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1. Tree regrowth duration map from LCMAP collection 1.0 land cover products in the conterminous United States, 1985–2017

Author

Qiang Zhou, George Xian, Josephine Horton, Danika Wellington, Grant Domke, Roger Auch, Congcong Li, and Zhe Zhu

Subjects
tree regrowth, landsat, land cover, lcmap, Mathematical geography. Cartography, GA1-1776, Environmental sciences, GE1-350
Abstract

Forest covers about one-third of the land area of the conterminous United States (CONUS) and plays an important role in offsetting carbon emissions and supporting local economies. Growing interest in forests as relatively cost-effective nature-based climate solutions, particularly restoration and reforestation activities has increased the demand for information on forest regrowth and recovery following natural and anthropogenic disturbances (e.g. fire, harvest, or thinning). However, a wall-to-wall mapping of the CONUS tree regrowth duration at an annual time interval and 30-m resolution is still challenging. In this study, we utilized the annual land cover products to develop a dataset to quantify forest regrowth duration for CONUS over 1985–2017. The land cover data used to derive the tree regrowth duration map is from the primary land cover product in the U.S. Geological Survey’s Land Change Monitoring, Assessment, and Projection (LCMAP) collection. The LCMAP product used all available Landsat images to detect disturbances over forest and classify Grass/Shrub to Tree Cover transitions on an annual basis. The average regrowth duration was then calculated for each pixel. The regrowth duration map was validated using human-interpreted annual reference data that were collected independently. The validation results show 1 year of underestimation and 6-year standard deviation of error between the reference data and the regrowth duration map. In southeastern CONUS, where major tree regrowth activities have been observed, our map showed higher accuracy with less than one-year bias and 3.6 years standard deviation of error. Forest in the southeast took around 5 years to recover, which was faster than other regions of CONUS. Many pixels had multiple disturbances during the 33-year study period in the region. The spatial pattern of the tree regrowth indicated intense harvesting activities in this region. The Pacific Northwest coast region was the second main area of tree regrowth, but this region often took multiple decades to recover. Given the increasing interest in forests as nature-based climate solutions, the tree regrowth duration map can be used to assess reforestation activities as well as forest recovery following natural disturbance and harvesting.

Published
2022
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2. Development of the LCMAP annual land cover product across Hawaiʻi

Author

Congcong Li, George Xian, Danika Wellington, Kelcy Smith, Josephine Horton, and Qiang Zhou

Subjects
Training samples, Coverage, Time series classification, Hawaiʻi, Physical geography, GB3-5030, Environmental sciences, GE1-350
Abstract

Following the completion of land cover and change (LCC) products for the conterminous United States (CONUS), the U.S. Geological Survey's (USGS’s) Land Change Monitoring, Assessment, and Projection initiative has broadened the capability of characterizing continuous historical land change across the full Landsat records for Hawaiʻi at 30-meter resolution. One of the challenges of implementing the LCMAP framework to process annual land cover maps in Hawaiʻi is to collect sufficient high-quality training data. Although multiple datasets depicting land cover information are available in Hawaiʻi, they covered limited time frames and were produced from various remote sensing sources with different, classification categories, spatial resolution, and mapping accuracies. No solo product is suitable to provide LCMAP training data labels on its own. In this paper, we focused on enhancing the LCMAP training datasets to generate land cover products from 2000 to 2019 in Hawaiʻi. A total of 200 independent reference data plots were generated and manually interpreted for validating the mapping results produced by the training datasets. The results revealed that using the appropriate filter of multiple products as training data pools improved the classification model performance. The effect of training datasets (e.g., spatial coverage, quality) on accuracies for different land cover types were summarized. The LCMAP land surface change products for Hawaiʻi are available at https://doi.org/10.5066/P91E8M23.

Published
2022
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4. Toward More Realistic Simulation and Prediction of Dust Storms on Mars

Author

Claire E Newman, Mackenzie Day, Francesca Esposito, Steven J Greybush, Melinda Kahre, Mathieu Lapotre, Ralph D Lorenz, Michael A Mischna, Alexey Pankine, Isaac B Smith, Aymeric Spiga, Orkun Temel, Paulina Wolkenberg, Tanguy Bertrand, Manuel De La Torre Juarez, Lori Fenton, Scott D Guzewich, Ozgur Karatekin, Christopher Lee, German Martinez Martinez, Luca Montabone, Jorge Pla-garcia, Michael D. Smith, Christy Swann, Daniel Viudez-moreiras, Gerhard Wurm, Joseph Battalio, Meredith K Elrod, Claus Gebhardt, Henrik Kahanpaa, Brian Jackson, Stephen R. Lewis, Javier Martin-Torres, Lynn Neakrase, Peter L. Read, Alejandro Soto, Leslie Tamppari, Danika Wellington, and Maria Paz Zorzano Mier

Subjects
Lunar And Planetary Science And Exploration
Abstract

Major (regional and global)dust storms dominate weather and climate variability on present-day Mars. Absorption and scattering of visible and IR radiation by dust strongly affect the thermal state of the thin Mars atmosphere, while dust provides condensation nuclei for water and CO2 cloud particles, which also affect radiative fluxes. Global dust storms (GDS) occur ~three times per Mars decade and to date have been observed in only northern fall and winter,when the global circulation is strongest. Tenfold increases in column dust opacity are typical during GDS, with intense vertical motions transporting dust to far higher altitudes than usual. The key processes and feedbacks that produce GDS remain poorly understood, hence current atmospheric models fail to self-consistently simulate observed dust storm activity. This means we have no predictive capability for when GDS may occur, either now or in Mars’s past. And crucially, due to the huge impact of GDS on the atmosphere and surface, our lack of ability to simulate realistic dust storms has major implications for Mars science and exploration: from understanding the present climate (§2.1),to modeling past climates and water cycles (§2.2), to exploring how wind, water, and dust cycles varied over time to interpret geology and assess potential habitability(§2.3), to quantifying and mitigating risks posed to Mars missions (§2.4)

Published
2020

6. Comparison of novelty detection methods for multispectral images in rover-based planetary exploration missions

Author

James F. Bell, S. Jacob, Heni Ben Amor, Kiri L. Wagstaff, Chiman Kwan, Danika Wellington, Paul Horton, Brian D. Bue, and Hannah Kerner

Subjects
010504 meteorology & atmospheric sciences, Mean squared error, Computer Networks and Communications, business.industry, Computer science, Multispectral image, Hyperspectral imaging, 02 engineering and technology, Mars Exploration Program, Machine learning, computer.software_genre, 01 natural sciences, Novelty detection, Space exploration, Computer Science Applications, Principal component analysis, 0202 electrical engineering, electronic engineering, information engineering, Unsupervised learning, 020201 artificial intelligence & image processing, Artificial intelligence, business, computer, 0105 earth and related environmental sciences, Information Systems
Abstract

Science teams for rover-based planetary exploration missions like the Mars Science Laboratory Curiosity rover have limited time for analyzing new data before making decisions about follow-up observations. There is a need for systems that can rapidly and intelligently extract information from planetary instrument datasets and focus attention on the most promising or novel observations. Several novelty detection methods have been explored in prior work for three-channel color images and non-image datasets, but few have considered multispectral or hyperspectral image datasets for the purpose of scientific discovery. We compared the performance of four novelty detection methods—Reed Xiaoli (RX) detectors, principal component analysis (PCA), autoencoders, and generative adversarial networks (GANs)—and the ability of each method to provide explanatory visualizations to help scientists understand and trust predictions made by the system. We show that pixel-wise RX and autoencoders trained with structural similarity (SSIM) loss can detect morphological novelties that are not detected by PCA, GANs, and mean squared error autoencoders, but that the latter methods are better suited for detecting spectral novelties—i.e., the best method for a given setting depends on the type of novelties that are sought. Additionally, we find that autoencoders provide the most useful explanatory visualizations for enabling users to understand and trust model detections, and that existing GAN approaches to novelty detection may be limited in this respect.

Published
2020

7. Spectral diversity of rocks and soils in Mastcam observations along the Curiosity rover’s traverse in Gale crater, Mars

Author

Melissa S. Rice, Christina Seeger, Jim Bell, Fred Calef, Michael St. Clair, Alivia Eng, Abigail A. Fraeman, Cory Hughes, Briony Horgan, Samantha Jacob, Jeff Johnson, Hannah Kerner, Kjartan Kinch, Mark Lemmon, Chase Million, Mason Starr, and Danika Wellington

Subjects
SPECTROSCOPY, IDENTIFICATION, MINERALOGY, EXPLORATION ROVERS, DUST, REFLECTANCE SPECTRA, SCIENCE, Mars exploration, BAGNOLD DUNES, Mars geology, image processing, Geophysics, reflectance spectroscopy, Space and Planetary Science, Geochemistry and Petrology, ENDEAVOR CRATER, multispectral imaging, Earth and Planetary Sciences (miscellaneous), VNIR MULTISPECTRAL OBSERVATIONS
Abstract

The Mars Science Laboratory Curiosity rover has explored over 400 m of vertical stratigraphy within Gale crater to date. These fluvio-deltaic, lacustrine, and aeolian strata have been well-documented by Curiosity's in situ and remote science instruments, including the Mast Camera (Mastcam) pair of multispectral imagers. Mastcam visible to near-infrared spectra can broadly distinguish between iron phases and oxidation states, and in combination with chemical data from other instruments, Mastcam spectra can help constrain mineralogy, depositional origin, and diagenesis. However, no traverse-scale analysis of Mastcam multispectral data has yet been performed. We compiled a database of Mastcam spectra from >600 multispectral observations and quantified spectral variations across Curiosity's traverse through Vera Rubin ridge (sols 0-2302). From principal component analysis and an examination of spectral parameters, we identified nine rock spectral classes and five soil spectral classes. Rock classes are dominated by spectral differences attributed to hematite and other oxides (due to variations in grain size, composition, and abundance) and are mostly confined to specific stratigraphic members. Soil classes fall along a mixing line between soil spectra dominated by fine-grained Fe-oxides and those dominated by olivine-bearing sands. By comparing trends in soil versus rock spectra, we find that locally derived sediments are not significantly contributing to the spectra of soils. Rather, varying contributions of dark, mafic sands from the active Bagnold Dune field is the primary spectral characteristic of soils. These spectral classes and their trends with stratigraphy provide a basis for comparison in Curiosity's ongoing exploration of Gale crater.

Published
2022

8. Implementation of the CCDC algorithm to produce the LCMAP Collection 1.0 annual land surface change product

Author

George Z. Xian, Kelcy Smith, Danika Wellington, Josephine Horton, Qiang Zhou, Congcong Li, Roger Auch, Jesslyn F. Brown, Zhe Zhu, and Ryan R. Reker

Subjects
Environmental sciences, QE1-996.5, General Earth and Planetary Sciences, GE1-350, Geology
Abstract

The increasing availability of high-quality remote sensing data and advanced technologies has spurred land cover mapping to characterize land change from local to global scales. However, most land change datasets either span multiple decades at a local scale or cover limited time over a larger geographic extent. Here, we present a new land cover and land surface change dataset created by the Land Change Monitoring, Assessment, and Projection (LCMAP) program over the conterminous United States (CONUS). The LCMAP land cover change dataset consists of annual land cover and land cover change products over the period 1985–2017 at a 30 m resolution using Landsat and other ancillary data via the Continuous Change Detection and Classification (CCDC) algorithm. In this paper, we describe our novel approach to implement the CCDC algorithm to produce the LCMAP product suite composed of five land cover products and five products related to land surface change. The LCMAP land cover products were validated using a collection of ∼25 000 reference samples collected independently across CONUS. The overall agreement for all years of the LCMAP primary land cover product reached 82.5 %. The LCMAP products are produced through the LCMAP Information Warehouse and Data Store (IW+DS) and shared Mesos cluster systems that can process, store, and deliver all datasets for public access. To our knowledge, this is the first set of published 30 m annual land change datasets that include land cover, land cover change, and spectral change spanning from the 1980s to the present for the United States. The LCMAP product suite provides useful information for land resource management and facilitates studies to improve the understanding of terrestrial ecosystems and the complex dynamics of the Earth system. The LCMAP system could be implemented to produce global land change products in the future. The LCMAP products introduced in this paper are freely available at https://doi.org/10.5066/P9W1TO6E (LCMAP, 2021).

Published
2022

10. Large Dust Aerosol Sizes Seen During the 2018 Martian Global Dust Event by the Curiosity Rover

Author

S. Jacob, Mark T. Lemmon, Scott D. Guzewich, A. De Vicente-Retortillo, James F. Bell, German Martinez, Danika Wellington, Timothy H. McConnochie, and Michael D. Smith

Subjects
Effective radius, Martian, education.field_of_study, Opacity, Population, Mars Exploration Program, Atmospheric sciences, complex mixtures, respiratory tract diseases, Aerosol, Atmosphere, Geophysics, General Earth and Planetary Sciences, Solstice, Environmental science, education
Abstract

Mars' atmosphere typically supports dust aerosol with an effective radius near 1.5 μm, varying from ~1 μm during low dust times near northern summer solstice to ~2 μm during higher dust times in southern spring and summer. After global dust events, size variations outside this range have not previously been observed. We report on imaging and spectral observations by the Curiosity rover through the 2018 global dust event. These observations show that the dust effective radius was seasonally normal prior to the local onset of increased opacity, increased rapidly above 4 μm with increasing opacity, remained above 3 μm over a period of ~50 Martian solar days, then returned to seasonal values before the opacity did so. This demonstrates lifting and regional‐scale transport of a dust population ~3 times the size of typical dust aerosol.

