LIBS; Water; Hydrogen; ChemCam; Mars; Low pressure; Roughness;CHEMCAM INSTRUMENT SUITE; QUANTITATIVE-ANALYSIS; INDUCED DESORPTION; SOLID-SURFACES; INDUCED PLASMA; LOW-PRESSURES; GALE CRATER; MARS; CONFINEMENT; IMPROVEMENT

On Mars, Laser-Induced Breakdown Spectroscopy CUBS) as performed by the ChemCam instrument can be used to measure the hydrogen content of targets in situ, under a low pressure CO2 atmosphere. However, unexpected variations observed in the Martian dataset suggest an effect related to target roughness. Here, we present a series of laboratory experiments that reproduce the effect observed on Mars and explore possible causes. We show that the hydrogen peak intensity increases significantly with increasing exposure of the target surface to the LIBS plasma, and that these variations are specific to hydrogen, as other emission lines in the spectra are not affected. The increase of the signal could be related to an addition of hydrogen to the plasma due to interaction with the surrounding target surface, yet the exact physical process to explain such effect remains to be identified. More generally, this effect should be taken into account for the quantification of hydrogen in any LIBS applications where the roughness of the target is significant. (C) 2017 Elsevier B.V. All rights reserved.

INDUCED PLASMA SPECTROSCOPY; CHEMCAM INSTRUMENT SUITE; VACUUM-ULTRAVIOLET; QUANTITATIVE-ANALYSIS; GALE CRATER; RADIATION CONDITIONS; STEEL ANALYSIS; SURFACE; MOLECULES; ROVER

Organic matter has been continuously delivered by meteorites and comets to Mars since its formation, and possibly formed in situ by abiogenic and/or biogenic processes, This organic matter may be preserved from the harsh oxidizing environment of Mars in specific locations. Together with water, organic molecules are necessary to the emergence of life as we know it. Since the first martian landers, scientists have been searching for organics and until today, only one positive detection has been made by a Gas Chromatography Mass Spectrometer (GCMS) instrument onboard the Curiosity rover. In this article we investigate a complementary approach to guide the search for organic matter using ChemCam, the first Laser-Induced Breakdown Spectroscopy (LIBS) instrument on Mars. This experimental study focuses on the analysis of carbon and nitrogen LIBS signatures in organoclay samples and allows the determination of the critical level (L-c) and limit of detection (LoD) of these elements with LIBS under Mars-like conditions, giving new insights into the search of organic matter on Mars. (C) 2017 Elsevier B.V. All rights reserved.

Laser-induced breakdown spectroscopy; ChemCam; Hydrogen; Water; Hydration;CHEMCAM INSTRUMENT SUITE; GALE CRATER; OMEGA/MARS EXPRESS; CURIOSITY; HYDROGEN; CALIBRATION; ROVER; MINERALS; CHLORINE; REGOLITH

Laser induced breakdown spectroscopy (LIBS), as performed by the ChemCam instrument, provides a new technique to measure hydrogen at the surface of Mars. Using a laboratory replica of the LIBS instrument onboard the Curiosity rover, different types of hydrated samples (basalts, calcium and magnesium sulfates, opals and apatites) covering a range of targets observed on Mars have been characterized and analyzed. A number of factors related to laserparameters, atmospheric conditions and differences in targets properties can affect the standoff LIBS signal, and in particular the hydrogen emission peak. Dedicated laboratory tests were run to identify a normalization of the hydrogen signal which could best compensate for these effects and enable the application of the laboratory calibration to Mars data. We check that the hydrogen signal increases linearly with water content; and normalization of the hydrogen emission peak using to oxygen and carbon emission peaks (related to the breakdown of atmospheric carbon dioxide) constitutes a robust approach. Moreover, the calibration curve obtained is relatively independent of the samples types. (C) 2017 Elsevier B.V. All rights reserved.

laser-induced breakdown spectroscopy; ChemCam; Mars Science Laboratory; trace elements; weathering; magmatic differentiation;INDUCED BREAKDOWN SPECTROSCOPY; MARTIAN SOIL COMPONENT; NORTHWEST AFRICA 7034; IN-SITU; INSTRUMENT SUITE; METEORITE; LITHIUM; MINERALOGY; TARGETS; WATER

The Chemistry Camera (ChemCam) instrument onboard Curiosity can detect minor and trace elements such as lithium, strontium, rubidium, and barium. Their abundances can provide some insights about Mars' magmatic history and sedimentary processes. We focus on developing new quantitative models for these elements by using a new laboratory database (more than 400 samples) that displays diverse compositions that are more relevant for Gale crater than the previous ChemCam database. These models are based on univariate calibration curves. For each element, the best model is selected depending on the results obtained by using the ChemCam calibration targets onboard Curiosity. New quantifications of Li, Sr, Rb, and Ba in Gale samples have been obtained for the first 1000 Martian days. Comparing these data in alkaline and magnesian rocks with the felsic and mafic clasts from the Martian meteorite NWA7533from approximately the same geologic periodwe observe a similar behavior: Sr, Rb, and Ba are more concentrated in soluble- and incompatible-element-rich mineral phases (Si, Al, and alkali-rich). Correlations between these trace elements and potassium in materials analyzed by ChemCam reveal a strong affinity with K-bearing phases such as feldspars, K-phyllosilicates, and potentially micas in igneous and sedimentary rocks. However, lithium is found in comparable abundances in alkali-rich and magnesium-rich Gale rocks. This very soluble element can be associated with both alkali and Mg-Fe phases such as pyroxene and feldspar. These observations of Li, Sr, Rb, and Ba mineralogical associations highlight their substitution with potassium and their incompatibility in magmatic melts.