher T, Ferrazzini V, Peltier A, Kowalski P, Boissier P, Catherine P, Lauret F, Massin F (2009)J Volcanol Geotherm Res 184:126-137

Strasdeit H (2010) Palaeodiversity 3(Supplement):107-116; http://www.palaeodiversity.org/pdf/03Suppl/Supplement_Strasdeit.pdf

48

O3.5 Investigating the geochemical composition of early life sig-natures and environment of deposition in highly silicified Ar-chaean cherts - Analytical methods

Axelle Hubert1∗, Frances Westall1, Claire Ramboz2, Alexandre Simionovici3, Laurence Lemelle4, BarbaraCavalazzi5,

1Centre de Biophysique Moleculaire, CNRS, France2Institut des Sciences de la Terre d’Orleans, CNRS, France3Institut des Sciences de la Terre , Grenoble, France4Laboratoire des Sciences de la Terre, ENS Lyon, France5University of Bologna, Italy∗E-mail of corresponding author: axelle.hubert@cnrs-orleans.fr

Some of the earliest traces of life are found in Archaean sediments. The Archean era was characterizedby a silica-rich environment (oceans, hydrothermal activity, volcanic sediments). As a result, sedimen-tary samples from this era that are likely to contain ancient traces of life are highly silicified. Even ifthe silicification allows good preservation of traces of life through geological time ( and through weath-ering, metamorphism), this process also dilutes the organic and elemental signatures in the sample. Theprimary mineralogical composition of these cherts is still recognizable with optical microscope or Ramanspectrometry, in spite of the replacement by silica. Carbon composition can be studied by a variety oftechniques, such as Raman spectrometry, Nano-SIMS, ToF-SIMs, NEXAFS, XANES, or ICP-MS for theisotopic composition. Scanning Electron Microscopy analyses can bring further information on major andminor elements. However, as a result of the dilution by silica, the investigation of the minor and traceelement composition, necessary to learn about the environment of deposition and the signatures peculiarto early life, requires state-of-the art analytical techniques, such as synchrotron X-Ray Fluorescence orParticle Induced X-ray Emission analyses. Although powerful techniques, they are nevertheless sensitiveto this high silica signal. We here propose analytical and data processing methods to avoid silica-signalproblems and highlight the original geochemical signature.

49

O3.6 Sulfur disproportionators as a model of a chemolithoau-totrophic “LUCA”

Kai Finster

∗Biosciences- Microbiology Section, Ny Munkegade 116, Aarhus University, 8000 Aarhus C, Denmark∗E-mail of corresponding author: Kai.Finster@biology.au.dk

The disproportionation of elemental sulfur in which elemental sulfur serves both as electron donor andacceptor and generates simultaneously hydrogen sulfide and sulfate (Bak & Cypionka, 1987; Thamdrupet al., 1993; Finster, 2008) is a fascinating microbiological process at the borderlinein the transition zonebetween biology and geochemistry. Recently, the genomes of the two isolated representatives of the genusıDesulfocapsa were sequenced and the preliminary inspections provide evidence for the presence of thecomplete pathways of sulfate reduction, CO2 fixation via the CODH-pathway thus confirming physio-logical and isotopic studies. Also the genes behind nitrogen fixation are present. In addition, an operonwas identified, which is made responsible for elemental sulfur reduction in representatives of the genusıChlorobium and relatives. The organisms make a living out of this process from a minimum amountof energy and completely rely scavenging of hydrogen sulfide. The process is endergonic under standardcondition with a ∆G0 of +10 KJ per mol of elemental sulfur. Only at hydrogen sulfide concentrationsless then 0.1 mM elemental sulfur disproportionation becomes sufficiently exergonic to support microbialgrowth. In natural environments this may be achieved by removal/scavenging of hydrogen sulfide byFeIII or FeII. The process is carried out by microorganisms affiliated with the metabolic guild of sulfate-reducing bacteria within the genus ıDesulfocapsa (Janssen et al., 1996; Finster et al., 1998; Finster, 2008).Studies of the biochemistry of a few isolates using enzyme assays and sulfur isotope discrimination indi-cate that disproportionating microbes reverse the sulfate reduction pathway during disproportionation.In addition, it has been demonstrated that ıDesulfocapsa sulfexigens shifts to sulfur reduction insteadof disproportionation when hydrogen is supplied as electron donor. Carbon isotope signatures indicatethat CO2 is fixed via the carbon monoxide dehydrogenase (CODH) pathway (Frederiksen & Finster,2003, 2004). Further on the disproportionation of elemental sulfur is accompanied by accelerated pyriteformation, partly through the hydrogen generating “Wachtershauser-reaction” (Canfield et al., 1998).Studies of the isotopic signatures of 3.5 billion year old barium sulfate deposits provided strong evidencefor biological elemental sulfur disproportionation. Thus elemental sulfur disproportionation would beone the oldest documented biological processes on Earth (Philippot et al., 2007). Based on the availablegeological, physiological, biochemical and genetic information the hypothesis is put forward that sulfurdisproprotionating members of the genus ıDesulfocapsa could be studied as models of a chemolithoau-totrophic version of “LUCA”, which meets the complex demands of the early Earth environment.

References:

Bak, F.; Cypionka, H., Nature. 1987, 326, 891.

Canfield, D.E.; Thamdrup, B.; Fleischer, S., Limnol.Oceanogr. 1998, 43, 253.

Finster, K. J. Sulfur Chem. 2008, 29, 281.

Finster, K.; Liesack, W.; Thamdrup, B. Appl. Environ. Microbiol. 1998, 64, 119.

Frederiksen, T.M.; Finster, K. Biodegradation 2003, 14, 189.

Frederiksen, T.M.; Finster, K. Antonie van Leeuwenhoek. 2004, 85, 141.

Janssen, P.H.; Schuhmann, A.; Bak, F.; Liesack, W. Arch. Microbiol. 1996, 166, 184.

Philippot, P.; Van Zuilen, M.; Lepot, K.; Thomazo, C.; Farquhar, J.; Van Kranendonk, M.J. Science2007, 317, 1534.

Thamdrup, B.; Finster, K.; Hansen, J.W.; Bak, F. Appl. Environ. Microbiol. 1993, 64, 119.

50

Student contest I

Tuesday, 16 October 2012:

9:00 Siddharth Hegde: Colors of extreme exoEarth environments

9:15 Jan Marie Andersen: M dwarfs as planet hosts: consequences of stellar activity on exoplanet de-tection

9:30 Aris Vasileiadis: Isotopic Abundances in Evolving, Star-forming Giant Molecular Clouds

9:45 Arkadii Tarasevych: Crystallization and sublimation of non-racemic mixtures of natural aminoacids: a path towards homochirality

10:00 Stefanie Lutz: Cryo-life habitability on a polythermal glacier in Greenland

10:15 Ebbe Norskov Bak: Wind-driven erosion of silicates as a source of oxidants in Martian soil

51

52

SC1 Colors of extreme exoEarth environments

Siddharth Hegde1∗, Lisa Kaltenegger2

1Max Planck Institute for Astronomy, Heidelberg, Germany2Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA∗E-mail of corresponding author: hegde@mpia.de

The search for extrasolar planets has already detected rocky planets and several planetary candidateswith minimum masses that are consistent with rocky planets in the Habitable Zone of their host stars.A low-resolution spectrum in the form of a color-color diagram of an exoplanet is likely to be one of thefirst post-detection quantities to be measured for the case of direct detection.

In this talk, we explore potentially detectable surface features and their connection to and importanceas a habitat for extremophiles, as known on Earth. Extremophiles provide us with the minimum knownenvelope of environmental limits for life on our planet. The color of a planet reveals information onits properties, especially for surface features of rocky planets with clear atmospheres. We use filterphotometry in the visible as a first line of characterization for rocky exoplanets.Many surface environments on Earth have characteristic albedos and occupy a different color space inthe visible waveband (0.4 µm – 0.9 µm) that can be distinguished remotely. These detectable surfacefeatures can be linked to the extreme niches that support extremophiles and provides a link betweengeomicrobiology and observational astronomy. This talk shows that filter photometry can serve as a firstline of characterization for Earth-analog exoplanets for an aerobic as well as an anaerobic atmosphereand prioritizes targets for follow up characterization.

53

SC2 M dwarfs as planet hosts: consequences of stellar activityon exoplanet detection

Jan Marie Andersen1,2∗, Heidi Korhonen2

1Boston University, USA2Centre for Star and Planet Formation, Copenhagen, Denmark∗E-mail of corresponding author: janmarie@bu.edu

In the search for habitable planets, M dwarfs have both been hailed as the Holy Grail of target starsand condemned as unsuitable planet hosts. Their large population (∼ 70% of stars in the Milky Wayare M dwarfs), as well as their low luminosities and temperatures combined with small masses should inprinciple boost the radial velocity signatures of small planets in the “habitable zone”. However, their highlevels of activity could create enough noise to mask a planetary signature and/or render such a planetinhospitable to life. Here, we investigate radial velocity variations caused by different activity patternson M dwarf stars in order to determine the limits of detectability for small planets orbiting active Mdwarfs. We introduce artificial spot patterns on a stellar surface, from which spectral line profiles atdifferent rotational phases of the star are calculated. We include cases for stars with active regions, aswell as random spot distribution, and different spot filling factors. The variations are monitored overa typical stellar activity cycle taking into account spot lifetimes, different rotation rates and spectraltypes, and using different surface differential rotation rates. We investigate the RV noise caused by thesedifferent spot configurations, and compare this to ‘true’ RV variations resulting from orbiting planets.We find that there are cases where activity from the M Dwarf host star can mask the RV signature of ajovian-mass planet with an orbit on the order of tenths of an Astronomical Unit.

54

SC3 Isotopic Abundances in Evolving, Star-forming Giant Molec-ular Clouds

Aristodimos Vasileiadis1,2∗, Ake Nordlund1,2,3, Martin Bizzarro2

1Niels Bohr Institute, Rockefeller Komplekset, University of Copenhagen, Juliane Maries Vej 30, 2100Copenhagen, Denmark2Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen,Østervoldgade 5-7, 1350 Copenhagen Ø, Denmark3Niels Bohr International Academy, University of Copenhagen, Blegdamsvej 17, 2100 Copenhagen, Den-mark∗E-mail of corresponding author: aris@nbi.dk

Meteorites and their components, including calcium-aluminum rich inclusions, the Solar Systemsoldest dated native solids, contain evidence for the former presence of 26Al and 60Fe that has been in-terpreted as proof for abundance at levels that were apparently higher than expected from the galacticbackground (Larsen et al., 2011; Quitte et al., 2007). Additionally, the 26Al/60Fe ratio is well constrainedby space-borne gamma-ray observations (Wang et al., 2007). Those facts have been interpreted as re-flecting a late-stage contamination of the nascent Solar System from a nearby supernova (Cameron &Truran, 1977; Ouellette et al., 2007, 2010). However, the majority of Sun-like stars form in cold anddense molecular cloud regions encapsulated in Giant Molecular Cloud structures, an astrophysical envi-ronment distinctly different from that of the average galactic Interstellar Medium. To better understandthe abundance levels of 26Al and 60Fe in star-forming regions, we used a three-dimensional magnetohy-drodynamic model of a self-gravitating Giant Molecular Cloud to simulate the time-integrated productionand ejection of these radioactive species, and to track their incorporation into star-forming clumps. Wefind that an overall galactic abundance level of 26Al and 60Fe is not necessarily representative of levelsencountered in star-forming regions, where newly born stars and and their encapsulated proto-planetarydisks may inherit local molecular cloud material enriched in freshly synthesized matter by earlier gen-erations of stars. We further demonstrate how variability in isotopic abundances between star-formingregions occurs naturally in our simulations as a consequence of the overall chemical evolution and thephysical properties of Giant Molecular Clouds.

References:

Cameron, A. G. W., & Truran, J. W. 1977, Icarus, 30, 447

Larsen, K. K., Trinquier, A., Paton, C., Schiller, M., Wielandt, D., Ivanova, M. A., Connelly, J. N.,Nordlund, A., Krot, A. N., & Bizzarro, M. 2011, ApJl, 735, L37

Ouellette, N., Desch, S. J., & Hester, J. J. 2007, ApJ, 662, 1268

Ouellette, N., Desch, S. J., & Hester, J. J. 2010, ApJ, 711, 597

Quitte, G., Halliday, A. N., Meyer, B. S., Markowski, A., Latkoczy, C., & Gunther, D. 2007, ApJ, 655,678

Wang, W., Harris, M. J., Diehl, R., Halloin, H., Cordier, B., Strong, A. W., Kretschmer, K., Knodlseder,J., Jean, P., Lichti, G. G., Roques, J. P., Schanne, S., von Kienlin, A., Weidenspointner, G., &Wunderer, C. 2007, A&A, 469, 1005

55

SC4 Crystallization and sublimation of non-racemic mixtures ofnatural amino acids: a path towards homochirality

Arkadii V. Tarasevych1∗, Jean-Claude Guillemin2,

1Institute of Bioorganic Chemistry and Petrochemistry, NAS of Ukraine, Kiev, Ukraine2Institut des Sciences Chimiques de Rennes, Ecole Nationale Superieure de Chimie de Rennes, CNRS,France∗E-mail of corresponding author: arkadiitarasevych@gmail.com

Homochirality of biologically important molecules such as amino acids and sugars is a prerequisite forthe origin of life. There are different forces or mechanisms in the Universe to trigger off the primary im-balance in the enantiomeric ratio. Very likely the initial bias of one type of enantiomers over the other onEarth was arisen from the inflow of extraterrestrial matter (carbonaceous meteorites). The phase transi-tions (crystallization, sublimation) of non-racemic mixtures of enantiomers are ones of the most probablemechanisms for the homochirogenesis [1]. The sublimation, almost uninvestigated subject and forgottenfor 30 years, revealed recently a pathway to the enantioenrichment of natural amino acids [2]. Startingfrom a mixture with a low content of an enantiopure amino acid a partial sublimation gives a considerableenrichment (Fig. 4). In our further experiments we combined two first-order phase transitions of aminoacid(s) mixtures: crystallization and sublimation. The results show the possibility of the transfer ofenantiopurity between different amino acids [3]. Subliming a crystallized mixture of racemic amino acidswith an enantiopure one we found that the sublimate is a non-racemic mixture of the same handednessfor all components (Fig. 5). The significance of the studies can be realized taking into account that just 5of 22 proteinogenic amino acids are able to homochiral self-organization. The relevance of these studies tothe Prebiotic Earth and to the evolution of the single handedness of biological molecules will be discussed.

References:

1. D. G. Blackmond, Phil. Trans. R. Soc. B, 366, 2878 (2011)

2. A. Bellec, J.-C. Guillemin, Chem. Commun., 46, 1482 (2010)

3. A. V. Tarasevych, A. E. Sorochinsky, V. P. Kukhar, J.-C. Guillemin, Chem. Commun., submitted(2012)

Figure 4: Diagrams of changing of enantiomeric excess during partial slow sublimation of non-racemicmixtures of natural amino acids (Ala, Leu, Phe, Pro, Val). •- L+DL, H - L+D mixtures.

56

Figure 5: Deracemization of natural aliphatic AA via ”crystallization - sublimation” protocol.

57

SC5 Cryo-life habitability on a polythermal glacier in Greenland

Stefanie Lutz1∗, Alexandre M. Anesio2, Liane G. Benning1

11 School of Earth & Environment, University of Leeds, UK2School of Geographical Sciences, University of Bristol, UK∗E-mail of corresponding author: s.lutz@leeds.ac.uk

Modern surface glacial ice and snow are extreme environments at the edge of Earth’s biosphere andpotential sites of biosignatures in future planetary missions. The primary colonization of snow and ice isan important biogeological scenario with clear implications for the life detection on other icy planets [1].Hence, knowledge of the adaptations and survival strategies adopted by extremophiles – cryophiles – interrestrial cryogenic environments is vital for our ability to process data from future planetary missions.Despite it being one of the most extreme habitats on Earth, glacial ice and snow-fields are colonised bya plethora of organisms including snow algae, bacteria, fungi, protozoa, rotifers and even invertebrates[2]. Although low in number and diversity compared to other habitats, snow and ice algae are a majorprimary producer in glacial settings [3,4]. Their life cycle influences the structure and diversity of neigh-bouring microbial communities [5] and they produce a suite of complex molecules to protect themselvesagainst cold [6], UV [7], or nutrient deficiency [8]. However, these adaptations are poorly understoodand we know very little about the complexity of the biological inventory contained within snow and iceenvironments. We will present results from an initial study carried out on the polythermal Mittivakkatglacier in SE Greenland. Our aim was to gain a better understanding of the parameters controllingcryo-life habitability signals and start developing a comprehensive cryogenic life signal database. Dueto its Atlantic position, the coastal Mittivakkat Glacier has low average summer temperatures and longice/snow persistence, and its remoteness warrants low levels of contamination from anthropogenic inputs.We characterized the complementary microbiological and geochemical characteristics at a suite of sam-pling sites in the ablation, superimposed and accumulation zone of the glacier. The biological signaturesin various snow and glacial habitats (e.g., snow fields, cryoconites glacial outflow, clean snow) quantifiedvia variations in microbial diversity and distribution using standard microbiological methods combinedwith metagenomic approaches helped investigated the preservation and adaptations of snow algae specificbiosignatures. Furthermore, these were cross correlated with analyses of the main biogeochemical (nu-trients, pigments, lipids, trace metals) and mineralogical characteristics of the solid materials associatedwith each cryogenic habitat.

References:

1. Jakosky et al (2003) Astrobiology, 3: 343-350

2. Anesio, and Laybourn-Parry (2012) Trends Ecol Evol in press

3. Leya et al (2009) FEMS Microbiol Ecol, 67: 432-443

4. Remias et al (2005) Eur J Phycol, 40: 259-268

5. Amato et al (2007) FEMS Microbiol Ecol, 59: 255-264

6. Inglis et al (2006) Cur Protein&Pept Sci, 7: 509-522

7. Holzinger et al (2006) Phycol, 45: 168-177

8. Telling, Anesio et al (2011) J Geophy Res -Biogeosci 116: G03039

58

SC6 Wind-driven erosion of silicates as a source of oxidants inMartian soil

Ebbe Norskov Bak∗, Svend Knak Jensen, Jon Merrison, Per Nørnberg, Kai W. Finster

Mars Simulation Laboratory, Aarhus University, Denmark∗E-mail of corresponding author: ebbe.bak@biology.au.dk

It is unknown which agents are responsible for the oxidizing properties of the Martian soil and howthey are formed. Crushing quartz leads to surface radicals that can create hydrogen peroxide in water.We propose saltation and the resulting erosion of silicates on Mars as a source of oxidants. To simulatethe saltation, we gently tumbled quartz sand under different atmospheres in sealed quartz flasks. Thequarts sand was subsequently analyzed for oxidizing properties. We saw erosion of the quartz sand andaggregations of fine quartz particles within weeks of tumbling. The eroded quartz caused production ofhydrogen peroxide in amounts positively correlated with tumbling time. As long as the eroded quartzwas kept in a dry atmosphere it remained reactive. This process may thus allow for accumulation ofpotentially oxidizing surface radicals on Mars.

Student contest II

Tuesday, 16 October 2012:

11:00 Gayathri Murukesan: Local Martian resources allow efficient cyanobacterial biomass and biohydro-gen production

11:15 Alfonso Delgado-Bonal: Accurate calculations of Ozone and liquid water over Gale Crater

11:30 Mickael Baque: BIOMEX-Desert Cyanobacteria: ground simulations of the EXPOSE-R2 mission

11:45 Petra Schwendner: Monitoring of the microbial community during simulated flight to Mars

59

60

SC7 Local Martian resources allow efficient cyanobacterial biomassand biohydrogen production

Gayathri Murukesan, Taina Laiho, Kirsi Lehto

University of Turku, Finland∗E-mail of corresponding author: gamuru@utu.fi

With the anticipation of manned missions to Mars, new means need to be explored and investi-gated for the production of different life support supplies (oxygen, food and fresh water) for the crews.Long-duration mission to Mars will require high total amount of the supplies, and replenishment of thelife-support supplies from the local Martian resources would be very useful. Water is available on theMartian surface, either in form of the ground water or permafrost and in the polar glaciers, and carbondioxide is abundant in the Martian atmosphere. With sunlight, these substrates can be converted tocarbohydrates and to oxygen, via the photosynthetic process. However, this process requires also mineralnutrients, mainly P, N, K, Ca, which are required in levels that contribute a few percent of the total freshbiomass, plus a set of important micronutrient, which are required in much lower levels, mounting up toabout 0.02% of the produced biomass. These also could be obtained from the local resource, i.e. releasedfrom basaltic regolith, except for N, which is not present in the basalt, and is present in the Martianatmosphere only on 2.7% level. Therefore, recycling of the nitrogenous nutrients becomes essential forstable maintenance of the life-support supplies. It is well established that several cyanobacterial species,e.g. Cynechococcus and Synechocystis, and also the edible Arthrospira sp. thrive well in 100% CO2, in lowpressures (100 mbars or less). In Mars, the air pressure and temperature of the large scale cell-culturefacilities need to be adjusted to some minimal level where the water evaporation can be controlled by sat-urated vapor, but where the temperature still allows adequate cell growth. Such low pressure conditionsalso reduce the toxic or harmful effects that would be caused by high (nearly 100%) CO2 concentrationin high (1 atm) pressure. It is known that certain cyanobacterial species (e.g. Anabaena cylindrical) canreadily grow on rocky surfaces, and particularly on basalt, which has a suitable mineral composition tosupport bacterial growth [1]. Here we report that A. cylindrical thrives well on plain powdered basalt,supplemented by a N-source, also in the high CO2/low pressure atmospheric conditions. The effect of thisatmosphere on the acidification of the growth medium and the bioweathering of the nutrients is currentlyinvestigated. Interestingly, the growth of the A. cylindrical in these low-nitrogen/high CO2 conditions wasfound to induce strong heterocyst formation, associated with strongly enhanced biohydrogen production,providing a potential new form of energy production from this system. For recycling of the nitrogenousnutrients from organic waste it is important that they are bound to some insoluble form, particularlyto prevent the evaporation and leaching of ammonia. At university of Turku, a new vermiculite-basedmineral substrate (GeoTrapRM) has been developed that efficiently absorbs ammonium-ions into its crys-talline structure, and binds also other nitrogenous compounds (nitrate and nitrite) to its surface. Thesebound nitrogen compounds are still available for bioweathering, and are thus easily recyclable to plantnutrient. We have shown that nitrogen-loaded GeoTrapRM serves as a very efficient matrix for supplyingnitrogen to the basalt-based microbial or plant cultures.

References:

1. Olsson-Francis and Cockell, 2010, Planet. Spa. Sci. 58 1279–1285.

61

SC8 Accurate calculations of Ozone and liquid water over GaleCrater

A. Delgado-Bonal∗, F.J. Martın-Torres, E. Simoncini,

Centro de Astrobiologıa (INTA-CSIC)∗E-mail of corresponding author: alfonso.delgado.bonal@gmail.com

The determination of the existence of water on Mars is one of the primary targets in astrobiologydue to the importance of liquid water for life. However, the different thermodynamic conditions are notconsidered in many studies about the abundance of liquid water, leading to wrong calculations of availablewater and related quantities. We have improved a photochemical model for Mars atmosphere with theproper thermodynamical conditions and coupled it with realistic profiles of Temperature and Pressurepreviously calculated with PRAMS GCM. The study is applied to Gale and determine the abundance ofthis compound over the surface. To better model local conditions, we add surface-atmosphere reactions,among Gale minerals and atmospheric gases, in order to calculate the dissipation of free energy due tochemical processes and the actual chemical activity of water in Gale Crater. The existence and reactivityof liquid water on Mars is highly linked with the presence of other compounds in the atmosphere suchas Ozone or OH, and the determination of those also require the thermodynamical studies. Finally,the sorption of water over the surface by physical and chemical processes is reviewed with the newconcentrations,

62

SC9 BIOMEX-Desert Cyanobacteria: ground simulations of theEXPOSE-R2 mission

Mickael Baque1, Daniela Billi1, Jean-Pierre Paul de Vera2

1University of Rome Tor Vergata, Italy2Deutsches Zentrum fur Luft- und Raumfahrt e.V. (DLR), Germany∗E-mail of corresponding author: mickael.baque@gmail.com

Presumably in 2013, new experiments will be performed in space on the EXPOSE facility of theEuropean Space Agency (ESA) attached to the exterior of the International Space Station (ISS). Amongthe selected experiments for the new mission, called EXPOSE-R2, BIOMEX (BIOlogy and Mars EXper-iment) focuses on extremophiles such as lichens, Achaea, cyanobacteria, fungi, bacteria and their cellularcomponents. BIOMEX aims to investigate their resistance when embedded with Martian and lunarmineral analogues. Moreover, resistance of their constituents (biomolecules such as pigments, cell wallcomponents) will be investigated in order to create a biosignature database for the search of life beyondEarth. One of the organisms selected for this experiment is the cyanobacterium Chroococcidiopsis isolatedfrom extremely dry, hot and cold deserts on Earth. Being one of the first phototrophic organisms to ap-pear on the early Earth, its relevance for astrobiology has been assessed in the past years concerning thesearch for life or future space applications (life support systems, biomining). Indeed its resistance to spaceand Martian simulated conditions (Billi et al. 2011) as well as real space exposure (Cockell et al. 2011)along with ionizing radiations (Billi et al. 2000) and prolonged desiccation (Billi 2009) have been alreadyreported. To further decipher the molecular basis of its resistance and protection mechanisms and in thepreparation of the future EXPOSE mission, ground simulations have been performed and the first resultsare being exploited. Chroococcidiopsis strain CCMEE 029 (isolated from Negev desert, Israel) exhibits ahigh survival to the Experiment Verification Tests (EVTs) and Science Verification Tests (SVTs) basedon colony forming ability, integrity of cellular components, like presence of undamaged DNA (assessedby PCR genomic fingerprinting) and permanence of photosynthetic pigments (revealed by CLSM). Newexperimental approaches techniques are being developed in order to complete our understanding of itsextreme resistance.

References:

Billi D, Viaggiu E, Cockell CS, Rabbow E, Horneck G, Onofri S. (2011). Damage escape and repairin dried Chroococcidiopsis spp. from hot and cold deserts exposed to simulated space and Martianconditions. Astrobiology 11:65-73

Billi D. (2009). Subcellular integrities in Chroococcidiopsis sp. CCMEE 029 survivors after prolongeddesiccation revealed by molecular probes and genome stability assays. Extremophiles 13:4957

Billi D, Friedmann EI, Hofer KG, Caiola MG, Ocampo-Friedmann R. (2000). Ionizing-Radiation Re-sistance in the Desiccation-Tolerant Cyanobacterium Chroococcidiopsis. Appl. Environ. Microbiol.66:14891492

Cockell CS, Rettberg P, Rabbow E, Olsson-Francis K. (2011). Exposure of phototrophs to 548 days inlow Earth orbit: microbial selection pressures in outer space and on early earth. ISME J 5:16711682

63

SC10 Monitoring of the microbial community during simulatedflight to Mars

Petra Schwendner1,4∗, Simon Barczyk1, Francesco Canganella2, Viacheslav Ilyin3, Reinhard Wirth4, Har-ald Huber4, Reinhard Rachel4, Petra Rettberg1,

1German Aerospace Center, Institute of Aerospace Medicine, Radiation Biology Department, Cologne,Germany2University of Tuscia, Viterbo, Italy3Institute of Biomedical Problems, Moscow, Russia4Center for Microbiology and Archaea, University of Regensburg, Regensburg, Germany∗E-mail of corresponding author: petra.schwendner@dlr.de

The skin is the largest human organ consisting of 1.8 m2 of diverse habitats and niches. Estimationsrevealed that the human body is colonized by approximately 1014 diverse microbial cells. The majority ofthe skin microbiome (ca. 1013 microbes) is consisting of symbiotic microorganisms that protect the bodyagainst invasion by more pathogenic or harmful microbes which can be of potential danger for humans.Furthermore, prolonged confinement of humans will have influences on the selection, development andcomposition of different microbial populations in closed habitats. These circumstances might lead tochanges in the interactions between microbes and the human. It is unclear if commensally pathogensmight thrive better, spread and accumulate in this confined niche. This effect might lead to an increasedthreat for a weakened person. Additionally, conditions during spaceflight appear to down regulate theimmune system of astronauts. The influence of closed systems on the microbial community is stillunknown and not comparable with natural environments. The here reported survey will deepen theknowledge of the impact of closed systems on the microbial composition.

Mars 500 was the first ground based full duration simulation of a manned flight to Mars from June2010 till November 2011. The crew, six candidates from different countries, lived, worked and performedscientific experiments in this closed habitat where the exchange with the external environment is veryrestricted. This isolation program is a unique opportunity to investigate the impact of confinement onhuman and environmental microbial communities. One of the scientific experiments is called MICHA(Microbial ecology of confined habitats and human health). The aim of the project is the survey of themicrobial flora in different biotopes from the start till the end of the simulation study. During the 520days confinement the natural colonisation and changes over the time (monthly samplings) were monitoredusing different sampling tools. One focus is on the microbial accumulation of selected surfaces via swabsamples, but in addition another point of interest are airborne germs obtained by air filtration. Airsampling included the filtration of 500 l air with 30 l/min on a gelatine filter at nine different locations.Additionally, 25 cm2 of twelve selected surfaces were swabbed. One aliquot of each surface sample wasused to cultivate mesophilic bacteria whereas the other half was heat-shocked for determination of spore-forming and/or heat-resistant strains. The investigation of cultivable microorganisms showed that theoverall bioburden in the air and on different surfaces was moderate compared to other non-confined rooms.The highest number of microorganisms was found in the air of complex EU-150 where the crew membersspent most of their time, i.e. community room, dining area and one tested individual compartment. Thiscorresponds roughly to the results from surfaces at the different locations. First phylogenetic resultsindicate the dominance of microorganisms associated with humans, especially Staphylococcus species,whereas environmental microorganisms are found to a lower extent.

Besides cultivation based analyses, the microbial inventory will be also studied on molecular level viaDNA isolation and 16S rRNA gene specific amplification.

The collection of bioburden and biodiversity data is essential to develop strategies to maintain a non-hazardous environment for the astronauts during long time manned space missions. Furthermore, all ourinvestigations are required for the implementation of planetary protection guidelines for manned Marsmissions.

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Session 4:Cryobiosphere, dedicated to DavidGilichinsky

Tuesday, 16 October 2012:

14:00 Elizaveta Rivkina: Microbial Life within Permafrost (In Memory of David Gilichinsky)

14:30 Sergey Bulat: Assessing microbial life in extreme subglacial Lake Vostok, East Antarctica fromaccretion ice-lake water boundary samples

14:45 Paloma Serrano: Methanogenic archaea from Siberian permafrost: survival in simulated Mars con-ditions and biosignature detection

15:00 Lada Petrovskaya: Structure-functional study of ”permafrost-adapted” proteins

15:15 John Wettlaufer: Ice Growth and Melting Modifications by Antifreeze Proteins

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O4.1 Microbial Life within Permafrost (In Memory of DavidGilichinsky)

Elizaveta Rivkina

Institute of Physicochemical and Biological Problems in Soil Science, Russian Academy of Sciences, Rus-sia∗E-mail of corresponding author: elizaveta.rivkina@gmail.com

Terrestrial permafrost is the only widespread and rich depository of viable ancient microorganismson Earth. In the permafrost environment, cells survive significantly longer than in any other knownhabitat. The age of the isolates corresponds to the longevity of the frozen state of the embedding strata.The oldest known microorganisms date back to the late Pliocene. The existence of the viable Cenozoicmicroorganisms within the permafrost is intriguing as it provides a window into microbial life as it wasbefore the impact of humans. It also serves as a storage for the ancient genetic pool the preexistinglife, which had long since vanished from the Earth surface. The answer to a fundamental question “howlong the life might be preserved” could be found within permafrost natural conservatory of the viablesystems over geological time, where paleoorganisms realize unknown possibilities and unique mechanismsof physiological and biochemical adaptation that allow them to maintain viability over very long periodsof cold climate. Permafrost represents a wide range of possible habitats and inhabitants on the planetswithout obvious surface ice such as Mars. If life existed during the early stages of development on thisEarth-like planet, then, similar to the Earth, remnants of the primitive forms may be found withinMartian permafrost.

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O4.2 Assessing microbial life in extreme subglacial Lake Vostok,East Antarctica from accretion ice-lake water boundary samples

Sergey A. Bulat1∗, Dominique Marie2, Jean-Robert Petit3

1Petersburg Nuclear Physics Institute, St Petersburg, Gatchina, 188300, Russia2Station Biologique de Roscoff, Place Georges Teissier, 29682 Roscoff Cedex, France3LGGE CNRS-UJF, 38402, Grenoble, France∗E-mail of corresponding author: bulat@lgge.obs.ujf-grenoble.fr

The objective was to estimate microbial content of accretion ice originating from frozen water of thesubglacial Lake Vostok buried beneath 4 km thick East Antarctic ice sheet as well as first samples ofthe lake water (RAE57) with the ultimate goal to discover the life in this extreme icy environment. Asa result, the DNA study constrained by Ancient DNA research criteria along with cell enumeration byflow cytometry pointed out that the deepest closest to the ice-water boundary accretion ice (3714 m anddeeper) contains the very low microbial biomass generating no reliable DNA signals and is comparablewith background contamination level (a few cells per ml). The preliminary analyses of the first lake watersamples being frozen on a drill bit at 3769.3 m depth upon the subglacial Lake Vostok entry (February 5,2012) are still in a progress, thus, leaving the possibility the life exists in the most upper water horizonof the lake water column. The findings will be reviewed in the context of what we expect to discover aswell as in terms of astrobiology since the subglacial Lake Vostok settings are thought to be analogous toextraterrestrial icy moons and planets.

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O4.3 Methanogenic archaea from Siberian permafrost: survivalin simulated Mars conditions and biosignature detection

Paloma Serrano 1, Antje Hermelink2, Ute Boettger3, Jean Pierre de Vera3, Dirk Wagner1

1GFZ-German Research Centre for Geosciences, Germany2Robert Koch Institute, Germany3German Aerospace Center (DLR) Berlin, Institute of Planetary Research, Germany∗E-mail of corresponding author: paloma.serrano@gfz-potsdam.de

Methanogenic archaea from Siberian permafrost have proven to be interesting candidates for potentialpast or present life on the Martian subsurface. Several novel strains were recently isolated from the LenaDelta (Russia), which show an anaerobic chemolithotrophic metabolism generating methane gas. They arealso remarkably resistant against desiccation, osmotic stress, low temperatures and starvation. Previousstudies show that these methanogens are able to survive simulated thermo-physical Martian conditionsas well as high doses of UV-C and ionizing radiation, making them exciting candidates for astrobiologicalresearch. As part of the ”Biology and Mars Experiment” (BIOMEX) project in collaboration withESA, this study aims to gain a deeper insight into the response of methanogenic archaea from Siberianpermafrost to simulated Mars conditions on Earth and in space, as well as unveil the biosignatures ofthese microorganisms. For this purpose, a freeze-thaw and a dehydration experiment using Mars regolithand gas analogues have been performed on four different strains, showing differences in the survival rates.On the other hand, the biosignatures of methanogenic archaea are being studied by means of Ramanspectroscopy, a new and powerful approach for describing such signatures. In this first-ever Raman studyon methanogenic archaea, the preliminary results of Fourier-transformed and confocal spectroscopy haveshown that the strain SMA21 (candidatus Methanosarcina gelisolum) shows different spectra dependingon the phase of cell growth, evidencing changes in the cell composition over time, as well as the synthesisof biogenic products.

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O4.4 Structure-functional study of “permafrost-adapted” pro-teins

Lada Petrovskaya1∗, Ksenia A. Novototskaya-Vlasova2, Elizaveta M. Rivkina2, Dmitry A. Dolgikh1,3

1Shemyakin and Ovchinnikov Institute of Bioorganic Chemistry, RAS, Russia2Institute of Physicochemical and Biological Problems in Soil Sciences, RAS, Russia3Moscow State University, Department of Biology, Russia∗E-mail of corresponding author: lpetr65@yahoo.com

To survive in extreme conditions including long-term freezing, cumulative radiation level, high waterosmolarity etc, microbial community of Siberian permafrost utilizes an array of mechanisms including thesynthesis of proteins which can be called “permafrost-adapted” (by analogy with cold-adapted proteins).Characterization of their structural and functional features represents an important contribution to thestudies of adaptation strategies of microorganisms which can be possibly encountered on Mars and othercold planets. Recent genomic sequencing of Exiguobacterium sibiricum, Psychrobacter cryohalolentis andPsychrobacter arcticus opened the possibility of heterologous expression and extensive studies of suchproteins. Several genes coding for potential enzymes (lipases, laccases etc.) with homology to knownbiocatalysts were found in the genomes of Psychrobacter and Exiguobacterium. After their cloning andexpression in E. coli recombinant proteins activity and stability at various conditions were assessed. Wehave shown that several “permafrost-adapted” esterases and lipases display temperature maximum typicalfor their cold-adapted counterparts, but preserve relatively high activity after incubation at elevatedtemperatures (up to 90◦C). Retinal-containing proteins are now known to be present in microorganismswhich occupy nearly all natural environments on Earth, and contribute significantly to global sunlight-driven biomass production. The potential rhodopsin gene predicted in the genome of E. sibiricum (ESR)was expressed heterologously in E. coli membrane. The amino acid sequence of ESR exhibits certainhomology with bacteriorhodopsin, proteorhodopsin and xanthorhodopsin, however, it possesses the uniquestructural feature of a lysine residue in the position corresponding to the proton donor which in all otherknown proton-pumping retinal proteins is occupied with a carboxylic residue. We have shown that ESRphotocycle has several distinctive features, including proton uptake followed by proton release, fast andslow components in M rise and unusual pH dependence. Crystallization experiments aimed at three-dimensional structure investigation of these “permafrost-adapted” proteins are now under way.

The work is supported by Federal Targeted Programme on Scientific and Pedagogical-Scientific Staffof Innovative Russia and RFBR grant 12-05-01085.

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O4.5 Ice Growth and Melting Modifications by Antifreeze Pro-teins

John S. Wettlaufer1,2∗, Maya Bar-Dolev3, Yeliz Celik4, Peter L. Davies5, Ido Braslavsky3,4

1Yale University, USA2NORDITA, Stockholm, Sweden3Hebrew University, Israel4Ohio University, USA5Queen’s University, Canada∗E-mail of corresponding author: john.wettlaufer@yale.edu

Antifreeze proteins (AFPs) protect many organisms in cold climates by controlling the growth of icecrystals within them. A compelling characteristic of AFPs is that the details of ice crystal shapes arespecific to the AFP type. Here, we have demonstrated that the shaping of crystals occurs not only duringgrowth but also during melting. This is particularly striking in so-called hyperactive AFP solutions inwhich the protein exhibits an affinity for the basal plane of ice. The distinction between the ice shapingmechanisms of moderate and hyperactive AFPs has implications for both fundamental understanding ofAFP interactions and to their potential applications.

Session 5:Homochirality

Tuesday, 16 October 2012:

16:00 Francoise Pauzat: Is it possible to enhance homochirality in space?

16:15 Axel Brandenburg: Spatial competition of opposing chiralities

16:30 Søren Toxvaerd: The role of carbohydrates at the origin of homochirality in biosystems

16:45 Coryn Bailer-Jones: Assessing the influence of the solar Galactic orbit on terrestrial biodiversityvariations

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O5.1 Is it possible to enhance homochirality in space?A theoretical study of an enantio-selective adsorption process

Francoise Pauzat

UMPC Universite Paris 06, UMR CNRS 7616, Laboratoire de Chimie Theorique, Paris, France∗E-mail of corresponding author: muzat@lct.jussieu.fr

Life as we know it today seems to need a specific kind of building bricks characterized by a well-definedhomochirality: L-aminoacids, D-sugars and DNA are demonstrative enough examples. Consequently theemergence of biochemical homochirality has to be considered as a key step in the process leading tolife and, has to be elucidated in the early time of this process. Though no chiral molecule has beenidentified so far in the interstellar medium [1,2], encouraging enough is the presence of biological chiralmolecules and of a measurable enantiomeric excess in the organic matter of well-defined families ofmeteorites (carbonaceous chondrites) [3,4]. This is a strong support to the hypothesis of an extra-terrestrial formation of prebiotic elements, then delivered to the Earth by meteorites and comet infalls.

With such a background in mind, we investigated the possibilities linked to the phenomena of selectiveadsorption. We have studied the adsorption of enantiomers on a chiral solid surface, supposed to pre-exist,looking for the parameters that would govern the selectivity of the adsorption/desorption mechanisms.We determined the geometries and the adsorption energies within two types of approaches, the super-molecule and the periodic ones, using methods of quantum chemistry.

The chiral surface was modeled by α-quartz and the main targeted chiral molecules were the α-aminoacids. Tests of the reliability of the methods used as well as that of the modeling of the adsorptionsites, were performed on different molecules, chiral or not, that are constitutive parts of the moleculartargets. In addition to the problem of finding a compromise between the dimension of the solid consideredversus the computational effort, we were confronted to the real versatility of the adsorption energies of amolecule all over the surface and had to rely on a statistical procedure to take into account all possiblesites on a surface.

The results obtained for alanine and lactic acid showing an enantiomeric selectivity will be presentedand the possibilities opened by the exploitation of such computational procedures discussed.

References:

1. http://www.astro.uni-koeln.de/cdms/molecules

2. G. Marloie, M. Lattelais, F. Pauzat, J. Pilme and Y. Ellinger, Interdiscip. Sci. Comput. Life Sci.,2, 48 (2010)

3. J.R. Cronin and S. Pizzarello, Science, 275, 951 (1997)

4. S. Pizzarello and J.R. Cronin, Geochim Cosmochim Acta, 64, 329 (2000)

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O5.2 Spatial competition of opposing chiralities: similarities be-tween biochemical and magnetohydrodynamic processes

Axel Brandenburg1,2∗, Alfio Bonanno3,4, Fabio Del Sordo1,2, Dhrubaditya Mitra1

1Nordita, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden2Department of Astronomy, Stockholm University, SE 10691 Stockholm, Sweden3INAF, Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy4INFN, Sezione di Catania, Via S. Sofia 72, 95123 Catania, Italy∗E-mail of corresponding author: brandenb@nordita.org

A leading theory for the occurrence of complete homochirality of living systems on Earth involvesmutual competition (or antagonism) and auto-catalysis (Frank 1953). These two factors can be iden-tified in various biochemical systems. For example, Sandars (2003) identified mutual antagonism withthe enantiomeric cross-inhibition of nucleotides (Joyce et al. 1984), which is a destructive process anni-hilating pairs of opposite enantiomers. A related process is epimerization in peptides, which can leads tohomochirality in a constructive manner by converting one enantiomer into another (Plasson et al. 2004).Auto-catalysis has also been identified in some chemical systems (Soai et al. 1995), and leads to exponen-tial growth of both chiralities without, on its own, changing the enantiomeric excess (e.e.). The examplesfor nucleotides and peptides have been quantified using kinetic rate equations, which in turn have beenreduced to simple amplitude equations (Brandenburg et al. 2005, 2007). In the very different contextof magnetohydrodynamics, two analogous examples have recently been found: the magnetic buoyancyinstability (Chatterjee et al. 2011) and the Tayler instability (Gellert et al. 2011). For the latter, thesame amplitude equations have been found as in the biochemical case (Bonanno et al. 2012).

The goal of the present work is to explore more deeply this analogy by focussing on spatial aspects.Both for nucleotides and peptides, it has been found that the inclusion of spatial diffusion leads tofront propagation between domains with left- and right-handed molecules. Such fronts propagate inthe direction of the curvature vector (Brandenburg & Multaki 2004), leading thus to a shrinkage ofclosed convex domains. On can therefore easily construct geometric examples where a negative initialenantiomeric excess can become positive, and vice versa. To examine the possibility of a similar processin the magnetohydrodynamic case, we employ three-dimensional simulations of the Tayler instabilitybetween cylinders of inner radius rin and outer radius rout. We adopt a helical perturbation that consistsof a superposition of fields with positive helicities in rin < r < r∗ and negative helicity in r∗ < r < rout,where r∗ is the radius separating the regions of opposite helicity. The results are shown in Fig. 6.

In this work we have compared the evolution of enantiomeric excess in both biochemical and mag-netohydrodynamic case, demonstrating that an initial e.e. of +0.3 can develop into a negative one with

Figure 6: (Right) Shrinkage of initially dominant right-handed chirality (white) in favor of left-handedone (black), leading to a decrease of the e.e. for the same case (middle); and evolution of relative kinetichelicity in the magnetohydrodynamic case (right).

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e.e.=−1 after some time (panels 1 and 2), and that for the Tayler instability initially different helicitieslead to the same sign of helicity (or e.e.) in the end (panel 3). However, there are two caveats to thisresult. Firstly, no 100% e.e. can be produced in the magnetohydrodynamic case, because the magneticfield redistributes with time, shutting off thereby the instability. Secondly, based on the analogy withthe biochemical case, we would have expected the solutions with large values of r∗ to change their signof helicity (as in panels 1 and 2), but the opposite is the case. The reason for this is not entirely clear,but we suspect that it is connected with the global nature of the magnetic field and the importance ofthe Lorentz force that tries to expand the magnetic structures rather than letting them shrink.

References:

Bonanno, A., Brandenburg, A., Del Sordo, F., & Mitra, D., “Breakdown of chiral symmetry duringsaturation of the Tayler instability,” Phys. Rev. E, in press, arXiv:1204.0081 (2012).

Brandenburg, A., Andersen, A. C., Hofner, S., & Nilsson, M., “Homochiral growth through enantiomericcross-inhibition,” Orig. Life Evol. Biosph. 35, 225-241 (2005).

Brandenburg, A., Lehto, H. J., & Lehto, K. M., “Homochirality in an early peptide world,” Astrobiol.7, 725-732 (2007).

Brandenburg, A., & Multamaki, T., “How long can left and right handed life forms coexist?” Int. J.Astrobiol. 3, 209-219 (2004).

Chatterjee, P., Mitra, D., Brandenburg, A., & Rheinhardt, M., “Spontaneous chiral symmetry breakingby hydromagnetic buoyancy,” Phys. Rev. E 84, 025403R (2011).

Frank, F. C., “On spontaneous asymmetric synthesis,” Biochim. Biophys. Acta 11, 459-464 (1953).

Gellert, M., Rudiger, G., & Hollerbach, R., “Helicity and alpha-effect by current-driven instabilities ofhelical magnetic fields,” Monthly Notices Roy. Astron. Soc. 414, 2696-2701 (2011).,

Joyce, G. F., Visser, G. M., van Boeckel, C. A. A., van Boom, J. H., Orgel, L. E., and Westrenen, J.,“Chiral selection in poly(C)-directed synthesis of oligo(G),” Nature 310, 602-603 (1984).

Plasson, R., Bersini, H., and Commeyras, A., “Recycling Frank: spontaneous emergence of homochiralityin noncatalytic systems,” Proc. Nat. Acad. Sci. 101, 16733-16738 (2004).

Sandars, P. G. H., “A toy model for the generation of homochirality during polymerization,” Orig. LifeEvol. Biosph. 33, 575-587 (2003).

Soai, K., Shibata, T., Morioka, H., and Choji, K., “Asymmetric autocatalysis and amplification ofenantiomeric excess of a chiral molecule,” Nature 378, 767-768 (1995).

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O5.3 The role of carbohydrates at the origin of homochirality inbiosystems

Søren Toxvaerd∗

DNRF center, Dept. of Science, Roskilde University, Postbox 260, DK-4000 Roskilde, Denmark∗E-mail of corresponding author: st@ruc.dk

Chiral discrimination ensures that for some molecules there is an energy gain by packing homochiralmolecules together instead of in pairs of enantiomers. A measure of the strength of the chiral discrimina-tion, ∆crH

, can be given as the difference in (standard) formation enthalpies of the two enantiomers.

Experimental data for a series of central and simple molecules in biosystems show that some amino acidsand a simple sugar molecule have a chiral discrimination in favor of homochirality. Models for segregationof racemic mixtures of chiral amphiphiles and lipophiles in aqueous solutions show that the amphiphileswith an active isomerization kinetics can perform a spontaneous break of symmetry during the segrega-tion and self-assembly to homochiral matter. Based on this observation it is argued that biomoleculeswith a sufficiently strong chiral discrimination could be the origin of homochirality in biological systems.

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O5.4 Assessing the influence of the solar Galactic orbit on ter-restrial biodiversity variations

C.A.L. Bailer-Jones∗, F. Feng

Max Planck Institute for Astronomy, Heidelberg, Germany∗E-mail of corresponding author: calj@mpia.de

The fossil record shows that biodiversity has varied considerably over the Phanerozoic eon (past 550Myr). Some investigators have claimed there to be a periodic component in this variation, and havefurther suggested this could arise from the (quasi)-periodic motion of the Sun about the Galactic planeand/or through the spiral arms. However, many researchers have pointed out that methods used toanalyze the data – and even the data themselves – are problematic. We report on two studies in whichwe have investigated this in more detail. First, in order to assess the plausibility of the Sun’s orbitmodulating biodiversity, we have performed a Monte Carlo study of the sensitivity of the periodicity ofthe solar orbit to initial conditions and parameters of the Galactic potential model. A strictly periodicorbit occurs only for an exact circular orbit, or at specific values of the initial conditions which give riseto a resonance between the perpendicular and azimuthal motions. However, a large fraction of orbitsin our simulations are quasi-periodic, with a deviation from strict periodicity of less than 10%. Second,assuming some non-specific mechanism in which the extinction rate is proportional to the local stellardensity, we assess how well different parametrized dynamical models of the solar orbit can explain thefossil record. We calculate the distribution of the likelihood of the extinction record over the modelparameters, and then by marginalizing over the parameters calculate the Bayesian evidence for eachmodel. We find that the evidence is not significantly higher for these dynamical models than it is for asimple stochastic model of extinction. This suggests that the solar orbit, through variations in the localstellar density, has a limited overall impact on the long-term variation of the terrestrial extinction rate.A more detailed investigation continues.

