Exobiology in the Solar System & the Search for Life on Mars

Total Page:16

File Type:pdf, Size:1020Kb

Exobiology in the Solar System & the Search for Life on Mars SP-1231 SP-1231 October 1999 Exobiology in the Solar System & The Search for Life on Mars for The Search Exobiology in the Solar System & Exobiology in the Solar System & The Search for Life on Mars Report from the ESA Exobiology Team Study 1997-1998 Contact: ESA Publications Division c/o ESTEC, PO Box 299, 2200 AG Noordwijk, The Netherlands Tel. (31) 71 565 3400 - Fax (31) 71 565 5433 SP-1231 October 1999 EXOBIOLOGY IN THE SOLAR SYSTEM AND THE SEARCH FOR LIFE ON MARS Report from the ESA Exobiology Team Study 1997-1998 Cover Fossil coccoid bacteria, 1 µm in diameter, found in sediment 3.3-3.5 Gyr old from the Early Archean of South Africa. See pages 160-161. Background: a portion of the meandering canyons of the Nanedi Valles system viewed by Mars Global Surveyor. The valley is about 2.5 km wide; the scene covers 9.8 km by 27.9 km centred on 5.1°N/48.26°W. The valley floor at top right exhibits a 200 m-wide channel covered by dunes and debris. This channel suggests that the valley might have been carved by water flowing through the system over a long period, in a manner similar to rivers on Earth. (Malin Space Science Systems/NASA) SP-1231 ‘Exobiology in the Solar System and The Search for Life on Mars’, ISBN 92-9092-520-5 Scientific Coordinators: André Brack, Brian Fitton and François Raulin Edited by: Andrew Wilson ESA Publications Division Published by: ESA Publications Division ESTEC, Noordwijk, The Netherlands Price: 70 Dutch Guilders/ EUR32 Copyright: © 1999 European Space Agency Contents Foreword 7 I An Exobiological View of the Solar System 15 I.1 Introduction 17 I.2 Chemical Evolution in the Solar System 19 2.1 Terrestrial Prebiotic Chemistry 19 2.1.1 Terrestrial Production of Reduced Organic Molecules 19 2.1.2 Extraterrestrial Delivery of Organic Molecules to the Earth 20 2.2 Chemical Evolution on Other Bodies of the Solar System 21 2.2.1 The Icy Bodies: Comets, Europa, Ganymede 21 2.2.2 The Non-Icy Bodies: Titan, Giant Planets, Venus, 22 Moon, Mars I.3 Limits of Life under Extreme Conditions 27 3.1 Introduction 27 3.2 Extreme Temperature Regimes 27 3.2.1 High Temperatures 27 3.2.2 Low Temperatures 29 3.3 High-Salt Environments 30 3.4 Acidic and Alkaline Environments 31 3.5 High-Pressure Environments 31 3.6 Subterranean Life 32 3.7 Survival of Lifeforms in Space 34 3.8 Implications for Exobiology in Future Searches 36 I.4 Morphological and Biochemical Signatures of Extraterrestrial Life: 41 Utility of Terrestrial Analogues 4.1 Introduction 41 4.2 Evidence of Extant Life 41 4.2.1 The Microbial World 41 4.2.2 Structural Indications of Life 42 4.2.3 Evidence of Microbial Activity as a Functional 44 Characteristic of Life 4.2.4 Chemical Signatures and Biomarkers 47 4.2.5 Indirect Fingerprints of Life 48 4.2.6 Conclusions 48 4.3 Evidence of Extinct (Fossil) Extraterrestrial Life 49 4.3.1 Paleontological Evidence 49 4.3.1.1 Microbialites 51 4.3.1.2 Cellular Microfossils 51 4.3.2 Biogeochemical Evidence 53 4.3.2.1 Sedimentary Organic Carbon as a Recorder 54 of Former Life Processes 4.3.2.2 13C/12C in Sedimentary Organic Matter: 54 Index of Autotrophic Carbon Fixation 4.3.2.3 Molecular Biomarkers (‘Chemical Fossils’) 57 in Sediments 3 I.5 Potential Non-Martian Sites for Extraterrestrial Life 65 5.1 The Icy Satellites 65 5.1.1 Europa 65 5.1.2 Ganymede 66 5.1.3 Other Icy Satellites 67 5.2 Titan 67 5.2.1 The Titan Atmosphere 67 5.2.2 The Titan Surface 69 5.2.3 The Cassini/Huygens Mission 71 I.6 Science and Experiment Strategy 73 6.1 Where to Search? 