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18 results on '"D. N. Harpold"'

1. Sample Analysis at Mars

Author

W B Brinckerhoff, P R Mahaffy, M Cabane, S K Atreya, P Coll, T J Cornish, D N Harpold, G Israel, H B Niemann, and T Owen

Subjects
Lunar And Planetary Science And Exploration
Abstract

The next landed missions to Mars, such as the planned Mars Science Laboratory and ExoMars, will require sample analysis capabilities refined well beyond what has been flown to date. A key science objective driving this requirement is the determination of the carbon inventory of Mars, and particularly the detection of organic compounds. While the gas chromatograph mass spectrometers (GC/MS) on the Viking landers did not detect any indigenous organics in near surface fines, it is possible that these measurements were not representative of Mars on the whole. That is, those compounds to which the GC/MS was sensitive would likely not have survived the strong oxidative decomposition in the regolith at the landing sites in question. The near surface fines could very well contain a significant quantity of refractory compounds that would not have been volatilized in the sample ovens on Viking. It is also possible that volatile organics exist on Mars in sedimentary, subsurface, or polar niches.

Published
2003

2. The Neutral Gas and Ion Mass Spectrometer on the Mars Atmosphere and Volatile Evolution Mission

Author

Cynthia Gundersen, Ryan M. Miller, E. Raaen, Marvin Noriega, Patrick Kimvilakani, J. Thomas Nolan, Ferzan Jaeger, Todd King, Charles Edmonson, Ken Arnett, James W. Kellogg, Robert Arvey, Florence Tan, Edwin Weidner, Steven Battel, Kiran Patel, Felix Noreiga, Curt Cooper, B. D. Prats, Anthony Melak, Christopher S. Johnson, Therese Errigo, Mehdi Benna, Paul R. Mahaffy, Jerome Hengemihle, Matthew Lefavor, Vincent Holmes, Daniel Carrigan, Eric Lyness, John Maurer, Bruce P. Block, Michael Barciniak, D. N. Harpold, and Mirl Bendt

Subjects
Atmospheric escape, Astronomy and Astrophysics, Atmosphere of Mars, Mars Exploration Program, Atmospheric sciences, Ion source, Astrobiology, Atmosphere, Solar wind, Planetary science, Space and Planetary Science, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Environmental science, Astrophysics::Earth and Planetary Astrophysics, Ionosphere, Physics::Atmospheric and Oceanic Physics
Abstract

The Neutral Gas and Ion Mass Spectrometer (NGIMS) of the Mars Atmosphere and Volatile Evolution Mission (MAVEN) is designed to measure the composition, struc- ture, and variability of the upper atmosphere of Mars. The NGIMS complements two other instrument packages on the MAVEN spacecraft designed to characterize the neutral upper atmosphere and ionosphere of Mars and the solar wind input to this region of the atmo- sphere. The combined measurement set is designed to quantify atmosphere escape rates and provide input to models of the evolution of the martian atmosphere. The NGIMS is designed to measure both surface reactive and inert neutral species and ambient ions along the space- craft track over the 125-500 km altitude region utilizing a dual ion source and a quadrupole analyzer.

Published
2014
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3. The Neutral Mass Spectrometer on the Lunar Atmosphere and Dust Environment Explorer Mission

Author

Paul R. Mahaffy, Ferzan Jaeger, Charles Edmonson, Matthew Lefavor, R. Richard Hodges, Ryan M. Miller, D. N. Harpold, Mehdi Benna, B. D. Prats, T. Nolan, Patrick Kimvilakani, Felix Noreiga, E. Raaen, Steven Battel, John Maurer, Bruce P. Block, Todd King, Kiran Patel, Eric Lyness, Michael Barciniak, Vincent Holmes, Daniel Carigan, Robert Arvey, Florence Tan, Edwin Weidner, Therese Errigo, Christopher S. Johnson, Jerome Hengemihle, Cynthia Gundersen, Marvin Noriega, Mirl Bendt, Omar Quinones, Ken Arnett, Michael Woronowicz, James W. Kellogg, Curt Cooper, and Daniel Nguyen

Subjects
Argon, Atmosphere of the Moon, chemistry, Spacecraft, business.industry, chemistry.chemical_element, Mass spectrometry, business, Lunation, Helium, Ion source, Astrobiology
Abstract

The Neutral Mass Spectrometer (NMS) of the Lunar Atmosphere and Dust Environment Explorer (LADEE) Mission is designed to measure the composition and variability of the tenuous lunar atmosphere. The NMS complements two other instruments on the LADEE spacecraft designed to secure spectroscopic measurements of lunar composition and in situ measurement of lunar dust over the course of a 100-day mission in order to sample multiple lunation periods. The NMS utilizes a dual ion source designed to measure both surface reactive and inert species and a quadrupole analyzer. The NMS is expected to secure time resolved measurements of helium and argon and determine abundance or upper limits for many other species either sputtered or thermally evolved from the lunar surface.

Published
2015
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4. Noble gas abundance and isotope ratios in the atmosphere of Jupiter from the Galileo Probe Mass Spectrometer

Author

Tobias Owen, D. N. Harpold, Hasso B. Niemann, T. M. Donahue, J. Demick, Paul R. Mahaffy, S. K. Atreya, and A. Alpert

Subjects
Atmospheric Science, Materials science, Atmosphere of Jupiter, Analytical chemistry, Galileo Probe, Soil Science, chemistry.chemical_element, Aquatic Science, Oceanography, Jovian, Astrobiology, Jupiter, Xenon, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Isotopes of xenon, Earth-Surface Processes, Water Science and Technology, Ecology, Krypton, Paleontology, Noble gas, Forestry, Geophysics, chemistry, Space and Planetary Science
Abstract

The Galileo Probe Mass Spectrometer provided the first data on the noble gas mixing and isotope ratios in the Jovian atmosphere. These measurements and the comparison with solar values constrain models of Jupiter's formation. Significant refinements to the initially reported abundances of argon, krypton, and xenon have been enabled through post-encounter laboratory calibrations using a refurbished engineering unit mass spectrometer nearly identical to the flight unit. The abundances relative to hydrogen for argon, krypton, and xenon are respectively 2.5 +/- 0.5, 2.7 +/- 0.5, and 2.6 +/- 0.5 times the solar ratios. The mixing ratios of He and Ne found in these studies are consistent with previously reported values of 0.8 and 0.1 times solar respectively. The Jovian Ar-36/Ar-38 ratio is 5.6 +/- 0.25 and the Ne-20/Ne-22 ratio is 13 +/- 2, consistent with the solar values of 5.77 and 13.81, respectively, that are derived from lunar mineral grain analysis. The distribution of xenon isotopes at Jupiter also resembles the solar distribution.

