No / Calcium and magnesium carbonates are important minerals found in sedimentary environments. Although sandstones are the most common rock colonized by endolith organisms, the production of calcium and magnesium carbonates is important in survival strategies of organisms and as a source for the removal of oxalate ions. Extremophile organisms in some situations may convert or destroy carbonates of calcium and magnesium, which gives important information about the conditions under which these organisms can survive. The identification on the surface of Mars of 'White Rock' formations, in Juventae Chasma or Sabaea Terra, as possibly carbonate rocks makes the study of these minerals a prerequisite of remote Martian exploration. Here, we show the protocol for the identification by Raman spectroscopy of different calcium and magnesium carbonates and we present a database of relevance in the search for life, extinct or extant, on Mars; this will be useful for the assessment of data obtained from remote, miniaturized Raman spectrometers now proposed for Mars exploration.

Depuis 2004, les rovers Spirit et Opportunity de la mission MER (Mars Exploration Rover) explorent leurs sites d'atterrissage respectifs, le cratère Gusev et les plaines de Meridiani. Ces travaux de thèse portent sur l'analyse et l'interprétation des données de l'instrument APXS (Alpha-Particle X-ray Spectrometer), situé au bout du bras articulé de chacun des rovers, dont le rôle est de déterminer la composition chimique des roches et des sols martiens par spectrométrie X. Grâce à leur surprenante longévité, Spirit et Opportunity ont pu s'éloigner à plusieurs km de leurs lieux d'atterrissage initiaux et les APXS ont analysé de nombreux échantillons fournissant des indices sur le rôle que l'eau a pu jouer dans le passé martien. J'ai d'abord choisi d'étudier cette diversité d'échantillons à l'aide d'une approche d'analyse multidimensionnelle. Ceci m'a permis de réaliser une classification des échantillons et de mettre en évidence les relations pétrogénétiques entre les roches et les sols de Gusev et Meridiani. Je présenterai les principaux résultats obtenus grâce à cette méthode ainsi que leur lien avec l'organisation spatiale et stratigraphique des échantillons. Je montrerai ensuite comment ces résultats m'ont incité à tester un modèle géochimique numérique d'altération de basalte martien par un brouillard acide de SO3. Je décrirai les hypothèses de ce modèle avant d'en comparer les résultats avec les données MER. Nous verrons enfin quelles en sont les implications, au niveau de la géologie des sites de Gusev et Meridiani et plus généralement vis-à-vis de l'histoire géologique de Mars et des conditions qui ont prévalu à sa surface dans le passé.

How the dust cycle works on Mars is a key atmospheric issue, as the dust cycle is arguably the dominant cycle in the current Martian climate. In addition, how much is known about the Martian planetary boundary layer is mostly determined from models with very little in-situ data from contemporaneous studies to validate such boundary layer characteristic assumptions, and the model studies have not been able to define a known height for a possible boundary layer on Mars using ground-based investigations prior to this research. The Mars Exploration Rovers (MERs), however, show promise in offering a unique chance to take surface-based measurements to offer support for dust and boundary layer measurements made from remote sensors. There are three main objectives of this study: to constrain the late-afternoon maximum height of the boundary layer for both MER sites, to constrain the mean particle size and variance of the size distribution in the atmosphere, and to use these results to demonstrate that sunset and twilight imaging is a useful survey of otherwise difficult-to-determine parameters that are needed in several tools for studying Mars’ atmosphere. A modeling approach using twilight-based Sun imaging by the MERs (Sol 1959 for Spirit and Sol 695 for Opportunity) is used to constrain boundary layer and dust particle size parameters. After determining which parameters control which observables, resulting elevations and azimuths are matched up to specific observations from the available MER datasets. A Monte Carlo code produces the model that is then compared to Sol data with plotting of resulting error. Results include PBL height and structure estimations and plots along with generalized particle size information for each MER site on the given Sol. Figures show comparisons of this study’s particle size results with that of previous studies as well as maps of fit qualities for boundary layer parameters compared to a contemporaneous modeled scale height estimation. Results show promise for planning future MER-based campaigns and models.

The Alpha Particle X-ray Spectrometer (APXS) on the Mars Exploration Rovers possesses the ability to detect carbon and oxygen within martian samples via Rutherford backscattering principles. Several consecutive measurements of the martian atmosphere by Spirit, paralleled by Monte Carlo simulations, provided an energy calibration to mitigate the absence of an alpha-mode calibration pre-flight. Data from a pre-flight thermal acceptance test agreed with this energy calibration, confirming the presence of an unexpected offset. Correcting a bug in the APXS firmware resulted in a temperature-independent energy scale. A model was developed and applied to all atmospheric data illustrating a dip in atmospheric peak areas, potentially arising from a week-long weather event on Mars. An early expansion of this model to solid samples has not yet been able to detect any hydrated minerals or carbonates. Preliminary investigations into determining martian atmospheric pressure and potential elemental layering within samples shows promise.

