Dissertation (Ph.D.)--Worcester Polytechnic Institute. / Keywords: Ranging Error, Ranging, Positioning, Indoor Geolocation, Distance Measurement Error. Includes bibliographical references (p.168-171).

Orientador: José Cláudio Martins Segalla / Banca: Paulo Martins Ferreira / Banca: João Neudenir Arioli Filho / Resumo: O objetivo deste trabalho foi o de observar a previsibilidade da presença ou ausência da papila gengival interproximal, em relação à distância do ponto de contato interproximal dentário até a crista óssea, e da distância das faces interproximais de dentes adjacentes. Para isso, foram selecionados pacientes divididos em 3 grupos com faixas etárias distintas, sendo que o grupo 1 ia dos 20 aos 30 anos, o grupo 2 ia dos 31 aos 40 anos, e o grupo 3 ia dos 41 aos 50 anos. Os pacientes eram, então, submetidos a um exame clínico que tinha por objetivo a constatação da presença ou ausência da papila gengival nas áreas examinadas. Essas áreas situavam-se entre os incisivos centrais superiores, e entre o canino e o primeiro pré-molar superior. Assim, ambas as regiões, anterior e superior, foram estudadas. Para ser considerada presente, a papila gengival deveria ocupar todo o espaço interproximal, não deixando nenhum espaço visível da área interproximal. Depois do exame clínico, os pacientes eram submetidos a tomadas radiográficas das regiões anterior e posterior, sendo que uma tela milimetrada (grid) com fios de bário era adaptada junto ao filme para que a imagem radiográfica obtida pudesse ser mensurada mais satisfatoriamente. Depois de obtidas as radiografias, as medidas eram realizadas e relacionadas com a presença ou ausência da papila gengival. Com a análise dos dados obtidos, permitiu-se concluir que a região anterior apresenta uma tendência maior à ausência da papila gengival interproximal. Além disso, verificou-se que a idade dos pacientes não interferiu na presença ou ausência da papila gengival. Por fim, observou-se que a distância das raízes adjacentes não interferiu nos resultados obtidos, o que não aconteceu com a distância do ponto de contato interproximal até a crista óssea, já que esse fator teve grande influência sobre a presença ou ausência da papila gengival interproximal. / Abstract: The purpose of this work was to observe the predictability of the presence or absence of the gingival papilla, in relation to the distance from dental contact point to the crest of the bone, and in relation to the distance between the interproximal faces of adjacent teeth. For that they were selected 45 patients, divided into 3 well defined age groups: Group 1: 20 to 30 years old; Group 2: 31 to 40 years old and Group 3: 41 to 50 years old. The patients were submitted to a clinical examination to verify the presence or absence of the gingival papilla on the examined areas. Those areas were between the maxillary cuspids and maxillary bicuspids, so, they were studied both anterior and posterior regions. If the gingival papilla occupied all interproximal site and didn't last any visible area of that, it was deemed to be present. After the clinical examination, the patients were submitted to radiographic examinations of the anterior and posterior regions, with a radiographic grid with barium wires, copled to the film, permitting correct measurements. The measurements were made on the obtained radiographs and related to the presence or absence of the gingival papilla. From the obtained results, it was concluded that the anterior region presents a high tendency to show the absence of the interproximal gingival papilla. Moreover, the age factor had no influence on the presence or absence of the gingival papilla. Finally, it was observed that the distance of adjacent roots didn't influenced on the obtained results, what didn't occur with the distance between the contact point and the crest of the bone, since this factor showed high influence on the presence or absence of the interproximal gingival papilla. / Mestre