Published
2000
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5. Volatile and Organic Compositions of Sedimentary Rocks in Yellowknife Bay, Gale Crater, Mars

Author

M. A. Meyer, Mark I. Richardson, Robert C. Anderson, Marisa C. Palucis, Sara Navarro Lopez, Rodney C. Ewing, Sanjeev Gupta, Caroline Freissinet, Edward M. Stolper, James F. Bell, M. A. Ravine, I. G. Mitrofanov, Thomas F. Bristow, Dawn Y. Sumner, Joel A. Hurowitz, Robert M. Haberle, Claire E. Newman, Andrew Steele, Muriel Saccoccio, Leslie Keely, E. Pallier, Jason P. Dworkin, Claude Geffroy, Mary A. Voytek, Michael Caplinger, Fred Goesmann, Yann Parot, Maria-Paz Zorzano Mier, A. B. Sanin, S. W. Squyres, Javier Caride Rodriguez, J. L. Griffes, Julio José Romeral-Planello, Jason Feldman, Katherine L. French, V. Sautter, Nicolas Mangold, David L. Bish, Vivian Lafaille, Michael D. Smith, François Raulin, V. Prokhorov, Gilles Berger, S. Slavney, Heather B. Franz, S. Johnstone, Susanne P. Schwenzer, Felipe Gómez, Harri Haukka, Francis A. Cucinotta, J. Hudgins, T. Cleghorn, Pascaline Francois, Alain Lepinette Malvitte, Shuai Li, Paul R. Mahaffy, K. M. Robertson, Bruce M. Jakosky, J. Guo, Juergen Schieber, Rafael Navarro-González, G. J. Flesch, Scott M. McLennan, Jennifer G. Blank, M. Carmosino, Kenneth A. Farley, Yves Langevin, P. D. Archer, A. E. Brunner, M. D. Dyar, S. Le Mouélic, V. Hipkin, Sara Alejandra Sans Fuentes, Kenneth S. Edgett, Sabrina Feldman, Gale Paulsen, Paul Herrera, Alberto G. Fairén, Kirsten L. Siebach, Jan-Peter Muller, M. J. Schoppers, Eldar Noe Dobrea, Nina Lanza, Marc Gailhanou, Genevieve Marchand, Sönke Burmeister, Craig Hardgrove, Justin N. Maki, Ari-Matti Harri, Michael C. Malin, M. J. Wolff, Roger E. Summons, H. Blau, Jacqueline Cameron, Jeff A. Berger, Didier Keymeulen, Agnes Cousin, Guillermo M. Muñoz Caro, Eric Lyness, Cedric Pilorget, Michael B. Baker, Christopher S. Edwards, M. L. Litvak, Brian M. Duston, Rebecca M. E. Williams, T. Nolan, Robert T. Downs, V. E. Hamilton, Walter Goetz, Pamela G. Conrad, J. Baroukh, Nathan T. Bridges, Meenakshi Wadhwa, Roger C. Wiens, Samuel M. Clegg, Philippe Sarrazin, L. Bleacher, Eric Lorigny, Mike Toplis, Michael H. Wong, Timothy H. McConnochie, Ian Mcewan, Kiran Patel, Mary Beth Wilhelm, John P. Grotzinger, Jeffrey E. Moersch, Michael A. Wilson, Mark Paton, I. Plante, Eric Lewin, Franck Poitrasson, Tori M. Hoehler, P. Guillemot, Mackenzie Day, David F. Blake, José Antonio Rodríguez Manfredi, G. W. Lugmair, Robert F. Wimmer-Schweingruber, Dorothy Z. Oehler, Samuel Teinturier, Bent Ehresmann, Jérémie Lasue, K. E. Herkenhoff, Daniel C. Berman, Scott VanBommel, Jeffrey R. Johnson, Emily M. McCullough, A. A. Fraeman, Ezat Heydari, Penelope L. King, K. M. Stack, Diana L. Blaney, A. Salamon, John G. Spray, L. Posiolova, Jeff Hollingsworth, David Choi, Kevin W. Lewis, B. D. Prats, Tonci Balic-Zunic, Mehdi Benna, H. M. Elliott, Jesús Martínez-Frías, R. Mueller-Mellin, William V. Boynton, Lance E. Christensen, Richard Leveille, John A. Grant, David E. Harker, J. M. Morookian, Caleb I. Fassett, S. Jacob, Donald Fay, R. Perez, Horton E. Newsom, Morten Madsen, M. G. Trainer, G. Israel, B. E. Nixon, Claude d’Uston, John E. Moores, Olivier Gasnault, Daniel J. Krysak, Vladislav Tretyakov, G. M. Perrett, Andrew D. Aubrey, L. E. Kirkland, F. Stalport, B. L. Barraclough, Alain Cros, Stephan Böttcher, Michel Cabane, William B. Brinckerhoff, Jack D. Farmer, James J. Wray, P. Y. Meslin, Arnaud Buch, Allan H. Treiman, S. C. R. Rafkin, B. C. Clark, Noureddine Melikechi, R. Jackson, Luther W. Beegle, Angela Lundberg, Bethany L. Ehlmann, William E. Dietrich, Karl Iagnemma, K. Supulver, Radu Popa, R. Zimdar, Melissa Floyd, Wesley T. Huntress, Paul B. Niles, D. M. Delapp, C. N.. Achilles, Darrell Drake, T. Nelson, Alain Gaboriaud, Verónica Peinado-Gonzalez, Edward P. Vicenzi, T. Boucher, Jennifer L. Eigenbrode, C. Tate, David J. Des Marais, F. Javier Martin-Torres, Antoine Charpentier, Chris Webster, Mildred P. Martin, Robert M. Sucharski, Lucy M. Thompson, Cyril Szopa, D. Halleaux, Antonio Molina Jurado, Richard V. Morris, Andrey Vostrukhin, Peter C. Thomas, Ara V. Nefian, Pablo Sobron Sanchez, Manuel de la Torre Juárez, B. Elliott, Hannu Savijärvi, J. Bentz, Sergey Nikiforov, S. Gordon, Shaunna M. Morrison, Jean-Luc Lacour, Günter Reitz, M. E. Newcombe, David E. Brinza, C. Yana, Gary Kocurek, L. J. Lipkaman, C. M. Garcia, Maria Genzer, Fred Calef, A. Godber, Stubbe F. Hviid, C. Donny, T. Van Beek, Ruslan O. Kuzmin, Alexander Hayes, T. S. Olson, George D. Cody, J. Martín-Soler, N. Karpushkina, John Bridges, Mercedes Jiménez, M. Lefavor, Sylvestre Maurice, H. L. K. Manning, Ralph E. Milliken, Susanne Schröder, N. Spanovich, L. J. Edwards, A. Koefoed, Roser Urqui-O'Callaghan, Eduardo Sebastian Martinez, Cary Zeitlin, Noël Stewart, David T. Vaniman, E. A. Breves, Laurent Favot, A. Varenikov, Gérard Manhès, R. B. Williams, David Martin, Steven J. Rowland, E. Boehm, Adrian P. Jones, Alexis Paillet, R. Francis, Sushil K. Atreya, Mariek E. Schmidt, David Baratoux, N. I. Boyd, Qiu-Mei Lee, I. L. ten Kate, Bernard Hallet, K. Stoiber, Vivian Z. Sun, M. R. Kennedy, Gillian M. Krezoski, Mark A. Bullock, T. Stein, Michelle E. Minitti, I. Pradler, Susan L. S. Stipp, Scott Davis, Robert O. Pepin, B. L. Ehlmann, Janne Kauhanen, Dmitry Golovin, Steve J. Chipera, Raymond E. Arvidson, Javier Gómez-Elvira, L. C. Kah, Melissa S. Rice, Isaias Carrasco Blazquez, Cécile Fabre, John J. Simmonds, Joy A. Crisp, Jens Frydenvang, Florence Tan, Julia DeMarines, S. P. Gorevan, Elizabeth B. Rampe, E. McCartney, Lauren DeFlores, K. Harshman, D. N. Harpold, J. Van Beek, Luis Mora-Sotomayor, Douglas W. Ming, Kristen E. Miller, John Campbell, Amy McAdam, L. Saper, Robert Sullivan, Lorenzo Fluckiger, Kjartan M. Kinch, Arik Posner, H. Bower, A. A. Pavlov, D. Scholes, Insoo Jun, Brigitte Gondet, Patrice Coll, Burt Baker, Donald M. Hassler, Ralf Gellert, Laurie A. Leshin, T. Siili, Gilles Dromart, Lauren A. Edgar, Ryan B. Anderson, Robert Dingler, Leon Radziemski, Jean-Baptiste Sirven, G. Weigle, Cynthia K. Little, A. Mezzacappa, Olivier Forni, A. S. Kozyrev, Edward A. Cloutis, Ashwin Vasavada, A. Behar, François Robert, D. M. Rubin, Alexey Malakhov, E. Jensen, T. C. Owen, Sebastien Hettrich, Miguel Ramos, B. Sutter, Melinda A. Kahre, Patrick Pinet, John H. Jones, Claude Brunet, B. Pavri, Nilton O. Renno, Evgeny Atlaskin, Laurent Peret, Maxim Mokrousov, David Lees, J. J. B. Avalos, Jennifer C. Stern, Ann Ollila, Josefina Torres Redondo, Miles J. Johnson, M. A. D. P. Hernandez, Daniel P. Glavin, Albert S. Yen, Christophe Agard, Jouni Polkko, Christopher P. McKay, J. Peterson, Oliver Botta, Mark T. Lemmon, Marion Nachon, K. M. Bean, Bruce A. Cantor, Jan Köhler, M. Fitzgibbon, Carlos Armiens-Aparicio, Jorge Pla-Garcia, Henrik Kahanpää, Frances Westall, Walter Schmidt, M.