Published
2019

11. Novelty Detection for Multispectral Images with Application to Planetary Exploration

Author

Hannah Kerner, James F. Bell, Kiri L. Wagstaff, Danika Wellington, Chiman Kwan, and Heni Ben Amor

Subjects
010504 meteorology & atmospheric sciences, business.industry, Computer science, Multispectral image, Novelty, Pattern recognition, 02 engineering and technology, General Medicine, 01 natural sciences, Autoencoder, Novelty detection, 0202 electrical engineering, electronic engineering, information engineering, 020201 artificial intelligence & image processing, Artificial intelligence, business, 0105 earth and related environmental sciences, Planetary exploration
Abstract

In this work, we present a system based on convolutional autoencoders for detecting novel features in multispectral images. We introduce SAMMIE: Selections based on Autoencoder Modeling of Multispectral Image Expectations. Previous work using autoencoders employed the scalar reconstruction error to classify new images as novel or typical. We show that a spatial-spectral error map can enable both accurate classification of novelty in multispectral images as well as human-comprehensible explanations of the detection. We apply our methodology to the detection of novel geologic features in multispectral images of the Martian surface collected by the Mastcam imaging system on the Mars Science Laboratory Curiosity rover.

Published
2019

12. Assessing martian bedrock mineralogy through 'windows' in the dust using near-infrared and thermal infrared remote sensing

Author

James F. Bell, Briony Horgan, Jason C. Lai, and Danika Wellington

Subjects
Martian, geography, Thermal Emission Spectrometer, geography.geographical_feature_category, 010504 meteorology & atmospheric sciences, Bedrock, Tharsis Montes, Mineralogy, Astronomy and Astrophysics, Mars Exploration Program, 01 natural sciences, Elysium, Space and Planetary Science, Martian surface, 0103 physical sciences, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences, Tharsis
Abstract

Much of Mars' surface is mantled by bright dust, which masks the spectral features used to interpret the mineralogy of the underlying bedrock. Despite the wealth of near-infrared (NIR) and thermal infrared (TIR) data returned from orbiting spacecraft in recent decades, the detailed bedrock composition of approximately half of the Martian surface remains relatively unknown due to dust cover. To address this issue, and to help gain a better understanding of the bedrock mineralogy in dusty regions, Dust Cover Index results from the Mars Global Surveyor Thermal Emission Spectrometer (TES) and analysis of images from the Mars Reconnaissance Orbiter Mars Color Imager (MARCI) were used to identify 63 small localized areas within the classical bright dusty regions of Arabia Terra, Elysium Planitia, and Tharsis Montes as potential “windows” through the dust; that is, areas where the dust cover is thin enough to permit infrared remote sensing of the underlying materials. The mineralogy of each candidate window was inferred using spectra from the Mars Express Observatoire pour la Mineralogie, l'Eau, les Glaces et l'Activite (OMEGA) NIR spectrometer and, where possible, TES. Twelve areas of interest returned spectra that are consistent with mineral species expected to be present at the regional scale, such as high- and low-calcium pyroxene, olivine, and iron-bearing glass. Distribution maps were created using previously defined index parameters for each species present within an area. High-quality TES spectra, if present within an area of interest, were deconvolved to estimate modal mineralogy and to support NIR interpretations. OMEGA data from Arabia Terra and Elysium Planitia are largely similar and indicate the presence of high-calcium pyroxene with significant contributions of glass and olivine, while TES data suggest an intermediate between the established compositions of the southern highlands and Syrtis Major. Limited data from Tharsis are consistent with low-calcium pyroxene mixed with lesser amounts of glass and high-calcium pyroxene. TES data from southern Tharsis correlate well with the previously inferred compositions of the Aonium and Mare Sirenum highlands immediately to the south. Of particular note is the detection of iron-bearing glass as a significant component of all three analyzed regions, especially in Tharsis. Overall, the underlying compositions of the classically dust-covered regions of Mars appear consistent with the compositions of adjacent and other low-albedo (not dust covered) regions of the planet identified in previous studies, with the noted contribution from iron-bearing glass.

Published
2019

13. Toward More Realistic Simulation and Prediction of Dust Storms on Mars

Author

Tanguy Bertrand, Daniel Viudez Moreiras, Peter L. Read, Michael Mischna, German Martinez, Christopher Lee, Lori K. Fenton, Danika Wellington, Orkun Temel, Alexey A. Pankine, Ralph D. Lorenz, Steven J. Greybush, J. M. Battalio, Mathieu G.A. Lapotre, Isaac B. Smith, J. Pla-Garcia, Meredith Elrod, C. Swann, Claire E. Newman, Melinda A. Kahre, Javier Martin-Torres, Claus Gebhardt, Manuel de la Torre Juárez, Stephen R. Lewis, Aymeric Spiga, Scott D. Guzewich, Francesca Esposito, Özgür Karatekin, Alejandro Soto, Henrik Kahanpää, Paulina Wolkenberg, Michael D. Smith, María Paz Zorzano, Brian Jackson, Lynn D. V. Neakrase, Mackenzie Day, Leslie K. Tamppari, Gerhard Wurm, Luca Montabone, Department of Electronics and Nanoengineering, Aalto-yliopisto, and Aalto University

Subjects
media_common.quotation_subject, Art, Humanities, media_common
Abstract

Written by: Claire E. Newman (Aeolis Res.) Tanguy Bertrand (NASA Ames) Joseph Battalio (Yale Univ.) Mackenzie Day (UCLA) Manuel de la Torre Juarez (JPL) Meredith K. Elrod (NASA GSFC) Francesca Esposito (INAF-OAC) Lori Fenton (SETI Inst.) Claus Gebhardt (UAEU) Steven J. Greybush (Penn. State) Scott D. Guzewich (NASA GSFC) Henrik Kahanpaa (FMI) Melinda Kahre (NASA Ames) Ozgur Karatekin (Royal Obs. Belg.) Brian Jackson (Boise State Univ.) Mathieu Lapotre (Stanford Univ.) Christopher Lee (Aeolis Res.) Stephen R. Lewis (Open Univ.) Ralph D. Lorenz (APL) German Martinez Martinez (LPI) Javier Martin-Torres (Aberdeen U.) Michael A. Mischna (JPL) Luca Montabone (SSI) Lynn Neakrase (New Mexico State) Alexey Pankine (SSI) Jorge Pla-Garcia (CAB/SwRI/SSI) Peter L. Read (Univ. of Oxford) Isaac B. Smith (PSI/York Univ.) Michael D. Smith (NASA GSFC) Alejandro Soto (SwRI) Aymeric Spiga (Sorbonne Univ.) Christy Swann (NRL SSC) Leslie Tamppari (JPL) Orkun Temel (Royal Obs. Belgium) Daniel Viudez Moreiras (CAB) Danika Wellington (Ariz. State) Paulina Wolkenberg (INAF) Gerhard Wurm (Duisburg-Essen) Maria-Paz Zorzano (CAB)

Published
2021

15. Spectral, Compositional, and Physical Properties of the Upper Murray Formation and Vera Rubin Ridge, Gale Crater, Mars

Author

Danika Wellington, James F. Bell, Sylvestre Maurice, E. B. Rampe, Briony Horgan, G. H. Peters, Lucy M. Thompson, Roger C. Wiens, Abigail A. Fraeman, Cherie N. Achilles, Jeffrey R. Johnson, and S. Jacob

Subjects
multispectral, Mineralogy, Mars, Spectral line, hematite, Remote Sensing, Planetary Sciences: Solar System Objects, Mastcam, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), phyllosilicates, Absorption (electromagnetic radiation), Planetary Sciences: Solid Surface Planets, Research Articles, Mineralogy and Petrology, geography, Mineral, geography.geographical_feature_category, ferric iron, Mars Exploration Program, Hematite, Physical Properties of Materials, CRISM, Planetary Mineralogy and Petrology, Geophysics, Stratigraphy, Space and Planetary Science, Ridge, visual_art, visual_art.visual_art_medium, Investigations of Vera Rubin Ridge, Gale Crater, laboratory, Composition, Research Article
Abstract

During 2018 and 2019, the Mars Science Laboratory Curiosity rover investigated the chemistry, morphology, and stratigraphy of Vera Rubin ridge (VRR). Using orbital data from the Compact Reconnaissance Imaging Spectrometer for Mars, scientists attributed the strong 860 nm signal associated with VRR to the presence of red crystalline hematite. However, Mastcam multispectral data and CheMin X‐ray diffraction (XRD) measurements show that the depth of the 860 nm absorption is negatively correlated with the abundance of red crystalline hematite, suggesting that other mineralogical or physical parameters are also controlling the 860 nm absorption. Here, we examine Mastcam and ChemCam passive reflectance spectra from VRR and other locations to link the depth, position, and presence or absence of iron‐related mineralogic absorption features to the XRD‐derived rock mineralogy. Correlating CheMin mineralogy to spectral parameters showed that the ~860 nm absorption has a strong positive correlation with the abundance of ferric phyllosilicates. New laboratory reflectance measurements of powdered mineral mixtures can reproduce trends found in Gale crater. We hypothesize that variations in the 860 nm absorption feature in Mastcam and ChemCam observations of VRR materials are a result of three factors: (1) variations in ferric phyllosilicate abundance due to its ~800–1,000 nm absorption; (2) variations in clinopyroxene abundance because of its band maximum at ~860 nm; and (3) the presence of red crystalline hematite because of its absorption centered at 860 nm. We also show that relatively small changes in Ca‐sulfate abundance is one potential cause of the erosional resistance and geomorphic expression of VRR., Key Points Hematite likely controls the wavelength position of the ~860 nm absorption in Mastcam multispectral observations of drill targetsLab results show that the ~860 nm band depth increases with ferric phyllosilicate abundance due to its ~800–1,000 nm featureThe reflectance maximum near 860 nm in pyroxene affects the ~860 nm band depth in spectra of lab mixtures and drilled rocks on Mars

Published
2020

16. Synergistic Ground and Orbital Observations of Iron Oxides on Mt. Sharp and Vera Rubin Ridge

Author

S. Jacob, Danika Wellington, James F. Bell, Briony Horgan, Melissa S. Rice, Jeffrey R. Johnson, Roger C. Wiens, Raymond E. Arvidson, R. V. Morris, Patrick Pinet, Valerie Fox, Vivian Z. Sun, Mark R. Salvatore, Abigail A. Fraeman, Ashwin R. Vasavada, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)

Subjects
spectroscopy, curiosity, Surface Materials and Properties, 010504 meteorology & atmospheric sciences, Infrared, Mineralogy, Mars, 01 natural sciences, Planetary Geochemistry, hematite, Remote Sensing, Planetary Sciences: Solar System Objects, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), medicine, Instruments and Techniques, Spectroscopy, Planetary Sciences: Solid Surface Planets, Research Articles, 0105 earth and related environmental sciences, Mineralogy and Petrology, CRISM<, geography, geography.geographical_feature_category, Bedrock, Mars Exploration Program, Hematite, CRISM, Planetary Mineralogy and Petrology, Geophysics, Geochemistry, 13. Climate action, Space and Planetary Science, Ridge, [SDU]Sciences of the Universe [physics], visual_art, [SDE]Environmental Sciences, visual_art.visual_art_medium, Investigations of Vera Rubin Ridge, Gale Crater, Ferric, Geology, medicine.drug, Composition, Research Article
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., Key Points Areas on Vera Rubin ridge with deep ferric absorptions from orbit also have deep ferric absorptions in Curiosity spectral data setsFerric phases are more widespread on Mt. Sharp than originally reported. Diagenesis deepened ferric absorptions in several locationsCombining orbital and in situ observations enhances planetary exploration

Published
2020

17. Evidence for a diagenetic origin of vera rubin ridge, gale crater, Mars: summary and synthesis of curiosity's exploration campaign

