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A Stringent Upper Limit of 20 Pptv for Methane on Mars and Constraints on Its Dispersion Outside Gale Crater F
A&A 650, A140 (2021) Astronomy https://doi.org/10.1051/0004-6361/202140389 & © F. Montmessin et al. 2021 Astrophysics A stringent upper limit of 20 pptv for methane on Mars and constraints on its dispersion outside Gale crater F. Montmessin1 , O. I. Korablev2 , A. Trokhimovskiy2 , F. Lefèvre3 , A. A. Fedorova2 , L. Baggio1 , A. Irbah1 , G. Lacombe1, K. S. Olsen4 , A. S. Braude1 , D. A. Belyaev2 , J. Alday4 , F. Forget5 , F. Daerden6, J. Pla-Garcia7,8 , S. Rafkin8 , C. F. Wilson4, A. Patrakeev2, A. Shakun2, and J. L. Bertaux1 1 LATMOS/IPSL, UVSQ Université Paris-Saclay, Sorbonne Université, CNRS, Guyancourt, France e-mail: [email protected] 2 Space Research Institute (IKI) RAS, Moscow, Russia 3 LATMOS/IPSL, Sorbonne Université, UVSQ Université Paris-Saclay, CNRS, Paris, France 4 AOPP, Oxford University, Oxford, UK 5 Laboratoire de Météorologie Dynamique, Sorbonne Université, Paris, France 6 BIRA-IASB, Bruxelles, Belgium 7 Centro de Astrobiología (CSIC?INTA), Torrejón de Ardoz, Spain 8 Southwest Research Institute, Boulder, CO, USA Received 20 January 2021 / Accepted 23 April 2021 ABSTRACT Context. Reports on the detection of methane in the Martian atmosphere have motivated numerous studies aiming to confirm or explain its presence on a planet where it might imply a biogenic or more likely a geophysical origin. Aims. Our intent is to complement and improve on the previously reported detection attempts by the Atmospheric Chemistry Suite (ACS) on board the ExoMars Trace Gas Orbiter (TGO). This latter study reported the results of a campaign that was a few months in length, and was significantly hindered by a dusty period that impaired detection performances. -
General Index
General Index Italicized page numbers indicate figures and tables. Color plates are in- cussed; full listings of authors’ works as cited in this volume may be dicated as “pl.” Color plates 1– 40 are in part 1 and plates 41–80 are found in the bibliographical index. in part 2. Authors are listed only when their ideas or works are dis- Aa, Pieter van der (1659–1733), 1338 of military cartography, 971 934 –39; Genoa, 864 –65; Low Coun- Aa River, pl.61, 1523 of nautical charts, 1069, 1424 tries, 1257 Aachen, 1241 printing’s impact on, 607–8 of Dutch hamlets, 1264 Abate, Agostino, 857–58, 864 –65 role of sources in, 66 –67 ecclesiastical subdivisions in, 1090, 1091 Abbeys. See also Cartularies; Monasteries of Russian maps, 1873 of forests, 50 maps: property, 50–51; water system, 43 standards of, 7 German maps in context of, 1224, 1225 plans: juridical uses of, pl.61, 1523–24, studies of, 505–8, 1258 n.53 map consciousness in, 636, 661–62 1525; Wildmore Fen (in psalter), 43– 44 of surveys, 505–8, 708, 1435–36 maps in: cadastral (See Cadastral maps); Abbreviations, 1897, 1899 of town models, 489 central Italy, 909–15; characteristics of, Abreu, Lisuarte de, 1019 Acequia Imperial de Aragón, 507 874 –75, 880 –82; coloring of, 1499, Abruzzi River, 547, 570 Acerra, 951 1588; East-Central Europe, 1806, 1808; Absolutism, 831, 833, 835–36 Ackerman, James S., 427 n.2 England, 50 –51, 1595, 1599, 1603, See also Sovereigns and monarchs Aconcio, Jacopo (d. 1566), 1611 1615, 1629, 1720; France, 1497–1500, Abstraction Acosta, José de (1539–1600), 1235 1501; humanism linked to, 909–10; in- in bird’s-eye views, 688 Acquaviva, Andrea Matteo (d. -
Martian Crater Morphology
ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter. -
Aurora Crater (Updated 2015)