-H. Kim, Kenneth G. Miller, Sharon A. Wilson, S. McNair, O. Kortmann, David Grinspoon, E. M. Lee, S. Indyk, Osku Kemppinen, E. Raaen, Michael Mischna, R. S. Sletten, James B. Garvin, John M. Ward, R. L. Tokar, Paulo M. Vasconcelos, Charles Malespin, T. J. Parker, Aaron J. Sengstacken, S. Bender, Jean-Pierre Williams, F. Fedosov, Patrick Mauchien, Audrey Dupont, R. A. Yingst, David Coscia, David A. Cremers, Danika Wellington, Kenneth H. Nealson, J. K. Jensen, Martin R. Fisk, J. Joseph, Amy J. Williams, W. Brunner, NASA Johnson Space Center (JSC), NASA, NASA Goddard Space Flight Center (GSFC), Center for Research and Exploration in Space Science and Technology [GSFC] (CRESST), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Guelph], University of Guelph, Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, ASU School of Earth and Space Exploration (SESE), Arizona State University [Tempe] (ASU), Laboratoire de Génie des Procédés et Matériaux - EA 4038 (LGPM), CentraleSupélec, Space Science and Astrobiology Division at Ames, NASA Ames Research Center (ARC), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Astronomy [Ithaca], Cornell University [New York], Center for Earth and Planetary Studies [Washington] (CEPS), Smithsonian National Air and Space Museum, Smithsonian Institution-Smithsonian Institution, Department of Earth Science and Technology [Imperial College London], Imperial College London, United States Geological Survey [Reston] (USGS), Department of Geosciences [Stony Brook], Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), Rensselaer Polytechnic Institute (RPI), Princeton University, State University of New York (SUNY), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Department of Earth and Planetary Sciences [Knoxville], The University of Tennessee [Knoxville], Instituto de Ciencias Nucleares [Mexico], Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Geophysical Laboratory [Carnegie Institution], Carnegie Institution for Science, Department of Earth and Planetary Science [UC Berkeley] (EPS), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), NOAA Earth System Research Laboratory (ESRL), National Oceanic and Atmospheric Administration (NOAA), Lunar and Planetary Institute [Houston] (LPI), Planetary Science Institute [Tucson] (PSI), School of Earth and Atmospheric Sciences [Atlanta], Georgia Institute of Technology [Atlanta], Aalto University, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Applied Research Associates, Inc. (ARA), Center for Meteorite Studies [Tempe], Ashima Research, ATOS Origin, Australian National University (ANU), Bay Area Environmental Research Institute (BAER), Big Head Endian LLC, Brock University [Canada], Brown University, Canadian Space Agency (CSA), Capgemini Consulting [Paris], Carnegie Mellon University [Pittsburgh] (CMU), Catholic University of America, Institut des Matériaux, de Microélectronique et des Nanosciences de Provence (IM2NP), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Chesapeake Energy Corporation, Service de la Corrosion et du Comportement des Matériaux dans leur Environnement (SCCME), Département de Physico-Chimie (DPC), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Interaction Laser Matière (LILM), Concordia College, Moorhead, CS-Systèmes d'Information [Toulouse] (CS-SI), Delaware State University (DSU), Denver Museum of Nature and Science, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Finnish Meteorological Institute (FMI), GeoRessources, Institut national des sciences de l'Univers (INSU - CNRS)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Géosciences Environnement Toulouse (GET), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Global Science and Technology, Inc., Honeybee Robotics Ltd, Indiana University [Bloomington], Indiana University System, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Chimie des Milieux et Matériaux de Poitiers (IC2MP), Université de Poitiers-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Institut des Sciences de la Terre (ISTerre), Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-PRES Université de Grenoble-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Jackson State University (JSU), Jacobs Technology ESCG, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Minéralogie et Cosmochimie du Muséum (LMCM), Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), Space Remote Sensing Group (ISR-2), Malin Space Science Systems (MSSS), Depertment of Polymer Chemistry, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, DLR Institute of Planetary Research, German Aerospace Center (DLR), NASA Headquarters, Oregon State University (OSU), Search for Extraterrestrial Intelligence Institute (SETI), Smithsonian Institution, Department of Space Studies [Boulder], Southwest Research Institute [Boulder] (SwRI), Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), TechSource Inc., Texas A&M University [College Station], The Open University [Milton Keynes] (OU), University of Arizona, Met Office Hadley Centre for Climate Change (MOHC), United Kingdom Met Office [Exeter], Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), California Institute of Technology (CALTECH)-NASA, Universidad Nacional Autónoma de México (UNAM), Carnegie Institution for Science [Washington], University of California [Berkeley], University of California-University of California, Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), Centre National de la Recherche Scientifique (CNRS)-Université de Lorraine (UL)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-PRES Université de Grenoble-Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry]), University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), NWO-NSO: The role of perchlorates in the preservation of organic compounds on Mars, Petrology, Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Centre National de la Recherche Scientifique (CNRS)-Muséum national d'Histoire naturelle (MNHN), and Kruch, Catherine