One of the most important steps in the search for life on Mars is to determine if a specific sub-surface location it is "habitable", or that it provides the conditions and requirements to support life as we know it. In this thesis, I present a miniature, thermal-IR radiometer and reflectometer designed to determine temperature, the presence of water ice, and the discrimination of minerals, all necessary for a habitable environment. A dual use detector was selected for the thermal and five reflectance channels. The IR source is provided by five LEDs. These components were embedded in a thermally controlled aluminium block. Integrated electronics provided signal amplification and demodulation. This device will be suitable for drilling applications with less than 25 mm diameter boreholes and with limited available power (<5watts). Thermal testing was within a simulated borehole mounted in a thermal vacuum chamber. The results were compared to a theoretical model of the expected temperature. The maximum temperature error between predicted and measured was 0.21 K (∼0.08%). The total RMS error of all sources were calculated to be <3%. Reflectance testing in all five channels included a variety of minerals and a two point calibration method. The results were compared to the predicted reflectance values for the samples. The results of the reflectance channel testing demonstrated that the measured values matched the predicted values with a 2.5% measured error. The total RMS error was 6.1%. Detection and discrimination of water ice and hydrated minerals included a non-linear mixing model and/or testing. The model predicted that water ice mixed in a pyroxene mineral matrix can be detected and discriminated from 5% to 60% concentration by weight. Testing with a hydrated mineral mixed within a non-hydrated mineral matrix demonstrated that the measured result matched the predicted result from 5-45% concentration by weight.

abstract: Future robotic and human missions to the Moon and Mars will need in situ capabilities to characterize the mineralogy of rocks and soils within a microtextural context. Such spatially-correlated information is considered crucial for correct petrogenetic interpretations and will be key observations for assessing the potential for past habitability on Mars. These data will also enable the selection of the highest value samples for further analysis and potential caching for return to Earth. The Multispectral Microscopic Imager (MMI), similar to a geologist's hand lens, advances the capabilities of current microimagers by providing multispectral, microscale reflectance images of geological samples, where each image pixel is comprised of a 21-band spectrum ranging from 463 to 1735 nm. To better understand the capabilities of the MMI in future surface missions to the Moon and Mars, geological samples comprising a range of Mars-relevant analog environments as well as 18 lunar rocks and four soils, from the Apollo collection were analyzed with the MMI. Results indicate that the MMI images resolve the fine-scale microtextural features of samples, and provide important information to help constrain mineral composition. Spectral end-member mapping revealed the distribution of Fe-bearing minerals (silicates and oxides), along with the presence of hydrated minerals. In the case of the lunar samples, the MMI observations also revealed the presence of opaques, glasses, and in some cases, the effects of space weathering in samples. MMI-based petrogenetic interpretations compare favorably with laboratory observations (including VNIR spectroscopy, XRD, and thin section petrography) and previously published analyses in the literature (for the lunar samples). The MMI was also deployed as part of the 2010 ILSO-ISRU field test on the slopes of Mauna Kea, Hawaii and inside the GeoLab as part of the 2011 Desert RATS field test at the Black Point Lava Flow in northern Arizona to better assess the performance of the MMI under realistic field conditions (including daylight illumination) and mission constraints to support human exploration. The MMI successfully imaged rocks and soils in outcrops and samples under field conditions and mission operation scenarios, revealing the value of the MMI to support future rover and astronaut exploration of planetary surfaces. / Dissertation/Thesis / Ph.D. Geological Sciences 2012

An unsupervised fuzzy logic navigation algorithm is designed and implemented in simulation for the Subsurface Explorer planetary exploration robot. The robot is intended for the subterranean exploration of Mars, and will be equipped with acoustic sensing for detecting obstacles. Measurements of obstacle distance and direction are anticipated to be imprecise however, since the performance of acoustic sensors is degraded in underground environments. Fuzzy logic is a satisfactory means of addressing imprecision in plant characteristics, and has been implemented in a variety of autonomous vehicle navigation applications. However, most fuzzy logic algorithms that perform well in unknown environments have large rule-bases or use complex methods for tuning fuzzy membership functions and rules. These qualities make them too computationally intensive to be used for planetary exploration robots like the SSX. In this thesis, we introduce an unsupervised fuzzy logic algorithm that can determine a trajectory for the SSX through unknown environments. This algorithm uses a combination of simple fusion of robot behaviors and self-tuning membership functions to determine robot navigation without resorting to the degree of complexity of previous fuzzy logic algorithms. Finally, we present some simulation results that demonstrate the practicality of our algorithm in navigating in different environments. The simulations justify the use of our fuzzy logic technique, and suggest future areas of research for fuzzy logic navigation algorithms. / Master of Science