Author

Craig Hardgrove, Kirsten L. Siebach, John P. Grotzinger, Christopher S. Edwards, Alexander B. Bryk, Susanne P. Schwenzer, Sarah Stewart Johnson, William E. Dietrich, Lauren A. Edgar, Sunetra Gupta, Steven G. Banham, Jeffrey G. Catalano, S. Czarnecki, K. M. Stack, Ashwin R. Vasavada, R. V. Morris, Danika Wellington, John Bridges, Christopher H. House, Kristen A. Bennett, S. M. R. Turner, David M. Rubin, Jonas L'Haridon, Jeffrey R. Johnson, Roger C. Wiens, Valerie Fox, S. Jacob, Raymond E. Arvidson, Amy J. Williams, Vivian Z. Sun, Christopher M. Fedo, Jens Frydenvang, Travis Gabriel, Briony Horgan, Woodward W. Fischer, E. B. Rampe, Abigail A. Fraeman, Lucy M. Thompson, N. Mangold, G. M. Wong, Mark R. Salvatore, Nathaniel Stein, G. David, Science and Technology Facilities Council (STFC), UK Space Agency, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), and Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Geochemistry & Geophysics, 010504 meteorology & atmospheric sciences, Outcrop, Lacustrine, Geochemistry, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mars, Hematite, FLUID-FLOW, Geologic record, 01 natural sciences, Diagenesis, Geochemistry and Petrology, 0201 Astronomical and Space Sciences, Earth and Planetary Sciences (miscellaneous), 0402 Geochemistry, CHEMCAM INSTRUMENT SUITE, 0105 earth and related environmental sciences, geography, geography.geographical_feature_category, Spectral signature, Science & Technology, SEDIMENTARY-ROCKS, MOUNT SHARP, Bedrock, DYNAMIC ALBEDO, Gale crater, Mars Exploration Program, MURRAY FORMATION, 15. Life on land, ATOM EXCHANGE, Geophysics, Curiosity, 0403 Geology, Space and Planetary Science, visual_art, Physical Sciences, visual_art.visual_art_medium, PAHRUMP HILLS, (U-TH)/HE DATES, Geology
Abstract

This paper provides an overview of the Curiosity rover's exploration at Vera Rubin ridge and summarizes the science results. Vera Rubin ridge (VRR) is a distinct geomorphic feature on lower Aeolis Mons (informally known as Mt. Sharp) that was identified in orbital data based on its distinct texture, topographic expression, and association with a hematite spectral signature. Curiosity conducted extensive remote sensing observations, acquired data on dozens of contact science targets, and drilled three outcrop samples from the ridge, as well as one outcrop sample immediately below the ridge. Our observations indicate that strata composing VRR were deposited in a predominantly lacustrine setting and are part of the Murray formation. The rocks within the ridge are chemically in family with underlying Murray formation strata. Red hematite is dispersed throughout much of the VRR bedrock, and this is the source of the orbital spectral detection. Gray hematite is also present in isolated, gray‐colored patches concentrated towards the upper elevations of VRR, and these gray patches also contain small, dark Fe‐rich nodules. We propose that VRR formed when diagenetic event(s) preferentially hardened rocks, which were subsequently eroded into a ridge by wind. Diagenesis also led to enhanced crystallization and/or cementation that deepened the ferric‐related spectral absorptions on the ridge, which helped make them readily distinguishable from orbit. Results add to existing evidence of protracted aqueous environments at Gale crater and give new insight into how diagenesis shaped Mars’ rock record.

Published
2020

18. Mineralogy and geochemistry of sedimentary rocks and eolian sediments in Gale crater, Mars: A review after six Earth years of exploration with Curiosity

Author

J. M. Morookian, B. Lafuente, John P. Grotzinger, N. Castle, G. W. Downs, Horton E. Newsom, T. S. Peretyazhko, Vivian Z. Sun, R. Walroth, Ashwin R. Vasavada, Christopher M. Fedo, David J. Des Marais, R. M. Hazen, Kirsten L. Siebach, P. R. Mahaffy, A. H. Treiman, John Bridges, Juergen Schieber, R. Gellert, Roger C. Wiens, C. N. Achilles, C. Freissinet, D. F. Blake, Steve J. Chipera, Robert T. Downs, Joy A. Crisp, Jeffrey R. Johnson, Elizabeth B. Rampe, Philippe Sarrazin, Shaunna M. Morrison, Linda C. Kah, D. T. Vaniman, Lauren A. Edgar, P. I. Craig, V. Tu, D. W. Ming, Albert S. Yen, T. F. Bristow, R. V. Morris, Michael T. Thorpe, Danika Wellington, NASA Johnson Space Center (JSC), NASA, NASA Ames Research Center (ARC), Planetary Science Institute [Tucson] (PSI), NASA Goddard Space Flight Center (GSFC), Geophysical Laboratory [Carnegie Institution], Carnegie Institution for Science [Washington], Jacobs Technology ESCG, Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, University of Arizona, California Institute of Technology (CALTECH), Lunar and Planetary Institute [Houston] (LPI), SETI Institute, Space Research Centre [Leicester], University of Leicester, Astrogeology Science Center [Flagstaff], United States Geological Survey [Reston] (USGS), The University of Tennessee [Knoxville], PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Department of Physics [Guelph], University of Guelph, The University of New Mexico [Albuquerque], Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Rice University [Houston], Department of Geological Sciences [Bloomington], Indiana University [Bloomington], Indiana University System-Indiana University System, ASU School of Earth and Space Exploration (SESE), Arizona State University [Tempe] (ASU), and Los Alamos National Laboratory (LANL)

Subjects
Basalt, Olivine, 010504 meteorology & atmospheric sciences, Geochemistry, Mineralogy, Mars, Mars Science Laboratory, Mars Exploration Program, engineering.material, 01 natural sciences, Diagenesis, CheMin, Sedimentary depositional environment, Igneous rock, Geophysics, 13. Climate action, Geochemistry and Petrology, [SDU]Sciences of the Universe [physics], 0103 physical sciences, engineering, Sedimentary rock, Sedimentology, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

International audience; The Mars Science Laboratory Curiosity rover arrived at Mars in August 2012 with a primary goal of characterizing the habitability of ancient and modern environments. Curiosity was sent to Gale crater to study a sequence of ∼3.5 Ga old sedimentary rocks that, based on orbital visible and near- to short-wave infrared reflectance spectra, contain secondary minerals that suggest deposition and/or alteration in liquid water. The sedimentary sequence in the lower slopes of Mount Sharp in Gale crater preserves a dramatic shift on early Mars from a relatively warm and wet climate to a cold and dry climate, based on a transition from smectite-bearing strata to sulfate-bearing strata. The rover is equipped with instruments to examine the sedimentology and identify compositional changes in the stratigraphy. The Chemistry and Mineralogy (CheMin) instrument is one of two internal laboratories on Curiosity and includes a transmission X-ray diffractometer (XRD) and X-ray fluorescence (XRF) spectrometer. CheMin measures loose sediment samples scooped from the surface and drilled rock powders, and the XRD provides quantitative mineralogy to a detection limit of ∼1 wt.% for crystalline phases. Curiosity has traversed >20 km since landing and has primarily been exploring an ancient lake environment fed by streams and groundwater. Of the 19 drilled rock samples analyzed by CheMin as of sol 2300 (January 2019), 15 are from fluvio-lacustrine deposits that comprise the Bradbury and Murray formations. Most of these samples were drilled from units that did not have a clear mineralogical signature from orbit. Results from CheMin demonstrate an astounding diversity in the mineralogy of these rocks that signifies geochemical variations in source rocks, transportation mechanisms, and depositional and diagenetic fluids. Most detrital igneous minerals are basaltic, but the discovery in a few samples of abundant silicate minerals that usually crystallize from evolved magmas on Earth remains enigmatic. Trioctahedral smectite and magnetite at the base of the section may have formed from low-salinity pore waters with a circumneutral pH in lake sediments. A transition to dioctahedral smectite, hematite, and Ca-sulfate going up section suggests a change to more saline and oxidative aqueous conditions in the lake waters themselves and/or in diagenetic fluids. Perhaps one of the biggest mysteries revealed by CheMin is the high abundance of X-ray amorphous materials (15–73 wt.%) in all samples drilled or scooped to date. CheMin has analyzed three modern eolian sands, which have helped constrain sediment transport and mineral segregation across the active Bagnold Dune Field. Ancient eolian sandstones drilled from the Stimson formation differ from modern eolian sands in that they contain abundant magnetite but no olivine, suggesting that diagenetic processes led to the alteration of olivine to release Fe(II) and precipitate magnetite. Fracture-associated halos in the Stimson and the Murray formations are evidence for complex aqueous processes long after the streams and lakes vanished from Gale crater. The sedimentology and composition of the rocks analyzed by Curiosity demonstrate that habitable environments persisted intermittently on the surface or in the subsurface of Gale crater for perhaps more than a billion years.

Published
2020

19. The albedo of Mars: Six Mars years of observations from Pancam on the Mars Exploration Rovers and comparisons to MOC, CTX and HiRISE

Author

Kjartan M. Kinch, Michael Reynolds, Danika Wellington, Melissa S. Rice, Jeffrey R. Johnson, Genevieve Studer-Ellis, James F. Bell, and Kenneth E. Herkenhoff

Subjects
Meridiani Planum, Thermal Emission Spectrometer, 010504 meteorology & atmospheric sciences, Astronomy and Astrophysics, Atmosphere of Mars, Mars Exploration Program, Exploration of Mars, 01 natural sciences, law.invention, Orbiter, Space and Planetary Science, law, Martian surface, 0103 physical sciences, Thermal Emission Imaging System, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences, Remote sensing
Abstract

The Mars Exploration Rovers (MER) Spirit and Opportunity have systematically used their Panoramic Camera (Pancam) instruments to estimate the Lambert albedo of the surface across their traverses in Gusev crater and Meridiani Planum. The 360˚ “albedo pan” observations acquired with Pancam's broadband (739 ± 338 nm) L1 filter allow for quantitative estimates of the overall surface albedo and measurements of individual surface features. As of November 2016, over nearly six Mars years of the MER mission, Spirit acquired 20 albedo pans (over 7,730 m of traverse distance) and Opportunity acquired 117 albedo pans (over 42,368 m of traverse distance). For Spirit, this comprises the rover's complete dataset. The ranges of Pancam-derived albedos at Gusev crater (0.14–0.24) and at Meridiani Planum (0.11–0.22, with one anomalously high measurement of 0.27 during the July 2007 global dust storm) are consistent with large-scale albedos of the sites as previously determined by the Viking Orbiter Infrared Thermal Mapper (IRTM), Mars Global Surveyor (MGS) Thermal Emission Spectrometer (TES), MGS Mars Orbiter Camera (MOC), Mars Odyssey Thermal Emission Imaging System (THEMIS), Mars Reconnaissance Orbiter (MRO) Context Camera (CTX) and MRO Mars Color Imager (MARCI) instruments. Through comparisons with atmospheric opacity measurements, temporal changes in Pancam albedo values provide insights into interactions between the Martian surface and atmosphere. Pancam observations are also used to “ground truth” measurements from orbit and validate radiometric calibrations, and we present comparisons across the full rover traverses to MOC, CTX, and MRO High Resolution Imaging Science Experiment (HiRISE) data. Albedo averages from the same regions observed by Pancam and all three orbital instruments generally agree to within ± 15%. The few instances found where cross-instrument comparisons exceed the estimated instrument calibration uncertainties can be attributed to atmospheric effects and/or differences in viewing geometries.

Published
2018

20. Diagenesis of Vera Rubin ridge, Gale crater, Mars from Mastcam multispectral images

Author

Lucy M. Thompson, S. Jacob, Jens Frydenvang, Elizabeth B. Rampe, Nicolas Mangold, Edward A. Cloutis, James F. Bell, Frances Rivera-Hernandez, Lauren A. Edgar, Abigail A. Fraeman, Jeffrey R. Johnson, John P. Grotzinger, Briony Horgan, Jonas L'Haridon, Vivian Z. Sun, Danika Wellington, C. H. Seeger, Kristen A. Bennett, Melissa S. Rice, Purdue University [West Lafayette], Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), and Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
spectroscopy, 010504 meteorology & atmospheric sciences, Multispectral image, Geochemistry, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mars, 01 natural sciences, Remote Sensing, Planetary Sciences: Solar System Objects, Geochemistry and Petrology, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), 010303 astronomy & astrophysics, Planetary Sciences: Solid Surface Planets, Research Articles, Mineralogy and Petrology, 0105 earth and related environmental sciences, Martian, Spectral properties, Gale crater, Mars Exploration Program, Hematite, 15. Life on land, Mineral Physics, Optical, infrared, and Raman spectroscopy, Diagenesis, Planetary Mineralogy and Petrology, Geophysics, Space and Planetary Science, visual_art, visual_art.visual_art_medium, Investigations of Vera Rubin Ridge, Gale Crater, Sedimentary rock, mineralogy, Alteration and Weathering Processes, diagenesis, Composition, Research Article
Abstract

Images from the Mars Science Laboratory (MSL) mission of lacustrine sedimentary rocks of Vera Rubin ridge on “Mt. Sharp” in Gale crater, Mars, have shown stark color variations from red to purple to gray. These color differences crosscut stratigraphy and are likely due to diagenetic alteration of the sediments after deposition. However, the chemistry and timing of these fluid interactions is unclear. Determining how diagenetic processes may have modified chemical and mineralogical signatures of ancient Martian environments is critical for understanding the past habitability of Mars and achieving the goals of the MSL mission. Here we use visible/near‐infrared spectra from Mastcam and ChemCam to determine the mineralogical origins of color variations in the ridge. Color variations are consistent with changes in spectral properties related to the crystallinity, grain size, and texture of hematite. Coarse‐grained gray hematite spectrally dominates in the gray patches and is present in the purple areas, while nanophase and fine‐grained red crystalline hematite are present and spectrally dominate in the red and purple areas. We hypothesize that these differences were caused by grain‐size coarsening of hematite by diagenetic fluids, as observed in terrestrial analogs. In this model, early primary reddening by oxidizing fluids near the surface was followed during or after burial by bleaching to form the gray patches, possibly with limited secondary reddening after exhumation. Diagenetic alteration may have diminished the preservation of biosignatures and changed the composition of the sediments, making it more difficult to interpret how conditions evolved in the paleolake over time., Key Points Vera Rubin ridge exhibits strong color differences that crosscut stratigraphy, consistent with postdepositional alteration (diagenesis)Color differences correspond to variations in spectral signatures of nanophase, fine‐grained, and coarse‐grained hematiteBased on terrestrial analogs, these variations can be explained by early oxidation and later coarsening of hematite by diagenetic fluids