Site Description Aurora Crater (Updated 2015) Geologic setting: The Aurora Crater geothermal area is located in western Mineral County, northeast of Mono Lake. The geothermal area sits within an area known as the Aurora-Bodie volcanic field. The Bodie Hills are located to the west while the Wassuk Range is located to the east. The rocks in this region are composed of Calc-alkaline andesite, dacite and trachyandesite lavas, breccias and ashflow tuffs, deposited between 15 and 8 million years ago. These units are overlain by a series of younger alkaline- calcic cinder cone deposits and flows. Aurora Crater, located approximately 6 km southwest of the Aurora Crater geothermal area, is a 250,000 year old breached crater surrounded by lava flows. This region has been abundantly cut by faults and covered in ash from more recent eruptions from the Mono Craters to the southwest (Geologic Points of Interest by Activity – Volcanic Activity). Gold and silver deposits found in Miocene volcanic rocks were mined in both Bodie (CA) and Aurora (NV) until the 1950s (Geologic Points of Interest by Activity – Volcanic Activity). The Aurora District was the most productive mining district in Mineral County. Between 1861 and 1869, nearly $29,500,000 in gold and silver were produced from the Aurora mines (Ross, 1961). Geothermal features: A blind geothermal anomaly is reported between Aurora Crater and the Borealis open-pit gold mine 12 km northeast (Richards and Blackwell, 2002). The Aurora prospect consists of 29,000 acres in an area of Quaternary basaltic volcanism. Seventeen temperature gradient wells indicate a large geothermal anomaly. -
Experience of 80 Cases with Fournier's Gangrene and “Trauma” As a Trigger
ORIGINAL ARTICLE Experience of 80 cases with Fournier’s gangrene and “trauma” as a trigger factor in the etiopathogenesis Teoman Eskitaşcıoğlu, M.D., İrfan Özyazgan, M.D., Atilla Coruh, M.D., Galip K Günay, M.D., Mehmet Altıparmak, M.D., Yalcin Yontar, M.D., Fatih Doğan, M.D.† Department of Plastic Reconstructive and Aesthetic Surgery, Erciyes University Faculty of Medicine, Kayseri †Current affiliation: Department of Plastic Reconstructive and Aesthetic Surgery, Adıyaman University Faculty of Medicine, Adıyaman ABSTRACT BACKGROUND: The purpose of the present study was to retrospectively analyze the patients’ data presented with Fournier’s gangrene (FG), to compare obtained data with the literature and to investigate the role of “trauma” in the etiopathogenesis. METHODS: A retrospective study was conducted on 126 patients with FG that consulted to our department. RESULTS: There were 76 male and four female patients. The mean age of the patients was 53.5±13.6 years. The most common presentation of patients was swelling (n=74). The scrotum has been shown to be the most commonly affected area in the patients (n=75). Diabetes mellitus was the leading predisposing factor and trauma was the leading responsible cause for FG. Escherichia coli was the most frequently identified microorganism (n=43, 53.75%). Primary closure was the most common technique used for all patients. Three patients exhibited a mortal course due to sepsis and multi-organ failure. CONCLUSION: FG still has a high mortality rate. Rapid and correct diagnosis of the disease can avoid inappropriate or delayed treatment and even death of the patient. The healthcare professionals should be aware that any trauma in the perineal region could lead to FG. -
Pre-Mission Insights on the Interior of Mars Suzanne E
