Pattern speed is an important parameter of the density wave theory for spiral galaxies. In this thesis we have determined the pattern speed for warped galaxies (flat galaxies being a special case of this generalization) using the observable data of the surface brightness and line-of-sight velocity distribution of the galaxy. We have also extracted the transverse velocity field for the warped galaxy using the same data. Here we have simulated the data and applied our method to it and we found that our method works well in warped galaxy. We assume a parameterized model of the warp and by the method of minimizing χ2 error we can determine the parameters of the model also and thus we can construct the warp equation. We have also discussed the implications and the limitations of this method.

Parmi les douzaines d’expériences qui visent à découvrir la matière sombre, l’expérience de détection directe PICO utilise des détecteurs à liquide surchauffé comme moyen pour s’y prendre. La chambre à bulle PICO-40L remplie de C3F8, présentement située dans le laboratoire sous-terrain SNOLAB, est en cours de test en vue d’une recherche aveugle de WIMP (Weakly Interacting Massive Particle) d’une durée de 1 an. Pour assurer la stabilité du détecteur pendant les périodes de préparation et pendant l’acquisition de données, un logiciel de surveillance a été écrit. Un moyen fiable de surveiller les paramètres importants du détecteur et d’envoyer des alarmes en cas d’urgence joue un rôle important à non seulement au succès de PICO-40L, mais aussi au développement du futur détecteur PICO-500. Située à l’Université de Montréal, la chambre à bulle PICO-0.1 a été conçue afin de calibrer les nombreux événements de fond qui se présentent dans ce type de détecteur. De plus, cette chambre à bulle a été utilisée comme première tentative au monde de mesurer la diffusion Thomson sur un noyau d’atome en exposant le détecteur rempli de C3F8 à une source de gamma produite par la réaction 19F proton à alpha et gamma 16O à l’aide d’un faisceau de protons crée par l’accélérateur de particules de l’Université de Montréal. Ce type d’interaction s’avérera à un événement de fond important pour les expériences de détection directe de matière sombre à bas seuil. / Amongst the dozens of experiments aiming to be the first to claim a dark matter signal, PICO is a direct dark matter detection experiment that utilizes superheated liquid detectors as a means of doing so. The latest C3F8 filled PICO-40L bubble chamber currently located in the SNOLAB underground laboratory is under testing to prepare for a 1 live-year blinded WIMP (Weakly Interacting Massive Particle) search. To ensure the stability of the detector during both the testing and the data acquisition phases, a monitoring software was coded. A reliable way to monitor all the parameters and to send alerts accordingly plays an important role in not only the success of PICO-40L, but also the development of the future larger-scale PICO-500 detector. PICO-0.1 is a test bubble chamber located at the University of Montreal that was built to calibrate for the numerous background events that can occur in this kind of technology. This test chamber was also used as a world’s first attempt to measure the coherent (Thomson) photon scattering onto a nucleus by exposing the C3F8 filled detector to a gamma source produced by the 19F proton to alpha and gamma 16O reaction using a proton beam created by the University of Montreal particle accelerator. This kind of interaction will prove to be a significant background for future sub-keV direct dark matter detection experiments.

