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Searching Mass-Balance Analysis to Find the Composition of Martian Blueberries. MINERALS 2022. [DOI: 10.3390/min12060777] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
Between 2004 and 2018, NASA’s rover Opportunity found huge numbers of small, hematite-rich spherules (commonly called blueberries) on the Meridiani Planum of Mars. The standard oxide composition distributions of blueberries have remained poorly constrained, with previous published analyses leaving hematite content somewhere in the broad range of 24–100 wt%. A searching mass-balance analysis is introduced and applied to constrain possible standard oxide composition distributions of blueberries consistent with the non-detection of silicates in blueberries by Opportunity’s instruments. This analysis found three groups of complete solution sets among the mass-balance ions consistent with the non-detection of silicates; although, a simple extension of the analysis indicates that one larger space of solutions incorporates all three groups of solutions. Enforcing consistency with the non-detection of silicates in blueberries constrains the hematite content in most of blueberry samples to between 79.5 and 99.85 wt%. A feature of the largest group of complete solution sets is that five oxides/elements, MgO, P2O5, Na2O, SO3, and Cl, collectively have a summed weight percentage that averages close to 6 wt%, while the weight percentage of nickel is close to 0.3 wt% in all solutions. Searches over multidimensional spaces of filtering composition distributions of basaltic and dusty soils were a methodological advance.
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2
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Ruan T, Young RMB, Lewis SR, Montabone L, Valeanu A, Read PL. Assimilation of Both Column- and Layer-Integrated Dust Opacity Observations in the Martian Atmosphere. EARTH AND SPACE SCIENCE (HOBOKEN, N.J.) 2021; 8:e2021EA001869. [PMID: 35864913 PMCID: PMC9286790 DOI: 10.1029/2021ea001869] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 06/02/2021] [Revised: 11/10/2021] [Accepted: 11/30/2021] [Indexed: 06/15/2023]
Abstract
A new dust data assimilation scheme has been developed for the UK version of the Laboratoire de Météorologie Dynamique Martian General Circulation Model. The Analysis Correction scheme (adapted from the UK Met Office) is applied with active dust lifting and transport to analyze measurements of temperature, and both column-integrated dust optical depth (CIDO), τ ref (rescaled to a reference level), and layer-integrated dust opacity (LIDO). The results are shown to converge to the assimilated observations, but assimilating either of the dust observation types separately does not produce the best analysis. The most effective dust assimilation is found to require both CIDO (from Mars Odyssey/THEMIS) and LIDO observations, especially for Mars Climate Sounder data that does not access levels close to the surface. The resulting full reanalysis improves the agreement with both in-sample assimilated CIDO and LIDO data and independent observations from outside the assimilated data set. It is thus able to capture previously elusive details of the dust vertical distribution, including elevated detached dust layers that have not been captured in previous reanalyzes. Verification of this reanalysis has been carried out under both clear and dusty atmospheric conditions during Mars Years 28 and 29, using both in-sample and out of sample observations from orbital remote sensing and contemporaneous surface measurements of dust opacity from the Spirit and Opportunity landers. The reanalysis was also compared with a recent version of the Mars Climate Database (MCD v5), demonstrating generally good agreement though with some systematic differences in both time mean fields and day-to-day variability.
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Affiliation(s)
- Tao Ruan
- Department of PhysicsAtmospheric, Oceanic and Planetary PhysicsUniversity of OxfordClarendon LaboratoryOxfordUK
| | - R. M. B. Young
- Department of PhysicsAtmospheric, Oceanic and Planetary PhysicsUniversity of OxfordClarendon LaboratoryOxfordUK
- Department of Physics & National Space Science and Technology CenterUAE UniversityAl AinUnited Arab Emirates
| | - S. R. Lewis
- School of Physical SciencesThe Open UniversityMilton KeynesUK
| | - L. Montabone
- Department of PhysicsAtmospheric, Oceanic and Planetary PhysicsUniversity of OxfordClarendon LaboratoryOxfordUK
- Space Science InstituteBoulderCOUSA
| | - A. Valeanu
- Department of PhysicsAtmospheric, Oceanic and Planetary PhysicsUniversity of OxfordClarendon LaboratoryOxfordUK
| | - P. L. Read
- Department of PhysicsAtmospheric, Oceanic and Planetary PhysicsUniversity of OxfordClarendon LaboratoryOxfordUK
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3
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Recognition of Sedimentary Rock Occurrences in Satellite and Aerial Images of Other Worlds—Insights from Mars. REMOTE SENSING 2021. [DOI: 10.3390/rs13214296] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/31/2022]
Abstract
Sedimentary rocks provide records of past surface and subsurface processes and environments. The first step in the study of the sedimentary rock record of another world is to learn to recognize their occurrences in images from instruments aboard orbiting, flyby, or aerial platforms. For two decades, Mars has been known to have sedimentary rocks; however, planet-wide identification is incomplete. Global coverage at 0.25–6 m/pixel, and observations from the Curiosity rover in Gale crater, expand the ability to recognize Martian sedimentary rocks. No longer limited to cases that are light-toned, lightly cratered, and stratified—or mimic original depositional setting (e.g., lithified deltas)—Martian sedimentary rocks include dark-toned examples, as well as rocks that are erosion-resistant enough to retain small craters as well as do lava flows. Breakdown of conglomerates, breccias, and even some mudstones, can produce a pebbly regolith that imparts a “smooth” appearance in satellite and aerial images. Context is important; sedimentary rocks remain challenging to distinguish from primary igneous rocks in some cases. Detection of ultramafic, mafic, or andesitic compositions do not dictate that a rock is igneous, and clast genesis should be considered separately from the depositional record. Mars likely has much more sedimentary rock than previously recognized.
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Hobbs S, Lambert A, Ryan MJ, Paull DJ, Haythorpe J. Appraisal of Low-Cost Pushbroom Hyper-Spectral Sensor Systems for Material Classification in Reflectance. SENSORS (BASEL, SWITZERLAND) 2021; 21:4398. [PMID: 34199026 PMCID: PMC8271520 DOI: 10.3390/s21134398] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 05/18/2021] [Revised: 06/07/2021] [Accepted: 06/24/2021] [Indexed: 12/03/2022]
Abstract
Near infrared (NIR) remote sensing has applications in vegetation analysis as well as geological investigations. For extra-terrestrial applications, this is particularly relevant to Moon, Mars and asteroid exploration, where minerals exhibiting spectral phenomenology between 600 and 800 nm have been identified. Recent progress in the availability of processors and sensors has created the possibility of development of low-cost instruments able to return useful scientific results. In this work, two Raspberry Pi camera types and a panchromatic astronomy camera were trialed within a pushbroom sensor to determine their utility in measuring and processing the spectrum in reflectance. Algorithmic classification of all 15 test materials exhibiting spectral phenomenology between 600 and 800 nm was easily performed. Calibration against a spectrometer considers the effects of the sensor, inherent image processing pipeline and compression. It was found that even the color Raspberry Pi cameras that are popular with STEM applications were able to record and distinguish between most minerals and, contrary to expectations, exploited the infra-red secondary transmissions in the Bayer filter to gain a wider spectral range. Such a camera without a Bayer filter can markedly improve spectral sensitivity but may not be necessary.
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Affiliation(s)
- Steven Hobbs
- School of Engineering and Information Technology (SEIT), University of New South Wales Canberra, Northcott Drive, Canberra, ACT 2600, Australia;
| | - Andrew Lambert
- School of Engineering and Information Technology (SEIT), University of New South Wales Canberra, Northcott Drive, Canberra, ACT 2600, Australia;
| | - Michael J. Ryan
- Capability Associates Pty Ltd., Canberra, ACT 2600, Australia;
| | - David J. Paull
- School of Science, University of New South Wales Canberra, Northcott Drive, Canberra, ACT 2600, Australia;
| | - John Haythorpe
- Mars Society Australis, Clifton Hill, VIC 3068, Australia;
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5
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The Temporal Variation of Optical Depth in the Candidate Landing Area of China’s Mars Mission (Tianwen-1). REMOTE SENSING 2021. [DOI: 10.3390/rs13051029] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
Abstract
The atmospheric dust is an important factor in the evolution of the Martian climate and has a major impact on the scientific exploration of the Martian lander or rover and its payload. This paper used remote sensing images to calculate atmospheric optical depth that characterizes the spatial distribution of the atmospheric dust of Mars. The optical depth calculated by the images of the High Resolution Imaging Science Experiment (HiRISE) in the inspection area of the Spirit rover had a similar temporal variation to the optical depth directly measured by the Spirit rover from the sunlight decay. We also used the HiRISE images to acquire the seasonal variation of optical depths in the candidate landing area of China’s Mars Mission (Tianwen-1). The results have shown that the seasonal pattern of the optical depth in the candidate landing area is consistent with the dust storm sequences in this area. After Tianwen-1 enters the orbit around Mars, the images collected by the Moderate Resolution Imaging Camera (MoRIC), and the High Resolution Imaging Camera (HiRIC) can be used to study the atmospheric optical depth in the candidate landing area, providing reference for the safe landing and operation of the lander and rover.
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6
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Hayes AG, Corlies P, Tate C, Barrington M, Bell JF, Maki JN, Caplinger M, Ravine M, Kinch KM, Herkenhoff K, Horgan B, Johnson J, Lemmon M, Paar G, Rice MS, Jensen E, Kubacki TM, Cloutis E, Deen R, Ehlmann BL, Lakdawalla E, Sullivan R, Winhold A, Parkinson A, Bailey Z, van Beek J, Caballo-Perucha P, Cisneros E, Dixon D, Donaldson C, Jensen OB, Kuik J, Lapo K, Magee A, Merusi M, Mollerup J, Scudder N, Seeger C, Stanish E, Starr M, Thompson M, Turenne N, Winchell K. Pre-Flight Calibration of the Mars 2020 Rover Mastcam Zoom (Mastcam-Z) Multispectral, Stereoscopic Imager. SPACE SCIENCE REVIEWS 2021; 217:29. [PMID: 33678912 PMCID: PMC7892537 DOI: 10.1007/s11214-021-00795-x] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/22/2020] [Accepted: 01/12/2021] [Indexed: 05/28/2023]
Abstract
UNLABELLED The NASA Perseverance rover Mast Camera Zoom (Mastcam-Z) system is a pair of zoomable, focusable, multi-spectral, and color charge-coupled device (CCD) cameras mounted on top of a 1.7 m Remote Sensing Mast, along with associated electronics and two calibration targets. The cameras contain identical optical assemblies that can range in focal length from 26 mm ( 25.5 ∘ × 19.1 ∘ FOV ) to 110 mm ( 6.2 ∘ × 4.2 ∘ FOV ) and will acquire data at pixel scales of 148-540 μm at a range of 2 m and 7.4-27 cm at 1 km. The cameras are mounted on the rover's mast with a stereo baseline of 24.3 ± 0.1 cm and a toe-in angle of 1.17 ± 0.03 ∘ (per camera). Each camera uses a Kodak KAI-2020 CCD with 1600 × 1200 active pixels and an 8 position filter wheel that contains an IR-cutoff filter for color imaging through the detectors' Bayer-pattern filters, a neutral density (ND) solar filter for imaging the sun, and 6 narrow-band geology filters (16 total filters). An associated Digital Electronics Assembly provides command data interfaces to the rover, 11-to-8 bit companding, and JPEG compression capabilities. Herein, we describe pre-flight calibration of the Mastcam-Z instrument and characterize its radiometric and geometric behavior. Between April 26 t h and May 9 t h , 2019, ∼45,000 images were acquired during stand-alone calibration at Malin Space Science Systems (MSSS) in San Diego, CA. Additional data were acquired during Assembly Test and Launch Operations (ATLO) at the Jet Propulsion Laboratory and Kennedy Space Center. Results of the radiometric calibration validate a 5% absolute radiometric accuracy when using camera state parameters investigated during testing. When observing using camera state parameters not interrogated during calibration (e.g., non-canonical zoom positions), we conservatively estimate the absolute uncertainty to be < 10 % . Image quality, measured via the amplitude of the Modulation Transfer Function (MTF) at Nyquist sampling (0.35 line pairs per pixel), shows MTF Nyquist = 0.26 - 0.50 across all zoom, focus, and filter positions, exceeding the > 0.2 design requirement. We discuss lessons learned from calibration and suggest tactical strategies that will optimize the quality of science data acquired during operation at Mars. While most results matched expectations, some surprises were discovered, such as a strong wavelength and temperature dependence on the radiometric coefficients and a scene-dependent dynamic component to the zero-exposure bias frames. Calibration results and derived accuracies were validated using a Geoboard target consisting of well-characterized geologic samples. SUPPLEMENTARY INFORMATION The online version contains supplementary material available at 10.1007/s11214-021-00795-x.
