O presente trabalho realizou simulações meteorológicas e de dispersão de poluentes com fontes de emissão da Região Metropolitana de São Paulo (RMSP) e de Cubatão, entre 23 a 26/08/2006. Neste período ocorreu um experimento de inverno realizado pelo IGC-USP, me- dindo e fazendo a análise elementar de Material Particulado Inalável (diâmetro aerodinâmico médio < 10m, M P 10 ) em Cubatão e em outros dois pontos de amostragem da RMSP (USP e Juquitiba). Empregou-se de modo articulado o modelo meteorológico de mesoescala BRAMS (Brazilian Regional Atmospheric Modelling System) e o modelo lagrangeano estocástico de dispersão de partículas SPRAY. Na área da RMSP considerou-se a dispersão das emissões de Monóxido de Carbono (CO) por veículos, enquanto em Cubatão tomou-se o MP proveniente das fábricas do Polo industrial de Cubatão. Os resultados da simulação de dispersão foram comparados com os valores medidos nas estações da CETESB (Companhia Ambiental do Estado de São Paulo), na estação meteorológica do IAG-USP e no experimento de inverno. O acoplamento BRAMS/SPRAY mostrou boa habilidade para simulação da meteorologia e das concentrações de poluentes. Foi possível discutir o transporte de poluentes entre a RMSP, Cubatão e arredores, durante este período, considerando inclusive um episódio particular ocorrido nos dias 25 e 26/08/2006. / This work performed meteorological and pollutants dispersion simulations using sources of the Metropolitan Area of São Paulo (MASP) and Cubatão city, between 23 and 26 August, 2006. During this period, a wintertime experiment was realized by IGC-USP (Institute of Geosciences - University of São Paulo) to measure and make the elemental analysis of the inhalable particulate matter from Cubatão, USP (In São Paulo, capital of São Paulo State, and MASPs major city) and Juquitiba (a MASPs border limits city). BRAMS/SPRAY (Brazilian Regional Atmospheric Modelling System, and the lagrangean stochastic dispersion Model SPRAY) were coupled to simulate meteorological variables and pollutant concentrations. The vehicular emissions of CO was the source used as input at MASP for SPRAY, and the imput used at Cubatão was the industrial emissions of PM at Cubatão industrial city. The results of the simulations were compared with meteorological data and the concentrations of pollutants measured in the CETESBs stations (CETESB - São Paulos Environmental Agency), at IAGs meteorological station (IAG - Institute for Astronomy, Geophisics and Atmospheric Sciences of University of São Paulo), and in the wintertime experiment stations. BRAMS/SPRAY coupled model showed good skill to simulate meteorological data and the concentrations of pollutants. They enabled the discussion of the pollutants transport between MASP, Cubatão and nearby areas, during studied period, specially a particular episode that took place in August 25 and 26, 2006

O presente trabalho realizou simulações meteorológicas e de dispersão de poluentes com fontes de emissão da Região Metropolitana de São Paulo (RMSP) e de Cubatão, entre 23 a 26/08/2006. Neste período ocorreu um experimento de inverno realizado pelo IGC-USP, me- dindo e fazendo a análise elementar de Material Particulado Inalável (diâmetro aerodinâmico médio < 10m, M P 10 ) em Cubatão e em outros dois pontos de amostragem da RMSP (USP e Juquitiba). Empregou-se de modo articulado o modelo meteorológico de mesoescala BRAMS (Brazilian Regional Atmospheric Modelling System) e o modelo lagrangeano estocástico de dispersão de partículas SPRAY. Na área da RMSP considerou-se a dispersão das emissões de Monóxido de Carbono (CO) por veículos, enquanto em Cubatão tomou-se o MP proveniente das fábricas do Polo industrial de Cubatão. Os resultados da simulação de dispersão foram comparados com os valores medidos nas estações da CETESB (Companhia Ambiental do Estado de São Paulo), na estação meteorológica do IAG-USP e no experimento de inverno. O acoplamento BRAMS/SPRAY mostrou boa habilidade para simulação da meteorologia e das concentrações de poluentes. Foi possível discutir o transporte de poluentes entre a RMSP, Cubatão e arredores, durante este período, considerando inclusive um episódio particular ocorrido nos dias 25 e 26/08/2006. / This work performed meteorological and pollutants dispersion simulations using sources of the Metropolitan Area of São Paulo (MASP) and Cubatão city, between 23 and 26 August, 2006. During this period, a wintertime experiment was realized by IGC-USP (Institute of Geosciences - University of São Paulo) to measure and make the elemental analysis of the inhalable particulate matter from Cubatão, USP (In São Paulo, capital of São Paulo State, and MASPs major city) and Juquitiba (a MASPs border limits city). BRAMS/SPRAY (Brazilian Regional Atmospheric Modelling System, and the lagrangean stochastic dispersion Model SPRAY) were coupled to simulate meteorological variables and pollutant concentrations. The vehicular emissions of CO was the source used as input at MASP for SPRAY, and the imput used at Cubatão was the industrial emissions of PM at Cubatão industrial city. The results of the simulations were compared with meteorological data and the concentrations of pollutants measured in the CETESBs stations (CETESB - São Paulos Environmental Agency), at IAGs meteorological station (IAG - Institute for Astronomy, Geophisics and Atmospheric Sciences of University of São Paulo), and in the wintertime experiment stations. BRAMS/SPRAY coupled model showed good skill to simulate meteorological data and the concentrations of pollutants. They enabled the discussion of the pollutants transport between MASP, Cubatão and nearby areas, during studied period, specially a particular episode that took place in August 25 and 26, 2006

The study of white dwarfs (WDs) provides insight into understanding WD formation rates, evolution, and space density. Individually, nearby WDs are excellent candidates for astrometric planetary searches because the astrometric signature is greater than for an identical, more distant WD system. As a population, a complete volume-limited sample is necessary to provide unbiased statistics; however, their intrinsic faintness has allowed some to escape detection. The aim of this dissertation is to identify nearby WDs, accurately characterize them, and target a subset of potentially interesting WDs for follow-up analyses. The most unambiguous method of identifying new WDs is by their proper motions. After evaluating all previous southern hemisphere proper motion catalogs and selecting viable candidates, we embarked on our own southern hemisphere proper motion survey, the SuperCOSMOS-RECONS (SCR) survey. A number of interesting objects were discovered during the survey, including the 24th nearest star system -- an M dwarf with a brown dwarf companion. After a series of spectroscopic observations, a total of 56 new WD systems was identified (18 from the SCR survey and 38 from other proper motion surveys). CCD photometry was obtained for most of the 56 new systems in an effort to model the physical parameters and obtain distance estimates via spectral energy distribution fitting. An independent distance estimate was also obtained by deriving a color-MV relation for several colors based on WDs with known distances. Any object whose distance estimate was within 25 pc was targeted for a trigonometric parallax via our parallax program, CTIOPI. Currently, there are 62 WD systems on CTIOPI. A subset of 53 systems has enough data for at least a preliminary parallax (24 are definitive). Of those 53 systems, nine are previously known WDs within 10 pc that we are monitoring for perturbations from unseen companions, and an additional 29 have distances within 25 pc. Previously, there were 109 known WDs with parallaxes placing them within 25 pc; therefore, our effort has already increased the nearby sample by 27%. In addition, at least two objects show hints of perturbations from unseen companions and need follow-up analyses.

Remarkably, the central regions of galaxies are very important in shaping and influencing galaxies as a whole. As such, galaxy cores can be used for classification, to determine which processes may be important in galaxy formation and evolution. Past studies, for example, have found a dichotomy in the inner slopes of early-type galaxy surface brightness profiles. Using deprojections of the galaxies from the ACS Virgo and Fornax Cluster Surveys (ACSVCS/FCS), we show that, in fact, this dichotomy does not exist. Instead, we demonstrate that the brightest early-type galaxies tend to have central light deficits, a trend which gradually transitions to central light excesses – also known as compact stellar nuclei – as we go to fainter galaxies. This effect is quantified, and can be used to determine what evolutionary factors are important as we move along the galaxy luminosity function. The number of stellar nuclei that we observe is, in fact, an unexpected result emerging from the ACSVCS/FCS. Being three times more common than previously thought, they are present in the vast majority of intermediate and low-luminosity galaxies. Conversely, it has been known for over a decade that there is likely a supermassive black hole weighing millions to billions of solar masses at the center of virtually every galaxy of sufficient size. These black holes are known to follow scaling relations with their host galaxies. Using the ACSVCS, along with new kinematical data from long-slit spectroscopy, we measure the dynamical masses of 83 galaxies, and show that supermassive black holes and nuclei appear to fall along the same scaling relation with host mass. Both represent approximately 0.2% of their host’s mass, implying an important link between the two types of central massive objects. Finally, we extract elliptical isophotes and fit parameterized models to the surface brightness profiles of new Hubble Space Telescope imaging of the ACSVCS galaxies, observed in infrared and ultraviolet bandpasses. Taken together, the two surveys represent an unprecedented collection of isophotal and structural parameters of early-type galaxies, and will allow us to learn a great deal about the stellar populations and formation histories of galaxy cores. / Graduate

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Denna uppsats kommer att undersö̈ka hur designen och anvä̈ndandet av mobildejtingtjä̈nsten Tinder har påverkat beteenden och normer gä̈llande nä̈tdejting bland unga vuxna i Sverige. Ett huvudsyfte är att undersöka hur olika interaktionsmekanismer i Tinder påverkar synen på nätdejting och potentiella partners. Vidare undersöker vi faktorer som skiljer Tinder från övriga nätdejtingtjänster, samt vilka normer som synliggörs genom användandet av Tinder. Genom en nätbaserad enkätundersökning kunde vi samla användarupplevelser och åsikter från användare av Tinder. Baserat på materialet från enkätundersökningen utförde vi tre fokusgrupper vars syfte var att fördjupa perspektiv unga vuxna hade gällande nätdejting och Tinder. Resultatet presenteras genom att analysera data från informanterna kombinerat med teorier om användarupplevelse (User Experience), affordanser, designkvalitéer, självrepresentation, spelifiering och marknadsmetaforer. Vi kunde se åtskilliga mekanismer associerade med spelifiering i Tinder gällande design och användarbeteende. Generellt verkar också Tinderanvändare reproducera rådande könsnormer i en annars neutral och minimalistisk design. Vidare fanns marknadsmetaforer gällande nätdejting i Tinder. Tinder tycks även ha tilltalat en ny målgrupp inom nätdejting, således ansedd avslappnad och jämbördig annan social media. Kopplingen till Facebook bidrar också till en ökad tillit för självrepresantationen bland Tinderanvändare. Slutligen ser vi att den svepcentrerade “ja-eller-nej-funktionaliteten” i Tinder verkar ha skapat en standard som kommer att påverka framtida dejtingtjänster och användarupplevelser. / This report aims to examine how the design and usage of the mobile dating application Tinder has affected behaviors and norms regarding online dating amongst young adults in Sweden. One main purpose is to examine how different interaction mechanisms in Tinder affects the view of online dating and potential partners. Additionally factors that differentiate Tinder from other online dating services will be examined. Furthermore social norms that are made visible through the usage of Tinder will be addressed. By creating an online survey it was possible to retrieve user experiences of Tinder usage and opinions about Tinder and online dating. Based on material from the survey three focus group interviews were conducted, which gathered different perspectives young adults had regarding online dating and Tinder. The conclusion will be presented by analyzing the data from the informants combined with theories such as User Experience, affordances, design qualities, self representation, gamification and market metaphors. Several mechanism associated with gamification were found in Tinder regarding design and user behavior. The Tinder users in general also seem to reproduce current gender norms in an otherwise neutral and minimalistic design. Furthermore market metaphors were found regarding online dating in Tinder. Additionally Tinder seems to target a new group of users in online dating, accordingly considered as ”laid-back” and equal to other social media. The connection to Facebook also contributes to an increased trust towards the self representation of Tinder users. Finally the swipe centered “yes-or-no-functionality” of Tinder seems to create a standard that will affect future dating services and User Experience.