Session 6:Life’s evolution / Extremophiles

Wednesday, 17 October 2012:

9:00 Lynn Rothschild: From Extremophiles to Star Trek, The Use of Synthetic Biology in Astrobiology

9:30 Anthony Poole: Evaluating RNA world relics with comparative genomics

9:45 Sean McMahon: Targeting the Deep Biosphere in the Search for Life

10:00 Ricardo Amils: Iberian Pyrite Belt Subsurface Life (IPBSL), a drilling project of astrobiologicalinterest

10:15 Helga Stan-Lotter: Exposure to low water activity converts Halobacterium rods into small viablespheres - implications for microbial survival in ancient halite

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O6.1 From Extremophiles to Star Trek, The Use of SyntheticBiology in Astrobiology

Lynn Rothschild1∗, Kosuke Fujishima2, Ivan Paulino Lima1, Diana Gentry3,1, Samson Phan3,1, JesicaNavarette2, Jesse Palmer4, Andre Burnier4,

1NASA Ames Research Center, Moffett Field CA 94035-0001, USA2University of California, Santa Cruz and NASA Ames Research Center3Stanford University4Education Associates Program, NASA Ames Research Center∗E-mail of corresponding author: lynn.j.rothschild@nasa.gov

Synthetic biology the design and construction of new biological parts and systems and the redesign ofexisting ones for useful purposes has the potential to transform fields from pharmaceuticals to fuels. Ourlab has focused on the potential of synthetic biology to revolutionize all three major parts of astrobiology:Where do we come from? Where are we going? and Are we alone? For the first and third, syntheticbiology is allowing us to answer whether the evolutionary narrative that has played out on planet earthis likely to have been unique or universal. For example, in our lab we are re-evolving biotic functionsusing only the most thermodynamically stable amino acids in order to understand potential capabilitiesof an early organism with a limited repertoire of amino acids. In the future synthetic biology will playan increasing role in human activities both on earth, in fields as diverse as bio-mining, human health andthe industrial production of novel bio-composites. Beyond earth, we will rely increasingly on biologically-provided life support, as we have throughout our evolutionary history. In order to do this, the field willbuild on two of the great contributions of astrobiology: studies of the origin of life and life in extremeenvironments.

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O6.2 Evaluating RNA world relics with comparative genomics

Anthony M. Poole

University of Canterbury, Christchurch, New Zealand∗E-mail of corresponding author: anthony.poole@canterbury.ac.nz

The RNA world hypothesis, that modern DNA genomes and protein synthesis evolved from RNA-based precursors, has prompted efforts to reconstruct the RNA world by comparing contemporary RNA-based processes. However previous analyses have primarily been derived from literature searches. Wetherefore performed comparative genomic analyses of over 3 million RNA annotations spanning 1446families. We find that 99% of known RNA families are restricted to a single domain of life, with discreteRNA family repertoires for Archaea, Bacteria and Eukaryotes. For the 1% of RNA families/clans presentin more than one domain, over half show evidence of horizontal gene transfer (HGT). While only a fewRNAs are present across all three domains, some families present in two domains may have an earlierorigin, their non-universal distribution being the result of loss from one domain. This has previouslybeen argued for small nucleolar RNAs (snoRNAs), present in Archaea and Eukaryotes, and we soughtto establish whether other indicators are consistent with an RNA world origin. We therefore specificallytested the introns-first hypothesis, which proposes that the location of snoRNAs within the introns ofribosomal genes can be directly traced to the origins of messenger RNA. Briefly this hypothesis is thatintronic snoRNAs predate their surrounding protein-coding exons, the latter being recruited as messengerRNA following the origin of genetically-encoded protein synthesis. Consequently, a historical evolutionarytrace consistent with the introns-first hypothesis would be the stable association between eukaryoticsnoRNAs and their host introns. Our analysis of the evolutionary history of snoRNA families across 44eukaryote genomes reveals that dozens of snoRNA families can be traced back to the Last EukaryoticCommon Ancestor (LECA), and, in agreement with earlier studies, we can trace numerous introns tothe LECA. However, snoRNAs housed within such positionally conserved introns are not themselvesorthologs. Consistent with mobility over antiquity, we present a case of demonstrable intronic snoRNAgain, where an evolutionarily ancient snoRNA has migrated into the intron of a mammalian mitochondrialribosomal protein gene. Together, these data best fit a model wherein snoRNAs are intragenomicallymobile, frequently residing in the introns of broadly-expressed protein-coding genes. In summary, broadcomparative genomic analyses do not broaden the repertoire of RNA world relics. Rather, it seems thatmuch of the intracellular fossil record has been erased by ongoing evolutionary processes.

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O6.3 Targeting the Deep Biosphere in the Search for Life

John Parnell∗, Sean McMahon

School of Geosciences, University of Aberdeen, Aberdeen, UK∗E-mail of corresponding author: J.Parnell@abdn.ac.uk

We are now familiar with the concept of the deep biosphere, in which life inhabits the subsurface ratherthan the surface. On Earth there is evidence for microbial life in sea floor volcanic rocks, in deep aquifers,in deep oil reservoirs, in hydrothermal systems, in the vicinity of buried gas hydrates, and in fracturesystems in crystalline basement rocks (Fig. 7) [1]. In the case of sea floor volcanic rocks, where large porescan survive burial, there is also evidence of eukaryotic life. These are not rare cases of something thathas happened by accident: Estimates of the abundance of life by mass suggest that the deep biospherecould represent up to half of the total. The deep biosphere may also have been fundamental to thedevelopment of life on Earth, as a setting for the earliest life if it was thermophilic, and as a refuge forlife during periods of extensive surface conditions, such as meteorite bombardment or global freezing. Onother planets where surface conditions are extreme for longer proportions of time, including also wherethe surface is not protected from harmful irradiation, a deep biosphere may represent the normal, or only,safe environment. We, as surface dwellers, may be abnormal. If there are indeed millions to billions ofother inhabited worlds, many (most) may be subsurface.

If life elsewhere is subsurface, how will we find it? The sampling of ejecta from the aprons around mete-orite impact craters is already appreciated as a valuable way of accessing samples from depth. Discerningcritical evidence for life in them would probably involve sample return. In the absence of macroscopicfossils, the evidence could include morphological evidence of microscopic life forms, biomolecular evi-dence, and isotopic fractionation. However, this can be difficult even on Earth, where we know that sucha biosphere exists and is abundant, where we can be highly selective in sampling, and where we canundertake the sampling on a repeated basis.

We have started to examine the terrestrial geological record for evidence of a deep biosphere, asa test of how difficult this will be on other planets. Evidence used to deduce microbial activity in thesubsurface includes sulphur isotopic compositions of sulphides, carbon isotopic compositions of diageneticcarbonates, and microfossils in hydrothermal mineral veins. Constraining the depth at which microbialactivity occurred is usually very difficult, but clues can be had from compactional fabrics in sedimentaryrocks, and fluid inclusion temperatures in veins.

A widely proposed environment for microbial life on the early Earth and other planets is in me-teorite impact craters [2]. Positive attributes for craters include hydrothermal circulation of fluids toprovide nutrients, fracture porosity to provide space, and ephemeral high heat flow to cause melting ofice and enhance mineral reactivity. These attributes are conducive to supporting subsurface life in impactcraters. In terrestrial craters, there is rare morphological evidence of microbial life in fracture systems [3].Evidence for pervasive subsurface microbial life has been measured in the Paleocene Haughton ImpactStructure using sulphur isotopic analysis on the sulphide minerals marcasite and pyrite. The sulphidesare widely distributed through the impact melt breccias, and yield isotopic compositions which indicatea fractionation from sulphate that can only be explained by biological activity [4,5]. In mineral veins,marcasite occurs paragenetically before calcite which yields fluid inclusion homogenization temperaturesmostly in the range 70−95◦C. This implies that the microbes which caused microbial sulphate reductionwere thermophilic. The breccia is at least 300 m thick, and most of the microbes must have inhabited thedeep biosphere. The cooling time for the hydrothermal system was about 10’000 years, so colonizationmust have occurred on this timescale. In this case, evidence has survived because a high availability ofsulphate in crater groundwaters has yielded abundant sulphides for sampling. However, it suggests thatmicrobial colonization is a normal aspect of the evolution of an impact crater. Craters therefore offerthe prospect of both exposing pre-existing deep biosphere, and selectively hosting their own subsurface life.

References:

1. J. Parnell et al., International Journal of Astrobiology, 9, 193-200 (2010)

2. C.S. Cockell et al., Astrobiology, 3, 181-191 (2003)

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Figure 7: Schematic cross-section through Earth’s crust, showing settings for deep biosphere microbialactivity. Based on (1).

3. P. Lindgren et al., International Journal of Astrobiology, 9, 137-146 (2010)

4. J. Parnell et al., Geology, 38, 271-274 (2010)

5. J. Parnell et al., International Journal of Astrobiology, 11, 93-101 (2012)

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O6.4 Iberian Pyrite Belt Subsurface Life (IPBSL), a drillingproject of astrobiological interest

Ricardo Amils1,2∗, Vıctor Parro1, David Fernandez-Remolar1, Jose A. Manfredi1, Kenneth Timmis3,Monika Oggerin1, Enoma Omoregie1, Francisco J. Lopez de Saro1, Jose P. Fernandez Rodrıguez1, MonicaSanchez-Roman1, Carlos Briones Llorente1, Felipe Gomez Gomez1, Miriam Garcıa Villadangos1, NuriaRodrıguez1, David Gomez-Ortiz4, Jose L. Sanz5, the IPBSL Team,

1Centro de Astrobiologıa (CSIC-INTA), Torrejon de Ardoz, Spain2Centro de Biologıa Molecular Severo Ochoa (CSIC-UAM), Madrid, Spain3Technical University of Braunschweig, Germany4Universidad Rey Juan Carlos, Madrid, Spain5Departamento de Biologıa Molecular, Universidad Autonoma de Madrid, Cantoblanco, Spain∗E-mail of corresponding author: ramils@cbm.uam.es

The geomicrobiological characterization of Rio Tinto, Iberian Pyrite Belt (IPB), has proven the im-portance of the iron cycle, not only in generating the extreme conditions of acidity and high concentrationof heavy metals of the habitat, but also in maintaining the high level of microbial diversity detected in theecosystem. It has been hypothesized that the extreme conditions found in the Tinto basin are the productof the subsurface chemolithotrophic metabolism of microorganisms thriving on the high concentration ofmetal sulfides (mainly pyrite) of the IPB. To test this hypothesis, a drilling project (IPBSL) is currentlyunder development to provide evidence of subsurface microbial activities and the potential resources tosupport them. A dedicated geophysical characterization of the area selected two drilling sites due to thepossible existence of water with high ionic content. Two wells have been drilled so far in the selectedarea, 340 and 630 meters deep, with recovery of cores and generation of samples in anaerobic and sterileconditions. Preliminary results showed an important alteration of mineral structures associated withthe presence of water, with production of expected products from the microbial oxidation of pyrite. Ionchromatography of water soluble compounds from uncontaminated core samples showed the existenceof putative electron donors (hydrogen, ferrous iron, methane and nitrite in addition of metal sulfides),electron acceptors (ferric iron, sulfate and nitrate) as well as variable concentration of metabolic organicacids (mainly acetate, formate, propionate and oxalate), which are strong indications of the presence ofactive subsurface ecosystems associated to the high sulfidic mineral content of the IPB. The geological,geomicrobiological and molecular biology analysis which are under way, should allow the characterizationof this ecosystem of astrobiological interest.

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O6.5 Exposure to low water activity converts Halobacterium rodsinto small viable spheres - implications for microbial survival inancient halite

Helga Stan-Lotter1∗, Sergiu Fendrihan2, Marion Dornmayr-Pfaffenhuemer1, Friedrich W. Gerbl1

1Division of Molecular Biology, University of Salzburg, 5020 Salzburg, Austria2Romanian Bioresource Centre and Advanced Research Association, 061912 Bucharest, Romania∗E-mail of corresponding author: helga.stan-lotter@sbg.ac.at

Viable extremely halophilic archaea (haloarchaea) have been isolated from million-year-old salt de-posits around the world [1], however, an explanation of their supposed longevity in a desiccated state andin the absence of nutrients remains a profound challenge. Recently small roundish particles of about 0.4 mdiameter in fluid inclusions of about 30,000 year old halite were identified as haloarchaea capable of pro-liferation [2]. Searching for a method to produce such particles in the laboratory we exposed rod-shapedcells of Halobacterium species to reduced external water activity (aw). We observed gradual formation ofspherical particles which occurred in fluid inclusions upon drying of cultures in buffered saturated NaClsolution of aw < 0.75. Exposure to buffered 4M LiCl (aw < 0.73), however, split cells into spheres withinseconds, with concomitant release of several proteins. From one rod, several spheres emerged, which grewout to normal rods in nutrient media [3]. Biochemical properties of rods and spheres were similar, exceptfor a markedly reduced ATP content (about 50-fold lower) and an increased lag phase of spheres, similaras is known from dormant bacteria [3]. The presence of viable particles of identical sizes in ancient fluidinclusions [2] suggested that spheres might represent dormant states of haloarchaea. The production ofspheres by lowering aw is a simple procedure which should facilitate their investigation and might clarifymechanisms for survival of haloarchaea over geological times. Haloarchaea are of particular astrobiologicalinterest since extraterrestrial halite has been identified in Martian meteorites, in the chloride contain-ing surface pools on Mars and in the presumed salty ocean beneath the ice cover of Jupiter’s moon Europa.

References:

1. Fendrihan S, Legat A, Gruber C, Pfaffenhuemer M, Weidler G, Gerbl F, Stan-Lotter H. Extremelyhalophilic archaea and the issue of long-term microbial survival. Reviews in Environmental Scienceand Biotechnology 5, 203218 (2006)

2. Schubert BA, Lowenstein TK, Timofeeff MN, Parker MA. Halophilic Archaea cultured from ancienthalite, Death Valley, California. Environmental Microbiology 12, 440–454 (2010)

3. Fendrihan S, Dornmayr-Pfaffenhuemer M, Gerbl FW, Holzinger A, Grasbacher M, Briza P, ErlerA, Gruber C, Plotzer K, Stan-Lotter H (2012) Spherical particles of halophilic Archaea correlatewith exposure to low water activity - implications for microbial survival in fluid inclusions of ancienthalite. Geobiology (in press).

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Session 7:Astrobiology on the ISS

Wednesday, 17 October 2012:

11:00 Kafila Saiagh: Photostability of prebiotioc organic compounds from Low Earth Orbit experiments,ground laboratory photolysis, and from measurements of absorption vacuum UV (VUV) spectra

11:15 Ralf Moeller: Bacillus subtilis spores in space: what can we learn from gene expression data?

11:30 Yuko Kawaguchi: Resistance of Deinococcus sp. to environmental factors of International SpaceStation (ISS) orbit - Microbes exposure experiment at ISS in the mission ‘Tanpopo’

11:45 Daniela Billi: BOSS-Cyanobacteria: subcellular integrities of Chroococcidiopsis biofilms after spaceand Martian simulations

12:00 Michel Viso: VITRINE: A new orbital facility for Astrobiology, Astrochemistry and Planetology

12:15 Gerda Horneck: Forty years of astrobiology experimentation in space

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O7.1 Photostability of prebiotioc organic compounds from LowEarth Orbit experiments, ground laboratory photolysis, and frommeasurements of absorption vacuum UV (VUV) spectra

Saiagh K.1, Fray N.1, Guan Y.Y.1, Cloix M. 1, Chaput D.2, Cottin H1

1Laboratoire Interuniversitaire des Systemes Atmospheriques (LISA), UMR CNRS 7583, UniversiteParisEst Creteil et Universite Paris Diderot, Institut Pierre Simon Laplace, France2Centre National d’Etudes Spatiales, 18 avenue Edouard Belin, 31401 Toulouse Cedex 9, France∗E-mail of corresponding author: kafila.saiagh@lisa.u-pec.fr

The emergence of life is the final stage of complex processes involving liquid water and organic matter.This organic matter may have been brought on Earth by impact of small bodies (carbonaceous chon-drites and comets) and micrometeorites. The importance of this exogenous contribution is linked to thephotochemical stability of each organic molecule in space conditions. Thus, in order to understand theevolution of organic matter in the solar system, photochemical experiments are conducted both in thelaboratory and in Low Earth Orbit (LEO) on facilities such as EXPOSE-E & -R outside the InternationalSpace Station. These experiments aim to measure photodissociation rates of organic molecules. Suchdata are necessary to model the chemical evolution of specific molecules on a comet dust particle betweenits ejection and its arrival on Earth. Photodissociation rates are controlled by UV and VUV solar radia-tions. To calculate them in these wavelengths, we can use different approaches: (i) direct measurementsin the laboratory or in LEO and (ii) indirect measurements through cross section absorption spectrain the VUV domain. Such absorption spectra are very scarce for solid organic compounds in currentliterature. We will present our newly developed methodology to measure VUV cross section absorptionspectra of thin organic films. Measurements of the VUV spectra for two purines, adenine and guanine,will be presented. Photodissociation rates derived from such measurements will be compared to directmeasurements with laboratory UV lamps, or measurements after direct exposure to the Sun in Low EarthOrbits. Advantages and limits of each method will be discussed.

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O7.2 Bacillus subtilis spores in space: what can we learn from geneexpression data?

Ralf Moeller1∗, Petra Rettberg1, Gerda Horneck1, Gunther Reitz1, Wayne L. Nicholson2

1German Aerospace Center, Institute of Aerospace Medicine, Radiation Biology Department, Cologne,Germany2University of Florida, Department of Microbiology and Cell Science, Space Life Sciences Laboratory,Kennedy Space Center, Florida, USA∗E-mail of corresponding author: ralf.moeller@dlr.de

In a variety of space experiments, spores of Bacillus subtilis have been used as biological dosimetersto determine the effects of extreme environmental conditions of space or simulating Mars [1,2]. Under-standing bacterial spore resistance to radiation, vacuum, heat and chemicals is important in the areasof astrobiology, sterilization and space exploration. Spores of the model organism Bacillus subtilis aremonogenomic, thus there is no protection provided by duplication of genetic information. Spore radiationresistance results from mechanisms of two types: those which (i) prevent DNA damage in the dormantspore and (ii) repair DNA damage during spore germination. During sporulation, spore DNA is sat-urated with a group of unique proteins called ?/?-type small, acid-soluble spore proteins (SASP) [2].SASP binding to DNA changes the DNA from the B-like to the A-like helix conformation, promotingspore photoproduct (SP) formation and suppressing formation of cyclobutane pyrimidine dimers (CPD)in UV exposed spores. DNA reactivity to a variety of other DNA-damaging agents is also dramaticallylowered when DNA is bound by α/β-type SASP. Several additional key factors in the spore core (e.g.lowered pH and water content, and the presence of dipiciolinic acid [DPA]) are also involved in pre-venting DNA damage in dormant spores. However, despite the protection mechanisms provided by thecomponents of the dormant spore, potentially lethal or mutagenic damage can still accumulate in thespore DNA. Germinating spores activate a number of DNA repair pathways dedicated to the removal orrepair of induced lesions. Among these are the SP-specific enzyme SP lyase, the generalized base excisionrepair (BER) and nucleotide excision repair (NER) pathways, recombinational (REC) repair, and thenewly-described non-homologous end joining (NHEJ) pathway for repair of double-strand DNA breaks[2,3,4]. We will present our results from physiological and genetic studies regarding spore resistance toUV and ionizing radiation (from protons, X-rays, and heavy ions) [3,4,5]. Furthermore, we will presentdata from the transcriptome analyses of germinating Bacillus subtilis spores, which were exposed for1.5 years to space and simulated martian conditions in the EXPOSE-E Experiment PROTECT. Uponreturn of the PROTECT experiment, those spores were germinated, total RNA extracted, fluorescentlylabeled, and used to probe a custom Bacillus subtilis microarray to identify genes preferentially acti-vated or repressed relative to ground control spores [6]. Increased transcript levels were detected for anumber of stress-related regulons responding to DNA damage (SOS response, SPb prophage induction),protein damage (CtsR/Clp system), oxidative stress (PerR regulon), and cell envelope stress (SigV reg-ulon). Partially overlapping responses of spores exposed to space and other extreme conditions (e.g.radiation, vacuum) point to the existence of a general ”built-in”-transcriptional germination program inspores with key transcriptional events as checkpoints for ensuring DNA restoration and integrity. In-ternal spore protection mechanisms are established during sporulation, such as Ca2+-DPA-complexes,dehydration, A-DNA conformation, spore coat layers, spore core minerals, DNA binding by SASP andthe synthesis of the DNA repair systems such as spore photoproduct lyase, non-homologous end joining,and apurinic/apyrimidinic endonucleases. Several germination-activated mechanisms such as the reac-tivation of ATP, SAM (S-adenosylmethionine) and macromolecular biosynthesis, activation of SP lyaseand NHEJ enzymes, SOS induction of the REC and NER pathways, active DNA repair of accumulateddamage and de novo nucleotide/nucleic acid synthesis. This concerted interaction of both, protection andrepair, events constitute the major strategy of spores to maintain their high resistance towards a varietyof stresses. The identification of transcriptional and biochemical changes occurring during sporulationand germination has contributed substantially to our understanding of the unique resistance of bacterialspores to astrobiology-relevant conditions.

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References:

1. Horneck G, Klaus DM, Mancinelli RL. (2010) Space microbiology. Microbiol Mol Biol Rev. 74(1):121-56

2. Nicholson WL, Munakata N, Horneck G, Melosh HJ, Setlow P. (2000) Resistance of Bacillusendospores to extreme terrestrial and extraterrestrial environments. Microbiol Mol Biol Rev.64(3):548-72

3. Moeller R, Setlow P, Horneck G, Berger T, Reitz G, Rettberg P, Doherty AJ, Okayasu R, NicholsonWL. (2008) Roles of the major, small, acid-soluble spore proteins and spore-specific and universalDNA repair mechanisms in resistance of Bacillus subtilis spores to ionizing radiation from X raysand high-energy charged-particle bombardment. J Bacteriol. 190(3):1134-40

4. Moeller R, Setlow P, Pedraza-Reyes M, Okayasu R, Reitz G, Nicholson WL. (2011) Role of theNfo and ExoA apurinic/apyrimidinic endonucleases in radiation resistance and radiation-inducedmutagenesis of Bacillus subtilis spores. J Bacteriol. 193(11):2875-9

5. Horneck G, Moeller R, Cadet J, Douki T, Mancinelli RL, Nicholson WL, Panitz C, Rabbow E,Rettberg P, Spry A, Stackebrandt E, Vaishampayan P, Venkateswaran KJ. (2012) Resistance ofBacterial Endospores to Outer Space for Planetary Protection Purposes-Experiment PROTECT ofthe EXPOSE-E Mission. Astrobiology 12(5):445-56

6. Nicholson WL, Moeller R, The Protect Team, Horneck G. (2012) Transcriptomic Responses of Ger-minating Bacillus subtilis Spores Exposed to 1.5 Years of Space and Simulated Martian Conditionson the EXPOSE-E Experiment PROTECT. Astrobiology 12(5):469-86

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O7.3 Resistance of Deinococcus sp. to environmental factors ofInternational Space Station (ISS) orbitMicrobes exposure experiment at ISS in the mission ”Tanpopo”

Yuko Kawaguchi1∗,Yinjie Yang1,Narutoshi Kawashiri1,Keisuke Shiraishi1,Yasuyuki Simizu1, T1,omohiroSugino Yuta Takahashi1, Yoshiaki Tanigawa2, Issay Narumi3, Katsuya Satoh3, Hirofumi Hashimoto4,Satoshi Yoshida5, Kensei Kobayashi6, Kazumichi Nakagawa2, Shin-ichi Yokobori1, Akihiko Yamagishi1,Tanpopo WG

1Sch. Life Sci., Tokyo Univ. Pharm. Life Sci., Tokyo, Japan2Grad. Sch. Human Develop. Environ., Kobe Univ., Kobe, Japan3Japan Atomic Energy Agency / Quantum Beam Science Directorate (JAEA/QuBS), Takasaki, Japan4Japan Aerospace Exploration Agency/ Institute of Space and Astronautical Science (JAXA/ISAS),Tokyo, Japan5Res. Cent. Radiation Protect. NIRS, Ciba, Japan6Grad. Sch. Eng., Yokohama Natl. Univ. Yokohama, Japan∗E-mail of corresponding author: s08756@toyaku.ac.jp

Origin of life on the Earth is one of the most important issues in the biological studies. To explainhow organisms on the Earth were originated in the quite early stage of the history of Earth, Panspermiahypothesis has been proposed [1,2]. Recent findings on the possible microbe fossils of the Martian me-teorite suggested possible existence of extraterrestrial life [3]. Horneck et al. (2008) proposed the viabletransport of microbes via meteorites (lithopansperumia) [4]. We propose that aggregation of microbescould survive to transport interplanetary space [5]. We proposed the ‘Tanpopo’ mission to examinepossible interplanetary migration of microbes, and organic compounds on Japan Experimental Module(JEM) of the International Space Station (ISS) [6]. Tanpopo consists of six subthemes. Two of them areon the possible interplanetary migration of microbes – capture experiment of microbes at the ISS orbitand space exposure experiment of microbes. Dried vegetative cells of D. radiodurans R1,D. geothermalis,and our novel deinococcal species (D. aerius and D. aetherius) isolated from high altitude [7] are thecandidates for the exposure experiment. In addition, some defective mutant strains on the DNA repairsystems , which might affect survivability of cells under these conditions, are candidates. We are nowanalyzing resistance of deinococcal species and strains to the harsh environmental conditions simulatingISS environment (exposure to heavy ion beams such as helium ions and repeated temperature change).The microbial tolerance to heavy ion beams was investigated at National Institute of Radiological Sci-ences Heavy Ion Medical Accelerator in Ciba (HIMAC) under room temperature and normal pressurewith dry cells. We also investigated the microbial tolerance to simulated temperature changes in ISS.Temperature becomes high on the sun side, but very low on the shadow side. Temperature cycles werefor 80◦C to −80◦C in 90 minute, for 60◦C to −60◦C in 90 minutes under 10−1 Pa with dry cells. Thesurvival rates after a year experiment were estimated. Starting from the initial 2.3 · 109 cells, more thanone cell will be recovered after the exposure to the temperature cycle for 60◦C to −60◦C and most ofstrains we tested will be survival after 80◦C to −80◦C temperature cycles. So we concluded all strainwill be appropriate to exposure experiment.

References:

1. Arrhenius, S., Worlds in the Making–the Evolution of the Universe (translation to English by H.Borns) Harper and Brothers Publishers, New York (1908)

2. Crick, F., Life Itself. Simon & Schuster, New York (1981)

3. McKay et al., Science, 273, 924–930 (1996)

4. Horneck et al., Astrobiology, 8, 17–44 (2008) [5] Yang, Y., et al, Biol. Sci. Space, 23, 151–169(2009)

5. Yamagishi, A. et al., Int. Symp. Space Tech. & Sci. (ISTS) Web Paper Archives. 2008-k-05 (2008)

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6. Yang, Y. et al., Int. J. Syst. Evol. Microbiol., 59, 1862–1866 (2009)

7. Yang, Y. et al., Int. J. Syst. Evol. Microbiol., 60, 776–779 (2010)

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O7.4 BOSS-Cyanobacteria: subcellular integrities of Chroococcid-iopsis biofilms after space and Martian simulations

Daniela Billi1∗, Mickael Baque1, Giuliano Scalzi1, Elke Rabbow2, Petra Rettberg2

1University of Rome Tor Vergata, Department of Biology, Rome, Italy2DLR, Institute of Aerospace Medicine, Radiation Biology Department, Koln, Germany∗E-mail of corresponding author: billi@uniroma2.it

BOSS (Biofilm Organisms Surfing Space) is one of the ESA selected international space researchprojects for the next mission EXPOSE-R2, which presumably will launch in 2013 new experiments intospace for a one-year stay on the EXPOSE facility attached to the exterior of the International SpaceStation. The hypothesis will be tested that biofilm form of life with microorganisms embedded andaggregated in their EPS matrix, is better suited to resist harsh environmental conditions as they exist inspace and on Mars, compared to their planktonic counterparts.

BOSS focuses on microorganisms thriving in extreme environments on Earth such as Deinococcusgeothermalis, spores of Bacillus horneckiae, natural biofilms within volcanic rocks, achaea and desertstrains of cyanobacterium Chroococcidiopsis. These cyanobacteria have been selected as a consequence oftheir capability to survive in extreme hot and cold deserts, like the Atacama in Chile and the Dry Valleysin Antarctica, which are considered the closest terrestrial analogs of Mars [1]. These strains have beenalready exposed to space [2] and simulated space and Martian conditions [3]; in addition their suitabilityto genetic manipulation further supports their employment for astrobiology research [4].

Results will be presented on the survival of Chroococcidiopsis biofilms versus planktonic cultures asassessed by cellular and molecular techniques including colony-forming ability, cell membrane integrity,DNA integrity, confocal spectral imaging and photosynthetic performance.

ESA-ILSRA AO-2009 proposals BOSS-Cyano and BIOMEX-Cyano are supported by the Italian SpaceAgency.

References:

1. D. Billi, Anhydrobiotic rock- inhabiting cyanobacteria: potential for astrobiology and biotechnology.In Adaptation of Microbial Life Organisms in Extreme Environments: Novel Research Results andApplication (eds Stan-Lotter H, Fendrihan F) Springer Wien New York, pp119 (2012).

2. C.S. Cockell, P. Rettberg, E. Rabbow and K. Olsson-Francis, Exposure of phototrophs to 548 daysin low Earth orbit: microbial selection pressures in outer space and on early earth. ISME J 5, 1671(2011).

3. D. Billi, E. Viaggiu, C.S. Cockell, E. Rabbow, G. Horneck and S. Onofri, Damage escape and repairin dried Chroococcidiopsis spp. from hot and cold deserts exposed to simulated space and Martianconditions. Astrobiology 11, 65 (2011).

4. D. Billi, Plasmid stability in dried cells of the desert cyanobacterium Chroococcidiopsis and itspotential for GFP imaging of survivors on Earth and in space. Orig Life Evol Biosph in press(2012).

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O7.5 VITRINE: A new orbital facility for Astrobiology, Astro-chemistry and Planetology

Michel Viso1∗, Herve Cottin2, Pascale Chazalnoel3, Michel Villenave3, Didier Chaput3

1Centre national d’etudes spatiales, Paris, France2Universit Paris-Est Creteil, Creteil, France3Centre national d’etudes spatiales, Toulouse, France∗E-mail of corresponding author: michel.viso@cnes.fr

A group of scientist, submitted to the French Space Agency (CNES) a R&D proposal to define a newgeneration of instrument to perform what could be call ”active laboratory astrobiology and astrochem-istry” in orbit. The facilities Expose E and Expose R; built and operated by the European Space Agencyare delivering many results in the field of astrobiology and planetology. A special issue of the journalAstrobiology (12, 5 (2012)) is gathering the most recent results to date. These facilities are exposingdifferent samples ranging from gas mixtures to seeds to the space environment and mainly the radiationsfrom the Sun. Most of the samples are exposed “under” a material (behind a window) which is trans-parent to the UV starting at, or around, the Lyman alpha ray frequency. The experiments are based onground analyses of the samples before and after the exposure as described, amongst others, by Cottinet al. [1], Bertrand et al. [2], Noblet et al. [3]. This procedure is relevant for some experiments butthe past experience already showed that a facility providing permanent data during the exposure wouldtremendously increase the scientific return of these experiments. Based on this preliminary requirements,CNES with the interested scientists defined the preliminary requirements of such an instrument whichcould gather the heritage of the previous Expose facilities as well as the heritage of several instrumentsdeveloped for planetary exploration with the addition of new features. This instrument currently namedVitrine could be flown on a space station as well as on a retrievable capsule or an independent carrierwith appropriate adaptations. The presentation will describe the performances and some of the antici-pated technical solutions to obtain in flight measurement and for some samples, in flight preparation andwindowless exposure to the sun. This project is currently submitted for a phase A study at CNES.

References:

1. Cottin, H. et al., Astrobiology, 12, 5 (2012), pp 412-425

2. Bertrand, M. et al., Astrobiology, 12, 5 (2012), pp 426-435

3. Noblet, A. et al., Astrobiology, 12, 5 (2012), pp 436-444.

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O7.6 Forty years of astrobiology experimentation in space

Gerda Horneck∗

German Aerospace Center, DLR, Institute of Aerospace Medicine, 51170 Cologne, Germany∗E-mail of corresponding author: gerda.horneck@dlr.de

The vast, cold and radiation filled regimes of outer space present on one hand an environmental chal-lenge for any form of terrestrial life; on the other hand they constitute a unique platform for astrobiologyresearch. Major environmental parameters of space that are of interest to astrobiology are (i) space vac-uum, (ii) solar electromagnetic radiation, above all the high energy UV, (iii) galactic cosmic radiation,(iv) extreme temperature fluctuations, and (v) microgravity. These conditions applied individually or inspecific combinations, allow studying several aspects of astrobiology, such as research related to chem-ical evolution, to life’s origin, to life’s evolution, to the habitability of Mars, and to life’s distributionwithin the solar system. Some of those questions cannot easily be studied in Earth-based laboratories.In 1972, Europe became first involved in such studies in space during the Apollo 16 lunar mission, withthe experiment BIOSTACK, conducted under the umbrella of the Council of Europe [1] as well as withthe participation in the Microbial Ecology Equipment Device (MEED) project [2], reviewed in [3]. WithBIOSTACK, that was repeatedly flown (on Apollo 16, 17, Apollo-Soyuz Test Project, LDEF, EURECA,Spacelab 1, D1 and D2) the biological effects of single heavy ions of cosmic radiation were determined fora variety of biological systems, from bacterial spores to plant seeds and insect eggs. It was shown that ahit of a single heavy ion could induce severe genetic alterations, such as mutations, malformations and cellkilling [4]. These data have contributed to assessing radiation hazards for astronauts during exploratorymissions. Inspired by the results of the MEED experiment with bacterial spores as test system, ESAhas initiated an intense research program by providing and operating several space exposure facilities,such as exposure possibilities in the cargo bay of Spacelab missions, the Exobiology Radiation AssemblyERA on the free flying satellite EURECA, 6 BIOPAN missions on Russian retrievable Foton carriers, andfinally three EXPOSE missions with platforms attached to the outside of the International Space Station.During the last 2 EXPOSE missions, the responses of a variety of chemical and biological test systemsto space were studied. Exposing them to selected parameters of the space environment, the followingastrobiological issues were studied (i) dynamic chemistry of prebiotic chemical evolution as it proceedsin the interstellar medium or in the clouds of Saturn’s moon Titan; (ii) stability of organic compoundsand microorganisms under simulated martian surface conditions; (iii) role of solar UV radiation on theevolution of biospheres; (iv) planetary protection issues for surface missions to Mars; and (v) likelihood oflithopanspermia: the interplanetary transfer of life via impact-ejected rocks. The results of EXPOSE-Ehave recently been published in a special issue of the journal Astrobiology [5]. The follow-on missionEXPOSE-R2 will be launched in 2013 to the ISS for a 1 year exposure. In order to address the astrobi-ological issues mentioned above in more detail, several technical improvements have been recommendedfor future astrobiology experiments in space, such as (i) improved simulation of certain extraterrestrialconditions in our solar system, e.g. of planets and moons of our solar system (Mars, Titan), (ii) improvedsimulation of the conditions of the interstellar medium and comets, e.g., with low temperatures, (iii)solar pointing device in order to control the insolation, (iv) on board on-line monitoring of the kinetics ofphotochemical and photobiological reactions, (iv) devices to capture particles of astrobiological interestin Earth orbit.

References:

1. H. Bucker, G. Horneck, Studies on the effects of cosmic HZE-particles in different biological systemsin the Biostack experiments I and II, flown on board of Apollo 16 and 17, in: Radiation Research,O.F. Nygaard, H.I. Adler, and W.K. Sinclair (eds.), Academic Press, pp. 1138-1151 (1975)

2. H. Bucker, G. Horneck, H. Wollenhaupt, M. Schwager, G.R. Taylor. Viability of Bacillus subtilisspores exposed to space environment in the M-191 experiment system aboard Apollo 16. Life Sci.and Space Res. 12: 209-213 (1974)

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3. G. Horneck, D.M. Klaus, R.L. Mancinelli. Space microbiology. Microbiol. Mol. Biol. Rev. 74:121-156 (2010)

4. G. Horneck, Radiobiological experiments in space: A review, Nucl. Tracks Radiat. Meas. 20:185-205 (1992)

5. G. Horneck, M. Zell (guest eds.) Special Collection: The EXPOSE-E Mission. Astrobiology 12:373-528 (2012)

Panel:Pan-European Projects related toAstrobiology

• Felipe Gomez: Astrobiology Road Mapping (AstRoMap) - A project within FP7 of the EuropeanCommission

• Nigel Mason: The Chemical Cosmos, Understanding Chemistry in Astronomical Environments, aCOST project

• Helmut Lammer: EUROPLANET - Astrobiological activities within the European PlanetologyNetwork FP7 Research Infrastructure project

• Jean-Pierre Bibring: From Mars Express to Exomars: ESA goes Astrobiology!

• Christian Muller: The ULISSE project, a step towards long term data preservation and distribution

• Martin Zell: ESA Human exploration and ELIPS programme: Activities related to astrobiology

• Herve Cottin: ESA Astrobiology Topical Team - one year report

• Petra Rettberg: The ESA Topical Team EANA (European Astrobiology Network Association)

• Charles Cockell: Geobiology and Its Space Applications, an ESA Topical Team

• Dag Linnarson: Toxicity of Lunar dust

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PA1 Astrobiology Road Mapping (AstRoMap) - A project withinFP7 of the European Commission

Felipe Gomez1∗, Nicolas Walter2, Gerda Horneck3, Christian Muller4, Petra Rettberg5, Maria T. Capria6,

1Centro de Astrobiologıa (INTA-CSIC), Torrejon de Ardoz, Madrid, Spain2European Science Foundation, Strasbourg, France3Association pour une Reseau Europeen d’Exo/Astrobiology (EANA), France4B-USOC, Brussels, Belgique5Deutsches Zentrum fr Luft- und Raumfahrt (DLR), Cologne, Germany6National Institute for Astrophysics (INAF), Naples, Italy∗E-mail of corresponding author: gomezgf@cab.inta-csic.es

Background: Astrobiology and space exploration have received growing attention within the last phaseof Framework Programme 7 of the European Commission, e.g., with EuroPlaNet (European Planetol-ogy Network), CAREX (Coordination Action for Research Activities on life in Extreme Environments),THESEUS (Towards Human Exploration of Space – a EUropean Strategy) and HAMLET (Human modelMATROSHKA for radiation exposure determination of astronauts). The need for a European Space Ex-ploration Programme is rooted in the European space policy in Article 189 of the TFEU (Treaty of theFunctioning of the European Union) “to support research and technological development and coordinatethe efforts needed for the exploration and exploitation of space.” Noting that Europe has committed toparticipate in the international space exploration initiatives, the Space Advisory Group of the EuropeanCommission recommended that Europe should prepare a European vision for space exploration and in-vest its key competences in this international enterprise [1]. The 5th Call of the European Commissionwithin FP7 invited proposals for research activity roadmaps concentrating on planetary exploration andastrobiology - among other disciplines. Following this call, the proposal ‘AstRoMap’ was formulatedand proposed under the coordination of INTA-CAB, and was accepted by the European Commission.Description of AstRoMap. AstRoMap will be executed within the following four steps:

1. Community consultation. This activity will include the following tasks:

• Reach and expand the astrobiology community in order to perform a wide consultation oncurrent and future research and space activities in astrobiology in relation with AstRoMaproadmap definition process.

• Map the astrobiology and planetary sciences science landscape in Europe and beyond.

• Facilitate networking and exchange of information within the research community

2. Workshops organisation. On the basis of the feedbacks from the community consultation, thepotential participants and interesting topics will be identified. Each workshop will address oneastrobiology topic, specially tailored according to the Astrobiology community needs. Themes ofthe workshops are suggested as follows:

(a) Origin of Solar system

(b) Origin of organic compounds, steps to life

(c) Physico-chemical boundary conditions for habitability

(d) Biosignatures as facilitating life detection

Each workshop will be structured according to the following steps:

• Step: Definition of science goals

• Step: Identification of knowledge gaps – Science and technology

• Step: Suggested missions/instrumentation and experiments to reach the goals

In addition, the following three cross-cutting activities will be discussed during the workshops, ifrelevant:

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• Earth analogues: How Earth analogues can contribute to identify putative extraterrestrialhabitats and technology test?

• Planetary protection: What are the conditions and requirements for planetary protection andplanetary ethics?

• Technology: What new technologies need to be developed for space missions designed to answerthe questions defined in the workshops?

3. Astrobiology road-mapping. Based on the results and major conclusions elaborated during theworkshops, an astrobiology roadmap will be constructed tailed to the European needs and compe-tences.

4. Education and public outreach. Parallel to the workshop and consultation activities, AstRoMapwill provide a comprehensive education and outreach program and disseminate the progress ofAstRoMap through its web site (in progress).

References:

1. G. Horneck, A. Coradini, G. Haerendel, M.-B. Kallenrode, P. Kamoun, J- P Swings., A. Tobias,J.-J. Tortora, Towards a European vision for space exploration: Recommendations of the spaceadvisory group of the European Commission. Space Policy, 26, 109-112 (2010)

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PA2 COST Action CM0805 - The Chemical Cosmos

Nigel J. Mason∗

Dept of Physical Sciences, The Open University, Walton Hall, Milton Keynes, MK7 6AA, United King-dom∗E-mail of corresponding author: n.j.mason@open.ac.uk

This Action aims to bring together European astronomers and planetary scientists to discuss andexplore the chemistry that underpins molecular formation in the interstellar medium and in planetaryatmospheres. The Action is arranged in three ’working groups’; The first is dedicated to ion moleculechemistry and the second to the role of surface chemistry in molecular synthesis. The third workinggroup is of more direct interest to EANA exploring chemistry in planetary atmospheres such as Marsand Titan. Working Group 3 also explores exoplanetary atmospheres and seeks to identify biosignatureswhich may be used to determine whether such planets are habitable (or even inhabited!).The Action has no membership per se rather all researchers in a country which joins the Action are eligibleto attend meetings and apply for funds for Short Term Scientific Missions (STSMs) which support staffexchanges to conduct research. Details can be found on the Action website www.astrochemistry.eu.

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PA3 EUROPLANET - Astrobiological activities within the Eu-ropean Planetology Network FP7 Research Infrastructure project

Helmut Lammer∗

Space Research Institute, Austrian Academy of Sciences, Graz, Austria∗E-mail of corresponding author: helmut.lammer@gmail.com

The EU FP7 funded EUROPLANET project was initiated for demonstrating the advantages of com-bined European research infrastructures so that pan European research projects can be developed. Theproject consist on various networking activities related from Observational Infrastructure Networking(NA1), Science Networking (NA2), Outreach Innovation and Media Service (NA3), Dissemination (NA4),to Joint Research and Transnational Access activities as well as the development of an Integrated andDistributed Information Service (IDIS). The provision of access to research activities and facilities acrossEurope allows the research and development of integrated projects and provides excellent training oppor-tunities for early stage researchers particularly for young scientists which are based in countries whichlack currently a strong planetary science infrastructure. Past and present activities related to and inter-esting to the Astrobiology community and ideas for the sustainability of project related activities in thefuture will briefly be discussed.

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PA4 From Mars Express to Exomars: ESA goes Astrobiology!

Jean-Pierre Bibring∗

IAS (Institut d’Astrophysique Spatiale), Orsay, France∗E-mail of corresponding author: jean-pierre.bibring@ias.u-psud.fr

The Mars Express ESA small mission, although conceived and designed as a small mission, hasand still is acquiring data of utmost relevance to astrobiology: it has enabled an in-depth revisitingof Mars History, and in particular of the role water played in its most ancient times. Specifically, itdemonstrated that Mars once harboured environmental conditions of potential habitability, through theidentification and location of specific minerals. These key discoveries paved the way for the further Marsspace exploration, both from orbit (NASA/MRO) and in situ (NASA/MSL). With Mars Express, ESAentered the Mars space exploration as a major partner, while cementing a strong European space involvedcommunity. For ESA, the follow-on step is to explore one site still hosting minerals and context of thisera, with a dedicated and still unprecedented payload: this is the ExoMars mission, with its roving anddrilling capabilities, still to be confirmed by the end of 2012. It would be highly frustrating and damagingto see the crucial contributions of the Mars European community with no follow-on perspective. On theother hand, if decided, ExoMars would provide key clues to decipher the ancient history of Mars andinner planets, and address the question of life emergence, on Earth and beyond.

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PA5 The ULISSE project, a step towards long term data preser-vation and distribution

Christian Muller∗ and the ULISSE consortium

B-USOC, Brussels, Belgium∗E-mail of corresponding author: christian.muller@busoc.be

ULISSE intends to pursue the exploitation and valorization of scientific data from previous and futurespace science experiments on ISS and on other space platforms, through:

• making available scientific data and knowledge

• increasing information exchange among different components of the scientific community, SpaceAgencies and public bodies.

• implementing services to maximize the exploitation of space experimentation results. The ULISSEdeliverable are: Development of applications (services) to archive, access, analyse space data fromdifferent sources based on the user needs analysis.

• Definition and implementation of a demonstrator of the upgraded capability of the network alsoin support of actions for the dissemination of space culture for educational purposes and publicoutreach.

• Design and implementation of a distributed environment (Middleware platform) for knowledgesharing and cooperation improvement. The ULISSE expected benefits are to Maximise the scientificreturn from space missions by maximizing the exploitation of available data.

• Promote possible applications derived from space experiments results and technologies.

• Increase the public awareness about space research results and benefits involving a wider community.

• Contribute to formation activities in space field also including educational bodies.

The final outcome of the ULISSE demonstration programme as well as its continuation in the ESA LongTerm Data Preservation Programme will be described.

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PA6 ESA Human exploration and ELIPS programme: Activitiesrelated to astrobiology

Martin Zell∗

Directorate of Human Spaceflight and Operations, ESTEC & EAC, European Space Agency, NL-2200AG Noordwijk, The Netherlands∗E-mail of corresponding author: Martin.Zell@esa.int

When ESA’s laboratory module Columbus was attached to the International Space Station in February2008, an external research platform has been deployed with it - the European Technology ExposureFacility (EuTEF). On EuTEF, among several other experiments, was EXPOSE-E, the first of a seriesof Astrobiology experiments performed by ESA under the ELIPS program on ISS. EXPOSE-E returnedin September 2009 after 1.5 years in space, after having been retrieved by astronauts during an EVA.EXPOSE-R followed for a 22 months exposure mission and next year EXPOSE-R2 will be deployed.Later the experiment Oreocube is planned, which will make close to real-time measurements. Thisshort presentation will say a few words about the overall European Life and Physical Sciences in SpaceProgramme (ELIPS), but certainly concentrate on the elements related to astrobiology on ISS.

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PA7 ESA Astrobiology Topical Team - one year report

Herve Cottin1∗, Julia M. Kotler2, topical team members & guests

1Laboratoire Interuniversitaire des Systemes Atmospheriques (LISA), UMR CNRS 7583, Universite ParisEst Creteil et Universite Paris Diderot, Institut Pierre Simon Laplace, France2Leiden Institute of Chemistry, Leiden University, Netherlands∗E-mail of corresponding author: herve.cottin@lisa.u-pec.fr

A Topical Team dealing with astrobiology has been created at ESA. Its goal is to review and discussrecent research in astrobiology, with a special focus to low earth orbit instrumentation, analogue fieldresearch and exploration of the Solar System. The topical team meets twice a year with the objectiveto produce a document that discusses the field of astrobiology in the contexts of space research and alsoprovides recommendations to ESA about anticipated trends and future activities. The Topical Teamenvisions strengthening the role of European scientific expertise as an important user of earth orbitinstrumentation, actor analogue field research and exploration of the Solar System.

Topical team members: Prof. Dr. Charles Cockell, Open University, Milton-Keynes, UK / Dr.Rosa de la Torre Noetzel, INTA, Madrid, E / Dr. Jean Pierre de Vera, DLR, Berlin, D / Prof. PascaleEhrenfreund, Leiden University, Leiden, NL / Dr. Louis D’Hendecourt, IAS, Orsay, F / Dr. Zita Martins,ICL, London, UK / Prof. Dr. Silvano Onofri, Universita della Tuscia Viterbo, I / Dr. Richard Quinn,SETI, Mountain View, USA / Dr. Petra Rettberg, DLR, D / Dr. Antonio Ricco, NASA Ames, MountainView, USA / Dr. K. Slenzka, Jacobs University, Bremen & OHB, D.

Guests: Dr. Elke Rabbow, DLR, D Jack J.W.A. van Loon, Amsterdam University, NL AndreasElsaesser, Leiden Institute of Chemistry, NLESA staff: Oliver Angerer Ren Demets

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PA8 The ESA Topical Team EANA (European AstrobiologyNetwork Association)

Petra Rettberg1∗,Gerda Horneck1,Andre Brack2, Charles Cockell3, Cristiano Cosmovici4, Pascale Ehrenfreund5,Nils G. Holm6, Jan Jehlicka7, Kensei Kobayashi8, Helmut Lammer9, Harry Lehto10, Kirsti Lehto10,Nigel J. Mason11, Christian Muller12, Francois Raulin13, Alan Schwarz14, Helga Stan-Lotter15, EwaSzuszkiewicz16

1DLR, Institute of Aerospace Medicine, Koln, Germany2CNRS, F3Edinburgh University, UK4IFSI-INAF, I5Leiden University, NL6Stockholm University, SE7Charles University in Prague, CZ8Yokohama National University, JP9Austrian Academy of Sciences, AT10University of Turku, FI11The Open University, UK12B.USOC Earth and Space Science Coordination, B13Universites Paris 12 & Paris 7, F14Radboud University Nijmegen, NL15University of Salzburg, AT16University of Szczecin, PL∗E-mail of corresponding author: petra.rettberg@dlr.de

Astrobiology is the study of the origin, evolution and distribution of life in the universe, includingthe Earth. To understand the different aspects of where and how life formed, astrobiology encompassesmany scientific disciplines such as chemistry, biology, palaeontology, geology, atmospheric physics, plan-etary physics and stellar physics. In 2001 the European Astrobiology Network Association (EANA) wasfounded as a scientific non-profit organisation with the purpose to bring together European researchersinterested in that new field of astrobiology, to foster their cooperation also with international partners,to attract students and young scientists and to popularize astrobiology. EANA currently combines rep-resentatives of 19 European nations active in astrobiology: Austria, Belgium, Czech Republic, Denmark,Finland, France, Germany, Greece, Hungary, Italy, Poland, Portugal, Romania, Russia, Spain, Sweden,Switzerland, The Netherlands, United Kingdom. EANA is associated with international astrobiologygroups in Brazil, China, Japan, Mexico and USA (NAI).

In 2011 the ESA Topical Team European Astrobiology Network Association was initiated to foster thecooperation among European astrobiology groups and facilitate the dissemination of information relevantfor those groups. The objectives of this Topical Team EANA are:

• to coordinate the activities of different research groups working on the same topic, bringing togethercomplementary expertise (theoretical, experimental, computational);

• to identify scientific problems for which series of well-defined microgravity/space experiments cangenerate crucial data;

• to identify industries specifically interested in the research planned by the tearm, and to encouragetheir participation in the applications-oriented aspects of the research activities;

• to agree on the best strategy to accomplish a given research goal;

• to define the required experimental programne, including microgravity/space experiments, and toadequately use the different microgravity/space platforms ESA can provide access to;

• to select and define, in close cooperation with ESA, the experiment facilities needed to conductthese flight experiments;

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• to possibly set up a Virtual Institute (within ESA’s Virtual Campus) addressing the Topical Team’spJanned research;

• to apply for research funds in the framewerk of the relevant R&D programmes funded by the EC.

