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McKeeby BE, Ramsey MS, Tai Udovicic CJ, Haberle C, Edwards CS. Quantifying Sub-Meter Surface Heterogeneity on Mars Using Off-Axis Thermal Emission Imaging System (THEMIS) Data. EARTH AND SPACE SCIENCE (HOBOKEN, N.J.) 2022; 9:e2022EA002430. [PMID: 36588669 PMCID: PMC9788145 DOI: 10.1029/2022ea002430] [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: 05/16/2022] [Revised: 07/26/2022] [Accepted: 08/03/2022] [Indexed: 06/17/2023]
Abstract
Surface heterogeneities below the spatial resolution of thermal infrared (TIR) instruments result in anisothermality and can produce emissivity spectra with negative slopes toward longer wavelengths. Sloped spectra arise from an incorrect assumption of either a uniform surface temperature or a maximum emissivity during the temperature-emissivity separation of radiance data. Surface roughness and lateral mixing of different sub-pixel surface units result in distinct spectral slopes with magnitudes proportional to the degree of temperature mixing. Routine Off-nadir Targeted Observations (ROTO) of the Thermal Emission Imaging Spectrometer (THEMIS) are used here for the first time to investigate anisothermality below the spatial resolution of THEMIS. The southern flank of Apollinaris Mons and regions within the Medusae Fossae Formation are studied using THEMIS ROTO data acquired just after local sunset. We observe a range of sloped TIR emission spectra dependent on the magnitude of temperature differences within a THEMIS pixel. Spectral slopes and wavelength-dependent brightness temperature differences are forward-modeled for a series of two-component surfaces of varying thermal inertia values. Our results imply that differing relative proportions of rocky and unconsolidated surface units are observed at each ROTO viewing geometry and suggest a local rock abundance six times greater than published results that rely on nadir data. High-resolution visible images of these regions indicate a mixture of surface units from boulders to dunes, providing credence to the model.
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Affiliation(s)
- B. E. McKeeby
- Department of Geology and Environmental ScienceUniversity of PittsburghPittsburghPAUSA
| | - M. S. Ramsey
- Department of Geology and Environmental ScienceUniversity of PittsburghPittsburghPAUSA
| | - C. J. Tai Udovicic
- Department of Astronomy and Planetary ScienceNorthern Arizona UniversityFlagstaffAZUSA
| | - C. Haberle
- Department of Astronomy and Planetary ScienceNorthern Arizona UniversityFlagstaffAZUSA
| | - C. S. Edwards
- Department of Astronomy and Planetary ScienceNorthern Arizona UniversityFlagstaffAZUSA
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2
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Sun M, Zheng Y, Shi Y, Zhang G, Shao Y. Low-intensity-low-temperature stability assessment of perovskite solar cells operating on simulated Martian surface conditions. Phys Chem Chem Phys 2022; 24:17716-17722. [PMID: 35838540 DOI: 10.1039/d2cp01450e] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/21/2022]
Abstract
Immigration to Mars, which is expected to be powered mainly by photovoltaics, is one of the greatest dreams of humanity. However, the extreme temperature difference and high-energy cosmic radiation on the surface of Mars make it difficult for conventional photovoltaics to operate steadily over time. With their advantages of being lightweight, having a high irradiation tolerance, and an outstanding power conversion efficiency (PCE), perovskite solar cells (PSCs) have shown themselves to be a promising candidate for Martian applications. In this study, we simulated the low-intensity-low-temperature (LILT) environment of the Mars surface, and monitored the in situ device performance of PSCs. Surprisingly, the device PCE was not only maintained at a high level but was even improved slightly. Further investigation revealed that the self-healing effect of perovskites under LILT conditions could be attributed to the light-induced decomposition of the perovskite film and the β-phase perovskite recrystallization process at the perovskite/hole transport layer interface. Interfacial β-phase perovskites are stable at low temperatures, which can facilitate charge extraction and protect the perovskite bulk from long-term light damage. This study demonstrated the feasibility of PSCs and provides a reference for Martian applications.
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Affiliation(s)
- Mengjie Sun
- School of Physics and Optoelectronic Engineering, Hangzhou Institute for Advanced Study, UCAS, 310024, Hangzhou, China.,Key Laboratory of Materials for High-Power Laser, Shanghai Institute of Optics and Fine Mechanics, Chinese Academy of Sciences, 201800, Shanghai, China
| | - Yifan Zheng
- Key Laboratory of Materials for High-Power Laser, Shanghai Institute of Optics and Fine Mechanics, Chinese Academy of Sciences, 201800, Shanghai, China.,Center of Materials Science and Optoelectronics Engineering, University of Chinese Academy of Sciences, 100049, Beijing, China
| | - Yifeng Shi
- Key Laboratory of Materials for High-Power Laser, Shanghai Institute of Optics and Fine Mechanics, Chinese Academy of Sciences, 201800, Shanghai, China
| | - Guodong Zhang
- Key Laboratory of Materials for High-Power Laser, Shanghai Institute of Optics and Fine Mechanics, Chinese Academy of Sciences, 201800, Shanghai, China.,Center of Materials Science and Optoelectronics Engineering, University of Chinese Academy of Sciences, 100049, Beijing, China
| | - Yuchuan Shao
- School of Physics and Optoelectronic Engineering, Hangzhou Institute for Advanced Study, UCAS, 310024, Hangzhou, China.,Key Laboratory of Materials for High-Power Laser, Shanghai Institute of Optics and Fine Mechanics, Chinese Academy of Sciences, 201800, Shanghai, China.,Center of Materials Science and Optoelectronics Engineering, University of Chinese Academy of Sciences, 100049, Beijing, China
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3
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Mizuochi H, Iwao K, Yamamoto S. Thermal remote sensing over heterogeneous urban and suburban landscapes using sensor-driven super-resolution. PLoS One 2022; 17:e0266541. [PMID: 35385560 PMCID: PMC8986004 DOI: 10.1371/journal.pone.0266541] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/25/2021] [Accepted: 03/22/2022] [Indexed: 11/19/2022] Open
Abstract
Thermal remote sensing is an important tool for monitoring regional climate and environment, including urban heat islands. However, it suffers from a relatively lower spatial resolution compared to optical remote sensing. To improve the spatial resolution, various “data-driven” image processing techniques (pan-sharpening, kernel-driven methods, and machine learning) have been developed in the previous decades. Such empirical super-resolution methods create visually appealing thermal images; however, they may sacrifice radiometric consistency because they are not necessarily sensitive to specific sensor features. In this paper, we evaluated a “sensor-driven” super-resolution approach that explicitly considers the sensor blurring process, to ensure radiometric consistency with the original thermal image during high-resolution thermal image retrieval. The sensor-driven algorithm was applied to a cloud-free Moderate Resolution Imaging Spectroradiometer (MODIS) scene of heterogeneous urban and suburban landscape that included built-up areas, low mountains with a forest, a lake, croplands, and river channels. Validation against the reference high-resolution thermal image obtained by the Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) shows that the sensor-driven algorithm can downscale the MODIS image to 250-m resolution, while maintaining a high statistical consistency with the original MODIS and ASTER images. Part of our algorithm, such as radiometric offset correction based on the Mahalanobis distance, may be integrated with other existing approaches in the future.