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Affiliation(s)
- Alexander G. Hayes
- Department of Astronomy, Cornell University, Ithaca, NY 14850 USA
- Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY 14850 USA
| | - P. Corlies
- Department of Astronomy, Cornell University, Ithaca, NY 14850 USA
- Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139 USA
| | - C. Tate
- Department of Astronomy, Cornell University, Ithaca, NY 14850 USA
| | - M. Barrington
- Department of Astronomy, Cornell University, Ithaca, NY 14850 USA
| | - J. F. Bell
- School of Earth and Space Exploration, Arizona State University, Phoenix, AZ 85287 USA
| | - J. N. Maki
- Jet Propulsion Laboratory, Pasadena, CA 91109 USA
| | - M. Caplinger
- Malin Space Science Systems, San Diego, CA 92121 USA
| | - M. Ravine
- Malin Space Science Systems, San Diego, CA 92121 USA
| | - K. M. Kinch
- Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark
| | - K. Herkenhoff
- USGS Astrogeology Science Center, 2255 N. Gemini Drive, Flagstaff, AZ 86001 USA
| | - B. Horgan
- Earth, Atmospheric, and Planetary Sciences Department, Purdue University, West Lafayette, IN 47907 USA
| | - J. Johnson
- Johns Hopkins Applied Physics Laboratory, Laurel, MD 20723 USA
| | - M. Lemmon
- Space Science Institute, 4765 Walnut St., Suite B, Boulder, CO 80301 USA
| | - G. Paar
- Joanneum Research Forschungsgesellschaft mbH, Steyrergasse 17, 8010 Graz, Austria
| | - M. S. Rice
- Geology Department, Western Washington University, Bellingham, WA 98225 USA
| | - E. Jensen
- Malin Space Science Systems, San Diego, CA 92121 USA
| | - T. M. Kubacki
- Malin Space Science Systems, San Diego, CA 92121 USA
| | - E. Cloutis
- Geography Department, University of Winnepeg, 515 Portage Ave, Winnipeg, MB R3B 2E9 Canada
| | - R. Deen
- Jet Propulsion Laboratory, Pasadena, CA 91109 USA
| | - B. L. Ehlmann
- Jet Propulsion Laboratory, Pasadena, CA 91109 USA
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91101 USA
| | - E. Lakdawalla
- The Planetary Society, 60 S Los Robles, Pasadena, CA 91101 USA
| | - R. Sullivan
- Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY 14850 USA
| | - A. Winhold
- School of Earth and Space Exploration, Arizona State University, Phoenix, AZ 85287 USA
| | - A. Parkinson
- Centre for Terrestrial and Planetary Exploration, University of Winnipeg, 515 Portage Ave, Winnipeg, MB R3B 2E9 Canada
| | - Z. Bailey
- Jet Propulsion Laboratory, Pasadena, CA 91109 USA
| | - J. van Beek
- Jet Propulsion Laboratory, Pasadena, CA 91109 USA
| | - P. Caballo-Perucha
- Joanneum Research Forschungsgesellschaft mbH, Steyrergasse 17, 8010 Graz, Austria
| | - E. Cisneros
- School of Earth and Space Exploration, Arizona State University, Phoenix, AZ 85287 USA
| | - D. Dixon
- Malin Space Science Systems, San Diego, CA 92121 USA
| | - C. Donaldson
- Malin Space Science Systems, San Diego, CA 92121 USA
| | - O. B. Jensen
- Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark
| | - J. Kuik
- Centre for Terrestrial and Planetary Exploration, University of Winnipeg, 515 Portage Ave, Winnipeg, MB R3B 2E9 Canada
| | - K. Lapo
- Geology Department, Western Washington University, Bellingham, WA 98225 USA
| | - A. Magee
- Malin Space Science Systems, San Diego, CA 92121 USA
| | - M. Merusi
- Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark
| | - J. Mollerup
- Geology Department, Western Washington University, Bellingham, WA 98225 USA
| | - N. Scudder
- Earth, Atmospheric, and Planetary Sciences Department, Purdue University, West Lafayette, IN 47907 USA
| | - C. Seeger
- Geology Department, Western Washington University, Bellingham, WA 98225 USA
| | - E. Stanish
- Centre for Terrestrial and Planetary Exploration, University of Winnipeg, 515 Portage Ave, Winnipeg, MB R3B 2E9 Canada
| | - M. Starr
- Malin Space Science Systems, San Diego, CA 92121 USA
| | - M. Thompson
- Jet Propulsion Laboratory, Pasadena, CA 91109 USA
| | - N. Turenne
- Centre for Terrestrial and Planetary Exploration, University of Winnipeg, 515 Portage Ave, Winnipeg, MB R3B 2E9 Canada
| | - K. Winchell
- Malin Space Science Systems, San Diego, CA 92121 USA
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7
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Wiens RC, Maurice S, Robinson SH, Nelson AE, Cais P, Bernardi P, Newell RT, Clegg S, Sharma SK, Storms S, Deming J, Beckman D, Ollila AM, Gasnault O, Anderson RB, André Y, Michael Angel S, Arana G, Auden E, Beck P, Becker J, Benzerara K, Bernard S, Beyssac O, Borges L, Bousquet B, Boyd K, Caffrey M, Carlson J, Castro K, Celis J, Chide B, Clark K, Cloutis E, Cordoba EC, Cousin A, Dale M, Deflores L, Delapp D, Deleuze M, Dirmyer M, Donny C, Dromart G, George Duran M, Egan M, Ervin J, Fabre C, Fau A, Fischer W, Forni O, Fouchet T, Fresquez R, Frydenvang J, Gasway D, Gontijo I, Grotzinger J, Jacob X, Jacquinod S, Johnson JR, Klisiewicz RA, Lake J, Lanza N, Laserna J, Lasue J, Le Mouélic S, Legett C, Leveille R, Lewin E, Lopez-Reyes G, Lorenz R, Lorigny E, Love SP, Lucero B, Madariaga JM, Madsen M, Madsen S, Mangold N, Manrique JA, Martinez JP, Martinez-Frias J, McCabe KP, McConnochie TH, McGlown JM, McLennan SM, Melikechi N, Meslin PY, Michel JM, Mimoun D, Misra A, Montagnac G, Montmessin F, Mousset V, Murdoch N, Newsom H, Ott LA, Ousnamer ZR, Pares L, Parot Y, Pawluczyk R, Glen Peterson C, Pilleri P, Pinet P, Pont G, Poulet F, Provost C, Quertier B, Quinn H, Rapin W, Reess JM, Regan AH, Reyes-Newell AL, Romano PJ, Royer C, Rull F, Sandoval B, Sarrao JH, Sautter V, Schoppers MJ, Schröder S, Seitz D, Shepherd T, Sobron P, Dubois B, Sridhar V, Toplis MJ, Torre-Fdez I, Trettel IA, Underwood M, Valdez A, Valdez J, Venhaus D, Willis P. The SuperCam Instrument Suite on the NASA Mars 2020 Rover: Body Unit and Combined System Tests. SPACE SCIENCE REVIEWS 2021; 217:4. [PMID: 33380752 PMCID: PMC7752893 DOI: 10.1007/s11214-020-00777-5] [Citation(s) in RCA: 26] [Impact Index Per Article: 8.7] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/16/2020] [Accepted: 11/27/2020] [Indexed: 05/16/2023]
Abstract
The SuperCam instrument suite provides the Mars 2020 rover, Perseverance, with a number of versatile remote-sensing techniques that can be used at long distance as well as within the robotic-arm workspace. These include laser-induced breakdown spectroscopy (LIBS), remote time-resolved Raman and luminescence spectroscopies, and visible and infrared (VISIR; separately referred to as VIS and IR) reflectance spectroscopy. A remote micro-imager (RMI) provides high-resolution color context imaging, and a microphone can be used as a stand-alone tool for environmental studies or to determine physical properties of rocks and soils from shock waves of laser-produced plasmas. SuperCam is built in three parts: The mast unit (MU), consisting of the laser, telescope, RMI, IR spectrometer, and associated electronics, is described in a companion paper. The on-board calibration targets are described in another companion paper. Here we describe SuperCam's body unit (BU) and testing of the integrated instrument. The BU, mounted inside the rover body, receives light from the MU via a 5.8 m optical fiber. The light is split into three wavelength bands by a demultiplexer, and is routed via fiber bundles to three optical spectrometers, two of which (UV and violet; 245-340 and 385-465 nm) are crossed Czerny-Turner reflection spectrometers, nearly identical to their counterparts on ChemCam. The third is a high-efficiency transmission spectrometer containing an optical intensifier capable of gating exposures to 100 ns or longer, with variable delay times relative to the laser pulse. This spectrometer covers 535-853 nm ( 105 - 7070 cm - 1 Raman shift relative to the 532 nm green laser beam) with 12 cm - 1 full-width at half-maximum peak resolution in the Raman fingerprint region. The BU electronics boards interface with the rover and control the instrument, returning data to the rover. Thermal systems maintain a warm temperature during cruise to Mars to avoid contamination on the optics, and cool the detectors during operations on Mars. Results obtained with the integrated instrument demonstrate its capabilities for LIBS, for which a library of 332 standards was developed. Examples of Raman and VISIR spectroscopy are shown, demonstrating clear mineral identification with both techniques. Luminescence spectra demonstrate the utility of having both spectral and temporal dimensions. Finally, RMI and microphone tests on the rover demonstrate the capabilities of these subsystems as well.