73 6.2 What to Search For? 75 6.3 What to Search With? 76 I.7 Summary of the Science Team Recommendations 77 7.1 The Search for Extant and Extinct Life 77 7.2 The Study of the Precursors of Life 77 7.3 Organic Chemistry Processes and Microorganisms in Space 78 7.4 Laboratory-based Studies 78 II The Search for Life on Mars 79 II.1 Introduction 81 II.2 The Planet Mars 83 2.1 The Geology of Mars 83 2.2 Volcanism and Tectonism 84 2.3 The Bulk Chemical Composition of Mars 85 2.4 The Geochemistry of the Martian Surface Layers 87 2.5 Water and Ground Ice 88 2.6 The Climate of Mars 89 2.7 NASA-Proposed Sites for Mars Exploration 90 2.7.1 Water and a Favourable Environment 91 2.7.2 Explorations for Extinct Life 92 2.7.3 Exploration for Extant Life 92 2.7.4 NASA Priority Landing Sites for Exobiology 93 II.3 The Martian Meteorites 95 3.1 Introduction 95 3.2 The Origin of SNC Meteorites 96 3.3 The Martian Meteorites 97 3.4 Exobiology and the Martian Meteorites 98 3.5 Carbon Compounds in Other Meteorites (Carbonaceous Chondrites) 101 3.6 Carbon Compounds in Micrometeorites 103 II.4 Team I: Exobiology and the Mars Surface Environment 109 4.1 Environments and Rocks with Exobiology Potential 109 4.1.1 Lacustrine Environments 109 4.1.2 Sebkha Environments 110 4.1.3 Thermal-Spring Deposits 113 4.1.4 Duricrusts 113 4.1.5 Glacial Deposits 113 4 4.1.6 Polar Deposits 114 4.1.7 Ground Ice-Permafrost 114 4.2 General Remarks on Subsurface Microbial Fossils 115 4.3 Climatic and Environmental Models 115 4.4 The Radiation Environment 117 4.4.1 The Current Atmospheric Radiation Budget 118 4.4.2 The Current Particle and Radiation Environment 119 4.4.3 The Radiation Environment in the Past 119 4.5 The Rationale for Landing Site Selection 120 4.6 Rovers and Drilling Operations 122 4.7 Landing Sites 122 II.5 Team II: The Search for Chemical Indicators of Life 129 Scientific Objectives: 5.1 Sample Acquisition and Distribution Subsystem 129 5.2 Mineralogy, Petrology and Geochemistry 130 5.2.1 Mineralogy and Petrology 130 5.2.2 Geochemistry (Elemental Composition Analysis) 132 5.3 Isotopic Analysis 132 5.3.1 Carbon and Hydrogen 132 5.3.2 Sulphur 133 5.4 Molecular Analysis 133 5.4.1 Inorganics 133 5.4.2 Organics 133 5.5 The Search for Homochirality 135 Instrumentation to Satisfy the Scientific Objectives: 5.6 Sample Acquisition and Distribution Subsystem 135 5.7 Mineralogy, Petrology and Geochemistry 135 5.7.1 General Considerations 135 5.7.2 Optical Microscopy 138 5.7.3 Alpha-Proton-X-ray Spectrometer (APX) 138 5.7.4 Mössbauer Spectrometer 140 5.7.5 Ion/Electron Probes, X-ray Spectroscopy 142 5.7.6 IR Spectroscopy 142 5.7.7 Raman Spectroscopy 144 5.8 Isotopic Analysis 145 5.9 Molecular Analysis 147 5.9.1 Gas Chromatography (GC) 147 5.9.2 Mass Spectroscopy (MS) 148 5.9.3 Pyrolysis (PYR) 148 5.9.4 Available PYR-GC-MS Techniques 148 5.9.5 Laser Ablation-Inductive Coupled Plasma-MS (LA-ICP-MS) 149 5.9.6 Other Techniques 150 5.9.7 The Analysis of H2O2 150 5.10 Chirality Measurements 151 5.10.1 Bulk Chirality Measurements 151 5.10.2 Enantiomeric Separations 152 Recommended Payload and Technology Research Programme: 153 II.6 Team III: The Inspection of Subsurface Aliquots and Surface Rocks 157 Scientific Justification: 6.1 The Investigation of Unweathered Rock Material 157 5 6.2 Imaging of Fossilised Material