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PA9 Geobiology and Its Space Applications

Charles S. Cockell∗

UK Centre for Astrobiology, School of Physics and Astronomy, James Clerk Maxwell Building, Universityof Edinburgh, Edinburgh, UK∗E-mail of corresponding author: c.s.cockell@ed.ac.uk

Microbe-mineral interactions on the Earth have widespread impacts on global biogeochemical pro-cesses. By dissolving minerals through changes in pH, the secretion of chelators or organic compounds orby changing the redox state of elements within rocks, microbes facilitate nutrient release and accessibilityof rock components. The practical applications of microbe-mineral interactions to space applications arediverse. The rock degrading capability of organisms might be used to release nutrients from local regolithin life support systems to reduce the mass cost in transporting nutrients to planetary bases and they couldbe used in microbial fuel cells to generate a source of electron acceptors. Microbes could also be used toenhance elemental release from rocks in biomining operations. The biomining organism, Acidithiobacillusferrooxidans is shown to be capable of growing and oxidising iron in carbonaceous chrondites, which makeup ∼ 75% of asteroidal material. New experiments proposed for ISS and Cubesats (BIO-ROCK) willlook at water-rock and microbe-rock interactions in space and investigate the potential for organisms tobe used in extraterrestrial industrial processes such as biomining.

References:

1. C.S Cockell. Geomicrobiology Beyond Earth. Trends Ecol. Evol. 18, 308-314

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PA10 Toxicity of lunar dust

Dag Linnarsson1∗, James Carpenter2, Bice Fubini3, Per Gerde4,5, Lars L. Karlsson6, David J. Loftus7,G. Kim Prisk8, Urs Staufer9, Erin M. Tranfield10, Wim van Westrenen11,

1Section of Environmental Physiology, Department of Physiology and Pharmacology, Karolinska Insti-tutet, Stockholm, Sweden2European Space Agency ESTEC, HME-HFR, Noordwijk, The Netherlands3Department of Chemistry and Interdepartmental Center ”G. Scansetti” for Studies on Asbestos andother Toxic Particulates, University of Torino, Torino, Italy4Division of Physiology, The National Institute of Environmental Medicine, Karolinska Institutet, 171 77Stockholm, Sweden5Inhalation Sciences Sweden AB, Scheeles vg 1, 171 77 Stockholm, Sweden6Section of Environmental Physiology, Department of Physiology and Pharmacology, Karolinska Insti-tutet, Stockholm, Sweden7Space Biosciences Division, NASA Ames Research Center, Moffett Field, CA, USA8Departments of Medicine and Radiology, University of California, San Diego, La Jolla, CA , USA9Micro and Nano Engineering Laboratory, Delft University of Technology, Delft, the Netherlands10Cell Biology and Biophysics Unit, European Molecular Biology Laboratory, Heidelberg, Germany11Faculty of Earth and Life Sciences, VU University Amsterdam, Amsterdam, the Netherlands∗E-mail of corresponding author: dag.linnarsson@ki.se

The formation, composition and physical properties of lunar dust are incompletely characterised withregard to human health. While the physical and chemical determinants of dust toxicity for materialssuch as asbestos, quartz, volcanic ashes and urban particulate matter have been the focus of substantialresearch efforts, lunar dust properties, and therefore lunar dust toxicity may differ substantially. In thiscontribution, past and ongoing work on dust toxicity is reviewed, and major knowledge gaps that preventan accurate assessment of lunar dust toxicity are identified. Finally, a range of studies using ground-based, low-gravity, and in situ measurements is recommended to address the identified knowledge gaps.Because none of the curated lunar samples exist in a pristine state that preserves the surface reactivechemical aspects thought to be present on the lunar surface, studies using this material carry with themconsiderable un certainty in terms of fidelity. As a consequence, in situ data on lunar dust properties willbe required to provide ground truth for ground-based studies quantifying the toxicity of dust exposureand the associated health risks during future manned lunar missions.

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Poster abstracts

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P1.01 Space Missions Relevant to Astrobiology

Rene Liseau

Earth and Space Sciences, Chalmers University of Technology, Sweden∗E-mail of corresponding author: rene.liseau@chalmers.se

I will review the status of planned space missions which address both astrophysical and astrochemicalchallenges and which also have astrobiological implications. I will focus, in particular, on missionsdesigned to study exoplanets, exempting solar system objects, but also observatory-type missions withexoplanet detection capabilities. The most important of these include (in alphabetical order) CHEOPS,ECHO, GAIA, JWST, micro-NEAT, PAX, PLATO, SPICA. At the time of writing (June 22, 2012), onlyGAIA (ESA) and the JWST (NASA) are confirmed, with launch dates before 2020.

• CHEOPS: CHaracterizingExOPlanet Satellite, planetary transits, ESA S-mission proposal

• ECHO: Exoplanet CHaracterization Observatory, ESA M-mission proposal

• GAIA: General astrometry mission, ESA, launch in 2013/14

• JWST: Observatory mission, James Webb Space Telescope, NASA, launch in 2018

• micro-NEAT: Planetary astrometry mission, ESA S-mission proposal

• PAX: Planetary Atmosphere Xplorer, planetary spectroscopy proposal for next ESA L-mission call

• PLATO: PLAnetary Transits and Oscillations of stars, ESA M-mission proposal

• SPICA: Observatory mission, Space Infrared Telescope for Cosmology and Astrophysics, Missionof Opportunity M-3 ESA, JAXA

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P1.02 Taxonomy of extrasolar planet: constancy of the classes

Eva Plavalova∗

Comenius University in Bratislava, Slovakia∗E-mail of corresponding author: plavalova@komplet.se

The numbers of extrasolar planets are growing rapidly and some classification (catalogue) mechanismwould be inevitable. The classes for planets have to be quite stable in order to successfully fit intotaxonomy (classification). I discussed the extent of change in the taxonomy classes for planets for whichthe initial data had changed, in the proposal taxonomy by Plavalova (2012). I showed that the datafor planets can change fractionally then the taxonomy class doesnt change radically. Only when planetswith certain characteristics fundamentally changed, the taxonomy class altered radically. I defined theparameters where the change of the initial input data for planets and their parent stars does not changethe taxonomy class radically. I showed that this taxonomy is suitable for implementation in extrasolarplanetary science.

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P1.03 Ground-based Spectroscopy of Exoplanet Atmospheres

Lisa Nortmann∗, Stefan Dreizler

Institut fur Astrophysik, Georg-August-Universitat Gottingen, Germany∗E-mail of corresponding author: nortmann@astro.physik.uni-goettingen.de

While the quest for a habitable exoplanet may start with the discovery of a suitable target it willhave to rely on further investigation of such a target for actual signs of habitability. Suitable targetswould be rocky planets which orbit their host star in a distance that would allow liquid water to existon their surface. It is true that life might also occur in other environments such as sub-surface waterreservoirs beneath thick layers of ice and, thus, not be limited by the occurrence liquid surface water.The interaction, however, that would be possible between surface life and the planet atmosphere is of keyimportance for our chances of detecting life on an exoplanet. While traveling to those distant planets willnot be an option in the foreseeable future their atmosphere can be investigated remotely by measuringtheir reflection and transmission spectra. Such measurements allow us an insight into their atmosphereschemical composition where we might be able to discover evidence for the fingerprints associated withlife.

Transmission spectra can be measured if the planets orbit is aligned to our line of sight in a way thatallows the planet to be seen transiting in front of its host star. During such a transit event part of thestar light will travel though the upper layers of the atmosphere before it reaches the observer.

So far, the precision reachable with the current generation of telescopes and instruments is sufficientto characterize planets with highly extended atmospheres. While most of these potential targets are hotJupiters the used observing method is not limited to those planets and has already been used to probethe transmission spectrum of the highly irradiated Super-Earth GJ1214 b [1].

In order to aid the design of the next generation of instruments that will be able to reach the precisionneeded to probe the atmosphere of rocky and potentially habitable exoplanets it is imperative to applythe existing methods to the planets for which they are currently applicable. This allows us to identifyand study the factors that limit the precision of the measurements and, thus, help us to develop newobserving strategies and improve the existing ones.

In our poster we will explain the observational methods used for exoplanet atmosphere characteri-zation in detail and show results for the transmission spectra of several transiting hot Jupiters. Theseplanet atmospheres were probed in the visible wavelength region between 740–1000 nm where potassium,water and titanium oxide absorption is predicted by theoretical models.

References:

1. J. Bean, E. Miller-Ricci Kempton, D. Homeier, Nature, 468, 669 (2010)

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P1.04 Origin and atmosphere evolution scenarios of Venus, Earthand Mars: Implications for super-Earths

Helmut Lammer1∗, Kristina G. Kislyakova1,2, Petra Odert2, Nikolai V. Erkaev3, Manuel Gudel4, ArnoldHanslmeier2

1Space Research Institute, Austrian Academy of Sciences, Graz, Austria2Institute for Physics/IGAM, University of Graz, Austria3Institute of Computational Modeling, Russian Academy of Sciences, Krasnoyarsk, Russia4Institute of Astrophysics, University of Vienna, Austria∗E-mail of corresponding author: helmut.lammer@gmail.com

The origin and evolution of the atmospheres of early Venus, Earth, Mars and exosolar super-Earthswill be discussed. A focus will be given to the origin and escape of protoatmospheres and further evolutionof secondary atmospheres during a planet’s history. It will be shown that the formation age of a terrestrialplanet, its mass and size, as well as the lifetime in the EUV-saturated early phase of its host star playa significant role in its atmosphere evolution. Scenarios will be presented which indicate how the earlyterrestrial planetary atmospheres most likely evolved through the extreme phase of the young Sun. Itwill also be shown that super-Earths in orbits within the habitable zone of their host stars might haveproblems to lose nebular- or catastrophically outgassed initial protoatmospheres. In such a case theseplanets could end up as water worlds with CO2 and hydrogen- or abiotic oxygen-rich upper atmospheres.If an atmosphere of a terrestrial planet evolves to an N2-rich atmosphere too early in its lifetime, theatmosphere may be lost.

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P1.05 Characterizing exoplanet upper atmosphere-plasma envi-ronments around hot Jupiters and terrestrial exoplanets

Kristina G. Kislyakova1,2,Helmut Lammer1,Mats Holmstroem3,Nikolai V. Erkaev4,Maxim L. Khodachenko1

1Space Research Institute, Austrian Academy of Sciences, Graz, Austria2Institute for Physics/IGAM, University of Graz, Austria3Swedish Institute of Space Physics, Kiruna, Sweden4Institute of Computational Modeling, Russian Academy of Sciences, Krasnoyarsk, Russia∗E-mail of corresponding author: helmut.lammer@gmail.com

For the analyzing of stellar plasma flows around planetary magnetospheres Energetic Neutral Atom(ENA) imaging has become an important remote-sensing tool in planetary science. ENAs are producedwhenever solar- or stellar wind protons interact via charge exchange with a neutral particle from an upperatmosphere of a planetary body so that their signals constrain both, ion distributions and neutral gasdensities. In this study ENA-observations and data interpretations of hydrogen-cloud observations in UVLyman-α absorption around a hydrogen-rich exoplanet HD 209458b is presented. It is discussed how theseobservations together with numerical models can be used for the study of the upper atmosphere structureof planets, the planets magnetospheric shape and information on stellar wind properties. Because thesefactors are relevant for the interaction of between stellar plasma and planetary atmospheres we willalso show that our proposed technique can be applied to terrestrial exoplanets within orbits of M-stars.Detailed analysis of future observations of hydrogen clouds around Earth-type exoplanets will also enhanceour understanding how the atmospheres of terrestrial planets evolve during the extreme active phase ofyoung stars and in case of the Earth through the young Sun period so that the planet could establishhabitable conditions which are the basic environments for the origin of life.

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P1.06 Reconstruction of solar variability during the Holocenebased on 10Be record

Fadil Inceoglu1,2∗,Mads Faurschou Knudsen2, Christoffer Karoff1, Jan Heinemeier1,Margit Schwikowski3,Pierre-Alain Herren3, Anna Sturevik Storm4, Ala Aldahan4, Goran Possnert4

1Department of Physics and Astronomy, Aarhus University, Denmark2Department of Geoscience, Aarhus University, Denmark3Paul Scherrer Institute, University of Bern, Switzerland4Uppsala University, Sweden∗E-mail of corresponding author: fadil@phys.au.dk

The Sun is a magnetically active late type star as well as the main energy source for the atmosphere ofits habitable planet, the Earth. In order to investigate the possible influences of solar activity on Earth’sclimate, and to achieve a comprehensive understanding of changes in the interplanetary magnetic field(IMF) and thus the solar dynamo processes, a better understanding of past variations in solar activityis needed. To investigate the basic relationship between solar variability and climate, it is necessary tofocus on the pre-industrial era when green gas concentrations were relatively constant and during theHolocene when the degree of orbital forcing was relatively small. Moreover, obtaining variations in bothheliospheric index (i.e., IMF) and in this way solar index (i.e., sunspot number) for such a long period willenable investigation of centennial-scale changes in magnetic structures at the solar surface, i.e. sunspots,faculae and magnetic networks, and hence solar dynamo processes. To achieve these objectives, we willconstruct the first high-resolution 10Be record from a non-polar ice core. The Tsambagarav ice core,which spans the last 5–6 millennia, was cored in Mongolia in 2009. The fact that this ice core extends allthe way up to present will make it possible to conduct detailed studies of the link between cosmogenicnuclide production rates, the heliospheric index as well as the solar index, and therefore solar irradiance,during the space age, i.e. the last 50 years. We therefore intend to measure 10Be at an annual, orbi-annual, resolution over the past 50 years, whereas samples will be studied at a 5-year resolution overthe preceding 1,200 years. This will not only enable detailed comparisons to satellite observations of theSun, but also to observations of sunspots over the past 400 years. The overarching objective is to obtaina more comprehensive understanding of changes in solar activity during the last millennium, i.e. aninterval encompassing the Medieval Climate Anomaly (950-1250 AD) and the Little Ice Age (1500–1850AD).

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P1.07 Energetic Neutral Atoms in Planetary Systems

Mats Holmstrom∗

Swedish Institute of Space Physics∗E-mail of corresponding author: matsh@irf.se

We review observations of energetic neutral atoms (ENAs) in the Solar System. This is done with afocus on the populations that could be remotely observed in other stellar system, and we present howLyman-alpha (Ly-a) observations of transiting extrasolar planets could detect ENAs near these planets.We also discuss the problems and uncertainties in interpreting such transit spectra. Finally, we concludewith an outlook to future observations, and possible directions in modeling.

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P1.08 Colors of extreme exoEarth environments

Siddharth Hegde1∗, Lisa Kaltenegger2

1Max Planck Institute for Astronomy, Heidelberg, Germany; hegde@mpia.de2Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA∗E-mail of corresponding author: hegde@mpia.de

The search for extrasolar planets has already detected rocky planets and several planetary candidateswith minimum masses that are consistent with rocky planets in the Habitable Zone of their host stars.A low-resolution spectrum in the form of a color-color diagram of an exoplanet is likely to be one of thefirst post-detection quantities to be measured for the case of direct detection.

In this talk, we explore potentially detectable surface features and their connection to and importanceas a habitat for extremophiles, as known on Earth. Extremophiles provide us with the minimum knownenvelope of environmental limits for life on our planet. The color of a planet reveals information onits properties, especially for surface features of rocky planets with clear atmospheres. We use filterphotometry in the visible as a first line of characterization for rocky exoplanets.Many surface environments on Earth have characteristic albedos and occupy a different color space inthe visible waveband (0.4 µm – 0.9 µm) that can be distinguished remotely. These detectable surfacefeatures can be linked to the extreme niches that support extremophiles and provides a link betweengeomicrobiology and observational astronomy. This talk shows that filter photometry can serve as a firstline of characterization for Earth-analog exoplanets for an aerobic as well as an anaerobic atmosphereand prioritizes targets for follow up characterization.

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P1.09 M dwarfs as planet hosts: consequences of stellar activityon exoplanet detection

Jan Marie Andersen1,2∗, Heidi Korhonen2

1Boston University, USA2Centre for Star and Planet Formation, Copenhagen, Denmark∗E-mail of corresponding author: janmarie@bu.edu

In the search for habitable planets, M dwarfs have both been hailed as the Holy Grail of target starsand condemned as unsuitable planet hosts. Their large population (∼ 70% of stars in the Milky Wayare M dwarfs), as well as their low luminosities and temperatures combined with small masses should inprinciple boost the radial velocity signatures of small planets in the “habitable zone”. However, their highlevels of activity could create enough noise to mask a planetary signature and/or render such a planetinhospitable to life. Here, we investigate radial velocity variations caused by different activity patternson M dwarf stars in order to determine the limits of detectability for small planets orbiting active Mdwarfs. We introduce artificial spot patterns on a stellar surface, from which spectral line profiles atdifferent rotational phases of the star are calculated. We include cases for stars with active regions, aswell as random spot distribution, and different spot filling factors. The variations are monitored overa typical stellar activity cycle taking into account spot lifetimes, different rotation rates and spectraltypes, and using different surface differential rotation rates. We investigate the RV noise caused by thesedifferent spot configurations, and compare this to ‘true’ RV variations resulting from orbiting planets.We find that there are cases where activity from the M Dwarf host star can mask the RV signature of ajovian-mass planet with an orbit on the order of tenths of an Astronomical Unit.

119

P1.10 Where is the carbon gas in the debris disk around β Pic-toris located?

Gianni Cataldi1,2∗, Alexis Brandeker1,2

1Department of Astronomy, Stockholm University, Stockholm, Sweden2Stockholm University Astrobiology Centre, Stockholm, Sweden∗E-mail of corresponding author: gianni.cataldi@astro.su.se

Circumstellar debris disks consist mostly of dust and planetesimals leftover from the protoplanetaryphase. They are gas-poor, in contrast to protoplanetary disks, but gas can still be detected. However,this gas is probably not just leftover protoplanetary material, but is thought to be produced by collidingdust grains (Czechowski & Mann 2007) or through photodesorption of dust (Chen et al. 2007; Grigorievaet al. 2007). If the gas indeed originates from the dust, observations of the gas could reveal interestingfacts about the chemical composition and the physical properties of the dust (Zagorovsky et al. 2010).It is even conceivable that something can be said about the composition of potentially present planets.The debris disk of the young star β Pictoris is one of the most prominent we know and has been observedextensively. A main motivation for these observations is the possibility of learning more about the earlyphase of our own solar system (by viewing the β Pictoris system as an analogue) and to put constraintson the mechanism of planet formation (Brandeker et al. 2004). Both issues are obviously of high astro-biological relevance.Metallic gas has been seen in Keplerian orbit around β Pictoris (Olofsson et al. 2001) and the distributionin the disk of some elements of the gas (Na, Fe, Ca, Cr, Ti, Ni) has been observed (Brandeker et al.2004). The location of the carbon component (which is the dominant component by mass) remainedhowever obscure.We obtained a high resolution spectrum of the carbon gas emission (CII line at 157 µm) with the HIFIinstrument on the infrared space telescope Herschel. Since the gas is known to be in a Keplerian orbitaround β Pictoris, and since we see the disk edge-on, we can investigate the line profile of the emissionspectrum to constrain the location of the carbon gas. This will give clues about the origin of the gas andits possible interaction with the giant planet orbiting β Pictoris at a distance of about 10 AU. It will alsocontribute to a better understanding of debris disks in general.Our first results show that the observations are consistent with a carbon gas distribution derived fromprevious observations of other metallic gas species, but that there is possibly more carbon gas at largedistances from the star than anticipated.

References:

Brandeker A., Liseau R., Olofsson G. and Fridlund M., A&A, 413, 681 (2004)

Chen C.H., Li A., Bohac C. et al., ApJ, 666, 466 (2007)

Czechowski A. and Mann I., ApJ, 660, 1541 (2007)

Grigorieva A., Thebault P., Artymowicz P. and Brandeker A., A&A, 475, 755 (2007)

Olofsson G., Liseau R. and Brandeker A., ApJ, 563, L77 (2001)

Zagorovsky K., Brandeker A. and Wu Y., ApJ, 720, 923 (2010)

120

P1.11 Spectral Synthesis for Protoplanetary disk models

Samuel Regandell1∗, Susanne Hofner1, Wladimir Lyra2,3, Nikolai Piskunov1

1Department of Physics and Astronomy, Uppsala University, SE751 20 Uppsala, Sweden2Department of Astrophysics, American Museum of Natural History, New York, NY 10024, USA3Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA91109, USA∗E-mail of corresponding author: samreg@astro.uu.se

The physical properties and dynamics of protoplanetary disks define the environment for formationand early evolution of planetary systems. Unfortunately today it is not yet possible to resolve theinner parts of circumstellar disks in order to study their physical properties and observe planet formationdirectly. Instead we rely on numerical simulations to explain the diversity of known exoplanetary systemsand their relations to the properties of the parent dust-gas disks. Disk models come in two flavours:(magneto-)hydrodynamic simulations of the whole disk or so-called ”sheering box” simulations. The twoare complementary in terms of spatial resolution and realistic boundary conditions but also share somerestrictions. In particular, it is hard to incorporate realistic opacities and energy transport by radiationin 3D simulations. These features are the key components for getting the correct vertical stratification ofa disk and to produce meaningful synthetic observables that can be directly compared with observations.These restrictions do not apply to 1D and ”1.5”D simulations where all relevant microphysics can oftenbe included in as much details as possible. ProDiMo is one such tool and the corresponding simulationswere presented by Woitke et al. 2009.

One aspect rarely covered by modelling is deviations from axisymmetry. Such deviations are indicativeof various extra perturbations on the disk structure. Examples include the disk being perturbed byparent stars, protoplanets forming, or disk instabilities. From probability arguments disk disruptions bya neighbouring star is highly unlikely, even in a dense cluster (Williams and Cieza 2011). Disk instabilitiesdo exist in dense-enough regions of the disk but on larger scales the formation of protoplanets shouldlikely dominate the deviation from axisymmetry by forming gaps (e.g. (Wolf et al. 2007).

In this work we present a pipeline combining the tracing of disk dynamics (including the feedbackfrom forming planets) and detailed physical modelling including non-grey radiative transfer across anon-axisymmetric disk. The modelling presented here starts from a “snapshot” of a 3D magneto-hydrodynamic (MHD) model of a disk (Lyra et al. 2009) that is then refined locally through constructinga hydrostatic disk profile (in the direction perpendicular to the disk middle plane) taking into accountthe global radiation field from the disk and the central star. This approach lacks self-consistency butthe volume occupied by the disk is mostly optically thin and the (vertical) sound crossing time is muchshorter than the period of Keplerian rotation. The result from these simulations are used as input ahigh-resolution raytracing routine for outputting model observables for comparing with observations.

References:

Woitke, P. Kamp, I. & Thi, W.-F. “Radiation thermo-chemical models of protoplanetary disks. I. Hy-drostatic disk structure and inner rim”, A&A 501, 383–406 (2009)

Lyra, W., Johansen, A., Klahr, H., & Piskunov, N. “Global magnetohydrodynamical models of turbu-lence in protoplanetary disks. I. A cylindrical potential on a Cartesian grid and transport of solids”,A&A, 479, 883–901 (2009)

Williams, J. P., & Cieza, L. A., “Protoplanetary Disks and Their Evolution”, Annual. Rev. 49, 67–117(2011)

Wolf, S., Moro-Martın, A. & D’Angelo, G., “Signatures of planets in protoplanetary and debris disks”,Plan. and Space Sci., 55, 693 (2007)

121

P1.12 Polarimetric effects simulation for HD189733

Kateryna Frantseva1, Nadia M. Kostogryz2, Taras M. Yakobchuk2

1Taras Shevchenko National University of Kyiv, Ukraine; gagarinfff@gmail.com1Main Astonomical Observatory of the National Academy of Sciences, Ukraine∗E-mail of corresponding author: gagarinfff@gmail.com

The main idea of our simulations is the famous effect that the polarization of centrosymmetric unre-solved stars is zero and during the planet transiting or spot appearing on the host star, the symmetryis broken that results in partial polarization. We have simulated the flux and polarization in differentfilters (U, B, V, R, I) for HD189733 system at this work. A Monte-Carlo method for the simulation ofthe polarization that occurs at the planet’s transit was used. As the host star is active and spots maycover up to 1% of planetary surface, we simulated the flux and Stokes parameters for linear polarizationand polarization degree for different spot parameters such as size and location on the stellar disk and thetemperatures.

122

P1.13 Isotopic Abundances in Evolving, Star-forming Giant Molec-ular Clouds

Aristodimos Vasileiadis1,2∗, Ake Nordlund1,2,3, Martin Bizzarro2

1Niels Bohr Institute, Rockefeller Komplekset, University of Copenhagen, Juliane Maries Vej 30, 2100Copenhagen, Denmark2Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen,Østervoldgade 5-7, 1350 Copenhagen Ø, Denmark3Niels Bohr International Academy, University of Copenhagen, Blegdamsvej 17, 2100 Copenhagen, Den-mark∗E-mail of corresponding author: aris@nbi.dk

Meteorites and their components, including calcium-aluminum rich inclusions, the Solar Systemsoldest dated native solids, contain evidence for the former presence of 26Al and 60Fe that has been in-terpreted as proof for abundance at levels that were apparently higher than expected from the galacticbackground (Larsen et al., 2011; Quitte et al., 2007). Additionally, the 26Al/60Fe ratio is well constrainedby space-borne gamma-ray observations (Wang et al., 2007). Those facts have been interpreted as re-flecting a late-stage contamination of the nascent Solar System from a nearby supernova (Cameron &Truran, 1977; Ouellette et al., 2007, 2010). However, the majority of Sun-like stars form in cold anddense molecular cloud regions encapsulated in Giant Molecular Cloud structures, an astrophysical envi-ronment distinctly different from that of the average galactic Interstellar Medium. To better understandthe abundance levels of 26Al and 60Fe in star-forming regions, we used a three-dimensional magnetohy-drodynamic model of a self-gravitating Giant Molecular Cloud to simulate the time-integrated productionand ejection of these radioactive species, and to track their incorporation into star-forming clumps. Wefind that an overall galactic abundance level of 26Al and 60Fe is not necessarily representative of levelsencountered in star-forming regions, where newly born stars and and their encapsulated proto-planetarydisks may inherit local molecular cloud material enriched in freshly synthesized matter by earlier gen-erations of stars. We further demonstrate how variability in isotopic abundances between star-formingregions occurs naturally in our simulations as a consequence of the overall chemical evolution and thephysical properties of Giant Molecular Clouds.

References:

Cameron, A. G. W., & Truran, J. W. 1977, Icarus, 30, 447

Larsen, K. K., Trinquier, A., Paton, C., Schiller, M., Wielandt, D., Ivanova, M. A., Connelly, J. N.,Nordlund, A., Krot, A. N., & Bizzarro, M. 2011, ApJl, 735, L37

Ouellette, N., Desch, S. J., & Hester, J. J. 2007, ApJ, 662, 1268

Ouellette, N., Desch, S. J., & Hester, J. J. 2010, ApJ, 711, 597

Quitte, G., Halliday, A. N., Meyer, B. S., Markowski, A., Latkoczy, C., & Gunther, D. 2007, ApJ, 655,678

Wang, W., Harris, M. J., Diehl, R., Halloin, H., Cordier, B., Strong, A. W., Kretschmer, K., Knodlseder,J., Jean, P., Lichti, G. G., Roques, J. P., Schanne, S., von Kienlin, A., Weidenspointner, G., &Wunderer, C. 2007, A&A, 469, 1005

123

P1.14 Modeling the evolution of molecular clouds as a functionof metallicity

Eduardo M. Penteado1,∗, Herma M Cuppen1, Helio J Rocha-Pinto2

1Radboud University Nijmegen, Institute for Molecules and Materials, Nijmegen, Netherlands2Universidade Federal do Rio de Janeiro, Observatorio do Valongo, Rio de Janeiro, Brazil∗E-mail of corresponding author: eduardo@science.ru.nl

Stars form from the collapse of dense molecular clouds and may result in planetary systems with pos-sibly planets located in the habitable zone. This process is probably influenced by the material availableat the moment of the molecular clouds collapse. Since new elements produced by the stars are constantlydelivered to the interstellar medium, the formation of new generations of planetary systems may be influ-enced by this enrichment of metallicity. This work describes the role of the change on metallicity for thegas phase chemistry of the interstellar medium, by varying the initial elemental abundance, taken fromTimmes et al. (1995), an astrochemical model for the molecular evolution of clouds. Results show thatthe variation of metallicity has a strong effect on carbon chain length: the final abundances of moleculeswith larger carbon chain decrease as the metallicity increases. This is mostly due to the change in theC/O ratio. The chemical timescales of molecular clouds are also effected: the overall abundance of simplemolecules tend to be higher for solar metallicity and the steady state tends to be reached earlier forpoor metallicities then to solar metallicity, which suggest that molecular clouds of higher metallicitiesmay collapse before steady state is reached. Molecules are preferentially destroyed after 105 years of themolecular cloud’s lifetime, which means that the peak of abundance is reached before this time. Metallic-ities between -0.5 and 0.0 present the highest percentages of molecules being destroyed for all moments,except around 105 years.

References:

Timmes, F. X., Woosley, S. E., Weaver, T. A., The Astrophys. J. Suppl. Ser., 98, 617-658 (1995)

124

P1.15 SETV: A new frontier for SETI

Eamonn Ansbro∗

Kingsland Observatory, Ireland∗E-mail of corresponding author: eansbro@eircom.net

The recent surge of interest in SETV has been no surprise in light of the research findings of theHessdalen Project. In the absence of results from conventional SETI approaches, the logic of wideningthe search strategy and bringing adequate scientific resources to the near Earth search is increasinglycompelling. Recent literature in SETV research has already shown data that is interesting and puzzlingand does not seem to indicate known natural or man-made sources. This new frontier of SETI requiresa ground-based approach with astrophysical methodologies and analysis of a new and complex nature.There are inherent challenges when dealing with any new phenomenon and in particular testing newtheories. In particular, ETI interstellar probes may take forms that would not be recognized by us astechnological. Ongoing analysis of data already obtained is necessary for further refining the range ofequipment, taking into consideration the nature of multi-frequency instrumentation that will produce themost significant data and represent the best use of available funds. (Ansbro & Overhauser, 2001) Theinstrumentation already developed and operational at Kingsland Observatory is a significant modificationof the commercial-off-the-shelf approach to SETV as suggested by others. Search for ExtraterrestrialVisitation or SETV is aimed at searching for evidence of visiting ET probes, possibly of a robotic type,within a radius of 50 astronomical units with Earth at its center. The range of search targets could bein the regions of the Earth-Moon libration points, the asteroid belt, the Moon and the circumlunar andcircumterrestrial orbits. As there is no scientific proof that Earth has been visited, the SETV strategyconsiders the possibility of monitoring Earth with specifically developed instruments. The existence ofET robotic probes, could appear as anomalies in our atmosphere, such as an anomalous observationalphenomena (AOP) in the form of non-luminous or luminous phenomena. About 30 of the areas of Earthhave been identified to experience sustained AOP activity for several years or even decades. One of themost important regions is Hessdalen in Norway. The SETV search strategy is to detect ET probes. Toaccomplish this goal, we must define ET probe type, in measurable terms, and strive to understand thenature of possible ET probes observed from the physics that we understand. The choice of solar systemtarget to search will determine the conception, design and development of the proposed instrumentation.In the case of AOPs within our Earths atmosphere this paper will describe the design of instrumentationthat not only has the potential of recording meaningful scientific data but also can include application ofthe SETV hypothesis as a possible corollary.

125

P2.01 Pyrophosphate Synthesis in a Proton Gradient Across IronSulfide Membranes Simulating Hadean Submarine HydrothermalSystems

Laura Barge

Caltech/Jet Propulsion Laboratory, USA∗E-mail of corresponding author: laura.m.barge@jpl.nasa.gov

The availability of a pyrophosphate ‘energy carrier’ molecule in prebiotic systems is one of the mostimportant considerations for the origin of life. It is thought that pyrophosphate (PPi) would haveserved as the earliest version of ATP/ADP in the first metabolizing entities (Baltscheffsky et al. FEBSLett. 457, 527), and may have been synthesized inorganically, e.g. by mineral reactions in hydrothermalenvironments driven by thermal and/or ionic gradients in conditions of very low water activity. We havedemonstrated the formation of PPi from acetyl phosphate and inorganic phosphate assisted by catalyticiron minerals in a simulated alkaline hydrothermal vent scenario. We show temperature dependentsynthesis (and stability) of PPi with various catalysts, and also demonstrate large yields of PPi in ironsulfide membranes separating acidic and alkaline solution, perhaps indicating the influence of an ambientproton motive force. The synthesis of PPi and ATP in a proton (or sodium) gradient is significantsince modern biochemistry generates a pH (or Na+) difference across membranes through oxidativephosphorylation so that as the protons flow back down gradient through an ATPase or PPase theyproduce pyrophosphate energy storage molecules. Our results suggest that a similar polarity of naturalproton gradient may have assisted in the production of pyrophosphate in submarine alkaline hydrothermalvent systems.

126

P2.02 Low pH Geothermal Chemistry on the Vatnajokull Glacier.Provision of Activated Phosphorus on the Early Earth

Barry Herschy1∗, Tasnim Munshi2, Ian Scowen2, David Greenfield3, Matthew A. Pasek4, Claire Cousins5,Ian Crawford5, Terence P. Kee1∗

1School of Chemistry, University of Leeds, Woodhouse Lane, Leeds, LS2 9JT, UK2School of Life Science, University of Bradford, Richmond Road, Bradford, BD7 1DP, UK3Centre for Corrosion Technology, Materials and Engineering Research Institute, Sheffield Hallam Uni-versity, Sheffield, S1 1WB, UK4Department of Geology, University of South Florida, Tampa, FL 33620, USA5Department of Earth and Planetary Sciences, Birkbeck College, University of London, Gower Street,WC1E 6BT, UK

∗E-mail of corresponding author: t.p.kee@leeds.ac.uk

Described here are our studies on the hydrothermal modification of the type IIAB iron meteoriteSikhote Alin, which fell in eastern Siberia in 1947, under low pH conditions which simulate those prevalentwithin geothermally heated volcanic environments. In addition to these simulations, we also reporthere in situ hydrothermal studies of Sikhote Alin in sub-glacial, geothermally heated fluids from theKverkfjoll Mountains in the northern region of the Icelandic Vatnajokull glacier (Figure 1) during arecent field expedition, between 8–21 June 2011. We have explored the changes which occur to thesurface morphology, corrosion and solution chemistry via a unique combination of elemental (inductivelycoupled plasma) analysis, mapping Raman spectroscopy, scanning electrochemistry, X-ray photoelectronspectroscopy (XPS), 31P-NMR spectroscopy and infinite focus microscopy techniques. Collectively, thesetools have allowed us to draw important conclusions on the following problems:

• where, upon an iron meteoritic surface, anaerobic corrosion is most likely to occur;

• what phosphorus (P)-containing products result from the hydrothermal modification of P-containinginclusions within the meteorite Sikhote Alin

• suggest possible consequences of such corrosion for primitive earth solution chemistry.

We have focused on the relative anodic potentials of meteoritic matrix and schreibersite inclusions whichallow us to comment upon, (i) the nature, (ii) location and (iii) release of reactive, water-soluble P duringsurface corrosion under putative early earth environments. Our key conclusions therefore centre aroundthe availability of reactive P-species resulting from hydrothermal modification of meteoritic surfaces andalso how these P-species can be readily converted to condensed P-oxyacids, specifically pyrophosphite[H2P2O2−

5 , PPi(III)] which has recently been demonstrated to have properties commensurate with anability to act as energy currency molecules within putative early earth environments [1].

References:

1. D. E. Bryant, K. E. R. Marriott, S. A. MacGregor, C. Kilner, M. A. Pasek and T. P. Kee Chem.Commun., 46, 3726 (2010)

127

P2.03 On the ferrobrucite role as reactive intermediate of ser-pentines in pyrophosphate production, and its potential role inthe phosphorylation reactions in hydrothermal systems on earlyEarth

Enrique Iniguez, Nils G. Holm

Department of Geological Sciences, Stockholm University, Sweden.

∗E-mail of corresponding author: enrique.iniguez@geo.su.se

The phosphate group is central to modern biological systems. It most widely occurs as phosphatediesters in the genetic materials RNA and DNA, as phosphoanhydrides in the cellular energy currencyATP, and as phosphomonoesters in numerous metabolic intermediates (1). Phosphorus is not an es-pecially abundant element with crustal rocks containing on average only 0.09%. Pyrophosphate andpolyphosphates can be synthesized under conditions considered to be prebiotic, but the yields are gener-ally low and the conditions are rather forced. The yields are increased if the temperature is increased to200-600C, where the production of polyphosphates is enhanced, but this scenario has not been consideredcompatible with the stability of organic compounds, causing the destruction of them (1). The chemicaldisequilibria in hydrothermal ecosystems provide substantial amounts of energy, which can drive anabolicreactions in thermophilic and hyperthermophilic chemoautotrophs (2). Here we report an experimentaland theoretical study of the ferrobrucite, (Fe,Mg)(OH)2 as a reducing agent and polymerization initiatororiginating from the weathering of olivines and pyroxenes. The ferrobrucite is a metastable interme-diary in the formation of magnetite, Fe3O4, and brucite, Mg(OH)2, with the release of H2 (3). Thisreaction coupled with the polymerization of phosphate in a simulated hydrothermal system, leads tothe formation of phosphides by means of the reduction of phosphate by iron oxidation. This couplingrepresents a significant advantage since the phosphides have higher solubility and larger reactivity thanthe orthophosphates. The reduction takes place at low temperatures between 70 − 150◦C and at lowpressures according with the thermodynamic model used. This model fits with a shallow hydrothermalsystem. On the other hand, the dimerization of phosphites has been reported to occur at 140◦ C (4),allowing that the phosphorylation could occur in a milder environment and compatible with the preser-vation of organic compounds. This result has great importance due to the reduction and dimerization oforthophosphates caused by the ferrobrucite. In the hydrothermal setting two different almost incompat-ible chemical requirements, such as the high energetic milieu required for generation of polyphosphates,together with the milder and reducing environment where the organic compounds could be synthesized,can be combined. In this single environment the prebiotic emergence of phosphorylated compounds ascellular energy currency would have been possible, which is of major relevance to astrobiology.

References:

1. Keefe, A., & Miller, S. (1995). Are polyphosphates or phosphate esters prebiotic reagents? Journalof molecular evolution, 41(6).

2. Amend, J. P., & Shock, E. L. (1998). Energetics of Amino Acid Synthesis in Hydrothermal Ecosys-tems. Science, 281, 1659.

3. Holm, N. G., & Neubeck, A. (2009). Reduction of nitrogen compounds in oceanic basement and itsimplications for HCN formation and abiotic organic synthesis. Geochemical Transactions, 10(1), 9.

4. Bryant, D. E., et al., (2010). On the prebiotic potential of reduced oxidation state phosphorus: theH-phosphinatepyruvate system. Chemical Communications, 46(21), 37263728.

128

P2.04 About the presence of arsenic in prebiotic species: a quan-tum chemical view

Yves Ellinger∗, Mathias Toulouze, Julien Pilme, Francoise Pauzat

UMPC Universite Paris 06, UMR CNRS 7616, Laboratoire de Chimie Theorique, Paris, France∗E-mail of corresponding author: ellinger@lct.jussieu.fr

Since the publications of Wolfe-Simon et al. reporting the replacement of phosphorus by arsenic inbio-molecules of a bacterium [1,2], numerous comments have claimed that such a substitution cannotbe possible. The present report is a prospective study aimed at identifying if arsenic can substitute forthe lighter elements of the same column in prebiotic molecules. Arsenic indeed is a chemical analog ofphosphorus with a similar atomic radius, as well as near identical electronegativity. Systematic com-putational experiments were carried out on simple systems able to form a peptide or analogous bond,and sufficiently small to be potentially identified in space. Density Functional Theory (DFT) within theB3LYP formalism, MP2 and CCSD(T) methods were used to determine the most stable isomers thatcan possibly form from the [C,H,O,As] and [C,3H,O,As] sets of atoms. It was found that HAsCO, likeHPCO and HNCO was the most stable isomer [3]. With three hydrogen atoms, the peptide-like bond(AsH2-CH=O) is not the most stable structure, contrary to NH2-CH=O. It is 9 kcal/mol higher thanthe most stable structure, CH2=As-OH. To assess the plausibility of the As to P substitution in a DNAarchitecture (see also [4] for another approach), a comparative study of the Dimethylphosphate (DMP)and Dimethyl-arsenate (DMA) anions was then carried out. It was found that the gauche-gauche ar-rangement that mimics the helix structure is the most stable one in both model molecules, showing thatthere is no structural evidence to discard the hypothesis of the possible inclusion of As in place of P inthe DNA architecture. The topological analysis of the ELF function [5] showed a weakening by 50% oftwo As-O covalent bonds in all the DMA conformers. It means that if As replaces P, the structure ofthe DNA helix could be weakened. It is also consistent with the well known far less stability of arsenatewith respect to phosphate. As to the formation of complex systems including arsenic in space, one needsto keep in mind that the cosmic abundance of the element is ∼ 103 less abundant than that of phos-phorus. It is then very unlikely that As bearing organics can be formed in the ISM gas phase with anabundance large enough to be detected. However, if concentrated in the ice, As, as well as P, could formmolecular ions to be searched for in the infrared. Full details will be found in a forthcoming publication [6].

References:

1. F. Wolfe-Simon, J. Switzer Blum, T.R. Kulp, G.W. Gordon, S.E. Hoeft, J. Pett-Ridge, J. F. Stolz,S.M. Webb, P.K. Weber, P.C.W. Davies, et al. Science DOI: 10.1126/science.1197258

2. F. Wolfe-Simon, P.C.W. Davies and A.D. Anbar, Int. J. Astrobiol, 8, 69 (2009)

3. M. Lattelais, F. Pauzat, J. Pilm, Y. Ellinger, Phys. Chem. Chem. Phys, 10, 2089 (2008)

4. A. Mladek, J. Sponer, B.G. Sumpter, M. Fuentes-Cabrera and J.E. Sponer, J. Phys. Chem. Lett,2, 389 (2011)

5. B. Silvi and A. Savin, Nature, 1994, 371, 683

6. M. Toulouze, J. Pilm, F. Pauzat and Y. Ellinger, Phys. Chem. Chem. Phys, DOI: 10.1039/C2CP41042G,in press (2012)

129

P2.05 Prebiotic Organic Microstructures

Marie-Paule Bassez1∗, Yoshinori Takano2, Kensei Kobayashi3

1Universite de Strasbourg, France2JAMSTEC-Yokosuka, Japan3Yokohama National University, Japan∗E-mail of corresponding author: marie-paule.bassez@unistra.fr

Micro- and sub-micrometer spheres, tubules and fiber-filament soft structures have been synthesized inour experiments conducted with 3 MeV proton irradiations of a mixture of simple inorganic constituents,CO, N2 and H2O. We analysed the irradiation products, with scanning electron microscopy (SEM) andatomic force microscopy (AFM). These laboratory organic structures produced wide variety of proteinousand non-proteinous amino acids after HCl hydrolysis. The enantiomer analysis for D,L-alanine confirmedthat the amino acids were abiotically synthesized during the laboratory experiment. We consider the pres-ence of CO2 and the production of H2 during exothermic processes of serpentinization and consequentlywe consider the production of hydrothermal CO in ferromagnesian silicate mineral environment. We alsoconsider the low intensity of the Earth magnetic field during Paleoarchaean Era and consequently weconsider excitation sources arising from cosmic radiation which were much more abundant during Pale-oarchaean Era. We then show that our laboratory prebiotic microstructures might be synthesized duringArchaean Eon, as a product of the serpentinization process of the rocks and of their mineral contents.We show similarities in morphology and in formation with some observed Paleoarchaean microstructuresand we suggest that some of the Paleoarchaean carbon spherical and filamentous microstructures mightbe composed of abiogenic organic molecules. We further propose a search for such prebiotic organicsignatures on Mars. This article has been posted on Nature Precedings on 21 July 2010 (Bassez andTakano 2010). A new version considering the Earth magnetic field has been presented at the ORIGINSconference in Montpellier in July 2011 and posted on Nature Precedings on 14 November 2011 (Bassezet al. 2011).

References:

1. Bassez MP, Takano Y (2010) Prebiotic organic globules. Available from Nature Proceedings

2. Bassez MP, Takano Y, Kobayashi K (2011) Prebiotic organic microstructures. Available fromNature Proceedings

3. Bassez MP, Takano Y, Kobayashi K, OLEB submitted

130

P2.06 Characterization of proteinoid microspheres on their for-mation and degradation

Hiroshi Kanamaru∗, Hikaru Koda, Kyoko Yokomizo, Yuta Hatae, Shoichi Nakamura, Mami Turuyama,Hajime Mita

Fukuoka Institute of Technology, Japan∗E-mail of corresponding author: solevient@yahoo.co.jp

Proteins are ones of the most abundant and important organic compounds in the terrestrial livingorganisms. Amino acids widely distribute in the universe, since amino acids are found in carbonaceouschondrites [1, 2], interplanetary dust particles [3], cometary dust [4], lunar fines [5, 6] and various kindsof simulated experiments [7]. Therefore, protein or its related compounds (polyamino acids) would beformed in the prebiotic world. There are some reports of prebiotic polyamino acids formation, butmost of them are limited reactions for specific amino acids. One of the famous experiments of prebioticpolyamino acid formations is thermal polycondenastion of monoammonium malate [8]. Proteinoid whichis a polyaspartic acid is formed in molten stage of monoammonium malate and it forms a globular struc-ture called proteinoid microsphere after heating and cooling process of its aqueous solution [9]. Thereby,we focused on the proteinoid microsphere and characterized the physical and chemical properties of theproteinoid microsphere using by LC-MS, GPC, IR, DLS, and SEM. In this paper, metal ions effects onmicrosphere formation were studied. Firstly, thermal proteinoid was synthesized by heating of monoam-monium malate at 180◦C for 6 h. Then, 10 g of proteinoid was dissolved into 1 L of water and heatedat 100◦C for 10 min. The solution was gradually cooling after removal of insoluble matter by filtration.Once microsphere was collected by centrifugation and dissolved into some aqueous solutions containingmetal ions (0.1 mol/L). Finally, microsphere was formed by the heating and cooling process describedabove (Fig. 8). Microspheres were formed in the all metal ion solutions examined in this study (Na+, K+,Mg2+, Mn2+, and Cu2+). Their size distribution of microspheres were determined on the SEM imagesand DLS measurements. The results were approximately 1 µm which was a similar size described in theprevious report [9] and prepared in the pure water (without metal ion). In the previous paper [10], controlof ionic strength of potassium ion was important for microsphere formation and electrostatic interactionsis a key factors for microsphere formation. However, we found that microspheres were formed in variousmetal ion solutions. In addition, microsphere was even formed in the pure water. We also found thatmicrospheres were formed from polyamino acids synthesized from hydrophobic amino acids in the moltenurea [11, 12]. Proteinoid synthesized from monoammonium malate is unhydropolyaspartic acid and is arather hydrophobic compound. Therefore, hydrophobic interaction would be more important for micro-sphere formation than electrostatic interaction.

References:

1. Kvenvolden, K. Lawless, J., Pering, K., Peterson, E., Flores, J., Ponnamperuma, C., Kapkan, I. R.and Moore, C., Nature 228, 923-926 (1970).

2. Cronin, J. R., and Moore, C. B. Science 172, 1327-1329 (1971).

3. Brinton K., Engrand C., Glavin D., Bada J., and Maurette M., Origin Life Evol. Biosphere 28,413-424 (1998).

4. Elsila J. E., Glavin, D. P., and Dworkin, J. P., Meterites & Planet Sci. 44, 1323-1330 (2009).

5. Harada, K., Hare, P. E., Windsor, C. R., and Fox, S. W., Science 173, 433-435 (1971).

6. Karen et al., 1996) Crick, F., Life Itself. Simon & Schuster, New York. (1981).

7. Miller,S.L., Science 117 ,528-529 (1953).

8. Fox, S. W., Harada, K., and Kendrich, J., Science 129, 1221-1223 (1959).

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Figure 8: Proteinoid microphere formed in sodium solution.

9. Harada, K. J. Org. Chem., 24, 1662-1666 (1959).

10. Ishima, Y., Pizybyiski, A. T. and Fox, S. W. Biosystems 13, 243-251 (1981).

11. Kuwahara, Y., Kanamaru, ., Tsuruyama, M., and Mita, H. Abstract book of International ChemicalCongress of Pacific Basin Societies 2011, #551 (2011).

12 Mita, H., Nomoto, S., Terasaki, M., Shimoyama, A., and Yamamoto, Y. Int. J. Astrobiol. 4, 145-154(2005).

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P2.07 Possible Scenario of the Prebiotic Formation of OrganicAggregates by High-Energy Radiation and Hydrothermal Pro-cesses

Kensei Kobayashi1∗, Hironari Kurihara1, Yukinori Kawamoto1, Takuto Okabe1, Midori Eto1, YumikoObayashi1, Takeo Kaneko1, Hikaru Yabuta2, Hajime Mita3, Kazuhiro Kanda4

1Graduate School of Engineering, Yokohama National University, Yokohama, Japan2Graduate School of Science, Osaka University, Toyonaka, Japan3Faculty of Engineering, Fukuoka Institute of Technology, Fukuoka, Japan4Laboratory of Advanced Science and Technology for Industry, University of Hyogo, Kamigori, Japan∗E-mail of corresponding author: kkensei@ynu.ac.jp

Formation of organic aggregation or molecular self-assembly is necessary in prior to the generation oflife. A number of so-called proto-cell models have been proposed including Oparins coacervates and Foxand Haradas proteinoid microspheres. In these reports, high concentration of pure organic monomerssuch as amino acids or other biological molecules should be used. Here we propose possible pathways oforganic aggregate formation under possible prebiotic conditions.

At first, we irradiate a gas mixture of carbon monoxide, nitrogen and water with high-energy protonsfrom a van de Graaff accelerator to simulate possible reactions in primitive planetary atmosphere by theaction of cosmic rays [1]. The resulting products (hereafter referred to as CNW) were hydrophilic complexmolecules with high molecular weights (ca. 3000), and they yielded amino acids after acid-hydrolysis.

Then the aqueous solution of CNW was heated at 200–400◦C in a flow reactor, which was constructedto simulate submarine hydrothermal systems [2], for 2 min, and then quenched to 0◦C. The effluent wasfiltered through a membrane filter without any condensation, and the residue was observed by SEM.

Aggregates were observed when CNW was heated: When CNW was heated at 300◦C, larger andmore aggregates were formed than 200 or 400◦C, while no aggregates were detected without heating.Aggregates gave amino acids after acid-hydrolysis. C- and N-XANES spectra of CNW before and afterheating suggested that hydrophobicity of CNW increased by hydrothermal reaction [3].