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Affiliation(s)
| | - Sylvestre Maurice
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse, UPS, CNRS, Toulouse, France
| | | | | | - Philippe Cais
- Laboratoire d’astrophysique de Bordeaux, Univ. Bordeaux, CNRS, Bordeaux, France
| | - Pernelle Bernardi
- Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Meudon, France
| | | | - Sam Clegg
- Los Alamos National Laboratory, Los Alamos, NM USA
| | | | | | | | | | | | - Olivier Gasnault
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse, UPS, CNRS, Toulouse, France
| | - Ryan B. Anderson
- U.S. Geological Survey Astrogeology Science Center, Flagstaff, AZ USA
| | - Yves André
- Centre National d’Etudes Spatiales, Toulouse, France
| | | | - Gorka Arana
- University of Basque Country, UPV/EHU, Bilbao, Spain
| | | | - Pierre Beck
- Institut de Planétologie et d’Astrophysique de Grenoble, Université Grenoble Alpes, Grenoble, France
| | | | - Karim Benzerara
- Institut de Minéralogie, Physique des Matériaux et Cosmochimie, CNRS, Museum National d’Histoire Naturelle, Sorbonne Université, Paris, France
| | - Sylvain Bernard
- Institut de Minéralogie, Physique des Matériaux et Cosmochimie, CNRS, Museum National d’Histoire Naturelle, Sorbonne Université, Paris, France
| | - Olivier Beyssac
- Institut de Minéralogie, Physique des Matériaux et Cosmochimie, CNRS, Museum National d’Histoire Naturelle, Sorbonne Université, Paris, France
| | - Louis Borges
- Los Alamos National Laboratory, Los Alamos, NM USA
| | - Bruno Bousquet
- Centre Lasers Intenses et Applications, University of Bordeaux, Bordeaux, France
| | - Kerry Boyd
- Los Alamos National Laboratory, Los Alamos, NM USA
| | | | | | - Kepa Castro
- University of Basque Country, UPV/EHU, Bilbao, Spain
| | - Jorden Celis
- Los Alamos National Laboratory, Los Alamos, NM USA
| | - Baptiste Chide
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse, UPS, CNRS, Toulouse, France
- Institut Supérieur de l’Aéronautique et de l’Espace (ISAE), Toulouse, France
| | - Kevin Clark
- Jet Propulsion Laboratory/Caltech, Pasadena, CA USA
| | | | | | - Agnes Cousin
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse, UPS, CNRS, Toulouse, France
| | | | | | | | | | | | | | - Gilles Dromart
- Univ Lyon, ENSL, Univ Lyon 1, CNRS, LGL-TPE, 69364 Lyon, France
| | | | | | - Joan Ervin
- Jet Propulsion Laboratory/Caltech, Pasadena, CA USA
| | - Cecile Fabre
- GeoRessources, Université de Lorraine, Nancy, France
| | - Amaury Fau
- Institut de Minéralogie, Physique des Matériaux et Cosmochimie, CNRS, Museum National d’Histoire Naturelle, Sorbonne Université, Paris, France
| | | | - Olivier Forni
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse, UPS, CNRS, Toulouse, France
| | - Thierry Fouchet
- Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Meudon, France
| | | | | | | | | | | | - Xavier Jacob
- Institut de mécanique des fluides de Toulouse (CNRS, INP, Univ. Toulouse), Toulouse, France
| | - Sophie Jacquinod
- Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Meudon, France
| | | | | | - James Lake
- Los Alamos National Laboratory, Los Alamos, NM USA
| | - Nina Lanza
- Los Alamos National Laboratory, Los Alamos, NM USA
| | | | - Jeremie Lasue
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse, UPS, CNRS, Toulouse, France
| | - Stéphane Le Mouélic
- Laboratoire de Planétologie et Géodynamique, Université de Nantes, Université d’Angers, CNRS UMR 6112, Nantes, France
| | - Carey Legett
- Los Alamos National Laboratory, Los Alamos, NM USA
| | | | - Eric Lewin
- Institut de Planétologie et d’Astrophysique de Grenoble, Université Grenoble Alpes, Grenoble, France
| | | | - Ralph Lorenz
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - Eric Lorigny
- Centre National d’Etudes Spatiales, Toulouse, France
| | | | | | | | | | - Soren Madsen
- Jet Propulsion Laboratory/Caltech, Pasadena, CA USA
| | - Nicolas Mangold
- Laboratoire de Planétologie et Géodynamique, Université de Nantes, Université d’Angers, CNRS UMR 6112, Nantes, France
| | | | | | | | | | | | | | | | | | - Pierre-Yves Meslin
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse, UPS, CNRS, Toulouse, France
| | | | - David Mimoun
- Institut Supérieur de l’Aéronautique et de l’Espace (ISAE), Toulouse, France
| | | | | | - Franck Montmessin
- Laboratoire Atmosphères, Milieux, Observations Spatiales, Paris, France
| | | | - Naomi Murdoch
- Institut Supérieur de l’Aéronautique et de l’Espace (ISAE), Toulouse, France
| | | | - Logan A. Ott
- Los Alamos National Laboratory, Los Alamos, NM USA
| | | | - Laurent Pares
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse, UPS, CNRS, Toulouse, France
| | - Yann Parot
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse, UPS, CNRS, Toulouse, France
| | | | | | - Paolo Pilleri
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse, UPS, CNRS, Toulouse, France
| | - Patrick Pinet
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse, UPS, CNRS, Toulouse, France
| | - Gabriel Pont
- Centre National d’Etudes Spatiales, Toulouse, France
| | | | | | - Benjamin Quertier
- Laboratoire d’astrophysique de Bordeaux, Univ. Bordeaux, CNRS, Bordeaux, France
| | | | - William Rapin
- Institut de Minéralogie, Physique des Matériaux et Cosmochimie, CNRS, Museum National d’Histoire Naturelle, Sorbonne Université, Paris, France
| | - Jean-Michel Reess
- Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Meudon, France
| | - Amy H. Regan
- Los Alamos National Laboratory, Los Alamos, NM USA
| | | | | | - Clement Royer
- Institut d’Astrophysique Spatiale (IAS), Orsay, France
| | | | | | | | - Violaine Sautter
- Institut de Minéralogie, Physique des Matériaux et Cosmochimie, CNRS, Museum National d’Histoire Naturelle, Sorbonne Université, Paris, France
| | | | - Susanne Schröder
- Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany
| | - Daniel Seitz
- Los Alamos National Laboratory, Los Alamos, NM USA
| | | | | | - Bruno Dubois
- Université de Toulouse; UPS-OMP, Toulouse, France
| | | | - Michael J. Toplis
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse, UPS, CNRS, Toulouse, France
| | | | | | | | | | - Jacob Valdez
- Los Alamos National Laboratory, Los Alamos, NM USA
| | - Dawn Venhaus
- Los Alamos National Laboratory, Los Alamos, NM USA
| | - Peter Willis
- Jet Propulsion Laboratory/Caltech, Pasadena, CA USA
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8
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Rodriguez-Manfredi JA, de la Torre Juárez M, Alonso A, Apéstigue V, Arruego I, Atienza T, Banfield D, Boland J, Carrera MA, Castañer L, Ceballos J, Chen-Chen H, Cobos A, Conrad PG, Cordoba E, del Río-Gaztelurrutia T, de Vicente-Retortillo A, Domínguez-Pumar M, Espejo S, Fairen AG, Fernández-Palma A, Ferrándiz R, Ferri F, Fischer E, García-Manchado A, García-Villadangos M, Genzer M, Giménez S, Gómez-Elvira J, Gómez F, Guzewich SD, Harri AM, Hernández CD, Hieta M, Hueso R, Jaakonaho I, Jiménez JJ, Jiménez V, Larman A, Leiter R, Lepinette A, Lemmon MT, López G, Madsen SN, Mäkinen T, Marín M, Martín-Soler J, Martínez G, Molina A, Mora-Sotomayor L, Moreno-Álvarez JF, Navarro S, Newman CE, Ortega C, Parrondo MC, Peinado V, Peña A, Pérez-Grande I, Pérez-Hoyos S, Pla-García J, Polkko J, Postigo M, Prieto-Ballesteros O, Rafkin SCR, Ramos M, Richardson MI, Romeral J, Romero C, Runyon KD, Saiz-Lopez A, Sánchez-Lavega A, Sard I, Schofield JT, Sebastian E, Smith MD, Sullivan RJ, Tamppari LK, Thompson AD, Toledo D, Torrero F, Torres J, Urquí R, Velasco T, Viúdez-Moreiras D, Zurita S. The Mars Environmental Dynamics Analyzer, MEDA. A Suite of Environmental Sensors for the Mars 2020 Mission. SPACE SCIENCE REVIEWS 2021; 217:48. [PMID: 34776548 PMCID: PMC8550605 DOI: 10.1007/s11214-021-00816-9] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 03/08/2021] [Indexed: 05/16/2023]
Abstract
NASA's Mars 2020 (M2020) rover mission includes a suite of sensors to monitor current environmental conditions near the surface of Mars and to constrain bulk aerosol properties from changes in atmospheric radiation at the surface. The Mars Environmental Dynamics Analyzer (MEDA) consists of a set of meteorological sensors including wind sensor, a barometer, a relative humidity sensor, a set of 5 thermocouples to measure atmospheric temperature at ∼1.5 m and ∼0.5 m above the surface, a set of thermopiles to characterize the thermal IR brightness temperatures of the surface and the lower atmosphere. MEDA adds a radiation and dust sensor to monitor the optical atmospheric properties that can be used to infer bulk aerosol physical properties such as particle size distribution, non-sphericity, and concentration. The MEDA package and its scientific purpose are described in this document as well as how it responded to the calibration tests and how it helps prepare for the human exploration of Mars. A comparison is also presented to previous environmental monitoring payloads landed on Mars on the Viking, Pathfinder, Phoenix, MSL, and InSight spacecraft.
