Cette thèse traite des aspects astrophysiques de la détection directe (DD) de matière noire sous forme de WIMPs. On se concentre sur les contraintes observationnelles des quantités astrophysiques qui influent sur l'interprétation des résultats expérimentaux de DD.On revoit tout d'abord le formalisme de la DD et on résume les résultats expérimentaux les plus importants ainsi que les méthodes statistiques généralement utilisés pour interpréter les données. On reproduit ensuite les limites expérimentales sur la section efficace spin-indépendante. On résume l'ensemble des hypothèses astrophysiques couramment utilisées dans le modèle de halo standard et on décrit l'influence de ses paramètres sur les limites.Pour inscrire la DD dans un cadre plus général, on résume les concepts les plus importants de la dynamique Galactique. En particulier, on revoit comment modéliser la Galaxie avec des modèles de masse, tout en soulignant les relations entre les différentes quantités astrophysiques. On décrit des procédures qui permettent d'obtenir des distributions dans l'espace des phases de la matière noire qui soient consistantes avec un profil de matière noire et un potentiel Galactique donné. La plus simple procédure étant basée sur l'équation d'Eddington, on discute ses limites d'applicabilité. On revoit dans les détails la littérature récente concernant les déterminations et les incertitudes des quantités astrophysiques liées à la DD et des paramètres Galactiques fondamentaux.Dans la dernière partie de la thèse on s'intéresse aux estimations récentes de la vitesse d'échappement publiées par la collaboration RAVE. On étudie dans les détails les implications de ces résultats sur les expériences de DD. Pour cela on prends en compte les corrélations entre les quantités astrophysiques importantes pour la DD, et en assumant le modèles de masse de RAVE on calcule la distribution de matière noire dans l'espace des phases avec l'équation d'Eddington. Du fait des valeurs plus élevés de la densité locale de matière noire, cette procédure conduit à des limites plus contraignantes par rapport a celles standards. / This thesis deals with the astrophysical aspects of the direct detection of WIMP dark matter (DMDD). In particular, it focuses on the observational constraints on the astrophysical quantities relevant for DMDD, which impact on the interpretation of the experimental results.We review the formalism of DMDD and we summarize some of the main experimental results in this domain and the statistical methods usually employed to interpret the data, reproducing the associated constraints on the parameter space relevant for spin-independent WIMP-nucleon interaction. We summarize the set of astrophysical assumptions usually employed, the Standard Halo Model, and we point out the impact of variations in its parameters on such limits.We outline the main concepts of the dynamics of our galaxy that allow to put the astrophysics related to DMDD in a wider framework. In particular, we review the description of the Galaxy through Milky Way mass models (MWMM), pointing out how the astrophysical quantities are related. We describe some procedures to obtain dark matter phase-space distributions consistent with given dark matter profile and Galactic potential, the simplest being Eddington equation, of which we discuss the limits of applicability. We review in detail the recent literature on the main determinations and uncertainties of the astrophysical quantities relevant for DMDD and of the fundamental Galactic parameters.In the most original part of this thesis we focus on the recent estimates of the local Galactic escape speed published by the RAVE collaboration. We study in detail the implications of these results for the spin-independent interpretation of DMDD experiments. We take into account the correlations between the astrophysical quantities relevant for DMDD calculations, and from the assumed MWMM we compute the dark matter phase-space distribution using Eddington equation, which provides a self-consistent physical connection between the two. This procedure leads to more constraining exclusion curves with respect to the standard ones, due to higher values of the local dark matter density.