Subjects
Geologic Sediments, 010504 meteorology & atmospheric sciences, Extraterrestrial Environment, Curiosity rover, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mineralogy, [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mars, Sulfides, 01 natural sciences, organic compositions, Bassanite, 0103 physical sciences, Exobiology, [SDU.ASTR.SR] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Hydrocarbons, Chlorinated, MSL, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Total organic carbon, Martian, mudstone samples, Volatile Organic Compounds, Multidisciplinary, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Water, Mars Exploration Program, Carbon Dioxide, Oxygen, Bays, 13. Climate action, Rocknest, Sample Analysis at Mars, Sedimentary rock, Pyrolysis
Abstract

H 2 O, CO 2 , SO 2 , O 2 , H 2 , H 2 S, HCl, chlorinated hydrocarbons, NO, and other trace gases were evolved during pyrolysis of two mudstone samples acquired by the Curiosity rover at Yellowknife Bay within Gale crater, Mars. H 2 O/OH-bearing phases included 2:1 phyllosilicate(s), bassanite, akaganeite, and amorphous materials. Thermal decomposition of carbonates and combustion of organic materials are candidate sources for the CO 2 . Concurrent evolution of O 2 and chlorinated hydrocarbons suggests the presence of oxychlorine phase(s). Sulfides are likely sources for sulfur-bearing species. Higher abundances of chlorinated hydrocarbons in the mudstone compared with Rocknest windblown materials previously analyzed by Curiosity suggest that indigenous martian or meteoritic organic carbon sources may be preserved in the mudstone; however, the carbon source for the chlorinated hydrocarbons is not definitively of martian origin.

Published
2014
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6. The Sample Analysis at Mars Investigation and Instrument Suite