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Affiliation(s)
- Hiroki Mizuochi
- Geological Survey of Japan, National Institute of Advanced Industrial Science and Technology, Tsukuba, Ibaraki, Japan
- * E-mail:
| | - Koki Iwao
- Geological Survey of Japan, National Institute of Advanced Industrial Science and Technology, Tsukuba, Ibaraki, Japan
| | - Satoru Yamamoto
- Geological Survey of Japan, National Institute of Advanced Industrial Science and Technology, Tsukuba, Ibaraki, Japan
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4
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Bendia AG, Callefo F, Araújo MN, Sanchez E, Teixeira VC, Vasconcelos A, Battilani G, Pellizari VH, Rodrigues F, Galante D. Metagenome-Assembled Genomes from Monte Cristo Cave (Diamantina, Brazil) Reveal Prokaryotic Lineages As Functional Models for Life on Mars. ASTROBIOLOGY 2022; 22:293-312. [PMID: 34694925 DOI: 10.1089/ast.2021.0016] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
Microbial communities have been explored in various terrestrial subsurface ecosystems, showing metabolic potentials that could generate noteworthy morphological and molecular biosignatures. Recent advancements in bioinformatic tools have allowed for descriptions of novel and yet-to-be cultivated microbial lineages in different ecosystems due to the genome reconstruction approach from metagenomic data. Using shotgun metagenomic data, we obtained metagenome-assembled genomes related to cultivated and yet-to-be cultivated prokaryotic lineages from a silica and iron-rich cave (Monte Cristo) in Minas Gerais State, Brazil. The Monte Cristo Cave has been shown to possess a high diversity of genes involved with different biogeochemical cycles, including reductive and oxidative pathways related to carbon, sulfur, nitrogen, and iron. Three genomes were selected for pangenomic analysis, assigned as Truepera sp., Ca. Methylomirabilis sp., and Ca. Koribacter sp. based on their lifestyles (radiation resistance, anaerobic methane oxidation, and potential iron oxidation). These bacteria exhibit genes involved with multiple DNA repair strategies, starvation, and stress response. Because these groups have few reference genomes deposited in databases, our study adds important genomic information about these lineages. The combination of techniques applied in this study allowed us to unveil the potential relationships between microbial genomes and their ecological processes with the cave mineralogy and highlight the lineages involved with anaerobic methane oxidation, iron oxidation, and radiation resistance as functional models for the search for extant life-forms outside our planet in silica- and iron-rich environments and potentially on Mars.
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Affiliation(s)
- Amanda G Bendia
- Biological Oceanography Department, Oceanographic Institute, Universidade de São Paulo, São Paulo, Brazil
| | - Flavia Callefo
- Brazilian Synchrotron Light Laboratory, Brazilian Center for Research in Energy and Materials, Campinas, Brazil
| | - Maicon N Araújo
- Fundamental Chemistry Department, Institute of Chemistry, Universidade de São Paulo, São Paulo, Brazil
| | - Evelyn Sanchez
- Institute of Science and Technology, Federal University of the Jequitinhonha and Mucuri, Diamantina, Brazil
| | - Verônica C Teixeira
- Brazilian Synchrotron Light Laboratory, Brazilian Center for Research in Energy and Materials, Campinas, Brazil
| | - Alessandra Vasconcelos
- Institute of Science and Technology, Federal University of the Jequitinhonha and Mucuri, Diamantina, Brazil
| | - Gislaine Battilani
- Institute of Science and Technology, Federal University of the Jequitinhonha and Mucuri, Diamantina, Brazil
| | - Vivian H Pellizari
- Biological Oceanography Department, Oceanographic Institute, Universidade de São Paulo, São Paulo, Brazil
| | - Fabio Rodrigues
- Fundamental Chemistry Department, Institute of Chemistry, Universidade de São Paulo, São Paulo, Brazil
| | - Douglas Galante
- Brazilian Synchrotron Light Laboratory, Brazilian Center for Research in Energy and Materials, Campinas, Brazil
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5
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Rodriguez JAP, Dobrea EN, Kargel JS, Baker VR, Crown DA, Webster KD, Berman DC, Wilhelm MB, Buckner D. The Oldest Highlands of Mars May Be Massive Dust Fallout Deposits. Sci Rep 2020; 10:10347. [PMID: 32587301 PMCID: PMC7316829 DOI: 10.1038/s41598-020-64676-z] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/27/2019] [Accepted: 04/14/2020] [Indexed: 11/17/2022] Open
Abstract
The oldest terrains of Mars are cratered landscapes, in which extensive valleys and basins are covered by ubiquitous fluvial plains. One current paradigm maintains that an impact-generated megaregolith underlies these sediments. This megaregolith was likely largely generated during the Early Noachian (~4.1 to ~3.94 Ga) when most Martian impact basins formed. We examined the geologic records of NW Hellas and NW Isidis, which include this epoch’s most extensive circum-basin outcrops. Here, we show that these regions include widespread, wind-eroded landscapes, crater rims eroded down by several hundred meters, pitted plains, and inverted fluvial and crater landforms. These surfaces exhibit few fresh craters, indicating geologically recent wind erosion. The deep erosion, topographic inversions, and an absence of dunes on or near talus across these regions suggest that sediments finer than sand compose most of these highland materials. We propose that basin-impact-generated hurricane-force winds created sediment-laden atmospheric conditions, and that muddy rains rapidly settled suspended sediments to construct extensive Early Noachian highlands. The implied high abundance of fine-grained sediments before these impacts suggests large-scale glacial silt production and supports the previously proposed Noachian “icy highlands” hypothesis. We suggest that subglacial meltwater interactions with the sedimentary highlands could have promoted habitability, particularly in clay strata.
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Affiliation(s)
- J Alexis P Rodriguez
- Planetary Science Institute, 1700 East Fort Lowell Road, Suite 106, Tucson, AZ, 85719-2395, USA.