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Made available in DSpace on 2015-05-14T12:14:17Z (GMT). No. of bitstreams: 1 arquivototal.pdf: 8387291 bytes, checksum: 02ffc69a044d7312934d6910183b8440 (MD5) Previous issue date: 2015-04-25 / Coordenação de Aperfeiçoamento de Pessoal de Nível Superior - CAPES / In this work we consider a minimal local abelian gauge group extension with charge B - 3Le anomaly-free. We add a right-handed singlet Majorana fermion plus a neutral and charged scalars, responsible for spontaneous symmetry breaking and a charged singlet scalar to provide a connection between the electron and the Majorana fermion. The aim of this model is provide a low energy theory to Dark matter as a Majorana fermion. There are several evidences of a new kind of a non-baryonic matter but its nature and properties are not well established. So, based in some experiments (in particular those that main focus is the direct detection), we are going to constraint some parameters of the model to test its feasibility in this context. We have used a computational program called micrOMEGAs (based on CalCHEP) to compute the abundance and scattering cross section between dark matter and nucleon and compare with the experimental constraints arising from Planck (abundance) and LUX (scattering cross section). We show that the results support the restrictions imposed by the observations providing future perspectives for this extension, like indirect detection of dark matter. / Nesta dissertação consideramos uma extensão abeliana mínima local, de carga B-3Le, livre de anomalias, onde foi introduzido um férmion de majorana de mão direita juntamente com um novo bóson escalar, responsável pela quebra espontânea da simetria local, e um escalar carregado conectando a família de léptons ao férmion de majorana. Este modelo tem por objetivo fornecer uma teoria de baixas energias para a matéria escura atribuída a um férmion de majorana. Logo, baseado em alguns experimentos (em particular aqueles cujo principal objetivo é a detecção direta de uma possível nova partícula atribuída à esta matéria), iremos vincular os parâmetros de nosso modelo a fim de verificar sua aplicabilidade neste senário. Com isto, utilizaremos o programa computacional micrOMEGAS (que utiliza o CalcHEP) a fim de calcular alguns observáveis do modelo, tais como a abundância e secção transversal de choque do espalhamento elástico entre a matéria escura e o nucleon e, em seguida, comparamos aos dados experimentais do Planck (abundância) e LUX (seção de choque). Resultados preliminares apontam para a validade do modelo diante das restrições impostas pelas observações, possibilitando a perspectiva de aplicação desta extensão em outros contextos, como os da detecção indireta da matéria escura.

Lignes spectrales de rayons gammas provenants de la matière noire. <p>Approches indépendantes de modèles/ Gamma-Ray Lines from the Dark Side of Matter: Model-Independent Approaches<p><p> Cette thèse a pour thématique centrale la matière noire, et plus particulièrement un type de signal qu’elle pourrait émettre, à savoir des lignes spectrales de rayons gammas. La nature de la matière noire demeure mystérieuse, et ce que l’on sait de ses propriétés est exposé dans le premier chapitre. En particulier, la pertinence des lignes spectrales de rayons gammas dans l’étude de la matière noire est soulignée. Cette thèse est consacrée à l’étude des connexions possibles entre la phénoménologie de ce type de signal et d’autres manifestations, qu’il s’agisse de détection directe ou indirecte, ou bien de détection dans des collisionneurs tels que le LHC. Le but est d’établir la possibilité de discriminer différents modèles et/ou d’obtenir des contraintes indépendantes.<p>\ / Doctorat en Sciences / info:eu-repo/semantics/nonPublished

<p align="justify">The success of Big Bang Nucleosynthesis (BBN) combined with the detailed analysis of the small imperfections of the Cosmic Microwave Background blackbody spectrum lead to the conclusion that most of the matter content of our universe is made of some non-baryonic material, the dark matter!</p><p><p><p align="justify">In this thesis, we review the compiling indications of dark matter and the so-called freeze-out mechanism which may settle the relic density of the species in the framework of the standard Big Bang model. We also examine principally two methods of detection of dark matter, direct and indirect detection searches.</p><p><p><p align="justify">Let us stress that the Standard Model on its own is unable to provide enough aspirants for the role of dark matter. As a consequence, one has to dig into the tremendous domain of physics "Beyond the Standard Model" in order to have a chance to elucidate the problem of the missing mass.