Durant ma thèse j'ai exploré les liens morphologiques et physiques entre les phases poussière et stellaire des galaxies spirales proches.J'ai travaillé sur 46 galaxies de l'échantillon KINGFISH à l'aide des données IRAC/MIPS/PACS/SPIRE (de 3.6 à 500 microns).Un biais usuel dans la mesure de l'orientation des galaxies spirales est dû à l'utilisation d'une seule isophote. Pour supprimer ce biais j'ai extrait de nombreuses isophotes des cartes galactiques, j'ai créé un critère pour quantifier la similitude des forme des isophotes. J'ai extrait des zones dans chaque carte où les formes des isophotes se ressemblent. Dans de nombreuses cartes les formes des isophotes sont cohérentes avec l'idée d'un disque sous-jacent et ce malgré des variations de formes des isophotes qui peuvent ponctuellement être notable. De là j'ai obtenu pour chaque galaxie une orientation du disque par carte. En comparant les formes obtenues pour chaque galaxie dans différentes cartes j'ai selectionné 20 galaxies sur 46 dans lesquelles l'accord en terme d'orientation du disque entre les différentes cartes était acceptable. Dans ces galaxies les zones associées au disque galactique ont une taille typique allant jusqu'à 1/3 du rayon galactique visible (R25) que ce soit pour la phase poussière aussi bien que pour la phase stellaire. Ces 20 galaxies sont moins lumineuses dans le visible, moins lumineuses dans l'IR, moins barrées, et de type plus tardifs que la moyenne. Pour ces 20 galaxies, les orientations obtenues par ma méthode sont plus proches des orientations obtenues à partir d'études cinématiques H-alpha que de celles obtenues par une autre étude photometrique utilisant une seule isophote (RC3).A partir des orientations obtenues par ma méthode et par l'étude cinématique H-alpha j'ai moyenné azimuthalement les brillances de surface pour obtenir des profiles radiaux de distribution spectrales d'énergie. Après avoir ajusté dessus un modèle d'émission de la poussière cosmique (Galliano 2011), j'ai trouvé que la densité surfacique d'énergie interceptée par la poussière était proportionnelle au produit de la masse totale de poussière sur la ligne de visée par le champ de radiation interstellaire moyen ressenti par la poussière sur la ligne de visée. Cette densité d'énergie interceptée par la poussière est mieux corrélé à la luminosité bolométrique stellaire totale que la densité surfacique en masse de poussière ou le champ de radiation ressenti par la poussière. Il est donc probable que les étoiles agées à tout le moins soit une importante source de chauffage pour la poussière cosmique. L'énergie interceptée par la poussière est aussi très bien corrélée avec l'énergie totale émise dans l'infrarouge. J'ai également trouvé que la poussière semble intercepter une plus large quantité d'énergie provenant des étoiles dans les galaxies plus actives à former des étoiles.Les profiles radiaux en masse de poussière sont moins bien décrits que les profils en masse stellaire par des profiles de Sersic. Par ailleurs pour les ajustements acceptables par des fonctions de Sersic, les distributions statistiques des indices de Sersic et des rayons de demi masse totale ont des largeurs statistiques plus grandes pour la poussière que pour les étoiles.J'ai également trouvé que le rapport densité surfacique maximum de poussière sur densité surfacique maximum d'étoile est un facteur important à considérer pour expliquer la variation avec le type morphologique du rapport densité surfacique d'énergie interceptée par la poussière sur densité surfacique d'énergie émise par les étoiles. Cette variation pourrait être liée à une variation entre les galaxies de la force de la structure spirale. / In my PHD work I explored the links between the physical properties of interstellar dust and other components of nearby spiral galaxies especially their stellar content. I worked on 46 disk galaxies from KINGFISH with IRAC/MIPS/PACS/SPIRE maps (3.6 - 500 microns). A bias is usually introduced in estimating disk orientations by using only a single surface brightness isophote. Thus I devised different surface brightness levels separated by constant steps in surface brightness and extracted isophotes at these levels in all FIR maps as well as in all IRAC 4.5 microns maps. To further assess the coherence of the shapes of isophotes across galactic disks, I