Supersonic deceleration has been identified as a critical deficiency in extending heritage technologies to the high-mass systems required to achieve long-term exploration goals at Mars. Supersonic retropropulsion (SRP), or the use of retropropulsive thrust while an entry vehicle is traveling at supersonic conditions, is an approach addressing this deficiency. The focus of this dissertation is aerodynamic and performance evaluation of SRP as a decelerator technology for high-mass Mars entry systems. This evaluation was completed through a detailed SRP performance analysis, establishment of the relationship between vehicle performance and the aerodynamic-propulsive interaction, and an assessment of the required fidelity and computational cost in simulating SRP flowfields, with emphasis on the effort required in conceptual design. Trajectory optimization, high-fidelity computational aerodynamic analysis, and analytical modeling of the SRP aerodynamic-propulsive interaction were used to define the fidelity and effort required to evaluate individual SRP concepts across multiple mission scales.

Martian clouds and dust play an important part of the radiative transfer and energy balance budget. To assist in fully understanding the impact of clouds and dust, the complete diurnal cycle needs to be characterized. One of the best methods to track diurnal variations on Mars is by measuring optical depth. The spatial and temporal trends of optical depth give insight into the dust and water cycles of the Martian atmosphere. Until now, spacecraft could only obtain optical depth during the day. In this thesis, nighttime images from the Mars Exploration Rover Spirit are used to calculate nighttime optical depth using photometric methods to capture star flux. Bright stars in well-known constellations are used in this analysis. The observed flux was compared to the expected flux to give nighttime optical depth values. The observed nighttime optical depth was consistently similar to the daytime optical depth values on both an individual image and sol-averaged basis. Recommendations are made going forward to use the Mars Science Laboratory Curiosity for conducting an optimal nighttime optical depth campaign to fully characterize the diurnal dust and water cycles of Mars. The Curiosity rover is well suited for nighttime imaging and can potentially provide valuable insight into the nighttime dust and cloud trends.

Parmi les études novatrices que l'on peut aborder depuis l'orbite martienne en utilisant les données multiangulaires de l'instrument HRSC (canaux nadir, stéréographique et photométrique) de Mars Express, figure la détermination des caractéristiques physiques de la surface, pour cartographier les variations des propriétés physiques des sols et des roches de Mars et les relier aux observations spectroscopiques et thermiques réalisées par les instruments OMEGA, TES et THEMIS. <br /> Les modèles de Minnaert et de fonction de phase à deux termes de Hapke s'accordent pour démontrer que les observations multiangulaires de HRSC acquises au cours de la mission sur le cratère Gusev et le flanc sud de Apollinaris peuvent, sous certaines limites, être assemblées pour produire une fonction de phase couvrant un grand intervalle d'angles de phase (5-95°) avec une résolution spatiale de l'ordre de 400 mètres à 1.6 kilomètres.<br /><br />Combiné à la rugosité de surface, l'effet d'opposition joue un rôle significatif, <br />suggérant que les propriétés optiques de l'état de surface au niveau de Gusev sont fortement influencées par la porosité, l'état de compaction et l'organisation de la couche superficielle du régolite. L'aspect cartographique de la présente étude photométrique est utile pour donner une meilleure signification aux variations observées. Selon les tendances générales de cette analyse, il est très probable que la variation photométrique observée, au moins pour les régions centre et Ouest du cratère Gusev, soit partiellement due aux régimes des vents dominants, ces derniers ayant une orientation Nord - Nord Ouest / Sud - Sud Est et induisant une perturbation de la couche supérieure de la surface. Les résultats de cette étude photométrique sont en accord avec des études indépendantes basées sur les données orbitales d'inertie thermique et de spectroscopie de réflectance, et également des données photométriques et d'imagerie microscopique réalisées in situ par les instrument du rover Spirit. Cela conforte l'idée de l'existence en surface d'une couche composée de poussière à grains fins qui aurait été enlevée au niveau des unités de faible albédo révélant ainsi un substrat basaltique sombre formé de matériaux à grains plus grossiers. <br /><br />Ces résultats ouvrent de nouvelles possibilités pour documenter les processus de surface sur les planètes.