abstract: The James Webb Space Telescope (JWST) is expected to revolutionize the current understanding of Jovian worlds over the coming decade. However, as the field pushes towards characterizing cooler, smaller, “terrestrial-like” planets, dedicated next-generation facilities will be required to tease out the small spectral signatures indicative of biological activity. Here, the feasibility of determining atmospheric properties, from near to mid-infrared transmission spectra, of transiting temperate terrestrial M-dwarf companions, has been evaluated. Specifically, atmospheric retrievals were utilized to explore the trade space between spectral resolution, wavelength coverage, and signal-to-noise on the ability to both detect molecular species and constrain their abundances. Increasing spectral resolution beyond R=100 for near-infrared wavelengths, shorter than 5um, proves to reduce the degeneracy between spectral features of different molecules and thus greatly benefits the abundance constraints. However, this benefit is greatly diminished beyond 5um as any overlap between broad features in the mid-infrared does not deconvolve with higher resolutions. Additionally, the inclusion of features beyond 11um did not meaningfully improve the detection significance nor abundance constraints results. The findings of this study indicate that an instrument with continuous wavelength coverage from approximately 2-11um and with a resolution of R~50-300, would be capable of detecting H2O, CO2, CH4, O3, and N2O in the atmosphere of an Earth-analog transiting an M-dwarf (magK=8.0) within 50 transits, and obtain better than an order-of-magnitude constraint on each of their abundances. The Origins Space Telescope (Origins) is one of four flagship mission concepts, under review by the 2020 Decadal Survey, that may take the mantle of the next-generation space-based observatory. In conjunction with this research, a secondary trade space study was performed on behalf of the Origins Exoplanets Working Group. The primary purpose of this collaboration was to provide a scientific basis to the technical specifications for the mid-infrared detectors onboard the Mid-Infrared Spectrometer Camera Transit Spectrometer (MISC-T) instrument. The results of this work directly contributed to the alteration of the official technical specifications of the instrument design concept. / Dissertation/Thesis / Masters Thesis Astrophysics and Astronomy 2019

Modern microbialites provide the opportunity to explore the influences of biology on microbialite formation and understand how biosignatures can be preserved in these structures. In this study, we compared δ13Ccarb values from nodule and surface biofilm carbonates on microbialite structures across depths and locations throughout Pavilion Lake to evaluate whether variable light exposure produced limitations to biosignature formation. At depths below 21 m, vertical profiling of δ13Ccarb across colour transitions of surface biofilm on microbialite structures was performed to identify spatial arrangement of autotrophic and heterotrophic biosignatures. Finally, preservation of the photosynthetic biosignature over time was investigated by collecting carbonates beneath the microbialite surface. These investigations were performed in order to better characterize the factors controlling biosignature formation, distribution, and preservation within Pavilion Lake.Decreasing trends of δ13Ccarb with depth across study sites indicated that attenuated sunlight in the water column is likely the primary control on biosignature formation. Below 21 m, photosynthetic enrichments representing biosignatures on microbialite surfaces were reduced and recorded δ13Ccarb values that fell within the predicted equilibrium range. Biosignature loss is suggested to result from the relative proportions of autotrophic and heterotrophic processes changing at depths and producing average δ13Ccarb values. Variability of where biosignatures are lost on the microbialite surface indicated that the spatial extent of photosynthetic communities producing enrichments is potentially influenced by variable incidences of light at these depths. Although no definitive