Using extraterrestrial organics can draw another scenario. Most of organic compounds found incarbonaceous chondrites were insoluble, and some organic globules were reported in them [4]. Cometarydusts collected in the Stardust Mission showed wide variety of hydrophobicity (5). On the other hand,complex organic compounds synthesized from possible interstellar media (e.g., carbon monoxide and/ormethanol, ammonia and water) were quite hydrophilic and soluble in water. It is suggested that organicsin cometary dusts has various irradiation history. We irradiated amino acids and their precursors withsoft X-rays at BL06 in NewSUBARU facility of University of Hyogo [6]. After irradiation, water-insolubleproducts were formed. VUV light did not show such effects on amino acids and their related compounds.

Thus it is suggested that strong soft X-rays irradiation from the proto- and young Sun could havegiven hydrophobicity to organic compounds in dusts of interstellar origins. Such hydrophobic organicsmight have yielded globules by hydrolytic or hydrothermal reactions in meteorite parent bodies. Amphi-pathic molecules were formed from hydrophilic interstellar molecules by soft X-rays irradiation of dusts.They were delivered to Earth hydrosphere, and could form organic aggregates/globules in submarinehydrothermal systems more easily than endogenously synthesized organics like CNW.

References:

1. K. Kobayashi, T. Kaneko, T. Saito, T. Oshima, Orig. Life Evol. Biosph. 28, 155 (1998).

2. Md. N. Islam, T. Kaneko, K. Kobayashi, Bull. Chem. Soc. Jpn., 76, 1171 (2003).

3. H. Kurihara, H. Yabuta, T. Kaneko, Y. Obayashi, Y. Takano, K. Kobayashi, Chem. Lett., 41, 441(2012).

4. K. Nakamura-Messenger et al., Science, 314, 1439 (2006).

5. G. D. Cody et al., Meteor. Planet. Sci., 43, 353 (2008).

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6. Y. Kawamoto M. Eto, T. Okabe, Y. Obayashi, T. Kaneko, J. Takahashi, H. Mita, K. Kanda, K.Kobayashi, 12th European Workshop on Astrobiology, Stockholm, October 2012.

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P2.08 The Thermal Stability of Tetrapyrroles: Exploring theLimits

Franz Leißing∗, Stefan Fox, Henry Strasdeit

Department of Bioinorganic Chemistry, Institute of Chemistry, University of Hohenheim, 70599 Stuttgart,Germany∗E-mail of corresponding author: franz.leissing@uni-hohenheim.de

Tetrapyrrole derivatives occur in all organisms (Lesage et al., 1993). They are found in prokaryotesand in mitochondria and chloroplasts of eukaryotes. Chlorophylls, which are key molecules in photosyn-thesis, and haems, which are important in electron transfer and oxygen transport, are the most importanttetrapyrroles. The haem-containing cytochrome c protein, for example, is a constituent of membrane-bound electron-transfer chains. As a result of this electron transport, an electrochemical gradient isestablished that allows the phosphorylation of adenosine diphosphate (ADP) to adenosine triphosphate(ATP). ATP serves as the primary biochemical energy currency and therefore is essential for many otherreactions. The general occurrence in all organisms and the fundamental functions of tetrapyrroles mayindicate an early appearance in biological evolution. Thus, one can hypothesize that tetrapyrroles mayhave already played an important role in the metabolism of protocells and consequently in the origin oflife. Porphyrins, which are aromatic tetrapyrroles, are among the most resistant biomolecules. They aredetectable in petroleum and sediments of all ages. Even sediments that are older than 3 billion yearsmay contain porphyrins (Hodgson, 1973). Due to this long-term stability, it seems plausible that abioti-cally formed tetrapyrroles were not completely decomposed in the early-Earth environment. Thus, theycould have played an important role in prebiotic chemical evolution, for example on primordial volcanicislands. For several reasons (e. g. temperature gradients, volcanic lightning, locations with different pH),volcanic islands are promising locations for the prebiotic chemical evolution on young Earth-like planets(Strasdeit, 2010). To gain a deeper insight into the stability of tetrapyrroles, we have investigated thethermal behaviour of an open-chain tetrapyrrole (biliverdin) and two porphyrins (octaethylporphyrin andhaemin). These compounds were exposed to different temperatures in the range 100−300 ◦C for typically24 hours. To simulate the non-oxidizing conditions of the prebiotic atmosphere, the heating experimentswere conducted under pure nitrogen gas. The residues were analysed by ultraviolet-visible spectroscopyto determine the onset and extent of the thermal decomposition.

References:

Hodgson GW (1973) Ann NY Acad Sci 206:670-684

Lesage S, Xu H, Durham L (1993) Hydrol Sci J 38:343-354

Strasdeit H (2010) Chemical Palaeodiversity 3(Supplement):107116;http://www.palaeodiversity.org/pdf/03Suppl/Supplement Strasdeit.pdf

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P2.09 From Cytoplasm to Environment: the Inorganic Ingredi-ents for the Origin of Life

Alexey Novoselov1, Paloma Serrano2, Mırian Liza Alves Forancelli Pacheco3, Michael Scott Chaffin4, JackThomas O’Malley-James5, Susan Carla Moreno1, Filipe Batista Ribeiro6, Carlos Roberto de Souza Filho1

1UNICAMP, Brazil2Alfred Wegener Institute for Polar and Marine Research, Germany3USP, Brazil4University of Colorado, USA5University of St Andrews, UK6UNESP, Brazil∗E-mail of corresponding author: alexey@ige.unicamp.br

Early in its history the Earths surface developed from an uninhabitable magma ocean to a placewhere life could emerge. The first organisms, lacking ion transporters, fixed the composition of theircradle environment in their intracellular fluid. Later, though life adapted and spread, it preserved somequalities of its initial environment within. Modern prokaryotes could thus provide insights into theconditions of the early Earth and the requirements for the emergence of life. In this work, we constrainEarths life-forming environment through detailed analysis of prokaryotic intracellular fluid. This work:(i) conducts a survey of the elemental composition of the prokaryotes, identifying common chemicaltraits; (ii) computationally determines the fluid compositions produced by the range of early atmosphere,surface, and ocean conditions, and (iii) links the early Earth environment to the cytoplasmic environmentof life. Rigorous assessment of the constraints placed on the early Earth environment by intracellularliquid will provide insight into the conditions of abiogenesis, with implications not only for the earlyEarth but also for the formation of life elsewhere in the Universe.

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P2.10 Chemoinformatics and chemical evolution

Robert Bywater∗†

Magdalen College, High Street, Oxford, OX1 4AU, England∗E-mail of corresponding author: romeobravo@adelard.org.uk†E-mail of corresponding author: robpbyw@gmail.com

Any consideration of which prebiotic chemicals existed prior to the appearance of RNA, and wherethey appeared should also include answers to the questions “when” and “in what order”. In the workpresented here, chemical complexity and quantum chemical calculations are presented which suggest anordering of chemicals that are widely accepted as being candidates for representing the repertoire ofprebiotic chemicals.

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P2.11 Inversion concept of the origin of life, its consequencesand the experimental verification program

Vladimir N. Kompanichenko

Institute for Complex Analysis, Birobidzhan, Russia∗E-mail of corresponding author: kompanv@yandex.ru

Concept summary. The essence of the inversion concept of the origin of life can be narrowed downto the following theses: 1) thermodynamic inversion is the key transformation of prebiotic microsystemsleading to their transition into primary forms of life; 2) this transformation might occur only in themicrosystems oscillating around the bifurcation point under far-from-equilibrium conditions. The trans-formation consists in the inversion of the balance ‘free energy contribution/entropy contribution’ (as wellas ‘information contribution/informational entropy contribution’), from negative to positive values. Atthe inversion moment the microsystem radically reorganizes in accordance with the new negentropy (i.e.biological) way of organization. According to this concept, the origin-of-life process on the early Earthtook place in the fluctuating hydrothermal medium. The process was taking two successive stages: a)spontaneous self-assembly of initial three-dimensional prebiotic microsystems composed mainly of hydro-carbons, lipids and simple amino acids, or their precursors, within the temperature interval of 100–300◦C(prebiotic stage); b) non-spontaneous synthesis of sugars, ATP and nucleic acids started at the inversionmoment under the temperature 70–100◦C (biotic stage). Macro- and microfluctuations of thermodynamicand physico-chemical parameters able to sustain this way of chemical conversion have been detected inseveral contemporary hydrothermal systems (1,2).

Reconstruction of the thermodynamic inversion. The biological evolution proceeds in the thermody-namic direction opposite to the evolution of non-biological natural systems: free energy and informationaccumulate in biological systems, while entropy exports outside. How might the inversion of thermody-namic trend occur during the prebiotic microsystems transition into primary living units? The author’sreconstruction of this process is represented in Fig. 9. The picture shows the inversion of balance ‘freeenergy contribution/entropy contribution’. The oscillating prebiotic microsystem is characterized by anexchange of energy and matter with the outside world; a tendency to dichotomy; continuous reactionsresulted in free energy accumulation and preservation (Fig. 9 A). Changes in the outside world stress themicrosystem, provoking a release of preserved free energy. As a result, the total of internal and externalenergy contributions prevails over dissipation (Fig. 9 B). The resulted direction of free energy flow re-verses from the external to internal one (Fig. 9C). In this way, the microsystem undergoes thermodynamicinversion, importing free energy and exporting entropy (Fig. 9D).

Consequences from the concept. There are two consequences of the inversion approach which are ofimportance for the chemical aspect of the origin-of-life scenario:

1. Thermodynamic inversion results in accumulation and preservation of excessive free energy andinformation in a central part of the system (Fig. 9). It follows that such a transition might occuronly in a three-dimensional prebiotic microsystem.

2. The transition of prebiotic microsystems into living probionts might occur only in the changeablemedium, necessary for maintaining their internal oscillations with external oscillations of thermo-dynamic and physico-chemical parameters.

Therefore, the inversion concept imposes some restrictions on current chemical models for the origin oflife. Thus, on the assumption of the inversion approach, some notions of the RNA-World concept requireto be reconsidered. The experimentally proved synthesis of RNA World macromolecules, including self-replication with ribozymes, should be referred to the prebiotic processes. The biotic processes start withthe nucleoprotein interaction inside three-dimensional microsystems (the RNA molecules might permeatefrom the outside world), at the moment of thermodynamic inversion and the appearance of negentropymotive power. The negentropy motive power forms functional interaction between two main types ofbiopolymers (sequences of nucleotides and proteins) and transforms the accumulating information intobioinformation, through programming, algorithmic control and prescriptive instructions [2].

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Figure 9: Reconstruction of a prebiotic microsystem transition into living unit. Fint (internal) and Fext

(external) free energy contributions into a prebiotic system; ∆F+ (positive) and ∆F− (negative) freeenergy gradients of the system with respect to the surroundings; arrows - directions of free energy andentropy flows [1].

Program of experimental research. The inversion approach offers a new way for the laboratory ex-periments on the origin of life. The theoretically substantiated origin-of-life process (including bothprebiotic and biotic stages) should be tested in the experimental system with fluctuating conditionsin the chamber. Modeling the prebiotic stage, the behavior of relevant organic compounds (hydrocar-bons, lipids, amino acids, nucleic acids) should be explored in the fluctuating medium simulating thefluid rising in the thermo gradient field of the Earth’s crust upper layer. The continuous uncompletedsynthesis of organic (marco)molecules and self-assembly of organic microsystems (i.e. a change in the syn-thesis/oligomerization and destruction tendencies, due to external fluctuations) are the most interestingprocesses to investigate. These experiments could serve as a good basis for the following experimentalattempts to obtain probionts under optimum fluctuating environment.

The work was supported by the projects No. 09-I-II15-01 FEB of RAS and No. 10-05-98003 RFBR.

References:

1. V. Kompanichenko, Origin of Life and Evolution of Biospheres, Journal, DOI 10.1007/s11084-012-9279-0 (2012)

2. V. Kompanichenko, In the Beginning: Precursors of Life, Chemical Models and Early BiologicalEvolution (J. Seckbach Ed.), 22, 305-320, Springer Dordrecht (2012)

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P2.12 Categories of Life

Georg Hildenbrand∗, Michael Hausmann

Kirchhoff-Institute for Physics, University of Heidelberg, Im Neuenheimer Feld 227, 69120 Heidelberg,Germany∗E-mail of corresponding author: hilden@kip.uni-heidelberg.de

Definitions of life are controversially discussed; however, they are mostly depending on bio-evolutionarydriven arguments. Here, we propose a systematic, theoretical approach to the question what life is, bycategorization and classification of different levels of life. This approach is mainly based on the analy-sis of identity generating and maintaining operations occurring in systems being suspicious to be alive,and on the analysis of their power of environmental control. In a first step, we show that all biologicaldefinitions of life can be derived from basic physical principles of entropy (number of possible statesof a thermodynamic system) and of the energy needed for controlling entropic development. In a nextstep we discuss how any process where identity is generated, regardless of its materialization is definedand related to classical definitions of life. In a third step we resume the proposed classification schemein its most basic way, looking only for existence of data storage, its processing, and its environmentalcontrol. We join inhere a short discussion how the materialization of identity-operations can take placedepending on the special properties of the four basic physical forces. Having done all this we are able togive everybody a classification catalogue at hand that one can categorize the kind of life one is talkingabout, thus overcoming the obstacles deriving from the simple appearing question whether something isalive or not. On its most basic level as presented here, our scheme offers a categorization for fire, crystals,prions, viruses, spores, up to cells and even tardigrada in cryostasis, additionally extendable to artificialsystems of life.

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P3.01 Assessing the influence of the solar Galactic orbit on ter-restrial biodiversity variations

Coryn A.L. Bailer-Jones∗, Fabo Feng

Max Planck Institute for Astronomy, Heidelberg, Germany∗E-mail of corresponding author: calj@mpia.de

The fossil record shows that biodiversity has varied considerably over the Phanerozoic eon (past 550Myr). Some investigators have claimed there to be a periodic component in this variation, and havefurther suggested this could arise from the (quasi)-periodic motion of the Sun about the Galactic planeand/or through the spiral arms. However, many researchers have pointed out that methods used toanalyze the data – and even the data themselves – are problematic. We report on two studies in whichwe have investigated this in more detail. First, in order to assess the plausibility of the Sun’s orbitmodulating biodiversity, we have performed a Monte Carlo study of the sensitivity of the periodicity ofthe solar orbit to initial conditions and parameters of the Galactic potential model. A strictly periodicorbit occurs only for an exact circular orbit, or at specific values of the initial conditions which give riseto a resonance between the perpendicular and azimuthal motions. However, a large fraction of orbitsin our simulations are quasi-periodic, with a deviation from strict periodicity of less than 10%. Second,assuming some non-specific mechanism in which the extinction rate is proportional to the local stellardensity, we assess how well different parametrized dynamical models of the solar orbit can explain thefossil record. We calculate the distribution of the likelihood of the extinction record over the modelparameters, and then by marginalizing over the parameters calculate the Bayesian evidence for eachmodel. We find that the evidence is not significantly higher for these dynamical models than it is for asimple stochastic model of extinction. This suggests that the solar orbit, through variations in the localstellar density, has a limited overall impact on the long-term variation of the terrestrial extinction rate.A more detailed investigation continues.

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P3.02 Continuous, in situ measurement of the altitude-dependentchange of UV radiation and its effects on biological systems

Veronika Grosz1∗, Gergely Goldschmidt1, Attila Berces2

1Budapest University of Technology and Economics, Budapest, Hungary2Semmelweis University, Budapest, Hungary∗E-mail of corresponding author: veronica.grosz@gmail.com

The harmful effects of UV radiation on living organisms are based on the molecular changes mostlyin DNA. UV radiation induces the dimerisation of pyrimidine bases and leads to the formation of pho-toproducts such as 6-4 bipyrimidines and cyclobutane dimers [1-2]. Since the earliest microorganismsand organic molecules were present on Earth before the evolution of the ozone layer, and, accordingto the panspermia theory, they are also able to travel and survive in space, studying the dynamics ofthese changes can contribute to our knowledge on how living systems can survive without notable UVprotection.

The experiment presented here takes part in a program called BEXUS (Balloon Experiments forUniversity Students), and aims to study the dynamics of the UV-induced dimer formation of pyrimidinesin dependence of altitude. It employs a biodosimetric measurement method developed by the ResearchGroup for Biophysics of Semmelweis University, which is based on measuring the decrease of opticaldensity of uracil samples after UV irradiation [3]. The change of OD is proportional to the dose ofradiation (Fig. 10).

The experiment consists of uracil thin layer samples, photodiodes and a corresponding electronicdesign, mounted on the gondola of a stratospheric balloon. During the balloon’s flight, the UV com-ponents of sunlight irradiate the uracil samples. This induces dimerization and therefore the decreaseof optical density, which is constantly monitored by the photodiodes installed behind the samples. Themeasurement data are collected and stored by the onboard data handler. This experiment setup allowsa continuous, in situ measurement method.

References:

1. G.J. Fisher, H.E. Johns, Photochemistry and Photobiology of Nucleic Acids, 1 169-224, (1976)

2. B.S. Rosenstein, D.L. Mitchell, Photochem. Photobiol. 45; 775-780, (1987)

3. Ronto G, Berces A, Fekete A, Kovacs G, Grof P, Lammer H, Adv Space Res., 33(8):1302-5, (2004)

Figure 10: Decrease of the optical density of uracil in dependence of UV irradiation using a germicidallamp [3].

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P3.03 Glendonite minerals from Late Carboniferous glacioma-rine Dwyka Group, South Africa - palaeoenvironmental implica-tion and astrobiological potential

Barbara Cavalazzi1∗, Ian R. McLachlan2, Nicholas J. Beukes1,

1Department of Geology, University of Johannesburg, Johannesburg, South Africa2Bernard Price Institute for Palaeontological Research, School of Geoscience, Witwatersrand University,South Africa∗E-mail of corresponding author: cavalazzib@uj.ac.za

Ikaite, a Ca-carbonate hexaydrate, is a metastable carbonate that only forms in specific environmen-tal condition such as near-freezing temperatures, high alkalinity, and elevated orthophosphate. Ikaitehave been reported as occurring in marine, freshwater, and estuarine aqueous environments, and thereare is also strong evidence that forms in association with hydrocarbon/methane-dominated seepages andthe microbial anaerobic decomposition/oxidation of hydrocarbons during the early stage venting. Thus,glendonite, stable pseudomorph after Ikaite, in geological record is considered a good paleoenvironmen-tal indicator. Here, we report combined data of a detailed mineralogical, petrographical, geochemical(SEM-EDX, EMPA, Raman, XRD, stable isotope) study of glendonite in nodules from Late Carbonife-orus glaciomarine strata of Dwyka Group, Great Karoo Basin, South Africa. Glendonites from the topstrata of Dwyka Group show a granular internal fabric with concentrically zoned calcite grains linedby carbonaceous matter-rich phosphate and Mn-Fe-rich rims, cemented by calcite and certain amountpyrite. The zoned calcite grains represent the ikaite replacement phase. The presence of pyrite in thepore space suggests microbially-mediated methane oxidatation via sulphate reduction. The high δ18Oand depleted δ13C values of carbonate cements suggest an early diagenetic phase that forms in the zoneof suboxic diagenesis in organic matter (OM) rich sediments, and possibly associated to potential hydro-carbon seepage. These data, filed observations and the presence of hydrocarbon-seep carbonates from theequivalent glaciomarine deposits in Namibia, strongly suggest the possibility that studied South Africanglendonites where linked to a seepage events associated to Late Carboniferous deglaciation in the KarooBasin. To understand the significance of glendonite formation and the potential role of microorganismsin its formation is also related to (1) its possible occurrences on Mars, where an ancient, cold, alkali-richocean is postulated to have been conducive to the formation of ikaite, and (2) the relatively recentlyimaged nick-named “Sushi” rocks from Spirit showing features strongly resembling glendonite crystals.

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P3.04 X-Ray tomography and Raman characterization of waterexpulsion-related microfractures in glendonite nodules: an exam-ple from Late Carboniferous glaciomarine Dwyka Group, SouthAfrica

Barbara Cavalazzi1,2∗,Nicholas J. Beukes1, Frikkie C. de Beer3, Jakobus W. Hoffman3, Ian R. McLachlan4,Roberto Barbieri2

1Department of Geology, University of Johannesburg, Johannesburg, South Africa2Dipartimento di Scienze della Terra e Geologico-Ambienatli, Universite di Bologna, Bologna, Italy3Department of Radiation Science, South African Nuclear Energy Corporation Ltd, Pretoria, SouthAfrica4Bernard Price Institute for Palaeontological Research, School of Geoscience, Witwatersrand University,South Africa∗E-mail of corresponding author: cavalazzib@uj.ac.za

Ca-carbonate is an important constituent of the Earth’s crust and oceans, and occurs in a numberof crystallographic structures. Anhydrous and hydrous forms and polymorphs of CaCO3 include calcite,aragonite, vaterite, ikaite and monohydrocalcite.

Ikaite is the hexaydrate Ca-carbonate (CaCO3·6H2O) that only forms and is stable in specific hydrousenvironmental condition such as near-freezing temperatures, H2O pressures greater than ambient, highalkalinity, and elevated orthophosphate, and rapidly decomposes and recrystallize (e.g. at temperaturesabove 6 − 7◦C) to glendonite characterized by Ca-carbonate, mainly calcite, crystals [1]. It has beenhypothesized that glendonite pseudomorphs can be assumed to represent a typical manifestation atfossil and recent cold vents at high latitudes where microbes play an important role in the anaerobicdecomposition/oxidation of hydrocarbons by during the early stage venting [2].

Thus glendonite after ikaite represent an important indicator of peculiar geochemical conditions forcarbonate precipitation, paleoenvironmental reconstructions and extremophiles that inhabit the methaneseep ecosystems that definitively might represent terrestrial analogues for martian environments andpossible models for microbial life on other planets [3]. The interest of significance of glendonite formationin an astrobiological perspective relies on their relationship with its potential as paleoenvironmental proxywith is especially related to its possible occurrences on Mars, where an ancient, cold, alkali-rich oceanis postulated to have been conducive to the formation of ikaite, and where rocks with features stronglyresembling glendonite crystals, named ”Sushi” rocks, have been imaged from Spirit.

We have examined the 3-dimensional sill and microfracture network found in nodules with a glen-donitic cores from Late Carboniferous glaciomarine stata of Dwyka Group, Great Karoo Basin, SouthAfrica, using X-Ray tomography, Raman, SEM-EDX, C-O stable isotope and petrographic analysis. Thesill and microfractures, localized to the interface zone between host nodules and glendonite crystals, possi-bly result from the water expulsion during the recrystallization of hydrous ikaite to anhydrous glendoniticcalcite that results in considerable solid volume loss and production of a highly porous crystal mesh. Thewidths of the microfractures are, on average, less than 80 microns with a characteristic distribution, anddifferent morphologies. The Raman microscopy confirms the presence of dolomite cements inside thehydraulically induced fractures, and a Fe- and Mg-rich calcitic composition of the granular glendonitecrystals. Although the occurrence of ikaite/glendonite is not strictly related to methane-venting, the3-D distribution of the microfractures and the paragenetic sequences of the carbonate cements of studiedglendonites should represent an effect of an early stage methane-dominated vent activity at cold bottomwater temperatures as reported in glendonites from the Sea of Okhotsk, Eastern Siberia [2].

References:

1. B.W. Selleck, P.F. Carr and B.G. Jones, Journal of Sedimentary Research, 77, 980-991 (2007).

2. J. Greinert and A. Derkachev, Marine Geology, 204, 129-144 (2004)

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3. R. Barbieri and B. Cavalazzi, In J. Seckbach and M. Walsh (eds.), From Fossils to Astrobiology,297317 (2009)

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P3.05 Integration of protocellular components

Philipp M.G. Loffler1, Anders Albertsen1, Rafal Wieczorek1, Michael Wamberg1, Mark Dorr1, PernilleL. Pedersen1, Carsten Svaneborg1, Harold Fellermann1, Joseph B. Edson2, Jonathan L. Cape2, MartinHanczyc1, Hans Ziock3, James M. Boncella2, Pierre-Alain Monnard1, and Steen Rasmussen1,4,

1Center for Fundamental Living Technology (FLinT), Department of Physics, Chemistry & Pharmacy,University of Southern Denmark, 5230 Odense M, Denmark2Materials, Physics and Applications &3Earth and Environmental Science, Los Alamos National Laboratory, New Mexico 87545, USA4Santa Fe Institute, Santa Fe NM 87501 USA∗E-mail of corresponding author: steen@sdu.dk

It is still not clear how to implement a self-reproducing chemical system possessing simplified capa-bilities of a living cell. Such a minimal living physicochemical system, a protocell, should encompassinformation, energy transformation and co-localization in a mutually interdependent manner. A funda-mental design strategy to achieve such minimal living system was outlined in Rasmussen et al. (2003,2004), and to reach that goal we have defined a chemical dependency between each of the three componentsubsystems. The replication of the information molecules must depend on the formation of the containeras well as the work of the metabolism. The formation of the container must depend on the work of themetabolism, and the work of the metabolism must depend on the information molecules. The presentedwork focuses in the problems and accomplishments associated with integrating these three components.We have recently developed a template-directed synthesis of oligonucleotides by non-enzymatic ligation(Cape et al., 2012), which is connected to the growth of the container by the action of a Ruthenium cata-lyst. In earlier studies we have demonstrated how the presence of a particular nucleobase (8-oxoguanine)– out of a possible combinatorial set – controls the growth metabolism in the formation of the protocellcontainers through the production of fatty acids (DeClue et al., 2009 & Maurer et al., 2011). Recentexperimental results indicate that a metabolically driven oligonucleotide formation and fatty acid pro-duction can occur in concert. Regarding template directed replication through ligation, recent theoreticalstudies indicate a replication advantage for longer strands at lower temperatures in the regime where theligation rate is rate limiting. In addition, these results indicate the existence of an optimal replicationrate at the boundary between the two regimes where the ligation rate and the dehybridization rates arerate limiting – long strands and low temperatures (Fellermann & Rasmussen, 2011). Although we haveexperimentally demonstrated simplified life-cycle iteration through cyclic protocellular growth and divi-sion (without template directed replication), we are still not at a point where we can test the predictedcoordinated component growth through life-cycle iteration (Rouchelau et al., 2007 & Munteanu et al.,2007). The open challenges will be discussed.

References:

Cape, J.L., Edson, J.B., Spencer, L.P., DeClue, M. S., Ziock, H., Maurer, S.E., Rasmussen, S., Monnard,P.A. and Boncella, J.M. (submitted). Phototriggered DNA ligation using visible light in a tandem5-amine deprotection / 3-phosphorimidazolide coupling reaction.

Cape, J.L., Edson, J.B., Spencer, L.P., DeClue, M. S., Ziock, H., Maurer, S.E., Rasmussen, S., Monnard,P.A. and Boncella, J.M. (submitted). Phototriggered DNA ligation using visible light in a tandem5-amine deprotection / 3-phosphorimidazolide coupling reaction. DeClue, M. S., Monnard, P. A.,Bailey, J. A., Maurer, S. E., Collis, G. E., Ziock, H. J., Rasmussen, S. and Boncella, J.M. (2009).Nucleobase Mediated, Photocatalytic Vesicle Formation from an Ester Precursor. J. Am. Chem.Soc., 131:931-933.

Fellermann, H., Rasmussen, S. (2011). On the Growth Rate of Non-Enzymatic Molecular Replicators.Entropy, 13:1882-1903

Maurer, S.E., DeClue, M.S., Albertsen A.N., Dorr, M., Kuiper, D.S., Ziock, H., Rasmussen, S., Boncella,J.M. and Monnard, P.A. (2011). Interactions between catalyst and amphiphilic structures and theirimplications for a protocell model. Chemphyschem., 12:828-35.

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Munteanu, A.; Attolini, C.; Rasmussen, S.; Ziock, H. & Sol, R.V., Generic Darwinian Selection inCatalytic Protocell Assemblies. (2007) Philosophical Transactions of the Royal Society of London.Biological Sciences; vol. 362, no. 1489; pp. 1847-1856.

Rasmussen, S., Chen, L., Nilsson, M. and Abe, S. (2003). Bridging nonliving and living matter. ArtifLife, 9:269-316.

Rasmussen, S., Chen, L., Deamer, D.W., Krakauer, D.C., Packard, N.H., Stadler, P.F. and Bedau, M.A.(2004). Transitions from nonliving to living matter. Science, 303:963965

Rouchelau, T.; Rasmussen, S.; Nielsen, P.; Jacobi, M. & Ziock, H., Emergence of Protocellular GrowthLaws. (2007) Philosophical Transactions of the Royal Society of London. Biological Sciences; vol.362, nr. 1486; pp. 1841-1845.

147

P3.06 Origin of cellular life: The earliest genome was of eukary-otic type?

Lauri Nikkanen∗, Kirsi Lehto

University of Turku, Finland∗E-mail of corresponding author: lenikk@utu.fi

We have proposed that the earliest membraneous containment for the replicating RNAs, during theRNA-protein era, would have been similar to the membrane vesicles that are still induced by contem-porary RNA viruses and used as protective compartments for their replication complexes (Laitera andLehto 2009). We now propose that such replication vesicles may have been the direct progenitors ofthe emerging eukaryotic nuclear membranes, and that these renewable nuclear structures have been firstestablished within the early molecular community prior to the separation of individual cytoplasms, orthe three domains of cellular life. Thus the early molecular community would have produced the proto-cytoplasm, and the first emerging genomes were defined by their containment into the replication vesicles.This is supported by the primitive structure of eukaryotic genomes and by the synthesis, cleavage, methy-lation and assembly mechanisms of the proposed early replication machinery (i.e. of the ribosomal RNAsand tRNAs) as well as by the preserved function of snoRNAs and snRNAs inside the nucleus (Poole etal. 1999; Meli et al. 2001). Further support is provided by the fact that the highly conserved DEAD-Box-helicase proteins that still transport mRNAs through nuclear pores in contemporary eukaryotes areRNA helicases, which could have originally served as components of the RNA replication machinery.Furthermore, we propose that the division machinery for the early genomes and nuclei evolved beforethe encapsulation of individual cytoplasms into individual cell membranes – hence, it evolved before thedivergence of the three domains of cellular life. The division of the eukaryotic genome is still initiatedwith the disappearance of the nuclear membrane and appearance of the nuclear spindle, composed oftubulin fibers, which guides the separation of the daughter chromosomes into two equal genomic sets.Tubulins are homologs of the prokaryotic cell division protein FtsZ, and both are derived from an an-cestral form of FtsZ whose earliest function may well have been replication-related, as is suggested bythe discovery of FtsZ-paralogs in bacteria that are involved in replication of plasmid DNA instead of celldivision (Tinsley & Khan 2006). Moreover, it is well known that the genomic division does not need tobe associated with cell division, but can lead to temporary or permanent state of polynucleated cells, ase.g. in Drosphila embryos, or the slime molds, respectively. We suggest that this stage has also occurredin the early evolution of life, in the transition period from the earliest molecular communities to theindividual cellular lineages.

References:

Laitera T, Lehto K (2009) Protein-mediated selective enclosure of early replicators inside of membranousvesicles: First step towards cell membranes. - Orig. Life Evol. Biosph. 39:545–558

Poole AM, Jeffares DC, Penny D (1999) Early evolution: prokaryotes, the new kids on the block.Bioessays 21(10): 880–889

Rodin AS, Szatmary E, Rodin SN (2011) On origin of genetic code and tRNA before translation. BiologyDirect 6:14

Tinsley E, Khan, SA (2006) A Novel FtsZ-Like Protein Is Involved in Replication of the Anthrax Toxin-Encoding pXO1 Plasmid in Bacillus anthracis. J. Bacteriol. 88(8): 2829–2835

148

P3.07 Role of fungi in the weathering of different iron-bearingminerals

Clarisse Balland-Bolou-Bi1∗, Sara J. M. Holmstrom1, Sabina Hoppe2, Nils G. Holm1,

1Stockholm University, Deptartment of Geological Sciences, Stockholm, Sweden2Stockholm University, Deptartment of Applied Environmental Science, Sweden∗E-mail of corresponding author: Clarissebolou-bi@geo.su.se

Fungi belong to the microorganisms including yeast and mold that likely play a critical role in rockand mineral weathering and in soils formation. These biological processes are important for geochemicalcycles. Fungi likely invaded land millions of years ago before plants. Moreover, after the apparition ofearly terrestrial plants that did not really have true roots, the colonisation of land by photosyntheticeukaryotes depends strongly on mycchorizal fungi. Fungi are of primary importance in the formation ofsoil via the weathering of rocks. Fungi weather rocks in two ways: mechanically by forming tunnels wherethe hyphae grow, and chemically by lowering the pH of water and by producing low-molecular organicmolecules (siderophores and organic acids).

To quantify the rates and to investigate the mechanisms of fungal weathering, fungal strains wereisolated from podzolic soil in Norunda site in Sweden under three different tree species (spruce, birch andscots pine). This study is focused on the characteristics of individual species regarding the mechanismsby which they regulate chemical weathering. The ability of each fungal strains to weather differentiron-bearing minerals (olivine, biotite, magnetite and hendenbergite) were tested in miniaturized devices.We monitored low-molecular organic molecules produced by fungi, microbial biomass, pH, and free andlabile iron fraction released during the experiments using electro chemical detection - Anodic StrippingVoltammetry (ASV). The use of different iron-bearing minerals will permit to define if the mechanismused by fungi depends of the genotype or depends of the cristallochemistry of the minerals.

149

P3.08 Comet Hazard to the Earth

Oleksandr Potashko

Department of Marine Geology and Sedimentary Ore Formation NASU, Kiev, Ukraine∗E-mail of corresponding author: tumburland@gmail.com

It is known that in the Middle Ages comets were considered a threat to humanity. These days themain hazard for the Earth seem to be asteroids as impact factors. Comets are impact hazards too,besides they contain organics and maybe microorganisms. The organic components have been found oncomets as remotely so directly – trapping particles passing through a comet’s tail. Mission ”Stardust”returned to Earth samples of a comet in 2006. An even stronger result can be obtained from the missionwith a landing on a comet, and succeeding in the analysis of captured organic matter and the deliveryof samples back to the Earth. The Earth periodically passes through the remnants of cometary tails. Itmakes sense to explore these organic residues. First attempts have been made – air probes sent to theheight of 40 km and they brought ‘new species of bacteria, which are not found on Earth’ [1]. Of coursenew species may originate from the Earth – new species have regularly been found in extreme environ-ment – near underwater volcano, in Antarctica, in deserts. Nevertheless, some of these microorganismsmay have originated from a comet. This is an important question for future research.

References:

1. Discovery of New Microorganisms in the Stratospherehttp://www.isro.org/pressrelease/scripts/pressreleasein.aspx?Mar16 2009

150

P3.09 Crystallization and sublimation of non-racemic mixturesof natural amino acids: a path towards homochirality

Arkadii V. Tarasevych1∗, Jean-Claude Guillemin2,

1Institute of Bioorganic Chemistry and Petrochemistry, NAS of Ukraine, Kiev, Ukraine2Institut des Sciences Chimiques de Rennes, Ecole Nationale Superieure de Chimie de Rennes, CNRS,France∗E-mail of corresponding author: arkadiitarasevych@gmail.com

Homochirality of biologically important molecules such as amino acids and sugars is a prerequisite forthe origin of life. There are different forces or mechanisms in the Universe to trigger off the primary im-balance in the enantiomeric ratio. Very likely the initial bias of one type of enantiomers over the other onEarth was arisen from the inflow of extraterrestrial matter (carbonaceous meteorites). The phase transi-tions (crystallization, sublimation) of non-racemic mixtures of enantiomers are ones of the most probablemechanisms for the homochirogenesis (1). The sublimation, almost uninvestigated subject and forgottenfor 30 years, revealed recently a pathway to the enantioenrichment of natural amino acids (2). Startingfrom a mixture with a low content of an enantiopure amino acid a partial sublimation gives a considerableenrichment (Fig. 11). In our further experiments we combined two first-order phase transitions of aminoacid(s) mixtures: crystallization and sublimation. The results show the possibility of the transfer ofenantiopurity between different amino acids (3). Subliming a crystallized mixture of racemic amino acidswith an enantiopure one we found that the sublimate is a non-racemic mixture of the same handedness forall components (Fig. 12). The significance of the studies can be realized taking into account that just 5 of22 proteinogenic amino acids are able to homochiral self-organization. The relevance of these studies tothe Prebiotic Earth and to the evolution of the single handedness of biological molecules will be discussed.

References:

1. D. G. Blackmond, Phil. Trans. R. Soc. B, 366, 2878 (2011)

2. A. Bellec, J.-C. Guillemin, Chem. Commun., 46, 1482 (2010)

3. A. V. Tarasevych, A. E. Sorochinsky, V. P. Kukhar, J.-C. Guillemin, Chem. Commun., submitted(2012)

Figure 11: Diagrams of changing of enantiomeric excess during partial slow sublimation of non-racemicmixtures of natural amino acids (Ala, Leu, Phe, Pro, Val). •- L+DL, H - L+D mixtures.

151

Figure 12: Deracemization of natural aliphatic AA via ”crystallization - sublimation” protocol.

152

P3.10 Accounting the effect of life on Earth using AtmosphericChemical Disequilibrium. Impact on the definition of HabitableZone

Eugenio Simoncini∗, Alfonso Delgado-Bonal, Francisco J. Martin-Torres

CAB - INTA-CSIC, Torrejon de Ardoz, Madrid, Spain∗E-mail of corresponding author: eugenio.simoncini@gmail.com

The presence of living systems has affected (and still affects) the thermodynamic conditions of Earth.Clear evidences can be seen in atmospheric and crust composition and biogeochemical cycles charac-teristics. Most importantly, during the 1960s, atmospheric disequilibrium has been proposed as a signof habitability of Earth and, in general, of a planet (Lovelock 1965, 1975). Here we study chemicaldisequilibrium in planetary atmospheres. In particular we compare, at first order, the disequilibrium inEarth’s and Mars’ atmospheres, using a newly developed methodology which takes into considerationchemical non-equilibrium conditions. Our results have an impact on the definition of Habitable Zone byconsidering appropriate physical-chemical conditions of planetary atmospheres.

References:

Lovelock J. E., A physical basis for life detection experiments. Nature, Vol. 207, 568-570. 1965

Lovelock J. E., Thermodynamics and the recognition of alien biospheres. Proc. R. Soc. Lond., B. 189,167 - 181. 1975

153

P4.01 MarcoPolo-R Asteroid Sample Return Mission: tracingorigins

Antonella Barucci1, Pascale Ehrenfreund2∗, Patrick Michel3, Hermann Bohnhardt4, John R. Brucato5,Elisabetta Dotto6, Ian A. Franchi7, Simon F. Green7, Luisa-M. Lara8, Bernard Marty9, Detlef Koschny10

1LESIA-Observatoire de Paris, 92195 Meudon Principal Cedex, France2Space Policy Institute, George Washington University, Washington DC, USA3Univ. Nice, CNRS, OCA, France4MPS, Katlenburg-Lindau, Germany5INAF-Obs. of Arcetri, Italy6INAF-Obs. of Roma, Italy7Open Univ., Milton Keynes, UK8IAA-CSIC, Granada, Spain9CRPG, Nancy, France10ESTEC, ESA, Netherlands∗E-mail of corresponding author: pehren@gwu.edu

MarcoPolo-R is a sample return mission to a primitive Near-Earth Asteroid (NEA) selected for anassessment study at ESA in the framework of ESA Cosmic Vision program. MarcoPolo-R will rendezvouswith a primitive NEA, scientifically characterize the object at multiple scales, and return a unique sampleto Earth unaltered by the atmospheric entry process or terrestrial weathering. The baseline target is abinary asteroid (175706) 1996 FG3, which provides enhanced science return. MarcoPolo-R will returnbulk samples from an organic-rich binary asteroid to Earth for laboratory analyses, allowing us to:

• explore the origin of planetary materials and initial stages of habitable planet formation

• identify and characterize the organics and volatiles in a primitive asteroid

• understand the unique geophysics, dynamics and evolution of a binary NEA.

The baseline mission scenario of MarcoPolo-R to 1996 FG3 includes a single primary spacecraft, carryingthe Earth re-entry capsule and sample acquisition and transfer system, will be launched by a Soyuz-Fregatrocket from Kourou.The scientific payload includes state-of-the-art instruments, e.g. a camera systemfor high resolution imaging from orbit and on the surface, spectrometers covering visible, near-infraredand mid-infrared wavelengths, a neutral-particle analyser, a radio science experiment and optional laseraltimeter. The mission will answer to fundamental astrobiological questions “How does the Solar Systemwork?” and “What are the conditions for life and planetary formations?”.

154

P4.02 COSIMA-Cometary Secondary Ion Mass Analyzer

Khawaja Nozair Ashraf1∗, Harry Lehto1, Johan Silen2, Kirsi Lehto1, Tuomo Lonnberg1, Harald Kruger3,Martin Hilchenbach3, COSIMA team

1University of Turku, Finland2Finnish meteorological institute, Finland3Max Planck institute for solar system research, Germany∗E-mail of corresponding author: khaash@utu.fi

Comets are icy conglomerates of rock and dust. They were formed during the earliest phases of thesolar system. Ground based observations reveal limited information about the detailed composition ofcomets. Nearly everything we know about the shapes and the other details of comets come from pre-vious cometary missions. The Rosetta mission of the European Space Agency was launched in 2004towards the comet 67P/Churyumov-Gerasimenko. It will rendez-vous the comet in 2014 and remain inits proximity for the two years. Twenty-two [1] experiments are onboard Rosetta spacecraft consisting ofa lander and an orbiter. The Cometary Secondary Ion Mass Analyzer (COSIMA) is one of instrumentsonboard Rosetta orbiter. It is a high resolution time-of-flight (TOF) mass spectrometer with a resolutionof m/∆(m) ∼ 2000 at m=100 [2]. COSIMA will collect cometary dust particles in situ at low speedfor characterizing the elemental, molecular, mineralogical and isotopic composition of dust particles inthe coma of comet 67P/CG. Understanding the details of the chemical composition of dust at cometswill address questions such as what is the role of comets in delivering the raw materials for the onset oflife on Earth and at what state and complexity this raw material is. In the calibration campaign of theCOSIMA, the errors in the data follows the Poisson properties.

References:

1. R. Schulz et al, 2009, Solar System Research, 43, 343

2. J. Kissel et al, 2007, Space Sci. Rev., 128, 823

155

P4.03 The history of liquid water in the early solar system: cluesfrom carbonate minerals in carbonaceous chondrite meteorites

Paula Lindgren∗

School of Geographical and Earth Sciences, University of Glasgow, Glasgow G12 8QQ, UK∗E-mail of corresponding author: Paula.Lindgren@glasgow.ac.uk

Carbonaceous chondrite meteorites are derived from asteroidal parent bodies that formed during theearliest history of the solar system when a mixture of anhydrous minerals, amorphous material and icesaccreted in the solar nebula. Liquid water became available as the water ice melted, probably due to heatreleased from the decay of radioactive isotopes and possibly also from impact heating and/or redistribu-tion of Al26-rich material via impacts [e.g. 1, 2]. Evidence of this once liquid water can be seen in theCI and CM carbonaceous chondrites, which have undergone extensive aqueous alteration resulting in theformation of secondary minerals including carbonates [e.g. 3, 4]. We have studied the composition andmicrostructure of carbonates in a range of CI and CM carbonaceous chondrites to better understand themechanism, timescale and spatial distribution of liquid water in the early solar system. The techniquesused are scanning and transmission electron microscopy (SEM and TEM), electron backscatter diffrac-tion (EBSD) and isotope analyses via nanoSIMS. Results include multi-phase generations of carbonatesand several episodes of deformation recorded in the carbonate microstructure, demonstrating a complexaqueous system and deformation history. Mn-Cr dating of carbonates shows that the onset of aqueousalteration took place within 3.9±1.2 Ma after solar system formation.

References:

1. A.J. Brearley, In: H.S. Lauretta and H.Y.Jr McSween (eds). Meteoritics and the Early Solar SystemII. The University of Arizona Press, Tuscon, 587-624 (2006).

2. F.J. Ciesla, T.M. Davison and G.S. Collins, 43rd Lunar and Planetary Science Conference, Ab-stract#1676. (2012).

3. M.E. Zolensky, R. Barrett and L. Browning, Geochimica et Cosmochimica Acta, 57, 3123-3148(1993).

4. M.E. Zolensky, D.W. Mittlefehldt, M.E. Lipschutz, M-S. Wang, R.N. Clayton, T.K. Mayeda, M.M.Grady, C. Pillinger and D. Barber, Geochimica et Cosmochimica Acta, 61, 5099-5115 (1997).

156

P4.04 Cathodoluminescence microcharacterization of apatite andcalcite in the Martian meteorites: An Implication for Astrobiol-ogy

Arnold Gucsik1, Ulrich Ott1, Hirotsugu Nishido2, Kiyotaka Ninagawa3

1Max Planck Institute for Chemistry, Mainz, Germany2Research Institute for Natural Sciences, Okayama University of Sciences, Okayama, Japan3Department of Applied Physics, Okayama University of Sciences, Okayama, Japan∗E-mail of corresponding author: a.gucsik@mpic.de

It has been already demonstrated that the Scanning Electron Microscope-Cathodoluminescence (SEM-CL) microscopy and spectroscopy are powerful techniques for the study of minerals from different originsuch as from volcanic, tectonic and metamorphic formations. This systematic work of a combination of themicroscopical and spectroscopical instruments has been performed on the Martian meteorites emphasizingthe water-related rock types such as carbonates, sulphates, phosphates, and chlorides. Moreover, theterrestrial reference materials have been compared with these minerals from the Martian meteorites. Theresults from these studies might give some new insights to understand more about the presence of thewater and its astrobiological application as well as possible evolution of the life forms on Mars in pastand present. A technological development of the in-situ planetary cathodoluminescence microscopy andspectroscopy for the robotic missions in Mars is discussed in this study as it would be a potentially usefultool to detect the above-mentioned mineralogical and astrobiological samples.

157

P4.05 Habitability in the Solar System and new planetary mis-sions

Pauli E. Laine

University of Turku, Turku, Finland∗E-mail of corresponding author: paerla@utu.fi

Definition of habitability depends on the organisms under consideration. One way to determine hab-itability of some environment is to compare it’s certain parameters to environments where extremophilicmicroorganisms thrive on Earth. Some current limit values are, e.g. temperature −20 to −121◦C, pH0–13, and radiation up to 16,000 Gy. We can also define more common habitability criterions from thelife as we know it. These criterions include basic elements (CHNOPS), liquid water and an energy source.We know that some locations in our Solar System fit in at least some of these limits and criterions.

This presentation has emphasis on possibilities raised by new planetary missions, such as NASA’s MarsScience Laboratory Curiosity in 2012, ESA’s ExoMars missions in 2016 and 2018, and JUICE (JUpiterICy moons Explorer) in 2033. These missions will explore habitability of Mars, Europa, Ganymede andCallisto. In this paper I will compare defined habitability criterions to instrumentation (e.g. Curiosity’sSAM(1)) documentation whether these missions could validate the habitability of Mars and those Jovianmoons. We can see that Mars will have more in depth analysis.

References:

1. P. Mahaffy, Sample Analysis at Mars: Developing Analytical Tools to Search for a HabitableEnvironment on the Red Planet, Geochemical Society Publication, 141 (2009)

158

P4.06 Exploring Martian Habitability

Anna Neubeck1∗, Magnus Ivarsson2

1Department of geological sciences, Stockholm university, Stockholm, Sweden2Swedish Museum of Natural History, Stockholm, Sweden∗E-mail of corresponding author: anna.neubeck@geo.su.se

Ever since localized release of CH4 was detected in the martian atmosphere in 2003 the concept ofa subsurface biosphere on Mars has been revived and discussed (Formisano et al. 2004; Mumma et al.2009; Ehlmann et al. 2011). The H2-driven deep biosphere on Earth consisting of methanogens has beenused as a representative to explain a potential martian counterpart. The presence of such a subsurfacebiosphere on Earth has involved a change of view regarding the distribution of life on our planet, whichhave consequences for the understanding of habitability on other terrestrial bodies (Pedersen 1993; Helle-vang 2008). Methanogens require Ni for their growth and as a consequence the microbial fractionation ofNi isotopes can be used as a biomarker for activity of methanogenic communities. Methanogens use thelighter of the Ni isotopes that result in an enrichment of the heavier isotopes and thus a mass dependentfractionation of the Ni isotopes (Cameron et al. 2009). This suggests that the stable isotopes of Ni maybe a fundamental trace metal biomarker for methanogens, and possible other microorganisms (Cameronet al. 2009). In fact, the extent of the fractionation produced by methanogens have the potential for Niisotopes to function as a class-specific indicator for these microorganisms since other non-methanogenicmicroorganisms do not fractionate Ni. The Ni system may be more straightforward and useful in thisrespect than stable isotopes of other elements like Fe, Se and Cu. Nickel is not as easily affected byabiotic redox conditions as Fe and that makes it more easily preserved in the rock record and demon-strably addressed to methanogenesis. However, there are still uncertainties of how the Ni uptake ofmethanogens work and whether it leaves detectable variations in minerals and rocks that can be usedas reliable biomarkers (Hausrath 2007). Terrestrial basalts are also often associated with Ni and couldpotentially be a source of Ni for methanogens in the deep subsurface on Earth as well as on Mars. Nickelis typically measured in soils and rocks on Mars (Yen et al. 2006) and is often associated with basalts.Samples from Mars could therefore be analyzed for stable Ni isotope fractionation in order to identifyany possible influences from life or other processes. However, prior to such analyzes is the need for com-parable data of analogous material from Earth and experimental tests for the Ni fractionating propertiesof methanogenic archaea. Only a few studies on the Ni fractionating properties of methanogens havebeen made and much more work is needed. Nickel fractioning ratios have to be measured in fossilizedmicroorganisms as well as in laboratory experiments. Today, no studies have been published on the frac-tionation of Ni in fossilized microorganisms. However, we have detected enrichments of Ni in fossilizedmicroorganisms and ichnofossils, respectively, from two separate locations (unpublished data). The firstlocation is La Galega Ni mine, Ojen, located in the ultra mafic Ronda massif, Spain, where ichnofossilsenriched in Ni (∼ 5 wt% Ni) are observed in olivines. The second location is in drilled basalts from theODP Leg 197, collected at the Koko Seamount, Pacific Ocean. Fossilized microorganisms observed incarbonate filled veins and vesicles have been found to contain small amounts of Ni (∼ 1 wt% Ni). Thus,Ni is present in association with fossilized microorganisms from environments and more extensive analysisis required to understand the magnitude, uptake, preservation and fractionation of Ni in microfossils. So,by analyzing Ni fractionation in terrestrial fossilized microorganisms as well as in laboratory experiments,we could gain a deeper understanding of the processes of chemolithoautotrophy as well as the extent ofNi fractionating capabilities of abiotic and biological processes. This knowledge could be useful in theanalysis of terrestrial samples from the deep biosphere and samples returned from Mars.