in Sediments 157 6.2.1 Macroscopic Scale 158 6.2.2 Microscopic Scale 160 6.3 Investigation of Biominerals 161 6.4 Investigation of the Rock Structure 163 6.4.1 Extinct Microbes in Rock 163 6.4.2 Rock Formation and Composition 164 6.5 Investigation of Sedimentary Layering 165 6.6 Investigation of the Soil 165 6.7 Investigation of Dust Particles 166 Scientific Method and Requirements: 6.8 Initial Survey and Target Selection 167 6.9 High-Resolution Studies 168 6.10 Subsurface Investigations 170 6.11 Raman Spectrometry 170 6.12 Optical Spectroscopy 170 6.13 Mössbauer Spectroscopy 171 6.14 IR Spectroscopy 171 6.15 Thermal-IR Spectroscopy 171 6.16 Chemical Inspection of Subsurface Material 172 6.17 Summary of Possible Instrumentation 173 Sampling Aspects: 6.18 Mobility Requirements 173 6.19 Grinding/Polishing/Immersion 174 6.20 Drilling and Digging 174 6.21 Sieving and Magnetic Separation 174 6.22 Cutting and Sawing 174 6.23 Data Analysis 175 6.24 Summary of Major Conclusions 175 II.7 Conclusions 179 7.1 Landing Sites for Exobiology 179 7.2 The Sample Acquisition, Distribution and Preparation System 180 7.2.1 Subsurface Sample: Acquisition and Preparation 180 7.2.2 Surface Rock Sample: Acquisition and Preparation 180 7.2.3 Soil Samples 181 7.3 The Exobiology Observation System 181 7.4 The Exobiology Analysis System 181 7.5 A Possible Exobiology Experiment Package 184 and Operating Arrangement Annex 1: Team IV. A Manned Mars Station and Exobiology Research 185 6 FOREWORD The Exobiology Science Team was established in September 1996 by Dr. P. Clancy of ESA’s Directorate of Manned Spaceflight and Microgravity. The task of the Team was to survey current research in exobiology and related fields and then to make recommendations to ESA on the nature of a future search for life elsewhere in the Solar System.
Recommended publications
  • SPACE RESEARCH in POLAND Report to COMMITTEE
    SPACE RESEARCH IN POLAND Report to COMMITTEE ON SPACE RESEARCH (COSPAR) 2020 Space Research Centre Polish Academy of Sciences and The Committee on Space and Satellite Research PAS Report to COMMITTEE ON SPACE RESEARCH (COSPAR) ISBN 978-83-89439-04-8 First edition © Copyright by Space Research Centre Polish Academy of Sciences and The Committee on Space and Satellite Research PAS Warsaw, 2020 Editor: Iwona Stanisławska, Aneta Popowska Report to COSPAR 2020 1 SATELLITE GEODESY Space Research in Poland 3 1. SATELLITE GEODESY Compiled by Mariusz Figurski, Grzegorz Nykiel, Paweł Wielgosz, and Anna Krypiak-Gregorczyk Introduction This part of the Polish National Report concerns research on Satellite Geodesy performed in Poland from 2018 to 2020. The activity of the Polish institutions in the field of satellite geodesy and navigation are focused on the several main fields: • global and regional GPS and SLR measurements in the frame of International GNSS Service (IGS), International Laser Ranging Service (ILRS), International Earth Rotation and Reference Systems Service (IERS), European Reference Frame Permanent Network (EPN), • Polish geodetic permanent network – ASG-EUPOS, • modeling of ionosphere and troposphere, • practical utilization of satellite methods in local geodetic applications, • geodynamic study, • metrological control of Global Navigation Satellite System (GNSS) equipment, • use of gravimetric satellite missions, • application of GNSS in overland, maritime and air navigation, • multi-GNSS application in geodetic studies. Report
    [Show full text]