biosignatures of heterotrophy were identified, several interfaces were identified where the balancing proportions of autotrophic and heterotrophic processes influenced by light variability potentially mediate biosignature loss. Decreasing trends of δ13Ccarb beneath the microbialite surface and estimates of past microbialite growth rates indicated that surface biosignatures are lost within 100 – 400 years. It is suggested that infilling processes overprint enrichments and deplete δ13Ccarb values due to heterotrophic abundance below the microbialite surface. This is supported by an isotopic mass balance that predicts smaller inputs of heterotrophically-depleted DIC are required to sufficiently overprint δ13Ccarb enrichments. These results concluded that the photosynthetic biosignature identified in Pavilion Lake is short-lived and mitigated by biological processes. / Thesis / Master of Science (MSc)

No / Morphological biosignatures (features related to life) and associated terrestrial sedimentary structures that provide possible sampling targets for the remote astrobiological exploration of planets have been analysed using Raman spectroscopic techniques. The spectral data from a suite of samples comprising crypto-chasmoendoliths, preserved microbial filaments and relict sedimentary structures comprise a preliminary database for the establishment of key Raman biosignatures. This will form the basis for the evaluation of prototype miniaturised instrumentation for the proposed ESA ExoMars mission scheduled for 2013. The Raman spectral biosignatures of carotenoids and scytonemin, organic biomolecules characteristic of the cyanobacterial colonisation of geological matrices and biogeologically modified minerals are also identifiable in the sedimentary specimen materials. The results of this study demonstrate the basis of the molecular recognition of extinct and extant exobiology that will feed into the elemental structural analyses of morphological structures provided by associated SEM, XRD and laser-induced breakdown spectroscopy (LIBS) techniques on robotic analytical landers.

Le European Extremely Large Telescope présentement en construction au Chili, sera le plus grand télescope optique jamais construit, avec son miroir primaire de 39 mètres de diamètre. Un de ses instruments, ANDES (ArmazoNes high Dispersion Echelle Spectrograph), combinera l’optique adaptative et la spectroscopie à haute dispersion dans les bandes photométriques YJH pour permettre notamment l’étude de la composition chimique d’atmosphères d’exoplanètes potentiellement habitables. La détection de la vie sur une exoplanète candidate commence nécessairement par l’étude de son atmosphère, et spécifiquement sa composition chimique. Celle-ci peut en effet révéler la présence de biosignatures, c’est-à-dire la signature spectrale de molécules qui ne pourraient exister sans la présence de la vie. Une paire de molécules particulièrement intéressante est la paire dioxygène (O2) et méthane (CH4), soient deux molécules qui peuvent être créées par des processus biotiques, mais qui, laissées à elles-mêmes, réagissent ensemble dans l’atmosphère pour générer de l’eau (H2O) et du dioxyde de carbone (CO2) jusqu’à la déplétion de l’une des deux (Thompson et al., 2022). La présence simultanée d’O2 et de CH4 nécessite donc des réactions chimiques hors équilibre comme celles associées avec l’activité biologique. ANDES sera équipé de tous les modules théoriquement nécessaires pour détecter la lumière réfléchie d'une exoplanète, incluant une interface d'optique adaptative qui minimise la lumière parasite de l'exoplanète localisée tout près du coeur de l'étoile, une unité de champ intégral permettant de disséquer l'image de l'étoile en des dizaines de spaxels, chacun alimentant un spectrographe infrarouge à haute dispersion. Des techniques statistiques bayesiennes sont ensuite utilisées pour détecter le signal atmosphérique de l'exoplanète enfoui dans le spectre de l'étoile. Ce travail décrit des simulations détaillées de tous ces modules afin de déterminer les capacités d’ANDES à détecter l’atmosphère d’exoplanètes potentiellement habitables, notamment Proxima b, la plus rapprochée du Système Solaire. Les simulations révèlent que si Proxima b a une atmosphère identique à celle de la Terre, l’eau y serait détectable en moins d'une nuit (6 heures), alors que les détections d’O2, de CO2 et de CH4 nécessiteraient jusqu’à 320, 420 et 1200 heures d’observation, respectivement. / The European Extremely Large Telescope, currently under construction in Chile, will be the largest telescope ever built, with its primary mirror measuring 39 meters in diameter. One of its instruments, ANDES (ArmazoNes high Dispersion Echelle Spectrograph), will combine adaptive optics and high dispersion dpectroscopy in the Y JH photometric bands. This combination will allow the study of the chemical composition of atmospheres of potentially habitable exoplanets. The search for life on a candidate exoplanet necessitates the study of its atmosphere, specically its chemical composition. This can reveal the presence of biosignatures, i.e the spectral signature of molecules that cannot exist without life. One inriguing pair of molecules is dioxygen (O2) and methane (CH4). Both can be created through biotic processes, but left to themselves, they form water (H2O) and carbon dioxide (CO2) until one of the two is depleted. The simultaneous presence of O2 and CH4 requires out-of-equilibrium chemical reactions, such as those associated with biological activity. ANDES will be equipped with all the crucial modules to detect the reflected light from an exoplanet. It includes an adaptive optics front-end interface that minimizes the stray light from the exoplanet located very close to the star’s core, an integrated field unit that dissects the star’s image into dozens of spaxels, each feeding a high-dispersion infrared spectrograph. Bayesian statistics are then used to detect the exoplanet’s atmospheric signal buried within the star’s spectrum This work describes detailed simulations of all these modules to determine ANDES’ ca- pabilities in detecting the atmosphere of potentially habitable exoplanets, notably Proxima b, the closest to the Solar System. The simulations reveal that if Proxima b has an atmo- sphere similar to Earth’s, water could be detectable in less than one night (6 hours), while detections of O2, CO2 and CH4 could require up to 320, 420 and 1200 hours of observations, respectively.

A Astrobiologia é uma área de pesquisa crescente no Brasil, na qual se estuda o fenômeno da vida no Universo. Um de seus subtemas estuda as bioassinaturas: substâncias que evidenciam da presença de vida, passada ou presente. Foram investigadas em laboratório a detectabilidade de biomoléculas, que são potenciais bioassinaturas moleculares, e a fotoestabilidade de suas assinaturas espectroscópicas em ambientes extraterrestres simulados. Os experimentos foram baseados em irradiações no ultravioleta, que é a principal faixa da radiação solar responsável pela evolução e degradação de moléculas orgânicas em ambientes espaciais. Um maior foco foi dado aos pigmentos biológicos β-caroteno e clorofila a, os quais foram irradiados puros e/ou misturados a diferentes substratos inorgânicos, mimetizando superfícies de planetas rochosos, satélites e asteroides. Foram utilizadas as instalações do Laboratório Nacional de Luz Síncrotron (LNLS), em especial a linha de luz TGM, na faixa do UV, VUV e EUV, e também lâmpadas de baixa pressão que emitem na faixa do UVC. Na Câmara de Simulação Espacial e Planetária (AstroCam), do Núcleo de Pesquisa em Astrobiologia da USP (NAP/Astrobio), diversos parâmetros ambientais foram controlados para simular as condições da superfície de Marte. E balões de alta-altitude foram utilizados para testar a resposta de biomoléculas na estratosfera, cujas condições são similares às da superfície marciana, além de validar experimentos que podem ser enviados em missões espaciais. As mudanças nas respostas espectroscópicas das biomoléculas foram medidas por absorbância no UV-Vis e no IR e por espalhamento Raman, algumas in situ e em tempo real e outras ex situ. As técnicas provaram ser adequadas para esses estudos pois forneceram informações sobre as fotoestabilidades das respostas espectroscópicas das biomoléculas, permitindo testar seus potenciais como bioassinaturas