| | - Eldar Noe Dobrea
- Planetary Science Institute, 1700 East Fort Lowell Road, Suite 106, Tucson, AZ, 85719-2395, USA
| | - Jeffrey S Kargel
- Planetary Science Institute, 1700 East Fort Lowell Road, Suite 106, Tucson, AZ, 85719-2395, USA
| | - V R Baker
- Department of Hydrology & Atmospheric Sciences, University of Arizona, Tucson, AZ, 85721, USA
| | - David A Crown
- Planetary Science Institute, 1700 East Fort Lowell Road, Suite 106, Tucson, AZ, 85719-2395, USA
| | - Kevin D Webster
- Planetary Science Institute, 1700 East Fort Lowell Road, Suite 106, Tucson, AZ, 85719-2395, USA
| | - Daniel C Berman
- Planetary Science Institute, 1700 East Fort Lowell Road, Suite 106, Tucson, AZ, 85719-2395, USA
| | | | - Denise Buckner
- University of North Dakota, Department of Space Studies, Grand Forks, ND, 58202, USA.,Blue Marble Space Institute of Science, 1001 4th Ave, Suite 3201, Seattle, WA, 98154, USA
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6
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Development and Mechanical Properties of Basalt Fiber-Reinforced Acrylonitrile Butadiene Styrene for In-Space Manufacturing Applications. JOURNAL OF COMPOSITES SCIENCE 2019. [DOI: 10.3390/jcs3030089] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
A new basalt fiber reinforced acrylonitrile butadiene styrene (ABS) filament has been developed for fused filament fabrication (FFF, 3D printing) to be used in Mars habitat construction. Building habitats on Mars will be expensive, especially if all material must be shipped from earth. However, if some materials can be used from Mars, costs will dramatically decrease. Basalt is easily mined from the surface of Mars. This study details the production process of the material, experimental results from mechanical testing, and preliminary X-ray shielding characteristics. The addition of chopped 3 mm basalt fibers to standard FFF material, ABS, increased strength and stiffness of the composite material. By adding 25% (by weight) basalt fiber to ABS, tensile strength improved nearly 40% by increasing from 36.55 MPa to 50.58 MPa, while Modulus of Elasticity increased about 120% from 2.15 GPa to 4.79 GPa. Flexural strength increased by about 20% from 56.94 MPa to 68.51 MPa, while Flexural Modulus increased by about 70% from 1.81 GPa to 3.05 GPa. While compression results did not see much strength improvements, the addition of fibers also did not decrease compressive strength. This is important when considering that basalt fibers provide radiation shielding and the cost of adding basalt fibers to construction materials on Mars will be negligible compared to the cost of shipping other materials from earth. In preliminary digital radiography testing, it was shown that 77% of X-rays were shielded with 25% basalt fiber added (as compared to neat ABS). In small-scale 3D printing applications, the 25% fiber ratio seems to be the highest ratio that provides reliable FFF printing.
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7
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Exploration of Planetary Hyperspectral Images with Unsupervised Spectral Unmixing: A Case Study of Planet Mars. REMOTE SENSING 2018. [DOI: 10.3390/rs10050737] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
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8
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Oehler DZ, Etiope G. Methane Seepage on Mars: Where to Look and Why. ASTROBIOLOGY 2017; 17:1233-1264. [PMID: 28771029 PMCID: PMC5730060 DOI: 10.1089/ast.2017.1657] [Citation(s) in RCA: 19] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/01/2017] [Accepted: 05/14/2017] [Indexed: 05/09/2023]
Abstract
Methane on Mars is a topic of special interest because of its potential association with microbial life. The variable detections of methane by the Curiosity rover, orbiters, and terrestrial telescopes, coupled with methane's short lifetime in the martian atmosphere, may imply an active gas source in the planet's subsurface, with migration and surface emission processes similar to those known on Earth as "gas seepage." Here, we review the variety of subsurface processes that could result in methane seepage on Mars. Such methane could originate from abiotic chemical reactions, thermogenic alteration of abiotic or biotic organic matter, and ancient or extant microbial metabolism. These processes can occur over a wide range of temperatures, in both sedimentary and igneous rocks, and together they enhance the possibility that significant amounts of methane could have formed on early Mars. Methane seepage to the surface would occur preferentially along faults and fractures, through focused macro-seeps and/or diffuse microseepage exhalations. Our work highlights the types of features on Mars that could be associated with methane release, including mud-volcano-like mounds in Acidalia or Utopia; proposed ancient springs in Gusev Crater, Arabia Terra, and Valles Marineris; and rims of large impact craters. These could have been locations of past macro-seeps and may still emit methane today. Microseepage could occur through faults along the dichotomy or fractures such as those at Nili Fossae, Cerberus Fossae, the Argyre impact, and those produced in serpentinized rocks. Martian microseepage would be extremely difficult to detect remotely yet could constitute a significant gas source. We emphasize that the most definitive detection of methane seepage from different release candidates would be best provided by measurements performed in the ground or at the ground-atmosphere interface by landers or rovers and that the technology for such detection is currently available. Key Words: Mars-Methane-Seepage-Clathrate-Fischer-Tropsch-Serpentinization. Astrobiology 17, 1233-1264.
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Affiliation(s)
| | - Giuseppe Etiope
- Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma 2, Roma, Italy, and Faculty of Environmental Science and Engineering, Babes-Bolyai University, Cluj-Napoca, Romania
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9
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Abstract
Spectral remote sensing in the visible/near-infrared (VNIR) and mid-IR (MIR) regions has enabled detection and characterisation of multiple clays and clay minerals on Earth and in the Solar System. Remote sensing on Earth poses the greatest challenge due to atmospheric absorptions that interfere with detection of surface minerals. Still, a greater variety of clay minerals have been observed on Earth than other bodies due to extensive aqueous alteration on our planet. Clay minerals have arguably been mapped in more detail on the planet Mars because they are not masked by vegetation on that planet and the atmosphere is less of a hindrance. Fe/Mg-smectite is the most abundant clay mineral on the surface of Mars and is also common in meteorites and comets where clay minerals are detected.
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Affiliation(s)
- Janice L Bishop
- SETI Institute, Carl Sagan Center, 189 Bernardo Ave, Suite 200, Mountain View, CA 94043, USA
| | | | - John Carter
- Institut d'Astrophysique Spatiale, CNRS/Paris-Sud University, Orsay, France
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10
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Viera-López G, Serrano-Muñoz A, Amigó-Vega J, Cruzata O, Altshuler E. Note: Planetary gravities made simple: Sample test of a Mars rover wheel. THE REVIEW OF SCIENTIFIC INSTRUMENTS 2017; 88:086107. [PMID: 28863644 DOI: 10.1063/1.4998261] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/07/2023]
Abstract
We introduce an instrument for a wide spectrum of experiments on gravities other than our planet's. It is based on a large Atwood machine where one of the loads is a bucket equipped with a single board computer and different sensors. The computer is able to detect the falling (or rising) and then the stabilization of the effective gravity and to trigger actuators depending on the experiment. Gravities within the range 0.4 g-1.2 g are easily achieved with acceleration noise of the order of 0.01 g. Under Martian gravity, we are able to perform experiments of approximately 1.5 s duration. The system includes features such as WiFi and a web interface with tools for the setup, monitoring, and data analysis of the experiment. We briefly show a case study in testing the performance of a model Mars rover wheel in low gravities.
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Affiliation(s)
- G Viera-López
- Group of Complex Systems and Statistical Physics, Physics Faculty, University of Havana, 10400 Havana, Cuba
| | - A Serrano-Muñoz
- Group of Complex Systems and Statistical Physics, Physics Faculty, University of Havana, 10400 Havana, Cuba
| | - J Amigó-Vega
- Group of Complex Systems and Statistical Physics, Physics Faculty, University of Havana, 10400 Havana, Cuba
| | - O Cruzata
- Laboratory of Laser Technology, IMRE, University of Havana, 10400 Havana, Cuba
| | - E Altshuler
- Group of Complex Systems and Statistical Physics, Physics Faculty, University of Havana, 10400 Havana, Cuba
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11
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Kereszturi A, Chatzitheodoridis E. Searching for the Source Crater of Nakhlite Meteorites. ORIGINS LIFE EVOL B 2016; 46:455-471. [PMID: 27021613 DOI: 10.1007/s11084-016-9498-x] [Citation(s) in RCA: 8] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/15/2015] [Accepted: 03/16/2016] [Indexed: 11/24/2022]
Abstract
We surveyed the Martian surface in order to identify possible source craters of the nakhlite Martian meteorites. We investigated rayed craters that are assumed to be younger than 11 Ma, on lava surfaces with a solidification age around 1.2 Ga. An area of 17.3 million km2 Amazonian lava plains was surveyed and 53 rayed craters were identified. Although most of them are smaller than the threshold limit that is estimated as minimum of launching fragments to possible Earth crossing trajectories, their observed size frequency distribution agrees with the expected areal density from cratering models characteristic for craters that are less than few tens of Ma old. We identified 6 craters larger than 3 km diameter constituting the potentially best source craters for nakhlites. These larger candidates are located mostly on a smooth lava surface, and in some cases, on the earlier fluvial-like channels. In three cases they are associated with fluidized ejecta lobes and rays - although the rays are faint in these craters, thus might be older than the other craters with more obvious rays. More work is therefore required to accurately estimate ages based on ray system for this purpose. A more detailed search should further link remote sensing Martian data with the in-situ laboratory analyses of Martian meteorites, especially in case of high altitude, steep terrains, where the crater rays seems to rarely survive several Ma.