  • Evidence for Volcanism in and Near the Chaotic Terrains East of Valles Marineris, Mars
    43rd Lunar and Planetary Science Conference (2012) 1057.pdf EVIDENCE FOR VOLCANISM IN AND NEAR THE CHAOTIC TERRAINS EAST OF VALLES MARINERIS, MARS. Tanya N. Harrison, Malin Space Science Systems ([email protected]; P.O. Box 910148, San Diego, CA 92191). Introduction: Martian chaotic terrain was first de- ple chaotic regions are visible in CTX images (Figs. scribed by [1] from Mariner 6 and 7 data as a “rough, 1,2). These fractures have widened since the formation irregular complex of short ridges, knobs, and irregular- of the flows. The flows overtop and/or bank up upon ly shaped troughs and depressions,” attributing this pre-existing topography such as crater ejecta blankets morphology to subsidence and suggesting volcanism (Fig. 2c). Flows are also observed originating from as a possible cause. McCauley et al. [2], who were the fractures within some craters in the vicinity of the cha- first to note the presence of large outflow channels that os regions. Potential lava flows are observed on a por- appeared to originate from the chaotic terrains in Mar- tion of the floor as Hydaspis Chaos, possibly associat- iner 9 data, proposed localized geothermal melting ed with fissures on the chaos floor. As in Hydraotes, followed by catastrophic release as the formation these flows bank up against blocks on the chaos floor, mechanism of chaotic terrain. Variants of this model implying that if the flows are volcanic in origin, the have subsequently been detailed by a number of au- volcanism occurred after the formation of Hydaspis thors [e.g. 3,4,5]. Meresse et al.
    [Show full text]
  • No. 40. the System of Lunar Craters, Quadrant Ii Alice P
    NO. 40. THE SYSTEM OF LUNAR CRATERS, QUADRANT II by D. W. G. ARTHUR, ALICE P. AGNIERAY, RUTH A. HORVATH ,tl l C.A. WOOD AND C. R. CHAPMAN \_9 (_ /_) March 14, 1964 ABSTRACT The designation, diameter, position, central-peak information, and state of completeness arc listed for each discernible crater in the second lunar quadrant with a diameter exceeding 3.5 km. The catalog contains more than 2,000 items and is illustrated by a map in 11 sections. his Communication is the second part of The However, since we also have suppressed many Greek System of Lunar Craters, which is a catalog in letters used by these authorities, there was need for four parts of all craters recognizable with reasonable some care in the incorporation of new letters to certainty on photographs and having diameters avoid confusion. Accordingly, the Greek letters greater than 3.5 kilometers. Thus it is a continua- added by us are always different from those that tion of Comm. LPL No. 30 of September 1963. The have been suppressed. Observers who wish may use format is the same except for some minor changes the omitted symbols of Blagg and Miiller without to improve clarity and legibility. The information in fear of ambiguity. the text of Comm. LPL No. 30 therefore applies to The photographic coverage of the second quad- this Communication also. rant is by no means uniform in quality, and certain Some of the minor changes mentioned above phases are not well represented. Thus for small cra- have been introduced because of the particular ters in certain longitudes there are no good determi- nature of the second lunar quadrant, most of which nations of the diameters, and our values are little is covered by the dark areas Mare Imbrium and better than rough estimates.