Esse trabalho objetiva motivar os professores que ensinam trigonometria, no ensino médio, propondo formas e propostas de ensino que facilitem o desenvolvimento da capacidade dos alunos em dominar as funções trigonométricas de tal forma, que eles possam fazer uso desse conhecimento para a resolução de problemas da vida cotidiana. O ensino de trigonometria, como vem sendo ministrado, não é, geralmente, apreciado por grande parte dos alunos os quais, muitas vezes, sofrem com a exigência de memorização de uma quantidade de informações sem nenhuma aplicabilidade prática em seu dia a dia. A proposta, aqui apresentada, fundamenta-se na libertação da metodologia de fixação de definições e fórmulas, sem relação entre fato e conceito bem como das maneiras de resolução de exercícios mecânicos, evitando a obrigatoriedade de memorização forçada de algoritmos. Este trabalho foi realizado em duas etapas complementares: uma teórica e outra experimental. Na parte teórica, trouxemos as definições das funções trigonométricas; as definições das medidas dos ângulos, tanto em graus como em radianos, com o objetivo de mostrar e explicar as razões da existência das duas unidades de medidas de ângulos e as diferenças e formas mais vantajosas que cada uma delas apresenta na representação de uma função trigonométrica. Na parte experimental, foi feita uma aplicação prática dos conceitos estudados, como o cálculo de distâncias inacessíveis, utilizando o método Paralaxe. Nessa etapa, fizemos uma simulação de situações reais presentes no dia a dia de todos a partir da semelhança de triângulos. Em seguida, mostramos situações em que se pode utilizar a trigonometria de forma prática e contextualizada. Para tanto, contamos com a participação de alguns alunos da ONG Pedra Bruta - Lapidando Talentos. As atividades realizadas são de simples aplicação e mostraram um resultado significativo, pois otimizaram o processo ensino aprendizagem e extrapolaram os limites da sala de aula já que a metodologia usada para a construção do conhecimento não se restringiu apenas à lousa, ao giz, caderno e ao espaço da sala de aula. A abordagem dada trouxe uma prática capaz de ressignificar o conteúdo aos discentes, deixando mais envolvente o ensino de trigonometria, pois, embora haja muita literatura sobre o assunto, não há um detalhamento de descrições e interpretações de práticas de ensino voltadas à contextualização. Portanto, foi realizado um passo a passo de como desenvolver situações de aprendizagem, fazendo uso de recursos simples e de baixo custo. / This paper aims at motivating teachers who teach Trigonometry in high school by suggesting ways and teaching proposals that can make it easier to lead the students into developing their abilities so as to master trigonometric functions in order to make use of such knowledge for solving everyday life problems. The teaching of Trigonometry as it has been done is not generally enjoyable for the most part of the students who resent the demands of memorization of a volume of information which can hardly find any practical applicability day to day. The suggestion presented in this thesis is based on freeing one from such a methodology that requires memorizing definitions and formulas without correlating fact and concept and from employing mechanical solving of exercises and by doing so avoid mandatory memorizing of algorithms. This work has been done in two complementary phases: a theoretical and an experimental one. Within the theoretical part we have brought in the definitions of trigonometric functions; the definitions of measurement of angles both in degrees and radians in order to demonstrate and explain the reason for the existence of two different measurement units for angles as well as the differences and the more advantageous forms each of them presents for the representation of a trigonometric function. In the experimental part a practical application of the concepts studied was done such as the calculation of inaccessible distances using the Parallax method. In this phase we have done a simulation of common real life situations using the similarity of triangles. After we showed situations in which one can make practical and contextualized use of Trigonometry. For such we invited some students from the NGO Pedra Dura - LapidandoTalentos. The activities done are easily applicable and showed significant results when they optimized the teaching and learning process and extrapolated the classroom limits once the methodology used for the building of knowledge was not restricted to a board, a piece of chalk, a notebook and the classroom.The approach given has brought forward a practice capable of bringing new meaning to contents for the students by making the teaching of Trigonometry more involving because, although there is extensive literature about this subject there is not a detailed description or interpretation of teaching practices aimed at such contextualization. A step by step was thus built on how to develop situated learning sequences making use of simple and low cost resources.

We present spectra of five ultra-diffuse galaxies (UDGs) in the vicinity of the Coma cluster obtained with the Multi-object Double Spectrograph on the Large Binocular Telescope. We confirm four of these as members of the cluster, quintupling the number of spectroscopically confirmed systems. Like the previously confirmed large (projected half-light radius > 4.6 kpc) UDG, DF44, the systems we targeted all have projected half-light radii > 2.9 kpc. As such, we spectroscopically confirm a population of physically large UDGs in the Coma cluster. The remaining UDG is located in the field, about 45 Mpc behind the cluster. We observe Balmer and Ca II H and K absorption lines in all of our UDG spectra. By comparing the stacked UDG spectrum against stellar population synthesis models, we conclude that, on average, these UDGs are composed of metal-poor stars ([Fe/H] less than or similar to -1.5). We also discover the first UDG with [O II] and [O III] emission lines within a clustered environment, demonstrating that not all cluster UDGs are devoid of gas and sources of ionizing radiation.