Author

David Martin, Michel Cabane, Tobias Owen, John H. Jones, Ryan M. Miller, Greg Flesch, Florence Tan, James J. Wray, L. Bleacher, Didier Keymeulen, Cyril Szopa, E. Raaen, Douglas W. Ming, Paul R. Mahaffy, Robert A. Chalmers, Douglas L. Hawk, Curt Baffes, Laurie A. Leshin, Pamela G. Conrad, Oren E. Sheinman, Jennifer L. Eigenbrode, Robert Kline-Schoder, Paul Sorensen, D. Sheppard, Mark Cascia, Gregory Frazier, Daniel P. Glavin, Richard V. Morris, Arnaud Buch, Christopher P. McKay, Rafael Navarro-González, Charles Malespin, Patrice Coll, Rodger Farley, Christopher S. Johnson, Chris Webster, Cindy Gundersen, Bruce M. Jakosky, Daniel Carignan, Paula Everson, Heather B. Franz, Jason Feldman, Steve Woodward, Ray Garcia, Andrea Jones, Eric Lyness, Ken Arnett, Samuel Teinturier, Melissa G. Trainer, Mehdi Benna, Alexander A. Pavlov, E. Mumm, Steven W. Squyres, Marvin Noriega, James W. Kellogg, Jesse Lewis, Oliver Botta, David Coscia, H. L. K. Manning, John Maurer, Charles Edmonson, Steven Feng, Caroline Freissinet, Siamak Forouhar, Andrew Steele, Robert Arvey, Jason P. Dworkin, Douglas McLennan, Stephen Gorevan, Jennifer C. Stern, François Raulin, James Smith, Patrick R. Jordan, Sushil K. Atreya, Robert Sternberg, B. D. Prats, Therese Errigo, Bruce P. Block, T. Nolan, Michael Barciniak, D. N. Harpold, Vincent Holmes, William B. Brinckerhoff, Amy McAdam, Steve Battel, NASA Goddard Space Flight Center (GSFC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, NASA Johnson Space Center (JSC), NASA, AMU Engineering, Inc., Geophysical Laboratory [Carnegie Institution], Carnegie Institution for Science [Washington], School of Earth and Atmospheric Sciences [Atlanta], Georgia Institute of Technology [Atlanta], Swiss Space Office Bern (SSO), Department of Earth and Environmental Sciences [Troy, NY], Rensselaer Polytechnic Institute (RPI), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Battel Engineering, Inc., Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Concordia College, Moorhead, Department of Astronomy [Ithaca], Cornell University [New York], Laboratorio de Química de Plasmas y Estudios Planetarios [Mexico], Instituto de Ciencias Nucleares [Mexico], Universidad Nacional Autónoma de México (UNAM)-Universidad Nacional Autónoma de México (UNAM), NASA Ames Research Center (ARC), Ecole Centrale Paris, Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Space Physics Research Laboratory [Ann Arbor] (SPRL), IMPEC - LATMOS, Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Cornell University, Carnegie Institution for Science, Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM)-Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), NASA Goddard Space Flight Center ( GSFC ), Jet Propulsion Laboratory ( JPL ), NASA-California Institute of Technology ( CALTECH ), Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire inter-universitaire des systèmes atmosphèriques ( LISA ), Centre National de la Recherche Scientifique ( CNRS ) -Université Paris-Est Créteil Val-de-Marne - Paris 12 ( UPEC UP12 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Institut national des sciences de l'Univers ( INSU - CNRS ), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] ( AOSS ), NASA Johnson Space Center ( JSC ), Swiss Space Office Bern ( SSO ), Department of Earth and Environmental Sciences [Troy], Rensselaer Polytechnic Institute ( RPI ), University of Hawaii at Manoa ( UHM ), Laboratory for Atmospheric and Space Physics [Boulder] ( LASP ), University of Colorado Boulder [Boulder], Universidad Nacional Autónoma de México ( UNAM ) -Universidad Nacional Autónoma de México ( UNAM ), NASA Ames Research Center ( ARC ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), and Space Physics Research Laboratory [Ann Arbor] ( SPRL )

Subjects
Volatiles, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010504 meteorology & atmospheric sciences, Gas chromatography mass spectrometry, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Habitability, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mars, Life on Mars, 01 natural sciences, Astrobiology, Laboratory, Atmosphere, Isotopes, 0103 physical sciences, Organic compounds, 010303 astronomy & astrophysics, Quadrupole mass analyzer, 0105 earth and related environmental sciences, Spectrometer, [ SDU.ASTR.IM ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astronomy and Astrophysics, Mars Exploration Program, Curiosity Rover, Gale crater, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Noble gases, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [ PHYS.ASTR.EP ] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], 13. Climate action, Space and Planetary Science, Rocknest, Sample Analysis at Mars, Measuring instrument, Environmental science, Evolved gas analysis, [ PHYS.ASTR.IM ] Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract

International audience; The Sample Analysis at Mars (SAM) investigation of the Mars Science Laboratory (MSL) addresses the chemical and isotopic composition of the atmosphere and volatiles extracted from solid samples. The SAM investigation is designed to contribute substantially to the mission goal of quantitatively assessing the habitability of Mars as an essential step in the search for past or present life on Mars. SAM is a 40 kg instrument suite located in the interior of MSL's Curiosity rover. The SAM instruments are a quadrupole mass spectrometer, a tunable laser spectrometer, and a 6-column gas chromatograph all coupled through solid and gas processing systems to provide complementary information on the same samples. The SAM suite is able to measure a suite of light isotopes and to analyze volatiles directly from the atmosphere or thermally released from solid samples. In addition to measurements of simple inorganic compounds and noble gases SAM will conduct a sensitive search for organic compounds with either thermal or chemical extraction from sieved samples delivered by the sample processing system on the Curiosity rover's robotic arm.

Published
2012
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7. Composition of Titan's lower atmosphere and simple surface volatiles as measured by the Cassini-Huygens probe gas chromatograph mass spectrometer experiment

Author

J. A. Haberman, François Raulin, S. K. Atreya, J. E. Demick, Hasso B. Niemann, Jonathan I. Lunine, D. N. Harpold, Tobias Owen, D. Gautier, Wayne Kasprzak, National Aeronautics and Space Administration, Greenbelt, Atmospheric, Oceanic, and Space Science Department, University of Michigan (AOSS), Department of Physics and Physical Science, Huntington College, Montgomery, Alabama, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Università degli Studi di Roma Tor Vergata [Roma], Institute for Astronomy, University of Hawaii, Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), and Dipartimento di Fisica, Università di Roma 2 Tor Vergata

Subjects
Atmospheric Science, Analytical chemistry, Soil Science, chemistry.chemical_element, Aquatic Science, Oceanography, Mole fraction, Methane, Astrobiology, Atmosphere, chemistry.chemical_compound, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Atmosphere of Titan, Chemical composition, Earth-Surface Processes, Water Science and Technology, Life on Titan, Ecology, Krypton, Paleontology, Forestry, Trace gas, Geophysics, chemistry, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; The Cassini-Huygens probe gas chromatograph mass spectrometer (GCMS) determined the composition of the Titan atmosphere from ˜140 km altitude to the surface. After landing, it returned composition data of gases evaporated from the surface. Height profiles of molecular nitrogen (N2), methane (CH4), and molecular hydrogen (H2) were determined. Traces were detected on the surface of evaporating methane, ethane (C2H6), acetylene (C2H2), cyanogen (C2N2), and carbon dioxide (CO2). The methane data showed evidence that methane precipitation occurred recently. The methane mole fraction was (1.48 ± 0.09) × 10-2 in the lower stratosphere (139.8-75.5 km) and (5.65 ± 0.18) × 10-2 near the surface (6.7 km to the surface). The molecular hydrogen mole fraction was (1.01 ± 0.16) × 10-3 in the atmosphere and (9.90 ± 0.17) × 10-4 on the surface. Isotope ratios were 167.7 ± 0.6 for 14N/15N in molecular nitrogen, 91.1 ± 1.4 for 12C/13C in methane, and (1.35 ± 0.30) × 10-4 for D/H in molecular hydrogen. The mole fractions of 36Ar and radiogenic 40Ar are (2.1 ± 0.8) × 10-7 and (3.39 ± 0.12) × 10-5, respectively. 22Ne has been tentatively identified at a mole fraction of (2.8 ± 2.1) × 10-7. Krypton and xenon were below the detection threshold of 1 × 10-8 mole fraction. Science data were not retrieved from the gas chromatograph subsystem as the abundance of the organic trace gases in the atmosphere and on the ground did not reach the detection threshold. Results previously published from the GCMS experiment are superseded by this publication.