    [Show full text]
  • Glossary Glossary
    Glossary Glossary Albedo A measure of an object’s reflectivity. A pure white reflecting surface has an albedo of 1.0 (100%). A pitch-black, nonreflecting surface has an albedo of 0.0. The Moon is a fairly dark object with a combined albedo of 0.07 (reflecting 7% of the sunlight that falls upon it). The albedo range of the lunar maria is between 0.05 and 0.08. The brighter highlands have an albedo range from 0.09 to 0.15. Anorthosite Rocks rich in the mineral feldspar, making up much of the Moon’s bright highland regions. Aperture The diameter of a telescope’s objective lens or primary mirror. Apogee The point in the Moon’s orbit where it is furthest from the Earth. At apogee, the Moon can reach a maximum distance of 406,700 km from the Earth. Apollo The manned lunar program of the United States. Between July 1969 and December 1972, six Apollo missions landed on the Moon, allowing a total of 12 astronauts to explore its surface. Asteroid A minor planet. A large solid body of rock in orbit around the Sun. Banded crater A crater that displays dusky linear tracts on its inner walls and/or floor. 250 Basalt A dark, fine-grained volcanic rock, low in silicon, with a low viscosity. Basaltic material fills many of the Moon’s major basins, especially on the near side. Glossary Basin A very large circular impact structure (usually comprising multiple concentric rings) that usually displays some degree of flooding with lava. The largest and most conspicuous lava- flooded basins on the Moon are found on the near side, and most are filled to their outer edges with mare basalts.
    [Show full text]
  • Mawrth Vallis, Mars: a Fascinating Place for Future in Situ Exploration
    Mawrth Vallis, Mars: a fascinating place for future in situ exploration François Poulet1, Christoph Gross2, Briony Horgan3, Damien Loizeau1, Janice L. Bishop4, John Carter1, Csilla Orgel2 1Institut d’Astrophysique Spatiale, CNRS/Université Paris-Sud, 91405 Orsay Cedex, France 2Institute of Geological Sciences, Planetary Sciences and Remote Sensing Group, Freie Universität Berlin, Germany 3Purdue University, West Lafayette, USA. 4SETI Institute/NASA-ARC, Mountain View, CA, USA Corresponding author: François Poulet, IAS, Bâtiment 121, CNRS/Université Paris-Sud, 91405 Orsay Cedex, France; email: [email protected] Running title: Mawrth: a fascinating place for exploration 1 Abstract After the successful landing of the Mars Science Laboratory rover, both NASA and ESA initiated a selection process for potential landing sites for the Mars2020 and ExoMars missions, respectively. Two ellipses located in the Mawrth Vallis region were proposed and evaluated during a series of meetings (3 for Mars2020 mission and 5 for ExoMars). We describe here the regional context of the two proposed ellipses as well as the framework of the objectives of these two missions. Key science targets of the ellipses and their astrobiological interests are reported. This work confirms the proposed ellipses contain multiple past Martian wet environments of subaerial, subsurface and/or subaqueous character, in which to probe the past climate of Mars, build a broad picture of possible past habitable environments, evaluate their exobiological potentials and search for biosignatures in well-preserved rocks. A mission scenario covering several key investigations during the nominal mission of each rover is also presented, as well as descriptions of how the site fulfills the science requirements and expectations of in situ martian exploration.
    [Show full text]
  • Aqueous Minerals from Arsia Chasmata of Arsia Mons, Tharsis Region: Implications for Aqueous Alteration Processes on Mars
    45th Lunar and Planetary Science Conference (2014) 1826.pdf AQUEOUS MINERALS FROM ARSIA CHASMATA OF ARSIA MONS, THARSIS REGION: IMPLICATIONS FOR AQUEOUS ALTERATION PROCESSES ON MARS. N. Jain*, S. Bhattacharya, P. Chauhan, Space Applications Centre (ISRO), Ahmedabad, Gujarat, India ([email protected]/ Fax: +91-079- 26915825). Introduction: The Arsia Chasmata is a complex help of high resolution data such as MGS-MOC (Mars collapsed region located at the northeastern flank of Global Surveyor-Mars Orbiter Camera), Viking orbiter Arsia Mons (figure 1 A and B) within Tharsis region [3], fresh appearing lava flows [4], graben and glaciers of planet Mars and is the most important region for the on flanks of Arsia Mons [5], young lava flows [6] study of minerals like phyllosilicate and pyroxene. The small shields at floor of caldera [7]. reflectance data of MRO-CRISM (figure 1 C D) has Present study mainly focuses on the mineralogy of confirmed above mentioned minerals in the study area. Arsia Chasmata which interestingly contains The presence of these minerals at the Arsia Chasmata absorption features of aqueous altered minerals such as on Mars provides the evidence of its past watery serpentine (phyllosilicate). This mineral is also located environment and their processes of formation. In the in Nili Fossae region which is long, narrow depression present study the absorption features of serpentine present on Mars [8]. But in the present study (phyllosilicate) are obtained at 2.32 µm, 1.94 µm and occurrence of this mineral at high altitude region raise 2.51 µm. Previous studies on Mars show that the curiosity to know about their formation processes.