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Affiliation(s)
| | | | | | - V. Apéstigue
- Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain
| | - I. Arruego
- Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain
| | - T. Atienza
- Universidad Politécnica de Cataluña, Barcelona, Spain
| | - D. Banfield
- Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY USA
| | - J. Boland
- Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA
| | | | - L. Castañer
- Universidad Politécnica de Cataluña, Barcelona, Spain
| | - J. Ceballos
- Instituto de Microelectrónica de Sevilla (US-CSIC), Seville, Spain
| | - H. Chen-Chen
- Universidad del País Vasco (UPV/EHU), Bilbao, Spain
| | - A. Cobos
- CRISA-Airbus, Tres Cantos, Spain
| | | | - E. Cordoba
- Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA
| | | | | | | | - S. Espejo
- Instituto de Microelectrónica de Sevilla (US-CSIC), Seville, Spain
| | - A. G. Fairen
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | | | - R. Ferrándiz
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | - F. Ferri
- Università degli Studi di Padova, Padova, Italy
| | - E. Fischer
- University of Michigan, Ann Arbor, MI USA
| | | | | | - M. Genzer
- Finnish Meteorological Institute, Helsinki, Finland
| | - S. Giménez
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | - J. Gómez-Elvira
- Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain
| | - F. Gómez
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | | | - A.-M. Harri
- Finnish Meteorological Institute, Helsinki, Finland
| | - C. D. Hernández
- Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA
| | - M. Hieta
- Finnish Meteorological Institute, Helsinki, Finland
| | - R. Hueso
- Universidad del País Vasco (UPV/EHU), Bilbao, Spain
| | - I. Jaakonaho
- Finnish Meteorological Institute, Helsinki, Finland
| | - J. J. Jiménez
- Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain
| | - V. Jiménez
- Universidad Politécnica de Cataluña, Barcelona, Spain
| | - A. Larman
- Added-Value-Solutions, Elgoibar, Spain
| | - R. Leiter
- Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA
| | - A. Lepinette
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | | | - G. López
- Universidad Politécnica de Cataluña, Barcelona, Spain
| | - S. N. Madsen
- Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA
| | - T. Mäkinen
- Finnish Meteorological Institute, Helsinki, Finland
| | - M. Marín
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | | | - G. Martínez
- Lunar and Planetary Institute, Houston, TX USA
| | - A. Molina
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | | | | | - S. Navarro
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | | | - C. Ortega
- Added-Value-Solutions, Elgoibar, Spain
| | - M. C. Parrondo
- Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain
| | - V. Peinado
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | - A. Peña
- CRISA-Airbus, Tres Cantos, Spain
| | | | | | | | - J. Polkko
- Finnish Meteorological Institute, Helsinki, Finland
| | - M. Postigo
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | | | | | - M. Ramos
- Universidad de Alcalá, Alcalá de Henares, Spain
| | | | - J. Romeral
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | - C. Romero
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | | | - A. Saiz-Lopez
- Dept. of Atmospheric Chemistry and Climate, Institute of Physical Chemistry Rocasolano, CSIC, Madrid, Spain
| | | | - I. Sard
- Added-Value-Solutions, Elgoibar, Spain
| | - J. T. Schofield
- Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA
| | - E. Sebastian
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | - M. D. Smith
- NASA Goddard Space Flight Center, Greenbelt, MD USA
| | - R. J. Sullivan
- Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY USA
| | - L. K. Tamppari
- Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA
| | - A. D. Thompson
- Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA
| | - D. Toledo
- Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain
| | | | - J. Torres
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | - R. Urquí
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | | | | | - S. Zurita
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
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9
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Bell JF, Maki JN, Mehall GL, Ravine MA, Caplinger MA, Bailey ZJ, Brylow S, Schaffner JA, Kinch KM, Madsen MB, Winhold A, Hayes AG, Corlies P, Tate C, Barrington M, Cisneros E, Jensen E, Paris K, Crawford K, Rojas C, Mehall L, Joseph J, Proton JB, Cluff N, Deen RG, Betts B, Cloutis E, Coates AJ, Colaprete A, Edgett KS, Ehlmann BL, Fagents S, Grotzinger JP, Hardgrove C, Herkenhoff KE, Horgan B, Jaumann R, Johnson JR, Lemmon M, Paar G, Caballo-Perucha M, Gupta S, Traxler C, Preusker F, Rice MS, Robinson MS, Schmitz N, Sullivan R, Wolff MJ. The Mars 2020 Perseverance Rover Mast Camera Zoom (Mastcam-Z) Multispectral, Stereoscopic Imaging Investigation. SPACE SCIENCE REVIEWS 2021; 217:24. [PMID: 33612866 PMCID: PMC7883548 DOI: 10.1007/s11214-020-00755-x] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/22/2020] [Accepted: 09/25/2020] [Indexed: 05/16/2023]
Abstract
Mastcam-Z is a multispectral, stereoscopic imaging investigation on the Mars 2020 mission's Perseverance rover. Mastcam-Z consists of a pair of focusable, 4:1 zoomable cameras that provide broadband red/green/blue and narrowband 400-1000 nm color imaging with fields of view from 25.6° × 19.2° (26 mm focal length at 283 μrad/pixel) to 6.2° × 4.6° (110 mm focal length at 67.4 μrad/pixel). The cameras can resolve (≥ 5 pixels) ∼0.7 mm features at 2 m and ∼3.3 cm features at 100 m distance. Mastcam-Z shares significant heritage with the Mastcam instruments on the Mars Science Laboratory Curiosity rover. Each Mastcam-Z camera consists of zoom, focus, and filter wheel mechanisms and a 1648 × 1214 pixel charge-coupled device detector and electronics. The two Mastcam-Z cameras are mounted with a 24.4 cm stereo baseline and 2.3° total toe-in on a camera plate ∼2 m above the surface on the rover's Remote Sensing Mast, which provides azimuth and elevation actuation. A separate digital electronics assembly inside the rover provides power, data processing and storage, and the interface to the rover computer. Primary and secondary Mastcam-Z calibration targets mounted on the rover top deck enable tactical reflectance calibration. Mastcam-Z multispectral, stereo, and panoramic images will be used to provide detailed morphology, topography, and geologic context along the rover's traverse; constrain mineralogic, photometric, and physical properties of surface materials; monitor and characterize atmospheric and astronomical phenomena; and document the rover's sample extraction and caching locations. Mastcam-Z images will also provide key engineering information to support sample selection and other rover driving and tool/instrument operations decisions.
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Affiliation(s)
| | | | | | - M. A. Ravine
- Malin Space Science Systems, Inc., San Diego, CA USA
| | | | | | - S. Brylow
- Malin Space Science Systems, Inc., San Diego, CA USA
| | | | | | | | | | | | | | - C. Tate
- Cornell Univ., Ithaca, NY USA
| | | | | | - E. Jensen
- Malin Space Science Systems, Inc., San Diego, CA USA
| | - K. Paris
- Arizona State Univ., Tempe, AZ USA
| | | | - C. Rojas
- Arizona State Univ., Tempe, AZ USA
| | | | | | | | - N. Cluff
- Arizona State Univ., Tempe, AZ USA
| | | | - B. Betts
- The Planetary Society, Pasadena, CA USA
| | | | - A. J. Coates
- Mullard Space Science Laboratory, Univ. College, London, UK
| | - A. Colaprete
- NASA/Ames Research Center, Moffett Field, CA USA
| | - K. S. Edgett
- Malin Space Science Systems, Inc., San Diego, CA USA
| | - B. L. Ehlmann
- JPL/Caltech, Pasadena, CA USA
- Caltech, Pasadena, CA USA
| | | | | | | | | | | | - R. Jaumann
- Inst. of Geological Sciences, Free University Berlin, Berlin, Germany
| | | | - M. Lemmon
- Space Science Inst., Boulder, CO USA
| | - G. Paar
- Joanneum Research, Graz, Austria
| | | | | | | | - F. Preusker
- DLR/German Aerospace Center, Berlin, Germany
| | - M. S. Rice
- Western Washington Univ., Bellingham, WA USA
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10
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Maki JN, Gruel D, McKinney C, Ravine MA, Morales M, Lee D, Willson R, Copley-Woods D, Valvo M, Goodsall T, McGuire J, Sellar RG, Schaffner JA, Caplinger MA, Shamah JM, Johnson AE, Ansari H, Singh K, Litwin T, Deen R, Culver A, Ruoff N, Petrizzo D, Kessler D, Basset C, Estlin T, Alibay F, Nelessen A, Algermissen S. The Mars 2020 Engineering Cameras and Microphone on the Perseverance Rover: A Next-Generation Imaging System for Mars Exploration. SPACE SCIENCE REVIEWS 2020; 216:137. [PMID: 33268910 PMCID: PMC7686239 DOI: 10.1007/s11214-020-00765-9] [Citation(s) in RCA: 12] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/08/2020] [Accepted: 11/09/2020] [Indexed: 05/16/2023]
Abstract
The Mars 2020 Perseverance rover is equipped with a next-generation engineering camera imaging system that represents an upgrade over previous Mars rover missions. These upgrades will improve the operational capabilities of the rover with an emphasis on drive planning, robotic arm operation, instrument operations, sample caching activities, and documentation of key events during entry, descent, and landing (EDL). There are a total of 16 cameras in the Perseverance engineering imaging system, including 9 cameras for surface operations and 7 cameras for EDL documentation. There are 3 types of cameras designed for surface operations: Navigation cameras (Navcams, quantity 2), Hazard Avoidance Cameras (Hazcams, quantity 6), and Cachecam (quantity 1). The Navcams will acquire color stereo images of the surface with a 96 ∘ × 73 ∘ field of view at 0.33 mrad/pixel. The Hazcams will acquire color stereo images of the surface with a 136 ∘ × 102 ∘ at 0.46 mrad/pixel. The Cachecam, a new camera type, will acquire images of Martian material inside the sample tubes during caching operations at a spatial scale of 12.5 microns/pixel. There are 5 types of EDL documentation cameras: The Parachute Uplook Cameras (PUCs, quantity 3), the Descent stage Downlook Camera (DDC, quantity 1), the Rover Uplook Camera (RUC, quantity 1), the Rover Descent Camera (RDC, quantity 1), and the Lander Vision System (LVS) Camera (LCAM, quantity 1). The PUCs are mounted on the parachute support structure and will acquire video of the parachute deployment event as part of a system to characterize parachute performance. The DDC is attached to the descent stage and pointed downward, it will characterize vehicle dynamics by capturing video of the rover as it descends from the skycrane. The rover-mounted RUC, attached to the rover and looking upward, will capture similar video of the skycrane from the vantage point of the rover and will also acquire video of the descent stage flyaway event. The RDC, attached to the rover and looking downward, will document plume dynamics by imaging the Martian surface before, during, and after rover touchdown. The LCAM, mounted to the bottom of the rover chassis and pointed downward, will acquire 90 ∘ × 90 ∘ FOV images during the parachute descent phase of EDL as input to an onboard map localization by the Lander Vision System (LVS). The rover also carries a microphone, mounted externally on the rover chassis, to capture acoustic signatures during and after EDL. The Perseverance rover launched from Earth on July 30th, 2020, and touchdown on Mars is scheduled for February 18th, 2021.
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Affiliation(s)
- J. N. Maki
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - D. Gruel
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - C. McKinney
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | | | - M. Morales
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - D. Lee
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - R. Willson
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - D. Copley-Woods
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - M. Valvo
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - T. Goodsall
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - J. McGuire
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - R. G. Sellar
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | | | | | | | - A. E. Johnson
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - H. Ansari
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - K. Singh
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - T. Litwin
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - R. Deen
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - A. Culver
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - N. Ruoff
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - D. Petrizzo
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - D. Kessler
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - C. Basset
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - T. Estlin
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - F. Alibay
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - A. Nelessen
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - S. Algermissen
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
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11
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Fraeman AA, Johnson JR, Arvidson RE, Rice MS, Wellington DF, Morris RV, Fox VK, Horgan BHN, Jacob SR, Salvatore MR, Sun VZ, Pinet P, Bell JF, Wiens RC, Vasavada AR. Synergistic Ground and Orbital Observations of Iron Oxides on Mt. Sharp and Vera Rubin Ridge. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2020; 125:e2019JE006294. [PMID: 33042722 PMCID: PMC7539960 DOI: 10.1029/2019je006294] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/26/2019] [Revised: 07/21/2020] [Accepted: 07/23/2020] [Indexed: 05/04/2023]
Abstract
Visible/short-wave infrared spectral data from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) show absorptions attributed to hematite at Vera Rubin ridge (VRR), a topographic feature on northwest Mt. Sharp. The goals of this study are to determine why absorptions caused by ferric iron are strongly visible from orbit at VRR and to improve interpretation of CRISM data throughout lower Mt. Sharp. These goals are achieved by analyzing coordinated CRISM and in situ spectral data along the Curiosity Mars rover's traverse. VRR bedrock within areas that have the deepest ferric absorptions in CRISM data also has the deepest ferric absorptions measured in situ. This suggests strong ferric absorptions are visible from orbit at VRR because of the unique spectral properties of VRR bedrock. Dust and mixing with basaltic sand additionally inhibit the ability to measure ferric absorptions in bedrock stratigraphically below VRR from orbit. There are two implications of these findings: (1) Ferric absorptions in CRISM data initially dismissed as noise could be real, and ferric phases are more widespread in lower Mt. Sharp than previously reported. (2) Patches with the deepest ferric absorptions in CRISM data are, like VRR, reflective of deeper absorptions in the bedrock. One model to explain this spectral variability is late-stage diagenetic fluids that changed the grain size of ferric phases, deepening absorptions. Curiosity's experience highlights the strengths of using CRISM data for spectral absorptions and associated mineral detections and the caveats in using these data for geologic interpretations and strategic path planning tools.