Pre-mission InSights on the Interior of Mars Suzanne E. Smrekar, Philippe Lognonné, Tilman Spohn, W. Bruce Banerdt, Doris Breuer, Ulrich Christensen, Véronique Dehant, Mélanie Drilleau, William Folkner, Nobuaki Fuji, et al. To cite this version: Suzanne E. Smrekar, Philippe Lognonné, Tilman Spohn, W. Bruce Banerdt, Doris Breuer, et al.. Pre-mission InSights on the Interior of Mars. Space Science Reviews, Springer Verlag, 2019, 215 (1), pp.1-72. 10.1007/s11214-018-0563-9. hal-01990798 HAL Id: hal-01990798 https://hal.archives-ouvertes.fr/hal-01990798 Submitted on 23 Jan 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Open Archive Toulouse Archive Ouverte (OATAO ) OATAO is an open access repository that collects the wor of some Toulouse researchers and ma es it freely available over the web where possible. This is an author's version published in: https://oatao.univ-toulouse.fr/21690 Official URL : https://doi.org/10.1007/s11214-018-0563-9 To cite this version : Smrekar, Suzanne E. and Lognonné, Philippe and Spohn, Tilman ,... [et al.]. Pre-mission InSights on the Interior of Mars. (2019) Space Science Reviews, 215 (1). -
Inferences of Martian Atmospheric Dust and Water Ice Content Derived from Radiative Transfer Models of Passive Msl Observations by Mastcam
44th Lunar and Planetary Science Conference (2013) 1288.pdf INFERENCES OF MARTIAN ATMOSPHERIC DUST AND WATER ICE CONTENT DERIVED FROM RADIATIVE TRANSFER MODELS OF PASSIVE MSL OBSERVATIONS BY MASTCAM. E. M. McCul- lough1, J. E. Moores 1,2, R. Francis1, and the MSL Science Team. 1Centre for Planetary Science and Exploration (The University of Western Ontario, London, ON, Canada, [email protected]), 2Now at: Centre for Research in Earth and Space Sciences (CRESS, York University, Toronto, ON, Canada). Introduction: While the Mars Science Laboratory cameras [3]. The 440 nm and 750 nm combination of (MSL) Spacecraft was not designed primarily as a ve- wavelengths was chosen because this ratio is the least hicle from which to study the martian atmosphere, the ambiguous for distinguishing ice from dust. recent landing of MSL's rover Curiosity has provided The MastCam's left and right cameras can be used opportunities to extend the science return of the exist- simultaneously to image the sky, with a 440 nm blue ing instrument complement to include observations of filter on the right camera and a 750 nm red filter on the atmospheric water ice and dust. left. Alternately, sequential images taken in both wave- The participating science project “Observations of lengths with a single camera (typically MastCam Left), Water Ice and Winds from the MSL Rover” [1], in- can be used. The latter is the simplest case with which cluded proposed atmospheric measurements using sev- to begin as many camera-specific parameters will be eral MSL imagers. To date, several such data products identical for the pair of images. -
Appendix I Lunar and Martian Nomenclature
APPENDIX I LUNAR AND MARTIAN NOMENCLATURE LUNAR AND MARTIAN NOMENCLATURE A large number of names of craters and other features on the Moon and Mars, were accepted by the IAU General Assemblies X (Moscow, 1958), XI (Berkeley, 1961), XII (Hamburg, 1964), XIV (Brighton, 1970), and XV (Sydney, 1973). The names were suggested by the appropriate IAU Commissions (16 and 17). In particular the Lunar names accepted at the XIVth and XVth General Assemblies were recommended by the 'Working Group on Lunar Nomenclature' under the Chairmanship of Dr D. H. Menzel. The Martian names were suggested by the 'Working Group on Martian Nomenclature' under the Chairmanship of Dr G. de Vaucouleurs. At the XVth General Assembly a new 'Working Group on Planetary System Nomenclature' was formed (Chairman: Dr P. M. Millman) comprising various Task Groups, one for each particular subject. For further references see: [AU Trans. X, 259-263, 1960; XIB, 236-238, 1962; Xlffi, 203-204, 1966; xnffi, 99-105, 1968; XIVB, 63, 129, 139, 1971; Space Sci. Rev. 12, 136-186, 1971. Because at the recent General Assemblies some small changes, or corrections, were made, the complete list of Lunar and Martian Topographic Features is published here. Table 1 Lunar Craters Abbe 58S,174E Balboa 19N,83W Abbot 6N,55E Baldet 54S, 151W Abel 34S,85E Balmer 20S,70E Abul Wafa 2N,ll7E Banachiewicz 5N,80E Adams 32S,69E Banting 26N,16E Aitken 17S,173E Barbier 248, 158E AI-Biruni 18N,93E Barnard 30S,86E Alden 24S, lllE Barringer 29S,151W Aldrin I.4N,22.1E Bartels 24N,90W Alekhin 68S,131W Becquerei -