Published
2019

21. Visible/near-infrared spectral diversity from in situ observations of the Bagnold Dune Field sands in Gale Crater, Mars

Author

Danika Wellington, Cherie N. Achilles, Patrick Pinet, Jeffrey R. Johnson, James F. Bell, Victoria E. Hamilton, Lucy M. Thompson, Sylvestre Maurice, Olivier Gasnault, Bethany L. Ehlmann, Roger C. Wiens, Edward A. Cloutis, Abigail A. Fraeman, S. Bender, and Stéphane Le Mouélic

Subjects
Olivine, 010504 meteorology & atmospheric sciences, Mineralogy, Mars Exploration Program, Pyroxene, engineering.material, 01 natural sciences, Grain size, Geophysics, 13. Climate action, Space and Planetary Science, Geochemistry and Petrology, Absorption band, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), engineering, Aeolian processes, Mafic, Spectroscopy, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences
Abstract

As part of the Bagnold Dune campaign conducted by Mars Science Laboratory rover Curiosity, visible/near-infrared reflectance spectra of dune sands were acquired using Mast Camera (Mastcam) multispectral imaging (445–1013 nm) and Chemistry and Camera (ChemCam) passive point spectroscopy (400–840 nm). By comparing spectra from pristine and rover-disturbed ripple crests and troughs within the dune field, and through analysis of sieved grain size fractions, constraints on mineral segregation from grain sorting could be determined. In general, the dune areas exhibited low relative reflectance, a weak ~530 nm absorption band, an absorption band near 620 nm, and a spectral downturn after ~685 nm consistent with olivine-bearing sands. The finest grain size fractions occurred within ripple troughs and in the subsurface and typically exhibited the strongest ~530 nm bands, highest relative reflectances, and weakest red/near-infrared ratios, consistent with a combination of crystalline and amorphous ferric materials. Coarser-grained samples were the darkest and bluest and exhibited weaker ~530 nm bands, lower relative reflectances, and stronger downturns in the near-infrared, consistent with greater proportions of mafic minerals such as olivine and pyroxene. These grains were typically segregated along ripple crests and among the upper surfaces of grain flows in disturbed sands. Sieved dune sands exhibited progressive decreases in reflectance with increasing grain size, as observed in laboratory spectra of olivine size separates. The continuum of spectral features observed between the coarse- and fine-grained dune sands suggests that mafic grains, ferric materials, and air fall dust mix in variable proportions depending on aeolian activity and grain sorting.

Published
2017

22. An Instrument Anomaly in the Mars Exploration Rover Pancam 1,009‐nm Filter (R7): Characterization, Simulation, Correction, and Preliminary Verification

Author

Danika Wellington, Simone J. Jakobsen, Morten Madsen, Kjartan M. Kinch, James F. Bell, Lorinda Dajose, and Khaled Alizai

Subjects
multispectral, Anomaly (natural sciences), Multispectral image, Mars, Mars exploration rover, Mars Exploration Program, Environmental Science (miscellaneous), calibration, Characterization (materials science), Filter (video), MER, Calibration, General Earth and Planetary Sciences, Pancam, Geology, CCD, Remote sensing
Abstract

During pre-flight calibration of the panoramic camera (Pancam) instrument on board the Mars Exploration Rovers MER A (Spirit) and MER B (Opportunity), a discrepancy was noted between 11-band spectra extracted from Pancam images of the camera's radiometric calibration target and reflectance spectra obtained with a spectrometer. This discrepancy was observed in the longest-wavelength filter of the camera (the longpass R7 filter with system λ eff = 1,009 nm) and consisted of a reduction in contrast between bright and dark regions. Here we describe and characterize this effect. We propose that the effect arises because long-wavelength photons close to the silicon band-gap at 1,100 nm are allowed through the R7 filter, pass through the bulk charge-coupled device, scatter from the backside, pass through the charge-coupled device again, and are registered in a pixel other than the pixel through which they originally entered. Based on this hypothesis we develop a model capable of accurately simulating the effect, and correct for it. We present preliminary results from testing this correction on preflight, as well as in-flight, images. The effect is small, but in some specific cases in small regions of high contrast, the effect is significant. In in-flight images of Martian terrain we observed the signal in dark shadows to be artificially inflated by up to ∼ 33% and analysis of early-mission calibration target images indicated that the reduced contrast due to the artifact is equivalent to >100 DN (full well = 4095 DN) for a hypothetical perfectly dark pixel.

Published
2019

23. Corrigendum to 'Mineralogy and geochemistry of sedimentary rocks and eolian sediments in Gale crater, Mars: A review after six earth years of exploration with Curiosity' [Geochemistry 80 (2) (2020) 125605]

Author

Danika Wellington, R. V. Morris, J. M. Morookian, T. S. Peretyazhko, Albert S. Yen, David J. Des Marais, G. W. Downs, R. C. Walroth, N. Castle, Juergen Schieber, Caroline Freissinet, R. Gellert, Jeffrey R. Johnson, B. Lafuente, Robert M. Hazen, Horton E. Newsom, Paul R. Mahaffy, S. J. Chipera, John Bridges, D. W. Ming, C. Fedo, John P. Grotzinger, Allan H. Treiman, Joy A. Crisp, Kirsten L. Siebach, Cherie N. Achilles, Thomas F. Bristow, Linda C. Kah, Ashwin R. Vasavada, Vivian Z. Sun, Robert T. Downs, Philippe Sarrazin, Shaunna M. Morrison, E. B. Rampe, Michael T. Thorpe, P. I. Craig, Lauren A. Edgar, V. Tu, Roger C. Wiens, David F. Blake, and D. T. Vaniman

Subjects
Geophysics, Geochemistry and Petrology, Geochemistry, Gale crater, Sedimentary rock, Mars Exploration Program, Earth (classical element), Geology, Eolian sediments
Published
2020

24. Patterns of surface albedo changes from Mars Reconnaissance Orbiter Mars Color Imager (MARCI) observations

Author

Danika Wellington and James F. Bell

Subjects
Martian, 010504 meteorology & atmospheric sciences, Cloud cover, Astronomy and Astrophysics, Mars Exploration Program, Albedo, 01 natural sciences, law.invention, Orbiter, Space and Planetary Science, law, Climatology, Martian surface, 0103 physical sciences, Environmental science, Aeolian processes, Climate model, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

The Mars Reconnaissance Orbiter (MRO) Mars Color Imager (MARCI) instrument has been observing Mars since 2006, providing over five-and-a-half martian years of daily observations with near global coverage. We have used this dataset to generate a time series of mosaics of the martian surface, using the extensive imaging coverage to produce composites that are largely free of cloud cover and close to the 1 km/pixel spatial scale of the instrument along its center track. These mosaics have allowed us to investigate and constrain the seasonality of albedo changes that result from the redistribution of surface dust by aeolian processes. We find that many regions of the planet have seasonal cycles of dust deposition and erosion, but others show secular variations or multi-annual trends that alter the visible appearance of the planet on timescales that are comparable to or longer than the present dataset. Changes take place both following observable dust storms and in their absence, depending on location and season. Dust settling associated with seasonal atmospheric opacity declines provides an important reset to regions that experience significant dust removal. Detailed characterizations of the surface dust behavior of different regions provided here represent a portion of the global dust cycle (an important element of the martian climate system) and provide observational constraints for regional- and global-scale climate models. In addition, seasonal and longer-term variations in the surface dust cover have important implications for future remote sensing and human exploration efforts.

Published
2020

25. Bagnold Dunes Campaign Phase 2: Visible/Near-Infrared Reflectance Spectroscopy of Longitudinal Ripple Sands

Author

James F. Bell, Olivier Gasnault, S. Bender, Sylvestre Maurice, Patrick Pinet, Edward A. Cloutis, Lucy M. Thompson, Abigail A. Fraeman, Danika Wellington, Jeffrey R. Johnson, Bethany L. Ehlmann, Roger C. Wiens, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Arizona State University [Tempe] (ASU), Planetary Science Institute [Tucson] (PSI), Department of Geography [Winnipeg], University of Winnipeg, Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), University of Gothenburg (GU), Los Alamos National Laboratory (LANL), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
geography, geography.geographical_feature_category, 010504 meteorology & atmospheric sciences, Infrared, Bedrock, Mineralogy, Mars Exploration Program, Hematite, 01 natural sciences, Spectral line, Geophysics, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Barchan, Phase (matter), visual_art, 0103 physical sciences, visual_art.visual_art_medium, General Earth and Planetary Sciences, 010303 astronomy & astrophysics, Geology, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Visible spectrum
Abstract

As part of the Phase 2 Bagnold Dune campaign at Gale Crater, Mars, constraints on the geochemistry, mineralogy, and oxidation state of pristine and disturbed linear sand ripples were made using visible/near‐infrared spectral observations for comparison to Phase 1 spectra of the barchan dunes to the north. Spectra acquired by the ChemCam and Mastcam instruments (400–1,000 nm) at four Phase 2 locations revealed similar overall spectral trends between the two regions, but most Phase 2 sands were redder in the visible wavelengths. The majority of targets exhibited lower red/infrared ratios, higher ~530‐nm band depths, and higher red/blue ratios than Phase 1 samples, suggesting a greater proportion of redder, fine‐grained, ferric sands in Phase 2 samples. This is consistent with the slightly greater proportion of hematite in Phase 2 samples as determined from CheMin analyses of the Ogunquit sands, which may reflect contamination from the surrounding hematite‐bearing Murray formation bedrock.

Published
2018

26. VISIBLE/NEAR-INFRARED REFLECTANCE SPECTROSCOPY OF LONGITUDINAL RIPPLE SANDS OBSERVED DURING PHASE 2 OF THE BAGNOLD DUNE CAMPAIGN, GALE CRATER, MARS

Author

Lucy M. Thompson, S. Bender, B. L. Ehlmann, Abigail A. Fraeman, Edward A. Cloutis, James F. Bell, Danika Wellington, Olivier Gasnault, Patrick Pinet, Jeffrey R. Johnson, Sylvestre Maurice, and R. C. Wiens

Subjects
Visible near infrared, Reflectance spectroscopy, Phase (matter), Ripple, Mineralogy, Gale crater, Mars Exploration Program, Geology
Published
2018

27. The Mars Science Laboratory Curiosity rover Mastcam instruments: Preflight and in-flight calibration, validation, and data archiving

Author

E. Jensen, Robert G. Deen, S. McNair, Michael C. Malin, Kenneth E. Herkenhoff, Kjartan M. Kinch, Danika Wellington, J. Van Beek, Mark T. Lemmon, James F. Bell, R. V. Morris, A. Godber, Justin N. Maki, David E. Harker, M. A. Ravine, Craig Hardgrove, Michael Caplinger, Morten Madsen, E. Cisneros, and Ryan B. Anderson

Subjects
Bayer filter, 010504 meteorology & atmospheric sciences, Pixel, Computer science, Multispectral image, Curiosity rover, Mars, Field of view, Mars Exploration Program, Environmental Science (miscellaneous), Gale crater, calibration, 01 natural sciences, Planetary Data System, 0103 physical sciences, multispectral imaging, General Earth and Planetary Sciences, Focal length, RGB color model, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing
Abstract

The NASA Curiosity rover Mast Camera (Mastcam) system is a pair of fixed-focal length, multispectral, color CCD imagers mounted approximately 2 m above the surface on the rover's remote sensing mast, along with associated electronics and an onboard calibration target. The left Mastcam (M-34) has a 34 mm focal length, an instantaneous field of view (IFOV) of 0.22 mrad, and a FOV of 20 deg × 15 deg over the full 1648 × 1200 pixel span of its Kodak KAI-2020 CCD. The right Mastcam (M-100) has a 100 mm focal length, an IFOV of 0.074 mrad, and a FOV of 6.8 deg × 5.1 deg using the same detector. The cameras are separated by 24.2 cm on the mast, allowing stereo images to be obtained at the resolution of the M-34 camera. Each camera has an eight-position filter wheel, enabling it to take Bayer pattern red, green, and blue (RGB) 'true color' images, multispectral images in nine additional bands spanning approximately 400-1100 nm, and images of the Sun in two colors through neutral density-coated filters. An associated Digital Electronics Assembly provides command and data interfaces to the rover, 8 Gb of image storage per camera, 11 bit to 8 bit companding, JPEG compression, and acquisition of high-definition video. Here we describe the preflight and in-flight calibration of Mastcam images, the ways that they are being archived in the NASA Planetary Data System, and the ways that calibration refinements are being developed as the investigation progresses on Mars. We also provide some examples of data sets and analyses that help to validate the accuracy and precision of the calibration.