La propagation des ondes acoustiques dans le plasma primordial a laissé son empreinte sous la forme d'un pic dans la fonction de corrélation à deux points de la densité de matière. Ce pic d'oscillations acoustiques de baryons (BAO) constitue une échelle standard permettant de déterminer certains paramètres des différents modèles cosmologiques.Dans ce manuscrit de thèse, nous présentons une mise à jour de la mesure de BAO à un redshift z=2.40, à l'aide de la fonction de corrélation croisée entre deux traceurs des fluctuations primordiales de densité de matière: les quasars de SDSS-III (BOSS) et leurs fluctuations d'absorption du flux des forêts Lyman-α. Ces fluctuations tracent la distribution d'hydrogène neutre dans le milieu intergalactique (IGM).Cette étude constitue le premier développement d'un ajustement entièrement physique de la fonction de corrélation croisée; il prend notamment en compte la physique des quasars et la présence d'éléments plus lourds que l'hydrogène dans l'IGM. Nous y présentons également les premières simulations de notre analyse. Celles-ci nous permettent de valider l'ensemble de la procédure de mesure de l'échelle BAO.Cette étude mesure la distance de Hubble et la distance de diamètre angulaire avec respectivement une précision de 2% et 3% (intervalle à 1 σ). Nous combinons nos résultats avec d'autres mesures de BAO à des redshifts plus faibles et trouvons la densité de matière noire et d'énergie noire dans le cadre de deux différents modèles cosmologiques: ΛCDM et oΛCDM. / The acoustic wave propagation in the primordial plasma left its imprint in the two-point correlation function of the matter density field. This baryonic acoustic oscillation (BAO) peak builds up a standard ladder allowing us to infer some parameters of the different cosmological models.In this thesis manuscript we present an update of the BAO measurement at a redshift z=2.40, from the cross-correlation function between two tracers of the primordial matter density fluctuations: quasars of SDSS-III (BOSS) and their Lyman-α-forest absorption fluctuations. These fluctuations trace the neutral hydrogen distribution in the intergalactic medium (IGM).This study gives the first developpment of the full physical fit of the cross-correlation. Among other effects, it takes into account quasar physics and the distribution of IGM elements heavier than hydrogen. We also present the first simulations of our analysis. They allow us to validate the overall data analysis leading to the BAO measurement.This study measures the Hubble distance and the angular diameter distance at the 2%$ and 3%$ precision level respectivelly (1 σ interval). We combine our results with other BAO measurements at lower redshifts and find the dark matter density and dark energy density in the framework of two different cosmological models: ΛCDM et oΛCDM.

No description available.

Orientador: José Fernando de Jesus / Resumo: Estudamos o campo escalar real como um possível candidato para explicar a matéria escura no universo. No contexto de um campo escalar livre com potencial quadrático, após encontrar as equações dinâmicas do modelo usamos os dados observacionais para limitar os parâmetros livres e assim encontrar um limite inferior para o valor da massa que foi da ordem de $10^{-34}$eV, esse valor está próximo ao encontrado por alguns autores. Não foi possível encontrar um limite superior para a massa da matéria escura do campo escalar combinando os dados de $H(z)$, SN Ia. Como verificado neste trabalho e observado em outros estudos, a matéria escura pode ser descrita por um campo escalar real. Em outra linha de pesquisa, usando um método estatístico não-paramétrico envolvendo os chamados Processos Gaussianos, obtivemos um valor do redshift de transição, $z_t$, de $z_t = 0.59^{+0.12}_{-0.11}$ para dados de $H(z)$ e $z_t= 0.683^{+0.11}_{-0.082}$ para dados de SNs Ia. / Abstract: We studied the real scalar field as a possible candidate to explain the dark matter in the universe. In the context of a free scalar field with quadratic potential, after finding the dynamic equations of the model we used the observational data to limit the free parameters and thus find a lower limit for the mass value that was in the order of 10−34 eV , this value is close to that found by some authors. It was not possible to find an upper limit for the mass of dark matter in the scalar field by combining the H(z) + SNe Ia data. As verified in this work and observed in other studies, dark matter can be described by a real scalar field. In another line of research, using a non-parametric statistical method involving the so-called Gaussian Processes, we obtained a value of the transition redshift, zt , of zt = 0.59+0.12 −0.11 for H(z) data and zt = 0.683+0.11 −0.082 for SNs Ia data. / Mestre

Orientador: Julio Marny Hoff da Silva / Resumo: Teorias que violam as simetrias de Lorentz são de certa forma comumente encontradas na literatura. Com o estudo dos subgrupos do grupo de Lorentz, uma pergunta fica no ar. Será preciso todo o grupo de Lorentz para descrever as simetrias do espaço-tempo ou apenas um subgrupo já seria suficiente? Se isso for possível teríamos um teoria que violaria as simetrias de Lorentz e consequentemente outras peguntas surgem. Essa teoria serve para descrever a matéria bariônica ou outro tipo de matéria? Neste trabalho usaremos os grupos da very special relativity (VSR) que são subgrupos do grupo de Lorentz e tentaremos responder essas perguntas com base em cálculos e em experimentos largamente difundidos na literatura: o experimento de Michelson-Morley e o fenômeno da precessão de Thomas. Também discutiremos algumas consequências advindas de uma teoria quântica de campos que viola as simetrias de Lorentz. / Mestre