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Affiliation(s)
- A Kereszturi
- Research Centre for Astronomy and Earth Sciences, Budapest, Hungary.
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12
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Hanna RD, Hamilton VE, Putzig NE. The complex relationship between olivine abundance and thermal inertia on Mars. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2016; 121:1293-1320. [PMID: 31007993 PMCID: PMC6469700 DOI: 10.1002/2015je004924] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/09/2023]
Abstract
We examine four olivine-bearing regions at a variety of spatial scales with thermal infrared, visible to near-infrared, and visible imagery data to investigate the hypothesis that the relationship between olivine abundance and thermal inertia (i.e., effective particle size) can be used to infer the occurrence of olivine chemical alteration during sediment production on Mars. As in previous work, Nili Fossae and Isidis Planitia show a positive correlation between thermal inertia and olivine abundance in Thermal Emission Spectrometer (TES) and Thermal Emission Imaging System (THEMIS) data, which could be interpreted as indicating olivine chemical weathering. However, geomorphological analysis reveals that relatively olivine-poor sediments are not derived from adjacent olivine-rich materials, and therefore, chemical weathering cannot be inferred based on the olivine-thermal inertia relationship alone. We identify two areas (Terra Cimmeria and Argyre Planitia) with significant olivine abundance and thermal inertias consistent with sand, but no adjacent rocky (parent) units having even greater olivine abundances. More broadly, global analysis with TES reveals that the most typical olivine abundance on Mars is ~5-7% and that olivine-bearing (5-25%) materials have a wide range of thermal inertias, commonly 25-600 J m-2 K-1 s-1/2. TES also indicates that the majority of olivine-rich (>25%) materials have apparent thermal inertias less than 400 J m-2 K-1 s-1/2. In summary, we find that the relationship between thermal inertia and olivine abundance alone cannot be used in infer olivine weathering in the examined areas, that olivine-bearing materials have a large range of thermal intertias, and therefore that a complex relationship between olivine abundance and thermal inertia exists on Mars.
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Affiliation(s)
- Romy D Hanna
- Jackson School of Geological Sciences, University of Texas at Austin, Austin, Texas, USA
| | - Victoria E Hamilton
- Department of Space Studies, Southwest Research Institute, Boulder, Colorado, USA
| | - Nathaniel E Putzig
- Department of Space Studies, Southwest Research Institute, Boulder, Colorado, USA
- Now at the Planetary Science Institute, Lakewood, Colorado, USA
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13
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Rodriguez JAP, Fairén AG, Tanaka KL, Zarroca M, Linares R, Platz T, Komatsu G, Miyamoto H, Kargel JS, Yan J, Gulick V, Higuchi K, Baker VR, Glines N. Tsunami waves extensively resurfaced the shorelines of an early Martian ocean. Sci Rep 2016; 6:25106. [PMID: 27196957 PMCID: PMC4872529 DOI: 10.1038/srep25106] [Citation(s) in RCA: 108] [Impact Index Per Article: 13.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/27/2015] [Accepted: 04/08/2016] [Indexed: 11/25/2022] Open
Abstract
It has been proposed that ~3.4 billion years ago an ocean fed by enormous catastrophic floods covered most of the Martian northern lowlands. However, a persistent problem with this hypothesis is the lack of definitive paleoshoreline features. Here, based on geomorphic and thermal image mapping in the circum-Chryse and northwestern Arabia Terra regions of the northern plains, in combination with numerical analyses, we show evidence for two enormous tsunami events possibly triggered by bolide impacts, resulting in craters ~30 km in diameter and occurring perhaps a few million years apart. The tsunamis produced widespread littoral landforms, including run-up water-ice-rich and bouldery lobes, which extended tens to hundreds of kilometers over gently sloping plains and boundary cratered highlands, as well as backwash channels where wave retreat occurred on highland-boundary surfaces. The ice-rich lobes formed in association with the younger tsunami, showing that their emplacement took place following a transition into a colder global climatic regime that occurred after the older tsunami event. We conclude that, on early Mars, tsunamis played a major role in generating and resurfacing coastal terrains.
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Affiliation(s)
- J Alexis P Rodriguez
- Planetary Science Institute, 1700 East Fort Lowell Road, Suite 106, Tucson, AZ 85719-2395, USA.,NASA Ames Research Center, Mail Stop 239-20, Moffett Field, CA, 94035, USA
| | - Alberto G Fairén
- Department of Planetology and Habitability, Centro de Astrobiología (CSIC-INTA), Madrid 28850, Spain.,Department of Astronomy, Cornell University, Ithaca, NY 14850, USA
| | - Kenneth L Tanaka
- Astrogeology Science Center, U.S. Geological Survey, Flagstaff, AZ 86001, USA
| | - Mario Zarroca
- External Geodynamics and Hydrogeology Group, Department of Geology, Autonomous University of Barcelona, 08193 Bellaterra, Barcelona, Spain
| | - Rogelio Linares
- External Geodynamics and Hydrogeology Group, Department of Geology, Autonomous University of Barcelona, 08193 Bellaterra, Barcelona, Spain
| | - Thomas Platz
- Planetary Science Institute, 1700 East Fort Lowell Road, Suite 106, Tucson, AZ 85719-2395, USA.,Planetary Sciences and Remote Sensing, Institute of Geological Sciences, Freie Universität Berlin, 12249 Berlin, Germany
| | - Goro Komatsu
- International Research School of Planetary Sciences, Università d'Annunzio, Viale Pindaro 42, 65127 Pescara, Italy
| | | | - Jeffrey S Kargel
- Department of Hydrology &Water Resources, University of Arizona, Tucson, AZ 85721, USA
| | - Jianguo Yan
- State Key Laboratory of Information Engineering in Surveying, Mapping and Remote Sensing, Wuhan University, Wuhan 430070, China
| | - Virginia Gulick
- NASA Ames Research Center, Mail Stop 239-20, Moffett Field, CA, 94035, USA.,SETI Institute, 189 Bernardo Avenue, Mountain View, CA 94043, USA
| | - Kana Higuchi
- Department of Planetology and Habitability, Centro de Astrobiología (CSIC-INTA), Madrid 28850, Spain
| | - Victor R Baker
- Department of Hydrology &Water Resources, University of Arizona, Tucson, AZ 85721, USA
| | - Natalie Glines
- NASA Ames Research Center, Mail Stop 239-20, Moffett Field, CA, 94035, USA.,SETI Institute, 189 Bernardo Avenue, Mountain View, CA 94043, USA
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Marshall CP, Olcott Marshall A. Challenges Analyzing Gypsum on Mars by Raman Spectroscopy. ASTROBIOLOGY 2015; 15:761-769. [PMID: 26317670 DOI: 10.1089/ast.2015.1334] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/04/2023]
Abstract
Raman spectroscopy can provide chemical information about organic and inorganic substances quickly and nondestructively with little to no sample preparation, thus making it an ideal instrument for Mars rover missions. The ESA ExoMars planetary mission scheduled for launch in 2018 will contain a miniaturized Raman spectrometer (RLS) as part of the Pasteur payload operating with a continuous wave (CW) laser emitting at 532 nm. In addition, NASA is independently developing two miniaturized Raman spectrometers for the upcoming Mars 2020 rover mission, one of which is a remote (stand-off) Raman spectrometer that uses a pulse-gated 532 nm excitation system (SuperCam). The other is an in situ Raman spectrometer that employs a CW excitation laser emitting at 248.6 nm (SHERLOC). Recently, it has been shown with analyses by Curiosity that Gale Crater contains significantly elevated concentrations of transition metals such as Cr and Mn. Significantly, these transition metals are known to undergo fluorescence emission in the visible portion of the electromagnetic spectrum. Consequently, samples containing these metals could be problematic for the successful acquisition of fluorescence-free Raman spectra when using a CW 532 nm excitation source. Here, we investigate one analog environment, with a similar mineralogy and sedimentology to that observed in martian environments, as well as elevated Cr contents, to ascertain the best excitation wavelength to successfully collect fluorescence-free spectra from Mars-like samples. Our results clearly show that CW near-infrared laser excitation emitting at 785 nm is better suited to the collection of fluorescence-free Raman spectra than would be a CW laser emitting at 532 nm.