em diferentes superfícies do Sistema Solar. Os resultados também podem contribuir para missões espaciais, dando suporte ao desenvolvimento e otimização de técnicas e procedimentos para estudar os efeitos da exposição de biomoléculas a ambientes espaciais reais – em missões de pequeno porte e baixo custo, como CubeSats –, e até mesmo para a detecção de bioassinaturas em superfícies planetárias extraterrestres. / Astrobiology is a growing research area Brazil, which studies the phenomenon of life in the Universe. One of its sub-themes studies biosignatures: substances which evidence the presence of life, past or present. The detectability of biomolecules, which are potential molecular biosignatures, and the photostability of their spectroscopic signatures in simulated extraterrestrial environments were investigated in laboratory. The experiments were based on irradiations in the ultraviolet, which is the main range of solar radiation responsible for the evolution and degradation of organic molecules in space environments. The research was focused in the biological pigments β-carotene and chlorophyll a, which were irradiated in both pure form and/or mixed with different inorganic substrates, mimicking the surfaces of rocky planets, satellites and asteroids. The facilities of the Brazilian Synchrotron Light Laboratory (LNLS) were used, especially the TGM beamline in the UV, VUV and EUV range, as well as low pressure lamps emitting in the UVC range. In the Space and Planetary Simulation Chamber (AstroCam) of the Astrobiology Research Unit of USP, several environmental parameters were controlled to simulate the surface conditions of Mars. And high-altitude balloons were used to test the response of biomolecules in the stratosphere, where the conditions are similar to those of the Martian surface, in addition to validate experiments which can be sent in space missions. Changes in the biomolecules spectroscopic responses were measured by UV-Vis and IR absorbance and by Raman scattering, either in situ and in real time or ex situ. The techniques proved to be adequate for these studies, since they provided information on the photostability of the biomolecules spectroscopic responses, allowing the testing of their potential as biosignatures on different surfaces of the Solar System. The results can also contribute to space missions, supporting the development and optimization of techniques and procedures, both for the exposure of biomolecules to real space environments – in small and low-cost missions, such as CubeSats –, as well as for the actual detection of biosignatures on extraterrestrial planetary surfaces.

No description available.

A Astrobiologia é uma área de pesquisa crescente no Brasil, na qual se estuda o fenômeno da vida no Universo. Um de seus subtemas estuda as bioassinaturas: substâncias que evidenciam da presença de vida, passada ou presente. Foram investigadas em laboratório a detectabilidade de biomoléculas, que são potenciais bioassinaturas moleculares, e a fotoestabilidade de suas assinaturas espectroscópicas em ambientes extraterrestres simulados. Os experimentos foram baseados em irradiações no ultravioleta, que é a principal faixa da radiação solar responsável pela evolução e degradação de moléculas orgânicas em ambientes espaciais. Um maior foco foi dado aos pigmentos biológicos β-caroteno e clorofila a, os quais foram irradiados puros e/ou misturados a diferentes substratos inorgânicos, mimetizando superfícies de planetas rochosos, satélites e asteroides. Foram utilizadas as instalações do Laboratório Nacional de Luz Síncrotron (LNLS), em especial a linha de luz TGM, na faixa do UV, VUV e EUV, e também lâmpadas de baixa pressão que emitem na faixa do UVC. Na Câmara de Simulação Espacial e Planetária (AstroCam), do Núcleo de Pesquisa em Astrobiologia da USP (NAP/Astrobio), diversos parâmetros ambientais foram controlados para simular as condições da superfície de Marte. E balões de alta-altitude foram utilizados para testar a resposta de biomoléculas na estratosfera, cujas condições são similares às da superfície marciana, além de validar experimentos que podem ser enviados em missões espaciais. As mudanças nas