Orientador: Saulo Henrique Pereira / Resumo: Efeitos térmicos em teoria de campos são estudados pela chamada Teoria de Campos a Temperatura Finita. Nessa dissertação estudamos os efeitos de temperatura de um campo fermiônico de dimensão de massa um (MDO), que obedece à equação Klein-Gordon em vez da de Dirac. A função de partição foi obtida por meio do formalismo de tempo imaginário e o resultado foi o mesmo que o obtido para campos fermiônicos padrões de Dirac. Obtemos os limites de alta e baixa temperatura, sendo que o limite de baixas temperaturas é proposto como sendo o responsável por manter os halos de matéria escura da galáxia numa região da mesma ordem ou maior que o raio galáctico. Para uma partícula leve com massa de 1eV e densidade de 0.1 partículas por cm³, o valor da massa total da matéria escura devido a partículas MDO é da mesma ordem da massa de uma galáxia típica. Tal resultado pode explicar a matéria escura como sendo formada por partículas fermiônicas de dimensão de massa um. Por fim, comparamos as estimativas de densidade dessas partículas com densidades obtidas através de dados de simulações numéricas e concluímos que para valores de massa entre 0.1eV a 1eV, as partículas MDO produzem uma massa típica de galáxias desde que a densidade delas esteja no intervalo de 10^(-2) cm^(-3) a 10^(5)cm^(-3). / Abstract: Thermal effects in feld theory are studied by the so called Finite Temperature Field Theory. In this dissertation we study the effects of temperature of a mass dimension one (MDO) fermionic field, which obeys the Klein-Gordon equation rather than the Dirac equation. The partition function was obtained via the imaginary time formalism and the result was the same as for the a Dirac fermionic field. We obtained the high and low temperature limits, and the latter is proposed as being responsable for keeping the dark matter halos of galaxies in a region greater than or of the same order as a typical galaxy radius. For a light particle of about 1eV and density of 0.1 particles per cm3 , the value of the total dark mass due to MDO particles is of the same order of a typical galaxy. Such result can explain dark matter as being formed by fermionic particles. Lastly, we compared those particles densities estimates with the ones obtained numeric simulation data and conclude that for mass values between 0.1eV and 1eV, the MDO particles yield a typical galaxy mass as long as their density is in the 10−2 cm−3 to 105 cm−3 interval / Mestre

This dissertation presents a search for dark matter particles produced in association with a Z boson in proton-proton collisions. The dataset consists of 139 fb^{-1} of collision events with centre-of-mass energy of 13 TeV, and was collected by the ATLAS detector from 2015-2018 at the Large Hadron Collider. Signal region events are required to contain a Z boson that decays leptonically to either e^+e^- or μ^+μ^-, and a significant amount of missing transverse momentum, which indicates the presence of undetected particles. Two types of dark matter models are studied: (1) simplified models with an s-channel axial-vector or vector mediator that couples to dark matter Dirac fermions, and (2) two-Higgs-doublet models with an additional pseudo-scalar that couples to dark matter Dirac fermions. The main Standard Model background sources are ZZ, WZ, non-resonant l^+l^-, and Z+jets processes, which are estimated using a combination of data and/or simulation. A new reweighting technique is developed for estimating the Z+jets background using γ+jets events in data; the resulting estimate significantly improves on the statistical and systematic errors compared to the estimate obtained from simulation. The observed data in the signal region are compared to Standard Model prediction using a transverse mass discriminant distribution. No significant excess in data is observed for the simplified models and two-Higgs-doublet models studied. A statistical analysis is performed and several exclusion limits are set on the parameters of the dark matter models. Results are compared to direct detection experiments, the CMS experiment, and other ATLAS searches. Prospects and improvements for future iterations of the search are also presented. / Graduate