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Affiliation(s)
- A. A. Fraeman
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - J. R. Johnson
- Johns Hopkins University Applied Physics LaboratoryLaurelMDUSA
| | - R. E. Arvidson
- Department of Earth and Planetary SciencesWashington UniversitySt. LouisMOUSA
| | - M. S. Rice
- Geology Department, Physics and Astronomy DepartmentWestern Washington UniversityBellinghamWAUSA
| | - D. F. Wellington
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
| | | | - V. K. Fox
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | - B. H. N. Horgan
- Department of Earth, Atmospheric, and Planetary SciencesPurdue UniversityWest LafayetteINUSA
| | - S. R. Jacob
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
| | - M. R. Salvatore
- Department of Astronomy and Planetary ScienceNorthern Arizona UniversityFlagstaffAZUSA
| | - V. Z. Sun
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - P. Pinet
- Institut de Recherche en Astrophysique et PlanétologieUniversité de Toulouse, CNRS, UPS, CNESToulouseFrance
| | - J. F. Bell
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
| | - R. C. Wiens
- Los Alamos National LaboratoryLos AlamosNMUSA
| | - A. R. Vasavada
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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12
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Malin MC, Ravine MA, Caplinger MA, Tony Ghaemi F, Schaffner JA, Maki JN, Bell JF, Cameron JF, Dietrich WE, Edgett KS, Edwards LJ, Garvin JB, Hallet B, Herkenhoff KE, Heydari E, Kah LC, Lemmon MT, Minitti ME, Olson TS, Parker TJ, Rowland SK, Schieber J, Sletten R, Sullivan RJ, Sumner DY, Aileen Yingst R, Duston BM, McNair S, Jensen EH. The Mars Science Laboratory (MSL) Mast cameras and Descent imager: Investigation and instrument descriptions. EARTH AND SPACE SCIENCE (HOBOKEN, N.J.) 2017; 4:506-539. [PMID: 29098171 PMCID: PMC5652233 DOI: 10.1002/2016ea000252] [Citation(s) in RCA: 9] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/01/2017] [Revised: 04/18/2017] [Accepted: 06/08/2017] [Indexed: 05/13/2023]
Abstract
The Mars Science Laboratory Mast camera and Descent Imager investigations were designed, built, and operated by Malin Space Science Systems of San Diego, CA. They share common electronics and focal plane designs but have different optics. There are two Mastcams of dissimilar focal length. The Mastcam-34 has an f/8, 34 mm focal length lens, and the M-100 an f/10, 100 mm focal length lens. The M-34 field of view is about 20° × 15° with an instantaneous field of view (IFOV) of 218 μrad; the M-100 field of view (FOV) is 6.8° × 5.1° with an IFOV of 74 μrad. The M-34 can focus from 0.5 m to infinity, and the M-100 from ~1.6 m to infinity. All three cameras can acquire color images through a Bayer color filter array, and the Mastcams can also acquire images through seven science filters. Images are ≤1600 pixels wide by 1200 pixels tall. The Mastcams, mounted on the ~2 m tall Remote Sensing Mast, have a 360° azimuth and ~180° elevation field of regard. Mars Descent Imager is fixed-mounted to the bottom left front side of the rover at ~66 cm above the surface. Its fixed focus lens is in focus from ~2 m to infinity, but out of focus at 66 cm. The f/3 lens has a FOV of ~70° by 52° across and along the direction of motion, with an IFOV of 0.76 mrad. All cameras can acquire video at 4 frames/second for full frames or 720p HD at 6 fps. Images can be processed using lossy Joint Photographic Experts Group and predictive lossless compression.
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Affiliation(s)
| | | | | | | | | | - Justin N. Maki
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCaliforniaUSA
| | - James F. Bell
- School of Earth and Space ExplorationArizona State UniversityTempeArizonaUSA
| | | | - William E. Dietrich
- Department of Earth and Planetary ScienceUniversity of CaliforniaBerkeleyCaliforniaUSA
| | | | | | | | - Bernard Hallet
- Department of Earth and Space Sciences, College of the EnvironmentUniversity of WashingtonSeattleWashingtonUSA
| | | | - Ezat Heydari
- Department of Physics, Atmospheric Sciences, and GeoscienceJackson State UniversityJacksonMississippiUSA
| | - Linda C. Kah
- Department of Earth and Planetary SciencesUniversity of Tennessee, KnoxvilleKnoxvilleTennesseeUSA
| | - Mark T. Lemmon
- Department of Atmospheric SciencesTexas A&M UniversityCollege StationTexasUSA
| | | | | | - Timothy J. Parker
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCaliforniaUSA
| | - Scott K. Rowland
- Department of Geology and Geophysics, School of Ocean and Earth Science and TechnologyUniversity of Hawai'i at MānoaHonoluluHIUSA
| | - Juergen Schieber
- Department of Earth and Atmospheric SciencesIndiana University, BloomingtonBloomingtonIndianaUSA
| | - Ron Sletten
- Department of Earth and Space Sciences, College of the EnvironmentUniversity of WashingtonSeattleWashingtonUSA
| | | | - Dawn Y. Sumner
- Department of Earth and Planetary SciencesUniversity of CaliforniaDavisCaliforniaUSA
| | | | | | - Sean McNair
- Malin Space Science Systems, IncSan DiegoCaliforniaUSA
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13
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Abstract
The scientific objectives of the ExoMars rover are designed to answer several key questions in the search for life on Mars. In particular, the unique subsurface drill will address some of these, such as the possible existence and stability of subsurface organics. PanCam will establish the surface geological and morphological context for the mission, working in collaboration with other context instruments. Here, we describe the PanCam scientific objectives in geology, atmospheric science, and 3-D vision. We discuss the design of PanCam, which includes a stereo pair of Wide Angle Cameras (WACs), each of which has an 11-position filter wheel and a High Resolution Camera (HRC) for high-resolution investigations of rock texture at a distance. The cameras and electronics are housed in an optical bench that provides the mechanical interface to the rover mast and a planetary protection barrier. The electronic interface is via the PanCam Interface Unit (PIU), and power conditioning is via a DC-DC converter. PanCam also includes a calibration target mounted on the rover deck for radiometric calibration, fiducial markers for geometric calibration, and a rover inspection mirror. Key Words: Mars—ExoMars—Instrumentation—Geology—Atmosphere—Exobiology—Context. Astrobiology 17, 511–541.
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Yingst R, Berger J, Cohen B, Hynek B, Schmidt M. Determining best practices in reconnoitering sites for habitability potential on Mars using a semi-autonomous rover: A GeoHeuristic Operational Strategies Test. ACTA ASTRONAUTICA 2017; 132:268-281. [PMID: 29307922 PMCID: PMC5754930 DOI: 10.1016/j.actaastro.2016.12.018] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Indexed: 06/07/2023]
Abstract
We tested science operations strategies developed for use in remote mobile spacecraft missions, to determine whether reconnoitering a site of potential habitability prior to in-depth study (a walkabout-first strategy) can be a more efficient use of time and resources than the linear approach commonly used by planetary rover missions. Two field teams studied a sedimentary sequence in Utah to assess habitability potential. At each site one team commanded a human "rover" to execute observations and conducted data analysis and made follow-on decisions based solely on those observations. Another team followed the same traverse using traditional terrestrial field methods, and the results of the two teams were compared. Test results indicate that for a mission with goals similar to our field case, the walkabout-first strategy may save time and other mission resources, while improving science return. The approach enabled more informed choices and higher team confidence in choosing where to spend time and other consumable resources. The walkabout strategy may prove most efficient when many close sites must be triaged to a smaller subset for detailed study or sampling. This situation would arise when mission goals include finding, identifying, characterizing or sampling a specific material, feature or type of environment within a certain area.
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Affiliation(s)
- R.A. Yingst
- Planetary Science Institute, 1700 E. Ft. Lowell, Suite 106, Tucson, AZ 85719 USA
| | - J. Berger
- Department of Earth Sciences, University of Western Ontario, London, ON, Canada N6A 5B7
| | - B.A. Cohen
- NASA Marshall Space Flight Center, VP62, 320 Sparkman Dr., Huntsville, AL 35805 USA
| | - B. Hynek
- Laboratory for Atmospheric and Space Physics and Geological Sciences, University of Colorado, 392 UCB, Boulder, CO 80309 USA
| | - M.E. Schmidt
- Dept. of Earth Sciences, Brock University, St. Catharines, ON, Canada L2S 3A1
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Kinch KM, Bell JF, Goetz W, Johnson JR, Joseph J, Madsen MB, Sohl-Dickstein J. Dust deposition on the decks of the Mars Exploration Rovers: 10 years of dust dynamics on the Panoramic Camera calibration targets. EARTH AND SPACE SCIENCE (HOBOKEN, N.J.) 2015; 2:144-172. [PMID: 27981072 PMCID: PMC5125412 DOI: 10.1002/2014ea000073] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/23/2014] [Revised: 03/09/2015] [Accepted: 03/26/2015] [Indexed: 05/13/2023]
Abstract
The Panoramic Cameras on NASA's Mars Exploration Rovers have each returned more than 17,000 images of their calibration targets. In order to make optimal use of this data set for reflectance calibration, a correction must be made for the presence of air fall dust. Here we present an improved dust correction procedure based on a two-layer scattering model, and we present a dust reflectance spectrum derived from long-term trends in the data set. The dust on the calibration targets appears brighter than dusty areas of the Martian surface. We derive detailed histories of dust deposition and removal revealing two distinct environments: At the Spirit landing site, half the year is dominated by dust deposition, the other half by dust removal, usually in brief, sharp events. At the Opportunity landing site the Martian year has a semiannual dust cycle with dust removal happening gradually throughout two removal seasons each year. The highest observed optical depth of settled dust on the calibration target is 1.5 on Spirit and 1.1 on Opportunity (at 601 nm). We derive a general prediction for dust deposition rates of 0.004 ± 0.001 in units of surface optical depth deposited per sol (Martian solar day) per unit atmospheric optical depth. We expect this procedure to lead to improved reflectance-calibration of the Panoramic Camera data set. In addition, it is easily adapted to similar data sets from other missions in order to deliver improved reflectance calibration as well as data on dust reflectance properties and deposition and removal history.