References:

Cameron V, Vance D, Archer C & House CH (2009) A biomarker based on the stable isotopes of nickel.PNAS 106: 10944 - 10948

Ehlmann BL, Mustard JF, Murchie SL, Bibring JP, Meunier FC, Fraeman AA & Langevin Y (2011)Subsurface water and clay mineral formation during the early history of Mars. Nature 479: 53 - 60

159

Formisano V, Atreya S, Encrenaz T, Ignatiev & Giuranna M (2004) Detection of methane in the atmo-sphere of Mars. Science 306: 1758-1761

Hausrath EM, Liermann L. J., House C. H., Ferry J. G., Brantley S. L. (2007) The effect of methanogengrowth on mineral substrates: will Ni markers of methanogen-based communities be detectable inthe rock record? Geobiology 5: 49-61

Hellevang H (2008) On the forcing mechanism for the H2-driven deep biosphere. International Journalof Astrobiology 7: 157-167

Mumma MJ, Villanueva GL, Novak RE, Hewagama T, Bonev BP, DiSanti MA, Mandell AM & SmithMD (2009) Strong Release of Methane on Mars in Northern Summer 2003. Science 323: 1041-1045

Pedersen K (1993) The deep subterranean biosphere. Earth-Science Reviews 34: 243-260

Yen AS, Mittlefehldt DW, McLennan SM, Gellert R, Bell JF, III, McSween HY, Jr., Ming DW, McCoyTJ, Morris RV, Golombek M, Economou T, Madsen MB, Wdowiak T, Clark BC, Jolliff BL, SchroderC, Bruckner J, Zipfel J & Squyres SW (2006) Nickel on Mars: Constraints on meteoritic materialat the surface. J. Geophys. Res. 111: E12S11

160

P4.07 Habitability and early life on Mars

Frances Westall∗, Marylene Bertrand, Frederic Foucher, Nicolas Bost

CNRS-OSUC-Centre de Biophysique Moleculaire, Rue Charles Sadron, 45071 Orleans cedex 2, France∗E-mail of corresponding author: frances.westall@cnrs-orleans.fr

The last ten years of orbital and in situ missions to Mars have provided a wealth of information thatare beginning to show that there may never have been an extended period when Mars was ‘warm andwet’ and globally habitable. There is still much discussion concerning past habitability of Mars based onthe mineralogical and geomorphological records. The picture that is emerging is of a planet that mayhave been partially habitable at different periods of time. The question here is, did habitable conditionsexist for long enough for life to appear (105-106 y)? If so, were the habitable conditions sustained longenough to allow any evolution from the stage of tiny primitive cells (more primitive than prokaryotes)?What if martian life (if it ever appeared) remained in a really primitive state, more primitive thanknown terrestrial prokaryotes and perhaps somewhat similar (in terms of size) to virus-like organisms,because of the limited possibilities for evolution? What would be the implications for its distribution,biosignatures, and detection? To what extent can knowledge of early terrestrial life help in the searchfor potentially very primitive martian life? We conclude that, if life appeared on Mars, either at thesurface or eventually in the subsurface, the changing spatial and temporal habitability conditions meanthat (1) its distribution will be very heterogenous, (2) that the life forms may have been smaller and moresimple than the oldest preserved terrestrial prokaryotes, and (3) that their detection in situ on Mars maybe extremely challenging. The eventuality of super-imposed signatures due to changing habitability aswell as variability in the conservation of eventual traces of past/present life will have great influence onstrategies to search for traces of life in situ, and on the collection and return samples for study on Earth.

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P4.08 Limitations to a biological iron cycle on Mars

Sophie L. Nixon1, Charles Cockell1∗, Martyn Tranter2

1School of Physics and Astronomy, The University of Edinburgh, Edinburgh, UK2Bristol Glaciology Centre, School of Geographical Sciences, University of Bristol. BS8 1SS, UK∗E-mail of corresponding author: c.s.cockell@ed.ac.uk

Anaerobic microbial metabolisms found on the Earth are the most plausible candidates for under-standing potentially analogous energy gathering metabolisms on Mars. The iron-rich nature of Marsraises important questions as to whether the planet could support energy acquisition by iron-reducingmicroorganisms past or present. On Earth, these microorganisms reduce ferric iron typically by oxidisinga variety of organic compounds; the transfer of electrons in these redox reactions is exploited and ulti-mately used to generate ATP [1]. Although numerous ferric iron-bearing minerals have been identifiedon Mars, such as hematite [2], nontronite [3] and jarosite [4], organics have not been unambiguouslydetected on the Martian surface. We therefore have evidence of only half of the iron reduction redoxcouple. However, the absence of evidence does not necessarily demonstrate evidence for the ubiquitousabsence of organic matter on Mars. It has been estimated that 8.6×106 kg of meteoritic material reachesthe surface of Mars each year, and 2.4×105 kg of this is thought to represent the unaltered carbon content[5].

The organic-bearing class of meteorites, carbonaceous chondrites, contain a number of solvent-solubleorganic compounds that have been identified as utilisable electron donors for microbial iron reduction,including alcohols, carboxylic acids and amino acids. However, the amino acids tested to date representstandard protein-forming amino acids, such as alanine, serine and leucine; although these amino acids havebeen identified in meteorites, a number of non-proteinogenic amino acids are also common to carbonaceouschondrites [6], and represent potential electron donors that have yet to be tested. It is important to testthese less typical compounds in order to constrain the range of potential electron donors, and hencecandidate redox couples, that may support microbial iron reduction on Mars.

We report results from incubations with a model iron-reducing microorganism, Geobacter metallire-ducens [7], in which a range of non-proteinogenic meteoritic amino acids were supplied as the sole electrondonors with ferric iron as the terminal electron acceptor. Where candidate amino acids exhibit chirality,enantiomers (D- and L-) were tested separately as well as the mixed form (DL-) of the compound. Ironreduction was monitored by periodic measurements of ferrous iron (Fe2+) production in solution usingthe ferrozine assay, and cell growth was evaluated by total cell counts throughout the course of the in-cubations. Incubations with amino acids in which cell numbers increased and Fe2+ was produced wereconsidered representative of utilisable electron donors for microbial iron reduction. These results haveimplications for our understanding of the feasibility for Mars to support microbial energy acquisitionthrough iron reduction, past or present.

References:

1. Madigan, M.T., Martinko, J.M., 2006. Brock Biology of Microorganisms, 11th ed. Pearson PrenticeHall.

2. Christensen, P.R. et al., 2001. Journal of Geophysical Research, 106, 23,823-823,871.

3. Bibring, J.-P. et al., 2005. Science, 307, 1576-1581.

4. Squyres, S.W. et al., 2006. Journal of Geophysical Research, 111, E12S12.

5. Flynn, G.J., 1996. Earth, Moon, and Planets, 72, 469-474.

6. Cronin, J.R., Pizzarello, S., 1983. Advances in Space Research, 3, 5-18.

7. Lovley, D.R. et al., 1993. Archives of Microbiology, 159, 336-344.

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P4.09 Scale-integrated spectral characterisation of mineralogicalanalogues to Mars at Rio Tinto

Damhnait Gleeson1,2, David Fernandez-Remolar1, P. Martin3, V. Ruiz2

1Centro de Astrobiologıa, CSIC-INTA, Madrid, Spain2Ingenierıa y Servicios Aeroespaciales, Spain3European Space Astronomy Center, ESA, Spain∗E-mail of corresponding author: dgleeson@cab.inta-csic.es

Iron-sulfur and phyllosilicate assemblages within the Rio Tinto basin of Huelva province in Spain showmineralogical similarities to sites on the surface of Mars as determined by orbital and lander datasets.Exploration of Mars surface environments is intermittent and resolution-limited, and additional layers ofinformation available for terrestrial analogue sites may extend incomplete planetary datasets. Character-ising mineralogy in satellite, field and laboratory reflectance spectra of Rio Tinto sites can determine howaccurately Mars-relevant mineralogies are represented in orbital data. Comparisons with Mars datasets,such as OMEGA and CRISM, will provide insights into planetary surface conditions. 1. IntroductionDepositional environments of interest on the surface of Mars include the sulfate- and hematite-rich sed-imentary deposits characterised by Opportunity at Meridiani Planum, and the extensive phyllosilicatedeposits of the early Noachian detected by the OMEGA instrument onboard Mars Express. Partial en-vironmental analogues to both mineralogies may be found within the Rio Tinto Basin in southwesternSpain [1,2]. Carrying out a detailed spectral characterisation of the visible-near infrared (Vis-NIR) signa-tures of Rio Tinto minerals across varying scales will allow direct comparisons to be made between theseterrestrial datasets and analogous Mars datasets provided by hyperspectral imagers including OMEGAand CRISM, which are currently providing information on Mars surface environments. The additionallevel of detail provided by laboratory analysis of hand samples, which provides ground truth for remotelysensed datasets in terrestrial environments, can also provide insights into Mars surface conditions forareas which have yet to be visited by lander. 2. Methods Hyperspectral satellite coverage of sites withinthe Rio Tinto basin were acquired from the Hyperion instrument onboard Earth Observing 1 (EO-1).Vis-NIR field spectra of sites within the Rio Tinto basin were collected using an ASD field spectrometer,and laboratory-based measurements of returned samples were made in the same wavelength range. MIR,Raman and XRD of returned samples will provide additional mineralogical ground truth. The datasetsgenerated can be utilized to characterise mineralogy from orbital to in situ scales to determine howaccurately ground conditions are represented in orbital datasets. 3. Discussion and Conclusions Interac-tion between materials in field mixtures can lead to potential interferences between endmembers and/oroffsets in spectral features, which can obscure or hinder the identification of certain minerals [e.g. 3].Such interactions can be difficult to predict on the basis of library spectra collected using pure materials.Determination of which diagnostic spectral features can be identified in field mixtures is an advantage ofcollecting data in real world environments, and can be used to aid interpretation of planetary datasets.This study will utilize the dynamic sulfur and iron deposits of Rio Tinto as an analogue of Mars sitessuch as Meridiani Planum, using the many scales of observation available for the terrestrial sites as ameans of extending our view of Mars surface conditions from the orbital view to which we are frequentlylimited. The development of a scale-integrated (orbital to in-situ) approach to exobiological investiga-tions and the design of effective surface science in planetary environments are facilitated by investigationof terrestrial analogues and biosignatures, which can inform our view of how microbiological activitiesare tied to macroscopic mineral deposits [4, 5].

Acknowledgements: This work is supported by an ESA SRE-OD Research Contract with INSA/CAB.

References:

1 Fernandez-Remolar, D.C., Morris, R.V., Gruener, J.E., Amils, R., & Knoll, A.H. (2005). TheRio Tinto basin, Spain: Mineralogy, sedimentary geobiology, and implications for interpretation ofoutcrop rocks at Meridiani Planum, Mars. Earth and Planetary Science Letters, 240, 149-167.

163

2 Fernandez-Remolar, D.C., Prieto-Ballesteros, O., Gomez-Ortiz, D., Fernandez- Sampedro, M., Sar-razin, P., Gailhanou, M., & Amils, R. (2011). Rio Tinto sedimentary mineral assemblages: Aterrestrial perspective that suggests some formation of phyllosilicates on Mars. Icarus, 211, 114-138.

3 Gleeson, D.F., Pappalardo, R.T., Grasby, S.E., Anderson, M.S., Castano, R., Chien, S., Doggett,T., Mandrake, L., & Wagstaff, K. (2010). Characterization of a sulfur-rich Arctic spring site andfield analog to Europa using hyperspectral data. Remote Sensing of Environment, 114, 1297-1311.

4 Gleeson, D.F., Williamson, C., Grasby, S.E., Pappalardo, R.T., Spear, J.R., & Templeton, A.S.(2011). Low temperature S0 biomineralization at a supraglacial spring system in the CanadianHigh Arctic. Geobiology, 9, 360-375.

5 Gleeson, D.F., Pappalardo R.T., Anderson, M.S., Grasby, S.E., Mielke, R.E., Wright K.E., andTempleton, A.S. (2012) Biosignature Detection at an Arctic Analog to Europa. Astrobiology,Volume 12, Number 2, 135-150.

164

P4.10 The International Space Analogue Rock Store (ISAR): Akey tool for future planetary and astrobiologicaly exploration

Nicolas Bost1,2∗, Frances Westall1, Claire Ramboz2, Frederic Foucher1

1Centre de Biophysique Moleculaire, CNRS, Rue Charles Sadron, 45071 Orleans Cedex 22Institut des Sciences de la Terre d’Orleans, 1A rue de la Ferollerie, 45071 Orleans Cedex 2∗E-mail of corresponding author: nicolas.bost@cnrs-orleans.fr

In order to prepare the next in situ space missions to Mars (MSL, ExoMars-2018), we have created acollection of Mars analogue rocks for calibrating and testing present and future space flight instruments.This collection is called the International Space Analogue Rockstore (ISAR) and is hosted at the CNRSand the Observatoire des Sciences de l’Univers en Region Centre (OSUC) in Orleans, France. For max-imum science return, all instruments on a single mission should ideally be tested with the same suiteof relevant analogue materials. The ISAR aims at fulfilling this role by providing suitable materials toinstrument teams [1, 2]. This collection is accompanied by an online database of all relevant structural,textural, and geochemical data (www.isar.cnrs-orleans.fr). The database will also be available duringmissions to aid interpretation of data obtained in situ. The collection is composed of different minerals(silicates, carbonates, phosphates, sulfates) and rocks. It includes a variety of basalts (tephrite, primitive,silicified), komatiites (fresh and weathered), as well as artificially fabricated Martian basalts having thesame geochemical composition as the Gusev Crater basalts on Mars [3]. The collection includes differentsedimentary rocks: carbonates associated with volcanic lithology, BIF, hydrothermal cherts, and silicifiedvolcanic sediments (some containing traces of fossil life [4]).

References:

1. Westall F. et al. LPI contribution 1608, 1346, 42nd LPSC, 2011

2. Bost N. et al. Icarus, in review

3. Bost N., et al. Meteorit. Planet. Sci. 45, 2012

4. Westall F. at al. Planet. Space Sci. 59, 2011.

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P4.11 Hydrothermal, deuteritic and acidic basalt alteration atthe Skouriotissa mine, Cyprus: relevance for Mars and astrobio-logical implications

Nicolas Bost1,2∗, Frances Westall1, Claire Ramboz2, Frederic Foucher1

1Centre de Biophysique Moleculaire, CNRS, Rue Charles Sadron, 45071 Orleans Cedex 22Institut des Sciences de la Terre d’Orleans, 1A rue de la Ferollerie, 45071 Orleans Cedex 2∗E-mail of corresponding author: nicolas.bost@cnrs-orleans.fr

Basalts are the most common rock type on the Martian surface and the products of aqueously alteredbasalts and hydrated minerals associated with basalts are of particular interest as possible tracers of apast, slightly more clement climate on the planet and/or magmatic processes [1,2]. Study of alterationprocesses of basalts on Earth that show some similarities to surface and subsurface processes occurringon Mars will help understand and interpret Martian features. Basalts and their alteration product arevery relevant in the search of traces of life [3,4].

The Skouriotissa mine in Cyprus is an open pit copper mine, consisting of a volcanogenic sulphidedeposit (VMS) and exposed in the upper pillow basalt formation in the Troodos ophiolitic area. Thebasalt has been altered by (1) hot hydrothermal processes, (2) seawater hydrothermal processes in sub-marine conditions before the ophiolite formation, and (3) acidic water (pH<5) associated with the miningactivities.

We have analysed the mineralogical evolution of the basalt through different alteration facies (phyl-losilicates, sulfates, and zeolite) depending on the type of alteration. Similar mineralogical associationshave been described on Noachian/early Hesperian period of Mars (e.g. [1,2,5]) and may have been formedby the same kinds of processes.

These suites of rocks form a part of the collection of Mars analogue rocks that is being prepared atthe CNRS - Observatoire des Sciences de l’Univers en Region Centre (OSUC) in Orleans to help calibratepresent and future flight instruments. This collection is named “International Space Analogue Rockstore(ISAR)” and the relevant information is contained in the website: http://www.isar.cnrs-orleans.fr[6,7].

References:

1. Bibring J.-P., et al. Science 312, 2006

2. Ehlmann B., et al. Nature 479, 2011

3. Cavalazzi B. et al. Astrobiology 11, 2011

4. Bost N., et al., Martian Exploration: Do not underestimate the volcanic rocks as a possible habitat,this conference;

5. Meunier A., et al. in prep.

6. Westall F. et al. LPI contribution 1608, 1346, 42nd LPSC, 2011

7. Bost N., et al., The International Space Analogue Rock Store (ISAR) : A key tool for futureplanetary and astrobiologicaly exploration, this conference.

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P4.12 Variation of the modern Martian atmospheric compositionas a result of cometary and asteroidal impacts

Anatoliy K. Pavlov1, Maria A. Vdovina1, Alexander A. Pavlov2

1 Laboratory of Mass Spectrometry, Ioffe Physico-Technical Institute of Russian Academy of Sciences,St. Petersburg, Russia2NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

∗E-mail of corresponding author: mariya.vdovina@gmail.com

Despite decades of research, Martian atmospheric composition still presents a number of excitingunresolved mysteries. Martian atmosphere contains both “main” components (CO2, N2, H2O) and ”sec-ondary” components N gases produced in the atmospheric photochemical processes. There are relativelystable ”secondary” gases such as CO, O2 and H2 and short-lived species like HOx, NOx radicals and O3.Mixing ratios of stable components are measured (Kliore et al., 1973; Owen et al., 1977; Krasnopolsky,2006; de Pater and Lissauer, 2001) experimentally and also predicted by theoretical modeling. Howevercurrent photochemical models have difficulties explaning the observed CO mixing ratio. Predicted valueof 5 · 10−4 is significantly lower than measured 8 · 10−4 (Krasnopolsky, 2006). Another unexplained mys-tery of the Martian atmosphere is the detection of methane by several independent groups (Formisanoet al., 2004; Mumma et al., 2004). Surprisingly, it was also reported that methane is variable seasonallyand geographically (refs) despite methane’s 300-year photochemical atmospheric lifetime. Regardless,whether methane variability is indeed real, any detection of methane requires a relatively recent source.Here we model the effects of cometary and asteroidal impacts on the chemical composition of the currentthin Martian atmosphere. We are particularly interested on the magnitude and longevity of variationsof CO, CH4 and sulfur bearing species. However, comets and asteroids will bring also a number of othergases. At the same time composition of impactor can significantly vary. Comets contain a lot of volatilehydrocarbons (0.1-10%) and frozen gases (CO, SO2, H2S, NH3 etc). From the other hand, asteroids arelack in volatiles but can be rich of carbon and sulfur in fixed form. Large impactors could have producednon-equilibrium state by step injection of great amounts of gases. Particularly impacts of comets orlarge-size meteorites cold lead to the input of H2, CO, CH4, SO2 etc. (Kress and McKay, 2004; Zahnle,1990) For objects like KT-impactor the injection of CO can exceed 1% of total mass of atmosphere. Ifthe impactor is a comet the input of H2 may even be more than CO injection. Injection of gases could beimportant for increasing of greenhouse effect and impact on climate and hypothetical Martian biosphere.We propose that the observed levels of CO and CH4 in the current Martian atmosphere could result froma continuous bombardment of the Martian surface by comets and asteroids of different sizes and chemicalcomposition.

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P4.13 Determining the extent of the martian water table usinga simple lithospheric model

Euan P. Monaghan∗, Manish R. Patel, Karen Olsson-Francis,

Department of Physical Sciences, The Open University, Milton Keynes, United Kingdom∗E-mail of corresponding author: e.p.monaghan@open.ac.uk

A key aspect in the search for habitable environments at the planetary level is the presence of liquidwater. A massive volume of water appears to have flowed across the early martian landscape [1, 2], butthe average pressure and temperature on the planet currently lies below the triple point. The ultimatefate of water on Mars remains an open question, however several mechanisms have been invoked toexplain its removal from the surface inventory; these include atmospheric escape [3, 4], crustal oxidationand trapping [5], and a water table persisting in the subsurface [6].

We have developed a pressure and temperature model of the martian crust in order to constrain thedepths at which liquid water - ranging from pure solution to hypersaline mixtures - may persist. Thedepth at which the eutectic temperature is reached - taken here as the uppermost boundary for bulkliquid water - is dependent on a number of variables including geothermal heatflow, thermal conductivityand lithospheric density. While creating an accurate model using these variables is limited by a paucityof data, boundary conditions for such a simple model are demonstrated, and key trends identified.

An example of further complication to this model is then discussed. Changes in martian surfacetemperature have a corresponding impact on the temperature at depth, at a rate determined primarilyby the thermal conductivity of the crust. Modeled temperature variation over a 30 Ma timescale [7] isused to estimate the likely persistence and nature of a subsurface habitable environment on Mars overrecent geological time.

References:

1. Carr, M.H., Water on Mars. 1996, New York: Oxford University Press

2. Squyres, S.W. and J.F. Kasting, Early Mars: How warm and how wet? Science, 1994. 265(5173):p. 744

3. McElroy, M.B. and Y.L. Yung, Oxygen isotopes in the Martian atmosphere: Implications for theevolution of volatiles. Planetary and Space Science, 1976. 24(12): p. 1107-1113

4. Watson, L.L., et al., Water on Mars: Clues from deuterium/hydrogen and water contents of hydrousphases in SNC meteorites. Science, 1994. 265(5168): p. 86-90

5. Bish, D.L., et al., Stability of hydrous minerals on the martian surface. Icarus, 2003. 164(1): p.96-103

6. Clifford, S.M., A model for the hydrologic and climatic behavior of water on Mars. Journal ofGeophysical research, 1993. 98(E6): p. 10,973-11,016

7. Laskar, J., et al., Long term evolution and chaotic diffusion of the insolation quantities of Mars.Icarus, 2004. 170(2): p. 343-364

168

P4.14 Local Martian resources allow efficient cyanobacterial biomassand biohydrogen production

Gayathri Murukesan, Taina Laiho, Kirsi Lehto

University of Turku, Finland∗E-mail of corresponding author: gamuru@utu.fi

With the anticipation of manned missions to Mars, new means need to be explored and investi-gated for the production of different life support supplies (oxygen, food and fresh water) for the crews.Long-duration mission to Mars will require high total amount of the supplies, and replenishment of thelife-support supplies from the local Martian resources would be very useful. Water is available on theMartian surface, either in form of the ground water or permafrost and in the polar glaciers, and carbondioxide is abundant in the Martian atmosphere. With sunlight, these substrates can be converted tocarbohydrates and to oxygen, via the photosynthetic process. However, this process requires also mineralnutrients, mainly P, N, K, Ca, which are required in levels that contribute a few percent of the total freshbiomass, plus a set of important micronutrient, which are required in much lower levels, mounting up toabout 0.02% of the produced biomass. These also could be obtained from the local resource, i.e. releasedfrom basaltic regolith, except for N, which is not present in the basalt, and is present in the Martianatmosphere only on 2.7% level. Therefore, recycling of the nitrogenous nutrients becomes essential forstable maintenance of the life-support supplies. It is well established that several cyanobacterial species,e.g. Cynechococcus and Synechocystis, and also the edible Arthrospira sp. thrive well in 100% CO2, inlow pressures (100 mbars or less). In Mars, the air pressure and temperature of the large scale cell-culturefacilities need to be adjusted to some minimal level where the water evaporation can be controlled by sat-urated vapor, but where the temperature still allows adequate cell growth. Such low pressure conditionsalso reduce the toxic or harmful effects that would be caused by high (nearly 100%) CO2 concentrationin high (1 atm) pressure. It is known that certain cyanobacterial species (e.g. Anabaena cylindrical) canreadily grow on rocky surfaces, and particularly on basalt, which has a suitable mineral composition tosupport bacterial growth [1]. Here we report that A. cylindrical thrives well on plain powdered basalt,supplemented by a N-source, also in the high CO2/low pressure atmospheric conditions. The effect of thisatmosphere on the acidification of the growth medium and the bioweathering of the nutrients is currentlyinvestigated. Interestingly, the growth of the A. cylindrical in these low-nitrogen/high CO2 conditions wasfound to induce strong heterocyst formation, associated with strongly enhanced biohydrogen production,providing a potential new form of energy production from this system. For recycling of the nitrogenousnutrients from organic waste it is important that they are bound to some insoluble form, particularlyto prevent the evaporation and leaching of ammonia. At university of Turku, a new vermiculite-basedmineral substrate (GeoTrapRM) has been developed that efficiently absorbs ammonium-ions into its crys-talline structure, and binds also other nitrogenous compounds (nitrate and nitrite) to its surface. Thesebound nitrogen compounds are still available for bioweathering, and are thus easily recyclable to plantnutrient. We have shown that nitrogen-loaded GeoTrapRM serves as a very efficient matrix for supplyingnitrogen to the basalt-based microbial or plant cultures.

References:

1. Olsson-Francis and Cockell, 2010, Planet. Spa. Sci. 58 1279–1285.

169

P4.15 Microbial community shifts within a spacecraft associatedclean room complex

Christine Moissl-Eichinger1∗, Alexander Probst1, Anna Auerbach1, Petra Rettberg2

1Department for Microbiology and Archaea Centre, University of Regensburg, Germany2German Aerospace Center (DLR), Linder Hoehe, 51147 Cologne, Germany∗E-mail of corresponding author: christine.moissl-eichinger@biologie.uni-r.de

Missions under planetary protection requirements are limited with respect to their biological contami-nation. In particular, microbes are of interest due to their potential survival and growth in extraterrestrialenvironments and the chance to affect life-detection experiments. Spacecraft is therefore constructed inclean rooms and is subject of frequent contamination measurements. As earlier studies have shown, cleanrooms can harbor an adapted, in many cases multi-resistant microbial community, which could possiblyendure desiccation and higher radiation doses as expected during space flight. These microbial charac-teristics are of particular interest for missions and planetary protection constraints. Before entering aclean room, staff has to change cloths and to pass an (air-shower) lock in order to minimize particle andbiological contamination. Technical items, however, are cleaned thoroughly and often sterilized beforebeing moved into the spacecraft assembly environment, so that human staff is in most cases the maincarrier of microbial contaminants. The influence of human activity is reflected by the cultivable andnon-cultivable microbial diversity: The overwhelming majority of detected microbes belong to human-associated bacterial genera like Staphylococcus, Acinetobacter or Propionibacterium. During our recentsampling campaign performed at the EADS facilities in Friedrichshafen, Germany, we took samples notonly from two clean rooms (ISO 8 and ISO 5) but also from the changing room and a typical office room(check-out room), located in very close vicinity to changing and clean room. We are currently analyzingthe microbial diversity by a multi-faceted approach, trying to detect the contamination route of bacterialand archaeal components. A combination of cultivation techniques were applied (ESA standard pro-tocols to determine microbial bioburden, specific enrichment of oligotrophic, anaerobic and alkalophilicbacteria), as well as several molecular techniques (qPCR, 16S rRNA gene cloning), to visualize specificmicrobial communities and their variation within the entire facility. In this talk, we will present theresults and discuss possible impacts on clean room maintenance and planetary protection in general.

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P4.16 The application of Cold Atmospheric Plasma (CAP) forthe sterilisation of spacecraft materials

Petra Rettberg1∗, Simon Barczyk1, Hubertus Thomas2, Satoshi Shimizu2, Tetsuji Shimizu2, TobiasKlampfl2, Gregor Morfill2

1DLR, Institute of Aerospace Medicine, Koln, Germany2Max-Planck-Institut fur extraterrestrische Physik, Garching, Germany∗E-mail of corresponding author: petra.rettberg@dlr.de

Plasma, often called the fourth state of matter after solid, liquid and gas, is defined by its ionizedstate. Ionization can be induced by different means, such as a strong electromagnetic field applied witha microwave generator. The concentration and composition of reactive atoms and molecules producedin Cold Atmospheric Plasma (CAP) depends on the gases used, the gas flow, the power applied, thehumidity level etc.. In medicine, low-temperature plasma is already used for the sterilization of surgicalinstruments, implants and packaging materials as plasma works at the atomic level and is able to reach allsurfaces, even the interior of small hollow items like needles. Its ability to sterilise is due to the generationof biologically active bactericidal agents, such as free radicals and UV radiation. In the project PLASMA-DECON (DLR/BMWi support code 50JR1005) a prototype of a device for sterilising spacecraft materialand components was built based on the surface micro-discharge (SMD) plasma technology. The producedplasma species are directed into a closed chamber which contains the parts that need to be sterilised. Totest the inactivation efficiency of this new device bacterial spores were used as model organisms because inthe COSPAR Planetary Protection Policy all bioburden constraints are defined with respect to the numberof spores (and other heat-tolerant aerobic microorganisms). Spores from different Bacillus species andstrains, i.e. wildtype strains from culture collections and isolates from spacecraft assembly cleanrooms,were dried on three different spacecraft relevant materials and exposed to CAP. The specificity, linearity,precision, and effective range of the device was investigated. From the results obtained it can be concludedthat the application of CAP proved to be a suitable method for bioburden reduction/sterilisation in theframe of planetary protection measures and the design of a larger plasma device is planned.

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P4.17 MSR backward contamination - Considering the requiredcontraints

Nicolas Walter (on behalf of the ESF Study Group)1

European Science Foundation∗E-mail of corresponding author: nwalter@esf.org

Potential Martian life is one of the key scientific issues supporting the development and implementationof a MSR mission. While the perspective of discovering forms of extra-terrestrial life is promising, it alsoleads to carefully considering the impact of bringing back alien biological entities to Earth with the riskof inadvertently releasing them in the terrestrial biosphere. In its 2009 report Assessment of PlanetaryProtection Requirements for Mars Sample Return Missions the NRC-SSB acknowledges that even ifprobabilities of large-scale pathogenic or ecological effects are considered to be very low, they are alsoconsidered not to be nil. The report recommended that: ”Based on current knowledge of past andpresent habitability of Mars, NASA should continue to maintain a strong and conservative program ofplanetary protection for Mars sample return. That is, samples returned from Mars by spacecraft should becontained and treated as though potentially hazardous until proven otherwise. No uncontained Martianmaterials, including spacecraft surfaces that have been exposed to the Martian environment, should bereturned to Earth unless sterilized.” Without any knowledge of potential Martian organisms, it is hardlypossible to predict how these could behave and evolve in the terrestrial environment and thus, what theconsequences of their release would be, if any. As this potential threat cannot be evaluated properly andconfidently, a cautious approach has to be applied. Under contract for the European Space Agency, theEuropean Science Foundation set up an international interdisciplinary group of experts to ”Recommendthe level of assurance for the exclusion of an unintended release of a potential Mars life form into theEarth’s biosphere for a Mars Sample Return mission”. The starting point of this activity was a guidelineexpressed in the late ’90s specifying that: ”The probability that a single unsterilised particle of 0.2 microndiameter or greater is released into the Earth environment shall be less than 10−6”. After consideringthe relevance of the approach adopted by this guideline, the Group reconsidered the two parameters itwas based upon: the size and the probability of a release. The size parameter was reviewed in the lightof the latest developments in the field of microbiology, in particular considering that some free livingmicroorganisms have been isolated after filtration through 0.1 µm filters. Great attention has been paidto viruses and Gene Transfer Agents (GTAs). The maximum recommended probability of a release hasbeen discussed and reconsidered using well defined benchmarks currently used by regulators and policymaking bodies worldwide in the field of risk tolerability.

1The presentation will give and detail the updated constraint recommended by the ESF study group. ESF Study Groupcomposition: Walter Ammann (Global Risk Forum GRF Davos, CH), John Barros (University of Washington, USA), AlanBennett (Health Protection Agency, UK), Jim Bridges (University of Surrey, UK), Joseph Fragola (Valador, Inc, USA),Armel Kerrest (University of Western Brittany, FR), Herve Raoul (INSERM - Jean Merieux P4 laboratory, FR), PetraRettberg (DLR, DE), John Rummel (COSPAR PPP - East Carolina University), Erko Mika Salminen (ECDC, EU/SE),Stackebrandt (DSMZ -Retired, DE)

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P4.18 Monitoring of the microbial community during simulatedflight to Mars

Petra Schwendner1,4∗, Simon Barczyk1, Francesco Canganella2, Viacheslav Ilyin3, Reinhard Wirth4, Har-ald Huber4, Reinhard Rachel4, Petra Rettberg1,

1German Aerospace Center, Institute of Aerospace Medicine, Radiation Biology Department, Cologne,Germany2University of Tuscia, Viterbo, Italy3Institute of Biomedical Problems, Moscow, Russia4Center for Microbiology and Archaea, University of Regensburg, Regensburg, Germany∗E-mail of corresponding author: petra.schwendner@dlr.de

The skin is the largest human organ consisting of 1.8 m2 of diverse habitats and niches. Estimationsrevealed that the human body is colonized by approximately 1014 diverse microbial cells. The majority ofthe skin microbiome (ca. 1013 microbes) is consisting of symbiotic microorganisms that protect the bodyagainst invasion by more pathogenic or harmful microbes which can be of potential danger for humans.Furthermore, prolonged confinement of humans will have influences on the selection, development andcomposition of different microbial populations in closed habitats. These circumstances might lead tochanges in the interactions between microbes and the human. It is unclear if commensally pathogensmight thrive better, spread and accumulate in this confined niche. This effect might lead to an increasedthreat for a weakened person. Additionally, conditions during spaceflight appear to down regulate theimmune system of astronauts. The influence of closed systems on the microbial community is stillunknown and not comparable with natural environments. The here reported survey will deepen theknowledge of the impact of closed systems on the microbial composition.

Mars 500 was the first ground based full duration simulation of a manned flight to Mars from June2010 till November 2011. The crew, six candidates from different countries, lived, worked and performedscientific experiments in this closed habitat where the exchange with the external environment is veryrestricted. This isolation program is a unique opportunity to investigate the impact of confinement onhuman and environmental microbial communities. One of the scientific experiments is called MICHA(Microbial ecology of confined habitats and human health). The aim of the project is the survey of themicrobial flora in different biotopes from the start till the end of the simulation study. During the 520days confinement the natural colonisation and changes over the time (monthly samplings) were monitoredusing different sampling tools. One focus is on the microbial accumulation of selected surfaces via swabsamples, but in addition another point of interest are airborne germs obtained by air filtration. Airsampling included the filtration of 500 l air with 30 l/min on a gelatine filter at nine different locations.Additionally, 25 cm2 of twelve selected surfaces were swabbed. One aliquot of each surface sample wasused to cultivate mesophilic bacteria whereas the other half was heat-shocked for determination of spore-forming and/or heat-resistant strains. The investigation of cultivable microorganisms showed that theoverall bioburden in the air and on different surfaces was moderate compared to other non-confined rooms.The highest number of microorganisms was found in the air of complex EU-150 where the crew membersspent most of their time, i.e. community room, dining area and one tested individual compartment. Thiscorresponds roughly to the results from surfaces at the different locations. First phylogenetic resultsindicate the dominance of microorganisms associated with humans, especially Staphylococcus species,whereas environmental microorganisms are found to a lower extent.

Besides cultivation based analyses, the microbial inventory will be also studied on molecular level viaDNA isolation and 16S rRNA gene specific amplification.

The collection of bioburden and biodiversity data is essential to develop strategies to maintain a non-hazardous environment for the astronauts during long time manned space missions. Furthermore, all ourinvestigations are required for the implementation of planetary protection guidelines for manned Marsmissions.

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P4.19 New technology developments in exploration techniques:what they mean for astrobiology

Christian Muller1∗, Nadia This1, Didier Gillotay2, Cedrik Depiesse2, Didier Moreau1

1B.USOC, Brussels, Belgium2Belgian Institute for Space Aeronomy, Brussels, Belgium∗E-mail of corresponding author: christian.muller@busoc.be

Recent developments in the ISS technology programme and new propulsion designs are currentlytested and might change the architecture of the exploration programme. These could give it for the firsttime in fifty years a rapid new impulsion and even lead to an earlier than expected manned mission toMars.

Three examples of these breakthroughs will be presented: the first is the METERON robot networkproject, robots are commanded from the station by the astronauts and simulates commanded operationson a planetary surface (Bosquillon de Frescheville et al, 2011) (1). The intent is to have more agileoperations than with a robot commanded from the earth. METERON involves NASA, ESA, ROSCOS-MOS and DLR. Currently, B.USOC manages the METERON operations on the ISS as Facility ReferenceCentre. A second example is the ‘Robotic Refuelling Mission (RRM)’ put forward by NASA and CSAand developing fresh satellite-servicing technologies which can be used either during the cruise to theplanets or during surface operations.

Both examples could lead to techniques reconciling Mars planetary protection with early mannedspace mission. Any Mars landing on Mars is catalogued by COSPAR as category IV: Lander or probemissions to locations with the potential to host life and for which there is a possibility of contaminationby Earth life. Presently, the category excludes human landing before Mars life is characterized or Mars isproved to be definitively sterile. COSPAR policy expanded category IV to three different subcategoriesand the stricter one (IVc will probably be definitively off-limit for human explorers. The designationof special regions for Mars, pertinent to Category IVc, has been addressed by COSPAR since 2002.COSPAR defined a special region as ‘a region within which microorganisms from Earth are likely topropagate, or a region which is interpreted to have a high potential for the existence of extant Martianorganisms (2).’

The third example is a proposed architecture of a network of surface and orbit based UV sensorsdesigned to characterise UV climatology on the surface of Mars to assess both habitability and potentialeffects on human explorer. The proposed designed will be made possible by novel electric propulsiontechniques using Hall effect which could reduce the transfer time to planetary targets and allow the dis-tribution of multiple payloads.

References:

1. Bosquillon de Frescheville, F., Martin,S. Policella, N., Patterson,D. , Aiple, M. and Steele, P.: Setup and Validation of METERON end-to-end Network for Robotic Experiments, 11th Symposiumon Advanced Space Technologies in Robotics and Automation - ASTRA 2011, 12-14 April 2011,ESTEC, (2011)

2. Committee on an Astrobiology Strategy for the Exploration of Mars, National Research Council,An Astrobiology Strategy for the Exploration of Mars, The National Academies Press, Washington,(2007)

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P4.20 Dust investigation on NASA’s Mars Science Laboratory

Jaqueline K. Jensen, Asmus Koefoed, Morten Bo MadsenMars Group, Astrophysics and Planetary Science, Niels Bohr Institute, University of Copenhagen, Den-mark

When NASA’s Mars Science Laboratory mission (MSL) lands August 6th, 2012, the Mars group atthe Niels Bohr Institute, University of Copenhagen will be participating with a small investigation usinginstrumentation on board the MSL rover (Blake, 2011; Wiens et al., 2011). The Danish investigation willfocus on dust and soils and in particular on the mineralogy of the nano-sized iron oxides or oxyhydroxidesand any potential connection between these minerals and organics on Mars. The reason for this interestis that the exact mineralogy reflects the environment in which these originally formed (if primary) – orthe processes they have undergone since formation (if secondary).

The MSL rover, Curiosity, will land in Gale crater, start investigations within the crater plains andwork its way at least somewhat up the 5 km high Mount Sharp in the center of the crater. Along thetraverse phyllosilicates resulting from long term contact of igneous minerals with liquid water more than3.5 billion years ago, and sulphates formed when water became less abundant and the environment morearid will be investigated (Ehlmann, 2011). Also ancient occurrences of pockets with high concentrationsof dust, expected to be present in the lowest layers of the sediments, will be investigated. Of particularinterest is any possible connection to activity of water – or even biology. Formation and evolution ofultrasmall particles of oxyhydroxides are particularly sensitive to the environment, including any putativepresence of organics.

About 20% of organic carbon in sediments on Earth is directly bound to reactive iron phases. OnEarth, therefore, reactive iron phases serve as a sink for organic carbon and thus strongly influence globalcycles of carbon, oxygen and sulphur. It is known that several bacteria catalyze reduction of structuralFe(III) in clay minerals (Nealson et al., 2011; Templeton et al., 2009). Will it be possible to see ancienttraces of results of such processes in the lowest and oldest layers of Mount Sharp? According to RobertHazen (Hazen et al., 2010) there are about 4500 mineral types on Earth today, what about Mars? Whatkind of mineral species and how many types are present in the most ancient sediments, and will there beany biominerals or bio-markers to be found on Mars?

During several years the Mars group has been studying Mars dust (Madsen et al., 2009). The figureabove shows results of studies of dust captured on magnets on Mars Exploration Rover Opportunity.Identification of a not yet identified component shown in the Mossbauer spectrum (marked with a redarrow), a component which for lack of a better name is called nanophase oxide, is the aim of the Danishinvestigation on MSL. As of 2012 no perfect Earth analogue to the reddish Martian dust has been found.In our laboratory nano-scale changes on surfaces of common silicate minerals which has been subjected toMars-similar environmental conditions are being studied in a Mars environmental chamber, an Arduino

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controlled vacuum chamber in which it is possible to irradiate samples with UV radiation in a CO2

containing atmosphere. Under usual circumstances, geological (solid-gas-) reactions are very slow. Innano-scale, some of these changes are something one can follow from week to week. One of the goals is tofind out what conditions are needed for the formation of the basic components of the Martian red dust.

We believe that this work will gain from participation in the meeting and interaction with other par-ticipants of the workshop.

References:

Blake, D. (2011), A historical perspective of the development of the CheMin mineralogical instrumentfor the Mars Science Laboratory (MSL 11) Mission, The Geochemical News 145, 22-40.

Ehlmann, B. (2011), Diverse aqueous environments during Mars first billion years: the emerging viewfrom orbital visible-near infrared spectroscopy, The Geochemical News 145, 11-21.

Hazen, R.M., D. Papineau, W. Bleeker, R.T. Downs, J.M. Ferry, T.J. McCoy, D.A. Sverjensky and H.Yang Mineral evolution, American Mineralogist 93. (2010),

Madsen, M.B., et al. (2009), Overview of the magnetic properties experiments on the Mars ExplorationRovers, J. Geophys. Res. 114, E06S90, doi:10.1029/2008JE003098.

Nealson, K.H. et. al., The Utility of Shewanella japonica for microbial fuel cells, Bioresour. Technol.,102, 290-7. (2011)

Templeton, A., and E. Knowles, Microbial transformations of minerals and metals, Annu. Rev. EarthPlanet Sci. 37, 367-91. (2009)

Wiens, R.C., S. Maurice, and the ChemCam team (2011), The ChemCam Instrument Suite on the MarsScience Laboratory Rover Curiosity: Remote Sensing by Laser-Induced Plasmas, The GeochemicalNews 145, 41-8.

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P4.21 Wind-driven erosion of silicates as a source of oxidants inMartian soil

Ebbe Norskov Bak∗, Svend Knak Jensen, Jon Merrison, Per Nørnberg, Kai W. Finster

Mars Simulation Laboratory, Aarhus University, Denmark∗E-mail of corresponding author: ebbe.bak@biology.au.dk

It is unknown which agents are responsible for the oxidizing properties of the Martian soil and howthey are formed. Crushing quartz leads to surface radicals that can create hydrogen peroxide in water.We propose saltation and the resulting erosion of silicates on Mars as a source of oxidants. To simulatethe saltation, we gently tumbled quartz sand under different atmospheres in sealed quartz flasks. Thequarts sand was subsequently analyzed for oxidizing properties. We saw erosion of the quartz sand andaggregations of fine quartz particles within weeks of tumbling. The eroded quartz caused production ofhydrogen peroxide in amounts positively correlated with tumbling time. As long as the eroded quartzwas kept in a dry atmosphere it remained reactive. This process may thus allow for accumulation ofpotentially oxidizing surface radicals on Mars.

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P4.22 The Moon polar volatiles: what they can tell us

Mikhail V. Gerasimov ∗

Space Research Institute of the Russian Academy of Sciences, Moscow, Russia∗E-mail of corresponding author: mgerasim@mx.iki.rssi.ru

Introduction

Relatively small and airless differentiated planetary bodies (the Mercury, the Moon, large asteroids, etc.)can be considered as an early transient state of accumulation of the Earth and other larger planets.Organic components of the building meteoritic blocks were sufficiently destroyed by starting differentia-tion. The search for organic compounds on such bodies is important for understanding the earliest pathsof exobiological processes. The discovery of noticeable hydrogen concentration in the polar regions ofthe Moon was among the most exciting events of its exploration. Analysis of lunar samples delivered byApollo and Lunar missions as well as of Moon meteorites showed that solid material was strongly depletedin volatiles. The amount of water in lunar samples is in the range of 64 ppb – 5 ppm [1]. Concentrationof hydrogen in polar regolith provides the estimation of water concentration at a level of 46wt.% [2,3]as average for meter to two meter deep surface layer. Such an increase in the water concentration is aresult of migration of water molecules from hot equatorial latitudes to cold traps of the polar northernand southern regions. The question about the diversity and source of volatiles (including organics) isstill open. The aim of the paper is to discuss possible sources of volatiles and related differences in theirpattern.

Degassing of the interior

Endogenous source of volatiles is provided by degassing of heated interior of planetary bodies. In thiscase chemical composition of released gases reflects thermodynamic equilibrium of gases over typicalmagmas at temperatures around 1000◦C. The composition of such gas mixtures is characterized bydomination of H2O, CO2, and SO2 over other H, C, and S containing components. Carbon containinggases are mainly present by CO2, CO, and hydrocarbons. CO/CO2 ratio here is typically far below 0.1level. Hydrocarbons are a minor part of carbon-containing gases and are mainly aromatic hydrocarbons,alkanes, and cycloalkanes. Sulfur containing gases are mainly SO2, H2S, and Sx with SO2 being dominant.Isotopic ratios of volatile elements should be the same as for the bulk Moon.

Interaction of solar wind protons with surface rocks

An interesting mechanism of water production on the Moon comes from the interaction of solar windprotons with lunar surface rocks. Energetic solar wind protons with the absence of an atmospheric shieldcan react with oxygen of surface rocks and produce water molecules as end product. Such a mechanismprovides a source of pure water on the Moon with solar hydrogen isotopes and Moon rocks oxygenisotopes. There can be an outcome for hydrocarbons if any reasonable quantity of carbon is presenton the surface. Degassing of impacting meteorites and comets Volatile components, which are deliveredby meteorites and comets, are released during hypervelocity impacts upon lunar surface. The formingimpact-generated vapor cloud is hot and dense enough to form gas mixture with a composition driven bychemistry of the cloud. It was shown experimentally [4] that despite differences in possible types of targetsilicates the forming compositions of gases are qualitatively similar and have the following characteristics.The portion of carbon monoxide is much higher compared to volcanic gases and the CO/CO2 ratio is 1.Hydrocarbons are presented mainly by alkenes and PAHs and amount up to 10% of CO+CO2. Sulfurcontaining gases are presented by SO2, CS2, H2S, and COS in decreasing sequence. CS2 production incase of ordinary chondrites amounted to about half of SO2 and for COS it amounted to about severalpercent [4]. Production of HCN was also measured. Noticeable release of water was also detected.Experimental investigation was performed for terrestrial minerals and rocks and for carbonaceous andordinary chondrites as well. No principal difference in the chemistry of cometary impacts is expected.

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What lunar polar volatiles can tell us

Information on the chemical composition of deposited gases and on isotopic composition of main volatileelements seams to be a key for discrimination between different sources of lunar polar volatiles. Almostpure water in the polar depositions with solar hydrogen isotopes and surface rocks oxygen isotopes willindicate in favor of solar wind interaction mechanism. The presence of CO2 and SO2 components ad-ditionally to H2O will indicate whether endogenous magmatic degassing or exogenous impact-induceddegassing of meteorites and comets. CO/CO2 ratio can be a good criterion between these two sourcesbut there is a problem of efficiency of CO trapping since it requires sufficiently lower temperature thanfor trapping of CO2. At least, CO/CO2 ratio higher than 0.1 can be an indication in favor of impactsource. Sufficient portion of CS2 also can be an argument in favor of impact source. This argument willbe supported additionally by the presence of HCN and domination of alkenes over alkanes. The cometarysource of volatiles can be indicated by isotopic composition of hydrogen while impacts of meteorites aswell as magmatic degassing will provide terrestrial D/H ratio. The complexity and diversity of organicmolecules will indicate the level of prebiotic synthesis related to small planetary bodies. There are twomissions - Luna-Globe and Lunar-Resource which are now under preparation in Russia for launch after2015. Both missions are aimed to put landers in northern and southern polar regions of the Moon forinvestigation of possible depositions of water and other volatile components. The gas-analytic experi-ment “ALPOL” is aimed on comprehensive investigation of the inventory of volatiles (including organiccompounds) in the regolith of polar regions.

References:

1. McCubbin, F.M. et al., PNAS, 107, 11223–11228 (2010).

2. Mitrofanov, I. G. et al., Science, 330, 483–486 (2010).

3. Colaprete, A. et al., Science, 330, 463–468 (2010).

4. Gerasimov, M.V., GSA Special Paper, 356, 705–716 (2002).

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P4.23 Raman mapping of silicified biological remains

Frederic Foucher∗, Frances Westall

Centre de Biophysique Moleculaire, UPR CNRS 4301, rue Charles Sadron, 45071 Orleans Cedex 2, France∗E-mail of corresponding author: frederic.foucher@cnrs-orleans.fr

In this study, we demonstrate the usefulness of Raman mapping as a very powerful tool for studyingcarbonaceous matter and for the detection and identification of (bio-)minerals associated with silicifiedbiological remains. In particular, these minerals include opal. Opaline silica is metastable and normallyconverts to quartz but, in poorly metamorphosed rocks, such as cherts from the Draken formation, Sval-bard, -800 Ma, conversion has been inhibited by the kerogen matrix within which the opal precipitated.Interestingly, the Raman maps also document very fine variations in the spectrum of the carbonaceousmatter in relation to the biological remains. Thus, Raman mapping permits identification of certaincharacteristics of the organic and mineral signature directly as a function of the microfossils studied.Moreover, trace phases, such as opal or rare sparsely disseminated mineral phases, or small changes inRaman spectra, are more likely to be observed in mapping mode compared to spot analysis mode.