We present the results of SPT-GMOS, a spectroscopic survey with the Gemini Multi-Object Spectrograph (GMOS) on Gemini South. The targets of SPT-GMOS are galaxy clusters identified in the SPT-SZ survey, a millimeter-wave survey of 2500 deg(2) of the southern sky using the South Pole Telescope (SPT). Multi-object spectroscopic observations of 62 SPT-selected galaxy clusters were performed between 2011 January and 2015 December, yielding spectra with radial velocity measurements for 2595 sources. We identify 2243 of these sources as galaxies, and 352 as stars. Of the galaxies, we identify 1579 as members of SPT-SZ galaxy clusters. The primary goal of these observations was to obtain spectra of cluster member galaxies to estimate cluster redshifts and velocity dispersions. We describe the full spectroscopic data set and resulting data products, including galaxy redshifts, cluster redshifts, and velocity dispersions, and measurements of several well-known spectral indices for each galaxy: the equivalent width, W, of [O II] lambda lambda 3727, 3729 and H-delta, and the 4000 angstrom break strength, D4000. We use the spectral indices to classify galaxies by spectral type (i.e., passive, post-starburst, star-forming), and we match the spectra against photometric catalogs to characterize spectroscopically observed cluster members as a function of brightness (relative to m*). Finally, we report several new measurements of redshifts for ten bright, strongly lensed background galaxies in the cores of eight galaxy clusters. Combining the SPT-GMOS data set with previous spectroscopic follow-up of SPT-SZ galaxy clusters results in spectroscopic measurements for >100 clusters, or similar to 20% of the full SPT-SZ sample.

The determination of galaxy redshifts in the James Webb Space Telescope's (JWST) blank-field surveys will mostly rely on photometric estimates, based on the data provided by JWST's Near-Infrared Camera (NIRCam) at 0.6-5.0 mu m and Mid Infrared Instrument (MIRI) at lambda > 5.0 mm. In this work we analyze the impact of choosing different combinations of NIRCam and MIRI broadband filters (F070W to F770W), as well as having ancillary data at lambda < 0.6 mu m, on the derived photometric redshifts (z(phot)) of a total of 5921 real and simulated galaxies, with known input redshifts z = 0-10. We found that observations at lambda < 0.6 mm are necessary to control the contamination of high-z samples by low-z interlopers. Adding MIRI (F560W and F770W) photometry to the NIRCam data mitigates the absence of ancillary observations at l < 0.6 mm and improves the redshift estimation. At z = 7-10, accurate zphot can be obtained with the NIRCam broadbands alone when S/N >= 10, but the z(phot) quality significantly degrades atb S/N <= 5. Adding MIRI photometry with 1 mag brighter depth than the NIRCam depth allows for a redshift recovery of 83%-99%, depending on spectral energy distribution type, and its effect is particularly noteworthy for galaxies with nebular emission. The vast majority of NIRCam galaxies with [F150W] = 29. AB mag at z =7-10 will be detected with MIRI at [F560W, F770W] < 28 mag if these sources are at least mildly evolved or have spectra with emission lines boosting the mid-infrared fluxes.

Thèse doctorat : Physique Photonique : Strasbourg 1 : 2006. / Titre provenant de l'écran-titre. Notes bibliogr.

The idea of `probabilistic distances' (also called divergences), which in some sense assess how `close' two probability distributions are from one another, has been widely employed in probability, statistics, information theory, and related fields. Of particular importance due to their generality and applicability are the Renyi divergence measures. While the closely related concept of Renyi entropy of a probability distribution has been studied extensively, and closed-form expressions for the most common univariate and multivariate continuous distributions have been obtained and compiled, the literature currently lacks the corresponding compilation for continuous Renyi divergences. The present thesis addresses this issue for analytically tractable cases. Closed-form expressions for Kullback-Leibler divergences are also derived and compiled, as they can be seen as an extension by continuity of the Renyi divergences. Additionally, we establish a connection between Renyi divergence and the variance of the log-likelihood ratio of two distributions, which extends the work of Song (2001) on the relation between Renyi entropy and the log-likelihood function, and which becomes practically useful in light of the Renyi divergence expressions we have derived. Lastly, we consider the Renyi divergence rate between two zero-mean stationary Gaussian processes. / Thesis (Master, Mathematics & Statistics) -- Queen's University, 2011-08-30 13:37:41.792