</p><p><p><p align="justify">In this thesis in particular, we consider the Inert Doublet Model (IDM) which includes an additional Higgs doublet, enclosing two neutral scalars candidates for dark matter. We invoke the Standard freeze-out mechanism for the production of dark matter. We get then dark matter candidates in two rather separate mass ranges, one between 40 and 80 GeV, the other one between 400 GeV and 1 TeV. We also show that dark matter annihilation at the galactic center can be at the origin of a gamma-ray flux which can be probed by the future GLAST experiment.</p><p><p><p align="justify">We address a low reheating temperature scenario for the genesis of dark matter in a Left-Right symmetric extension of the Standard Model. The candidate for dark matter is a MeV right-handed neutrino and we show that a baryon-dark matter interaction at the galactic center can be the source of the low energy positrons responsible for the 511 keV gamma-ray excess observed by the INTEGRAL experiment in the galactic bulge region.</p><p><p><p align="justify">Finally, prompted by the possibility to explain the baryon and dark matter rather similar abundances by one single "Matter Genesis" mechanism, we study a non-thermal production mechanism for dark matter. The framework is also Left-Right symmetric and dark candidate is a ~3 GeV right handed neutrino.</p> <p><p> / Doctorat en Sciences / info:eu-repo/semantics/nonPublished

Dark matter has been inferred from various observations such as in galaxy clusters, flat galactic rotation curves, gravitational lensing measurements and the cosmic microwave background. Despite overwhelming observational evidence and ongoing searches, a clear signal of dark matter has not yet been detected. Searches for dark matter include direct detection of dark matter scattering off target nuclei in underground detectors and indirect detection of dark matter annihilation- and decay products. A promising way to detect these invisible particles is by capture of dark matter in the Sun. Dark matter from the galactic halo is assumed to scatter off solar nuclei and being captured provided that their velocities are smaller than the Sun's escape velocity. The captured particles are assumed to continuously scatter until reaching thermal equilibrium. As dark matter is accumulated in the Sun, they will start to annihilate. The resulting annihilation products are what we hope to detect on Earth. We review the capture rate of elastic and inelastic dark matter in the Sun and dark matter direct detection. Lower bounds on the solar capture rate for a given dark matter mass can be obtained independently of halo-related properties e.g., the dark matter velocity distribution and local density, if one assumes that a direct detection signal has been observed. These bounds can be compared to solar neutrino flux bounds in detectors to obtain limits on the branching fraction of annihilation of dark matter resulting in neutrinos. Lower bounds for the elastic and exothermic inelastic dark matter are computed assuming the Standard Halo Model. The exothermic bounds are strong and larger than the elastic bounds as well as those that would be obtained in the endothermic case. / Existensen av mörk materia har idag gjorts trolig genom t.ex. observationer av galaktiska kluster, galaktiska rotationskurvor, gravitationslinsmätningar och den kosmiska mikrovågsbakgrunden. Trots ett stort antal observationer, så har vi emellertid inte lyckats detektera en tydlig signal för mörk materia. I sökandet ingår direkt detektion av kollisioner mellan mörk materia och atomkärnor i underjordiska detektorer samt indirekt detektion av dess annihilation- och sönderfallsprodukter. Ett särskilt lovande sätt, på vilket dessa osynliga partiklar kan tänkas detekteras, är genom infångning av mörk materia i solen. Mörk materia från den galaktiska halon antas då spridas på solatomkärnor och infångas förutsatt att deras hastighet är lägre än flykthastigheten från solen. De infångade partiklarna antas därefter kollidera tills dess att de uppnår termisk jämvikt. När mörk materia har ackumulerats i solen så börjar den att annihilera, och det är de resulterande annihilationsprodukterna som vi hoppas kunna detektera här på jorden. Vi undersöker infångning av elastisk och inelastisk mörk materia i solen och direkt detektion av mörk materia. Nedre gränser för solinfångning för en given mörk materiamassa kan erhållas oberoende av halo-relaterade egenskaper som t.ex. mörk materiahastighetsfördelning och lokal densitet, under antagandet att en direkt detektionssignal har observerats. