Antes de se fazer uma estimativa ou uma simulação geoestatística, os domínios geológicos devem ser modelados de forma que cada domínio utilize apenas dados que pertencem a ele. Na industria mineral a incerteza oriunda dos teores geralmente é levada em consideração, entretanto a incerteza gerada pelo modelo nem sempre é analisada. Sabendo que a maior fonte de incerteza está na transição de uma litologia para outra, essa dissertação visa avaliar a incerteza do modelo geológico através de simulações de funções distâncias assinaladas em zonas de maior incerteza, gerando vários modelos com diferentes proporções de cada litologias. Um estudo de caso em um banco de dados real com alta complexidade geológica é utilizado para avaliar o uso da metodologia. O método se mostrou eficaz para avaliar o impacto da diferença de volume que cada litologia pode alcançar, demonstrando a importância de medir a incerteza na construção de modelos geológicos. / Before making an estimation or a geostatistical simulation, geological domains must be modeled so that each domain uses only data that belongs to it. In the mineral industry the uncertainty derived from the grades is generally taken into account, however the uncertainty generated by the model is not always analyzed. Knowing that the greatest source of uncertainty is in the transition from one lithology to another, this dissertation aims to evaluate the uncertainty of the geological model through signed distances function simulation in uncertainty zones, generating several models with different proportions of each lithology. A case study in a real dataset with high geological complexity is used to evaluate the use of the methodology. The method proved effective in assessing the impact of the volume difference that each lithology can reach, demonstrating the importance of measuring uncertainty in the construction of geological models.

Nos encontramos em uma localização vantajosa para o estudo da formação e evolução de galáxias espirais. Situados no disco da Via-Láctea, somos capazes de fazer observações detalhadas sobre as estrelas individuais que a compõem. Com o avanço tecnológico das últimas décadas, foi possível coletar um grande conjunto de informações, (e.g. composição química, cinemática, astrometria e parâmetros atmosféricos), com alta resolução para uma vasta parte do volume Galáctico. Com o objetivo de compreender melhor a nossa Galáxia, desenvolvemos uma ferramenta, chamada StarHorse, que estima parâmetros como distâncias, idades, massas e avermelhamento utilizando informação disponível em levantamentos espectroscópicos, fotométricos e astrométricos. O código StarHorse estima os parâmetros através de um método Bayesiano, que constrói uma distribuição de probabilidade a partir do cálculo de verossimilhança entre observações e modelos de evolução teórica e a partir de priores Galácticos bem conhecidos. Os parâmetros que o StarHorse estima são cruciais para estudos de arqueologia Galáctica. Com eles é possível investigar a estrutura, o histórico de formação estelar, a função de massa inicial, o mapa tridimensional da nossa Galáxia e também adicionar vínculos a modelos quemodinâmicos da Via Láctea Neste trabalho, focaremos na descrição e validação do método, testando sua aplicabilidade em levantamentos recentes de espectroscópica, astrometria e fotometria. Também disponibilizamos catálogos com distâncias e extinção para comunidade astronômica. As nossas distâncias e extinções se tornaram referência dentro da colaboração APOGEE e foram liberadas junto com o seu Data Release 14. Ademais, catálogos foram liberados para os surveys RAVE, Gaia-ESO e GALAH. Neste trabalho, exploramos os resultados do StarHorse, especialmente os resultados APOGEE, em um contexto amplo de arqueologia Galáctica. / We are in an advantageous position to study the formation and evolution of disk galaxies. By being inside the Milky Way, we are able to make detailed observations about the individual stars that compose it. With the technological revolution of the latest years, it has been possible to collect a massive set of information, (e.g. chemical composition, kinematics, astrometry, and atmospheric parameters), with high resolution for a large portion of the Galactic volume. With the goal to understand better our Galaxy, we developed a tool, called StarHorse, that can estimate distances, ages, masses, and extinction from the available spectroscopic, astrometric, and photometric information. StarHorse makes these estimates through a Bayesian method, that builds a probability distribution over the models by calculating a likelihood function between observation and stellar evolution models, and by using common knowledge about our Galaxy as priors. The parameters that StarHorse estimates are crucial to Galactic archaeology studies. With them, we can investigate the structure, the star formation history, the initial mass function, the three-dimensional dust map of our Galaxy, and provide constraints to chemodynamical models of the Milky Way. In this work, we focus on the description and validation of the method, testing its applicability in recent spectroscopic and astrometric surveys. We also make available catalogs with distances and extinctions to the astronomy community. Our distances and extinctions became a reference inside the APOGEE-team and were released as part of the SDSS Data Release 14. Moreover, we made available catalogs also to other spectroscopic surveys such as Gaia-ESO, RAVE, and GALAH. In this work, we also explore these results, especially for APOGEE, in a broad Galactic archaeology context.