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Affiliation(s)
- Craig P Marshall
- 1 Department of Geology, The University of Kansas , Lawrence, Kansas
- 2 Department of Chemistry, The University of Kansas , Lawrence, Kansas
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15
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Hutchinson IB, Ingley R, Edwards HGM, Harris L, McHugh M, Malherbe C, Parnell J. Raman spectroscopy on Mars: identification of geological and bio-geological signatures in Martian analogues using miniaturized Raman spectrometers. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2014; 372:rsta.2014.0204. [PMID: 25368350 DOI: 10.1098/rsta.2014.0204] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/04/2023]
Abstract
The first Raman spectrometers to be used for in situ analysis of planetary material will be launched as part of powerful, rover-based analytical laboratories within the next 6 years. There are a number of significant challenges associated with building spectrometers for space applications, including limited volume, power and mass budgets, the need to operate in harsh environments and the need to operate independently and intelligently for long periods of time (due to communication limitations). Here, we give an overview of the technical capabilities of the Raman instruments planned for future planetary missions and give a review of the preparatory work being pursued to ensure that such instruments are operated successfully and optimally. This includes analysis of extremophile samples containing pigments associated with biological processes, synthetic materials which incorporate biological material within a mineral matrix, planetary analogues containing low levels of reduced carbon and samples coated with desert varnish that incorporate both geo-markers and biomarkers. We discuss the scientific importance of each sample type and the challenges using portable/flight-prototype instrumentation. We also report on technical development work undertaken to enable the next generation of Raman instruments to reach higher levels of sensitivity and operational efficiency.
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Affiliation(s)
- Ian B Hutchinson
- Department of Physics and Astronomy, Space Research Centre, University of Leicester, Leicester LE1 7RH, UK
| | - Richard Ingley
- Department of Physics and Astronomy, Space Research Centre, University of Leicester, Leicester LE1 7RH, UK
| | - Howell G M Edwards
- Department of Physics and Astronomy, Space Research Centre, University of Leicester, Leicester LE1 7RH, UK
| | - Liam Harris
- Department of Physics and Astronomy, Space Research Centre, University of Leicester, Leicester LE1 7RH, UK
| | - Melissa McHugh
- Department of Physics and Astronomy, Space Research Centre, University of Leicester, Leicester LE1 7RH, UK
| | - Cedric Malherbe
- Department of Physics and Astronomy, Space Research Centre, University of Leicester, Leicester LE1 7RH, UK Department of Inorganic Analytical Chemistry, Chemistry Institute (B6c), University of Liège, 4000 Liège, Belgium
| | - J Parnell
- Department of Geology & Petroleum Geology, University of Aberdeen, King's College, Aberdeen AB24 3UE, UK
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16
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Platz T, Byrne PK, Massironi M, Hiesinger H. Volcanism and tectonism across the inner solar system: an overview. ACTA ACUST UNITED AC 2014. [DOI: 10.1144/sp401.22] [Citation(s) in RCA: 41] [Impact Index Per Article: 4.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/04/2022]
Abstract
AbstractVolcanism and tectonism are the dominant endogenic means by which planetary surfaces change. This book, in general, and this overview, in particular, aim to encompass the broad range in character of volcanism, tectonism, faulting and associated interactions observed on planetary bodies across the inner solar system – a region that includes Mercury, Venus, Earth, the Moon, Mars and asteroids. The diversity and breadth of landforms produced by volcanic and tectonic processes are enormous, and vary across the inventory of inner solar system bodies. As a result, the selection of prevailing landforms and their underlying formational processes that are described and highlighted in this review are but a primer to the expansive field of planetary volcanism and tectonism. In addition to this extended introductory contribution, this Special Publication features 21 dedicated research articles about volcanic and tectonic processes manifest across the inner solar system. Those articles are summarized at the end of this review.