respostas espectroscópicas das biomoléculas foram medidas por absorbância no UV-Vis e no IR e por espalhamento Raman, algumas in situ e em tempo real e outras ex situ. As técnicas provaram ser adequadas para esses estudos pois forneceram informações sobre as fotoestabilidades das respostas espectroscópicas das biomoléculas, permitindo testar seus potenciais como bioassinaturas em diferentes superfícies do Sistema Solar. Os resultados também podem contribuir para missões espaciais, dando suporte ao desenvolvimento e otimização de técnicas e procedimentos para estudar os efeitos da exposição de biomoléculas a ambientes espaciais reais – em missões de pequeno porte e baixo custo, como CubeSats –, e até mesmo para a detecção de bioassinaturas em superfícies planetárias extraterrestres. / Astrobiology is a growing research area Brazil, which studies the phenomenon of life in the Universe. One of its sub-themes studies biosignatures: substances which evidence the presence of life, past or present. The detectability of biomolecules, which are potential molecular biosignatures, and the photostability of their spectroscopic signatures in simulated extraterrestrial environments were investigated in laboratory. The experiments were based on irradiations in the ultraviolet, which is the main range of solar radiation responsible for the evolution and degradation of organic molecules in space environments. The research was focused in the biological pigments β-carotene and chlorophyll a, which were irradiated in both pure form and/or mixed with different inorganic substrates, mimicking the surfaces of rocky planets, satellites and asteroids. The facilities of the Brazilian Synchrotron Light Laboratory (LNLS) were used, especially the TGM beamline in the UV, VUV and EUV range, as well as low pressure lamps emitting in the UVC range. In the Space and Planetary Simulation Chamber (AstroCam) of the Astrobiology Research Unit of USP, several environmental parameters were controlled to simulate the surface conditions of Mars. And high-altitude balloons were used to test the response of biomolecules in the stratosphere, where the conditions are similar to those of the Martian surface, in addition to validate experiments which can be sent in space missions. Changes in the biomolecules spectroscopic responses were measured by UV-Vis and IR absorbance and by Raman scattering, either in situ and in real time or ex situ. The techniques proved to be adequate for these studies, since they provided information on the photostability of the biomolecules spectroscopic responses, allowing the testing of their potential as biosignatures on different surfaces of the Solar System. The results can also contribute to space missions, supporting the development and optimization of techniques and procedures, both for the exposure of biomolecules to real space environments – in small and low-cost missions, such as CubeSats –, as well as for the actual detection of biosignatures on extraterrestrial planetary surfaces.

Life on Earth likely began as an RNA world, where cell-free or compartmentalized ribonucleic acid (RNA) molecules dominated as the replicating and evolving lifeforms prior to the emergence of DNA- and protein-based life. The focus of this thesis is on when and how this RNA world emerged. We use astrophysical and geophysical studies to constrain when the Earth was habitable, and biosignature studies to constrain when the Earth was inhabited. From this we obtain a time interval for the emergence of life. Considering all these constraints, we find that the Earth was habitable as early as 4.5 Ga, or as late as 3.9 Ga, depending on whether the early influx of asteroids inhibited life from emerging. The time that the Earth was inhabited is more precisely constrained to 3.7 Ga. This suggests life emerged within 800 Myr, and possibly in < 200 Myr. Between 4.5–3.7 Ga, the continental crust was slowly rising up from the global ocean, providing dry land on which warm little ponds could form. We develop the theory for the emergence of RNA polymers in these pond environments, whose wet-dry cycles promote polymerization. RNA is comprised of chains of nucleotides, and the latter