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P4.24 Infrared and Raman Study of the Thermal Degradationof Biomolecules

Bettina Bodeker1∗, Ute Bottger2, Heinz-Wilhelm Hubers2, Jean-Pierre deVera2, Stefan Fox1, HenryStrasdeit1

1Department of Bioinorganic Chemistry, Institute of Chemistry, University of Hohenheim, 70599 Stuttgart,Germany2DLR Institute of Planetary Research, 12489 Berlin, Germany∗E-mail of corresponding author: Bettina.Boedeker@gmx.de

On the Hadean Earth and the Noachian Mars, geochemical and geophysical conditions were probablysimilar (Strasdeit, 2010). Today, however, the conditions on the two planets differ substantially. Forexample, short-wavelength UV radiation hits the martian surface because of the thin atmosphere. Dueto the lack of a magnetic field, cosmic radiation even penetrates to a certain extent into the martiansurface. Therefore, it is more probable that possible life exists in the subsurface of Mars (Dartnell et al.,2012). The aim of future Mars missions to search for life and the study of terrestrial molecular fossilsprompted us to conduct experiments that might help to identify remains of extinct or extant life enclosedin rocks and sediments. The starting point of our study was the scenario of thermal events, such as im-pacts or volcanism that destroy mineral-embedded microorganisms. These organisms may leave chemicalsignatures characteristic for biomolecules. Their chemical remains may also contain information aboutthe details of the particular thermal event such as temperature and duration. In our study, we chose asmodel biomolecules lecithin and hemin, among others. Amphiphiles (in cell membranes) and porphyrins(e.g. as chlorophylls in photosynthesis) are of high relevance in past and modern biology because theyare very common in many organisms. Therefore, it seems plausible to regard lecithin, hemin and re-lated molecules as a reasonable approximation to the real biochemical components of early terrestrialand possible early and present Martian life forms. Additional experiments with whole microorganismswere conducted to get insights into the degradation process of life forms in the thermal events mentionedabove. As phyllosilicates have been discovered in various regions of the martian surface (Chevrier andMathe, 2007; Poulet et al., 2005), we used kaolinite as the mineral matrix for our biomolecules and or-ganisms. Raman spectroscopy is one of the techniques we apply. It is especially suited to gain uniquefingerprints of molecules (Tarcea et al., 2008). Each biomolecule and model organism was separatelymixed with kaolinite. These samples were exposed to temperatures between 200 and 900◦C in a non-oxidizing atmosphere of pure nitrogen. In addition to Raman spectroscopy, Fourier transform infraredspectroscopy has been used to analyze the residues. The resulting spectra will be discussed, especiallywith respect to their possible application in the detection of life from thermally altered biological material.

References:

Chevrier V, Mathe PE (2007) Planet Space Sci, 55:289-314

Dartnell LR, Page K, Jorge-Villar SE, Wright G, Munshi T, Scowen IJ, Ward JM, Edwards HGM (2012)Anal Bioanal Chem 403:131-144

Poulet F, Bibring J-P, Mustard JF, Gendrin A, Mangold N, Langevin Y, Arvidson RE, Gondet B,Gomez C & the Omega Team (2005) Nature 438:623-627

Strasdeit H. (2010) Palaeodiversity 3(Supplement):107-116; http://www.palaeodiversity.org/pdf/03Suppl/Supplement_Strasdeit.pdf

Tarcea N, Frosch T, Rosch P, Hilchenbach M, Stuffler T, Hofer S, Thiele H, Hochleitner R, Popp J(2008) Space Sci Rev 135:281-292

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P4.25 Raman Laser Spectroscopy - a valid tool to detect biogenicsubstances in Mars Regolith Simulants as well as bio-minerals andorganic substances produced by lichens

Joachim Meeßen1∗ Ute Bottger2 Dana Grunow2 Heinz-Wilhelm Hubers2 Jean-Pierre de Vera2 FranciscoJavier Sanchez3 Jorg Fritz4 Rosa de la Torre3 Elke Rabbow5 Sieglinde Ott1

1Institute of Botany, Heinrich-Heine-University, Dusseldorf, Germany2Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany3Instituto Nacional de Tcnica Aeroespacial (INTA), Torrejon de Ardoz, Madrid, Spain4Museum fur Naturkunde, Leibniz-Institute, Humboldt-University, Berlin, Germany5Institute of Aerospace Medicine, German Aerospace Center (DLR), Cologne, Germany∗E-mail of corresponding author: joachimmeessen@gmx.de

One objective of the ExoMars Mission scheduled for 2018 is to search for pre-cursors or indications ofpast and present life on Mars. With Raman Laser Spectroscopy (RLS) – a Pasteur Payload Instrumentonboard – organic compounds and mineral products of biological activity can be identified. The physicalproperties of biomolecules can be strongly influenced by surrounding substrata, displayed as divergingRaman spectra in the sample components. Furthermore, organic substances are discussed to be degradedby complex interactions with Martian substrates and UV radiation. Therefore, it is essential to know ifand how such interactions shift, conceal, or degrade the spectra of biogenic compounds.

In the context of the BIOMEX project (Biology and Mars Experiments, ILSRA-AO 2009) the spectralproperties of nine biogenic substances were investigated by means of confocal Raman microscopy (Witecalpha 300R, λ = 532 nm) as pure samples and combined with two types of Martian Regolith Simulants(S- and P-MRS): β-carotene, naringenin, quercitin, melanin, parietina (all serve as photoprotectants),chlorophyll α, chitin, cellulose, and agar-agar (as an EPS-substitute). Measurements were performedbefore and after exposition to the Sample Verification Test (SVT-) conditions at DLR Cologne, simulating18 month of exposure to conditions as foreseen for the BIOMEX experiment on EXPOSE-R2 (by meansof simulated Mars atmosphere, temperature, and irradiation). Representative data on their detectabilityand stability are presented.

Additionally, Raman spectral differences of the lichen Circinaria gyrosa were investigated (former As-picilia fruticulosa; proofed several times on their high resistance in astrobiological studies [1,2]). Differentstrata revealed different Raman signals and we were able to detect the biogenic mineral calcium oxalatein its inner medulla as well as chitin, β-carotene, and chlorophyll. As a result, mineral products of lichenactivity may be seen as suitable biomarkers.

References:

1. J. Raggio, et al. (2011). Astrobiology, 11 (4), 281-292

2. F. J. Sanchez, et al. (2012). Planetary and Space Sciences (submitted)

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P4.26 Electron detachment for collisions of carbon based molec-ular negative ions with molecular nitrogen

Rodrigo Nascimento1,2∗, Marcelo M. Sant’anna1, Ginette Jalbert1, Luiz F. Coelho1, N. V. de CastroFaria 1

1Instituto de Fısica, Universidade Federal do Rio de Janeiro - UFRJ, Brazil; rodfer@if.ufrj.br2Centro Federal de Educacao Tecnologica Celso Suckow da Fonseca - CEFET/RJ, Brazil∗E-mail of corresponding author: rodfer@if.ufrj.br

The Cassini mission has recently shown the presence of numerous molecular negative ions in theatmosphere of the Saturn’s moon, Titan. It is known that Titan, like the Earth, has N2 as the mostabundant gas in its atmospherical composition. In the present study, we have measured the electrondetachment cross sections for a number of molecular negative ions (in the keV range) colliding withmolecular Nitrogen. The ions produced in our laboratory for the present work are CH−, C−2 , C2H−,C4H−, CN−.

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P4.27 Does a strong magnetic field protect a planetary atmo-sphere from stellar winds?

Hans Nilsson, Masatoshi Yamauchi∗, Stas Barabash,

Swedish Institute of Space Physics (IRF), Kiruna, Sweden∗E-mail of corresponding author: M.Yamauchi@irf.se

Escape of matter from planetary atmosphere takes place mainly in two forms: as neutral atoms(thermal escape, photochemical escape and as energetic atoms after charge exchange from ions) and asions. Since the latter is trapped by the magnetic field, total loss in the form of ions are considered to bestrongly influenced by the presence of a planetary intrinsic magnetic field.

Using in-situ observation of ions that exceed the escape velocity at Venus, Earth and Mars, weexamined the atmospheric loss in the form of ions from these three planets. We found that for currentconditions the loss rate is similar for the three planets. A somewhat surprising fact is that for increasedsolar wind activities, the atmospheric escape may actually be stronger form a magnetized planet. Thismakes the current Mars condition a mystery because it has lost most of its atmospheres and oceans, ifthey were ever there. We discuss the possible cause of this peculiarity as well as the expected dependencyto the solar input (FUV, solar wind) in the meeting.

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P4.28 ”Following the Energy” in an arctic analogue for icy,sulphur-rich sites on Mars and Europa

Katherine E. Wright1∗, Charles Williamson2, Stephen E. Grasby3, John R. Spear2, Alexis S. Templeton1

1University of Colorado at Boulder, Boulder, CO 80309, USA2Civil and Environmental Engineering, Colorado School of Mines, USA3Geological Survey of Canada, Natural Resources Canada, Canada∗E-mail of corresponding author: wrightk@colorado.edu

The “Follow the Energy” [1] approach to habitability involves looking at the energy sources availablein an environment in order to predict the types of microbial metabolism that could survive there. Wetested the ”Follow the Energy” approach to assessing the habitability of icy sulphur-rich sites on Marsand Europa by studying an analogue site at Borup Fiord Pass Glacier in the Canadian High Arctic. Atthis site a cold, alkaline, spring containing sulphate, thiosulphate and very high levels of sulphide (4.2-6.3mM) rises through the glacier, surrounded by elemental sulphur, gypsum and carbonate deposits on theglacial surface, colonised by subsurface microbes that have therefore been transported from dark, reducingconditions to a light-abundant, oxidative environment. Bioenergetic calculations using the geochemicalanalysis of the site showed that oxidation of reduced sulphur species was highly energetically favourablein both the spring water (once it comes into contact with oxygen) and the elemental sulphur deposits.We used pyrosequencing of DNA extracted from the 2009 glacial sulfur deposits to analyze both the phy-logeny of the microbial population using the small subunit ribosomal RNA gene (SSU rRNA) and theirgenetic capabilities using metagenomic analysis of a shotgun library. We used this data to investigatehow the microbes obtained energy, carbon and nitrogen from their environment, in order to test whether“Following the Energy” would accurately predict the types of microbial energy metabolism we found.The deposit that we studied was strongly dominated by Epsilonproteobacteria overall (Sulfurovum andSulfuricurvum, both known as sulphur lithotrophs found in sulphidic environments), with a surface layerdominated by Flavobacterium (known as a heterotroph). Both the SSU rRNA data and the metagenomefunctional gene data were consistent with sulphur lithotrophy being the main source of primary pro-ductivity, and showed that photosynthetic organisms were almost completely absent from the sulphurdeposits. Photosynthesis was not being utilized as a major energy source by this community despite thefact that photosynthesis is energetically favourable due to the presence of abundant light in the arcticsummer, and has been shown to be significant in other arctic environments. Genes for both the aerobicoxidation of ammonium (nitrification) and the anaerobic oxidation of ammonium (anammox) are alsoabsent, even though both reactions could yield energy for growth. To better understand the potentialfor life on Mars and Europa, and to focus our search, we need to not just understand which types ofmetabolism are possible in an environment, but also which are the most likely to exist. The spring andsulphur deposits at Borup Fiord Pass Glacier are an excellent terrestrial analogue for the possible transferof any subsurface organisms in sulphur-rich sites on Mars or Europa to the surface or near-surface. Thisstudy has demonstrated that, in this type of site, although “Following the Energy” accurately predictedsulphur lithotrophy as a major energy source for primary productivity, some other microbial metabolismsthat were predicted to be energetically feasible were unexpectedly missing.

References:

1. T. M. Hoehler, J. P. Amend and E. L. Shock Astrobiology, 7(6), 819 (2007)

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P4.29 Understanding the Earth-Venus-Mars difference in Nitro-gen

Masatoshi Yamauchi1, Iannis Dandouras2, and the NITRO proposal team

1Swedish Institute of Space Physics (IRF), Kiruna, Sweden2Institut de Recherche en Astrophysique et Planetologie (IRAP), Toulouse, France∗E-mail of corresponding author: M.Yamauchi@irf.se

Nitrogen is a key element for life as an inevitable part of the amino acid and protein. While nitrogenis abundant on the Earth (the amount in the soil, crust, and ocean are small compared to the atmosphericamount) and on Venus (only 3% but pressure is 90 times of the Earth, resulting in three times as theEarth), Martian atmosphere has very little nitrogen, about only 0.01% of the Earth or Venus (with 10% ofplanetary mass). This contrasts the oxygen abundance, which is found in all three planets (Martian case,it is now believed to exist in the crust as oxidized rocks because the observed escape rate is equivalent only10 m deep water). Considering the fact that nitrogen is much more difficult to be ionized than oxygendue to triple chemical binding, absence of the nitrogen only on the Mars is a mystery, while this absensemight explain the absence of life at the present knowledge. From these viewpoints, it is important tounderstand the dynamic of nitrogen at different solar conditions, e.g., its difference from oxygen dynamicsfor whatever the planet. Such a study requires a dedicated space mission. We have recently proposed asatellite mission NITRO to study this problem, and we present the science and instrumentation of theNITRO mission.

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P4.30 Possible signs of life on Venus

Leonid Ksanfomality

Space research institute of the Russian Academy of Science, Russia∗E-mail of corresponding author: ksanf@rssi.ru

Basing on the premise of “normal” physical conditions in a habitable zone, i.e. pressure, temperaturerange, and atmospheric composition similar to those on the Earth, is a normal way searching for life inspace. But should not this approach be considered as “terrestrial chauvinism”? One should not excludecompletely the possibility of the existence of life at relatively high temperatures, despite the fact thatat the first glance it seems impossible. The planet Venus with its dense, hot (735 K), oxigenless CO2

– atmosphere and high 9.2 MPa pressure at the surface could be the natural laboratory for the studiesof this type. Amid the low mass exoplanets, celestial bodies with the physical conditions similar to theVenusian can be met. The only existing data of actual close-in observations of Venus’ surface are theresults of a series of missions of the soviet VENERA landers which took place the 1970’s and 80’s inthe atmosphere and on the surface of Venus. For 37 and 30 years since these missions, respectively, Irepeatedly returned to the obtained images of the Venus’ surface in order to reveal on them any unusualobjects observed in the real conditions of Venus. The new analysis of the Venus’ panoramas was based onthe search of unusual elements in two ways. Since the efficiency of the VENERA landers maintained for along time they produced a large number of primary television panoramas during the lander’s work. Thus,one can try to detect: (a) any differences in successive images (appearance or disappearance of parts ofthe image or change of their shape), and understand what these changes are related to (e.g., wind), orwhether they are related to hypothetical habitability of a planet. Another sign (b) of the wanted object istheir morphological peculiarities which distinguishes them from the ordinary surface details. The resultsof VENERA-9 (1975) and VENERA -13 (1982) are of the main interest. A few relatively large objectsranging from a decimeter to half meter and with unusual morphology were observed in some images,but were absent in the other or altered their shape. What sources of energy, in principle, could be usedby life in the high temperature oxigenless atmosphere? The objects found are large enough, they arenot micro-organisms. It is most natural to assume that, like on Earth, Venusian fauna is heterotrophic,and the source of its life is hypothetical autotrophic flora. There is enough light for this special flora’sphotosynthesis. Since the critical temperature of water on Venus is about 320◦C and the temperature atthe surface is about 460◦C, the metabolism of organisms on Venus (if any) should be built without water,on the basis of some other liquid medium. Based on data analyzed it has been suggested that because ofthe limited energy capacity of the Venusian fauna, the temporal characteristics of their physical actionscan be much longer than that of the Earth

187

P4.31 Self-assembly of Titan tholins in environments simulatingTitan liquidospheres andits implication to formation of primitivemembrane in Titan

Jun Kawai1, Seema Jagota2,Kensei Kobayashi1, Takeo Kaneko1,Yumiko Obayashi1,Yoshitaka Yoshimura4,Bishun N. Khare2, David W. Deamer3, Christopher P. McKay2

1Yokohama National University, Yokohama, Japan2NASA Ames Research Center, Moffett Field, USA3University of California, Santa Cruz, USA4Tamagawa University, Machida, Japan∗E-mail of corresponding author: j kawai0908@hotmail.com

Titan, the largest satellite of Saturn, has a thick atmosphere comprising nitrogen and methane.A variety of organic matters have been measured in the atmosphere, and it is supposed that they areirradiation products with ultraviolet light, electrons captured by the magnetosphere of Saturn, and cosmicrays. By Cassini/ Huygens investigation showed that the average temperature on the surface of Titanis 93.7 K, and that the existence of lake made of liquid ethane and methane. It was also suggested thatammonia water remains liquid under the ground. Laboratory experiments simulating Titan environmentsshowed that complex organic compounds were formed, which often referred to as Titan tholins. We havesynthesized Titan tholins by plasma discharges, and examined possible interaction between them andseveral kinds of liquids to simulate possible chemical evolution in Titans liquidosphere. Particularly, wefocus on a possible self-assembly of Titan tholins. In the present experiment, non-polar solvents such ashexane and chloroform were used on the behalf of liquid ethane and methane. Tholins was dissolved ineach solvent, and drops of the solutions were put on glass slides, and then ammonia aqueous solutionwas added to them. The self-assembly of tholins was confirmed by fluorescence microscopy. The presentexperiments suggested possible formation of primitive membranes on Titan environment.

188

P4.32 Accurate calculations of Ozone and liquid water over GaleCrater

A. Delgado-Bonal∗, F.J. Martın-Torres, E. Simoncini,

Centro de Astrobiologıa (INTA-CSIC)∗E-mail of corresponding author: alfonso.delgado.bonal@gmail.com

The determination of the existence of water on Mars is one of the primary targets in astrobiologydue to the importance of liquid water for life. However, the different thermodynamic conditions are notconsidered in many studies about the abundance of liquid water, leading to wrong calculations of availablewater and related quantities. We have improved a photochemical model for Mars atmosphere with theproper thermodynamical conditions and coupled it with realistic profiles of Temperature and Pressurepreviously calculated with PRAMS GCM. The study is applied to Gale and determine the abundance ofthis compound over the surface. To better model local conditions, we add surface-atmosphere reactions,among Gale minerals and atmospheric gases, in order to calculate the dissipation of free energy due tochemical processes and the actual chemical activity of water in Gale Crater. The existence and reactivityof liquid water on Mars is highly linked with the presence of other compounds in the atmosphere suchas Ozone or OH, and the determination of those also require the thermodynamical studies. Finally,the sorption of water over the surface by physical and chemical processes is reviewed with the newconcentrations,

189

P4.33 Signatures of Life on Earth and in Cosmos

Vivi Vajda1∗, Erik Persson2, Dag Ahren3, Anna Cabak Redei4, Dainis Dravins5, David Duner5, SofiaFeltzing5, Gustav Holmberg6, Arthur Holmer4, Petter Persson7

1Department of Geology, Lund University, Sweden2Department of Philosophy, Lund University, Sweden3Department of Biology, Lund University, Sweden4Centre for Languages and Literature, Lund University, Sweden5Lund Observatory, Lund University, Sweden6Lund University School of Economics and Management, Sweden7Department of Chemistry, Lund University, Sweden

∗E-mail of corresponding author: vivi.vajda@geol.lu.se

Our group completed a successful project Astrobiology, Past, Present and Future at the Pufendorfinstitute during 2010 and 2011. We now aim to develop our Theme and seek for further, larger mul-tidisciplinary applications towards e.g. European stakeholders and ESA. The Pufendorf institute is across-disciplinary research institute and part of Lund University.. The institute aims to be an open andcreative environment for academic study groups formed around current or emerging scientific and socialissues and problems to explore their management or resolution. The Pufendorf institute represents animportant link and encourages cross discipline interactions involving all faculties and also internationalexperts and research groups. We have now identified Signatures of Life on the Earth and in the Cosmosas a topic for an advanced study group at the Pufendorf Institute in order to develop our collaboration.The main aim of the study group is to have access to a platform for interaction and multidisciplinaryknowledge transfer, including workshops and guest lectures with a subsequent aim to prepare applicationsfor larger research projects within the theme outlined above. An important aspect of astrobiology is theunderstanding of how to distinguish signs of life from non-living processes. Signs of life can occur inthe form of chemical signatures, biogeology, or electromagnetic waves. To correctly interpret the signs itis necessary to have a deep understanding of the chemical, physical, geological, biological and semioticaspects involved. Of equal importance is a deep understanding of the linguistic and cognitive aspectsinvolved in producing and interpreting signs, and a conceptual understanding of life as a phenomenon. Inorder to put these aspects into perspective an understanding of the historical, philosophical, social andcultural aspects is crucial. In other words, to find, identify and interpret signatures of life, an interdis-ciplinary approach is essential. In order to target the challenges involved in identifying and interpretingsignals of life, the Astrobiology group at the Pufendorf Institue Lund University has initiated the researchproject Signatures of Life on Earth and in Cosmos involving a multidisciplinary group of scientist.

190

P5.01 Present time extreme environments as drivers of conver-gent evolution

Armando Azua-Bustos∗

Universidad de los Andes, Chile∗E-mail of corresponding author: ajazua@uc.cl

The Atacama Desert Coastal Range as a relevant model Convergent evolution describes the attainmentof similar biological/biochemical traits in phylogenetically unrelated lineages. This similarity can resultif organisms dwell in similar ecological niches. Thus, similar biological solutions may be reached whensimilar problems need to be solved. There are several examples in the literature where the results ofconvergent evolution are described, but few report on convergent evolution “in action”, where the endresults are yet to be observed. I propose the Coastal Range of the Atacama Desert as a model wherethese evolutionary processes may be observed in our geological time. At this interface between the PacificOcean and the driest desert of the world, key steps on the evolution of land plants are being retraced byextant microalgae and cyanobacteria.

191

P5.02 Meteorites as habitats for lichens and microorganisms inhot deserts

Natuschka M. Lee1∗, Olexandra Ganzenko1, Andreas Beck2, Edwin Gnosq3, Florian J. Zurfluhy4, BedaHofmann5

1Microbiology TUM, D-85354 Freising, Germany2Botanische Staatssammlung Munchen, Munich, Germany3Natural History Museum Geneva, Switzerland4Institute of Geological Sciences, University of Bern, Switzerland5Natural History Museum Bern, Switzerland∗E-mail of corresponding author: nlee@microbial-systems-ecology.de

The most common meteorites that are found in hot deserts are ordinary chondrites (OC) with aprimary mineralogy that is dominated by olivine, pyroxenes, feldspar/glass, metallic Fe-Ni and troilite(FeS). During the study of large numbers of OC in various degrees of weathering from Oman the questionarose whether these meteorites can serve as possible habitats for microbial life, and whether biologicalprocesses may influence the weathering. With their chemically reduced mineralogy and a significantporosity meteorites in the desert environment should be able to provide space and chemical energy forextremophilic life forms such as lichens and microorganisms. Possible limitations to microbial life arelimited water, extreme temperature variations between day and night (from 25 up to nearly 70◦C) anddepending on the meteorite type, high ionic strengths (several % Mg-Cl-SO4-brines). We observed macro-scopic growth of lichens to varying degrees on Oman meteorites only in areas up to 80 km from the coastwhere morning fog is very common and rocks in general are covered by lichen. A limited selection of thesemeteorites were analysed in order to explore the life forms associated to these. For this, an approachconsisting of microscopy, nucleic acid based approaches (targeting 16S rRNA genes and the intergenicspacer region, ISR), cultivation of thermophiles, and construction of a global database of organisms foundso far on meteorites and lichens in general was employed. So far, two different types of lichens have beenidentified based on the ITS region and macroscopic features and analysed for associated bacteria: i) thefoliose Ramalina maciformis, which is generally encountered in the Mediterranean area as well as in theMiddle East, and ii) Diploicia canescens s.l., which is often encountered in hot areas. Both have alsobeen detected on other meteorites [1]. A majority of the clones retrieved from prokaryotic 16S rRNAbased gene libraries showed generally low identities (between 85-98%) to other so far described prokary-otes (e.g. different taxa within the phyla Actinobacteria, Cyanobacteria, Firmicutes, GemmatimonadetesProteobacteria, Synergistetes). Interestingly, some of the closest relatives to these clones were also dis-tantly associated to other species associated either with meteorites [2] or different types of extremophilicenvironments. Although the function, activity level and origin of these species is for the time beingunknown, it is obvious that the prokaryotic life forms found on these meteorites may represent severalnovel microbial taxa some most likely different to species taxa described on other meteorites found onother locations on Earth. This suggests that it may be worthwhile to undertake larger screening stud-ies of various meteorites in order to gain a better understanding of how meteorites are colonized on Earth.

References:

1. http://www.lpi.usra.edu/meetings/metsoc2011/pdf/5277.pdf

2. K. Benzerara, V. Chapon, D. Moreira, D. P., Lopez-Garcia, F. Guyot and T. Heulin, T. Meteoriticsand Planetary Scienc, 41, 1249 (2006).

192

P5.03 Impact-induced hydrothermal systems as habitats for mi-crobial life

Magnus Ivarsson1, Curt Broman2, Erik Sturkell3, Jens Ormo4

1Swedish Museum of Natural History, Department of Palaeozoology, Sweden2Stockholm University, Department of Geological Sciences, Sweden3University of Gothenburg, Department of Earth Sciences, Sweden4Centro de Astrobiologia, Spain∗E-mail of corresponding author: magnus.ivarsson@nrm.se

Impact-generated hydrothermal systems are commonly proposed as good candidates for hosting micro-bial life on the early Earth and Mars. Large impacts result in impact melts that can support hydrothermalsystems with heat for thousands, sometimes up to million years. Impacts also create fractures in the targetrock which provide pathways for fluids and migrating microorganisms. However, evidence of fossil micro-bial colonization in impact-generated hydrothermal systems is rarely reported in the literature. Here, theoccurrence of putative fossilized microorganisms in a paleo-hydrothermal system of the Lockne impactstructure, Sweden, is reported. Putative fossilized microorganisms are observed in open vesicles associ-ated with hydrothermally formed quartz, calcite and kerogenous material. The putative fossils appear assemi-straight to twirled filaments, with a thickness of 5-20 µm, and a length varying between 50 µm and1 mm. The filaments branch frequently and anastomoses occur between branches. Their morphology iscomplex and they form mycelium-like networks anchored at the vesicle walls and sometimes boring inthe calcite. The size and morphology correspond to known fungal morphology rather than prokaryoticmorphologies. EDS analyses show that the filaments are totally kerogenous and the close associationwith kerogenous material and bitumen suggest that the microorganisms existed in a system of migratinghydrocarbons. The results from the Lockne impact structure show that hydrothermal systems associatedwith impact craters could potentially be capable of supporting microbial life. This could have playedan important role for the evolution of life on the early Earth but also for the sustainability of life onother planetary bodies like Mars. Based on these results impact structures are suggested as high prioritytargets for near future Mars sample return missions.

193

P5.04 Microbial colonization of halite and gypsum crusts fromthe Atacama Desert studied by combination of Raman spec-troscopy and microscopic imaging

Petr Vıtek1∗, Jacek Wierzchos2, Beatriz Camara-Gallego2, Jan Jehlicka1, Carmen Ascaso2, Ian Hutchinson3,Howell G. M. Edwards3,

1Institute of Geochemistry, Mineralogy and Mineral Resources, Charles University in Prague, Albertov6, 128 43 Prague 2, Czech Republic2Museo Nacional de Ciencias Naturales, CSIC, c/ Serrano 115 dpdo., 28006 Madrid, Spain3Department of Physics and Astronomy, Space Research Centre, University of Leicester, University Road,Leicester LE1 7RH, UK∗E-mail of corresponding author: petr.vitek@natur.cuni.cz

The hyperarid core of the Atacama Desert represents one of the driest places on Earth with anexceptional occurrence of microbial life coping with extreme environmental stress factors. Hence the areais considered as one of the most important Martian-analog sites. The halite rocks and gypsum crustshave already been found to harbor diverse microbial communities in this area. Here, we present a Ramanspectroscopic study, complemented by correlative microscopic imaging using fluorescence microscopy,SEM-BSE and confocal laser scanning microscopy of the endolithic microbial communities within thetwo different evaporitic systems which are of importance in the astrobiological context - namely, haliteand gypsum. The microbial communities are dominated by phototrophic microorganisms.

Spectral signatures obtained on cyanobacterial aggregates within halite crusts revealed the presenceof the UV-protective biomolecule scytonemin as well as light harvesting pigments indicative of the pho-tosynthetic activity. The difference in scytonemin content relative to other pigments within the differentzones were studied using a correlative approach benefitting from the information obtained using differentapproaches. This allows us to infer the adaptation strategies of these microorganisms to high UV andPAR irradiation as well as to derive information about the stability of individual pigments as biomarkers.

In the gypsum crust, variation of photosynthetic pigment composition within different zones can berelated to the cyanobacterial and algal colonization and also reveal the degradation of phycobiliproteinswithin the decayed biomass of cyanobacteria. Carotenoids of at least three different types were recognized,differing in their dependence on the particular phylum of the phototrophic microorganisms.

The different zones of halite, selected on the basis of their different scytonemin content, were also stud-ied using miniaturized Raman instrumentation. Two different types of instruments equipped with 532nm and 785 nm lasers for excitation, respectively, were assessed for the detection of microbial biomarkerswithin the natural halite matrices from the hyperarid region of the Atacama Desert. Measurements wereperformed directly on the rock as well as on the homogenized, powdered samples prepared from thismaterial - the effect of this sample preparation and excitation wavelength employed in analysis will becompared and discussed. The results have significant importance for the deployment of Raman instru-mentation in the forthcoming ExoMars mission scheduled for 2018 and for other future astrobiologicallyfocused missions to Mars.

194

Figure 13: The Raman spectral differences in scytonemin content relative to carotenoid between darkbrown cyanobacterial aggregates (upper spectrum) and green cyanobacterial aggregates (lower spectrum)from the interior of halite crusts in the Yungay region of the Atacama Desert. The spectra were obtainedusing a 532 nm laser for excitation. c=carotenoid, s=scytonemin

Figure 14: The Raman spectra of algae (upper spectrum) and cyanobacteria (lower spectrum) revealdifferences in pigment composition of these endolithic organisms inhabiting gypsum crusts in the AtacamaDesert. The spectra were obtained using a 785 nm laser for excitation. c=carotenoids, chl=chlorophyll,p=phycobiliproteins

195

P5.05 Cyanobacteria isolated from the high intertidal zone: amodel for studying the physiological prerequisites for survival inextraterrestrial environments

Karen Olsson-Francis1, Jon Watson2, Charles S. Cockell3

1CEPSAR, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK2Department of Earth Science and Engineering, Imperial College London, London SW7 2AZ, UK3UK Centre for Astrobiology, School of Physics and Astronomy, University of Edinburgh, Edinburgh, UK∗E-mail of corresponding author: k.olsson-francis@open.ac.uk

On Earth, cyanobacteria are ubiquitous and can be found in some of the most extreme environments.For example, cyanobacteria that live in the rocky high intertidal zone have to survive daily fluctuations inenvironmental parameters such as temperature, ultraviolet (UV) light, desiccation and salinity. Althoughthe physiological challenges that the high-intertidal zone creates result in a loss of microbial diversity,cyanobacteria can survive in this extreme environment. The physiological adaptations required to live inthis environment are also prerequisites for survival in extraterrestrial environments, for example, toler-ance to extreme temperatures, ability to tolerate extreme desiccation and intermittent water availability,as well UV resistance. We have previously isolated, Phormidium strain OU10, Gloeocapsa strain OU20and Leptolyngbya strain OU13, from the intertidal zone of cliff in Beer, Devon, United Kingdom, usingdesiccation, vacuum (0.7 × 10−3 kPa), low temperature (−80◦C) and Mars conditions (−27◦C, 0.8 kPaCO2) as selection factors in the laboratory [1]. Gloeocapsa strain OU20 was also able to survive 548 dexposure to low Earth orbit [2]. To understand how these cyanobacteria survived the adverse conditions,we investigated the physiological requirements for life in the high-intertidal zone. The cyanobacteria weregrown in a medium with 35.7% salinity, to represent the high-intertidal zone, and in a control mediumwith 6.7hsalinity. The stressed cells were more resistant to desiccation, low temperature and UV ra-diation than the controlled cells. For example, the dosage of UV radiation that reduces viability by afactor of 10 (the D value) was higher (111 J/m2 compared to 75.7 J/m2 (Phormidium strain OU10);135 J/m2 compared to 83 J/m2 (Gloeocapsa strain OU20), and 162 J/m2 compared to 105 J/m2 (Lep-tolyngbya strain OU13)). We suggest that this is due to the physiological differences we observed in thestressed cells. This included a thicker extracellular polysaccharide sheath (EPS); for example, the EPS ofGloeocapsa strain OU20 was 2.1-fold thicker. The fatty acid content of the cells was higher, for example,the content of Gloeocapsa strain OU20 was 2.22 mg/g compared to 4.16 mg/g. The stressed cells alsoproduced higher levels of UV absorbing pigments, scytonemin and mycosporine-like amino acids (MAAs).This study indicates that cyanobacteria have adapted physiologically to live in the high-intertidal zoneand this could be the key to understanding the physiological requirements for survival in extraterrestrialconditions.

References:

1. K. Olsson-Francis, R. de la Torre, C. Cockell, AEM, 76, 2115 (2010)

2. C. Cockell, P. Rettberg, E. Rabbow, K. Olsson-Francis, ISME, 46, 1671 (2011)

196

P5.06 Soil Microorganisms and Mineral Weathering: Mechanicsof Biotite Dissolution

Engy Ahmed∗, Sara J. M. Holmstrom, Volker Bruchert, Nils G. Holm

Department of Geological Sciences, Stockholm University, Stockholm, Sweden∗E-mail of corresponding author: engy.ahmed@geo.su.se

Soil microorganisms play an important role in the environment by contributing to leach and releaseof essential elements from soil minerals that are required not only for their own nutrition but also forplants growth. This study aims to compare between the mechanisms of different fungal and bacterialspecies isolated from podzol soil in biotite dissolution. Microplate devices with 6 wells were used for thebiological weathering experiments. All of the sterilized microplate wells were filled with 4g/l of biotitefollowed by 12 ml of an iron free diluted mineral liquid medium. In these conditions, biotite particlesare the only source of the essential elements for the microorganisms. To characterize the mechanisms ofbiotite dissolution, we monitored siderophores production, microbial biomass, pH, exchangeable cationsconcentration and SEM analysis for mineral surface. There was a significant difference between thebehavior of the fungal and bacterial species in dissolution of biotite. This difference may be due tothe variation of these microorganisms in their mechanics of interaction with mineral surface. It wasobserved also that these microorganisms directly and indirectly induce biotite dissolution. Defining soilas a system driven by biological mechanisms rather than chemical processes has major implications forour understanding of how the system functions and how it will respond to changing conditions.

197

P5.07 The influence of extracellular polymeric substances on thedesiccation tolerance of Deinococcus geothermalis biofilms

Jan Frosler∗, Hans-Curt Flemming, Jost Wingender,

University of Duisburg-Essen, Faculty of Chemistry, Biofilm Centre, Essen, Germany∗E-mail of corresponding author: jan.froesler@uni-due.de

Biofilms are accumulations of microorganisms at interfaces. In a biofilm the bacterial cells are embed-ded in a matrix of self-developed extracellular polymeric substances (EPS), comprising various types ofbiopolymers such as polysaccharides, proteins, and DNA [1]. Biofilm cells, in contrast to their planktoniccounterparts, exhibit an increased tolerance towards environmental stressors, including antimicrobials,extreme pH conditions, and desiccation, with the latter one being an important factor when consideringmicrobial life in open space or Martian environments. The availability of water is essential to maintainboth physiological activity and cell membrane integrity in bacterial cells. In the event of drying, biofilmsfeaturing hygroscopic EPS can retain water for a prolonged period of time, thus increasing the chancefor biofilm organisms to survive [2].

In this study, the desiccation tolerance of the Deinococcus geothermalis was evaluated. Planktonicbacteria were cultivated at 45◦C for 2 days in liquid growth media, while water-unsaturated biofilms ofD. geothermalis were grown at the same temperature on membrane filters placed on solid agar media.The EPS of D. geothermalis biofilms were isolated using different extraction techniques and analysed fortheir biochemical composition. The presence of polysaccharides, proteins and DNA within the EPS wasconfirmed; uronic acid-containing carbohydrates were not detected. Evidence for the presence of EPS inliquid cultures was obtained [3].

For both planktonic cells and biofilms, samples were air-dried and stored for a defined period of time(days to months) under desiccating conditions before analysing them for survival in terms of culturabil-ity on agar media and membrane integrity by using the Live/Dead viability kit. Biofilm cells showeda significantly higher survival than planktonic cells (2.4-fold higher portion of culturable cells, 1.3-foldhigher portion of membrane-intact cells after 5 days of desiccation) and could still be cultivated after 3months of desiccation (1.3% of total cell count). These results are in accord with previous reports thatother bacteria, when embedded in a biofilm, exhibit an elevated tolerance towards desiccation, probablyat least in part based on the protective role of EPS [4, 5].

References:

1. H.-C. Flemming and J. Wingender, Nature Reviews Microbiology, 8, 623-633 (2010).

2. E.B. Roberson and M.K. Firestone, Applied and Environmental Microbiology, 58, 1284-1291 (1992).

3. C. Saarimaa, M. Peltola, M. Raulio, T.R. Neu, M.S. Salkinoja-Salonen, and P. Neubauer, Journalof Bacteriology, 188, 7016-7021, (2006).

4. T. Ophir and D.L. Gutnick, Applied and Environmental Microbiology, 60, 740-745 (1994).

5. Y. Tamaru, Y. Takani, T. Yoshida, and T. Sakamoto, Applied and Environmental Microbiology,71, 7327-7333 (2005).

198

P5.08 Surviving rules: wide overlap in gene expression responseto desiccation and ionizing radiation in an anhydrobiotic midge

Oleg Gusev1,3∗, K. Mukae1, M. Sugimoto4, T. Kikawada1, T. Sakashita2, T. Okuda1

1Anhydrobiosis Research Group, National Institute of Agrobiological Sciences, Japan2Life Science and Biotechnology Division, QuBS, JAEA, Japan3Department of Invertebrate Zoology, Kazan Federal University, Russia4Institute of Plant Science and Resources, Okayama University, Japan∗E-mail of corresponding author: oleg@cryptobio.com

Resistance to both ionizing radiation and desiccation is a peculiar feature of larvae of the sleepingchironomid Polypedilum vanderplanki. We have recently showed that a link between anhydrobiosis andradio-resistance can be traced from similar patterns of DNA damaging effect of both desiccation andirradiation. In this study, using microarrays build on the basis of P. vanderplanki EST database, wehave conducted genome-wide analysis of gene expression response to two types of ionizing radiationand desiccation. Based on the observation that 4He (LET=16.2 keV/µm) ion beam (70 Gy) inflicts asimilar effect on nuclear DNA damage occurred in normal anhydrobiotic chironomid larvae, we comparedeffect of a gamma-ray at a dose of 70 Gy, 70 Gy of 4He ions and desiccation on genome-wide mRNAexpression in the larvae. We found that gamma-radiation, 4He and desiccation significantly altered geneexpression in the larvae and resulted in up-regulation in 553, 394 and 2077 clones correspondingly . Thedesiccation was the strongest factor affected the gene expression. Surprisingly, there was a major overlapin gene expression in the larvae stressed with radiation and desiccation. In total 43% of transcriptsupregulated by gamma irradiation and 52% of transcripts upregulated by 4He were also responsive todesiccation. Finally, 108 transcripts were upregulated in all three groups of larvae. We have furtherconducted transcripts scaffolding and annotation and found that the overlapped in all three groups highlyupregulated transcripts represent 51 unique genes. The major GO group included: long non-coding DNA(16 genes), unknown proteins (12 genes), LEA proteins (8 genes), antioxidants (6 genes), members ofprotein and DNA folding and reparation networks (6 genes). Taking together, our data suggest thatapart from clear similarities in nucleic acid damaging effect of desiccation and ionizing radiation, theenchanced radioresistance of the sleeping chironomid is a result of similarities in pathways controllingmRNA expression in response to these two stresses. Moreover, we found pos-irradiation response inthe larvae involve genes indispensable for successful anhydrobiosis, thus, evolvement and evolution ofdesiccation resistance in P. vanderplanki might be a natural factor of gradual increase of radioresistancein this species of insects.

199

P5.09 Growth and photochemical activity of snow algae in crossedgradients of temperature and irradiance

Jana Kviderova1,2, Linda Nedbalova1,2,3, Lenka Prochazkova3, Marie Drızhalova3

1Centre for Polar Ecology, Faculty of Science, University of South Bohemia, Ceske Budejovice, CzechRepublic2Institute of Botany, Academy of Science of the Czech Republic, Trebon, Czech Republic3Department of Ecology, Faculty of Science, Charles University, Prague, Czech Republic∗E-mail of corresponding author: kviderova@butbn.cas.cz

Snow algae represent unique model organism for study of adaptation/acclimatization mechanisms tolow temperature and high and variable irradiance (photosynthetically active and ultraviolet radiation).In this study, growth and photochemical activity of selected strains of snow algae was evaluated incrossed gradients of temperature and irradiance. The temperature ranged from 0.6 to 24.7◦C and thephotosynthetically active radiation ranged from 67 to 556µmol m−2 s−1. The growth was evaluated asa change in colony size measured as a photosynthetically active area and the photochemical efficiency asmaximum quantum yield after 15 min dark adaptation. According to the response to the experimentalstrains Chloromonas spp. should be considered rather psychrotolerant than psychrophilic. Similar patternwas also observed in response of the photochemical activity. While the growth was less sensitive toirradiance, slight decrease in the photochemical activity was observed in higher irradiances.

200

P5.10 Permafrost microorganisms under Mars-simulated pres-sure

Kirill Krivushin1,2, David Gilichinsky1, Andrew C. Schuerger2, Wayne L. Nicholson2

1Institute of Physicochemical and Biological Problems in Soil Science, Soil Cryology Laboratory, Russia,Pushchino, 1422902University of Florida, Space Life Sciences Laboratory, Kennedy Space Center, FL USA 32899∗E-mail of corresponding author: krivushin@bk.ru

It is known that the Mars subsurface contains substantial water ice, even at relatively low latitudes.Martian permafrost might hypothetically record genetic signatures of preexisting or putative present-daylife. Arctic permafrost is considered to be a close earth analogue to the Mars subsurface. In general, bothpermafrost environments characterized by subzero temperatures, low water activity and accumulatednatural background radiation. Current data shows band crossing of the environmental factors. To esti-mate effect of simulated Martian pressure and temperature on an Earth permafrost microbial communitywe collected eight samples from ancient Siberian permafrost horizon (Kolyma lowland; hole 2-09;159◦N69◦E, 8000 BP). We tested the capability of permafrost bacterial community to proliferate under simu-lated martian conditions (4◦C, 20 mbar) and estimated influence of low temperature (4◦C, 1 bar). Colonyforming units were counted on TSA plates incubated: 1) at 20◦C and 1 bar (RT); 2) at 4◦C in the fridgeat 1 bar (F); 3) at 4◦C in a vacuum desiccator at 20 mbar (D), respectively. A few single colonies (frommost abundant samples 5 and 8) were picked from plates 5-D and 8-D, then were grew on TSB mediaat 4◦C (1 bar) and finally plated on TSA for incubation in desiccators. To verify growth (at 4◦C and 20mbar) of the isolates a second set of TSA plates were established. Six pure cultures were isolated. Onthe basis of 16S rRNA phylogeny the isolates belongs to the genus Exigoubacterium. The results makea contribution to Astrobiology and advocate for future investigation of permafrost community under fullspectra of Martian conditions. Acknowledgments: The authors appreciate to Vasily Mironov and GlebKraev for excellent technical assistance. This work was supported in part by the NASA Planetary BiologyInternship program.

201

P5.11 Cryo-life habitability on a polythermal glacier in Green-land

Stefanie Lutz1∗, Alexandre M. Anesio2, Liane G. Benning1

11 School of Earth & Environment, University of Leeds, UK2School of Geographical Sciences, University of Bristol, UK∗E-mail of corresponding author: s.lutz@leeds.ac.uk

Modern surface glacial ice and snow are extreme environments at the edge of Earth’s biosphere andpotential sites of biosignatures in future planetary missions. The primary colonization of snow and ice isan important biogeological scenario with clear implications for the life detection on other icy planets [1].Hence, knowledge of the adaptations and survival strategies adopted by extremophiles – cryophiles – interrestrial cryogenic environments is vital for our ability to process data from future planetary missions.Despite it being one of the most extreme habitats on Earth, glacial ice and snow-fields are colonised bya plethora of organisms including snow algae, bacteria, fungi, protozoa, rotifers and even invertebrates[2]. Although low in number and diversity compared to other habitats, snow and ice algae are a majorprimary producer in glacial settings [3,4]. Their life cycle influences the structure and diversity of neigh-bouring microbial communities [5] and they produce a suite of complex molecules to protect themselvesagainst cold [6], UV [7], or nutrient deficiency [8]. However, these adaptations are poorly understoodand we know very little about the complexity of the biological inventory contained within snow and iceenvironments. We will present results from an initial study carried out on the polythermal Mittivakkatglacier in SE Greenland. Our aim was to gain a better understanding of the parameters controllingcryo-life habitability signals and start developing a comprehensive cryogenic life signal database. Dueto its Atlantic position, the coastal Mittivakkat Glacier has low average summer temperatures and longice/snow persistence, and its remoteness warrants low levels of contamination from anthropogenic inputs.We characterized the complementary microbiological and geochemical characteristics at a suite of sam-pling sites in the ablation, superimposed and accumulation zone of the glacier. The biological signaturesin various snow and glacial habitats (e.g., snow fields, cryoconites glacial outflow, clean snow) quantifiedvia variations in microbial diversity and distribution using standard microbiological methods combinedwith metagenomic approaches helped investigated the preservation and adaptations of snow algae specificbiosignatures. Furthermore, these were cross correlated with analyses of the main biogeochemical (nu-trients, pigments, lipids, trace metals) and mineralogical characteristics of the solid materials associatedwith each cryogenic habitat.

References:

1. Jakosky et al (2003) Astrobiology, 3: 343-350

2. Anesio, and Laybourn-Parry (2012) Trends Ecol Evol in press

3. Leya et al (2009) FEMS Microbiol Ecol, 67: 432-443

4. Remias et al (2005) Eur J Phycol, 40: 259-268

5. Amato et al (2007) FEMS Microbiol Ecol, 59: 255-264

6. Inglis et al (2006) Cur Protein&Pept Sci, 7: 509-522

7. Holzinger et al (2006) Phycol, 45: 168-177

8. Telling, Anesio et al (2011) J Geophy Res -Biogeosci 116: G03039

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P5.12 Snow cover of Central East Antarctica (Vostok station)as an ideal natural spot for collecting Cosmic Dust: preliminaryresults on recovery of chondritic micrometeorites

Elena S. Bulat1,5, V. A. Tselmovich2, Jean-Robert Petit3, L. M. Gindilis4, Sergey A. Bulat1∗

1FSBI Petersburg Nuclear Physics Institute, NRC Kurchatov Institute, Leningrad region, Gatchina, Rus-sia2Geophysical Observatory ”Borok”, Schmidt Institute of Physics of the Earth, RAS, Borok, Yaroslavlregion, Russia3Laboratoire de Glaciologie et Geophysique de lEnvironnement, CNRS/UJF Saint-Martin-d’Heres, France4Sternberg Astronomical Institute Moscow University, Moscow, Russia5Paleontological Institute, RAS, Moscow, Russia∗E-mail of corresponding author: bulat@omrb.pnpi.spb.ru, bulat@lgge.obs.ujf-grenoble.fr

During the 2010/2011 season nearby the Vostok station the 56th Russian Antarctic Expedition hascollected surface snow in a big amount from a 3 m deep pit using 15 220 L vol. containers (about 70 kg snoweach). Snow melting and processing by ultra-centrifugation was performed in a clean (class 10000 and100) laboratory. Total dust concentrations were not exceeded 37.4 mkg per liter with particle dispersalmode around 2.5 mkm. To analyze the elemental composition of fine dust particles aimed to revealAntarctic micrometeorites (AMM) two electron microscopy devices equipped with different micro-beamswere implemented. As a preliminary result, 3 particles (of 107 analyzed) featured by Mg content clearlydominated over Al along with Si and Fe as major elements (a feature of carbonaceous chondrites) wereobserved. By this the Vostok AMM CS11 collection was established. The occurrence of given particleswas averaged 2.8% - the factual value obtained for the first time for chondritic type AMM at Vostok whichshould be considered as the lowest estimate for all other families of AMM. Given the reference profile oftotal dust content in East Antarctic snow during Holocene (18 mkg/kg) the MM deposition in Antarcticawas quantified for the first time – 14 tons per day for carbonaceous chondrites for the Vostok AMM CS11collection and up to 245 tons per day for all MM types for the Concordia AMM DC02 collection.

The results obtained allowed to prove that snow cover (ice sheet in total) of Central East Antarcticais the best spot (most clean of other natural locations and always below 0◦ C) for collecting nativeMM deposited on the Earth during the last million years and could be useful in deciphering the originand evolution of solid matter in our Solar System and its effects on Earth-bound biogeochemical andgeophysical processes including the life origin. The farther analyses of the Vostok AMMs are in a progress.

203

P5.13 The application of a decontamination technique withinthe study of low bacterial density environments

Tina Santl Temkiv1,2∗, Kai Finster3, Ulrich Gosewinkel Karlson1

1Department of Environmental Science, Aarhus University, Roskilde, Denmark2Stellar Astrophysics Centre, Aarhus University, Aarhus, Denmark3Department of Bioscience, Aarhus University, Aarhus, Denmark∗E-mail of corresponding author: tina.santl@gmail.com

Current or past microbial life in extreme and extraterrestrial environments may only leave very minutetraces of DNA. Its detection by DNA-targeting techniques thus requires extremely sensitive procedures,which are compromised by the ubiquitous presence of contaminant DNA. Studying bacterial diversity oflarge hailstones, which are extreme environments characterized by the presence of very few bacterial cells,we show that a simple DNA-extraction method together with an efficient decontamination procedure canreduce background contamination. Due to the combination of low bacterial density and low volume ofour samples [1], a very sensitive approach, i.e. semi-nested PCR, was required for DNA amplificationprior to the construction of clone libraries. To extract DNA from the hailstone samples, we used a verysimple, one-step DNA extraction procedure, which reduced the loss of indigenous DNA as well as theamount of contaminant DNA introduced. In addition, a modified multistrategy DNA decontaminationprocedure, which was developed for work with ancient DNA [2], was carried out on laboratory surfaces,gloves, labware and reagents used in the first PCR reaction, in order to eliminate the contaminating DNA.We confirmed that the decontamination technique was effective by analyzing the bacterial diversity of 9hailstones, and contrasting it to the diversity found in 9 negative controls, which indicated the amountand the type of the background contamination. The obtained clone sequences from the negative controls(N=295) and the hailstone samples (N=485) confirmed that the samples were much more diverse and thatthe diversity of the background contamination was final and could be well described [Fig. 1]. In addition,the background contamination sequences were classified to only 9 known genera, whereas the hailstonesequences were affiliated to as many as 55 genera. In conclusion, we show that such a decontaminationprocedure can be efficiently employed within astrobiology and biology of extreme environments in orderto prevent false positive results. The analysis of several negative controls along with the samples canensure the reliability of results, even in cases where contamination cannot be entirely eliminated.

204

P5.14 Hailstones: a window into microbial life in storm clouds

Tina Santl Temkiv1∗, Kai Finster2, Thorsten Dittmar3, Bjarne Munk Hansen1, Runar Thyrhaug4, NielsWoetmann Nielsen5, Ulrich Gosewinkel Karlson1

1Department of Environmental Science, Aarhus University, Roskilde, Denmark2Department of Bioscience, Aarhus University, Aarhus, Denmark3Max Planck Research Group for Marine Geochemistry, University of Oldenburg, Oldenburg, Germany4Department of Biology, University of Bergen, Bergen, Norway, opus posthum5Danish Meteorological Institute, Copenhagen, Denmark∗E-mail of corresponding author: tina.santl@gmail.com

Diverse bacterial communities found in cloud droplets could, in spite of their low densities, contributeto the physical and chemical processes in the atmosphere [1]. Their unpredictable locations and shortlifetimes make storm clouds hardly accessible to microbial investigations. We thus proposed the use oflarge hailstones, which stochastically collect a large number (>109) of storm-cloud droplets, as naturalsampling devices giving insights into storm clouds as extreme bacterial environments [2]. By performingthe first comparative study on 50 individual large hailstones, we show how the pool of dissolved organicmatter may support bacterial metabolism in a storm cloud.

