MarsSI: Martian surface data processing information system

Quantin‐Nataf, Cathy; Lozac’h, L.; Thollot, P.; Loizeau, D.; Bultel, B.; Fernando, J.; Allemand, Pascal; Dubuffet, F.; Poulet, F.; Ody, A.; Clénet, H.; Leyrat, C.; Harrisson, Sandra

doi:10.1016/j.pss.2017.09.014

Cited by 46 publications

(34 citation statements)

References 29 publications

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“…All data cubes were downloaded via the MarsSI application (Quantin‐Nataf et al, ) and processed with CRISM Analysis Toolkit version 7.3.1 (Murchie et al, ). This process includes a photometric correction and a “volcano scan” correction for atmospheric gas absorptions (Langevin et al, ; McGuire et al, ).…”

Section: Methodsmentioning

confidence: 99%

“…The data were collected in the targeted mode in the spectral range of 1.00 to 3.92 μm, with a spectral resolution of ≈6 nm and a full spatial resolution of ≈18 m/pixel. All data cubes were downloaded via the MarsSI application (Quantin-Nataf et al, 2018) and processed with CRISM Analysis Toolkit version 7.3.1 . This process includes a photometric correction and a "volcano scan" correction for atmospheric gas absorptions (Langevin et al, 2005;McGuire et al, 2009).…”

Section: Crism Processingmentioning

confidence: 99%

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Detection of Carbonates in Martian Weathering Profiles

et al. 2019

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Noachian surfaces on Mars exhibit vertical assemblages of weathering horizons termed as weathering profiles; this indicates that surface water caused alteration of the rocks that required a different, warmer climate than today. Evidence of this early Martian climate with CO2 vapor as the main component causing greenhouse warming has been challenged by the lack of carbonate in these profiles. Here we report the analysis of Compact Reconnaissance Imaging Spectrometer for Mars L‐detector data leading to the detections of carbonates using a spectral signature exclusively attributed to them. The carbonates are collocated with hydroxylated minerals in weathering profiles over the Martian surface. The origin of CO2 for the formation of carbonates could be the atmosphere. The widespread distribution of weathering profiles with carbonates over the surface of the planet suggest global interactions between fluids containing carbonate/bicarbonate ions with the surface of Mars in the presence of atmospheric water until around 3.7 billion years ago.

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Section: Methodsmentioning

confidence: 99%

Section: Crism Processingmentioning

confidence: 99%

Detection of Carbonates in Martian Weathering Profiles

et al. 2019

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“…In order to achieve sufficient spatial resolution for our volume measurements, CTX digital elevation models (DEMs) were made for the floor central pits with MarsSI (https://emars.univ‐lyon1.fr; Quantin‐Nataf et al, ) and NASA's Ames Stereo Pipeline (Moratto et al, ) using CTX images downloaded from PILOT (https://pilot.wr.usgs.gov; Akins et al, ). Once the CTX images and DEMs were processed, they were analyzed in ArcMap 10.1 with sinusoidal projection centered on the host crater.…”

Section: Methodsmentioning

confidence: 99%

Formation of Central Pits in Impact Craters on Mars: A Statistical Investigation of Proposed Mechanisms

2019

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Central pit craters (CPCs) are complex craters that exhibit depressions within their floors or central uplifts. Some proposed models for central pit formation can be grouped by similar mechanism: (A) explosive volatile release, (B) central peak collapse, and (C) drainage of subsurface melted volatiles. We test these groups of mechanisms for central pit formation on Mars based on morphometries expected from each mechanism. Volatiles in the target (A and C) would be expected to result in a correlation with layered ejecta, also formed from volatiles, for CPCs over non‐CPCs. Central peak collapse (B) should result in larger diameters for pit rims than central peaks due to outward flow. Explosive volatile release (A) should yield smaller volumes for pit rims than pits due to mass loss. Data were collected on Context Camera images and digital elevation models for random samples of CPCs to assess the presence of these expected morphologies. Results of a Fisher exact test showed no preference in layered ejecta with CPCs over non‐CPCs, inconsistent with volatiles in the target. Results of an independent t test showed that central pit rim diameters are larger than central peak diameters, supporting some component of central peak collapse, although measurement uncertainty makes this interpretation tentative. Central pit rim volumes were not found to be statistically smaller than their pits, weighing against formation by explosive volatile release. Thus, our findings do not support any single group of formation mechanism tested here, although they allow for formation by some combination of these (or other) processes.

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“…Further connectivity is also planned with the MarsSI environment (Lozac'h et al, Quantin-Nataf et al, 2017). An automated procedure to set up an EPN-TAP service from existing planetary OGC Web Services is being devised, to populate the EPN-TAP parameters from existing OGC service functionalities.…”

Section: Figure 10: Mars Background Map Grabbed Through Wms With Crismentioning

confidence: 99%

VESPA: A community-driven Virtual Observatory in Planetary Science

Erard

Cecconi

Sidaner

et al. 2018

Planetary and Space Science

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The VESPA data access system focuses on applying Virtual Observatory (VO) standards and tools to Planetary Science. Building on a previous EC-funded Europlanet program, it has reached maturity during the first year of a new Europlanet 2020 program (started in 2015 for 4 years). The infrastructure has been upgraded to handle many fields of Solar System studies, with a focus both on users and data providers. This paper describes the broad lines of the current VESPA infrastructure as seen by a potential user, and provides examples of real use cases in several thematic areas. These use cases are also intended to identify hints for future developments and adaptations of VO tools to Planetary Science.

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MarsSI: Martian surface data processing information system

Cited by 46 publications

References 29 publications

Detection of Carbonates in Martian Weathering Profiles

Detection of Carbonates in Martian Weathering Profiles

Formation of Central Pits in Impact Craters on Mars: A Statistical Investigation of Proposed Mechanisms

VESPA: A community-driven Virtual Observatory in Planetary Science

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