Global Geometric Properties of Martian Impact Craters: a Preliminary Assessment Using Mars Orbiter Laser Altimeter (Mola)
GLOBAL GEOMETRIC PROPERTIES OF MARTIAN IMPACT CRATERS: A PRELIMINARY ASSESSMENT USING MARS ORBITER LASER ALTIMETER (MOLA). J. B. Garvin1, S. E. H. Sakimoto2, C. Schnetzler3, and J. J. Frawley4, 1(NASAÕs GSFC, Code 921, Greenbelt, MD 20771 USA; [email protected]), 2(USRA at NASAÕs GSFC, Code 921, Greenbelt, MD 20771), 3(SSAI at NASAÕs GSFC) 4(H-STX and Herring Bay Geophysics at NASAÕs GSFC). Introduction: Impact craters on Mars have been ÒshapeÓ (n), central peak height, diameter D, volume, used to provide fundamental insights into the proper- shape, and many others. In this report, we treat the ties of the martian crust, the role of volatiles, the rela- crater depth versus diameter relationship, the crater rim tive age of the surface, and on the physics of impact height vs. diameter pattern, the statistics of ejecta cratering in the Solar System [1,2,6]. Before the three- thickness and its spatial distribution, and cavity geo- dimensional information provided by the Mars Orbiter metric properties, including interior deposit geometry. Laser Altimeter (MOLA) instrument which is currently Crater depth vs. Diameter: Using MOLA topog- operating in Mars orbit aboard the Mars Global Sur- raphic profile data, we have computed the total depth veyor (MGS), impact features were characterized mor- (from rim crest to lowest point on crater cavity floor) phologically using orbital images from Mariner 9 and and true depth (i.e., from pre-impact surface to mean Viking. Fresh-appearing craters were identified and crater floor level) for over 1300 craters. When we exam- measurements of their geometric properties were de- ine the correlation of depth d against diameter D, a rived from various image-based methods [3,6]. -
Impact Craters) Into the Subsurface
SUBSURFACE MINERAL HETEROGENEITY IN THE MARTIAN CRUST AS SEEN BY THE THERMAL EMISSION IMAGING SYSTEM (THEMIS): VIEWS FROM NATURAL “WINDOWS” (IMPACT CRATERS) INTO THE SUBSURFACE. L. L. Tornabene1 , J. E. Moersch1, H. Y. McSween Jr.1, J. A. Piatek1 and P. R. Christensen2; 1Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, Tennessee 37996-1410, 2 Department of Geological Sciences, Arizona State University, Tempe, Arizona 85287–6305, USA. Introduction and Background: Impact craters have been effectively used as a “natural drill” into the crust of the moon, the Earth and on Mars, giving us a glimpse of the mineral and lithologic compositions that are otherwise not exposed or present on surfaces. A lunar study by Tomp- kins and Pieters [1] has demonstrated that Lunar Clementine data could be used to show that numerous craters on the Moon excavated distinct compositions within both the cen- tral uplift and craters walls/terraces of several complex cra- ters with respect to the surrounding lunar surface composi- tion. Later, Tornabene et al [2] demonstrated how Haughton impact structure was an excellent terrestrial analog for dem- onstrating the utility of using craters for studying both near- subsurface and the shallow crust of Mars. Using ASTER Thermal infrared (TIR) data, as an analog for THEMIS TIR, three subsurface units were distinguished within the structure as units that were excavated and uplifted by the impact event. These units, if not for the regional tilt and erosion, would otherwise not be presently exposed if not for the Haughton event. Meanwhile, recent studies on Mars by the Opportunity rover [3] revealed our first clear view of out- cropping bedrock of sedimentary layers within the walls of Eagle and Endurance craters. -