is made up of ribose, phosphate, and a characteristic nucleobase. We numerically model the survival and evolution of nucleobases in warm little ponds from meteorite and interplanetary dust sources. The wet-dry cycles of our ponds are controlled by precipitation, evaporation, and seepage. The nucleobase sinks include photodissociation, seepage, and hydrolysis. Nucleobase and nucleotide seepage is efficient, therefore nucleotides and RNA molecules must have emerged rapidly (< a few years) in order to avoid falling through pores at the base of the pond. We find that meteorites, not interplanetary dust particles, are the dominant source of nucleobases used for RNA synthesis. Finally, under these conditions, we find that first RNA polymers likely emerged before 4.17 Ga. / Thesis / Master of Science (MSc)

Mars is one of the best candidates among planetary bodies for supporting life. The presence of water in the form of ice and atmospheric vapour together with the availability of biogenic elements and energy are indicators of the possibility of hosting life as we know it. The occurrence of permanently frozen ground – permafrost, is a common phenomenon on Mars and it shows multiple morphological analogies with terrestrial permafrost. Despite the extreme inhospitable conditions, highly diverse microbial communities inhabit terrestrial permafrost in large numbers. Among these are methanogenic archaea, which are anaerobic chemotrophic microorganisms that meet many of the metabolic and physiological requirements for survival on the martian subsurface. Moreover, methanogens from Siberian permafrost are extremely resistant against different types of physiological stresses as well as simulated martian thermo-physical and subsurface conditions, making them promising model organisms for potential life on Mars. The main aims of this investigation are to assess the survival of methanogenic archaea under Mars conditions, focusing on methanogens from Siberian permafrost, and to characterize their biosignatures by means of Raman spectroscopy, a powerful technology for microbial identification that will be used in the ExoMars mission. For this purpose, methanogens from Siberian permafrost and non-permafrost habitats were subjected to simulated martian desiccation by exposure to an ultra-low subfreezing temperature (-80ºC) and to Mars regolith (S-MRS and P-MRS) and atmospheric analogues. They were also exposed to different concentrations of perchlorate, a strong oxidant found in martian soils. Moreover, the biosignatures of methanogens were characterized at the single-cell level using confocal Raman microspectroscopy (CRM). The results showed survival and methane production in all methanogenic strains under simulated martian desiccation. After exposure to subfreezing temperatures, Siberian permafrost strains had a faster metabolic recovery, whereas the membranes of non-permafrost methanogens remained intact to a greater extent. The strain Methanosarcina soligelidi SMA-21 from Siberian permafrost showed significantly higher methane production rates than all other strains after the exposure to martian soil and atmospheric analogues, and all strains survived the presence of perchlorate at the concentration on Mars. Furthermore, CRM analyses revealed remarkable differences in the overall chemical composition of permafrost and non-permafrost strains of methanogens, regardless of their phylogenetic relationship. The convergence of the chemical composition in non-sister permafrost strains may be the consequence of adaptations to the environment, and could explain their greater resistance compared to the non-permafrost strains. As part of this study, Raman spectroscopy was evaluated as an analytical technique for remote detection of methanogens embedded in a mineral matrix. This thesis contributes to the understanding of the survival limits of methanogenic archaea under simulated martian conditions to further assess the hypothetical existence of life similar to methanogens on the martian subsurface. In addition, the overall chemical composition of methanogens was characterized for the first time by means of confocal Raman microspectroscopy, with potential implications