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Affiliation(s)
- T. Platz
- Planetary Science Institute, 1700 East Fort Lowell Road, Tucson, AZ 85719-2395, USA
- Freie Universität Berlin, Institute of Geological Sciences, Planetary Sciences & Remote Sensing, Malteserstrasse 74-100, 12249 Berlin, Germany
| | - P. K. Byrne
- Lunar and Planetary Institute, Universities Space Research Association, 3600 Bay Area Boulevard, Houston, TX 77058, USA
- Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road NW, Washington, DC 20015-1305, USA
| | - M. Massironi
- Dipartimento di Geoscienze, Universita' degli Studi di Padova, via G. Gradenigo 6, 35131 Padova, Italy
| | - H. Hiesinger
- Institut für Planetologie, Westfälische Wilhelms-Universität Münster, Wilhelm-Klemm-Strasse 10, 48149 Münster, Germany
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17
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Sanchez-Valdes D, Alvarez-Alvarez A, Trivino G. Linguistic description about circular structures of the Mars’ surface. Appl Soft Comput 2013. [DOI: 10.1016/j.asoc.2013.08.003] [Citation(s) in RCA: 16] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
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18
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19
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Edwards CS, Christensen PR. Microscopic emission and reflectance thermal infrared spectroscopy: instrumentation for quantitative in situ mineralogy of complex planetary surfaces. APPLIED OPTICS 2013; 52:2200-2217. [PMID: 23670748 DOI: 10.1364/ao.52.002200] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/09/2012] [Accepted: 02/14/2013] [Indexed: 06/02/2023]
Abstract
The diversity of investigations of planetary surfaces, especially Mars, using in situ instrumentation over the last decade is unprecedented in the exploration history of our solar system. The style of instrumentation that landed spacecraft can support is dependent on several parameters, including mass, power consumption, instrument complexity, cost, and desired measurement type (e.g., chemistry, mineralogy, petrology, morphology, etc.), all of which must be evaluated when deciding an appropriate spacecraft payload. We present a laboratory technique for a microscopic emission and reflectance spectrometer for the analysis of martian analog materials as a strong candidate for the next generation of in situ instruments designed to definitively assess sample mineralogy and petrology while preserving geologic context. We discuss the instrument capabilities, signal and noise, and overall system performance. We evaluate the ability of this instrument to quantitatively determine sample mineralogy, including bulk mineral abundances. This capability is greatly enhanced. Whereas the number of mineral components observed from existing emission spectrometers is high (often >5 to 10 depending on the number of accessory and alteration phases present), the number of mineral components at any microscopic measurement spot is low (typically <2 to 3). Since this style of instrument is based on a long heritage of thermal infrared emission spectrometers sent to orbit (the thermal emission spectrometer), sent to planetary surfaces [the mini-thermal emission spectrometers (mini-TES)], and evaluated in laboratory environments (e.g., the Arizona State University emission spectrometer laboratory), direct comparisons to existing data are uniquely possible with this style of instrument. The ability to obtain bulk mineralogy and atmospheric data, much in the same manner as the mini-TESs, is of significant additional value and maintains the long history of atmospheric monitoring for Mars. Miniaturization of this instrument has also been demonstrated, as the same microscope objective has been mounted to a flight-spare mini-TES. Further miniaturization of this instrument is straightforward with modern electronics, and the development of this instrument as an arm-mounted device is the end goal.
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Affiliation(s)
- C S Edwards
- California Institute of Technology, Division of Geological and Planetary Sciences,Pasadena, California 91125, USA.
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Ody A, Poulet F, Langevin Y, Bibring JP, Bellucci G, Altieri F, Gondet B, Vincendon M, Carter J, Manaud N. Global maps of anhydrous minerals at the surface of Mars from OMEGA/MEx. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2012je004117] [Citation(s) in RCA: 114] [Impact Index Per Article: 9.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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21
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Mangold N, Adeli S, Conway S, Ansan V, Langlais B. A chronology of early Mars climatic evolution from impact crater degradation. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2011je004005] [Citation(s) in RCA: 100] [Impact Index Per Article: 8.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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22
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Beuthe M, Le Maistre S, Rosenblatt P, Pätzold M, Dehant V. Density and lithospheric thickness of the Tharsis Province from MEX MaRS and MRO gravity data. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2011je003976] [Citation(s) in RCA: 27] [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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23
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Edwards CS, Nowicki KJ, Christensen PR, Hill J, Gorelick N, Murray K. Mosaicking of global planetary image datasets: 1. Techniques and data processing for Thermal Emission Imaging System (THEMIS) multi-spectral data. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010je003755] [Citation(s) in RCA: 128] [Impact Index Per Article: 9.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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24
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Cousins CR, Crawford IA. Volcano-ice interaction as a microbial habitat on Earth and Mars. ASTROBIOLOGY 2011; 11:695-710. [PMID: 21877914 DOI: 10.1089/ast.2010.0550] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/31/2023]
Abstract
Volcano-ice interaction has been a widespread geological process on Earth that continues to occur to the present day. The interaction between volcanic activity and ice can generate substantial quantities of liquid water, together with steep thermal and geochemical gradients typical of hydrothermal systems. Environments available for microbial colonization within glaciovolcanic systems are wide-ranging and include the basaltic lava edifice, subglacial caldera meltwater lakes, glacier caves, and subsurface hydrothermal systems. There is widespread evidence of putative volcano-ice interaction on Mars throughout its history and at a range of latitudes. Therefore, it is possible that life on Mars may have exploited these habitats, much in the same way as has been observed on Earth. The sedimentary and mineralogical deposits resulting from volcano-ice interaction have the potential to preserve evidence of any indigenous microbial populations. These include jökulhlaup (subglacial outflow) sedimentary deposits, hydrothermal mineral deposits, basaltic lava flows, and subglacial lacustrine deposits. Here, we briefly review the evidence for volcano-ice interactions on Mars and discuss the geomicrobiology of volcano-ice habitats on Earth. In addition, we explore the potential for the detection of these environments on Mars and any biosignatures these deposits may contain.
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Affiliation(s)
- Claire R Cousins
- Department of Earth and Planetary Sciences, Birkbeck College, University of London, London, UK.
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25
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Tirsch D, Jaumann R, Pacifici A, Poulet F. Dark aeolian sediments in Martian craters: Composition and sources. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2009je003562] [Citation(s) in RCA: 62] [Impact Index Per Article: 4.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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26
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Buczkowski DL, Murchie S, Clark R, Seelos K, Seelos F, Malaret E, Hash C. Investigation of an Argyre basin ring structure using Mars Reconnaissance Orbiter/Compact Reconnaissance Imaging Spectrometer for Mars. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2009je003508] [Citation(s) in RCA: 21] [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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Burr DM, Williams RME, Wendell KD, Chojnacki M, Emery JP. Inverted fluvial features in the Aeolis/Zephyria Plana region, Mars: Formation mechanism and initial paleodischarge estimates. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2009je003496] [Citation(s) in RCA: 81] [Impact Index Per Article: 5.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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29
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Abstract
Organics are expected to exist on Mars based on meteorite infall, in situ production, and any possible biological sources. Yet they have not been detected on the martian surface; are they there, or are we not capable enough to detect them? The Viking gas chromatograph-mass spectrometer did not detect organics in the headspace of heated soil samples with a detection limit of parts per billion. This null result strongly influenced the interpretation of the reactivity seen in the Viking biology experiments and led to the conclusion that life was not present and, instead, that there was some chemical reactivity in the soil. The detection of perchlorates in the martian soil by instruments on the Phoenix lander and the reports of methane in the martian atmosphere suggest that it may be time to reconsider the question of organics. The high-temperature oxidizing properties of perchlorate will promote combustion of organics in pyrolytic experiments and may have affected the ability of both Phoenix's organic analysis experiment and the Viking mass spectrometer experiments to detect organics. So the question of organics on Mars remains open. A primary focus of the upcoming Mars Science Laboratory will be the detection and identification of organic molecules by means of thermal volatilization, followed by gas chromatography-mass spectrometry--as was done on Viking. However, to enhance organic detectability, some of the samples will be processed with liquid derivatization agents that will dissolve organics from the soil before pyrolysis, which may separate them from the soil perchlorates. Nonetheless, the problem of organics on Mars is not solved, and for future missions other organic detection techniques should therefore be considered as well.
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Affiliation(s)
- Inge L ten Kate
- NASA Goddard Space Flight Center, Greenbelt, Maryland 20771, USA.