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Affiliation(s)
- Kjartan M Kinch
- Niels Bohr Institute University of Copenhagen Copenhagen Denmark
| | - James F Bell
- School of Earth and Space Exploration Arizona State University Phoenix Arizona USA
| | - Walter Goetz
- Max Planck Institute for Solar System Research Göttingen Germany
| | - Jeffrey R Johnson
- Applied Physics Laboratory Johns Hopkins University Laurel Maryland USA
| | - Jonathan Joseph
- Department of Astronomy Cornell University Ithaca New York USA
| | - Morten Bo Madsen
- Niels Bohr Institute University of Copenhagen Copenhagen Denmark
| | - Jascha Sohl-Dickstein
- Neural Dynamics and Computation Laboratory Stanford University Stanford California USA
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Núñez JI, Farmer JD, Sellar RG, Swayze GA, Blaney DL. Science applications of a multispectral microscopic imager for the astrobiological exploration of Mars. ASTROBIOLOGY 2014; 14:132-69. [PMID: 24552233 PMCID: PMC3929460 DOI: 10.1089/ast.2013.1079] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/23/2013] [Accepted: 01/15/2014] [Indexed: 05/30/2023]
Abstract
Future astrobiological missions to Mars are likely to emphasize the use of rovers with in situ petrologic capabilities for selecting the best samples at a site for in situ analysis with onboard lab instruments or for caching for potential return to Earth. Such observations are central to an understanding of the potential for past habitable conditions at a site and for identifying samples most likely to harbor fossil biosignatures. The Multispectral Microscopic Imager (MMI) provides multispectral reflectance images of geological samples at the microscale, where each image pixel is composed of a visible/shortwave infrared spectrum ranging from 0.46 to 1.73 μm. This spectral range enables the discrimination of a wide variety of rock-forming minerals, especially Fe-bearing phases, and the detection of hydrated minerals. The MMI advances beyond the capabilities of current microimagers on Mars by extending the spectral range into the infrared and increasing the number of spectral bands. The design employs multispectral light-emitting diodes and an uncooled indium gallium arsenide focal plane array to achieve a very low mass and high reliability. To better understand and demonstrate the capabilities of the MMI for future surface missions to Mars, we analyzed samples from Mars-relevant analog environments with the MMI. Results indicate that the MMI images faithfully resolve the fine-scale microtextural features of samples and provide important information to help constrain mineral composition. The use of spectral endmember mapping reveals the distribution of Fe-bearing minerals (including silicates and oxides) with high fidelity, along with the presence of hydrated minerals. MMI-based petrogenetic interpretations compare favorably with laboratory-based analyses, revealing the value of the MMI for future in situ rover-mediated astrobiological exploration of Mars.
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Affiliation(s)
- Jorge I. Núñez
- School of Earth and Space Exploration, Arizona State University, Tempe, Arizona
| | - Jack D. Farmer
- School of Earth and Space Exploration, Arizona State University, Tempe, Arizona
| | - R. Glenn Sellar
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | | | - Diana L. Blaney
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
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Vaniman DT, Bish DL, Ming DW, Bristow TF, Morris RV, Blake DF, Chipera SJ, Morrison SM, Treiman AH, Rampe EB, Rice M, Achilles CN, Grotzinger JP, McLennan SM, Williams J, Bell JF, Newsom HE, Downs RT, Maurice S, Sarrazin P, Yen AS, Morookian JM, Farmer JD, Stack K, Milliken RE, Ehlmann BL, Sumner DY, Berger G, Crisp JA, Hurowitz JA, Anderson R, Des Marais DJ, Stolper EM, Edgett KS, Gupta S, Spanovich N, Agard C, Alves Verdasca JA, Anderson R, Archer D, Armiens-Aparicio C, Arvidson R, Atlaskin E, Atreya S, Aubrey A, Baker B, Baker M, Balic-Zunic T, Baratoux D, Baroukh J, Barraclough B, Bean K, Beegle L, Behar A, Bender S, Benna M, Bentz J, Berger J, Berman D, Blanco Avalos JJ, Blaney D, Blank J, Blau H, Bleacher L, Boehm E, Botta O, Bottcher S, Boucher T, Bower H, Boyd N, Boynton B, Breves E, Bridges J, Bridges N, Brinckerhoff W, Brinza D, Brunet C, Brunner A, Brunner W, Buch A, Bullock M, Burmeister S, Cabane M, Calef F, Cameron J, Campbell JI, Cantor B, Caplinger M, Caride Rodriguez J, Carmosino M, Carrasco Blazquez I, Charpentier A, Choi D, Clark B, Clegg S, Cleghorn T, Cloutis E, Cody G, Coll P, Conrad P, Coscia D, Cousin A, Cremers D, Cros A, Cucinotta F, d'Uston C, Davis S, Day MK, de la Torre Juarez M, DeFlores L, DeLapp D, DeMarines J, Dietrich W, Dingler R, Donny C, Drake D, Dromart G, Dupont A, Duston B, Dworkin J, Dyar MD, Edgar L, Edwards C, Edwards L, Ehresmann B, Eigenbrode J, Elliott B, Elliott H, Ewing R, Fabre C, Fairen A, Farley K, Fassett C, Favot L, Fay D, Fedosov F, Feldman J, Feldman S, Fisk M, Fitzgibbon M, Flesch G, Floyd M, Fluckiger L, Forni O, Fraeman A, Francis R, Francois P, Franz H, Freissinet C, French KL, Frydenvang J, Gaboriaud A, Gailhanou M, Garvin J, Gasnault O, Geffroy C, Gellert R, Genzer M, Glavin D, Godber A, Goesmann F, Goetz W, Golovin D, Gomez Gomez F, Gomez-Elvira J, Gondet B, Gordon S, Gorevan S, Grant J, Griffes J, Grinspoon D, Guillemot P, Guo J, Guzewich S, Haberle R, Halleaux D, Hallet B, Hamilton V, Hardgrove C, Harker D, Harpold D, Harri AM, Harshman K, Hassler D, Haukka H, Hayes A, Herkenhoff K, Herrera P, Hettrich S, Heydari E, Hipkin V, Hoehler T, Hollingsworth J, Hudgins J, Huntress W, Hviid S, Iagnemma K, Indyk S, Israel G, Jackson R, Jacob S, Jakosky B, Jensen E, Jensen JK, Johnson J, Johnson M, Johnstone S, Jones A, Jones J, Joseph J, Jun I, Kah L, Kahanpaa H, Kahre M, Karpushkina N, Kasprzak W, Kauhanen J, Keely L, Kemppinen O, Keymeulen D, Kim MH, Kinch K, King P, Kirkland L, Kocurek G, Koefoed A, Kohler J, Kortmann O, Kozyrev A, Krezoski J, Krysak D, Kuzmin R, Lacour JL, Lafaille V, Langevin Y, Lanza N, Lasue J, Le Mouelic S, Lee EM, Lee QM, Lees D, Lefavor M, Lemmon M, Malvitte AL, Leshin L, Leveille R, Lewin-Carpintier E, Lewis K, Li S, Lipkaman L, Little C, Litvak M, Lorigny E, Lugmair G, Lundberg A, Lyness E, Madsen M, Mahaffy P, Maki J, Malakhov A, Malespin C, Malin M, Mangold N, Manhes G, Manning H, Marchand G, Marin Jimenez M, Martin Garcia C, Martin D, Martin M, Martinez-Frias J, Martin-Soler J, Martin-Torres FJ, Mauchien P, McAdam A, McCartney E, McConnochie T, McCullough E, McEwan I, McKay C, McNair S, Melikechi N, Meslin PY, Meyer M, Mezzacappa A, Miller H, Miller K, Minitti M, Mischna M, Mitrofanov I, Moersch J, Mokrousov M, Molina Jurado A, Moores J, Mora-Sotomayor L, Mueller-Mellin R, Muller JP, Munoz Caro G, Nachon M, Navarro Lopez S, Navarro-Gonzalez R, Nealson K, Nefian A, Nelson T, Newcombe M, Newman C, Nikiforov S, Niles P, Nixon B, Noe Dobrea E, Nolan T, Oehler D, Ollila A, Olson T, Owen T, de Pablo Hernandez MA, Paillet A, Pallier E, Palucis M, Parker T, Parot Y, Patel K, Paton M, Paulsen G, Pavlov A, Pavri B, Peinado-Gonzalez V, Pepin R, Peret L, Perez R, Perrett G, Peterson J, Pilorget C, Pinet P, Pla-Garcia J, Plante I, Poitrasson F, Polkko J, Popa R, Posiolova L, Posner A, Pradler I, Prats B, Prokhorov V, Purdy SW, Raaen E, Radziemski L, Rafkin S, Ramos M, Raulin F, Ravine M, Reitz G, Renno N, Richardson M, Robert F, Robertson K, Rodriguez Manfredi JA, Romeral-Planello JJ, Rowland S, Rubin D, Saccoccio M, Salamon A, Sandoval J, Sanin A, Sans Fuentes SA, Saper L, Sautter V, Savijarvi H, Schieber J, Schmidt M, Schmidt W, Scholes DD, Schoppers M, Schroder S, Schwenzer S, Sebastian Martinez E, Sengstacken A, Shterts R, Siebach K, Siili T, Simmonds J, Sirven JB, Slavney S, Sletten R, Smith M, Sobron Sanchez P, Spray J, Squyres S, Stalport F, Steele A, Stein T, Stern J, Stewart N, Stipp SLS, Stoiber K, Sucharski B, Sullivan R, Summons R, Sun V, Supulver K, Sutter B, Szopa C, Tan F, Tate C, Teinturier S, ten Kate I, Thomas P, Thompson L, Tokar R, Toplis M, Torres Redondo J, Trainer M, Tretyakov V, Urqui-O'Callaghan R, Van Beek J, Van Beek T, VanBommel S, Varenikov A, Vasavada A, Vasconcelos P, Vicenzi E, Vostrukhin A, Voytek M, Wadhwa M, Ward J, Webster C, Weigle E, Wellington D, Westall F, Wiens RC, Wilhelm MB, Williams A, Williams R, Williams RBM, Wilson M, Wimmer-Schweingruber R, Wolff M, Wong M, Wray J, Wu M, Yana C, Yingst A, Zeitlin C, Zimdar R, Zorzano Mier MP. Mineralogy of a Mudstone at Yellowknife Bay, Gale Crater, Mars. Science 2013; 343:1243480. [DOI: 10.1126/science.1243480] [Citation(s) in RCA: 433] [Impact Index Per Article: 39.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
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Virtual Astronaut for Scientific Visualization—A Prototype for Santa Maria Crater on Mars. FUTURE INTERNET 2012. [DOI: 10.3390/fi4041049] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/16/2022] Open
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Tanaka Z, Perry M, Cooper G, Tang S, McKay CP, Chen B. Near-infrared (NIR) Raman spectroscopy of Precambrian carbonate stromatolites with post-depositional organic inclusions. APPLIED SPECTROSCOPY 2012; 66:911-916. [PMID: 22800768 DOI: 10.1366/11-06523] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/01/2023]
Abstract
Raman spectroscopy has promising potential for future Mars missions as a non-contact detection technique for characterizing organic material and mineralogy. Such a capability will be useful for selecting samples for detailed analysis on a rover and for selecting samples for return to Earth. Stromatolites are important evidence for the earliest life on Earth and are promising targets for Mars investigations. Although constructed by microorganisms, stromatolites are organo-sedimentary structures that can be large enough to be discovered and investigated by a Mars rover. In this paper, we report the Raman spectroscopic investigations of the carbonate mineralogy and organic layering in a Precambrian (~1.5 Gyr old) stromatolite from the Crystal Spring Formation of Southern California. Ultraviolet (UV: 266 nm), visible (514 nm, 633 nm), and near-infrared (NIR: 785 nm, 1064 nm) Raman spectra are presented. We conclude that 1064 nm excitation is the optimal excitation wavelength for avoiding intrinsic fluorescence and detecting organic carbon within the carbonate matrix. Our results confirm that NIR Raman spectroscopy has important applications for future Mars missions.
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Affiliation(s)
- Zuki Tanaka
- Department of Electrical Engineering, UC Santa Cruz, Santa Cruz, CA 95060, USA
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Squyres SW, Arvidson RE, Bell JF, Calef F, Clark BC, Cohen BA, Crumpler LA, de Souza PA, Farrand WH, Gellert R, Grant J, Herkenhoff KE, Hurowitz JA, Johnson JR, Jolliff BL, Knoll AH, Li R, McLennan SM, Ming DW, Mittlefehldt DW, Parker TJ, Paulsen G, Rice MS, Ruff SW, Schroder C, Yen AS, Zacny K. Ancient Impact and Aqueous Processes at Endeavour Crater, Mars. Science 2012; 336:570-6. [DOI: 10.1126/science.1220476] [Citation(s) in RCA: 151] [Impact Index Per Article: 12.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
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Dartnell LR, Storrie-Lombardi MC, Mullineaux CW, Ruban AV, Wright G, Griffiths AD, Muller JP, Ward JM. Degradation of cyanobacterial biosignatures by ionizing radiation. ASTROBIOLOGY 2011; 11:997-1016. [PMID: 22149884 DOI: 10.1089/ast.2011.0663] [Citation(s) in RCA: 16] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/31/2023]
Abstract
Primitive photosynthetic microorganisms, either dormant or dead, may remain today on the martian surface, akin to terrestrial cyanobacteria surviving endolithically in martian analog sites on Earth such as the Antarctic Dry Valleys and the Atacama Desert. Potential markers of martian photoautotrophs include the red edge of chlorophyll reflectance spectra or fluorescence emission from systems of light-harvesting pigments. Such biosignatures, however, would be modified and degraded by long-term exposure to ionizing radiation from the unshielded cosmic ray flux onto the martian surface. In this initial study into this issue, three analytical techniques--absorbance, reflectance, and fluorescence spectroscopy--were employed to determine the progression of the radiolytic destruction of cyanobacteria. The pattern of signal loss for chlorophyll reflection and fluorescence from several biomolecules is characterized and quantified after increasing exposures to ionizing gamma radiation. This allows estimation of the degradation rates of cyanobacterial biosignatures on the martian surface and the identification of promising detectable fluorescent break-down products.
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Affiliation(s)
- Lewis R Dartnell
- UCL Institute for Origins, University College London, London, UK.
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Ruff SW, Farmer JD, Calvin WM, Herkenhoff KE, Johnson JR, Morris RV, Rice MS, Arvidson RE, Bell JF, Christensen PR, Squyres SW. Characteristics, distribution, origin, and significance of opaline silica observed by the Spirit rover in Gusev crater, Mars. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010je003767] [Citation(s) in RCA: 125] [Impact Index Per Article: 9.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Hayes AG, Grotzinger JP, Edgar LA, Squyres SW, Watters WA, Sohl-Dickstein J. Reconstruction of eolian bed forms and paleocurrents from cross-bedded strata at Victoria Crater, Meridiani Planum, Mars. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010je003688] [Citation(s) in RCA: 30] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Chojnacki M, Burr DM, Moersch JE, Michaels TI. Orbital observations of contemporary dune activity in Endeavor crater, Meridiani Planum, Mars. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010je003675] [Citation(s) in RCA: 78] [Impact Index Per Article: 6.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Wang A, Ling ZC. Ferric sulfates on Mars: A combined mission data analysis of salty soils at Gusev crater and laboratory experimental investigations. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010je003665] [Citation(s) in RCA: 20] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Sullivan R, Anderson R, Biesiadecki J, Bond T, Stewart H. Cohesions, friction angles, and other physical properties of Martian regolith from Mars Exploration Rover wheel trenches and wheel scuffs. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010je003625] [Citation(s) in RCA: 69] [Impact Index Per Article: 5.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Geissler PE, Sullivan R, Golombek M, Johnson JR, Herkenhoff K, Bridges N, Vaughan A, Maki J, Parker T, Bell J. Gone with the wind: Eolian erasure of the Mars Rover tracks. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2010je003674] [Citation(s) in RCA: 37] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Cousins CR, Griffiths AD, Crawford IA, Prosser BJ, Storrie-Lombardi MC, Davis LE, Gunn M, Coates AJ, Jones AP, Ward JM. Astrobiological considerations for the selection of the geological filters on the ExoMars PanCam instrument. ASTROBIOLOGY 2010; 10:933-951. [PMID: 21118025 DOI: 10.1089/ast.2010.0517] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/30/2023]
Abstract
The Panoramic Camera (PanCam) instrument will provide visible-near IR multispectral imaging of the ExoMars rover's surroundings to identify regions of interest within the nearby terrain. This multispectral capability is dependant upon the 12 preselected "geological" filters that are integrated into two wide-angle cameras. First devised by the Imager for Mars Pathfinder team to detect iron oxides, this baseline filter set has remained largely unchanged for subsequent missions (Mars Exploration Rovers, Beagle 2, Phoenix) despite the advancing knowledge of the mineralogical diversity on Mars. Therefore, the geological filters for the ExoMars PanCam will be redesigned to accommodate the astrobiology focus of ExoMars, where hydrated mineral terrains (evidence of past liquid water) will be priority targets. Here, we conduct an initial investigation into new filter wavelengths for the ExoMars PanCam and present results from tests performed on Mars analog rocks. Two new filter sets were devised: one with filters spaced every 50 nm ("F1-12") and another that utilizes a novel filter selection method based upon hydrated mineral reflectance spectra ("F2-12"). These new filter sets, along with the Beagle 2 filter set (currently the baseline for the ExoMars PanCam), were tested on their ability to identify hydrated minerals and biosignatures present in Mars analog rocks. The filter sets, with varying degrees of ability, detected the spectral features of minerals jarosite, opaline silica, alunite, nontronite, and siderite present in these rock samples. None of the filter sets, however, were able to detect fossilized biomat structures and small (<2 mm) mineralogical heterogeneities present in silica sinters. Both new filter sets outperformed the Beagle 2 filters, with F2-12 detecting the most spectral features produced by hydrated minerals and providing the best discrimination between samples. Future work involving more extensive testing on Mars analog samples that exhibit a wider range of mineralogies would be the next step in carefully evaluating the new filter sets.
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Fleischer I, Brückner J, Schröder C, Farrand W, Tréguier E, Morris R, Klingelhöfer G, Herkenhoff K, Mittlefehldt D, Ashley J, Golombek M, Johnson JR, Jolliff B, Squyres SW, Weitz C, Gellert R, de Souza PA, Cohen BA. Mineralogy and chemistry of cobbles at Meridiani Planum, Mars, investigated by the Mars Exploration Rover Opportunity. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2010je003621] [Citation(s) in RCA: 13] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Greeley R, Waller DA, Cabrol NA, Landis GA, Lemmon MT, Neakrase LDV, Pendleton Hoffer M, Thompson SD, Whelley PL. Gusev Crater, Mars: Observations of three dust devil seasons. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2010je003608] [Citation(s) in RCA: 70] [Impact Index Per Article: 5.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Arvidson RE, Bell JF, Bellutta P, Cabrol NA, Catalano JG, Cohen J, Crumpler LS, Des Marais DJ, Estlin TA, Farrand WH, Gellert R, Grant JA, Greenberger RN, Guinness EA, Herkenhoff KE, Herman JA, Iagnemma KD, Johnson JR, Klingelhöfer G, Li R, Lichtenberg KA, Maxwell SA, Ming DW, Morris RV, Rice MS, Ruff SW, Shaw A, Siebach KL, de Souza PA, Stroupe AW, Squyres SW, Sullivan RJ, Talley KP, Townsend JA, Wang A, Wright JR, Yen AS. Spirit Mars Rover Mission: Overview and selected results from the northern Home Plate Winter Haven to the side of Scamander crater. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2010je003633] [Citation(s) in RCA: 97] [Impact Index Per Article: 6.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Tamppari LK, Bass D, Cantor B, Daubar I, Dickinson C, Fisher D, Fujii K, Gunnlauggson HP, Hudson TL, Kass D, Kleinböhl A, Komguem L, Lemmon MT, Mellon M, Moores J, Pankine A, Pathak J, Searls M, Seelos F, Smith MD, Smrekar S, Taylor P, Holstein-Rathlou C, Weng W, Whiteway J, Wolff M. Phoenix and MRO coordinated atmospheric measurements. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2009je003415] [Citation(s) in RCA: 36] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Squyres SW, Knoll AH, Arvidson RE, Ashley JW, Bell JF, Calvin WM, Christensen PR, Clark BC, Cohen BA, de Souza PA, Edgar L, Farrand WH, Fleischer I, Gellert R, Golombek MP, Grant J, Grotzinger J, Hayes A, Herkenhoff KE, Johnson JR, Jolliff B, Klingelhöfer G, Knudson A, Li R, McCoy TJ, McLennan SM, Ming DW, Mittlefehldt DW, Morris RV, Rice JW, Schröder C, Sullivan RJ, Yen A, Yingst RA. Exploration of Victoria Crater by the Mars Rover Opportunity. Science 2009; 324:1058-61. [DOI: 10.1126/science.1170355] [Citation(s) in RCA: 113] [Impact Index Per Article: 7.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- S. W. Squyres
- Department of Astronomy, Space Sciences Building, Cornell University, Ithaca, NY 14853, USA
| | - A. H. Knoll
- Botanical Museum, Harvard University, Cambridge, MA 02138, USA
| | - R. E. Arvidson
- Department of Earth and Planetary Sciences, Washington University, St. Louis, MO 63031, USA
| | - J. W. Ashley
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA
| | - J. F. Bell
- Department of Astronomy, Space Sciences Building, Cornell University, Ithaca, NY 14853, USA
| | - W. M. Calvin
- University of Nevada, Reno, Geological Sciences, Reno, NV 89557, USA
| | - P. R. Christensen
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA
| | - B. C. Clark
- Lockheed Martin Corporation, Littleton, CO 80127, USA
| | - B. A. Cohen
- National Aeronautics and Space Administration, Marshall Space Flight Center, Huntsville, AL 35812, USA
| | - P. A. de Souza
- Tasmanian Information and Communication Technologies Centre, Commonwealth Scientific and Industrial Research Organisation, Castray Esplanade, Hobart TAS 7000, Australia
| | - L. Edgar
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA
| | | | - I. Fleischer
- Institut für Anorganische und Analytische Chemie, Johannes Gutenberg-Universität, Mainz, Germany
| | - R. Gellert
- Department of Physics, University of Guelph, Guelph, ON, N1G 2W1, Canada
| | - M. P. Golombek
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - J. Grant
- Center for Earth and Planetary Studies, Smithsonian Institution, Washington, DC 20560, USA
| | - J. Grotzinger
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA
| | - A. Hayes
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA
| | | | | | - B. Jolliff
- Department of Earth and Planetary Sciences, Washington University, St. Louis, MO 63031, USA
| | - G. Klingelhöfer
- Institut für Anorganische und Analytische Chemie, Johannes Gutenberg-Universität, Mainz, Germany
| | - A. Knudson
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA
| | - R. Li
- Department of Civil and Environmental Engineering and Geodetic Science, Ohio State University, Columbus, OH 43210, USA
| | - T. J. McCoy
- Department of Mineral Sciences, National Museum of Natural History, Smithsonian Institution, Washington, DC 20560, USA
| | - S. M. McLennan
- Department of Geosciences, State University of New York, Stony Brook, NY 11794, USA
| | - D. W. Ming
- Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX 77058, USA
| | - D. W. Mittlefehldt
- Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX 77058, USA
| | - R. V. Morris
- Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX 77058, USA
| | - J. W. Rice
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA
| | - C. Schröder
- Institut für Anorganische und Analytische Chemie, Johannes Gutenberg-Universität, Mainz, Germany
| | - R. J. Sullivan
- Department of Astronomy, Space Sciences Building, Cornell University, Ithaca, NY 14853, USA
| | - A. Yen
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - R. A. Yingst
- Natural and Applied Sciences, University of Wisconsin Green Bay, Green Bay, WI 54311, USA
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Yingst RA, Crumpler L, Farrand WH, Li R, Cabrol NA, Neakrase LD. Morphology and texture of particles along the Spirit rover traverse from sol 450 to sol 745. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003179] [Citation(s) in RCA: 29] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Wang A, Bell JF, Li R, Johnson JR, Farrand WH, Cloutis EA, Arvidson RE, Crumpler L, Squyres SW, McLennan SM, Herkenhoff KE, Ruff SW, Knudson AT, Chen W, Greenberger R. Light-toned salty soils and coexisting Si-rich species discovered by the Mars Exploration Rover Spirit in Columbia Hills. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003126] [Citation(s) in RCA: 84] [Impact Index Per Article: 5.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Calvin WM, Shoffner JD, Johnson JR, Knoll AH, Pocock JM, Squyres SW, Weitz CM, Arvidson RE, Bell JF, Christensen PR, de Souza PA, Farrand WH, Glotch TD, Herkenhoff KE, Jolliff BL, Knudson AT, McLennan SM, Rogers AD, Thompson SD. Hematite spherules at Meridiani: Results from MI, Mini-TES, and Pancam. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003048] [Citation(s) in RCA: 34] [Impact Index Per Article: 2.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Lewis KW, Aharonson O, Grotzinger JP, Squyres SW, Bell JF, Crumpler LS, Schmidt ME. Structure and stratigraphy of Home Plate from the Spirit Mars Exploration Rover. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003025] [Citation(s) in RCA: 61] [Impact Index Per Article: 3.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Herkenhoff KE, Grotzinger J, Knoll AH, McLennan SM, Weitz C, Yingst A, Anderson R, Archinal BA, Arvidson RE, Barrett JM, Becker KJ, Bell JF, Budney C, Chapman MG, Cook D, Ehlmann B, Franklin B, Gaddis LR, Galuszka DM, Garcia PA, Geissler P, Hare TM, Howington-Kraus E, Johnson JR, Keszthelyi L, Kirk RL, Lanagan P, Lee EM, Leff C, Maki JN, Mullins KF, Parker TJ, Redding BL, Rosiek MR, Sims MH, Soderblom LA, Spanovich N, Springer R, Squyres SW, Stolper D, Sucharski RM, Sucharski T, Sullivan R, Torson JM. Surface processes recorded by rocks and soils on Meridiani Planum, Mars: Microscopic Imager observations during Opportunity's first three extended missions. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003100] [Citation(s) in RCA: 26] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Leer K, Bertelsen P, Binau CS, Djernis Olsen L, Drube L, Falkenberg TV, Haspang MP, Madsen MB, Olsen M, Sykulska H, Vijendran S, Pike WT, Staufer U, Parrat D, Lemmon M, Hecht MH, Mogensen CT, Gross MA, Goetz W, Marshall J, Britt D, Smith P, Shinohara C, Woida P, Woida R, Tanner R, Reynolds R, Shaw A. Magnetic properties experiments and the Surface Stereo Imager calibration target onboard the Mars Phoenix 2007 Lander: Design, calibration, and science goals. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003014] [Citation(s) in RCA: 14] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Thomson BJ, Bridges NT, Greeley R. Rock abrasion features in the Columbia Hills, Mars. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003018] [Citation(s) in RCA: 25] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Sullivan R, Arvidson R, Bell JF, Gellert R, Golombek M, Greeley R, Herkenhoff K, Johnson J, Thompson S, Whelley P, Wray J. Wind-driven particle mobility on Mars: Insights from Mars Exploration Rover observations at “El Dorado” and surroundings at Gusev Crater. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003101] [Citation(s) in RCA: 220] [Impact Index Per Article: 13.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Schmidt ME, Ruff SW, McCoy TJ, Farrand WH, Johnson JR, Gellert R, Ming DW, Morris RV, Cabrol N, Lewis KW, Schroeder C. Hydrothermal origin of halogens at Home Plate, Gusev Crater. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003027] [Citation(s) in RCA: 62] [Impact Index Per Article: 3.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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McCoy TJ, Sims M, Schmidt ME, Edwards L, Tornabene LL, Crumpler LS, Cohen BA, Soderblom LA, Blaney DL, Squyres SW, Arvidson RE, Rice JW, Tréguier E, d'Uston C, Grant JA, McSween HY, Golombek MP, Haldemann AFC, de Souza PA. Structure, stratigraphy, and origin of Husband Hill, Columbia Hills, Gusev Crater, Mars. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003041] [Citation(s) in RCA: 38] [Impact Index Per Article: 2.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Bell JF, Rice MS, Johnson JR, Hare TM. Surface albedo observations at Gusev Crater and Meridiani Planum, Mars. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002976] [Citation(s) in RCA: 28] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Goetz W, Leer K, Gunnlaugsson HP, Bartlett P, Basso B, Bell J, Bertelsen P, Binau CS, Chu PC, Gorevan S, Hansen MF, Hviid SF, Kinch KM, Klingelhöfer G, Kusack A, Madsen MB, Ming DW, Morris RV, Mumm E, Myrick T, Olsen M, Squyres SW, Wilson J, Yen A. Search for magnetic minerals in Martian rocks: Overview of the Rock Abrasion Tool (RAT) magnet investigation on Spirit and Opportunity. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2006je002819] [Citation(s) in RCA: 9] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Knoll AH, Jolliff BL, Farrand WH, Bell III JF, Clark BC, Gellert R, Golombek MP, Grotzinger JP, Herkenhoff KE, Johnson JR, McLennan SM, Morris R, Squyres SW, Sullivan R, Tosca NJ, Yen A, Learner Z. Veneers, rinds, and fracture fills: Relatively late alteration of sedimentary rocks at Meridiani Planum, Mars. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002949] [Citation(s) in RCA: 49] [Impact Index Per Article: 3.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Rogers AD, Aharonson O. Mineralogical composition of sands in Meridiani Planum determined from Mars Exploration Rover data and comparison to orbital measurements. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002995] [Citation(s) in RCA: 79] [Impact Index Per Article: 4.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Yen AS, Morris RV, Clark BC, Gellert R, Knudson AT, Squyres S, Mittlefehldt DW, Ming DW, Arvidson R, McCoy T, Schmidt M, Hurowitz J, Li R, Johnson JR. Hydrothermal processes at Gusev Crater: An evaluation of Paso Robles class soils. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002978] [Citation(s) in RCA: 109] [Impact Index Per Article: 6.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Campbell JL, Gellert R, Lee M, Mallett CL, Maxwell JA, O'Meara JM. Quantitative in situ determination of hydration of bright high-sulfate Martian soils. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002959] [Citation(s) in RCA: 35] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Cabrol NA, Wettergreen D, Warren-Rhodes K, Grin EA, Moersch J, Diaz GC, Cockell CS, Coppin P, Demergasso C, Dohm JM, Ernst L, Fisher G, Glasgow J, Hardgrove C, Hock AN, Jonak D, Marinangeli L, Minkley E, Ori GG, Piatek J, Pudenz E, Smith T, Stubbs K, Thomas G, Thompson D, Waggoner A, Wagner M, Weinstein S, Wyatt M. Life in the Atacama: Searching for life with rovers (science overview). ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006jg000298] [Citation(s) in RCA: 35] [Impact Index Per Article: 2.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Nathalie A. Cabrol
- Space Sciences Division; NASA Ames Research Center; Moffett Field California USA
- SETI Institute; Mountain View California USA
| | - David Wettergreen
- Robotics Institute; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Kim Warren-Rhodes
- Space Sciences Division; NASA Ames Research Center; Moffett Field California USA
- SETI Institute; Mountain View California USA
| | - Edmond A. Grin
- Space Sciences Division; NASA Ames Research Center; Moffett Field California USA
- SETI Institute; Mountain View California USA
| | - Jeffrey Moersch
- Department of Earth and Planetary Sciences; University of Tennessee; Knoxville Tennessee USA
| | | | - Charles S. Cockell
- Planetary and Space Sciences Research Institute; Open University; Milton Keynes UK
| | - Peter Coppin
- Robotics Institute; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | | | - James M. Dohm
- Hydrology and Water Resources Department; University of Arizona; Tucson Arizona USA
| | - Lauren Ernst
- Department of Biology; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Gregory Fisher
- Department of Biology; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Justin Glasgow
- Department of Industrial Engineering; University of Iowa; Iowa City Iowa USA
| | - Craig Hardgrove
- Department of Earth and Planetary Sciences; University of Tennessee; Knoxville Tennessee USA
| | - Andrew N. Hock
- Department of Earth and Space Sciences; University of California; Los Angeles California USA
| | - Dominic Jonak
- Robotics Institute; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | | | - Edwin Minkley
- Department of Biology; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | | | - Jennifer Piatek
- Department of Earth and Planetary Sciences; University of Tennessee; Knoxville Tennessee USA
| | - Erin Pudenz
- Department of Industrial Engineering; University of Iowa; Iowa City Iowa USA
| | - Trey Smith
- Robotics Institute; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Kristen Stubbs
- Robotics Institute; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Geb Thomas
- Department of Industrial Engineering; University of Iowa; Iowa City Iowa USA
| | - David Thompson
- Robotics Institute; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Alan Waggoner
- Department of Biology; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Michael Wagner
- Robotics Institute; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Shmuel Weinstein
- Department of Biology; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Michael Wyatt
- Department of Earth and Planetary Sciences; University of Tennessee; Knoxville Tennessee USA
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