built a quantitative indicator of the difference in shape between two ellipses with same center and same semi-major axis.I defined an acceptable level of difference between isophote shapes, by comparing disk orientations found in litterature. Using this level, I found regions inside the galactic disks where the isophotal shapes are similar. From these, I extracted one disk orientation per wavelength band. I found in the vast majority of the disk galaxy maps, be it dominated by stellar or dust emission, that a large fraction of the isophotes I extracted are coherent with the idea of an underlying disk. Comparing, for each galaxy, disk orientations extracted at all wavelengths, I found evidence in 20 galaxies out of 46, that on radial ranges as large as 1/3 of the visible disk (as measured by R25), the shapes of isophotes are morphologically similar. Thus for these 20 galaxies I devised consistent disk orientations both for the stellar and dust content. These 20 galaxies are less luminous, less emitting in the IR w.r.t. the optical, less barred, and characterized by later stage types than average. I also found that the disk orientations devised by my photometric method yield results more similar to H-alpha kinematic orientations than other photometric studies based on a single isophote level.Using the orientations I found and H-alpha dynamics disk orientations, I averaged azimuthally surface brightnesses to produce radial spectral energy distributions (SED) profiles. Once fitted with a cosmic dust emission model, they resulted in radial profiles of dust and stellar content properties. I found the dust intercepted power to be proportionnal to the product of the total dust mass and the average ISRF shining on dust. This former quantity is better correlated with the bolometric stellar luminosity than any of the dust mass or the dust heating ISRF separately. Thus the old stellar populations may be an important heating source for dust. The power intercepted by dust is also very well correlated with the total infrared power. The dust intercepts a larger quantity of power coming from stars in more actively star forming galaxies.Dust exhibit radial mass surface density profiles less well described by Sersic functions than stellar ones. When both profiles are well fitted by Sersic functions, stellar density profiles have smaller half mass radii than the isophotal optical radius (R25) separately in later type galaxies, but also in more quiescent galaxies. Sersic index and half mass radius distributions have larger widths for dust than for stellar surface density profiles.I also found that the ratio of dust over stellar surface density is an important factor to explain the variations with galactic morphological type of the ratio of dust intercepted power over the power emitted by old stellar populations. This later link could be intertwined with spiral structure strength in stage types later than 2.

Vers la fin des années 1990, l'utilisation des supernovae de type Ia (SNe Ia) comme indicateurs de distance a permis de mettre en évidence l'expansion accélérée de l'univers. Depuis lors, des campagnes d'observations de grandes envergures ont permis d'augmenter de façon significative le nombre de SNe Ia observées, mais les incertitudes systématiques liées à la qualité des échantillons de SNe Ia proches restent un facteur limitant sur la précision des mesures actuelles. C'est dans le but de réduire ces incertitudes que le projet the Nearby Supernova Factory (SNfactory), à l'aide d'un instrument spectro-photométrique dédié à l'observation des SNe Ia (the Supernova Integral Field Spectrograph), a collecté depuis 2004 plus de 3000 spectres de près de 200 SNe Ia proches. Une des limitations actuelles de leur utilisation, outre les aspects liés aux problèmes d'inter-calibration entre les différentes expériences, est celle du mélange des différentes composantes de leurs variabilités lors de la standardisation empirique de leur module de distance. Une meilleure séparation de ces composantes, ainsi que la découverte de nouveaux indicateurs de distance, font partie des améliorations que peut apporter un échantillon spectral de SNe Ia proches tel que celui de la collaboration SNfactory. Cette thèse de doctorat, effectuée à l'Institut de Physique Nucléaire de Lyon et au Lawrence Berkeley National Laboratory, s'inscrit