In the standard model of cosmology (ΛCDM) the first stars, star clusters, and galaxies are expected to have formed in short bursts of star formation in low-mass dark matter halos at high redshifts (<img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?z%5C,%20%5Csim%20%5C,6-10" data-classname="equation_inline" />). Up to this point, attempts to predict the properties and abundances of these luminous objects have made use of numerically expensive cosmological simulations. On top of being numerically expensive, these simulations often lack the required sub-parsec resolution needed to resolve the formation of compact star clusters and/or neglect possibly dominant stellar feedback processes. Motivated by this, I introduce Anaxagoras, as far as I know the most detailed analytical ab initio model of starbursts in low-mass halos to date. The model incorporates sub-models for gas cooling (including a new determination of the H2-cooling threshold in minihalos), central gas accretion and disk formation (using a new selfsimilarsolution), stellar feedback from radiation pressure (direct stellar radiation, Lyman-<img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?%5Calpha" data-classname="equation_inline" data-title="" /> scattering in H I, and multiple scattering of IR photons by dust), stellar winds, expanding HII regions, and (crudely) supernovae. The resulting star formation efficiency is used to predict the fraction of stars that remain gravitationally bound in a cluster following gas expulsion, andwhat fraction escape the central region of the halo, yet remain bound by the dark matter halo. I apply Anaxagoras to study star formation at <img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?z%5C,%20%3E%20%5C,6" data-classname="equation_inline" /> in satellite halos of the Milky Way using a halo merger tree code, as well as Population III (Pop III) star formation in minihalos. For the Milky Way setup, hundreds of galaxies are predicted to form with luminosities (<img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?L_%7B%5Crm%20V%7D%20%5C,%3C%5C,%20%5Crm%7Bfew%7D%5C,%20%5Ctimes%20%5C,%2010%5E4%20%5C:%20%5Crm%7BL%7D_%7B%5Codot%7D" data-classname="equation_inline" />), half-mass radii (<img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?%5Csim%2010-200%5C:%5Crm%20pc" data-classname="equation_inline" />), mass-to-light ratios (<img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?M/L_%7B%5Crm%20V%7D%20%5Csim%20100%20-%20%5Crm%7Bfew%7D%20%5C,%5Ctimes%5C,%2010%5E3%20%5C:%5Crm%7BM%7D_%7B%5Codot%7D/%5Crm%7BL%7D_%7B%5Codot%7D" data-classname="equation" />), and ages (<img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?13.18%5E%7B+0.29%7D_%7B-0.31%7D%5C:%5Crm%20Gyrs" data-classname="equation_inline" data-title="" />) in good agreement with the observed local population of Ultra-Faint Dwarfs. This shows that ΛCDM is able to explain the properties ofthe faintest dwarf galaxies without fine-tuning. Furthermore, at least ~ 40 compact (initial half-mass radii <img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?%5Csim%200.1-5%5C;%5Crm%7Bpc%7D" data-classname="equation_inline" />), old (<img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?13.27%5E%7B+0.21%7D_%7B-0.39%7D%5C:%5Crm%20Gyrs" data-classname="equation_inline" />) globular cluster (GC) candidates with initial stellar masses <img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?10%5E5%20-%2010%5E6%20%5C:%20%5Crm%7BM%7D_%7B%5Codot%7D" data-classname="equation_inline" />  are predicted to form at the center of low-mass halos, and could survive to the present-day and explain at least a fraction of the observed metal-poor GCs. Their properties are consistent with recent candidates for GCs residing in dark matter halos. Thus, Anaxagoras lends support to the viability of the scenario of GC formation in minihalos. Finally, the formation of Population III (Pop III) stars in minihalos is studied, with the conclusion that if Pop III stars are not overly massive (<img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?25%5C:%5Crm%7BM%7D_%7B%5Codot%7D" data-classname="equation_inline" />) between ~ 1 − 30 stars could form per minihalo at <img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?z%5C,%20%3E%20%5C,20" data-classname="equation_inline" />, with the number increasing to ~ 10 − 500 stars per minihalo at <img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?z%5C,%3C%5C,15" data-classname="equation_inline" /> as Lyman-Werner feedback delay star formation until halos reach larger masses. In the case where Pop III stars are more massive (<img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?140%5C:%5Crm%7BM%7D_%7B%5Codot%7D" data-classname="equation_inline" data-title="" />) most minihalos form just a single star. Due to self-shielding of H2 in minihalos, I find that the cosmological Lyman-Werner background is insufficient to produce Pop III galaxies in atomic-cooling halos, with the implication that the number of massive Pop III galaxies/star clusters in the early Universe has been greatly overestimated in the literature that ignores self-shielding.