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Resumo: Foram analisados 100 dentes primeiros molares e 100 dentes segundos molares superiores, direitos e esquerdos, permanentes, extraídos de humanos, com o objetivo de explorar a região anatômica da furca, mais especificamente realizar medidas das distâncias das aberturas das furcas vestibular, mesial, e distal até à junção esmalte-cemento, e das distâncias das referidas aberturas até às faces radiculares pertinentes: vestibular, mesial, distal e lingual. Utilizou-se para mensuração um microcomputador 486 DX-66Mhz, no qual estava instalado um software analisador de imagens Mocha-Jandel Scientific SigmaScan Pro, version 2.0. Em relação às distâncias das aberturas das furcas até à junção esmalte-cemento foi observado que as distâncias médias para a furca vestibular foram de 3,50mm e 3,03mm; para a furca mesial de 4,44mm e 4,69mm; para a furca distal de 4,26mm e 3,73mm, respectivamente para os primeiros e segundos molares superiores. Em relação às distâncias das aberturas das furcas até às faces radiculares pertinentes foi observado que as distâncias médias da furca vestibular até à face mesial da raiz mesio-vestibular foram de 3,78mm e 3,72mm; da furca vestibular até a face distal da raiz disto-vestibular 3,62 e 3,64mm; da furca mesial até à face vestibular da raiz mesio-vestibular 7,33mm e 6,89mm; da furca mesial até a face lingual da raiz lingual de 4,13mm e 4,33mm; da furca distal até à face vestibular da raiz disto-vestibular de 5,61mm e 5,09mm; da furca distal até a face lingual da raiz lingual de 4,73mm e 4,65mm, respectivamente para os primeiros e segundos molares superiores. / Abstract: Two hundred teeth were analysed, out of which 100 were first molars and 100 were second molars, extracted from humans, aiming the examination of the furcal anatomical region, more specifically the measurement of the distances from the buccal, mesial and distal furcal openings.to the cement-enamel junction, and the distances from the quoted openings to the bucal, mesial, distal and lingual root faces. It was made use of a 486 DX-66Mhz personal computer, in which a Mocha-Jandel Scientific SigmaScan Pro image software, version 2.0, was installed. In relation to the distances from the furcal openings to the cement-enamel junction, it was observed that the average distances for the bucal furcal were 3.50 mm and 3.03mm, for the mesial furcal , 4.44mm and 4.69mm; for the distal furcal, 4.26mm and 3.73mm, for the first and second maxillary molars, respectively. In relation to the distances from the furcal openings to the radicular faces , it was observed that the average distances from the bucal furcal to the mesial face of mesio-vestibular root were 3.78 mm and 3.72mm; from the bucal furcal to the (face distal da raiz disto-vestibular), 3.62mm and 3.64mm; from the mesial furcal to the buccal face of the mesio-vestibular root, 7.33mm and 6.89 mm; from the mesial furcal to the lingual face of the lingual root, 4.13mm and 4.33mm; from the distal furcal to the bucal face of the disto-vestibular root, 5.61mm and 5.09mm; from the distal furcal to the lingual face of the lingual root, 4.73mm and 4.65mm, for the first and second maxillary molars , respectively. Keywords: Molar; Molar - Radicular Faces; Molar - Average Distances; Radicular Furcal.

Antes de se fazer uma estimativa ou uma simulação geoestatística, os domínios geológicos devem ser modelados de forma que cada domínio utilize apenas dados que pertencem a ele. Na industria mineral a incerteza oriunda dos teores geralmente é levada em consideração, entretanto a incerteza gerada pelo modelo nem sempre é analisada. Sabendo que a maior fonte de incerteza está na transição de uma litologia para outra, essa dissertação visa avaliar a incerteza do modelo geológico através de simulações de funções distâncias assinaladas em zonas de maior incerteza, gerando vários modelos com diferentes proporções de cada litologias. Um estudo de caso em um banco de dados real com alta complexidade geológica é utilizado para avaliar o uso da metodologia. O método se mostrou eficaz para avaliar o impacto da diferença de volume que cada litologia pode alcançar, demonstrando a importância de medir a incerteza na construção de modelos geológicos. / Before making an estimation or a geostatistical simulation, geological domains must be modeled so that each domain uses only data that belongs to it. In the mineral industry the uncertainty derived from the grades is generally taken into account, however the uncertainty generated by the model is not always analyzed. Knowing that the greatest source of uncertainty is in the transition from one lithology to another, this dissertation aims to evaluate the uncertainty of the geological model through signed distances function simulation in uncertainty zones, generating several models with different proportions of each lithology. A case study in a real dataset with high geological complexity is used to evaluate the use of the methodology. The method proved effective in assessing the impact of the volume difference that each lithology can reach, demonstrating the importance of measuring uncertainty in the construction of geological models.

Nos encontramos em uma localização vantajosa para o estudo da formação e evolução de galáxias espirais. Situados no disco da Via-Láctea, somos capazes de fazer observações detalhadas sobre as estrelas individuais que a compõem. Com o avanço tecnológico das últimas décadas, foi possível coletar um grande conjunto de informações, (e.g. composição química, cinemática, astrometria e parâmetros atmosféricos), com alta resolução para uma vasta parte do volume Galáctico. Com o objetivo de compreender melhor a nossa Galáxia, desenvolvemos uma ferramenta, chamada StarHorse, que estima parâmetros como distâncias, idades, massas e avermelhamento utilizando informação disponível em levantamentos espectroscópicos, fotométricos e astrométricos. O código StarHorse estima os parâmetros através de um método Bayesiano, que constrói uma distribuição de probabilidade a partir do cálculo de verossimilhança entre observações e modelos de evolução teórica e a partir de priores Galácticos bem conhecidos. Os parâmetros que o StarHorse estima são cruciais para estudos de arqueologia Galáctica. Com eles é possível investigar a estrutura, o histórico de formação estelar, a função de massa inicial, o mapa tridimensional da nossa Galáxia e também adicionar vínculos a modelos quemodinâmicos da Via Láctea Neste trabalho, focaremos na descrição e validação do método, testando sua aplicabilidade em levantamentos recentes de espectroscópica, astrometria e fotometria. Também disponibilizamos catálogos com distâncias e extinção para comunidade astronômica. As nossas distâncias e extinções se tornaram referência dentro da colaboração APOGEE e foram liberadas junto com o seu Data Release 14. Ademais, catálogos foram liberados para os surveys RAVE, Gaia-ESO e GALAH. Neste trabalho, exploramos os resultados do StarHorse, especialmente os resultados APOGEE, em um contexto amplo de arqueologia Galáctica. / We are in an advantageous position to study the formation and evolution of disk galaxies. By being inside the Milky Way, we are able to make detailed observations about the individual stars that compose it. With the technological revolution of the latest years, it has been possible to collect a massive set of information, (e.g. chemical composition, kinematics, astrometry, and atmospheric parameters), with high resolution for a large portion of the Galactic volume. With the goal to understand better our Galaxy, we developed a tool, called StarHorse, that can estimate distances, ages, masses, and extinction from the available spectroscopic, astrometric, and photometric information. StarHorse makes these estimates through a Bayesian method, that builds a probability distribution over the models by calculating a likelihood function between observation and stellar evolution models, and by using common knowledge about our Galaxy as priors. The parameters that StarHorse estimates are crucial to Galactic archaeology studies. With them, we can investigate the structure, the star formation history, the initial mass function, the three-dimensional dust map of our Galaxy, and provide constraints to chemodynamical models of the Milky Way. In this work, we focus on the description and validation of the method, testing its applicability in recent spectroscopic and astrometric surveys. We also make available catalogs with distances and extinctions to the astronomy community. Our distances and extinctions became a reference inside the APOGEE-team and were released as part of the SDSS Data Release 14. Moreover, we made available catalogs also to other spectroscopic surveys such as Gaia-ESO, RAVE, and GALAH. In this work, we also explore these results, especially for APOGEE, in a broad Galactic archaeology context.