directement dans cette problématique, en se concentrant sur la mesure d'indicateurs spectraux sur l'échantillon spectral de la collaboration Snfactory. Le plan de cette thèse est le suivant : La première partie présente le contexte scientifique ainsi que l'échantillon de SNe Ia de la collaboration SNfactory utilisé dans les analyses. La deuxième partie se concentre sur la méthode de mesure d'indicateurs spectraux appliquée à l'échantillon spectrale présenté, ainsi que sur une étude de leur sensibilité à l'extinction par le milieu interstellaire. La troisième partie est une étude des corrélations des indicateurs spectraux et de leur utilisation pour la standardisation des Sne Ia. Dans la dernière partie, une utilisation de ces indicateurs spectraux pour la détermination d'une loi d'extinction moyenne est présentée

The main objective of this work is to demonstrate some new computational methods for estimation, optimization and modeling of dynamical systems that use automatic differentiation. Particular focus will be upon dynamical systems arising in Aerospace Engineering. Automatic differentiation is a recursive computational algorithm, which enables computation of analytically rigorous partial derivatives of any user-specified function. All associated computations occur, in the background without user intervention, as the name implies. The computational methods of this dissertation are enabled by a new automatic differentiation tool, OCEA (Object oriented Coordinate Embedding Method). OCEA has been recently developed and makes possible efficient computation and evaluation of partial derivatives with minimal user coding. The key results in this dissertation details the use of OCEA through a number of computational studies in estimation and dynamical modeling. Several prototype problems are studied in order to evaluate judicious ways to use OCEA. Additionally, new solution methods are introduced in order to ascertain the extended capability of this new computational tool. Computational tradeoffs are studied in detail by looking at a number of different applications in the areas of estimation, dynamical system modeling, and validation of solution accuracy for complex dynamical systems. The results of these computational studies provide new insights and indicate the future potential of OCEA in its further development.

因應各國中等教育普及化的潮流，教育部擬以高中職社區化為十二年國民教育奠基，將台灣劃分為四十五個適性學習社區，並以均衡高中職城鄉差距、提高國中畢業生就近入學之機會為目的。本研究以雲林縣三個適性學習社區為例，檢視各社區高中、職的就學機會是否均衡，並觀察學生通學活動的情形，是否符合社區內就近入學的期待，藉此對適性學習社區的地理範圍規劃，與其劃分原則提出修正的建議。 本研究發現，雲林縣整體就學機會率較他縣市低落，高中、職學校集中於特定鄉鎮，空間分布不甚平均，不利於學生就近就學，而產生部分學生向外縣市通學的情形。外縣市通學的人口中，以高職生為多，多往嘉義縣、市為就學地；顯示雲林縣境內就學機會的供給不敷需求，高職就學機會不均的現象比高中嚴重許多。而就雲林縣三個適性學習社區觀察，雲二區、雲三區內高中、職學生區內就讀的比例皆為六成以上，是為社區內就近就學的良好基礎；雲一區學生外流的情形嚴重，特別是高職學生，往嘉義縣、市通學的趨勢集中，顯示雲一區內就學機會供不應求的情形嚴重，值得注目。對教育當局的建議有二：（1）高中、職通學活動範圍不同，不宜以同一地理界線劃分；（2）雲一區學生向外通學現象嚴重，宜增設高中職校改善之。 / With the popularization of post-secondary education, the Ministry of Education adopts the plan of “Community Senior High School and Vocational School” to connect with the compulsory education. In this plan, Taiwan has been divided into 45 “Adaptive Learning Communities” and the purpose is to diminish the urban-rural difference and increase the opportunity of nearby school enrollment. This study observes the geographical distribution of students in the three communities in Yunlin to examine the condition of nearby school enrollment. The conclusions are as follows: Senior high schools and vocational schools distributes disproportionately in Yunlin. In other words, almost all schools concentrate in the few towns. It is common for students to commute between residential and school districts, especially for the students enrolled in vocational school. Many non-resident students commute to Chiayi, and the flow of the commuter shows that the supply is unable to meet the demand of school enrollment totally in Yun-1st community. Besides, there are still many students enrolled in nearby schools in Yun-2nd Community and Yun-3rd Community. Based on the results and discoveries of this study, the following suggestions are proposed: (1)The range of the community should be re-divided for senior high schools and vocational schools respectively. (2)It is necessary to establish more schools in Yun-1 community to increase the supply of the opportunity of the nearby school enrollment.