Published
2017

28. Visible to near-infrared MSL/Mastcam multispectral imaging: Initial results from select high-interest science targets within Gale Crater, Mars

Author

James F. Bell, A. Godber, Danika Wellington, Abigail A. Fraeman, Jeffrey R. Johnson, Craig Hardgrove, Melissa S. Rice, Bethany L. Ehlmann, and Kjartan M. Kinch

Subjects
010504 meteorology & atmospheric sciences, Multispectral image, Near-infrared spectroscopy, Mineralogy, Mars, Mars Exploration Program, Hematite, 01 natural sciences, Spectral line, Gale Crater, CRISM, Geophysics, Curiosity, Geochemistry and Petrology, Absorption band, Martian surface, visual_art, 0103 physical sciences, visual_art.visual_art_medium, multispectral imaging, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences, Remote sensing
Abstract

The Mastcam CCD cameras on the Mars Science Laboratory Curiosity Rover each use an 8-position filter wheel in acquiring up to 1600 × 1200 pixel images. The filter set includes a broadband near-infrared cutoff filter for RGB Bayer imaging on each camera and 12 narrow-band geology filters distributed between the two cameras, spanning the wavelength range 445–1013 nm. This wavelength region includes the relatively broad charge-transfer and crystal-field absorption bands that are most commonly due to the presence of iron-bearing minerals. To identify such spectral features, sequences of images taken with identical pointings through different filters have been calibrated to relative reflectance using pre-flight calibration coefficients and in-flight measurements of an onboard calibration target. Within the first 1000 sols of the mission, Mastcam observed a spectrally diverse set of materials displaying absorption features consistent with the presence of iron-bearing silicate, iron oxide, and iron sulfate minerals. Dust-coated surfaces as well as soils possess a strong positive reflectance slope in the visible, consistent with the presence of nanophase iron oxides, which have long been considered the dominant visible-wavelength pigmenting agent in weathered martian surface materials. Fresh surfaces, such as tailings produced by the drill tool and the interiors of rocks broken by the rover wheels, are grayer in visible wavelengths than their reddish, dust-coated surfaces but possess reflectance spectra that vary considerably between sites. To understand the mineralogical basis of observed Mastcam reflectance spectra, we focus on a subset of the multispectral data set for which additional constraints on the composition of surface materials are available from other rover instruments, with an emphasis on sample sites for which detailed mineralogy is provided by the results of CheMin X-ray diffraction analyses. We also discuss the results of coordinated observations with the ChemCam instrument, whose passive mode of operation is capable of acquiring reflectance spectra over wavelengths that considerably overlap the range spanned by the Mastcam filter set (Johnson et al. 2016). Materials that show a distinct 430 nm band in ChemCam data also are observed to have a strong near-infrared absorption band in Mastcam spectral data, consistent with the presence of a ferric sulfate mineral. Long-distance Mastcam observations targeted toward the flanks of the Gale crater central mound are in agreement with both ChemCam spectra and orbital results, and in particular exhibit the spectral features of a crystalline hematite layer identified in MRO/CRISM data. Variations observed in Mastcam multi-filter images acquired to date have shown that multispectral observations can discriminate between compositionally different materials within Gale Crater and are in qualitative agreement with mineralogies from measured samples and orbital data.

Published
2017

29. Chemistry, mineralogy, and grain properties at Namib and High dunes, Bagnold dune field, Gale crater, Mars: A synthesis of Curiosity rover observations

Author

Victoria E. Hamilton, Albert S. Yen, Pamela G. Conrad, R. Gellert, D. W. Ming, Ashwin R. Vasavada, Mathieu G.A. Lapotre, Scott K. Rowland, Abigail A. Fraeman, Roger C. Wiens, David F. Blake, Kenneth S. Edgett, Jeffrey R. Johnson, C. D. O'Connell-Cooper, P.-Y. Meslin, D. T. Vaniman, Danika Wellington, Ryan C. Sullivan, Michelle E. Minitti, Kirsten L. Siebach, Nathaniel Stein, Agnes Cousin, Sylvestre Maurice, Robert T. Downs, Nathan T. Bridges, Cherie N. Achilles, Stephen Kuhn, Craig Hardgrove, Lucy M. Thompson, Travis Gabriel, Paul R. Mahaffy, M. L. Litvak, Susanne Schröder, R. V. Morris, J. M. Morookian, Raymond E. Arvidson, Bethany L. Ehlmann, Patrick Pinet, Brad Sutter, M. McHenry, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and Services communs OMP (UMS 831)

Subjects
010504 meteorology & atmospheric sciences, Namib, 01 natural sciences, Planetary Sciences: Solar System Objects, Earth and Planetary Sciences (miscellaneous), 010303 astronomy & astrophysics, Research Articles, Martian, grain size, Mars Science Laboratory, Investigations of the Bagnold Dune Field, Gale crater, Mars Exploration Program, Mineralogy, Physical Properties of Materials, Grain size, Planetary Mineralogy and Petrology, Chemistry, Geophysics, volatiles, Aeolian processes, Erosion and Weathering, dust, Geology, Composition, Research Article, Dunes, Surface Materials and Properties, Bedform, Mars, engineering.material, Planetary Geochemistry, amorphous phase, Geochemistry and Petrology, 0103 physical sciences, Rover, Plagioclase, MSL, Planetary Sciences: Solid Surface Planets, Mineralogy and Petrology, 0105 earth and related environmental sciences, Olivine, Mars soils, Bagnold, Geochemistry, sand dunes, Curiosity, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Rocknest, engineering
Abstract

The Mars Science Laboratory Curiosity rover performed coordinated measurements to examine the textures and compositions of aeolian sands in the active Bagnold dune field. The Bagnold sands are rounded to subrounded, very fine to medium sized (~45–500 μm) with ≥6 distinct grain colors. In contrast to sands examined by Curiosity in a dust‐covered, inactive bedform called Rocknest and soils at other landing sites, Bagnold sands are darker, less red, better sorted, have fewer silt‐sized or smaller grains, and show no evidence for cohesion. Nevertheless, Bagnold mineralogy and Rocknest mineralogy are similar with plagioclase, olivine, and pyroxenes in similar proportions comprising >90% of crystalline phases, along with a substantial amorphous component (35% ± 15%). Yet Bagnold and Rocknest bulk chemistry differ. Bagnold sands are Si enriched relative to other soils at Gale crater, and H2O, S, and Cl are lower relative to all previously measured Martian soils and most Gale crater rocks. Mg, Ni, Fe, and Mn are enriched in the coarse‐sieved fraction of Bagnold sands, corroborated by visible/near‐infrared spectra that suggest enrichment of olivine. Collectively, patterns in major element chemistry and volatile release data indicate two distinctive volatile reservoirs in Martian soils: (1) amorphous components in the sand‐sized fraction (represented by Bagnold) that are Si‐enriched, hydroxylated alteration products and/or H2O‐ or OH‐bearing impact or volcanic glasses and (2) amorphous components in the fine fraction (, Key Points Because of ongoing aeolian activity, the Bagnold dunes consist of well‐sorted sands and lack the finer grains typical of Martian soilsDune sands are chemically distinct with elevated Si, Mg, and Ni and lower H2O, S, and Cl relative to all previously measured Martian finesTwo distinct, water‐/OH‐bearing amorphous components are identified: Fe‐, S‐, and Cl‐rich material in dust and Si‐rich material in the sands

Published
2017

33. Calcium sulfate veins characterized by ChemCam/Curiosity at Gale crater, Mars

Author

William Rapin, P. Y. Meslin, Dawn Y. Sumner, Ryan B. Anderson, John Bridges, Olivier Forni, Susanne Schröder, Marion Nachon, Richard Leveille, M. D. Dyar, S. Le Mouélic, Linda C. Kah, Sylvestre Maurice, Bethany L. Ehlmann, Agnes Cousin, Melissa S. Rice, James F. Bell, Ann Ollila, S. W. Squyres, Scott M. McLennan, K. Stack, Dorothy Z. Oehler, Danika Wellington, Roger C. Wiens, Samuel M. Clegg, Olivier Gasnault, John P. Grotzinger, Eric Lewin, Jeffrey R. Johnson, David T. Vaniman, Diana L. Blaney, Jérémie Lasue, N. Mangold, B. C. Clark, Gilles Dromart, and Cécile Fabre

Subjects
Anhydrite, Gypsum, Fracture (mineralogy), Mineralogy, Fluvial, engineering.material, Cementation (geology), chemistry.chemical_compound, Geophysics, Bassanite, chemistry, Space and Planetary Science, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), engineering, Sedimentary rock, Lithification, Geology
Abstract

The Curiosity rover has analyzed abundant light-toned fracture-fill material within the Yellowknife Bay sedimentary deposits. The ChemCam instrument, coupled with Mastcam and ChemCam/Remote Micro Imager images, was able to demonstrate that these fracture fills consist of calcium sulfate veins, many of which appear to be hydrated at a level expected for gypsum and bassanite. Anhydrite is locally present and is found in a location characterized by a nodular texture. An intricate assemblage of veins crosses the sediments, which were likely formed by precipitation from fluids circulating through fractures. The presence of veins throughout the entire similar to 5 m thick Yellowknife Bay sediments suggests that this process occurred well after sedimentation and cementation/lithification of those sediments. The sulfur-rich fluids may have originated in previously precipitated sulfate-rich layers, either before the deposition of the Sheepbed mudstones or from unrelated units such as the sulfates at the base of Mount Sharp. The occurrence of these veins after the episodes of deposition of fluvial sediments at the surface suggests persistent aqueous activity in relatively nonacidic conditions.

Published
2014

34. Saturn's aurora observed by the Cassini camera at visible wavelengths

Author

Danika Wellington, Shawn P. Ewald, Andrew P. Ingersoll, and Ulyana A. Dyudina

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Brightness, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Magnetosphere, Astronomy, Astronomy and Astrophysics, 01 natural sciences, Latitude, Space and Planetary Science, Magnetosphere of Saturn, Saturn, 0103 physical sciences, Longitude, 010303 astronomy & astrophysics, Saturn's hexagon, Geology, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences, Line (formation)
Abstract

The first observations of Saturn's visible-wavelength aurora were made by the Cassini camera. The aurora was observed between 2006 and 2013 in the northern and southern hemispheres. The color of the aurora changes from pink at a few hundred km above the horizon to purple at 1000-1500 km above the horizon. The spectrum observed in 9 filters spanning wavelengths from 250 nm to 1000 nm has a prominent H-alpha line and roughly agrees with laboratory simulated auroras. Auroras in both hemispheres vary dramatically with longitude. Auroras form bright arcs between 70 and 80 degree latitude north and between 65 and 80 degree latitude south, which sometimes spiral around the pole, and sometimes form double arcs. A large 10,000-km-scale longitudinal brightness structure persists for more than 100 hours. This structure rotates approximately together with Saturn. On top of the large steady structure, the auroras brighten suddenly on the timescales of a few minutes. These brightenings repeat with a period of about 1 hour. Smaller, 1000-km-scale structures may move faster or lag behind Saturn's rotation on timescales of tens of minutes. The persistence of nearly-corotating large bright longitudinal structure in the auroral oval seen in two movies spanning 8 and 11 rotations gives an estimate on the period of 10.65 $\pm$0.15 h for 2009 in the northern oval and 10.8$\pm$ 0.1 h for 2012 in the southern oval. The 2009 north aurora period is close to the north branch of Saturn Kilometric Radiation (SKR) detected at that time., 39 pages, 8 figures, 1 table, 6 supplementary movies, accepted to Icarus