Published
2010
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8. The abundances of constituents of Titan's atmosphere from the GCMS instrument on the Huygens probe

Author

G. Israel, Siegfried Bauer, S. Way, R. L. Frost, D. N. Harpold, François Raulin, Wayne Kasprzak, Tobias Owen, Sushil K. Atreya, D. Gautier, G. R. Carignan, Hasso B. Niemann, Jonathan I. Lunine, E. Raaen, Michael B. Paulkovich, J. E. Demick, Donald M. Hunten, J. A. Haberman, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Service d'aéronomie (SA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, Extraterrestrial Environment, Nitrogen, chemistry.chemical_element, Atmospheric sciences, 01 natural sciences, Methane, Gas Chromatography-Mass Spectrometry, Astrobiology, chemistry.chemical_compound, symbols.namesake, Isotopes, 0103 physical sciences, Atmosphere of Titan, Argon, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Multidisciplinary, Life on Titan, Atmosphere, Tholin, Space Flight, Carbon, Outgassing, chemistry, 13. Climate action, symbols, Titan (rocket family)
Abstract

Saturn's largest moon, Titan, remains an enigma, explored only by remote sensing from Earth, and by the Voyager and Cassini spacecraft. The most puzzling aspects include the origin of the molecular nitrogen and methane in its atmosphere, and the mechanism(s) by which methane is maintained in the face of rapid destruction by photolysis. The Huygens probe, launched from the Cassini spacecraft, has made the first direct observations of the satellite's surface and lower atmosphere. Here we report direct atmospheric measurements from the Gas Chromatograph Mass Spectrometer (GCMS), including altitude profiles of the constituents, isotopic ratios and trace species (including organic compounds). The primary constituents were confirmed to be nitrogen and methane. Noble gases other than argon were not detected. The argon includes primordial 36Ar, and the radiogenic isotope 40Ar, providing an important constraint on the outgassing history of Titan. Trace organic species, including cyanogen and ethane, were found in surface measurements.

Published
2005
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9. Did life exist on Mars? Search for organic and inorganic signatures, one of the goals for 'SAM' (sample analysis at Mars)

Author

Paul Mahaffy, Hasso B. Niemann, François Raulin, William B. Brinckerhoff, Patrice Coll, Michel Cabane, C. Rodier, Cyril Szopa, Robert Sternberg, D. N. Harpold, Alain Person, G. Israel, Rafael Navarro-González, Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), UPMC - Département de Géologie Sédimentaire, Université Pierre et Marie Curie - Paris 6 (UPMC), Synthèse et réactivité des substances naturelles (SRSN), Université de Poitiers-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Laboratorio de Química de Plasmas y Estudios Planetarios [Mexico], Instituto de Ciencias Nucleares [Mexico], Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM)-Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), and Laboratoire de Géologie des Bassins Sédimentaires

Subjects
chemistry.chemical_classification, Atmospheric Science, Gas chromatography, Sample (material), Aerospace Engineering, Biosphere, Mars, Astronomy and Astrophysics, Mars Exploration Program, Mass spectrometry, Astrobiology, Atmosphere, Geophysics, chemistry, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Sample Analysis at Mars, General Earth and Planetary Sciences, Environmental science, Organic matter, Derivatisation, Refractory (planetary science), Pyrolysis
Abstract

International audience; Observation of Mars shows signs of a past Earth-like climate, and, in that case, there is no objection to the possible development of life, in the underground or at the surface, as in the terrestrial primitive biosphere. Sample analysis at Mars (SAM) is an experiment which may be proposed for atmospheric, ground and underground in situ measurements. One of its goals is to bring direct or indirect information on the possibility for life to have developed on Mars, and to detect traces of past or present biological activity. With this aim, it focuses on the detection of organic molecules: volatile organics are extracted from the sample by simple heating, whereas refractory molecules are made analyzable (i.e. volatile), using derivatization technique or fragmentation by pyrolysis. Gaseous mixtures thus obtained are analyzed by gas chromatography associated to mass spectrometry. Beyond organics, carbonates and other salts are associated to the dense and moist atmosphere necessary to the development of life, and might have formed and accumulated in some places on Mars. They represent another target for SAM. Heating of the samples allows the analysis of structural gases of these minerals (CO2 from carbonates, etc.), enabling to identify them. We also show, in this paper, that it may be possible to discriminate between abiotic minerals, and minerals (shells, etc.) created by living organisms.

Published
2004
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10. The Gas Chromatograph Mass Spectrometer for the Huygens Probe

Author

Bruce P. Block, D. Gautier, G. R. Carignan, Tobias Owen, G. Israel, Hasso B. Niemann, Donald M. Hunten, D. N. Harpold, K. Biemann, Siegfried Bauer, Jonathan I. Lunine, R. L. Frost, J. A. Haberman, François Raulin, S. Way, J. E. Richards, Sushil K. Atreya, Konrad Mauersberger, and T. M. Donahue

Subjects
chemistry.chemical_compound, Boiling point, Materials science, chemistry, Analytical chemistry, Mixing ratio, Noble gas, Gas chromatography, Gas chromatography–mass spectrometry, Mass spectrometry, Quadrupole mass analyzer, Methane
Abstract

The Gas Chromatograph Mass Spectrometer (GCMS) on the Huygens Probe will meas- ure the chemical composition of Titan's atmosphere from 170 km altitude (∼ 1h Pa) to the surface (∼1500 hPa) and determine the isotope ratios of the major gaseous constituents. The GCMS will also analyze gas samples from the Aerosol Collector Pyrolyser (ACP) and may be able to investigate the composition (including isotope ratios) of several candidate surface materials. The GCMS is a quadrupole mass filter with a secondary electron multiplier detection system and a gas sampling system providing continuous direct atmospheric composition measurements and batch sampling through three gas chromatographic (GC) columns. The mass spectrometer employs five ion sources sequentially feeding the mass analyzer. Three ion sources serve as detectors for the GC columns and two are dedicated to direct atmosphere sampling and ACP gas sampling re- spectively. The instrument is also equipped with a chemical scrubber cell for noble gas analysis and a sample enrichment cell for selective measurement of high boiling point carbon containing constituents. The mass range is 2 to 141 Dalton and the nominal detection threshold is at a mixing ratio of 10 −8 . The data rate available from the Probe system is 885 bit/s. The weight of the instrument is 17.3 kg and the energy required for warm up and 150 minutes of operation is 110 Watt-hours.

Published
2003
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11. The composition of the Jovian atmosphere as determined by the Galileo probe mass spectrometer

Author

G. R. Carignan, T. C. Owen, Wayne Kasprzak, Donald M. Hunten, Richard E. Hartle, J. A. Haberman, Paul R. Mahaffy, D. N. Harpold, S. H. Way, Sushil K. Atreya, T. M. Donahue, and H. B. Niemann

Subjects
Atmospheric Science, Planetesimal, Materials science, Extraterrestrial Environment, Analytical chemistry, Galileo Probe, Soil Science, Aquatic Science, Oceanography, Mass spectrometry, Helium, Noble Gases, Jovian, Mass Spectrometry, Atmosphere, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Mixing ratio, Spacecraft, Mixing (physics), Earth-Surface Processes, Water Science and Technology, Ecology, Paleontology, Astronomy, Forestry, Space Flight, Galaxy, Carbon, Hydrocarbons, Geophysics, Space and Planetary Science, Jupiter, Calibration, Gases, Hydrogen
Abstract

The Galileo probe mass spectrometer determined the composition of the Jovian atmosphere for species with masses between 2 and 150 amu from 0.5 to 21.1 bars. This paper presents the results of analysis of some of the constituents detected: H2, He, Ne, Ar, Kr, Xe, CH4, NH3, H2O, H2S, C2 and C3 nonmethane hydrocarbons, and possibly PH3 and Cl. 4He/H2 in the Jovian atmosphere was measured to be 0.157 +/- 0.030. 13C/C12 was found to be 0.0108 +/- 0.0005, and D/H and 3He/4He were measured. Ne was depleted,or = 0.13 times solar, Aror = 1.7 solar, Kror = 5 solar, and Xeor = 5 solar. CH4 has a constant mixing ratio of (2.1 +/- 0.4) x 10(-3) (12C, 2.9 solar), where the mixing ratio is relative to H2. Upper limits to the H2O mixing ratio rose from 8 x 10(-7) at pressures3.8 bars to (5.6 +/- 2.5) x 10(-5) (16O, 0.033 +/- 0.015 solar) at 11.7 bars and, provisionally, about an order of magnitude larger at 18.7 bars. The mixing ratio of H2S was10(-6) at pressures less than 3.8 bars but rose from about 0.7 x 10(-5) at 8.7 bars to about 7.7 x 10(-5) (32S, 2.5 solar) above 15 bars. Only very large upper limits to the NH3 mixing ratio have been set at present. If PH3 and Cl were present, their mixing ratios also increased with pressure. Species were detected at mass peaks appropriate for C2 and C3 hydrocarbons. It is not yet clear which of these were atmospheric constituents and which were instrumentally generated. These measurements imply (1) fractionation of 4He, (2) a local, altitude-dependent depletion of condensables, probably because the probe entered the descending arm of a circulation cell, (3) that icy planetesimals made significant contributions to the volatile inventory, and (4) a moderate decrease in D/H but no detectable change in (D + 3He)/H in this part of the galaxy during the past 4.6 Gyr.

Published
2001

12. Chemical composition measurements of the atmosphere of Jupiter with the Galileo Probe mass spectrometer

Author

Paul R. Mahaffy, T. M. Donahue, Donald M. Hunten, Tobias Owen, Wayne Kasprzak, Hasso B. Niemann, D. N. Harpold, N. W. Spencer, J. A. Haberman, Richard E. Hartle, Sushil K. Atreya, and G. R. Carignan

Subjects
Atmospheric Science, Materials science, Extraterrestrial Environment, Atmosphere of Jupiter, Galileo Probe, Analytical chemistry, Aerospace Engineering, chemistry.chemical_element, Helium, Noble Gases, Mass Spectrometry, Astrobiology, Atmosphere, Neon, Xenon, Spacecraft, Argon, Atmospheric pressure, Krypton, Astronomy and Astrophysics, Space Flight, Hydrocarbons, Geophysics, Atmospheric Pressure, chemistry, Space and Planetary Science, Jupiter, General Earth and Planetary Sciences, Gases, Hydrogen
Abstract

The Galileo Probe entered the atmosphere of Jupiter on December 7, 1995. Measurements of the chemical and isotopic composition of the Jovian atmosphere were obtained by the mass spectrometer during the descent over the 0.5 to 21 bar pressure region over a time period of approximately 1 hour. The sampling was either of atmospheric gases directly introduced into the ion source of the mass spectrometer through capillary leaks or of gas, which had been chemically processed to enhance the sensitivity of the measurement to trace species or noble gases. The analysis of this data set continues to be refined based on supporting laboratory studies on an engineering unit. The mixing ratios of the major constituents of the atmosphere hydrogen and helium have been determined as well as mixing ratios or upper limits for several less abundant species including: methane, water, ammonia, ethane, ethylene, propane, hydrogen sulfide, neon, argon, krypton, and xenon. Analysis also suggests the presence of trace levels of other 3 and 4 carbon hydrocarbons, or carbon and nitrogen containing species, phosphine, hydrogen chloride, and of benzene. The data set also allows upper limits to be set for many species of interest which were not detected. Isotope ratios were measured for 3He/4He, D/H, 13C/12C, 20Ne/22Ne, 38Ar/36Ar and for isotopes of both Kr and Xe.