The ubiquity of Lyman alpha (Ly alpha) emission in a sample of four bright [O III]- strong star-forming galaxies with redshifts above seven has led to the suggestion that such luminous sources represent a distinct population compared with their fainter, more numerous counterparts. The presence of Lya emission within the reionization era could indicate that these sources created early ionized bubbles due to their unusually strong radiation, possibly because of the presence of active galactic nuclei. To test this hypothesis, we secured long integration spectra with XSHOOTER on the VLT for three z similar or equal to 7 sources selected to have similar luminosities and prominent excess fluxes in the IRAC 3.6 or 4.5 mu m band, usually attributed to strong [O III] emission. We secured additional spectroscopy for one of these galaxies at z = 7.15 using MOSFIRE at the Keck telescope. For the most well-studied source in our sample with the strongest IRAC excess, we detect significant nebular emission from He II and N V indicative of a non-thermal source. For the other two sources at z = 6.81 and z = 6.85, for which no previous optical/near-infrared spectroscopy was available, Ly alpha is seen in one and C III] emission in the other. Although based on a modest sample, our results further support the hypothesis that the phenomenon of intense [O III] emission is associated preferentially with sources lying in early ionized bubbles. However, even though one of our sources at z = 7.15 suggests the presence of non-thermal radiation, such ionized bubbles may not uniquely arise in this manner. We discuss the unique advantages of extending such challenging diagnostic studies with JWST.

The current paradigm shift in computing has placed mobile computation at the centre of focus. Users are now even more connected; demanding everything everywhere services. These services, such as social networking and media, benefit from the availability of context information seamlessly gathered and shared; providing customized and user-centric experiences. The distribution of context information no longer conforms to the paradigms of the existing Internet with regards to heterogeneity, connectivity and availability. This mandates new approaches towards its organization and provisioning in support of dependent applications and services. In response to these developments, the work summarized in this thesis addresses the fundamental problem of presenting context information in organized models as relevant subsets of global information. In approaching this problem, I introduced a distributed collection of context objects that can be arranged into simple relevant subsets called context schemata and presented to applications and services in supporting the realization of context based user experiences. Acknowledging the dynamic behaviour inherent of the real world interactions, I introduced an algorithm for measuring the proximities and similarities among these context objects, providing a metric through which to achieve organization. Additionally, I provided a means of ranking heterogeneous and distributed sensors in response to real time interaction between users and their digital ecosystem. Ranking provides an additional metric with which to achieve organization or identifying important and reputable information sources. The work I present here, additionally details my approach to realizing this complete behaviour an a distributed overlay, exploiting its properties for distribution, persistence and messaging. The overlay is also utilized for the provisioning of the supporting context information. Improvements in the ability to discover and attach new context information sources is fundamental to the ability to continually maintain expressions of context, derived from heterogeneous and disparate sources. By being able to create relevant subsets of organized data related to the requirements of applications and services in an end-point, infrastructures are realized for connecting and supporting the increasingly large numbers of users and their sources of information. Coupled with the distribution, these infrastructures realize improvements with regards to the effort required to achieve the same results. The culmination of the work presented in this thesis is an effort to enable seamless context-centric solutions on a future Internet of Things and thus constituting an adequate solution to the challenges raised above.