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The Mars Astrobiology Explorer-Cacher (MAX-C): a potential rover mission for 2018. Final report of the Mars Mid-Range Rover Science Analysis Group (MRR-SAG) October 14, 2009. ASTROBIOLOGY 2010; 10:127-163. [PMID: 20298148 DOI: 10.1089/ast.2010.0462] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/29/2023]
Abstract
This report documents the work of the Mid-Range Rover Science Analysis Group (MRR-SAG), which was assigned to formulate a concept for a potential rover mission that could be launched to Mars in 2018. Based on programmatic and engineering considerations as of April 2009, our deliberations assumed that the potential mission would use the Mars Science Laboratory (MSL) sky-crane landing system and include a single solar-powered rover. The mission would also have a targeting accuracy of approximately 7 km (semimajor axis landing ellipse), a mobility range of at least 10 km, and a lifetime on the martian surface of at least 1 Earth year. An additional key consideration, given recently declining budgets and cost growth issues with MSL, is that the proposed rover must have lower cost and cost risk than those of MSL--this is an essential consideration for the Mars Exploration Program Analysis Group (MEPAG). The MRR-SAG was asked to formulate a mission concept that would address two general objectives: (1) conduct high priority in situ science and (2) make concrete steps toward the potential return of samples to Earth. The proposed means of achieving these two goals while balancing the trade-offs between them are described here in detail. We propose the name Mars Astrobiology Explorer-Cacher(MAX-C) to reflect the dual purpose of this potential 2018 rover mission.
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31
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Cabrol NA, Grin EA, Chong G, Minkley E, Hock AN, Yu Y, Bebout L, Fleming E, Häder DP, Demergasso C, Gibson J, Escudero L, Dorador C, Lim D, Woosley C, Morris RL, Tambley C, Gaete V, Galvez ME, Smith E, Uskin-Peate I, Salazar C, Dawidowicz G, Majerowicz J. The High-Lakes Project. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008jg000818] [Citation(s) in RCA: 37] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Nathalie A. Cabrol
- Space Science and Astrobiology Division; NASA Ames Research Center; Moffett Field California USA
- SETI Carl Sagan Center; Mountain View California USA
| | - Edmond A. Grin
- Space Science and Astrobiology Division; NASA Ames Research Center; Moffett Field California USA
- SETI Carl Sagan Center; Mountain View California USA
| | - Guillermo Chong
- Centro de Investigación Científica y Tecnológica para Minería; Santiago Chile
| | - Edwin Minkley
- Department of Biological Sciences; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Andrew N. Hock
- Department of Earth and Space Sciences; University of California; Los Angeles California USA
| | - Youngseob Yu
- Department of Civil and Environmental Engineering; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Leslie Bebout
- Space Science and Astrobiology Division; NASA Ames Research Center; Moffett Field California USA
| | - Erich Fleming
- Space Science and Astrobiology Division; NASA Ames Research Center; Moffett Field California USA
| | - Donat P. Häder
- Department Botanik; University of Erlangen; Erlangen Germany
| | - Cecilia Demergasso
- Centro de Biotecnología; Universidad Católica del Norte; Antofagasta Chile
| | - John Gibson
- Marine Research Laboratories, Tasmanian Aquaculture and Fisheries Institute; University of Tasmania; Hobart, Tasmania Australia
| | - Lorena Escudero
- Centro de Investigación Científica y Tecnológica para Minería; Santiago Chile
| | - Cristina Dorador
- Centro de Biotecnología; Universidad Católica del Norte; Antofagasta Chile
| | - Darlene Lim
- Space Science and Astrobiology Division; NASA Ames Research Center; Moffett Field California USA
- SETI Carl Sagan Center; Mountain View California USA
| | - Clayton Woosley
- Space Science and Astrobiology Division; NASA Ames Research Center; Moffett Field California USA
- SETI Carl Sagan Center; Mountain View California USA
| | | | | | - Victor Gaete
- Departamento de Química; Universidad Católica del Norte; Antofagasta Chile
| | | | - Eric Smith
- Discoverer Ketty Lund Exploration Vessel; Key West Florida USA
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Edwards CS, Bandfield JL, Christensen PR, Fergason RL. Global distribution of bedrock exposures on Mars using THEMIS high-resolution thermal inertia. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2009je003363] [Citation(s) in RCA: 65] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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33
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Leverington DW. Reconciling channel formation processes with the nature of elevated outflow systems at Ophir and Aurorae Plana, Mars. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2009je003398] [Citation(s) in RCA: 27] [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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Osterrothová K, Jehlicka J. Raman spectroscopic identification of usnic acid in hydrothermal minerals as a potential Martian analogue. SPECTROCHIMICA ACTA. PART A, MOLECULAR AND BIOMOLECULAR SPECTROSCOPY 2009; 73:576-580. [PMID: 18980859 DOI: 10.1016/j.saa.2008.09.005] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/25/2008] [Accepted: 09/11/2008] [Indexed: 05/26/2023]
Abstract
Raman spectroscopy using 785 nm excitation was tested as a nondestructive method for determining the presence of the potential biomarker, usnic acid, in experimentally prepared mineral matrices. Investigated samples consisting of usnic acid mixed with powdered hydrothermal minerals, gypsum and calcite were studied. Various concentrations of usnic acid in the mineral matrix were studied to determine the detection limits of this biomarker. Usnic acid was mixed with gypsum (respectively, calcite) and covered by a UV-transparent crystal of gypsum (CaSO(4) x 2 H(2)O), thereby creating artificial inclusions similar to those which could be present in Martian minerals. A Raman usnic acid signal at the concentration level as low as 1 g kg(-1) was obtained in the powdered mineral matrix and 5 g kg(-1) when analyzed through the monocrystal. The number of registered usnic acid key Raman bands was dependent on the particular mineral matrix. If a similar concentration of usnic acid could persist in Martian samples, then Raman spectroscopy will be able to identify it. Obtained results will aid both in situ Raman analyses on Mars and on Earth.
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Affiliation(s)
- Katerina Osterrothová
- Institute of Geochemistry, Mineralogy and Mineral Resources, Faculty of Science, Charles University in Prague, Albertov 6, 128 43 Prague 2, Czech Republic.