for astrobiological research. / Der Mars ist unter allen Planeten derjenige, der aufgrund verschiedener Faktoren am wahrscheinlichsten Leben ermöglichen kann. Das Vorhandensein von Wasser in Form von Eis und atmosphärischem Dampf zusammen mit der Verfügbarkeit biogener Elemente sowie Energie sind Indikatoren für die Möglichkeit, Leben, wie wir es kennen, zu beherbergen. Das Auftreten von dauerhaft gefrorenen Böden, oder auch Permafrost, ist ein verbreitetes Phänomen auf dem Mars. Dabei zeigen sich vielfältige morphologische Analogien zum terrestrischen Permafrost. Permafrostgebiete auf der Erde, welche trotz extremer, Bedingungen durch eine große Zahl und Vielfalt mikrobieller Gemeinschaften besiedelt sind, sind hinsichtlich möglicher Habitate auf dem Mars die vielversprechendste Analogie. Die meisten methanogenen Archaeen sind anaerobe, chemolithotrophe Mikroorganismen, die auf der Marsoberfläche viele der metabolischen und physiologischen Erfordernisse zum Überleben vorfinden. Methanogene Archaeen aus dem sibirischen Permafrost sind zudem extrem resistent gegenüber unterschiedlichen Formen von physiologischem Stress sowie simulierten thermo-physikalischen Marsbedingungen. Die Hauptziele dieser Untersuchung bestehen darin, das Überleben der methanogenen Archaeen unter Marsbedingungen zu beurteilen, wobei der Fokus auf methanogenen Archaeen aus dem sibirischen Permafrost liegt, sowie deren Biosignaturen mit Hilfe der Raman-Spektroskopie zu charakterisieren, einer starken Technologie zur mikrobiellen Identifikation, welche bei der ExoMars-Mission zum Einsatz kommen wird. Zu diesem Zweck wurden methanogene Archaeen aus dem sibirischen Permafrost sowie aus Nicht-Permafrost-Habitaten in Simulationen Marsbedingungen ausgesetzt, wie Austrocknung durch Langzeitversuche bei ultraniedrigen Temperaturen unter dem Gefrierpunkt (-80ºC), Mars-analogen Mineralien (S-MRS und P-MRS) sowie einer Marsatmosphäre. Weiterhin wurden die Kulturen verschiedenen Konzentrationen von Magnesiumperchlorat, einem starken Oxidant, der im Marsboden nachgewiesenen wurde, ausgesetzt. Ferner wurden die Biosignaturen einzelner Zellen der methanogenen Archaeen mit Hilfe der konfokalen Raman-Mikrospektroskopie (CRM) charakterisiert. Die Ergebnisse zeigten für alle untersuchten methanogenen Stämme Überleben und Methanbildung, nachdem diese simulierten Austrocknungsbedingungen ausgesetzt worden waren. Nach Versuchen mit Temperaturen unter dem Gefrierpunkt zeigten die Stämme aus dem sibirischen Permafrost eine schnellere Wiederaufnahme der Stoffwechseltätigkeit, wohingegen bei den Referenzorganismen aus Nicht-Permafrost-Habitaten die Zell¬membranen im größeren Ausmaß intakt blieben. Der Stamm Methanosarcina soligelidi SMA-21 aus dem sibirischen Permafrost zeigte nach dem Belastungstest mit Marsboden und Mars-analoger Atmosphäre signifikant höhere Methanbildungsraten. Zudem überlebten alle untersuchten Stämme die Zugabe von Magnesiumperchlorat in der entsprechenden Konzentration, die auf dem Mars vorkommt. Weiterhin konnten durch die Raman-Spektroskopie beachtliche Unterschiede in der chemischen Zusammensetzung zwischen methanogenen Archaeen aus Permafrost- und Nicht-Permafrost-Habitaten, trotz ihrer phylogenetischen Verwandtschaft, ermittelt werden. Die Konvergenz der chemischen Zusammensetzung der Permafrost-Stämme könnte das Resultat ihrer Anpassung an die Umgebung sein, was auch die Unterschiede hinsichtlich ihrer Resistenz verglichen mit Nicht-Permafrost-Stämmen erklären könnte. Als Teil dieser Studie wurde die Raman-Spektroskopie als Analyse-Technik zur Ferndetektion von methanogenen Archaeen, welche in eine Mineral-Matrix eingebettet sind, evaluiert. Diese Dissertation trägt zu einem besseren Verständnis hinsichtlich der Grenzen für ein Überleben von methanogenen Archaeen unter simulierten Marsbedingungen bei und damit zu einer Beurteilung der Hypothese, ob es ähnliches Leben unter der Marsoberfläche geben könnte. Darüber hinaus wurde erstmalig die chemische Zusammensetzung von methanogenen Archaeen mit Hilfe der Raman-Mikrospektroskopie charakterisiert. Dieser Technologie kommt eine wesentliche Bedeutung für weitere Forschungstätigkeit in der Astrobiologie zu.