Published
2016

35. A Habitable Fluvio-Lacustrine Environment at Yellowknife Bay, Gale Crater, Mars

Author

J. P. Grotzinger, D. Y. Sumner, L. C. Kah, K. Stack, S. Gupta, L. Edgar, D. Rubin, K. Lewis, J. Schieber, N. Mangold, R. Milliken, P. G. Conrad, D. DesMarais, J. Farmer, K. Siebach, F. Calef, J. Hurowitz, S. M. McLennan, D. Ming, D. Vaniman, J. Crisp, A. Vasavada, K. S. Edgett, M. Malin, D. Blake, R. Gellert, P. Mahaffy, R. C. Wiens, S. Maurice, J. A. Grant, S. Wilson, R. C. Anderson, L. Beegle, R. Arvidson, B. Hallet, R. S. Sletten, M. Rice, J. Bell, J. Griffes, B. Ehlmann, R. B. Anderson, T. F. Bristow, W. E. Dietrich, G. Dromart, J. Eigenbrode, A. Fraeman, C. Hardgrove, K. Herkenhoff, L. Jandura, G. Kocurek, S. Lee, L. A. Leshin, R. Leveille, D. Limonadi, J. Maki, S. McCloskey, M. Meyer, M. Minitti, H. Newsom, D. Oehler, A. Okon, M. Palucis, T. Parker, S. Rowland, M. Schmidt, S. Squyres, A. Steele, E. Stolper, R. Summons, A. Treiman, R. Williams, A. Yingst, MSL Science Team, Osku Kemppinen, Nathan Bridges, Jeffrey R. Johnson, David Cremers, Austin Godber, Meenakshi Wadhwa, Danika Wellington, Ian McEwan, Claire Newman, Mark Richardson, Antoine Charpentier, Laurent Peret, Penelope King, Jennifer Blank, Gerald Weigle, Shuai Li, Kevin Robertson, Vivian Sun, Michael Baker, Christopher Edwards, Kenneth Farley, Hayden Miller, Megan Newcombe, Cedric Pilorget, Claude Brunet, Victoria Hipkin, Richard Léveillé, Geneviève Marchand, Pablo Sobrón Sánchez, Laurent Favot, George Cody, Lorenzo Flückiger, David Lees, Ara Nefian, Mildred Martin, Marc Gailhanou, Frances Westall, Guy Israël, Christophe Agard, Julien Baroukh, Christophe Donny, Alain Gaboriaud, Philippe Guillemot, Vivian Lafaille, Eric Lorigny, Alexis Paillet, René Pérez, Muriel Saccoccio, Charles Yana, Carlos Armiens-Aparicio, Javier Caride Rodríguez, Isaías Carrasco Blázquez, Felipe Gómez Gómez, Javier Gómez-Elvira, Sebastian Hettrich, Alain Lepinette Malvitte, Mercedes Marín Jiménez, Jesús Martínez-Frías, Javier Martín-Soler, F. Javier Martín-Torres, Antonio Molina Jurado, Luis Mora-Sotomayor, Guillermo Muñoz Caro, Sara Navarro López, Verónica Peinado-González, Jorge Pla-García, José Antonio Rodriguez Manfredi, Julio José Romeral-Planelló, Sara Alejandra Sans Fuentes, Eduardo Sebastian Martinez, Josefina Torres Redondo, Roser Urqui-O’Callaghan, María-Paz Zorzano Mier, Steve Chipera, Jean-Luc Lacour, Patrick Mauchien, Jean-Baptiste Sirven, Heidi Manning, Alberto Fairén, Alexander Hayes, Jonathan Joseph, Robert Sullivan, Peter Thomas, Audrey Dupont, Angela Lundberg, Noureddine Melikechi, Alissa Mezzacappa, Julia DeMarines, David Grinspoon, Günther Reitz, Benito Prats, Evgeny Atlaskin, Maria Genzer, Ari-Matti Harri, Harri Haukka, Henrik Kahanpää, Janne Kauhanen, Mark Paton, Jouni Polkko, Walter Schmidt, Tero Siili, Cécile Fabre, James Wray, Mary Beth Wilhelm, Franck Poitrasson, Kiran Patel, Stephen Gorevan, Stephen Indyk, Gale Paulsen, David Bish, Brigitte Gondet, Yves Langevin, Claude Geffroy, David Baratoux, Gilles Berger, Alain Cros, Claude d’Uston, Olivier Forni, Olivier Gasnault, Jérémie Lasue, Qiu-Mei Lee, Pierre-Yves Meslin, Etienne Pallier, Yann Parot, Patrick Pinet, Susanne Schröder, Mike Toplis, Éric Lewin, Will Brunner, Ezat Heydari, Cherie Achilles, Brad Sutter, Michel Cabane, David Coscia, Cyril Szopa, François Robert, Violaine Sautter, Stéphane Le Mouélic, Marion Nachon, Arnaud Buch, Fabien Stalport, Patrice Coll, Pascaline François, François Raulin, Samuel Teinturier, James Cameron, Sam Clegg, Agnès Cousin, Dorothea DeLapp, Robert Dingler, Ryan Steele Jackson, Stephen Johnstone, Nina Lanza, Cynthia Little, Tony Nelson, Richard B. Williams, Andrea Jones, Laurel Kirkland, Burt Baker, Bruce Cantor, Michael Caplinger, Scott Davis, Brian Duston, Donald Fay, David Harker, Paul Herrera, Elsa Jensen, Megan R. Kennedy, Gillian Krezoski, Daniel Krysak, Leslie Lipkaman, Elaina McCartney, Sean McNair, Brian Nixon, Liliya Posiolova, Michael Ravine, Andrew Salamon, Lee Saper, Kevin Stoiber, Kimberley Supulver, Jason Van Beek, Tessa Van Beek, Robert Zimdar, Katherine Louise French, Karl Iagnemma, Kristen Miller, Fred Goesmann, Walter Goetz, Stubbe Hviid, Micah Johnson, Matthew Lefavor, Eric Lyness, Elly Breves, M. Darby Dyar, Caleb Fassett, Laurence Edwards, Robert Haberle, Tori Hoehler, Jeff Hollingsworth, Melinda Kahre, Leslie Keely, Christopher McKay, Lora Bleacher, William Brinckerhoff, David Choi, Jason P. Dworkin, Melissa Floyd, Caroline Freissinet, James Garvin, Daniel Glavin, Daniel Harpold, David K. Martin, Amy McAdam, Alexander Pavlov, Eric Raaen, Michael D. Smith, Jennifer Stern, Florence Tan, Melissa Trainer, Arik Posner, Mary Voytek, Andrew Aubrey, Alberto Behar, Diana Blaney, David Brinza, Lance Christensen, Lauren DeFlores, Jason Feldman, Sabrina Feldman, Gregory Flesch, Insoo Jun, Didier Keymeulen, Michael Mischna, John Michael Morookian, Betina Pavri, Marcel Schoppers, Aaron Sengstacken, John J. Simmonds, Nicole Spanovich, Manuel de la Torre Juarez, Christopher R. Webster, Albert Yen, Paul Douglas Archer, Francis Cucinotta, John H. Jones, Richard V. Morris, Paul Niles, Elizabeth Rampe, Thomas Nolan, Martin Fisk, Leon Radziemski, Bruce Barraclough, Steve Bender, Daniel Berman, Eldar Noe Dobrea, Robert Tokar, Timothy Cleghorn, Wesley Huntress, Gérard Manhès, Judy Hudgins, Timothy Olson, Noel Stewart, Philippe Sarrazin, Edward Vicenzi, Mark Bullock, Bent Ehresmann, Victoria Hamilton, Donald Hassler, Joseph Peterson, Scot Rafkin, Cary Zeitlin, Fedor Fedosov, Dmitry Golovin, Natalya Karpushkina, Alexander Kozyrev, Maxim Litvak, Alexey Malakhov, Igor Mitrofanov, Maxim Mokrousov, Sergey Nikiforov, Vasily Prokhorov, Anton Sanin, Vladislav Tretyakov, Alexey Varenikov, Andrey Vostrukhin, Ruslan Kuzmin, Benton Clark, Michael Wolff, Oliver Botta, Darrell Drake, Keri Bean, Mark Lemmon, Susanne P. Schwenzer, Ella Mae Lee, Robert Sucharski, Miguel Ángel de Pablo Hernández, Juan José Blanco Ávalos, Miguel Ramos, Myung-Hee Kim, Charles Malespin, Ianik Plante, Jan-Peter Muller, Rafael Navarro-González, Ryan Ewing, William Boynton, Robert Downs, Mike Fitzgibbon, Karl Harshman, Shaunna Morrison, Onno Kortmann, Amy Williams, Günter Lugmair, Michael A. Wilson, Bruce Jakosky, Tonci Balic-Zunic, Jens Frydenvang, Jaqueline Kløvgaard Jensen, Kjartan Kinch, Asmus Koefoed, Morten Bo Madsen, Susan Louise Svane Stipp, Nick Boyd, John L. Campbell, Glynis Perrett, Irina Pradler, Scott VanBommel, Samantha Jacob, Tobias Owen, Hannu Savijärvi, Eckart Boehm, Stephan Böttcher, Sönke Burmeister, Jingnan Guo, Jan Köhler, César Martín García, Reinhold Mueller-Mellin, Robert Wimmer-Schweingruber, John C. Bridges, Timothy McConnochie, Mehdi Benna, Heather Franz, Hannah Bower, Anna Brunner, Hannah Blau, Thomas Boucher, Marco Carmosino, Sushil Atreya, Harvey Elliott, Douglas Halleaux, Nilton Rennó, Michael Wong, Robert Pepin, Beverley Elliott, John Spray, Lucy Thompson, Suzanne Gordon, Ann Ollila, Joshua Williams, Paulo Vasconcelos, Jennifer Bentz, Kenneth Nealson, Radu Popa, Jeffrey Moersch, Christopher Tate, Mackenzie Day, Raymond Francis, Emily McCullough, Ed Cloutis, Inge Loes ten Kate, Daniel Scholes, Susan Slavney, Thomas Stein, Jennifer Ward, Jeffrey Berger, John E. Moores, Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Department of Earth and Planetary Science [UC Berkeley] (EPS), University of California [Berkeley], University of California-University of California, The University of Tennessee [Knoxville], Department of Earth Science and Technology [Imperial College London], Imperial College London, ASU School of Earth and Space Exploration (SESE), Arizona State University [Tempe] (ASU), US Geological Survey [Santa Cruz], United States Geological Survey [Reston] (USGS), Princeton University, Department of Geological Sciences [Bloomington], Indiana University [Bloomington], Indiana University System-Indiana University System, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Geological Sciences [Providence], Brown University, NASA Goddard Space Flight Center (GSFC), NASA Ames Research Center (ARC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Geosciences [Stony Brook], Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), State University of New York (SUNY), NASA Johnson Space Center (JSC), NASA, Planetary Science Institute [Tucson] (PSI), Department of Physics [Guelph], University of Guelph, Space Remote Sensing Group (ISR-2), Los Alamos National Laboratory (LANL), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Center for Earth and Planetary Studies [Washington] (CEPS), Smithsonian National Air and Space Museum, Smithsonian Institution-Smithsonian Institution, Department of Earth and Space Sciences [Seattle], University of Washington [Seattle], Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Department of Geological Sciences [Austin], Jackson School of Geosciences (JSG), University of Texas at Austin [Austin]-University of Texas at Austin [Austin], Rensselaer Polytechnic Institute (RPI), Canadian Space Agency (CSA), NASA Headquarters, Institute of Meteoritics [Albuquerque] (IOM), The University of New Mexico [Albuquerque], University of Hawaii, Brock University [Canada], Cornell University [New York], Geophysical Laboratory [Carnegie Institution], Carnegie Institution for Science [Washington], Massachusetts Institute of Technology (MIT), Lunar and Planetary Institute [Houston] (LPI), GeoRessources, Centre National de la Recherche Scientifique (CNRS)-Université de Lorraine (UL)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Institut national des sciences de l'Univers (INSU - CNRS), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Carnegie Institution for Science, Institut national des sciences de l'Univers (INSU - CNRS)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), NWO-NSO: The role of perchlorates in the preservation of organic compounds on Mars, and Petrology

Subjects
Geologic Sediments, Salinity, Extraterrestrial Environment, Nitrogen, General Science & Technology, Iron, Curiosity rover, Mars, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Astrobiology, MSL Science Team, Exobiology, MSL, Martian, Multidisciplinary, fluvial-lacustrine environments, Biosphere, Water, Phosphorus, Mars Exploration Program, 15. Life on land, Hydrogen-Ion Concentration, Carbon, Oxygen, Planetary science, Bays, 13. Climate action, Rocknest, Sample Analysis at Mars, Sedimentary rock, Oxidation-Reduction, Geology, Sulfur, Hydrogen
Abstract

International audience; The Curiosity rover discovered fine-grained sedimentary rocks, which are inferred to represent an ancient lake and preserve evidence of an environment that would have been suited to support a martian biosphere founded on chemolithoautotrophy. This aqueous environment was characterized by neutral pH, low salinity, and variable redox states of both iron and sulfur species. Carbon, hydrogen, oxygen, sulfur, nitrogen, and phosphorus were measured directly as key biogenic elements; by inference, phosphorus is assumed to have been available. The environment probably had a minimum duration of hundreds to tens of thousands of years. These results highlight the biological viability of fluvial-lacustrine environments in the post-Noachian history of Mars.