    [Show full text]
  • Dynamic Consolidated Bioprocessing for Innovative Lab-Scale Production of Bacterial Alkaline Phosphatase from Bacillus Paraliche
    www.nature.com/scientificreports OPEN Dynamic consolidated bioprocessing for innovative lab‑scale production of bacterial alkaline phosphatase from Bacillus paralicheniformis strain APSO Soad A. Abdelgalil1,2*, Nadia A. Soliman1, Gaber A. Abo‑Zaid1 & Yasser R. Abdel‑Fattah1 To meet the present and forecasted market demand, bacterial alkaline phosphatase (ALP) production must be increased through innovative and efcient production strategies. Using sugarcane molasses and biogenic apatite as low‑cost and easily available raw materials, this work demonstrates the scalability of ALP production from a newfound Bacillus paralicheniformis strain APSO isolated from a black liquor sample. Mathematical experimental designs including sequential Plackett– Burman followed by rotatable central composite designs were employed to select and optimize the concentrations of the statistically signifcant media components, which were determined to be molasses, (NH4)2NO3, and KCl. Batch cultivation in a 7‑L stirred‑tank bioreactor under uncontrolled pH conditions using the optimized medium resulted in a signifcant increase in both the volumetric and specifc productivities of ALP; the alkaline phosphatase throughput 6650.9 U L−1, and µ = 0.0943 ­h−1; respectively, were obtained after 8 h that, ameliorated more than 20.96, 70.12 and 94 folds compared to basal media, PBD, and RCCD; respectively. However, neither the increased cell growth nor enhanced productivity of ALP was present under the pH‑controlled batch cultivation. Overall, this work presents novel strategies for the statistical optimization and scaling up of bacterial ALP production using biogenic apatite. Te bioeconomy represents the value chain of sustainable manufacturing using renewable, low-cost biological resources to sustainably produce food, energy, and industrial products1.
    [Show full text]
  • Cosmochemistry Cosmic Background RadiaOn
    6/10/13 Cosmochemistry Cosmic background radiaon Dust Anja C. Andersen Niels Bohr Instute University of Copenhagen hp://www.dark-cosmology.dk/~anja Hauser & Dwek 2001 Molecule formation on dust grains Multiwavelenght MW 1 6/10/13 Gas-phase element depleons in the Concept of dust depleon interstellar medium The depleon of an element X in the ISM is defined in terms of (a logarithm of) its reducon factor below the expected abundance relave to that of hydrogen if all of the atoms were in the gas phase, [Xgas/H] = log{N(X)/N(H)} − log(X/H) which is based on the assumpon that solar abundances (X/H)are good reference values that truly reflect the underlying total abundances. In this formula, N(X) is the column density of element X and N(H) represents the column density of hydrogen in both atomic and molecular form, i.e., N(HI) + 2N(H2). The missing atoms of element X are presumed to be locked up in solids within dust grains or large molecules that are difficult to idenfy spectroscopically, with fraconal amounts (again relave to H) given by [Xgas/H] (Xdust/H) = (X/H)(1 − 10 ). Jenkins 2009 Jenkins 2009 2 6/10/13 Jenkins 2009 Jenkins 2009 The Galacc Exncon Curve Extinction curves measure the difference in emitted and observed light. Traditionally measured by comparing two stars of the same spectral type. Galactic Extinction - empirically determined: -1 -1 <A(λ)/A(V)> = a(λ ) + b(λ )/RV (Cardelli et al. 1999) • Bump at 2175 Å (4.6 µm-1) • RV : Ratio of total to selective extinction in the V band • Mean value is RV = 3.1 (blue) • Low value: RV = 1.8 (green) (Udalski 2003) • High value: RV = 5.6-5.8 (red) (Cardelli et al.