Published
2001

13. Cassini orbiter ion and neutral mass spectrometer instrument

Author

J. E. Richards, Hasso B. Niemann, Heidi L. K. Manning, D. N. Harpold, Wayne Kasprzak, E. L. Patrick, and Paul Mahaffy

Subjects
Orbiter, Spectrometer, Ion beam, Radio-frequency quadrupole, law, Chemistry, Atomic physics, Atmosphere of Titan, Mass spectrometry, Ion source, law.invention, Ion
Abstract

The Cassini Orbiter Ion and Neutral Mass Spectrometer (INMS) is designed to measure the composition and density variations of low energy ions and neutral species in the upper atmosphere of Titan, in the vicinity of the icy satellites and in the inner magnetosphere of Saturn where densities are sufficiently high for measurement. The sensor utilizes a dual radio frequency quadrupole mass analyzer with a mass range of 1-99 amu, two electron multipliers operated in pulse-counting mode to cover the dynamic range required and two separate ion sources. A closed ion source measures non-surface reactive neutral species which have thermally accommodated to the inlet walls such as N2 and CH4. An open ion source allows direct beaming ions or chemically active neutral species such as N and HCN to be measured without surface interaction. The instrument can alternate between these three different modes. Characterization and calibration of each of these three modes is done using a low energy ion beam, a neutral molecular beam and a neutral thermal gas source. An onboard flight computer is used to control instrument operating parameters in accordance with pre-programmed sequences and to package the telemetry data. The sensor is sealed and maintained in a vacuum prior to launch to provide a clean environment for measurement of neutral species when it is opened to the ambient atmosphere after orbit insertion. The instrument is provided by NASA/Goddard Spaceflight Center, Code 915. Operation of the instrument and data analysis will be carried out by a Science Team.© (1996) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.

Published
1996
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14. Galileo Probe Mass Spectrometer experiment

Author

Sushil K. Atreya, Donald M. Hunten, Hasso B. Niemann, G. R. Carignan, D. N. Harpold, and Tobias Owen

Subjects
Atmosphere, Jupiter, Space and Planetary Science, Atmosphere of Jupiter, Analytical chemistry, Galileo Probe, Noble gas, Astronomy and Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Mass spectrometry, Quadrupole mass analyzer, Trace gas, Remote sensing
Abstract

The Galileo Probe Mass Spectrometer (GPMS) is a Probe instrument designed to measure the chemical and isotopic composition including vertical variations of the constituents in the atmosphere of Jupiter. The measurement will be performed by in situ sampling of the ambient atmosphere in the pressure range from approximately 150 mbar to 20 bar. In addition batch sampling will be performed for noble gas composition measurement and isotopic ratio determination and for sensitivity enhancement of non-reactive trace gases.

Published
1992
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16. Microfabricated silicon leak for sampling planetary atmospheres with a mass spectrometer

Author

M. D. Shappirio, B. G. Jamieson, B. A. Lynch, D. N. Harpold, Paul R. Mahaffy, and H. B. Niemann

Subjects
Silicon, Leak, Materials science, Planets, chemistry.chemical_element, Mass spectrometry, Sensitivity and Specificity, Mass Spectrometry, Optics, Etching (microfabrication), Instrumentation, Capillary Tubing, Miniaturization, business.industry, Reproducibility of Results, Conductance, Equipment Design, Semiconductor device, Space Flight, Equipment Failure Analysis, chemistry, Volume (thermodynamics), Flow Injection Analysis, Gases, business, Porosity, Environmental Monitoring
Abstract

A microfabricated silicon mass spectrometer inlet leak has been designed, fabricated, and tested. This leak achieves a much lower conductance in a smaller volume than is possible with commonly available metal or glass capillary tubing. It will also be shown that it is possible to integrate significant additional functionality, such as inlet heaters and valves, into a silicon microleak with very little additional mass. The fabricated leak is compatible with high temperature (up to 500 degrees C) and high pressure (up to 100 bars) conditions, as would be encountered on a Venus atmospheric probe. These leaks behave in reasonable agreement with their theoretically calculated conductance, although this differs between devices and from the predicted value by as much as a factor of 2. This variation is believed to be the result of nonuniformity in the silicon etching process which is characterized in this work. Future versions of this device can compensate for characterized process variations in order to produce devices in closer agreement with designed conductance values. The integration of an inlet heater into the leak device has also been demonstrated in this work.

Published
2007
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17. Horizontal distribution of helium in the Earth's upper atmosphere

Author

D. N. Harpold, A. E. Hedin, C. A. Reber, and R. Horowitz

Subjects
Atmospheric Science, Soil Science, chemistry.chemical_element, Aquatic Science, Oceanography, Spatial distribution, Atmospheric sciences, Atmosphere, Altitude, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Astrophysics::Solar and Stellar Astrophysics, Geomagnetic latitude, Nuclear Experiment, Physics::Atmospheric and Oceanic Physics, Helium, Earth-Surface Processes, Water Science and Technology, Physics, Ecology, Atmospheric models, Turbulence, Paleontology, Forestry, Geophysics, chemistry, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Thermosphere
Abstract

Horizontal He distribution in upper atmosphere from OGO 6 mass spectrometric data normalization for altitude by Jacchia model atmosphere

Published
1971
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18. The Planet-B neutral gas mass spectrometer

Author

S. Feng, H. J. Hayakawa, Siegfried Bauer, Naoji Sugiura, Tobias Owen, Stephen W. Bougher, Sushil K. Atreya, T. M. Donahue, Andrew F. Nagy, Donald M. Hunten, Yayoi N. Miura, Bruce P. Block, D. N. Harpold, T. Mukai, Hasso B. Niemann, S. H. Way, G. R. Carignan, and Wayne Kasprzak

Subjects
Geology, Mars Exploration Program, Atmosphere of Mars, Atomic mass unit, Computational physics, Atmosphere, Solar wind, Space and Planetary Science, Physics::Space Physics, Gas composition, Astrophysics::Earth and Planetary Astrophysics, Thermosphere, Quadrupole mass analyzer, Remote sensing
Abstract

著者人数：18名, Accepted：1998-06-04, 資料番号: SA1001219000

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