Published
2014

36. Volatile and Organic Compositions of Sedimentary Rocks in Yellowknife Bay, Gale Crater, Mars

Author

M. A. Meyer, Mark I. Richardson, Robert C. Anderson, Marisa C. Palucis, Sara Navarro Lopez, Rodney C. Ewing, Sanjeev Gupta, Caroline Freissinet, Edward M. Stolper, James F. Bell, M. A. Ravine, I. G. Mitrofanov, Thomas F. Bristow, Dawn Y. Sumner, Joel A. Hurowitz, Robert M. Haberle, Claire E. Newman, Andrew Steele, Muriel Saccoccio, Leslie Keely, E. Pallier, Jason P. Dworkin, Claude Geffroy, Mary A. Voytek, Michael Caplinger, Fred Goesmann, Yann Parot, Maria-Paz Zorzano Mier, A. B. Sanin, S. W. Squyres, Javier Caride Rodriguez, J. L. Griffes, Julio José Romeral-Planello, Jason Feldman, Katherine L. French, V. Sautter, Nicolas Mangold, David L. Bish, Vivian Lafaille, Michael D. Smith, François Raulin, V. Prokhorov, Gilles Berger, S. Slavney, Heather B. Franz, S. Johnstone, Susanne P. Schwenzer, Felipe Gómez, Harri Haukka, Francis A. Cucinotta, J. Hudgins, T. Cleghorn, Pascaline Francois, Alain Lepinette Malvitte, Shuai Li, Paul R. Mahaffy, K. M. Robertson, Bruce M. Jakosky, J. Guo, Juergen Schieber, Rafael Navarro-González, G. J. Flesch, Scott M. McLennan, Jennifer G. Blank, M. Carmosino, Kenneth A. Farley, Yves Langevin, P. D. Archer, A. E. Brunner, M. D. Dyar, S. Le Mouélic, V. Hipkin, Sara Alejandra Sans Fuentes, Kenneth S. Edgett, Sabrina Feldman, Gale Paulsen, Paul Herrera, Alberto G. Fairén, Kirsten L. Siebach, Jan-Peter Muller, M. J. Schoppers, Eldar Noe Dobrea, Nina Lanza, Marc Gailhanou, Genevieve Marchand, Sönke Burmeister, Craig Hardgrove, Justin N. Maki, Ari-Matti Harri, Michael C. Malin, M. J. Wolff, Roger E. Summons, H. Blau, Jacqueline Cameron, Jeff A. Berger, Didier Keymeulen, Agnes Cousin, Guillermo M. Muñoz Caro, Eric Lyness, Cedric Pilorget, Michael B. Baker, Christopher S. Edwards, M. L. Litvak, Brian M. Duston, Rebecca M. E. Williams, T. Nolan, Robert T. Downs, V. E. Hamilton, Walter Goetz, Pamela G. Conrad, J. Baroukh, Nathan T. Bridges, Meenakshi Wadhwa, Roger C. Wiens, Samuel M. Clegg, Philippe Sarrazin, L. 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Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), NWO-NSO: The role of perchlorates in the preservation of organic compounds on Mars, Petrology, Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Centre National de la Recherche Scientifique (CNRS)-Muséum national d'Histoire naturelle (MNHN), and Kruch, Catherine

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

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

Published
2014

37. Mars' surface radiation environment measured with the Mars science laboratory's curiosity rover

Author

Donald M. Hassler, Cary Zeitlin, Robert F. Wimmer-Schweingruber, Bent Ehresmann, Scot Rafkin, Jennifer L. Eigenbrode, David E. Brinza, Gerald Weigle, Stephan Böttcher, Eckart Böhm, Soenke Burmeister, Jingnan Guo, Jan Köhler, Cesar Martin, Guenther Reitz, Francis A. Cucinotta, Myung-Hee Kim, David Grinspoon, Mark A. Bullock, Arik Posner, Javier Gómez-Elvira, Ashwin Vasavada, John P. Grotzinger, MSL Science Team, Osku Kemppinen, David Cremers, James F. Bell, Lauren Edgar, Jack Farmer, Austin Godber, Meenakshi Wadhwa, Danika Wellington, Ian McEwan, Claire Newman, Mark Richardson, Antoine Charpentier, Laurent Peret, Penelope King, Jennifer Blank, Mariek Schmidt, Shuai Li, Ralph Milliken, Kevin Robertson, Vivian Sun, Michael Baker, Christopher Edwards, Bethany Ehlmann, Kenneth Farley, Jennifer Griffes, Hayden Miller, Megan Newcombe, Cedric Pilorget, Melissa Rice, Kirsten Siebach, Katie Stack, Edward Stolper, Claude Brunet, Victoria Hipkin, Richard Léveillé, Geneviève Marchand, Pablo Sobrón Sánchez, Laurent Favot, George Cody, Andrew Steele, Lorenzo Flückiger, David Lees, Ara Nefian, Mildred Martin, Marc Gailhanou, Frances Westall, Guy Israël, Christophe Agard, Julien Baroukh, Christophe Donny, Alain Gaboriaud, Philippe Guillemot, Vivian Lafaille, Eric Lorigny, Alexis Paillet, René Pérez, Muriel Saccoccio, Charles Yana, Carlos Armiens‐Aparicio, Javier Caride Rodríguez, Isaías Carrasco Blázquez, Felipe Gómez Gómez, Sebastian Hettrich, Alain Lepinette Malvitte, Mercedes Marín Jiménez, Jesús Martínez-Frías, Javier Martín-Soler, F. Javier Martín-Torres, Antonio Molina Jurado, Luis Mora-Sotomayor, Guillermo Muñoz Caro, Sara Navarro López, Verónica Peinado-González, Jorge Pla-García, José Antonio Rodriguez Manfredi, Julio José Romeral-Planelló, Sara Alejandra Sans Fuentes, Eduardo Sebastian Martinez, Josefina Torres Redondo, Roser Urqui-O'Callaghan, María-Paz Zorzano Mier, Steve Chipera, Jean-Luc Lacour, Patrick Mauchien, Jean-Baptiste Sirven, Heidi Manning, Alberto Fairén, Alexander Hayes, Jonathan Joseph, Steven Squyres, Robert Sullivan, Peter Thomas, Audrey Dupont, Angela Lundberg, Noureddine Melikechi, Alissa Mezzacappa, Thomas Berger, Daniel Matthia, Benito Prats, Evgeny Atlaskin, Maria Genzer, Ari-Matti Harri, Harri Haukka, Henrik Kahanpää, Janne Kauhanen, Mark Paton, Jouni Polkko, Walter Schmidt, Tero Siili, Cécile Fabre, James Wray, Mary Beth Wilhelm, Franck Poitrasson, Kiran Patel, Stephen Gorevan, Stephen Indyk, Gale Paulsen, Sanjeev Gupta, David Bish, Juergen Schieber, Brigitte Gondet, Yves Langevin, Claude Geffroy, David Baratoux, Gilles Berger, Alain Cros, Claude d’Uston, Olivier Forni, Olivier Gasnault, Jérémie Lasue, Qiu-Mei Lee, Sylvestre Maurice, Pierre-Yves Meslin, Etienne Pallier, Yann Parot, Patrick Pinet, Susanne Schröder, Mike Toplis, Éric Lewin, Will Brunner, Ezat Heydari, Cherie Achilles, Dorothy Oehler, Brad Sutter, Michel Cabane, David Coscia, Cyril Szopa, Gilles Dromart, François Robert, Violaine Sautter, Stéphane Le Mouélic, Nicolas Mangold, Marion Nachon, Arnaud Buch, Fabien Stalport, Patrice Coll, Pascaline François, François Raulin, Samuel Teinturier, James Cameron, Sam Clegg, Agnès Cousin, Dorothea DeLapp, Robert Dingler, Ryan Steele Jackson, Stephen Johnstone, Nina Lanza, Cynthia Little, Tony Nelson, Roger C. Wiens, Richard B. Williams, Andrea Jones, Laurel Kirkland, Allan Treiman, Burt Baker, Bruce Cantor, Michael Caplinger, Scott Davis, Brian Duston, Kenneth Edgett, Donald Fay, Craig Hardgrove, David Harker, Paul Herrera, Elsa Jensen, Megan R. Kennedy, Gillian Krezoski, Daniel Krysak, Leslie Lipkaman, Michael Malin, Elaina McCartney, Sean McNair, Brian Nixon, Liliya Posiolova, Michael Ravine, Andrew Salamon, Lee Saper, Kevin Stoiber, Kimberley Supulver, Jason Van Beek, Tessa Van Beek, Robert Zimdar, Katherine Louise French, Karl Iagnemma, Kristen Miller, Roger Summons, Fred Goesmann, Walter Goetz, Stubbe Hviid, Micah Johnson, Matthew Lefavor, Eric Lyness, Elly Breves, M. Darby Dyar, Caleb Fassett, David F. Blake, Thomas Bristow, David DesMarais, Laurence Edwards, Robert Haberle, Tori Hoehler, Jeff Hollingsworth, Melinda Kahre, Leslie Keely, Christopher McKay, Lora Bleacher, William Brinckerhoff, David Choi, Pamela Conrad, Jason P. Dworkin, Melissa Floyd, Caroline Freissinet, James Garvin, Daniel Glavin, Daniel Harpold, Paul Mahaffy, David K. Martin, Amy McAdam, Alexander Pavlov, Eric Raaen, Michael D. Smith, Jennifer Stern, Florence Tan, Melissa Trainer, Michael Meyer, Mary Voytek, Robert C. Anderson, Andrew Aubrey, Luther W. Beegle, Alberto Behar, Diana Blaney, Fred Calef, Lance Christensen, Joy A. Crisp, Lauren DeFlores, Jason Feldman, Sabrina Feldman, Gregory Flesch, Joel Hurowitz, Insoo Jun, Didier Keymeulen, Justin Maki, Michael Mischna, John Michael Morookian, Timothy Parker, Betina Pavri, Marcel Schoppers, Aaron Sengstacken, John J. Simmonds, Nicole Spanovich, Manuel de la Torre Juarez, Christopher R. Webster, Albert Yen, Paul Douglas Archer, John H. Jones, Douglas Ming, Richard V. Morris, Paul Niles, Elizabeth Rampe, Thomas Nolan, Martin Fisk, Leon Radziemski, Bruce Barraclough, Steve Bender, Daniel Berman, Eldar Noe Dobrea, Robert Tokar, David Vaniman, Rebecca M. E. Williams, Aileen Yingst, Kevin Lewis, Laurie Leshin, Timothy Cleghorn, Wesley Huntress, Gérard Manhès, Judy Hudgins, Timothy Olson, Noel Stewart, Philippe Sarrazin, John Grant, Edward Vicenzi, Sharon A. Wilson, Victoria Hamilton, Joseph Peterson, Fedor Fedosov, Dmitry Golovin, Natalya Karpushkina, Alexander Kozyrev, Maxim Litvak, Alexey Malakhov, Igor Mitrofanov, Maxim Mokrousov, Sergey Nikiforov, Vasily Prokhorov, Anton Sanin, Vladislav Tretyakov, Alexey Varenikov, Andrey Vostrukhin, Ruslan Kuzmin, Benton Clark, Michael Wolff, Scott McLennan, Oliver Botta, Darrell Drake, Keri Bean, Mark Lemmon, Susanne P. Schwenzer, Ryan B. Anderson, Kenneth Herkenhoff, Ella Mae Lee, Robert Sucharski, Miguel Ángel de Pablo Hernández, Juan José Blanco Ávalos, Miguel Ramos, Charles Malespin, Ianik Plante, Jan-Peter Muller, Rafael Navarro-González, Ryan Ewing, William Boynton, Robert Downs, Mike Fitzgibbon, Karl Harshman, Shaunna Morrison, William Dietrich, Onno Kortmann, Marisa Palucis, Dawn Y. Sumner, Amy Williams, Günter Lugmair, Michael A. Wilson, David Rubin, Bruce Jakosky, Tonci Balic-Zunic, Jens Frydenvang, Jaqueline Kløvgaard Jensen, Kjartan Kinch, Asmus Koefoed, Morten Bo Madsen, Susan Louise Svane Stipp, Nick Boyd, John L. Campbell, Ralf Gellert, Glynis Perrett, Irina Pradler, Scott VanBommel, Samantha Jacob, Tobias Owen, Scott Rowland, Hannu Savijärvi, César Martín García, Reinhold Mueller-Mellin, John C. Bridges, Timothy McConnochie, Mehdi Benna, Heather Franz, Hannah Bower, Anna Brunner, Hannah Blau, Thomas Boucher, Marco Carmosino, Sushil Atreya, Harvey Elliott, Douglas Halleaux, Nilton Rennó, Michael Wong, Robert Pepin, Beverley Elliott, John Spray, Lucy Thompson, Suzanne Gordon, Horton Newsom, Ann Ollila, Joshua Williams, Paulo Vasconcelos, Jennifer Bentz, Kenneth Nealson, Radu Popa, Linda C. Kah, Jeffrey Moersch, Christopher Tate, Mackenzie Day, Gary Kocurek, Bernard Hallet, Ronald Sletten, Raymond Francis, Emily McCullough, Ed Cloutis, Inge Loes ten Kate, Raymond Arvidson, Abigail Fraeman, Daniel Scholes, Susan Slavney, Thomas Stein, Jennifer Ward, Jeffrey Berger, John E. Moores, NWO-NSO: The role of perchlorates in the preservation of organic compounds on Mars, Petrology, Southwest Research Institute [Boulder] (SwRI), Kiel University, NASA Goddard Space Flight Center (GSFC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), German Aerospace Center (DLR), University of Nevada [Reno], Universities Space Research Association (USRA), Denver Museum of Nature and Science, NASA Headquarters, Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), GeoRessources, and Centre National de la Recherche Scientifique (CNRS)-Université de Lorraine (UL)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
Extraterrestrial Environment, Surface Properties, Mars, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Cosmic ray, Radiation Dosage, Exploration of Mars, Astrobiology, Martian surface, Exobiology, galactic cosmic rays, solar energetic particles, Mars Science Laboratory’s Curiosity rover, Humans, Organic Chemicals, Particle radiation, Martian, Radiation Assessment Detector (RAD), Multidisciplinary, Mars Exploration Program, Space Flight, Radiation assessment detector, 13. Climate action, Health threat from cosmic rays, Deinococcus, Cosmic Radiation
Abstract

International audience; The Radiation Assessment Detector (RAD) on the Mars Science Laboratory's Curiosity rover began making detailed measurements of the cosmic ray and energetic particle radiation environment on the surface of Mars on 7 August 2012. We report and discuss measurements of the absorbed dose and dose equivalent from galactic cosmic rays and solar energetic particles on the martian surface for similar to 300 days of observations during the current solar maximum. These measurements provide insight into the radiation hazards associated with a human mission to the surface of Mars and provide an anchor point with which to model the subsurface radiation environment, with implications for microbial survival times of any possible extant or past life, as well as for the preservation of potential organic biosignatures of the ancient martian environment.