MARS ORBITAL DATA — METHODS and INTERPRETATION 6:30 P.M
Lunar and Planetary Science XXXIX (2008) sess614.pdf Thursday, March 13, 2008 POSTER SESSION II: MARS ORBITAL DATA — METHODS AND INTERPRETATION 6:30 p.m. Fitness Center Farrand W. H. Johnson J. R. Schmidt M. E. Bell J. F. III VNIR Spectral Differences on Natural and Brushed/Wind-abraded Surfaces on Home Plate, Gusev Crater, Mars: Spirit Pancam and HiRISE Color Observations [#1774] Color differences between the eastern and western rims of Home Plate are examined using Spirit Pancam and HiRISE color observations. Differences between near-field and remote observations are considered. Rice M. S. Bell J. F. III Wang A. Cloutis E. A. Vis-NIR Spectral Characterization of Si-rich Deposits at Gusev Crater, Mars [#2138] The Spirit rover has discovered high concentrations of silica at Gusev Crater, and a distinct spectral feature near 1000 nm appears to be diagnostic of these materials. We hypothesize that the presence of H2O or OH may be responsible for this feature. Combe J.-Ph. McCord T. B. Mars-Express/HRSC Spectral Data of MER Landing Sites Analyzed by a Multiple-Endmember Linear Spectral Linear Unmixing Model (MELSUM) [#2381] HRSC multispectral data are analyzed for mapping the main surface spectral components and photometric properties of Mars. The unique geometry of observation of this dataset is investigated. Results will be compared to field observations from the MERs. Hauber E. Gwinner K. Gendrin A. Fueten F. Stesky R. Pelkey S. Reiss D. Zegers T. E. MacKinnon P. Jaumann R. Bibring J.-P. Neukum G. Hebes Chasma, Mars: Slopes and Stratigraphy of Interior Layered Deposits [#2375] We present new data from HRSC and CTX on the topography, stratigraphy, and structure of Interior Layered Deposits in Hebes Chasma, Valles Marineris, Mars. -
Science-Centric Sampling Approaches of Geo-Physical Environments for Realistic Robot Navigation
SCIENCE-CENTRIC SAMPLING APPROACHES OF GEO-PHYSICAL ENVIRONMENTS FOR REALISTIC ROBOT NAVIGATION A Thesis Presented to The Academic Faculty by Lonnie T. Parker, IV In Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy in the School of Electrical and Computer Engineering Georgia Institute of Technology August 2012 Copyright c 2012 by Lonnie T. Parker, IV SCIENCE-CENTRIC SAMPLING APPROACHES OF GEO-PHYSICAL ENVIRONMENTS FOR REALISTIC ROBOT NAVIGATION Approved by: Professor Ayanna M. Howard, Advisor Professor Jeff Shamma School of Electrical and Computer School of Electrical and Computer Engineering Engineering Georgia Institute of Technology Georgia Institute of Technology Professor Fumin Zhang Professor Mike Stilman School of Electrical and Computer College of Computing Engineering Georgia Institute of Technology Georgia Institute of Technology Professor George Riley Date Approved: June 15, 2012 School of Electrical and Computer Engineering Georgia Institute of Technology DEDICATION Based upon the infallible word of God, I dedicate this work to Him, according to Proverbs 16:3. iii ACKNOWLEDGEMENTS Before anyone else, I want to acknowledge and thank my Lord and Savior, Jesus Christ, whom I am in and who lives within me. This degree and this experience would not be possible without His provision, favor, and grace. Especially in the moments when I did not believe it was possible to finish, my faith in Him pushed me forward. Next, to my wife, Andrea, who has been my constant encourager, supporter, and living reminder that I could complete this journey, thank you. Simply your presence in my life has made this walk all the more bearable. I love you.