    [Show full text]
  • Download Complete Volume
    JOURNAL OF THE TRANSACTIONS OF THE - VICTOR I A INSTITUTE. VOL. XXI. SECTION NI;> I FROM SEA. COAST AT A.Sl(A,LA ~ H JERUSAlEM TO THE J,JR~AN IIIC.0 JEHi CH O." t<0~110,n·... lsc"lt3''"'EII -I,,..,;;": C.S. Wlc.Sw,a.~t,n,,,ofl'l,illutin., N. l. Nwri,.wlil,: .l,V,W,,tn,u,, C. l . Crct,rcc,,,,,, J.,,,.,,,.i,,,,..., _ N. 1.:. }Vu.blit.n. Sun.J&/.,)1.,. F. V, £,,1.~1,,,,~. SECTION N'? 2. FRO M T H E. T A.B LE · LANO Of' S ,JUD.EA TOT Mt PLAINS Of'MOA.B ~. oFKtRAH. 8YJEB£L USOUM. TA.SL£ L,.ND or MOAB SECTION N~ 7 !='ROM cuLr o F sun MEAFtTO R eY THE M OUNTAINS o, s 1ttA.1 ro-:-wt: PLAT EAU or TH£ TIH. No rt,h, G. &rcy !Jra..,,,i, t;,e, (F>1.r-i,.t(C11) a.n.d, 5,·'hi.tt. w.:.th. ·m.,,m.flr-OU.4 d.y1<.r f! , • ..,,po.-w,g s,uubto,.,, n,,d.Li,,,... •w,,.-B,:,i,, / S . 8 L j 11flRl20NTALSCALr 11MIL[ S• I INCH. J)y l~o;1nniu,on of th i:J Oommittce (•f the /'o,T,i:sti.1w E :cpluMtivn Fund. JOURNAL OF THE TRANSACTIONS OF ~ht lictoria Jnstitut~, <'lR l!gilosopgital cSotiet~ of ~reat Jritain. EDITED BY THE HONORARY SECRETARY, CAPTAIN FRANCIS W. H. PETRIE, F.G.fS., &c. VOL. XXI. LONDON: (tBublisbell n11 tbe Institute). INDIA: W. THACKER & Co. UNITED STATES: G. T.PUTNAM'S SONS, N.Y_.
    [Show full text]
  • (50000) Quaoar, See Quaoar (90377) Sedna, See Sedna 1992 QB1 267
    Index (50000) Quaoar, see Quaoar Apollo Mission Science Reports 114 (90377) Sedna, see Sedna Apollo samples 114, 115, 122, 1992 QB1 267, 268 ap-value, 3-hour, conversion from Kp 10 1996 TL66 268 arcade, post-eruptive 24–26 1998 WW31 274 Archimedian spiral 11 2000 CR105 269 Arecibo observatory 63 2000 OO67 277 Ariel, carbon dioxide ice 256–257 2003 EL61 270, 271, 273, 274, 275, 286, astrometric detection, of extrasolar planets – mass 273 190 – satellites 273 Atlas 230, 242, 244 – water ice 273 Bartels, Julius 4, 8 2003 UB313 269, 270, 271–272, 274, 286 – methane 271–272 Becquerel, Antoine Henry 3 – orbital parameters 271 Biermann, Ludwig 5 – satellite 272 biomass, from chemolithoautotrophs, on Earth 169 – spectroscopic studies 271 –, – on Mars 169 2005 FY 269, 270, 272–273, 286 9 bombardment, late heavy 68, 70, 71, 77, 78 – atmosphere 273 Borealis basin 68, 71, 72 – methane 272–273 ‘Brown Dwarf Desert’ 181, 188 – orbital parameters 272 brown dwarfs, deuterium-burning limit 181 51 Pegasi b 179, 185 – formation 181 Alfvén, Hannes 11 Callisto 197, 198, 199, 200, 204, 205, 206, ALH84001 (martian meteorite) 160 207, 211, 213 Amalthea 198, 199, 200, 204–205, 206, 207 – accretion 206, 207 – bright crater 199 – compared with Ganymede 204, 207 – density 205 – composition 204 – discovery by Barnard 205 – geology 213 – discovery of icy nature 200 – ice thickness 204 – evidence for icy composition 205 – internal structure 197, 198, 204 – internal structure 198 – multi-ringed impact basins 205, 211 – orbit 205 – partial differentiation 200, 204, 206,
    [Show full text]
  • Marine Extremophiles: a Source of Hydrolases for Biotechnological Applications