Published
2014

38. Isotope ratios of H, C, and O in CO2 and H2O of the martian atmosphere

Author

Chris R, Webster, Paul R, Mahaffy, Gregory J, Flesch, Paul B, Niles, John H, Jones, Laurie A, Leshin, Sushil K, Atreya, Jennifer C, Stern, Lance E, Christensen, Tobias, Owen, Heather, Franz, Robert O, Pepin, Andrew, Steele, Cherie, Achilles, Christophe, Agard, José Alexandre, Alves Verdasca, Robert, Anderson, Ryan, Anderson, Doug, Archer, Carlos, Armiens-Aparicio, Ray, Arvidson, Evgeny, Atlaskin, Andrew, Aubrey, Burt, Baker, Michael, Baker, Tonci, Balic-Zunic, David, Baratoux, Julien, Baroukh, Bruce, Barraclough, Keri, Bean, Luther, Beegle, Alberto, Behar, James, Bell, Steve, Bender, Mehdi, Benna, Jennifer, Bentz, Gilles, Berger, Jeff, Berger, Daniel, Berman, David, Bish, David F, Blake, Juan J, Blanco Avalos, Diana, Blaney, Jen, Blank, Hannah, Blau, Lora, Bleacher, Eckart, Boehm, Oliver, Botta, Stephan, Böttcher, Thomas, Boucher, Hannah, Bower, Nick, Boyd, Bill, Boynton, Elly, Breves, John, Bridges, Nathan, Bridges, William, Brinckerhoff, David, Brinza, Thomas, Bristow, Claude, Brunet, Anna, Brunner, Will, Brunner, Arnaud, Buch, Mark, Bullock, Sönke, Burmeister, Michel, Cabane, Fred, Calef, James, Cameron, John, Campbell, Bruce, Cantor, Michael, Caplinger, Javier, Caride Rodríguez, Marco, Carmosino, Isaías, Carrasco Blázquez, Antoine, Charpentier, Steve, Chipera, David, Choi, Benton, Clark, Sam, Clegg, Timothy, Cleghorn, Ed, Cloutis, George, Cody, Patrice, Coll, Pamela, Conrad, David, Coscia, Agnès, Cousin, David, Cremers, Joy, Crisp, Alain, Cros, Frank, Cucinotta, Claude, d'Uston, Scott, Davis, Mackenzie, Day, Manuel, de la Torre Juarez, Lauren, DeFlores, Dorothea, DeLapp, Julia, DeMarines, David, DesMarais, William, Dietrich, Robert, Dingler, Christophe, Donny, Bob, Downs, Darrell, Drake, Gilles, Dromart, Audrey, Dupont, Brian, Duston, Jason, Dworkin, M Darby, Dyar, Lauren, Edgar, Kenneth, Edgett, Christopher, Edwards, Laurence, Edwards, Bethany, Ehlmann, Bent, Ehresmann, Jen, Eigenbrode, Beverley, Elliott, Harvey, Elliott, Ryan, Ewing, Cécile, Fabre, Alberto, Fairén, Ken, Farley, Jack, Farmer, Caleb, Fassett, Laurent, Favot, Donald, Fay, Fedor, Fedosov, Jason, Feldman, Sabrina, Feldman, Marty, Fisk, Mike, Fitzgibbon, Melissa, Floyd, Lorenzo, Flückiger, Olivier, Forni, Abby, Fraeman, Raymond, Francis, Pascaline, François, Caroline, Freissinet, Katherine Louise, French, Jens, Frydenvang, Alain, Gaboriaud, Marc, Gailhanou, James, Garvin, Olivier, Gasnault, Claude, Geffroy, Ralf, Gellert, Maria, Genzer, Daniel, Glavin, Austin, Godber, Fred, Goesmann, Walter, Goetz, Dmitry, Golovin, Felipe, Gómez Gómez, Javier, Gómez-Elvira, Brigitte, Gondet, Suzanne, Gordon, Stephen, Gorevan, John, Grant, Jennifer, Griffes, David, Grinspoon, John, Grotzinger, Philippe, Guillemot, Jingnan, Guo, Sanjeev, Gupta, Scott, Guzewich, Robert, Haberle, Douglas, Halleaux, Bernard, Hallet, Vicky, Hamilton, Craig, Hardgrove, David, Harker, Daniel, Harpold, Ari-Matti, Harri, Karl, Harshman, Donald, Hassler, Harri, Haukka, Alex, Hayes, Ken, Herkenhoff, Paul, Herrera, Sebastian, Hettrich, Ezat, Heydari, Victoria, Hipkin, Tori, Hoehler, Jeff, Hollingsworth, Judy, Hudgins, Wesley, Huntress, Joel, Hurowitz, Stubbe, Hviid, Karl, Iagnemma, Steve, Indyk, Guy, Israël, Ryan, Jackson, Samantha, Jacob, Bruce, Jakosky, Elsa, Jensen, Jaqueline Kløvgaard, Jensen, Jeffrey, Johnson, Micah, Johnson, Steve, Johnstone, Andrea, Jones, Jonathan, Joseph, Insoo, Jun, Linda, Kah, Henrik, Kahanpää, Melinda, Kahre, Natalya, Karpushkina, Wayne, Kasprzak, Janne, Kauhanen, Leslie, Keely, Osku, Kemppinen, Didier, Keymeulen, Myung-Hee, Kim, Kjartan, Kinch, Penny, King, Laurel, Kirkland, Gary, Kocurek, Asmus, Koefoed, Jan, Köhler, Onno, Kortmann, Alexander, Kozyrev, Jill, Krezoski, Daniel, Krysak, Ruslan, Kuzmin, Jean Luc, Lacour, Vivian, Lafaille, Yves, Langevin, Nina, Lanza, Jeremie, Lasue, Stéphane, Le Mouélic, Ella Mae, Lee, Qiu-Mei, Lee, David, Lees, Matthew, Lefavor, Mark, Lemmon, Alain, Lepinette Malvitte, Richard, Léveillé, Éric, Lewin-Carpintier, Kevin, Lewis, Shuai, Li, Leslie, Lipkaman, Cynthia, Little, Maxim, Litvak, Eric, Lorigny, Guenter, Lugmair, Angela, Lundberg, Eric, Lyness, Morten, Madsen, Justin, Maki, Alexey, Malakhov, Charles, Malespin, Michael, Malin, Nicolas, Mangold, Gérard, Manhes, Heidi, Manning, Geneviève, Marchand, Mercedes, Marín Jiménez, César, Martín García, Dave, Martin, Mildred, Martin, Jesús, Martínez-Frías, Javier, Martín-Soler, F Javier, Martín-Torres, Patrick, Mauchien, Sylvestre, Maurice, Amy, McAdam, Elaina, McCartney, Timothy, McConnochie, Emily, McCullough, Ian, McEwan, Christopher, McKay, Scott, McLennan, Sean, McNair, Noureddine, Melikechi, Pierre-Yves, Meslin, Michael, Meyer, Alissa, Mezzacappa, Hayden, Miller, Kristen, Miller, Ralph, Milliken, Douglas, Ming, Michelle, Minitti, Michael, Mischna, Igor, Mitrofanov, Jeff, Moersch, Maxim, Mokrousov, Antonio, Molina Jurado, John, Moores, Luis, Mora-Sotomayor, John Michael, Morookian, Richard, Morris, Shaunna, Morrison, Reinhold, Mueller-Mellin, Jan-Peter, Muller, Guillermo, Muñoz Caro, Marion, Nachon, Sara, Navarro López, Rafael, Navarro-González, Kenneth, Nealson, Ara, Nefian, Tony, Nelson, Megan, Newcombe, Claire, Newman, Horton, Newsom, Sergey, Nikiforov, Brian, Nixon, Eldar, Noe Dobrea, Thomas, Nolan, Dorothy, Oehler, Ann, Ollila, Timothy, Olson, Miguel Ángel, de Pablo Hernández, Alexis, Paillet, Etienne, Pallier, Marisa, Palucis, Timothy, Parker, Yann, Parot, Kiran, Patel, Mark, Paton, Gale, Paulsen, Alex, Pavlov, Betina, Pavri, Verónica, Peinado-González, Laurent, Peret, Rene, Perez, Glynis, Perrett, Joe, Peterson, Cedric, Pilorget, Patrick, Pinet, Jorge, Pla-García, Ianik, Plante, Franck, Poitrasson, Jouni, Polkko, Radu, Popa, Liliya, Posiolova, Arik, Posner, Irina, Pradler, Benito, Prats, Vasily, Prokhorov, Sharon Wilson, Purdy, Eric, Raaen, Leon, Radziemski, Scot, Rafkin, Miguel, Ramos, Elizabeth, Rampe, François, Raulin, Michael, Ravine, Günther, Reitz, Nilton, Rennó, Melissa, Rice, Mark, Richardson, François, Robert, Kevin, Robertson, José Antonio, Rodriguez Manfredi, Julio J, Romeral-Planelló, Scott, Rowland, David, Rubin, Muriel, Saccoccio, Andrew, Salamon, Jennifer, Sandoval, Anton, Sanin, Sara Alejandra, Sans Fuentes, Lee, Saper, Philippe, Sarrazin, Violaine, Sautter, Hannu, Savijärvi, Juergen, Schieber, Mariek, Schmidt, Walter, Schmidt, Daniel, Scholes, Marcel, Schoppers, Susanne, Schröder, Susanne, Schwenzer, Eduardo, Sebastian Martinez, Aaron, Sengstacken, Ruslan, Shterts, Kirsten, Siebach, Tero, Siili, Jeff, Simmonds, Jean-Baptiste, Sirven, Susie, Slavney, Ronald, Sletten, Michael, Smith, Pablo, Sobrón Sánchez, Nicole, Spanovich, John, Spray, Steven, Squyres, Katie, Stack, Fabien, Stalport, Thomas, Stein, Noel, Stewart, Susan Louise Svane, Stipp, Kevin, Stoiber, Ed, Stolper, Bob, Sucharski, Rob, Sullivan, Roger, Summons, Dawn, Sumner, Vivian, Sun, Kimberley, Supulver, Brad, Sutter, Cyril, Szopa, Florence, Tan, Christopher, Tate, Samuel, Teinturier, Inge, ten Kate, Peter, Thomas, Lucy, Thompson, Robert, Tokar, Mike, Toplis, Josefina, Torres Redondo, Melissa, Trainer, Allan, Treiman, Vladislav, Tretyakov, Roser, Urqui-O'Callaghan, Jason, Van Beek, Tessa, Van Beek, Scott, VanBommel, David, Vaniman, Alexey, Varenikov, Ashwin, Vasavada, Paulo, Vasconcelos, Edward, Vicenzi, Andrey, Vostrukhin, Mary, Voytek, Meenakshi, Wadhwa, Jennifer, Ward, Eddie, Weigle, Danika, Wellington, Frances, Westall, Roger Craig, Wiens, Mary Beth, Wilhelm, Amy, Williams, Joshua, Williams, Rebecca, Williams, Richard B, Williams, Mike, Wilson, Robert, Wimmer-Schweingruber, Mike, Wolff, Mike, Wong, James, Wray, Megan, Wu, Charles, Yana, Albert, Yen, Aileen, Yingst, Cary, Zeitlin, Robert, Zimdar, and María-Paz, Zorzano Mier

Subjects
Atmosphere, Martian, chemistry.chemical_compound, Multidisciplinary, Meteorite, chemistry, Stable isotope ratio, Sample Analysis at Mars, Carbonate, Mars Exploration Program, Atmosphere of Mars, Astrobiology
Abstract

Mars' Atmosphere from Curiosity The Sample Analysis at Mars (SAM) instrument on the Curiosity rover that landed on Mars in August last year is designed to study the chemical and isotopic composition of the martian atmosphere. Mahaffy et al. (p. 263 ) present volume-mixing ratios of Mars' five major atmospheric constituents (CO 2 , Ar, N 2 , O 2 , and CO) and isotope measurements of 40 Ar/ 36 Ar and C and O in CO 2 , based on data from one of SAM's instruments, obtained between 31 August and 21 November 2012. Webster et al. (p. 260 ) used data from another of SAM's instruments obtained around the same period to determine isotope ratios of H, C, and O in atmospheric CO 2 and H 2 O. Agreement between the isotopic ratios measured by SAM with those of martian meteorites, measured in laboratories on Earth, confirms the origin of these meteorites and implies that the current atmospheric reservoirs of CO 2 and H 2 O were largely established after the period of early atmospheric loss some 4 billion years ago.

Published
2013

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