À l'heure actuelle, la voiture n'est plus un objet qui permet seulement de transporter une personne d'un endroit à un autre et il suffit de regarder les publicités automobiles pour en avoir la certitude. En effet, le champ lexical utilisé dans ces dernières se rapproche plus des sens, voire du rêve, que de la mobilité. La voiture n'est donc plus reléguée au simple rang de transporteur, mais à celui de véritable habitat dans lequel nous sommes amenés à découvrir de nouvelles sensations. Dans ce cadre, la réalité virtuelle est l'un des outils qui est utilisé dans l'industrie automobile afin de vérifier, en amont, l'ergonomie d'un prototype. En effet, en immergeant partiellement un usager dans cette autre réalité, il est possible d'avoir des retours pertinents quant à une maquette numérique, une interface, etc. Cela permet ainsi de tester différentes pièces avant même leur production ce qui est un gain notable en temps et en argent. Cependant, l'utilisation de cette technologie pose des questions quant au photo-réalisme de la reproduction virtuelle, et ce, tout particulièrement lorsque des pièces tels que les blocs optiques de la voiture sont analysés. Sur cette thématique, des études antérieures ont montré que le système reproduisait correctement les intensités lumineuses, mais pas la couleur des phares. Ainsi, dans le contexte du rendu de phare photoréaliste, nous avons tout d'abord proposé deux échelles colorimétriques afin d'analyser à quel point nous pouvions nous éloigner de la réalité sans que la différence de couleur ne gêne l'utilisateur final. À la suite de cela, nous avons proposé un système qui suit, au jour le jour, le vieillissement du simulateur dans le but de corriger ladite différence colorimétrique. Enfin, dans une étude exploratoire, nous avons souhaité regarder comment le comportement des conducteurs pouvait être influencé par la couleur des phares de voiture. Nous supposions que ce facteur pouvait avoir un impact sur la perception des distances et donc sur la distance intervéhiculaire à laquelle le conducteur se positionnait. / Nowadays, a car is not limited to the transportation of one or many people. Indeed, if we take a look at some automobile advertisement, it's more the idea of desir or even dream that is conveyed. Therefore, a car is no longer related to the simple rank of carrier but is a real new habitat in which we will discover new sensations. In this context, the car company that offers the best experience at the better price should be the one that dominates the market. For that purpose, virtual reality is one of the tools that is used by the automotive industry. Indeed, by partially immerging a user in this "other" reality, it is possible to get a relevent feedback for a digital model, Human-Machine Interface, etc. This allows to test different pieces before their production which is a significant gain in time and money. However, the use of this technology raises questions about the fidelity of the reproduction. Do the virtual reproduction of an object is close enough to the original ? If there is a difference, how could it impact the judgment of a person ? Those questions are even more important when it comes to the virtual evaluation of car headlight because they must respect international standard in term of color and light intensity. For these points, previous studies have shown that the system correctly reproduced the light intensities but not the headlights color. Thus, in the context of rendering photorealistic headlights, we first investigate on how a color difference can affect, discomfort the headlight specialist. To this end, we lead psychometric experiments and proposed two color difference scales (one for a naïve population and the other for an expert one). With this first result, we have proposed a system that follows, day by day, the aging simulator in order to correct the said color difference. Finally, in an exploratory study, we wanted to look at how the driver behavior could be influenced by the color of the car headlights. We assumed that this factor could affect depth perception and therefore the distance intercar in which the driver was positioning.

We characterize the absolute magnitudes and colors of RR Lyrae stars in the globular cluster M5 in the ugriz filter system of the Dark Energy Camera (DECam). We provide empirical period-luminosity (P-L) relationships in all five bands based on 47 RR Lyrae stars of the type ab and 14 stars of the type c. The P-L relationships were found to be better constrained for the fundamental-mode RR Lyrae stars in the riz passbands, with dispersions of 0.03, 0.02 and 0.02 mag, respectively. The dispersion of the color at minimum light was found to be small, supporting the use of this parameter as a means to obtain accurate interstellar extinctions along the line of sight up to the distance of the RR Lyrae star. We found a trend of color at minimum light with a pulsational period that, if taken into account, brings the dispersion in color at minimum light to <= 0.016 mag for the (r - i), (i - z), and (r - z) colors. These calibrations will be very useful for using RR Lyrae stars from DECam observations as both standard candles for distance determinations and color standards for reddening measurements.