O Distrito Grafitífero Aracoiába-Baturité apresenta depósitos do tipo gnaisse grafitoso (minério disseminado) e veio (minério maciço) com diferentes origens genéticas e com características físicas e ambientes geológicos de formação próprios. O minério tipo gnaisse grafitoso é de origem sedimentar, singenético, com teores de 1,5 a 8% de C, que se distribuem ao longo de duas extensas faixas paralelas, hospedadas na Subunidade Baturité, que constitui um importante metalotecto regional. A associação de grafita metamórfica disseminada em metassedimentos da Sequência Acarápe constitui um geoindicador de antiga bacia sedimentar neoproterozóica e, também, pode ser considerado como zona de geosutura resultante do subsequente fechamento de um oceano primitivo. As rochas desta subunidade correspondem na paleogeografia da Sequência Acarápe aos fácies de sopé de talude e de planície abissal. O minério tipo veio (fluido depositado) é epigenético e, com teores entre 20% e 70% de C, forma corpos tabulares e bolsões, controlados em escala local por estruturas de alívio (falhas, fraturas, zonas de contato, eixos de dobras etc.) que permitiram a percolação de soluções penumatolíticas relacionadas ao corpo plutônico de Pedra Aguda. As variações dos valores das relações entre isótopos estáveis de carbono (&#948;13C) na grafita do minério disseminado são de -26,72 a -23,52 e do minério maciço de -27,03 a -20,83, revelando sinal de atividades biológicas (bioassinaturas) e permitem afirmar que a grafita das amostras acima são derivadas de matéria orgânica. Foram apresentados os principais guias de prospecção para grafita e testados os seguintes métodos geofísicos: Eletro-Resistividade; GPR - Ground Penetrating Radar; Magnetometria; VLF (Very Low Frequency); e Polarização Induzida Espectral (IPS) / Resistividade (ER). A conjugação dos métodos de Polarização Induzida Espectral (IPS) e Eletro Resistividade (ER) foi o que demonstrou a melhor eficiência. Com relação à determinação do teor de carbono por termogravimetria (ATG), que é o método mais utilizado para este elemento. Verificou-se, que as faixas de queima atribuídas ao carbono no minério do Distrito de Aracoiába-Baturité (340&#61616; a 570C e de 570 a 1050C) eram diferentes das faixas do minério de Minas Gerais (350&#61616;C a 650&#61616;C e 650&#61616;C a 1.050&#61616;C). Esta constatação indica a necessidade de se determinar previamente as faixas de temperatura para cada região pesquisada. / The Aracoiába-Baturité Graphite-bearing District has graphitic gneiss deposits (disseminated ore) and vein (solid ore) with different genetic origins and their own physical characteristics and geological environments. The graphite gneiss ore is of sedimentary, syngenetic origin, with 1.5% to 8% C content, which is distributed along two long parallel belts, hosted in the Baturité Sub-unit, which consists of a major regional metallotect. The association of metamorphic graphite disseminated in metasediments of the Acarápe Sequence consists of a geoindicator of an old Neo-Proterozoic sedimentary basin and also can be considered a geosuture zone, the result of the subsequent closing of a primitive ocean. The rocks of this subunit correspond in the paleogeography of the Acarápe Sequence to the facies of the bottom of a slope and of an abyssal plain. The vein ore (deposited fluid) is epigenetic and, with C contents of between 20% and 70%, forms tabular bodies and pockets, controlled on a local scale by relief structures (faults, fractures, contact zones, fold axes, etc.), which allowed seepage of pneumatolithic solutions relating to the plutonic body of Pedra Aguda. The variations in the values of the ratios between stable carbon isotopes (&#948;13C) in the graphite of the disseminated ore are -26.72 to -23.52 and of the solid ore -27.03 to -20.83, showing a sign of biological activities (biosignatures), and it can be said that the graphite of the above samples is derived from organic matter. The main prospecting guides for graphite were presented and the following geophysical methods tested: Electro-resistivity (ER); Ground Penetrating Radar (GPR); Magnetometry; Very Low Frequency (VLF); and Spectral Induced Polarization (SIP) / Electro-resistivity (ER). It was found that the combination of the Spectral Induced Polarization (SIP) and Electro-resistivity (ER) methods proved the most efficient. In relation to determining the carbon content using thermogravimetry (TG), which is the most commonly used method for this element, it was found that the bands of burning attributed to the carbon in the ore in the Aracoiába-Baturité District (340 to 570C and from 570oC to 1050C) were different from the bands of the ore in Minas Gerais (350C to 650C and 650C to 1050C). This finding suggests the need to determine beforehand the temperature ranges for each region studied.