Submitted by Willian Eliseu da Silva null (willianeliseu@hotmail.com) on 2016-10-13T13:56:54Z No. of bitstreams: 1 simulacao_computacional_proteinas.pdf: 3524008 bytes, checksum: 981d0a947d1fa19cb9db73b4f48d993a (MD5) / Rejected by Juliano Benedito Ferreira (julianoferreira@reitoria.unesp.br), reason: Solicitamos que realize uma nova submissão seguindo a orientação abaixo: O arquivo submetido não contém o certificado de aprovação. Corrija esta informação e realize uma nova submissão com o arquivo correto. Agradecemos a compreensão. on 2016-10-19T17:12:33Z (GMT) / Submitted by Willian Eliseu da Silva null (willianeliseu@hotmail.com) on 2016-10-21T03:19:08Z No. of bitstreams: 1 simulacao_computacional_proteinas.pdf: 3716184 bytes, checksum: a3d8fc2e2a43d95d3033287e0fc1ad93 (MD5) / Approved for entry into archive by Juliano Benedito Ferreira (julianoferreira@reitoria.unesp.br) on 2016-10-21T20:00:33Z (GMT) No. of bitstreams: 1 silva_we_me_bauru.pdf: 3716184 bytes, checksum: a3d8fc2e2a43d95d3033287e0fc1ad93 (MD5) / Made available in DSpace on 2016-10-21T20:00:33Z (GMT). No. of bitstreams: 1 silva_we_me_bauru.pdf: 3716184 bytes, checksum: a3d8fc2e2a43d95d3033287e0fc1ad93 (MD5) Previous issue date: 2016-08-31 / Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq) / Proteínas são polímeros heterogêneos lineares essenciais a todos os organismos vivos. As proteínas apresentam diversas funções nos organismos, tais como: estruturação, catálise, síntese, transferências, entre tantas outras. Neste trabalho foram estudadas as proteínas que apresentam em suas estruturas nós do tipo 3-1. Foram calculadas as distâncias entre os carbonos alfa dessas proteínas e com estes valores foram traçados os gráficos de distâncias que permitem uma visualização geral da estrutura da proteína. Foram realizadas alterações no nó 31 padrão para que este se ajustasse à estrutura real da proteína na região do nó. A partir do gráfico de distâncias foi possível determinar a estrutura secundária presente na proteína, sendo que a alfa hélice apresenta oscilações de aproximadamente 5,5 angstrons. Com os gráficos de distâncias das proteínas e dos nós matemáticos foi possível comprovar a presença do nó e sua proximidade com a equação proposta. / Proteins are linear heterogeneous polymer essential to all living organisms. The proteins have different functions in organisms, such as: structuring, catalysis, synthesis, transfers, among many others. In this work were studied the proteins that presenting in their structure, type 31 knots. The distances between the alpha carbons of those proteins were calculated and with these values were plotted distances graphs that allow general visualization of the protein structure. Changes were made in the standard knot 31 so that it would fit the actual structure of the protein in the node region. From the distances graph was possible to determine the secondary structure of the protein, wherein the alpha helix presents oscillations proximately 5.5 angstroms. With distances graph from proteins and from mathematical knots was possible to prove the presence of the node and its proximity to the proposed equation. / CNPq: 131771/2014-0

We present a new algorithm to estimate quasar photometric redshifts (photo-zs), by considering the asymmetries in the relative flux distributions of quasars. The relative flux models are built with multivariate Skew-t distributions in the multidimensional space of relative fluxes as a function of redshift and magnitude. For 151,392 quasars in the SDSS, we achieve a photo-z accuracy, defined as the fraction of quasars with the difference between the photo-z z(p) and the spectroscopic redshift z(s), vertical bar Delta z vertical bar=vertical bar z(s)-z(p)vertical bar/(1 + z(s)) within 0.1, of 74%. Combining the WISE W1 and W2 infrared data with the SDSS data, the photo-z accuracy is enhanced to 87%. Using the Pan-STARRS1 or DECaLS photometry with WISE W1 and W2 data, the photo-z accuracies are 79% and 72%, respectively. The prior probabilities as a function of magnitude for quasars, stars, and galaxies are calculated, respectively, based on (1) the quasar luminosity function, (2) the Milky Way synthetic simulation with the Besancon model, and (3) the Bayesian Galaxy Photometric Redshift estimation. The relative fluxes of stars are obtained with the Padova isochrones, and the relative fluxes of galaxies are modeled through galaxy templates. We test our classification method to select quasars using the DECaLS g, r, z, and WISE W1 and W2 photometry. The quasar selection completeness is higher than 70% for a wide redshift range 0.5 < z < 4.5, and a wide magnitude range 18 < r < 21.5 mag. Our photo-z regression and classification method has the potential to extend to future surveys. The photo-z code will be publicly available.