High concentrations of total dissolved nitrogen (30 µM, Q1Q3 = 2735 µM) and dissolved organiccarbon (Me=179 µM, Q1Q3 = 132220 µM) indicated that the storm cloud was a nutrient-rich microbialenvironment. However, the ability of bacteria to metabolize dissolved organic matter (DOM) is notonly dependent on its quantity but also on the suitability of the compounds for microbial metabolism.We therefore analyzed the high molecular mass range of dissolved organic matter, identifying molecularformulae of almost 3000 compounds and grouping them according to their biodegradability. Less than3% of the identified compounds were plant waxes, fatty acids or carbohydrates, which are structurallysuitable for microbial degradation on the short time scales of storm clouds. From low bacterial densities(Me=1973 cells/ml, Q1-Q3=1485-2960) found in hailstones we could conclude that cloud water was avery sparsely populated environment, with bacterial cells found only in very few cloud droplets. Thussignificant bacterial growth is feasible even if only 3% of DOM is accessible as bacterial substrate.

As the residence time of bacteria in cloud droplets is short, only bacteria with opportunistic ecologicalstrategy, i.e. having fast growth responses and fast growth rates are likely to grow in clouds. In order toidentify the most likely actors that could metabolize DOM in cloud droplets, we performed a cultivation-independent study, yielding DNA clone libraries with 485 gene sequences, and a cultivation-dependantstudy, yielding 424 bacterial isolates. Clone libraries revealed a diverse bacterial community [Fig. 1],within which plant-associated bacteria seemed to be enriched compared to soil bacteria.

This suggested that bacteria coming from plant surfaces must possess some means of withstandingstressful conditions encountered by all aerosolized cells. The relevance of plant-associated bacteria wasfurther supported by the cultivation-dependant study, as the dominant isolates were affiliated to the plant-associated genus Methylobacterium [Fig. 1]. Members of Methylobacterium were shown to grow on diverseorganic compounds [2] and were previously demonstrated to have fast growth responses and high growthrates, which all indicate their opportunistic ecologic strategy. Both, having means of survival in theatmosphere and being opportunistic, suggests that Methylobacterium and possibly other plant-associatedgenera are good candidates for active growth in clouds. Based on the spectrum of biodegradable organicsas well as bacterial numbers and types, we conclude that storm clouds likely contain growing bacteria.

References:

1. A.-M. Delort, M. Vaıtilingom, P. Amato, M. Sancelme, M. Parazols, G. Mailhot, P. Laj and L.Deguillaume, Atmos. Res., 98, 249260 (2010)

2. T. Santl Temkiv, K. Finster, B. M. Hansen, N. W. Nielsen and U. G. Karlson, FEMS MicrobiologyEcology, DOI:10.1111/j.1574-6941.2012.01402.x (2012)

205

P5.15 A Permian hypersaline microbial community (AssistenciaFormation, Irati Subgroup - Permian, Brazil) as a potential ana-logue for early Martian life

Cleber Pereira Calca1∗, Thomas R. Fairchild1, Barbara Cavalazzi2, Jorge Hachiro1

1Instituto de Geociencias da Universidade de Sao Paulo, Sao Paulo, Brazil2Department of Geology, University of Johannesburg, Johannesburg, South Africa∗E-mail of corresponding author: atabike@yahoo.com.br

The study of signatures of life (e.g. bioconstructions, microfossils) in modern and fossilized extremeenvironments on Earth provides an important basis for comparison with possible counterparts that maybe found elsewhere in the universe. Life on Mars, for example, is believed to have developed withinan aqueous, albeit extreme environment (e.g. alkaline, hypersaline). Therefore, studies on microbialbiosignatures and microbial fossilization processes have demonstrated the potential of evaporitic depositsfor microbial paleontology, as microbial fossils and biomolecules are very well preserved in modern andancient evaporitic deposits on Earth. Here, we present a detailed study of a very well-preserved and uniquePermian microbial ecosystem from the Assistencia Formation, Irati Subgroup, Parana Basin, Brazil. Thisformation is widespread, well-exposed, and characterized by rhythmic dolostones and shales with commonblack chert. The Brecciated Evaporite Bed (BEB), at the base of this formation, varies from 1 to 2.5 mthick typified and commonly includes folded silicified layered dolomites. Layers of evaporitic minerals (nowpseudomorphs of gypsum and anhydrite) in dolomitic micrite have been observed in samples from cores.The massive portion of cherty dolomites is rich in benthic cyanobacteria within diffuse microbial matsmillimetres thick. Indeed, microfossils may comprise a significant volume of the sediment. Notably, onlyunicellular cyanobacteria are found, but scarce, dispersed planktonic cells are also present. Sedimentologicand taphonomic factors explain the concentration of microbiota in the BEB. Salt may have precipitated atthe water-sediment interface, forming an evaporite layer. Once buried, the continued growth of this layerwithin unconsolidated sediments would have distorted the layer into enterolithic folds due to the strengthof crystallization of the evaporite minerals. Locally, very early substitution and/or permineralization bysilica completed the process of lithification before complete decomposition of the microbial mats. Thisprocess may explain why the BEB microbiota of Assistencia Formation is so well preserved. First, themicroorganisms adapted to hypersaline environments are naturally more resistant to desiccation, whichalso increases their preservation potential. Second, under these conditions, colonies of microorganismsand communities could have been encompassed by rapid precipitation of evaporite minerals (and earlysilicification). Finally, it is known that unicellular cyanobacteria predominate in many water bodies withhigh concentrations of salt as inferred for the BEB and as may have been present on Mars. Thus, weconclude that the BEB may be considered a good analogue for terrestrial and extraterrestrial evaporiticenvironmental conditions present on early Earth, as well as the alkaline, evaporitic conditions present onearly Mars.

206

P6.01 The PROCESS and AMINO Experiments: Effects of VUVPhotochemistry on Amino Acids on the International Space Sta-tion and in Laboratory Simulations

Marylene Bertrand1∗, Annie Chabin1, Andre Brack1, Herve Cottin2, Frances Westall1,

1Centre de Biophysique Moleculaire, CNRS, rue Charles Sadron, 45071 Orleans Cedex 2, France2LISA, University Paris Est-Creteil & Paris Diderot, UMR 7583 CNRS, Creteil, France∗E-mail of corresponding author: marylene.bertrand@cnrs-orleans.fr

In the context of the importance of exogenous organic matter in the emergence of the life on Earthmore than four billion years ago, our group studies the formation and fate molecules synthesized in space.We are especially interested in amino acids and dipeptides because of their occurrence in carbonaceousmeteorites and micrometeorites and because of the diversity of their functional groups, an importantfactor for the formation of macromolecules. We have carried out studies on organic molecules that wereexposed to space conditions on board the International Space Station, as well as in experiments in labora-tory simulation chambers. The exposed molecules were the proteic and non proteic amino acids: glycine,alanine, amino isobutyric acid, amino butyric acid, aspartic acid, serine and the peptide dileucine. Themolecules were exposed both in the free state and embedded in meteoritic powder. After exposure, themolecules were extracted, derivatized and analyzed by gas chromatography coupled to a mass spectrom-eter (GC-MS). Specific procedures of derivatization using alkyl chloroformates or silylation reagents forchiral and non-chiral analysis of amino acids by GC-MS were developed for these projects, includingan original method to separate and quantify amino acid enantiomers by the formation of diastereoiso-mer derivatives (Bertrand et al. 2008). Two experiments (Process on EXPOSE-Eutef and Amino onEXPOSE-R) were run on the International Space Station in order to determine the effects on the VUV(vacuum ultra violet) light on organic molecules (Cottin et al. 2008; Rabbow et al. 2012). The resultsobtained for the Process Experiment and for experiments carried out in irradiation chambers in Kolnat the “Deutsches Zentrum fur Luft- und Raumfahrt”, and in Orleans at the “Centre de biophysiquemoleculaire” have been recently published in an special issue of Astrobiology (Bertrand et al. 2012).Analysis of the Amino Experiment is in progress. Both space (the Process experiments) and groundexperiments show that the resistance to irradiation is function of the chemical nature of the exposedmolecules and depends on the VUV range and on the mineral matter in which they were embedded. Theamino acids presenting functional groups in their side chain were more degraded than those with alkylchain. The photochemistry experiments allow us to better understand the availability of the exogenousmatter in the context of the origins of life on Earth and how the molecules synthesized in space could beorganized in water in order to produce macromolecules.

207

P6.02 OREOcube: ORganics Exposure in Orbit

Andreas Elsaesser1∗, Richard Quinn2, Pascale Ehrenfreund1, Alexander Kros1, Andrew Mattioda3, An-tonio Ricco3, Farid Salama3, Orlando Santos3, Herve Cottin4, Emmanuel Dartois5, Louis d’Hendecourt5,Rene Demets6, Bernard Foing6, Zita Martins5, Mark Sephton7, Marco Spaans8

1University of Leiden, Leiden, NL2SETI Institute, Mountain View, CA3NASA Ames, Moffett Field, CA4LISA, Universit Paris Est-Crteil, Paris, FR5IAS, Orsay, FR6ESA/ESTEC, Noordwijk, NL7Imperial College, London, UK8University of Groningen, Groningen, NL∗E-mail of corresponding author: a.elsaesser@umail.leidenuniv.nl

Photochemical evolution and distribution of organic compounds are of high interest to the astrobio-logical research community [1]. Studying the photostability of organic materials directly in space avoidsthe limitations and technical challenges of laboratory experiments which try to simulate near-space con-ditions. Whilst current exposure facilities on the International Space Station (ISS), such as EXPOSE-Eand EXPOSE-R [2], provide platforms to expose organic materials in Earth orbit, their ability to mea-sure photochemical processes is limited due to only pre-launch and after sample return analysis ratherthan in-situ monitoring. The O/OREOS (Organism/Organic Exposure to Orbital Stresses) satellite [3,4] on the other hand overcomes this limitation by performing in-situ UV-Vis-NIR spectroscopy in lowearth orbit. The OREOcube project will combine both approaches allowing in-situ as well as post-flightanalysis.

Based on two SEVO (Space Environment Viability of Organics) cubes from the O/OREOS spec-troscopy platform (see Fig. 15), OREOcube will investigate the effects of solar and cosmic radiation onorganic molecules in Earth orbit when deployed on the outside of the ISS. By depositing organic sam-ples as thin films onto inorganic substrates, structural changes and organic-inorganic interactions canbe examined in order to understand the role that solid mineral surfaces play in the (photo)chemicalevolution and distribution of organics in the interstellar medium, comets, meteorites, and other bodies.The photochemistry of organic molecules adsorbed on surfaces is substantially different from moleculesin the gas phase or in matrix isolation. An understanding of these processes is needed to characterize andmodel the chemistry of organic species associated with mineral surfaces in the astrobiological context.Candidate organic molecules for thin-film preparation include amino acids, polyaromatic hydrocarbonsand quinones. Inorganic compounds of interest include silicates, metal oxides, iron-sulfide and iron-nickelalloys. By measuring changes in the UV-Vis-NIR spectra of samples as a function of time in-situ, ORE-Ocube will provide data sets that capture critical kinetic and mechanistic details of sample reactions thatare not obtainable with the current exposure facilities on the ISS. Combining in-situ measurements withpost-flight sample analysis will provide time course studies as well as in-depth chemical analysis.

Acknowledgements

The European participation in OREOcube is funded by the Netherlands Organisation for Scientific Re-search (Evolution of organics in space: OREOcube in situ spectroscopy). U.S. participation in OREOcubeis funded by the NASA Astrobiology: Exobiology and Evolutionary Biology Program.References:

1. P. Ehrenfreund, W.M. Irvine, T. Owen, L. Becker, J. Blank, J.R. Brucato, L. Colangeli, S. Derenne,A. Dutrey, D. Despois, A. Lazcano, F. Robert, Kluwer Academic Publishers, 305, (2004).

2. K.L. Bryson, Z. Peeters, F. Salama, B. Foing, P. Ehrenfreund, A.J. Ricco, E. Jessberger, A. Bischoff,M. Breitfellner, W. Schmidt, F. Robert, Advances in Space Research, 48, 1980-1996 (2011).

208

Figure 15:

3. W.L. Nicholson, A.J. Ricco, E. Agasid, C. Beasley, M. Diaz-Aguado, P. Ehrenfreund, C. Friedericks,S. Ghassemieh, M. Henschke, J.W. Hines, C. Kitts, E. Luzzi, D. Ly, N. Mai, R. Mancinelli, M.McIntyre, G. Minelli, M. Neumann, M. Parra, M. Piccini, R.M. Rasay, R. Ricks, O. Santos, A.Schooley, D. Squires, L. Timucin, B. Yost, A. Young, Astrobiology, 11, 951-958 (2011).

4. N.E. Bramall, R. Quinn, A. Mattioda, K. Bryson, J.D. Chittenden, A. Cook, C. Taylor, G. Minelli,P. Ehrenfreund, A.J. Ricco, D. Squires, O. Santos, C. Friedericks, D. Landis, N.C. Jones, F. Salama,L.J. Allamandola, S.V. Hoffmann, Planetary and Space Science, 60, 121-130 (2012).

209

P6.03 Abiogenic synthesis of biologically important compoundsin open space conditions

Michael Simakov, Natalia Gontareva, Eugenia Kuzicheva

Group of Exobiology, Institute of Cytology, RAS, St. Petersburg, Russia∗E-mail of corresponding author: exobio@mail.cytspb.rssi.ru

The complex chemical processes could take place on surface of small bodies inside any planetarysystems at different stages of their evolution. There are a huge chemical reactor in the course of allstar system’s history and the transport of prebiotic and biotic molecules from outer space to planets isconsidered as an important source of organics. All young star system objects are subjected to energeticprocessing by photons and ions. As a result, the chemical and physical properties of the materialscomposing these objects will change significantly over time. Energetic processing of organic compoundsinto more complex species can be driven by a significantly enhanced UV-field in star forming regions,high-energy particle bombardment, and UV-radiation from the T-Tauri phase in stellar birth; at theearly stage of evolution and at the present, UV-radiation of different wavelengths, protons of the solarwind, and flares can drive this process. Among several energy sources available for abiogenic synthesis ofbiomolecules in space, UV-light with different wavelengths and cosmic rays are two of the most abundant.The reactions of the amino acids in solid mixtures were the primary objective of our investigation,primarily, the abiogenic synthesis of dipeptides from mixtures of simple amino acids. Four mixturesof aromatic (tyrosine or tryptophan) and aliphatic (glycine or alanine) amino acids were investigatedusually. Amino acids were irradiated in solid state with different sources of energy: (1) VUV-light of 145nm; (2) high energy protons (2-6 MeV); (3) gamma-radiation and (4) were installed on the surface ofbiosputnik in outstanding container when they were exposed to the action of all spectra of the open spaceenergy sources during the entire time of flight. We have shown experimentally that the solid mixtures ofamino acids produce more complex compounds when they are exposed to either vacuum UV photons orionizing radiation. Both irradiation and photolysis may destroy molecules as well as allow the synthesisof new and more complex ones. The chemical reaction of solid-state amino acids induced by differentenergy sources has been of increasing interest in several fields such as chemical evolution, polymerizationof simple molecules, origin of homochirality in biomolecules and so on. The aim of our work was alsoto study the in influence of mineral substrates on the reaction of oligomerization of amino acids underthe action of vacuum ultraviolet (VUV) radiation with wavelengths less than 200 nm, one of the mainenergy sources of the Sun. Simple oligopeptides can be formed on solid material not only by VUV-lightbut also by proton radiation, heat, and gamma-radiation. Thus, it can be assumed that the chemicalevolution would have taken place during the early stage of the solar system origin and reached the stageof polymerization before the end of planet accretion. Polymerization is an essential step in prebiologicalevolution and we have shown that this process probably could take place even at early stage of the solarsystem formation, on the surface of small bodies and inside them. The delivery of organic compoundsby carbonaceous chondrites to the early Earth and other planetary bodies could have been an importantsource of prebiotic compounds including simple biopolymers required for the emergence of life.

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P6.04 Photostability of prebiotioc organic compounds from LowEarth Orbit experiments, ground laboratory photolysis, and frommeasurements of absorption vacuum UV (VUV) spectra

Sohan Jheeta1, Nigel J. Mason1, Radmila Panajotovic1, Maria E. Palumbo2, Giovanni Strazzulla2,Daniele Fulvio3, Alicja Domaracka4, Elisabeta Burean5, Anne Lafosse6, Bhalamurugan Sivaraman7, Sly-wia Ptasinska8

1The Open University, Milton Keynes, England, UK2Instituto Nazional di AstroFisica, Catania, Italy3University of Virginia, Charlottesville, Virginia, USA4CEA/CNRS/ENSICAEN/Universite de Caen-Basse, Normandie, France5Universitat Bremen, Germany6Laboratorie des Collisions Atomiques et Moleculaires, Paris, France7NSPIRE Faculty, Indian Institute of Science, Bangalore, India8University of Notre Dame, Indiana, USA∗E-mail of corresponding author: sohan7@ntlworld.com

The field of astrobiology is rapidly becoming a discipline in its own right as it seeks to answer thefollowing questions:

• What are the conditions under which life can develop?• How widespread are these conditions in the Universe?• What are the mechanisms by which life evolves from basic building blocks into self replicating

systems?

It is believed that some of the necessary organic molecules may have been formed in the specialised areasof space (namely dark molecular clouds, eg Horsehead nebula) and delivered on to the Earth duringthe early period of its history, approximately 4.3–4.0×109 years ago. These organic molecules may haveplayed a pivotal role in the formation of life on Earth. In addition it is believed that life on Earth wasformed within a very short geological time frame of only 200–300 million years. So it is not unreasonableto suppose that these molecules were initially made in space as this could be, metaphorically speaking ahuge laboratory when compared to the Earth. Currently we have very little definite knowledge of how lifebegan on Earth, or whether there is life elsewhere in the Universe? These two questions are inextricablyinterlinked in that, as life exists on Earth, it is quite feasible that it should also flourish elsewhere in theUniverse. To answer these questions, mechanisms have to be found whereby non-living chemicals couldbe transformed into 3-dimensional first living organisms. This process is often termed chemical evolution.The research being presented at this conference focuses on the formation of molecules under a varietyof simulated space conditions (eg different temperatures, levels of radiation energies and different typesof impinging radiations). Results pertaining to irradiation of methyl cyanide ice at 15 K with 200 keVprotons and 1:1 mixture of NH3:CO2 ice at 30 K with 1 keV electrons, and 1:1 mixture of NH3:CH3OHice also at 30 K with 1 keV electrons will be presented; see table below. These molecules were chosenbecause they present in the interstellar medium (ISM) and on other satellites, for example carbon dioxide(CO2), ammonium (NH3) and methanol (CH3OH) are second, third and 5th most commonest compoundspresent in the ISM after water (Roush TL, 2001); and methyl cyanide (CH3CN) is the simplest of theorganic nitriles found in space. It was first identified in the molecular clouds, Sagittarius Sgr A and SgrB (Solomon, Jefferts et al. 1971) through its emission lines in the vicinity of 2.7 mm from the J=6-5transition. In addition, CH3CN along with HCN, HCCCN and NCCN, has been identified in the atmo-sphere of Saturn’s satellite, Titan (Raulin and Owen 2002; Raulin 2008). It has also been shown in atheoretical paper that cytosine can be formed from isocyanic acid and cyanate. cytosine, a pyrimidinederivative, is one of the four main bases found in DNA and RNA (Shapiro). The significance of this workfor astrobiology and future experiments will be discussed at the conference.

References:

211

1. Raulin, F. (2008). “Astrobiology and habitability of Titan.” Space Science Reviews 135(1-4): 37-48.

2. Raulin, F. and T. Owen (2002). “Organic chemistry and exobiology on Titan.” Space ScienceReviews 104(1-2): 377-394.

3. Roush, T. L. (2001). “Physical state of ices in the outer solar system.” Journal of GeophysicalResearch-Planets 106(E12): 33315-33323.

4. Shapiro, R. (1999). “Prebiotic cytosine synthesis: A critical analysis and implications for the originof life.” Proceedings of the National Academy of Sciences of the United States of America 96(8):4396-4401.

5. Solomon, P. M., K. B. Jefferts, et al. (1971). “Detection of Millimeter Emission Lines fromInterstellar Methyl Cyanide.” Astrophysical Journal 168(3): L107.

212

P6.05 Stability and alteration of amino acids and related com-pounds against soft X-rays in interplanetary space

Yukinori Kawamoto1,Midori Eto1, Takuto Okabe1,Yumiko Obayashi1, Takeo Kaneko1, Jun-ichi Takahashi2,Hajime Mita3, Kazuhiro Kanda4, Kensei Kobayashi1

1Yokohama National University, Japan2NTT, Japan3Fukuoka Institute of Technology, Japan4University of Hyogo, Japan∗E-mail of corresponding author: kawamoto-yukinori-tf@ynu.ac.jp

Prebiotic organic matters such as amino acids have been found in extraterrestrial bodies. It wassuggested that they were formed in cold space environment, and were delivered to the early Earth. Inter-planetary dust particles (IDPs) were promising carriers since they could deliver organics safer than largemeteorites or comets. On the other hand, IDPs are so small that they are directly exposed to the solarradiation, which may decompose or alter organic molecules in IDPs. In the present study, we evaluatedthe stability of amino acid-related compounds against soft X-rays and extreme ultraviolet light (EUV):Irradiation was performed at NewSUBARU BL-06 (Univ. Hyogo), and the irradiation products were ana-lyzed by several methods including HPLC and XANES. Five amino acid-related samples - Glycine (Gly),hydantoin (Hyd: precursor of glycine), isovaline (Ival), 5-Ethyl-5-methylhydantoin (EMHyd: precursorof isovaline) and complex organic compounds synthesized by proton irradiation of a mixture of CO, NH3

and H2O (referred to as CAW) - were irradiated with continuous light from soft X-rays to IR (hereafterreferred as to soft X-rays) at NewSUBARU BL-06 (University of Hyogo) under high vacuum condition.After collecting the irradiated sample with pure water, we measured the recovery ratio of each compoundby using ion exchange or reversed-phase HPLC systems. In some cases, CaF2 window was used to cutsoft X-rays and EUV (referred as to VUV irradiation; cut-off wavelength is ca. 130 nm). Amino acidsor their precursors were gradually decomposed by soft X-rays irradiation, and water-insoluble organicswere formed. The water-insoluble products could mostly dissolved in dichloromethane. Recovery of theamino acid precursors (Hyd, EMHyd, and CAW) was much more than that of the free amino acids (Gly,Ival) after soft X-rays irradiation. Thus, we could suggest that the precursor amino acids are likely topresent more stable than free amino acids in space environment such as meteorite surface and in IDPs.Neither racemization nor formation of glycine was observed even after 99% of the initial L-alanine wasdecomposed. When CaF2 window was used, little insoluble matters were formed. Thus, soft X-rays(including EUV) are responsible for the formation of insoluble organics. Soft X-rays fraction in the solarradiation is small in the present time, but it is supposed that the strong X-rays were emitted from theyoung Sun before the formation of planetesimals. It should be examined the possible formation of insol-uble organic matter, that is now found in carbonaceous chondrites and comets, by the irradiation withhigh-energy photons from the young Sun. We are now characterizing the samples before and after softX-rays irradiation to see possible alteration processes.

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P6.06 TANPOPO: Astrobiology exposure and micrometeoroidcapture experiments - Proposed experiments using the ExposureFacility on ISS-JEM

Shin-ichi Yokobori1, Hirofumi Hashimoto2, Nobuhiro Hayashi3, Eiichi Imai4, Hideyuki Kawai5, KenseiKobayashi6, Hajime Mita7, Kazumichi Nakagawa8, Issay Narumi9, Kyoko Okudaira10, Makoto Tabata2,5,Sumitaka Tachikawa2,Yuichi Takahashi11,Kaori Tomita-Yokotani12,Hikaru Yabuta13,Masamichi Yamashita2,Hajime Yano2, Akihiko Yamagishi1, Tanpopo WG2

1Sch. Life Sci., Tokyo Univ. Pharm. Life Sci., Hachioji, Tokyo, Japan2JAXA/ISAS, Sagamihara, Kanagawa, Japan3Grad. Sch. Biosci. Biotech., Tokyo Inst. Tech., Yokohama, Japan4Dept. Bioeng., Nagaoka Univ. Tech., Nagaoka, Niigata, Japan5Facl. Sci., Chiba Univ., Chiba, Japan6Grad. Sch. Eng., Yokohama Natl. Univ., Yokohama, Japan7Facl. Eng., Fukuoka Inst. Tech., Fukuoka, Japan8Grad. Sch. Human Develop. Environ., Kobe Univ., Kobe, Japan9JAEA/QuBS, Takasaki, Gunma, Japan10Univ. Aizu, Aizu-Wakamatsu, Fukushima, Japan11Grad. Sch. Sci., Yamagata Univ., Yamagata, Yamagata, Japan12Grad. Sch. Life Environ. Sci., Univ. Tsukuba, Tsukuba, Ibaraki, Japan13Grad. Sch. Sci., Osaka Univ., Toyonaka, Osaka, Japan∗E-mail of corresponding author: yokobori@ls.toyaku.ac.jp

Microbes have been collected from high altitude using balloons, aircraft and meteorological rocketssince 1936, even it is not clear how those microbes could be ejected up to such high altitude (see review in[1]). Spore forming fungi, spore-forming Bacilli, and Micrococci (probably Deinococci) have been isolatedin these experiments. We have also isolated two novel deinococcal species at high altitude (Deinococcusaerius and Deinococcus aetherius) [2, 3]. These spores and Deinococci are known by their extremely highresistance against UV, gamma rays, and other radiations. It is interesting to know which altitude is thehighest limit for the terrestrial lives. If microbes could be found even at the higher altitude of low earthorbit (400 km), the fact would endorse the possibility of interplanetary migration of terrestrial life.

For the origin of life on Earth emerged within a short period after the end of heavy bombardment,Panspermia hypothesis was proposed (e.g. [4, 5]). Recent the reports on the possible fossils of microbesin the Martian meteorite promote the debate on the possible existence of extraterrestrial life, and inter-planetary migration of life as well.

On the other hand, from the viewpoints of chemical evolution for study on the origin of terrestrial life,where is the home of organic compounds that might have become precursors of materials such as proteinand nucleic acids? Recent studies suggest that the some of such organic compounds were created in space.Then, they reached the surface of Earth via meteorites, cosmic dusts, and so on. One of the problemsto study such materials of extraterrestrial origin is the contamination of materials of terrestrial origin.Avoiding contamination of terrestrial materials from the extraterrestrial materials is quite importantissues for this kind of study. Capturing such extraterrestrial materials before falling down on the surfaceof Earth might be one of possible solutions.

TANPOPO, Japanese name of dandelion, is a plant species, whose seeds with floss are spread bywind. We propose this mission to examine possible interplanetary migration of microbes, and organiccompounds at the Exposure Faculty of Japan Experimental Module (JEM) of the International SpaceStation (ISS) [6]. The Tanpopo mission consists of six subthemes capture of microbes in space, exposureof microbes in space, capture of organic compounds in space, exposure of organic compounds in space,measurement of space debris at the ISS orbit, and evaluation of ultra low-density aerogel special for theTANPOPO mission.

Ultra low-density aerogel [7] will capture micrometeoroid and space debris. Particles captured byaerogel will be analyzed after the initial curation of the aerogel and tracks in it. Careful curation of

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the tracks in the aerogel will provide information on the size and velocity of meteorites captured. Theparticles will be characterized in terms of mineralogical, organic and microbiological properties. Theaerogel with low density and layered structure is ready for production in Japan.

In addition to particle-capture on ISS, we also proposed direct exposure experiments of microbial cellaggregates that might protect the microbes themselves from UV and cosmic rays. Deinococcus radiodurans(a type strain and three DNA repair defective mutants), Deinococcus geothermalis, novel deinococcalspecies isolated from specimen collected from high altitude by us (D. aerius and D. aetherius), terrestrialcyanobacteria, and fungi are under consideration for space exposure. Amino acids and complex organiccompounds that can be formed in space are also planed for space exposure.

Our proposal was accepted as a candidate experiment on Exposed Facility of ISS-JEM. In this paper,we overview the TANPOPO mission and discuss the current status of experiments related to the microbeexistence/survival set for this mission.

References:

1. Yang, Y., S. Yokobori, & A. Yamagishi, Biol. Sci. Space 23, 151 (2009)

2. Yang, Y., T. Itoh, S. Yokobori, S. Itahashi, H. Shimada, K. Satoh, H. Ohba, I. Narumi, & A.Yamagishi, Int. J. Syst. Evol. Microbiol. 59, 1862 (2009)

3. Yang, Y., T. Itoh, S. Yokobori, S. Itahashi, H. Shimada, K. Satoh, H. Ohba, I. Narumi, & A.Yamagishi, Int. J. Syst. Evol. Microbiol. 60, 776 (2010)

4. Arrhenius, S., Worlds in the Making-the Evolution of the Universe (translation to English by H.Borns) Harper and Brothers Publishers, New York. (1908)

5. Crick, F., Life Itself. Simon & Schuster, New York. (1981)

6. Yamagishi, A., H. Yano, K. Kobayashi, K. Kobayashi, S. Yokobori, M. Tabata, H. Kawai, M.Yamashita, H. Hashimoto, H. Naraoka, & H. Mita, International Symposium on Space Technologyand Science (ISTS) Web Paper Archives. 2008-k-05 (2008)

7. Tabata, M., Y. Kawaguchi, S. Yokobori, H. Kawai, J. Takahashi, H. Yano, & A. Yamagishi, Biol.Sci. Space 25, 7 (2011)

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P6.07 Experiment SPORES of the EXPOSE-R mission: Survivalof bacterial and fungal spores after nearly 2 years in low Earthorbit

Corinna Panitz1∗†, Gerda Horneck2, Katja Neuberger3, Ralf Moeller2, Elke Rabbow2, Petra Rettberg2,Astrid Lux-Endrich3, B. Hock3, D. P. Hader4, T. Dachev5, Gunther Reitz2

1Medical Faculty, RWTH Aachen, Institute of Flight-Medicine, 52074 Aachen, Germany2German Aerospace Center, DLR, Institute of Aerospace Medicine, 51170 Cologne, Germany3Technische Universitt Munchen, Wissenschaftszentrum Weihenstephan fur Ernahrung. Landnutzungund Umwelt. 85350 Freising, Germany4University, Erlangen, Germany5Space and Solar-Terrestrial Research Institute, Bulgarian Academy of Sciences (SSTRI-BAS), Sofia,Bulgaria∗E-mail of corresponding author: cpanitz@ukaachen.de†E-mail of corresponding author: corinna.panitz@dlr.de

The experiment SPORES “Spores in artificial meteorites” was part of ESA’s EXPOSE-R mission,which exposed chemical and biological samples for nearly 2 years (10.03.2009-21.02.2011) to outer space,when attached to the outside of the Russian Zvezda service module of the International Space Station[1-2]. The overall objective of the biological experiments was to provide experimental clues to the hypo-thetical scenario of Lithopanspermia, which assumes impact-driven interplanetary transfer of life. WithSPORES we addressed the question whether meteorite material offers enough protection against theharsh environment of space for spores to survive a long-term stay in space. For this purpose spores of thebacterium Bacillus subtilis strain 168 (DSM 402) and of the fungus Trichoderma longibrachiatum (DSM63060) were exposed to selected parameters of outer space (space vacuum, galactic cosmic radiation, solarUV radiation of >110 nm or >200 nm). Total UV (200-400 nm) fluence was 859 MJ/m2. Part of thebacterial spores was embedded in different concentrations artificial meteorite powder. The viability ofthe samples was analysed after retrieval. A Mission Ground Reference program was performed parallelto the flight experiment.

The R3D instrument located on the EXPOSE-R platform served as a device for monitoring ionizingand non-ionizing radiation as well as cosmic radiation reaching biological samples within the SPORESexperiment. It covered solar radiation with four channels in the wavelength ranges PAR (400–700 nm),UV-A (315–400 nm), UV-B (280–315 nm), and UV-C (<280 nm) every 10 s. In addition, it recorded thetemperature. Cosmic ionizing radiation was assessed by means of a 256-channel spectrometer dosimeter.The light and UV-sensors were calibrated using spectral measurement data obtained by the SORCEsatellite. The data were corrected with respect to the cosine error of the diodes. In addition, ther-molumescence dosimeters were located close to each biological sample to record their individual dosereceived.

Survival of flight dark samples: About 50% of the spores of B. subtilis 168 in multilayers (5–10spore layers) survived the nearly 2 years exposure to outer space (vacuum, cosmic radiation, extremetemperatures), if they were shielded against solar extraterrestrial electromagnetic radiation. Mixing withmeteorite powder of 0.01 g/mL or 0.03 g/mL did not alter the survival rate significantly. However, thesurvival of B. subtilis spores was reduced by 3 to 5 orders of magnitude, if they were in monolayerswhen experiencing the same treatment. About 30% survival was determined for the flight dark samplesof spores of T. longibrachiatum, demonstrating their high resistance to outer space parameters. In thisexperiment, the fungal spores were contained in UV transparent and air-permeable plastic bags.

Survival of flight sun-exposed samples: Simultaneous exposure of the spores to solar electromagneticradiation, especially to high energy vacuum-UV (¿110 nm) radiation caused a serious inactivation ofthe bacterial spores. B. subtilis spores in multilayers were inactivated by 6 orders of magnitude, and nosurvivors at all were recorded from bacterial spore samples in monolayers. In contrast, T. longibrachiatumspores showed with approximately 20% survival a high viability, even under insolation. The fungal sporeswere arranged in multilayers, so that the upper layer might have provided a certain UV screen for the

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layers beneith.UV shielding by meteorite dust: Embedding bacterial spores in simulated meteorite powder, led to a

slight increase in survival of the insolated samples in multilayers compared to those without meteoritepowder (inactivation by 5 orders of magnitude instead of 6).

Conclusions and outlook: The results of SPORES demonstrate the high resistance of certain bacterialand fungal spores to outer space conditions, if shielded from solar electromagnetic radiation, even afteran exposure time of nearly 2 years. These data confirm earlier results from the 6 year LDEF mission [3]and the 1.5 year EXPOSE-E mission [4], reviewed in [5]. They also demonstrate the high inactivatingpotential of solar UV radiation, especially of UV ¿110 nm. The UV-induced inactivation is most likelycaused by photo-damaging of the DNA. To elucidate the cellular and molecular mechanisms of injuryand protection, analyses of the molecular injuries in the DNA of the spores, produced by UV radiationand/or space vacuum, and mutation studies are currently in progress. With this, the data contribute toour understanding of the chances and limits of interplanetary transfer of spores, e.g. if embedded in rockmaterial.

References:

1. G. Horneck, D.D. Wynn-Williams, R.L. Mancinelli, J. Cadet, N. Munakata, G. Ronto, H.G.M.Edward , B. Hock, H. Wnke, G. Reitz, T. Dachev, D.P. Hder, C. Brillouet Biological experimentson the expose facility of the International Space Station ISS, In: Proceedings of the 2nd Euro-pean Symposium on the Utilitation of the International Space Station, ESTEC, Noordwijk, TheNetherlands, 16-18 November 1998, ESA SP-433, pp. 459-468. (1999)

2 E. Rabbow, G. Horneck, P. Rettberg, J.-U.Schott, C.Panitz, A. L’Afflitto, R.vonHeise-Rotenburg,R.Willnecker, P.Baglioni, J. Hatton, J.Dettmann, R.Demets, G.Reitz. EXPOSE, an astrobiologicalexposure facility on the International Space Station - from proposal to flight. Orig. Life Evol.Biosph. 39:581-598 (2009)

2. G. Horneck, H. Bucker, G. Reitz. Long-term survival of bacterial spores in space. Adv. Space Res.14:(10)41-45 (1994).

3. G. Horneck, R. Moeller, J. Cadet, T. Douki, R. L. Mancinelli, W. L. Nicholson, C. Panitz, E.Rabbow, P. Rettberg, A. Spry, E. Stackebrandt, P. Vaishampayan, K. Venkateswaran. Resistanceof bacterial endospores to outer space for Planetary Protection purposes – Experiment PROTECTof the EXPOSE-E mission, Astrobiology 12:445-456 (2012)

4. G. Horneck, D.M. Klaus, R.L. Mancinelli Space microbiology. Microbiol. Mol. Biol. Rev. 74:121-156 (2010).

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P6.08 Altered gravity conditions and its effect on the phagocyto-sis related ROS-production of Blue Mussel hemocytes – Resultsof the 56th ESA parabolic flight campaign

Eckehardt Unruh∗, Peter-Diedrich Hansen†

Berlin Institute of Technology, Dept. for Ecological Impact Research and Ecotoxicology, Berlin, Germany∗E-mail of corresponding author: e.unruh@tu-berlin.de†E-mail of corresponding author: peter-diedrich.hansen@tu-berlin.de

The production of reactive oxygen species (ROS) is a key component of the immune defense of anorganism. ROS is the precurser in the production of anti-microbial substances used by phagocytotic cellsfor destroying foreign particles. In this regard hemocytes of the Blue Mussel share a lot of similaritieswith macrophages of higher developed organisms.

For the experiment described, isolated Hemocytes in primary culture were used for investigating theeffects of altered gravity conditions during a parabolic flight campaign. The phagocytosis of the cellsbecame triggered with zymosan and the ROS-production of the cells became measured as luminescenceusing peroxidase and luminol as reporters.

The measurements were done with the PMT-clinostat (DLR/Cologne) under temperature controlledconditions on board of the Airbus Zero-G during the 56th parabolic flight campaigne in Mai 2012.

By choosing hemocytes of the Blue Mussel as a cell model TRIPLE-LUX B is investigating a type ofcells that is representing a phylogeneticaly earlier stage of development of immunesystems.

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P6.09 BIOMEX-Desert Cyanobacteria: ground simulations ofthe EXPOSE-R2 mission

Mickael Baque1∗, Daniela Billi1, Jean-Pierre Paul de Vera2

1University of Rome Tor Vergata, Italy2Deutsches Zentrum fur Luft- und Raumfahrt e.V. (DLR), Germany∗E-mail of corresponding author: mickael.baque@gmail.com

Presumably in 2013, new experiments will be performed in space on the EXPOSE facility of theEuropean Space Agency (ESA) attached to the exterior of the International Space Station (ISS). Amongthe selected experiments for the new mission, called EXPOSE-R2, BIOMEX (BIOlogy and Mars EXper-iment) focuses on extremophiles such as lichens, Achaea, cyanobacteria, fungi, bacteria and their cellularcomponents. BIOMEX aims to investigate their resistance when embedded with Martian and lunarmineral analogues. Moreover, resistance of their constituents (biomolecules such as pigments, cell wallcomponents) will be investigated in order to create a biosignature database for the search of life beyondEarth. One of the organisms selected for this experiment is the cyanobacterium Chroococcidiopsis iso-lated from extremely dry, hot and cold deserts on Earth. Being one of the first phototrophic organisms toappear on the early Earth, its relevance for astrobiology has been assessed in the past years concerning thesearch for life or future space applications (life support systems, biomining). Indeed its resistance to spaceand Martian simulated conditions (Billi et al. 2011) as well as real space exposure (Cockell et al. 2011)along with ionizing radiations (Billi et al. 2000) and prolonged desiccation (Billi 2009) have been alreadyreported. To further decipher the molecular basis of its resistance and protection mechanisms and in thepreparation of the future EXPOSE mission, ground simulations have been performed and the first resultsare being exploited. Chroococcidiopsis strain CCMEE 029 (isolated from Negev desert, Israel) exhibits ahigh survival to the Experiment Verification Tests (EVTs) and Science Verification Tests (SVTs) basedon colony forming ability, integrity of cellular components, like presence of undamaged DNA (assessedby PCR genomic fingerprinting) and permanence of photosynthetic pigments (revealed by CLSM). Newexperimental approaches techniques are being developed in order to complete our understanding of itsextreme resistance.

References:

Billi D, Viaggiu E, Cockell CS, Rabbow E, Horneck G, Onofri S. (2011). Damage escape and repair indried Chroococcidiopsis spp. from hot and cold deserts exposed to simulated space and Martianconditions. Astrobiology 11:65-73

Billi D. (2009). Subcellular integrities in Chroococcidiopsis sp. CCMEE 029 survivors after prolongeddesiccation revealed by molecular probes and genome stability assays. Extremophiles 13:4957

Billi D, Friedmann EI, Hofer KG, Caiola MG, Ocampo-Friedmann R. (2000). Ionizing-Radiation Resis-tance in the Desiccation-Tolerant Cyanobacterium Chroococcidiopsis. Appl. Environ. Microbiol.66:14891492

Cockell CS, Rettberg P, Rabbow E, Olsson-Francis K. (2011). Exposure of phototrophs to 548 days inlow Earth orbit: microbial selection pressures in outer space and on early earth. ISME J 5:16711682

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P6.10 Survival of Chroococcidiopsis and its biosignatures in LowEarth Orbit

Casey Bryce1∗, Sophie Nixon1, Howell Edwards2, Gerda Horneck3, Charles Cockell1

1School of Physics and Astronomy, The University of Edinburgh, Edinburgh, UK2Chemical and Forensic Sciences, University of Bradford, Bradford, UK3Institute of Aerospace Medicine, German Aerospace Center (DLR), Koln, Germany

∗E-mail of corresponding author: c.s.cockell@ed.ac.uk

An understanding of the ability of microorganisms to survive the harsh extremes of space contributesto a number of areas of Astrobiology. Microbes will be important in future efforts in space settlement,for example in life support systems or in situ resource utilisation. Therefore, knowledge of the survivalcapabilities of candidate organisms in the conditions encountered in space is essential. The survival ofmicrobes in the space environment also informs our efforts in planetary protection, whereby the contam-ination of other planetary bodies during space missions can be avoided.

We report results of the ROSE 1 experiment which was mounted externally aboard the InternationalSpace Station (ISS) in March 2009 for 22 months as part of the multi-user EXPOSE-R facility. Theseexperiments aimed to study the survival of cells of Chroococcidiopsis, a cyanobacterium demonstrated totolerate a wide array of extremes (Friedman & Ocampo-Friedman, 1995; Stoffler et al, 2007), and thelongevity of biosignatures associated with these. Cells were either desiccated on to glass discs or soakedinto the pore space of specifically designed discs of impact-shocked gneiss before being integrated into theEXPOSE-R facility. Using a range of filters, the glass discs were exposed to UV radiation at >110nmand >170nm wavelengths at 0.1%, 1% and 100% intensity and housed in containers either vented to thevacuum of space or filled with boron gas to simulate an atmosphere. The gneiss discs were all exposedto space vacuum and 100% UV intensity at wavelengths greater than 170nm.

We report the viability of the microbes subjected to conditions in Low Earth Orbit on their returnto Earth in the aim of establishing the tolerance of Chroococidiopsis to space conditions and the level ofprotection afforded to these microbes by the rocks. In addition, results of Raman spectroscopy allow usto investigate the effects of the space environment on the preservation of biosignatures which can conveyinformation about living organisms long after their death. This has implications for the detection ofmolecular signatures of life beyond the Earth.

References:

1. Friedmann & Ocampo-Friedmann (1995) Adv. Space Res. Vol. 15:3, (3)243-(3)246

2. Stoffler, D. et al (2007) Icarus. Vol. 186, 585-588

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P6.11 UV resistance properties of the space-tested lichens speciesRhizocarpon geographicum and Circinaria gyrosa : role of thecortex/screening substances and hydration state of the thalli

Francisco J. Sanchez Inigo1∗, Rosa de la Torre Noetzel1, Leopoldo Ga. Sancho2, Gerda Horneck3

1Earth Observation Department, INTA. Ctra. de Ajalvir, Km. 4, Torrejon de Ardoz, 28850 Madrid,Spain2Departamento de Biologa Vegetal II, Facultad de Farmacia, UCM, E-28040 Madrid, Spain3DLR, Institute of Aerospace Medicine, Radiation Biology, 51147 Koln, Germany∗E-mail of corresponding author: sanchezifj@inta.es

One of the major astrobiological challenges is to study the feasibility of life in space, as it helps to 1)understand the origin and evolution of life on Earth 2) deepen our knowledge of the limits of life. Manyexperiments have been designed to investigate the effects of the extraterrestrial environment on livingorganisms, and for this purpose, extremophile terrestrial organisms have been perfect candidates.

Rhizocarpon geographicum is a crustose bipolar lichen species that grows on high mountains of bothhemispheres with a very low growth rate (about 0.5 mm/year). During the development of the ex-periments LICHENS (2005) [1], LITHOPANSPERMIA (2007) [2] and LIFE (2010) [3], samples of R.geographicum were exposed to low Earth orbit (LEO) environment including vacuum (10−6 mbar), ex-traterrestrial radiation, and simulated Mars UV radiation (200-400nm). The first two experiments hadduration of two weeks approximately and after exposure in space, all samples showed cell integrity andlevels of photosynthesis comparable to those recorded before the flight. In the LIFE experiment theexposure time was of 1.5 year long and the samples vitality was considerably reduced after the flight.Circinaria gyrosa is an extremophile vagrant lichen (Megasporaceae family) with a coralloid thallus anda very compact internal structure; and it is characteristic of arid areas with extreme temperature fluctua-tions and high levels of solar irradiation. Samples of C. gyrosa were included in the LITHOPANSPERMIAexperiment, and this lichen did not reveal any significant physiological changes, demonstrating a highresistance towards real space flight conditions [2] & [4].

Field studies at the mountain system of Sierra de Gredos (Central Spain) have been performed todemonstrate that the upper pigmented cortex of R. geographicum has a protective function. Removal ofthis structure reduced the effective quantum yield to about a 50% [5]. Therefore, it has been proposedthat the cortex is a key mechanism to prevent UV damage [1]. Also the humidity content of the thallicould be a main factor in the resistance of these organisms against UV, as desiccated thalli possess uniqueand very efficient high-energy thermal dissipation mechanisms to avoid internal structural damages [6].In order to assess the actual influence of these hypothetical protective mechanisms involved in the pre-vention of UV damage in lichens, we have performed four sets of UV irradiation tests in the laboratorywith increasing doses of UV-B and UV-C: with and without cortex in R. geographicum, with and with-out lichenic screening compounds in C. gyrosa (as the removal of the cortex in C. gyrosa is technicallyimpossible, our approach has been to extract the secondary lichen products with acetone 100%); anddifferentiating between dry or wet thalli.

Experimental design:

• UV wavelengths: UV-B, UV-C

• Range of doses: 250 J/cm2 (≈10h) - 1200 J/cm2 (≈48h)

• Number of samples per dose: 3

– Sets:∗ Set 1: Intact, dry thalli (R. geographicum and C. gyrosa)∗ Set 2: Intact, wet thalli (R. geographicum and C. gyrosa)∗ Set 3: Cortex removed/Acetone rinsed, dry thalli (R. geographicum and C. gyrosa respec-

tively)

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∗ Set 4: Cortex removed/Acetone rinsed, wet thalli (R. geographicum and C. gyrosa respec-tively)

Before and after the irradiations, the viability of the samples was analyzed in terms of PSII activityby means of chlorophyll a fluorescence, measured with a Mini-PAM fluorometer (WALZ, Germany) andwas taken as a measure of the general status of the whole system. The comparison between previousand posterior values made it possible to assess the physiological state of the samples and the influenceof the different doses and conditions. Preliminary results show very high levels of UV resistance, withslight differences according to: 1) the presence or absence of cortex and/or secondary products and 2)the hydration state of the samples.

References:

1. L.G. Sancho, R. de la Torre, G. Horneck, C. Ascaso, A. de los Ros, A. Pintado, J. Wierzchos andM. Schuster, Astrobiology, 7(3), 443-454 (2007)

2. R. de la Torre, L.G. Sancho, G. Horneck, A. de los Ros, J. Wierzchos, K. Olsson-Francis, C. Cockell,P. Rettberg, T. Berger, J.P. de Vera, S. Ott, J.M. Fras, M.P. Gonzalez, M.M. Luca, M. Reina, A.Pintado and R. Demets, Icarus, 208, 735-754 (2010)

3. S. Onofri, R. de la Torre, J.P. de Vera, S. Ott, L. Zucconi, L., Selbmann, G. Scalzi, K.J. Venkateswaran,E. Rabbow, F.J. Sanchez and G. Horneck, Astrobiology, 12, 508-516 (2012)

4. J. Raggio, A. Pintado, C. Ascaso, R. de la Torre, A. de los Ros, J. Wierzchos and L.G. Sancho,Astrobiology, 11 (4), 281-292 (2011)

5. R. de la Torre, L.G. Sancho and G. Horneck, ESA Communications, ESA SP-1299, 145-150 (2007)

6. U. Heber, Physiologia plantarum, 142, (1):6578 (2010)

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P6.12 Survival of lichens to simulated Mars conditions

Rosa de la Torre Noetzel1∗, Francisco J. Sanchez Inigo1, Elke Rabbow2, Gerda Horneck2, Jean-Pierre deVera3, Leopoldo Ga. Sancho4

1INTA, Spanish Aerospace Research Establishment, Madrid, Spain2DLR, German Aerospace Center, Cologne, Germany3DLR, German Aerospace Center, Berlin, Germany4UCM, Univ. Complutense Madrid, Madrid, Spain∗E-mail of corresponding author: torrenr@inta.es

Lichens, as extremophilic organisms at Earth, have demonstrated their survival capacity at space.Previous experiments performed (LICHENS, Foton M2-2005 and LITHOPANSPERMIA, Foton M3-2007) [1,2] have shown that short term exposures to LEO (Low Earth Orbit) conditions do not havea significant deleterieous effect on their vitality, meanwhile long term experiments show more relevantchanges (LIFE experiment, EXPOSE-E, ISS, 2008-2009) [3]. This could be explained by the lichensstructural and physiological features, which allowed them to survive the harsh environmental conditionson Earth (high UV radiation, extreme temperatures and desiccation), as well as in space (high UV spaceradiation, UV-vacuum, extreme temperatures and microgravity). But not too much research has beenperformed with lichens at Mars environmental conditions that have been simulated in the laboratory(Mars UV radiation, Mars CO2 atmosphere and pressure, and Mars temperature) [4].