    Mar. Drugs 2015, 13, 1925-1965; doi:10.3390/md13041925 OPEN ACCESS marine drugs ISSN 1660-3397 www.mdpi.com/journal/marinedrugs Article Marine Extremophiles: A Source of Hydrolases for Biotechnological Applications Gabriel Zamith Leal Dalmaso 1,2, Davis Ferreira 3 and Alane Beatriz Vermelho 1,* 1 BIOINOVAR—Biotechnology laboratories: Biocatalysis, Bioproducts and Bioenergy, Institute of Microbiology Paulo de Góes, Federal University of Rio de Janeiro, Av. Carlos Chagas Filho, 373, 21941-902 Rio de Janeiro, Brazil; E-Mail: [email protected] 2 Graduate Program in Plant Biotechnology, Health and Science Centre, Federal University of Rio de Janeiro, Av. Carlos Chagas Filho, 373, 21941-902 Rio de Janeiro, Brazil 3 BIOINOVAR—Biotechnology Laboratories: Virus-Cell Interaction, Institute of Microbiology Paulo de Góes, Federal University of Rio de Janeiro, Av. Carlos Chagas Filho, 373, 21941-902 Rio de Janeiro, Brazil; E-Mail: [email protected] * Author to whom correspondence should be addressed; E-Mail: [email protected]; Tel.: +55-(21)-3936-6743; Fax: +55-(21)-2560-8344. Academic Editor: Kirk Gustafson Received: 1 December 2014 / Accepted: 25 March 2015 / Published: 3 April 2015 Abstract: The marine environment covers almost three quarters of the planet and is where evolution took its first steps. Extremophile microorganisms are found in several extreme marine environments, such as hydrothermal vents, hot springs, salty lakes and deep-sea floors. The ability of these microorganisms to support extremes of temperature, salinity and pressure demonstrates their great potential for biotechnological processes. Hydrolases including amylases, cellulases, peptidases and lipases from hyperthermophiles, psychrophiles, halophiles and piezophiles have been investigated for these reasons.
    [Show full text]
  • Orbital Evidence for More Widespread Carbonate- 10.1002/2015JE004972 Bearing Rocks on Mars Key Point: James J
    PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Orbital evidence for more widespread carbonate- 10.1002/2015JE004972 bearing rocks on Mars Key Point: James J. Wray1, Scott L. Murchie2, Janice L. Bishop3, Bethany L. Ehlmann4, Ralph E. Milliken5, • Carbonates coexist with phyllosili- 1 2 6 cates in exhumed Noachian rocks in Mary Beth Wilhelm , Kimberly D. Seelos , and Matthew Chojnacki several regions of Mars 1School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, Georgia, USA, 2The Johns Hopkins University/Applied Physics Laboratory, Laurel, Maryland, USA, 3SETI Institute, Mountain View, California, USA, 4Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA, 5Department of Geological Sciences, Brown Correspondence to: University, Providence, Rhode Island, USA, 6Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona, USA J. J. Wray, [email protected] Abstract Carbonates are key minerals for understanding ancient Martian environments because they Citation: are indicators of potentially habitable, neutral-to-alkaline water and may be an important reservoir for Wray, J. J., S. L. Murchie, J. L. Bishop, paleoatmospheric CO2. Previous remote sensing studies have identified mostly Mg-rich carbonates, both in B. L. Ehlmann, R. E. Milliken, M. B. Wilhelm, Martian dust and in a Late Noachian rock unit circumferential to the Isidis basin. Here we report evidence for older K. D. Seelos, and M. Chojnacki (2016), Orbital evidence for more widespread Fe- and/or Ca-rich carbonates exposed from the subsurface by impact craters and troughs. These carbonates carbonate-bearing rocks on Mars, are found in and around the Huygens basin northwest of Hellas, in western Noachis Terra between the Argyre – J.
    [Show full text]