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Affiliation(s)
- Michael P. Lamb
- Department of Earth and Planetary Science, University of California, Berkeley, California 94720, USA
| | - William E. Dietrich
- Department of Earth and Planetary Science, University of California, Berkeley, California 94720, USA
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37
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Fergason RL, Christensen PR. Formation and erosion of layered materials: Geologic and dust cycle history of eastern Arabia Terra, Mars. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002973] [Citation(s) in RCA: 24] [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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38
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Williams JP, Nimmo F, Moore WB, Paige DA. The formation of Tharsis on Mars: What the line-of-sight gravity is telling us. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003050] [Citation(s) in RCA: 22] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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39
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Tornabene LL, Moersch JE, McSween HY, Hamilton VE, Piatek JL, Christensen PR. Surface and crater-exposed lithologic units of the Isidis Basin as mapped by coanalysis of THEMIS and TES derived data products. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002988] [Citation(s) in RCA: 75] [Impact Index Per Article: 4.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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40
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Mangold N, Ansan V, Masson P, Quantin C, Neukum G. Geomorphic study of fluvial landforms on the northern Valles Marineris plateau, Mars. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002985] [Citation(s) in RCA: 58] [Impact Index Per Article: 3.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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41
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Ansan V, Mangold N, Masson P, Gailhardis E, Neukum G. Topography of valley networks on Mars from Mars Express High Resolution Stereo Camera digital elevation models. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002986] [Citation(s) in RCA: 43] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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42
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Koeppen WC, Hamilton VE. Global distribution, composition, and abundance of olivine on the surface of Mars from thermal infrared data. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002984] [Citation(s) in RCA: 169] [Impact Index Per Article: 10.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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43
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Keszthelyi L, Jaeger W, McEwen A, Tornabene L, Beyer RA, Dundas C, Milazzo M. High Resolution Imaging Science Experiment (HiRISE) images of volcanic terrains from the first 6 months of the Mars Reconnaissance Orbiter Primary Science Phase. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002968] [Citation(s) in RCA: 88] [Impact Index Per Article: 5.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Sutter B, Dalton JB, Ewing SA, Amundson R, McKay CP. Terrestrial analogs for interpretation of infrared spectra from the Martian surface and subsurface: Sulfate, nitrate, carbonate, and phyllosilicate-bearing Atacama Desert soils. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006jg000313] [Citation(s) in RCA: 30] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- B. Sutter
- SETI Institute; NASA Ames Research Center; Moffett Field California USA
| | - J. B. Dalton
- SETI Institute; NASA Ames Research Center; Moffett Field California USA
| | - S. A. Ewing
- Division of Ecosystem Sciences; University of California; Berkeley California USA
| | - R. Amundson
- Division of Ecosystem Sciences; University of California; Berkeley California USA
| | - C. P. McKay
- NASA Ames Research Center; Moffett Field California USA
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45
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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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46
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Wilson SA, Howard AD, Moore JM, Grant JA. Geomorphic and stratigraphic analysis of Crater Terby and layered deposits north of Hellas basin, Mars. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002830] [Citation(s) in RCA: 96] [Impact Index Per Article: 5.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Affiliation(s)
- Sharon A. Wilson
- Center for Earth and Planetary Studies, National Air and Space Museum; Smithsonian Institution; Washington D. C. USA
| | - Alan D. Howard
- Department of Environmental Sciences; University of Virginia; Charlottesville Virginia USA
| | - Jeffrey M. Moore
- Space Sciences Division; NASA Ames Research Center; Moffett Field California USA
| | - John A. Grant
- Center for Earth and Planetary Studies, National Air and Space Museum; Smithsonian Institution; Washington D. C. USA
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47
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Mangold N, Poulet F, Mustard JF, Bibring JP, Gondet B, Langevin Y, Ansan V, Masson P, Fassett C, Head JW, Hoffmann H, Neukum G. Mineralogy of the Nili Fossae region with OMEGA/Mars Express data: 2. Aqueous alteration of the crust. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002835] [Citation(s) in RCA: 134] [Impact Index Per Article: 7.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- N. Mangold
- Laboratoire IDES; UMR8148 CNRS and Université Paris-Sud; Orsay France
| | - F. Poulet
- Institut d'Astrophysique Spatiale; CNRS/Université Paris-Sud; Orsay France
| | - J. F. Mustard
- Department of Geological Sciences; Brown University; Providence Rhode Island USA
| | - J.-P. Bibring
- Institut d'Astrophysique Spatiale; CNRS/Université Paris-Sud; Orsay France
| | - B. Gondet
- Institut d'Astrophysique Spatiale; CNRS/Université Paris-Sud; Orsay France
| | - Y. Langevin
- Institut d'Astrophysique Spatiale; CNRS/Université Paris-Sud; Orsay France
| | - V. Ansan
- Laboratoire IDES; UMR8148 CNRS and Université Paris-Sud; Orsay France
| | - Ph. Masson
- Laboratoire IDES; UMR8148 CNRS and Université Paris-Sud; Orsay France
| | - C. Fassett
- Department of Geological Sciences; Brown University; Providence Rhode Island USA
| | - J. W. Head
- Department of Geological Sciences; Brown University; Providence Rhode Island USA
| | - H. Hoffmann
- Institut für Weltraumsensorik; DLR; Berlin Germany
| | - G. Neukum
- Institut für Geologische Wissenschaften; Freie Universität Berlin; Berlin Germany
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48
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Loizeau D, Mangold N, Poulet F, Bibring JP, Gendrin A, Ansan V, Gomez C, Gondet B, Langevin Y, Masson P, Neukum G. Phyllosilicates in the Mawrth Vallis region of Mars. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002877] [Citation(s) in RCA: 129] [Impact Index Per Article: 7.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- D. Loizeau
- Laboratoire IDES; Université Paris XI; Orsay France
| | - N. Mangold
- Laboratoire IDES; Université Paris XI; Orsay France
| | - F. Poulet
- Institut d'Astrophysique Spatiale; Université Paris XI; Orsay France
| | - J.-P. Bibring
- Institut d'Astrophysique Spatiale; Université Paris XI; Orsay France
| | - A. Gendrin
- Institut d'Astrophysique Spatiale; Université Paris XI; Orsay France
| | - V. Ansan
- Laboratoire IDES; Université Paris XI; Orsay France
| | - C. Gomez
- Institut d'Astrophysique Spatiale; Université Paris XI; Orsay France
| | - B. Gondet
- Institut d'Astrophysique Spatiale; Université Paris XI; Orsay France
| | - Y. Langevin
- Institut d'Astrophysique Spatiale; Université Paris XI; Orsay France
| | - P. Masson
- Laboratoire IDES; Université Paris XI; Orsay France
| | - G. Neukum
- Institut für Geologische Wissenschaften; Freie Universität Berlin; Berlin Germany
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49
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Poulet F, Gomez C, Bibring JP, Langevin Y, Gondet B, Pinet P, Belluci G, Mustard J. Martian surface mineralogy from Observatoire pour la Minéralogie, l'Eau, les Glaces et l'Activité on board the Mars Express spacecraft (OMEGA/MEx): Global mineral maps. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002840] [Citation(s) in RCA: 167] [Impact Index Per Article: 9.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- F. Poulet
- Institut d'Astrophysique Spatiale; CNRS/Université Paris-Sud; Orsay France
| | - C. Gomez
- Institut d'Astrophysique Spatiale; CNRS/Université Paris-Sud; Orsay France
| | - J.-P. Bibring
- Institut d'Astrophysique Spatiale; CNRS/Université Paris-Sud; Orsay France
| | - Y. Langevin
- Institut d'Astrophysique Spatiale; CNRS/Université Paris-Sud; Orsay France
| | - B. Gondet
- Institut d'Astrophysique Spatiale; CNRS/Université Paris-Sud; Orsay France
| | - P. Pinet
- Laboratoire Dynamique Terrestre et Planétaire/UMR5562; Centre National de la Recherche Scientifique; Toulouse France
| | - G. Belluci
- Istituto Nazionale Di Astrofiscia dello Spazio Interplanetario; Rome Italy
| | - J. Mustard
- Geological Sciences; Brown University; Providence Rhode Island USA
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50
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Fishbaugh KE, Poulet F, Chevrier V, Langevin Y, Bibring JP. On the origin of gypsum in the Mars north polar region. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002862] [Citation(s) in RCA: 77] [Impact Index Per Article: 4.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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