In this work we report the results obtained with the most resistant lichen species known until now toharsh space conditions: Circinaria gyrosa (renamed from A. fruticulosa see Sohrabi, M., 2012), a vagrantlichen collected at the steppic highlands of Central Spain. This lichen has been exposed to harsh spaceconditions, tested in the Experiment Lithopanspermia [5], and to Mars simulated conditions, reproducedat the EVT-1, EVT-2 and SVT tests performed at the DLR-Planetary simulation chambers of DLR(Deutsches Zentrum fur Luft- und Raumfahrt, Cologne, Germany). These tests are necessary to checkthe resistance and survival capacity of biological samples in preparation of the next EXPOSE R2 spacemission, sheduled for 2013, when the EXPOSE-R2 facility with 3 astrobiological experiments, one of themthe experiment BIOMEX-ESA (Biology and Mars Experiment, PI: DLR-Berlin, de Vera), including ourlichen Circinaria gyrosa, will be placed on the ISS, to real space and to simulated Mars conditions for 1to 1.5 years (2013 to 2014). Different sets of samples in contact with Martian regolith surrogates P-MRSand S-MRS (early acidic and late basic regolith simulants), were exposed to the same conditions. Theresults have shown no significant differences of the PS-II activity or photochemical efficiency measuredwith a PAM fluorometer before and after exposure to simulated Mars UV solar radiation (> 200 nm,Mars CO2 atmosphere at a pressure of 930 Pa. These tests demonstrate the optimal resistance andsurvival capacity of Circinaria gyrosa, a lichen species defined as model system in Astrobiology whichcould contribute to the better understanding of the habitability of a planets surface, i.e. Mars, as well asto the Lithopanspermia hypothesis [6].

References:

1. R. De la Torre Noetzel, L.G. Sancho, A. Pintado, P., Rettberg, E., Rabbow, C. Panitz, U.Deutschmann, M. Reina, G. Horneck BIOPAN experiment LICHENS on the Foton M2 mission:Pre-flight verification tests of the Rhizocarpon geographicum-granite ecosystem, Adv. Space Res.40, 1665-1671 (2007)

2. L.G. Sancho, R. De la Torre, Horneck, G., C. Ascaso, A.de los Ros, Pintado, J.Wierzchos, M.Schuster. Lichens survive in space: Results from 2005 LICHENS experiment. Astrobiology 7,450454 (2007)

3. S. Onofri, R. De la Torre, J.P. de Vera, S.Ott, L.Zucconi, L.Selbmann, G. Scalzi, K.J.Venkateswaran,E. Rabbow, F.J. Sanchez Inigo, G. Horneck. Survival of Rock-Colonizing Organisms After 1.5 Yearsin Outer Space. Astrobiology 12(5): 508-516 (2012)

223

4. J.P. de Vera, D. Mohlmann, F. Butina, A. Lorek, R. Wernecke, S. Ott. Survival Potential and Pho-tosynthetic Activity of Lichens Under Mars-Like Conditions: A Laboratory Study. Astrobiology,10: 215-227 (2010)

5. R. De la Torre, L.G. Sancho, G. Horneck, A.de los Ros, J. Wierzchos, K. Olsson-Francis, C.S.Cockell, Rettberg P., T. Berger, J.P. de Vera, S. Ott, J. Martinez Fras, P.Gonzalez Melendi M.M.Lucas, M. Reina, A. Pintado, R.Demets. Survival of lichens and bacteria exposed to outer spaceconditions. Results of the Lithopanspermia experiments. Icarus, doi:10.1016/j.icarus.2010.03.010(2010)

6. C. Mileikowsky, F.Cucinotta, J. W.Wilson, B.Gladman, G.Horneck, L.Lindegren, J.Melosh, H.Rickman,M.Valtonen, J.Q. Zheng. Natural transfer of viable microbes in space, Part 1: From Mars to Earthand Earth to Mars. Icarus 145, 391-427 (2000)

224

P6.13 Lichens as a model-system for survival of eukaryotic sym-biotic associations exposed to space conditions

Annette Brandt1∗, Jean-Pierre P. de Vera2, Joachim Meeßen1, Sieglinde Ott1

1Institute of Botany, Heinrich-Heine-University, Dusseldorf, Germany2Institute of Planetary Research, DLR, Berlin, Germany∗E-mail of corresponding author: annette.brandt@uni-duesseldorf.de

Lichens are symbiotic organisms consisting of a fungus (mycobiont) and a photosynthetic partner(cyanos or green algae; photobiont). The symbiosis of the different bionts enables these organisms tocolonize most extreme habitats as polar regions, deserts and alpine zones; handling aridness, chill, heat,solar insolation and UV irradiation. Lichens as poikilohydric organisms are well suitable model-systemsto study adaptation mechanisms to most extreme environmental conditions enabling eukaryotic life. Aslichens clearly demonstrated a high resistance to simulated space conditions [1], experiments with thelichen species Xanthoria elegans have been performed additionally to former studies on simulated spaceconditions as UV-radiation, X-ray-radiation, shock pressure resistance, vacuum (strong desiccation) totest the resistance to space conditions, emphasizing the (long term) viability of both bionts and the abilityto reproduce (including the production of sound offspring): Xanthoria elegans has been exposed to spaceand simulated Mars conditions for 1.5 years in the EXPOSE-E device of the International Space Station(EXPOSE-E / LIFE Project, ESA) in Low Earth Orbit. In first studies on the ability of photosyntheticactivity of the photobiont in Xanthoria elegans after 18 months exposure to space conditions the lichencould be reactivated [2]. Furthermore the current study includes investigations on vitality and repro-duction of the lichen and both of its bionts (chlorophyll fluorescence imaging, spore germination, CLSManalysis), their protective structures (i.e. the pigment layer), micro- and ultra-structural analysis (TEM,SEM) and DNA damage analysis, as well as the search for DNA damage repair systems. The up-to-dateresults of these examinations will be presented.

References:

1. de Vera et al. 2004, 2008, 2010

2. Onofri et al., 2012

225

P6.14 Microbial Fuel Cells in Life Support Systems

Ximena C. Abrevaya1∗, Pablo J.D. Mauas1, Eduardo Corton2

1Instituto de Astronoma y Fsica del Espacio - UBA - CONICET, Buenos Aires, Argentina2Depto. de Quımica Biologica, IQUIBICEN - FCEyN - UBA - CONICET, Buenos Aires, Argentina∗E-mail of corresponding author: abrevaya@iafe.uba.ar

Biological Life Support Systems (BLSSs) are already being developed as a way to maintain suitableliving conditions for humans during long manned missions to space including space flights, space stations,potential human exploratory missions to Mars, or even to be included in a Lunar base. Thought asartificial ecosystems, the involvement of photosynthetic organisms are an essential part of it, as occursnaturally in our biosphere on Earth. This is the case of MELIiSSA (Micro-Ecological Life SupportSystem Alternative), a platform originated in 1988 and fostered by the European Space Agency [1]. Itwas developed as a regenerative life support system based on plants and microorganisms. The main goalof this platform is to obtain O2 converting CO2 and H2O through biological processes, and also to obtainfood.

On the other hand, Biological Fuel Cells are bioelectrochemical devices developed for the generationof electrical power. In these devices, the power source is given by biocatalysts such as enzymes, or bymicroorganisms (in this case they are called Microbial Fuel Cells, MFCs) which as part of their metabolicprocesses release electrons that supply the electric current production. They work in a similar way to abattery, and the most common configuration contains an abiotic oxidative cathode and a biotic reductiveanode (both in an aqueous, close to neutral pH diluted media) separated by a cation exchange membrane,although numerous more configuration types are described in the literature.

These metabolic processes carried out by microorganisms in MFCs, allow oxidation of organic material,releasing electrons and protons. These electrons are captured by a corrosion- resistant conductor (anode),and travel through an external conductor, reaching the cathode and closing the circuit. This electronflow, proportional to metabolic and other redox processes in the anode and cathode region, can easily bemeasured as current if an adequate resistor is incorporated in the electric circuit.

At present, there is much work done with MFCs, with multiple combinations of electrode materialand microorganisms [2], [3], [4]. They were also built using different kind of complex substrates fromwastewaters to lignocellulosic biomass, and also in the form of plant-MFCs [5], [6].

Other applications of MFCs are related to remediation of soils and in the wastewater treatment[7], [8] and for autonomous remote power generation for robotic exploration in space (e.g. low powermicrorobotics as microrovers). Recently, we showed that MFCs can be used as in situ life detectiondevices [9].

In this work we propose the inclusion of MFCs in BLSSs, taking advantage of the involvement oforganisms in both systems, and we show that this could be applied to obtain energy, which would becoupled to obtaining O2 and food, and can also be used for the treatment of waste during long mannedmissions.

References:

1. M. Mergeay, W. Verstraete, G. Dubertret, M. Lefort-Tran, C. Chipaux, R. Binot, Proceedings ofthe 3rd symposium on space thermal control and life support systems. Noordwijk, The Netherlands(1998)

2. K. Rabaey and W. Verstraete, Trends in Biotechnology, 23, 291 (2005)

3. R.A. Bullen, T.C. Arnot, J.B. Lakemanand, F.C. Walsh, Biosensensors and Bioelectronics, 21, 2015(2006)

4. Davis, F. and Higson, P.J., Biosensors and Bioelectronics, 22, 1224 (2007)

5. D. Pant, G. Van Bogaert, L. Diels, K. Vanbroekhoven, Bioresource Technology, 101,1533 (2010)

6. M. Rosenbaum, Z. He and L.T Angenent, Current Opinion in Biotechnology, 21, 259 (2010)

226

7. K.B. Gregory and D.R. Lovley, Environmental Science and Technology, 39, 8943(2005)

8. B.E. Logan, Water Science Technology 52, 31 (2005)

9. X.C. Abrevaya, P.J.D. Mauas, E. Corton, Astrobiology, 10, 965 (2010)

227

P6.15 EXPOSE-R2 - the upcoming astrobiological exposure mis-sion

Elke Rabbow1∗, Petra Rettberg1, Rainer Willnecker2, Gunther Reitz1

1Institute of Aerospace Medicine, Radiation Biology, DLR, D-51147 Cologne, Germany2MUSC, DLR, D-51147 Cologne, Germany∗E-mail of corresponding author: Elke.Rabbow@dlr.de

In the upcoming year 2013, the 3rd EXPOSE mission is scheduled for launch to the InternationalSpace Station ISS. ESA selected 3 international astrobiological experiments for exposure on the multiuserfacility, plus one guest experiment from IBMP. It will be the 2nd EXPOSE attached to the URM-Dplatform on the Russian Zvezda Module, therefore named EXPOSE-R2.

The previous 2 EXPOSE missions, EXPOSE-E accommodated on the EuTEF platform on one ofthe external balconies of the European Columbus Module [1] and the first EXPOSE-R attached to theURM-D platform on the Russian Zvezda Module were performed successfully and returned to Earthfor subsequent analysis after 18 month and 22 month exposure in space respectively. The EXPOSEfacilities are comprised of a boxlike core structure with electronics and heating systems, and 3 insertedtrays harbouring the astrobiological samples. After the EXPOSE-R mission, the EXPOSE-R core facilityremained on board the ISS, while the 3 trays with the samples returned to Earth.

For EXPOSE-R2, 3 trays will be equipped with the samples of the EXPOSE-R2 investigator teams,brought to the ISS with a Progress and inserted into the core facility by the crew. The complete facilitywill be exposed for at least 12 month in space, and the trays returned to ground as for EXPOSE-R.

Starting in 2011, the pre-flight test program for EXPOSE-R2 was performed at DLR/MUSC inCologne, simulating the space parameters like vacuum, temperature oscillation and short wavelength UVas expected during the mission on the ISS. The extensive experience collected during the preparation andoperations of the previous 2 missions highly supported the preparation of the current mission.

Here, an overview of the EXPOSE-R2 design, the selected chemical, biological and dosimetric experi-ments, the mission, mission parameters and mission operations as expected from the previous 2 missionsas well as the planned mission parallel Mission Ground Reference MGR will be given. In addition, thepre-flight test program for the EXPOSE-R2 mission as performed and the current status of EXPSOE-R2will be presented.

References:

1. Special issue ASTROBIOLOGY, 12, (5)

228

P6.16 Comparative studies on the morphological-anatomical,chemical, and physiological properties of four space-relevant lichenspecies to assess their high potential in resisting extreme envi-ronmental conditions

Joachim Meeßen1∗ Francisco Javier Sanchez2 Annette Brandt1 Eva-Maria Balzer2 Kai Lyhme1 PaulWieners1 Jean-Pierre de Vera3 Rosa de la Torre2 Sieglinde Ott1

1Institute of Botany, Heinrich-Heine-University, Dusseldorf, Germany2Instituto Nacional de Tecnica Aeroespacial (INTA), Torrejon de Ardoz, Madrid, Spain3Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany∗E-mail of corresponding author: joachimmeessen@gmx.de

Lichens are symbiotic, generally extremo-tolerant associations between a heterotrophic fungus (my-cobiont) and photoautotrophic green algae or cyanobacteria (photobionts). Together, both bionts form anew and highly complex morphological and physiological phenotype. Its emergent properties adapt thelichen to extreme terrestrial habitats, what is the main reason to use them as targets for astrobiologicalexperiments. Amongst other factors (as morphological plasticity), their persistence is related to theirpoikilohydric nature, being able to resist harsh environmental conditions when dry and activating theirmetabolism when water is available, normally under milder conditions. Three lichen species are usedin astrobiological research: The lichens Rhizocarpon geographicum, Circinaria gyrosa (formerly Aspiciliafruticulosa), and Xanthoria elegans were utilized in several flight experiments (LICHENS II (BIOPAN5), LITHOPANSPERMIA and STONE (BIOPAN 6), and LIFE (EXPOSE-E) as well as in numeroussimulation studies [1]. In 2013, C. gyrosa and Buellia frigida an extremo-tolerant Antarctic endemiclichen are scheduled to take part in the BIOMEX exposure experiment (Biology and Mars Experiments,ILSRA-AO 2009) on EXPOSE-R2. These four lichens species are investigated in a comparative approachon their morphological and anatomical traits, on the chemical properties of their dominant secondarylichen compounds, and on selected physiological properties concerning their water balance. The resultspresented, will contribute to a better understanding of the high resistance potential towards and theremarkable viability after exposure to real or simulated space conditions of these four lichen species aseukaryotic model organisms. The results will extend the knowledge of damage caused by exposure to themost extreme conditions as present in space.

References:

1. L. G. Sancho, R. de la Torre, A. Pintado (2009): Lichens, new and promising material from exper-iments in astrobiology. Fungal Biology Reviews 22, 103-109

Index

13C/12C, 42Deinococcus, 89, 91, 198, 214

acetogenesis, 44alanine, 129amino acid, 185amino acids, 45, 55, 72, 75, 116, 129, 130, 150,

207, 210, 213ammonia, 32, 60, 132, 168, 188anaerobic, 126, 143, 161, 169arsenic, 128atmosphere, martian, 60, 168atmosphere, planetary, 183ATP, 45, 46, 83, 87, 125, 127, 137, 161

bacteria, planktonic, 198basalts, 158BIF, 164bio-mining, 78biodiversity, 76, 140biofilm, 198biology, synthetic, 78biomarker, 42, 158, 181, 194biopolymers, 45biosignatures, 62, 160, 206, 219biosphere, 57, 93, 158, 166, 171, 202black death, 149

carbohydrates, 75carbonaceous chondrites, 116, 130, 155Cassini mission, 182chondrites, 210chondrites, carbonaceous, 210CO2, 60, 168Columbus Module, 228contamination, 169corrosion, 126cryogenic, 57, 202crystallization, 55, 150crystals, 139cyanobacteria, 60, 168, 192, 196cycles, biogeochemical, 152

Darwinian Evolution, 33deep biosphere, 80, 158degradation, 42

density waves, 29DFT, 128disequilibrium, 152DNA, 63, 72, 79, 128, 141, 147, 172, 184, 204, 214,

216droplets, 205dust, 154dust grains, 32dust particles, 213

EANA, 104ESA, 37, 153escape velocity, 183eukaryotes, 79, 147, 148Europa, 31, 184EUROPLANET, 99EuroPlaNet, 96ExoMars, 100, 164, 181exoplanets, 31EXPOSE, 228extremophiles, 52, 57, 117, 202, 223

Fe2+, 44, 130, 161formaldehyde, 32formic acid, 32

gamma-rays, 54, 122glacier, 57, 126, 184, 202glycine, 45, 207, 210, 213Gusev Crater, 164

habitability, 28, 152habitable zone, 31Hadean Earth, 180Hesperian period, 165homochirality, 55, 72, 75, 150horizontal gene transfer, 79hot Jupiters, 31, 112, 114hydrocarbons, 137hydrothermal cherts, 164hydrothermal systems, 80hydrothermal vents, 44

ice, 32, 57, 66, 67, 70, 80, 112, 202, 203, 211ice, glacial, 57, 202inclusions, 54, 122

229

230 INDEX

ionization, 170ISM, 32, 128, 211ISS, 214, 228

komatiites, 41

LECA, 79lichen, 192, 229lichens, 223, 225lightning, 47, 134lithification, 206LUCA, 49luminol, 218

M dwarfs, 53, 118Mossbauer, 174Mars, 38, 39, 41, 42, 58, 60–63, 68, 83, 100, 129,

152, 156–158, 160, 161, 164–168, 171–174, 176, 184, 185, 189, 193, 201, 206,219, 223, 226

Mars Express, 100MATROSHKA, 96membranes, 125, 147metabolism, 44, 125, 145metabolisms, 161metallicities, 31, 123meteorite craters, 80meteorites, 54, 55, 122, 126, 150, 161, 177meteorites, martian, 156methane, 38, 82, 142methanogenesis, 44methanogens, 68, 158methyl cyanide, 211methylobacterium, 205microbes, 44, 63, 80, 82, 89, 142, 143, 161, 169,

172, 192, 205, 214, 218microbial, 142, 184, 194, 218microfossils, 80, 206micrometeorites, 207microorganisms, 66, 149, 193, 197, 226mixing, 166molecular clouds, 32, 123, 211mycobiont, 225

NAI, 104Noachian Mars, 180Noachian period, 165nucleic acids, 137nucleotides, 45

Ozone, 61, 189

panspermia, 89, 141PCR, 204permafrost, 66, 68, 201Phanerozoic eon, 76, 140

pharmaceuticals, 78photobiont, 225photosynthesis, 148, 226photosynthesize, 60, 168pillow basalt, 165planets, atmospheres, 28planets, extrasolar, 28planets, habitable, 53, 118planets, rocky, 28, 52, 117plasma, 114, 126, 170, 188polymerization, 45, 210prokaryotes, 135, 160protocell, 145pyrimidines, 141

radicals, 58, 176Raman spectroscopy, 41, 48, 181reactive oxygen species, 218Rio Tinto, 82, 162RNA world, 79

salinity, 196sample return, 228SEM, 116, 129, 130, 132, 156, 197serpentinization, 38, 44, 127, 129SETI, 33, 124siderophores, 148, 197snoRNA, 79, 147snow algae, 57, 202Solar System, 103solar system, 210solar wind, 210space missions, 110Stardust, 149sublimation, 55, 150sulfur, 49sulphur, 142Super-Earths, 28, 29, 112, 113

T-Tauri, 210Titan, 93, 182, 187, 188, 211titanium oxide, 112ToF-SIMs, 48troilite, 192

uracil, 141UV, 181, 196, 210UV radiation, 141

Venus, 113, 185, 186vesicles, 147viruses, 139, 147, 160, 171volatiles, 178volcanoes, 47

INDEX 231

weathering, 37, 38, 48, 60, 127, 148, 153, 168, 192,197

wetting-drying, 47

232 INDEX

$Header: /var/cvs/brandenb/tex/bio/SwAN/EANA/2012/Workshop/booklet.tex,v 1.331 2012-10-10 09:02:38 giannicataldi Exp $

Special meetings in connection withEANA’12

Location: Nordita Astrophysics Building (Auditorium # 122:026), Campus of AlbaNova,Roslagstullsbacken 17, Stockholm (for members only)

Sunday, October 14, 2012, 9:00-12:30: FP7 project AstRoMap Kick-off meeting

Sunday, October 14, 2012, 13:30-18:30: EANA Executive Council meeting

Location: AlbaNova Building (Auditorium # FA31), Roslagstullsbacken 21, Stockholm (for membersonly)

Monday, October 15, 2012, 12:30-14:00: EXPOSE-IWG meeting (Part 1)

Tuesday, October 16, 2012, 12:30-14:00: EXPOSE-IWG meeting (Part 2)

233

 

12TH EUROPEAN WORKSHOP ON ASTROBIOLOGY (EANA 2012)15—17 October 2012

193 REGISTERED PARTICIPANTS

  kiran adhikari jamuna‐keith astronomy research centre 

kathmandu, Nepal

sunlightforce@gmail.com 

    13—20 October 2012

  Engy Ahmed Stockholm University 

Stockholm, Sweden

engy.ahmed@geo.su.se 

    15—17 October 2012

  abdalla almohammad balqaa applied university 

huson‐jordan, Jordan

aseel_00@yahoo.com 

    14—19 October 2012

  Dilek Altutaş Ege University 

IZMIR, Turkey

dilekaltuntas87@gmail.com 

    13—20 October 2012

  Ricardo Amils Centro de Astrobiología 

Torrejón de Ardoz, Spain

ramils@cbm.uam.es 

    14—18 October 2012

  Jan Marie Andersen Boston University 

Boston, United States of America

janmarie@bu.edu 

    14—20 October 2012

  Eamonn Ansbro Kingsland Observatory 

Boyle County Roscommon, Ireland

eansbro@eircom.net 

    13—19 October 2012

  Khawaja Nozair Ashraf Tuorla Observatory, University of Turku, 

Finland 

Turku, Finland

khaash@utu.fi 

    14—17 October 2012

  Armando Azua‐Bustos Universidad de los Andes 

Santiago, Chile

ajazua@uc.cl 

    13—20 October 2012

  Coryn Bailer‐Jones Max Planck Institute for Astronomy 

Heidelberg, Germany

calj@mpia.de 

    14—17 October 2012

  Ebbe Norskov Bak Aarhus University 

Aarhus, Denmark

ebbe.bak@biology.au.dk 

    14—17 October 2012

  Clarisse 

BALLAND‐BOLOU‐BI

Department of Geological Sciences 

Stockholm University 

Stockholm, Sweden

clarissebolou‐bi@geo.su.se 

    15—17 October 2012

  Mickael Baqué University of Rome Tor Vergata 

ROMA, Italy

mickael.baque@gmail.com 

    13—18 October 2012

  Laura Barge Caltech / Jet Propulsion Laboratory 

Pasadena, United States of America

laura.m.barge@jpl.nasa.gov 

    13—20 October 2012

  Marie‐Paule BASSEZ Université de Strasbourg 

Strasbourg, France

marie‐paule.bassez@unistra.fr 

    14—19 October 2012

NORDITAy

LIST OF PARTICIPANTS

  Bettina Bödeker University of Hohenheim 

Stuttgart, Germany

bettina.boedeker@gmx.de 

    14—18 October 2012

  Stefan Bengtson Swedish Museum of Natural History / PZ 

Stockholm, Sweden

stefan.bengtson@nrm.se 

    15—17 October 2012

  Marylène Bertrand CNRS, Centre de Biophysique Moléculaire 

ORLEANS, France

marylene.bertrand@cnrs‐orleans.fr 

    14—17 October 2012

  Daniela Billi University of Rome Tor Vergata 

Rome, Italy

billi@uniroma2.it 

    13—18 October 2012

  Nicolas bost Centre de Biophysique Moleculaire ‐ CNRS 

Orleans Cedex 2, France

nicolas.bost@cnrs‐orleans.fr 

    15—17 October 2012

  Alexis Brandeker Astronomy, Stockholm University 

Stockholm, Sweden

alexis.brandeker@astro.su.se 

    13—20 October 2012

  Axel Brandenburg Nordita 

Stockholm, Sweden

brandenb@nordita.org 

    15—17 October 2012

  Annette Brandt Institute of Botany I, AG Ott; Heinrich‐

Heine‐Universität Düsseldorf 

40225 Düsseldorf, Germany

annette.brandt@uni‐duesseldorf.de 

    14—17 October 2012

  David Bryant University of Leeds 

Leeds LS29JT, United Kingdom

d.bryant@leeds.ac.uk 

    14—17 October 2012

  Elena Bulat FSBI PNPI 

St Petersburg‐Gatchina, Russian 

Federation

vlasovaes@gmail.com 

    14—18 October 2012

  SERGEY Bulat PNPI 

St Petersburg‐Gatchina, Russian 

Federation

bulat@lgge.obs.ujf‐grenoble.fr 

    14—18 October 2012

  Simon Candelaresi Nordita 

Stockholm, Sweden

iomsn@physto.se 

    13—20 October 2012

  Gianni Cataldi Stockholm University 

Stockholm, Sweden

gianni.cataldi@astro.su.se 

    13—20 October 2012

  Barbara Cavalazzi Department of Geology, 

University of Johannesburg 

Johannesburg, South Africa

cavalazzib@uj.ac.za 

    14—18 October 2012

  Jean François Clervoy ESA 

Paris, France

jean‐francois.clervoy@esa.int 

    15—17 October 2012

  Charles Cockell Uk Centre for Astrobiology, 

University of Edinburgh 

Edinburgh, United Kingdom

c.s.cockell@ed.ac.uk 

    13—20 October 2012

  Fiorella Coliolo Freelance for ESA 

Paris, France

fcoliolo@exoworld.net 

    15—17 October 2012

  Herve COTTIN LISA/Universite Paris Est Creteil 

Creteil, France

herve.cottin@lisa.u‐pec.fr 

    14—17 October 2012

  Kristine Dannenberg Swedish National Space Board 

Solna, Sweden

dannenberg@snsb.se 

    15—17 October 2012

  MubarakAli 

Davoodbasha

Bharathidasan University 

Tiruchirappalli, India

mubinano@gmail.com 

    13—20 October 2012

  Rosa 

De la Torre Noetzel

INTA (Spanish Aerospace Research 

Establishment) 

28850‐MADRID, Spain

torrenr@inta.es 

    14—19 October 2012

  Jean‐Pierre de Vera German Aerospace Center (DLR) 

Berlin, Germany

jean‐pierre.devera@dlr.de 

    14—18 October 2012

  Fabio Del Sordo NORDITA 

Stockholm, Sweden

fabio@nordita.org 

    13—20 October 2012

  Alfonso Delgado‐Bonal Centro de Astrobiología 

Torrejón de Ardoz, Madrid, Spain

alfonso.delgado.bonal@gmail.com 

    14—18 October 2012

  Gulnur Dogan High Altitude Observatory 

Boulder, CO, United States of America

gulnur@ucar.edu 

    14—17 October 2012

  Pascale Ehrenfreund Space Policy Institute 

Washington, United States of America

pehren@gwu.edu 

    14—18 October 2012

  Yves ELLINGER UPMC 

Paris 75005, France

ellinger@lct.jussieu.fr 

    14—19 October 2012

  Andreas Elsaesser Leiden University 

Leiden, Netherlands

a.elsaesser@umail.leidenuniv.nl 

    14—18 October 2012

  Adriana Errico Facultad de Ciencias (UdelaR) 

Montevideo, Uruguay

aberrico@gmail.com 

    13—20 October 2012

  pantea fathi Stockholm university 

stockholm, Sweden

panteaf@kth.se 

    13—20 October 2012

  Karine Aparecida 

Felix Ribeiro

Pompeo Fabra University 

Barcelona, Spain

karinefelix_@hotmail.com 

    15—17 October 2012

  Franco Ferrari CASA* 

Szczecin, Poland

ferrari@fermi.fiz.univ.szczecin.pl 

    13—18 October 2012

  Kai Finster Biosciences‐ Microbiology Section 

Aarhus, Denmark

kai.finster@biology.au.dk 

    14—18 October 2012

  Frédéric Foucher Centre de Biophysique Moléculaire, CNRS 

Orléans, France

frederic.foucher@cnrs‐orleans.fr 

    15—17 October 2012

  Stefan Fox University of Hohenheim 

Stuttgart, Germany

stefan.fox@uni‐hohenheim.de 

    14—18 October 2012

  Fulvio Franchi Dipartimento di Scienze Della Terra e 

Geologico Ambientali, Università di 

Bologna 

Bologna, Italy

fulvio.franchi2@unibo.it 

    13—20 October 2012

  Kateryna Frantseva Taras Shevchenko National 

University of Kyiv 

Kyiv, Ukraine

gagarinfff@gmail.com 

    13—20 October 2012

  Jan Frösler University of Duisburg‐Essen 

Essen, Germany

jan.froesler@uni‐due.de 

    14—20 October 2012

  Felipe Gómez Centro de Astrobiología 

Torrejon de Ardoz, Madrid 28850, Spain

gomezgf@cab.inta‐csic.es 

    14—18 October 2012

  Wolf Geppert Stockholm University 

Stockholm, Sweden

wgeppert@fysik.su.se 

    13—20 October 2012

  Mikhail Gerasimov Space Research Institute of the RAS (IKI) 

Moscow, Russian Federation

mgerasim@mx.iki.rssi.ru 

    13—19 October 2012

  Damhnait Gleeson Centro de Astrobiologia 

Madrid, Spain

dgleeson@cab.inta‐csic.es 

    14—18 October 2012

  Natalia Gontareva Institute of cytology Russian 

academy of sciences 

St Petersburg, Russian Federation

ngontar@mail.cytspb.rssi.ru 

    14—17 October 2012

  Veronika Grosz Budapest University of Technology and 

Economics 

Budapest, Hungary

veronika.grosz@gmail.com 

    14—18 October 2012

  Arnold Gucsik Max Planck Institute for Chemistry 

Mainz, Germany

a.gucsik@mpic.de 

    14—18 October 2012

  Jean‐Claude Guillemin CNRS 

35708 Rennes Cedex 7, France

jean‐claude.guillemin@ensc‐rennes.fr 

    14—18 October 2012

  Oleg Gusev NIAS 

Tsukuba, Japan

oleg@cryptobio.com 

    14—18 October 2012

  Jordi Gutiérrez Department of Applied Physics, 

Universitat Politècnica de Catalunya ‐ 

BarcelonaTech 

Castelldefels, Spain

jordi.gutierrez@upc.edu 

    14—17 October 2012

  Mitra Hajigholi Department of Earth & Space Sciences 

Onsala, Sweden

mitra.hajigholi@chalmers.se 

    14—18 October 2012

  Peter‐Diedrich Hansen TU Berlin, Department of Ecological 

Impact and Ecotoxicology 

Berlin, Germany

peter‐diedrich.hansen@tu‐berlin.de 

    14—17 October 2012

  Siddharth Hegde Max Planck Institute for Astronomy 

Heidelberg, Germany

hegde@mpia.de 

    13—18 October 2012

  Helge Hellevang University of Oslo 

Oslo, Norway

helghe@geo.uio.no 

    14—17 October 2012

  Georg Hildenbrand Kirchhoff‐Institute for Physics 

Heidelberg, Germany

hilden@kip.uni‐heidelberg.de 

    14—18 October 2012

  Beda Hofmann Natural History Museum Bern 

Bern, Switzerland

beda.hofmann@geo.unibe.ch 

    14—17 October 2012

  Nils Holm Stockholm University 

Stockholm, Sweden

nils.holm@geo.su.se 

    14—18 October 2012

  Mats Holmström Swedish Institute of Space Physics 

Kiruna, Sweden

matsh@irf.se 

    14—17 October 2012

  Gerda Horneck German Aerospace Center DLR, 

Institute of Aerospace Medicine 

51170 Cologne, Germany

gerda.horneck@dlr.de 

    13—18 October 2012

  Axelle Hubert CNRS‐Centre de Biophysique Moléculaire 

ORLEANS, France

axelle.hubert@cnrs‐orleans.fr 

    13—20 October 2012

  José Enrique 

Iñiguez Pacheco

Stockholm University 

Stockholm, Sweden

enrique.iniguez@geo.su.se 

    13—20 October 2012

  Leopold Ilag Stockholm University 

Stockholm, Sweden

leopold.ilag@anchem.su.se 

    13—18 October 2012

  Fadil Inceoglu Aarhus University 

Aarhus, Denmark

fadil@phys.au.dk 

    14—18 October 2012

  Magnus Ivarsson Swedish Museum of Natural History, 

Department of Palaeozoology 

Stockholm, Sweden

magnus.ivarsson@nrm.se 

    13—20 October 2012

  Seema Jagota NASA Ames Research Center 

Mountain View, United States of 

America

seema.ames@gmail.com 

    13—19 October 2012

  Ingemar Jönsson Department of genetics, Microbiology & 

Toxicology, Stockholm University 

Stockholm, Sweden

ingemar.jonsson@hkr.se 

    16—17 October 2012

  Jaqueline Kløvgaard 

Jensen

University of Copenhagen, NBI 

2100 Copenhagen Ø, Denmark

jaqueline@kloevgaard.dk 

    14—17 October 2012

  Sohan jheeta The Open University 

Milton Keynes, United Kingdom

sohan7@ntlworld.com 

    14—17 October 2012

  Elena Kadyshevich Obukhov Institute of Atmospheric 

Physics, RAS 

Moscow, Russian Federation

kadyshevich@mail.ru 

    13—20 October 2012

  Orcun KALKAN Ege University 

IZMIR, Turkey

orcunkalkan@yahoo.com 

    13—20 October 2012

  Hiroshi Kanamaru Fukuoka Institute of Technology 

Fukuoka, Japan

solevient@yahoo.co.jp 

    13—18 October 2012

  Yuko Kawaguchi Tokyo University of Pharmacy and Life 

Sciences 

Tokyo, Japan

s08756@toyaku.ac.jp 

    13—18 October 2012

  Jun Kawai Yokohama National University 

Yokohama, Japan

j_kawai0908@hotmail.com 

    14—18 October 2012

  Yukinori Kawamoto Yokohama National University 

Yokohama, Japan

kawamoto‐yukinori‐tf@ynu.ac.jp 

    14—19 October 2012

  Terence Kee University of Leeds 

Leeds, United Kingdom

t.p.kee@leeds.ac.uk 

    14—17 October 2012

  Yeghis Keheyan CNR 

Rome, Italy

yeghis.keheyan@uniroma1.it 

    13—19 October 2012

  adil hakeem khan Govt.Kasturba College Jiwaji University 

Gwalior Guna M.P.India 

Guna M.P., India

adilenviro@rediffmail.com 

    13—20 October 2012

  Ramon Khanna Springer 

Heidelberg, Germany

ramon.khanna@springer.com 

    14—17 October 2012

  K. G. Kislyakova Space Research Institute, Austrian 

Academy of Sciences 

Graz, Austria

kislyakova@xx.yy 

    14—18 October 2012

  Kensei Kobayashi Yokohama National University 

Yokohama, Japan

kkensei@ynu.ac.jp 

    14—19 October 2012

  Asmus Koefoed Niels Bohr Institute 

Copenhagen, Denmark

asmus.koefoed@nbi.ku.dk 

    14—18 October 2012

  Vladimir 

Kompanichenko

Institute for Complex Analysis, FEB of the 

Russian Academy of Science 

Birobidzhan 679016, Russian Federation

kompanv@yandex.ru 

    14—18 October 2012

  Ricardo Konrad Universidad de Chile 

Santiago, Chile

r.a.konrad@gmail.com 

    14—18 October 2012

  Kirill Krivushin Institute of Physicochemical and Biological 

Problems in Soil Science 

Pushchino, Russian Federation

krivushin@bk.ru 

    13—19 October 2012

  Leonid Ksanfomality Space research institute of RAS 

Moscow 117997, Russian Federation

leksanf@gmail.com;ksanf@rssi.ru 

    14—20 October 2012

  Jana Kviderova Faculty of Science, University of South 

Bohemia 

Ceske Budejovice, Czech Republic

kviderova@butbn.cas.cz 

    14—18 October 2012

  Pauli Laine University of Turku 

Turku, Finland

paerla@utu.fi 

    14—16 October 2012

  Jean‐François Lambert LRS ‐ UPMC 

Ivry‐sur‐Seine 94200, France

jean‐francois.lambert@upmc.fr 

    14—17 October 2012

  Helmut Lammer Space Research Institute, Austrian 

Academy of Sciences 

Graz, Austria

helmut.lammer@gmail.com 

    14—18 October 2012

  Natuschka M. Lee Department of Microbiology 

Freising/Munich, Germany

nlee@microbial‐systems‐ecology.de 

    14—18 October 2012

  Alexandra Lefort University of Tennessee 

Knoxville, United States of America

alefort@utk.edu 

    14—20 October 2012

  Kirsi Lehto University of Turku 

Turku, Finland

klehto@utu.fi 

    14—17 October 2012

  Franz Leißing University of Hohenheim 

Stuttgart, Germany

franz.leissing@uni‐hohenheim.de 

    14—18 October 2012

  Paula Lindgren University of Glasgow 

Glasgow, United Kingdom

paula.lindgren@glasgow.ac.uk 

    15—17 October 2012

  Dag Linnarsson Karolinska Institutet, Dept of Physiology 

and Pharmacology 

SE 17177 Stockholm, Sweden

dag.linnarsson@ki.se 

    15—17 October 2012

  Rene Liseau Chalmers University of Technology 

Onsala, Sweden

rene.liseau@chalmers.se 

    15—18 October 2012

  Stefanie Lutz University of Leeds 

Leeds, United Kingdom

s.lutz@leeds.ac.uk 

    14—18 October 2012

  Guruprasad M.R Indian Institute of Science 

Bangalore, India

mrpguru@gmail.com 

    13—20 October 2012

  Claudio Maccone International Academy of Astronautics 

Torino (Turin), Italy

clmaccon@libero.it 

    13—18 October 2012

  Rocco Mancinelli BAER Institute 

Moffett Field, CA, United States of 

America

rocco.l.mancinelli@nasa.gov 

    14—19 October 2012

  Bill Martin Institut of Molecular Evolution, 

University of Düsseldorf 

Düsseldorf, Germany

bill@hhu.de 

    15—17 October 2012

  F. Javier Martin‐Torres Centro de Astrobiología (CISC‐INTA) 

Torrejón de Ardoz, Madrid, Spain

javier.martin.torres@gmail.com 

    14—17 October 2012

  Zita Martins Imperial College London 

London, United Kingdom

z.martins@imperial.ac.uk 

    13—18 October 2012

  Sean McMahon University of Aberdeen 

Aberdeen, United Kingdom

sean.mcmahon@abdn.ac.uk 

    14—18 October 2012

  Joachim Meeßen Insitute of Botany, Heinrich‐Heine‐

University 

Duesseldorf, Germany

joachimmeessen@gmx.de 

    14—18 October 2012

  Joachim Meeßen Insitute of Botany, Heinrich‐Heine‐

University 

Duesseldorf, Germany

otts@uni‐duesseldorf.de 

    14—18 October 2012

  Yamila Miguel Max Planck Institut fur Astronomie 

Heidelberg, Germany

miguel@mpia‐hd.mpg.de 

    14—18 October 2012

  Dhrubaditya Mitra NORDITA 

Stockholm, Sweden

dhruba@nordita.org 

    13—20 October 2012

  Ralf Moeller German Aerospace Center 

Cologne, Germany

ralf.moeller@dlr.de 

    14—18 October 2012

  Euan Monaghan The Open University 

Milton Keynes, United Kingdom

e.p.monaghan@open.ac.uk 

    14—20 October 2012

  Christian Muller B.USOC 

Brussels, Belgium

christian.muller@busoc.be 

    14—18 October 2012

  Gayathri Murukesan University of Turku 

Turku‐ 20380, Finland

gamuru@utu.fi 

    15—17 October 2012

  Rodrigo Nascimento Centro Federal de Educação Tecnológica 

Celso Suckow da Fonseca ‐ CEFET/RJ 

Rio de Janeiro, Brazil

rodfer@if.ufrj.br 

    13—19 October 2012

  anna neubeck department of geological sciences, 

stockholm university 

stockholm, Sweden

anna.neubeck@geo.su.se 

    13—20 October 2012

  Lauri Nikkanen University of Turku 

Raisio, Finland

lenikk@utu.fi 

    14—17 October 2012

  Lennart Nordh Retired from Swedish National Space 

Board 

Solna, Sweden

lennart.nordh1@comhem.se 

    15—17 October 2012

  Lisa Nortmann Institut für Astrophysik Göttingen 

37077 Göttingen, Germany

nortmann@astro.physik.uni‐goettingen.de 

    14—18 October 2012

  Alexey Novoselov Institute of Geosciences, 

University of Campinas (UNICAMP) 

Campinas, Brazil

alexey@ige.unicamp.br 

    14—20 October 2012

  Karen Olsson‐Francis Open University 

Milton Keynes, United Kingdom

k.olsson‐francis@open.ac.uk 

    14—17 October 2012

  Victor Ostrovskii Karpov Institute of Physical Chemistry 

Moscow, Russian Federation

vostrov@cc.nifhi.ac.ru 

    13—20 October 2012

  Jack O\'Malley‐James University of St Andrews 

St Andrews, United Kingdom

jto5@st‐andrews.ac.uk 

    14—18 October 2012

  Corinna Panitz RWTH/Klinikum Aachen, 

Institute of Aerospace medicine 

Aachen, Germany

cpanitz@ukaachen.de,corinna.panitz@dlr.de 

    13—17 October 2012

  Chazalnoël Pascale CNES 

Toulouse, France

pascale.chazalnoel@cnes.fr 

    14—17 October 2012

  Manish Patel The Open University 

Milton Keynes, United Kingdom

m.r.patel@open.ac.uk 

    14—18 October 2012

  Francoise PAUZAT CNRS 

Paris 75005, France

pauzat@lct.jussieu.fr 

    14—19 October 2012

  Anatoliy Pavlov Ioffe Physical‐Technical 

Institute of Rassian Academy of Sciences 

Saint Petersburg, Russian Federation

anatoli.pavlov@mail.ioffe.ru 

    14—18 October 2012

  Eduardo Penteado Radboud University Nijmegen, Institute 

for Molecules and Materials 

Nijmegen, Netherlands

e.monfardini@science.ru.nl 

    14—18 October 2012

  Cleber Pereira Calça Instituto de Geociências, Universidade de 

São Paulo 

São Paulo, Brazil

atabike@yahoo.com.br 

    13—20 October 2012

  Juan Perez Mercader Harvard University 

Cambridge, MA 02142, United States of 

America

colby@fas.harvard.edu 

    13—16 October 2012

  Lada Petrovskaya Shemyakin–Ovchinnikov 

Institute of Bioorganic Chemistry RAS 

Moscow, Russian Federation

lpetr65@yahoo.com 

    13—19 October 2012

  Jorge Pla‐Garcia Center for Astrobiology 

Torrejon de Ardoz, Spain

jpla@cab.inta‐csic.es 

    14—17 October 2012

  Eva Plávalová Comenius University in Bratislava 

Bratislava 842 48, Slovakia

plavalova@komplet.sk 

    14—18 October 2012

  Anthony Poole University of Canterbury 

Christchurch, New Zealand

anthony.poole@canterbury.ac.nz 

    14—18 October 2012

  Oleksandr Potashko Department of Marine Geology and 

Sedimentary Ore Formation NASU 

Irpin, Kiev region, Ukraine

tumburland@gmail.com 

    13—19 October 2012

  Istvan Praet University of Roehampton 

London, United Kingdom

istvan.praet@roehampton.ac.uk 

    14—17 October 2012

  Ralph Pudritz Origins Institute ‐ McMaster University 

Hamilton, Canada

pudritz@mcmaster.ca 

    13—18 October 2012

  Lisa 

Quasthoff Holmström

Rymdgymnasiet 

Kiruna, Sweden

lisa@lisatext.se 

    14—18 October 2012

  Elke Rabbow DLR Institut of Aerospace Medicine, 

Radiation Biology 

51147 Koeln, Germany

elke.rabbow@dlr.de 

    14—18 October 2012

  Steen Rasmussen Fundamental Living Technology 

Odense 5000, Denmark

steen@sdu.dk 

    15—18 October 2012

  Francois RAULIN LISA 

Créteil, France

francois.raulin@lisa.u‐pec.fr 

    14—18 October 2012

  Samuel Regandell Uppsala Universitet 

Uppsala, Sweden

samreg@astro.uu.se 

    15—17 October 2012

  Yuping Ren Shandong University 

Beijing, China

lanyuanweizi@126.com 

    13—20 October 2012

  Petra Rettberg DLR, Institute of Aerospace Medicine 

51147 Koeln, Germany

petra.rettberg@dlr.de 

    13—19 October 2012

  Elizaveta Rivkina Institute of Physicochemical and Biological 

Problems in Soil Science Russian 

Academy of Sciences 

Pushchino, Russian Federation

elizaveta.rivkina@gmail.com 

    13—19 October 2012

  Lynn Rothschild NASA Ames Research Center 

Moffett Field, CA, United States of 

America

lynn.j.rothschild@nasa.gov 

    15—20 October 2012

  Kafila Saiagh LISA 

Créteil, France

kafila.saiagh@lisa.u‐pec.fr 

    14—18 October 2012

  Tina Santl Temkiv Stellar Astrophysics Centre, Aarhus 

University 

Aarhus, Denmark

tina.santl@gmail.com 

    13—18 October 2012

  Mikael Schelin Department of Physics, Lund University 

Lund, Sweden

hej@mikaelschelin.com 

    15—17 October 2012

  Andrew C. Schuerger University of Florida 

Kennedy Space Center, United States of 

America

schuerg@ufl.edu 

    13—18 October 2012

  Alan Schwartz Radboud University Nijmegen 

Nijmegen, Netherlands

alan@science.ru.nl 

    13—17 October 2012

  Petra Schwendner German Aerospace Center 

Cologne, Germany

petra.schwendner@dlr.de 

    15—17 October 2012

  Paloma Serrano GFZ‐German Research Centre for 

Geosciences 

Potsdam, Germany

paloma.serrano@gfz‐potsdam.de 

    14—17 October 2012

  Tejman Shrestha Pathivara Darshan Baikalpic Energy & 

Electronics Suppliers 

Itahari, Nepal

pdbu.electronic@gmail.com 

    14—18 October 2012

  Michael Simakov Institute of Cytology, RAS 

194064, Russian Federation

exobio@mail.cytspb.rssi.ru 

    14—18 October 2012

  Eugenio Simoncini CAB ‐ INTA‐CSIC 

Madrid, Spain

eugenio.simoncini@gmail.com 

    13—20 October 2012

  Helga stan‐lotter University of Salzburg 

Salzburg, Austria

helga.stan‐lotter@sbg.ac.at 

    14—19 October 2012

  Henry Strasdeit University of Hohenheim 

Stuttgart, Germany

henry.strasdeit@uni‐hohenheim.de 

    14—18 October 2012

  Maria Sundin Institute of Physics, Gothenburg 

Gothenburg, Sweden

maria.sundin@physics.gu.se 

    15—17 October 2012

  Ewa Szuszkiewicz CASA* and Institute of Physics, 

University of Szczecin 

70‐451 Szczecin, Poland

szusz@fermi.fiz.univ.szczecin.pl 

    13—18 October 2012

  Oxana Taran Boreskov Institute of Catalysis 

Novosibirsk, Russian Federation

oxanap@catalysis.ru 

    14—18 October 2012

  Arkadii Tarasevych Institute of Bioorganic Chemistry and 

Petrochemistry, National 

Academy of Sciences of Ukraine 

Kyiv, Ukraine

arkadiitarasevych@gmail.com 

    14—18 October 2012

  agha timothy lagos state university 

lagos, Nigeria

jfatai@yahoo.com 

    14—18 October 2012

  MADHAN TIRUMALAI UNIVERSITY OF HOUSTON 

HOUSTON, United States of America

mrtirum2@mail.uh.edu 

    13—20 October 2012

  Søren Toxvaerd DNRF center , Dept. of Science, Roskilde 

University 

Roskilde, Denmark

st@ruc.dk 

    14—17 October 2012

  Vivi Vajda Department of Geology/Pufendorf 

institute 

Lund, Sweden

vivi.vajda@geol.lu.se 

    15—17 October 2012

  Aris Vasileiadis Niels Bohr Institute, KU; STARPLAN 

Centre, National History 

Museum of Denmark, KU 

Copenhagen, Denmark

aris@nbi.dk 

    14—20 October 2012

  Mariya Vdovina Ioffe Physical‐Technical Institute 

St. Petersburg, Russian Federation

mariya.vdovina@gmail.com 

    14—17 October 2012

  Vassilissa Vinogradoff University aix marseille 

Marseille, France

vass_vino@yahoo.fr 

    14—18 October 2012

  Michel VISO CNES 

75001 Paris, France

michel.viso@cnes.fr 

    14—18 October 2012

  Petr Vitek Charles University in Prague 

Prague, Czech Republic

petr.vitek@natur.cuni.cz 

    14—18 October 2012

  Nicolas Walter European Science Foundation 

Strasbourg, France

nwalter@esf.org 

    13—20 October 2012

  Joern Warnecke Nordita 

Stockholm, Sweden

joern@nordita.org 

    13—20 October 2012

  Marko Wassmann DLR ‐ German Aerospace Center 

51147 Cologne, Germany

marko.wassmann@dlr.de 

    14—17 October 2012

  Frances Westall CNRS‐Centre de Biophysique Moleculaire 

45071 Orleans, France

frances.westall@cnrs‐orleans.fr 

    15—18 October 2012

  John Wettlaufer Yale University & NORDITA 

New Haven, USA & Stockholm, Sweden, 

Sweden

john.wettlaufer@yale.edu 

    15—17 October 2012

  Joachim Wiegert Chalmers university of technology, 

Department of Earth and space sciences, 

Onsala space observatory 

Göteborg, Sweden

wiegert@chalmers.se 

    14—18 October 2012

  Katherine Wright University of Colorado at Boulder 

Boulder, United States of America

wrightk@colorado.edu 

    14—17 October 2012

  fagbenro yakub university of ibadan 

lagos, Nigeria

fagbenroyakub2009@yahoo.com 

    14—18 October 2012

  Masatoshi Yamauchi Swedish Institute of Space Physics 

Kiruna, Sweden

m.yamauchi@irf.se 

    14—17 October 2012

  Shin‐ichi Yokobori Tokyo University of Pharmacy and Life 

Sciences 

Tokyo, Japan

yokobori@ls.toyaku.ac.jp 

    14—18 October 2012

SOC Members: • Ricardo Amils • Andre Brack • Axel Brandenburg • John Brucato • Charles Cockell • Pascale Ehrenfreund • Natalia Gontareva • Lee Grenfell • Nils Holm • Gerda Horneck • Helmut Lammer • Kirsi Lehto • Steen Rasmussen • François Raulin • Petra Rettberg • Ewa Szuszkiewicz • Frances Westall

Main Topics: • Extrasolar planets • Astrophysics and astrochemistry • Geochemical origin of life • Origin and evolution of the biosphere • Planetary habitability & exploration (Mars, Titan, Europa, ...) • Extremophiles and early life • Astrobiology on the International Space Station • Artificial life • Miscellaneous subjects in astrobiology

http://www.astrobiologia.pl/eana/

15 – 17 October 2012, AlbaNova University Center, Stockholm(EANA 2012)

12th European Workshop on Astrobiology