In this study, we investigate the feasibility of Feebly Interacting Massive particles (FIMP) as possible candidates to constitute the observed Dark Matter abundance in the universe. FIMPs are particles that couple very feebly with known particles in the Standard Model (SM). As such, they do not attain thermal equilibrium with the baryon abundant environment in the early universe before Nucleosynthesis. In contrast to a freeze-out mechanism common for Weakly Interacting Massive Particles (WIMP) as DM candidates, FIMPs are produced by the so-called freeze-in mechanism that we will describe in this study. The purpose of this study is to investigate how the Coleman Weinberg (C-W) mechanism affects the FIMP [freeze-in] mechanism. We specifically consider a minimal extension of SM in which an Electroweak Singlet-scalar ($S$) couples only to the Higgs-boson ($H$); This is called the Higgs-portal mechanism. We study the C-W effective potentials for the Higgs and Dark-scalar singlet and their implications on FIMP mechanism.Using these, we focus on the High-temperature production of the DM with just the $HH\mapsto SS$ to compute the reaction rates, comparing Bose-Einstein statistics ($\Gamma_{HH\mapsto S S}^{B-E}$) to Maxwell-Boltzmann statistics $\Gamma_{HH\mapsto S S}^{M-B}$. We employ only $\Gamma_{HH\mapsto S S}^{B-E}$ to compute DM relic abundance ($Y$) at several Dark-scalar masses ($m_S$) as a function of coupling $k$, establishing that Higgs-Dark scalar coupling $k$ $\mapsto$ $k_{DM}$ corresponding to actual DM abundance lies in between ${10}^{-8.7}$ and ${10}^{-8}$, i.e. ${10}^{-8.7}&lt;k_{DM}&lt;="" div=""&gt; / I denna studie undersöker vi mycket svagt interagerande massiva partiklar (FIMP) som möjliga kandidater till den observerade mängden av mörk materia i universum. FIMP:er är partiklar som interagerar väldigt svagt med de kända partiklarna i Standarmodellen (SM). Som sådana uppnår de ej termisk jämvikt med den baryonrika omgivningen i det tidiga universumet innan nukleosyntes sker. I kontrast med en frys-ut mekanism vanligt för svagt interagerade massiva partiklar (WIMPS) som DM kandidater, så produceras FIMP:er av en så kallad frys-in mekanism som vi skall beskriva i denna studie. Syftet med studien är att undersöka hur Coleman Weinberg (C-W) mekanismen påverkar frys-in mekanismen för FIMP:er. Vi tar särskilt hänsyn till en minimal utvidgning av SM i vilken en Elektrosvag singlettskalär ($S$) interagerar med endast Higgsbosonen. Denna mekanism kallas för Higgs-portalmekanism. Vi studerar de C-W effektiva pontetialerna för higgs och mörk-skalärsingletten och deras implikationer för FIMPmekanismen. När vi använder dessa, så fokuserar vi på högtemperatursproduktion av DM med endast $HH\mapsto SS$ för att beräkna reaktionshastigheter, och jämför Bose-Einstein statistik ($\Gamma_{HH\mapsto S S}^{B-E}$) med Maxwell-Boltzmann statistik $\Gamma_{HH\mapsto S S}^{M-B}$. Vi använder endast $\Gamma_{HH\mapsto S S}^{B-E}$ för att beräkna kvarvarande DM mängd ($Y$) för flera mörk-skalärmassor ($m_S$) som en funktion av interaktion $k$, vilket slår fast att Higgs-Mörk skalär interaktionen $k$ $\mapsto$ $k_{DM}$ som korresponderar mot den faktiska DM mängden ligger mellan ${10}^{-8.7}$ and ${10}^{-8}$, i.e. ${10}^{-8.7}&lt;k_{DM}&lt;="" div=""&gt;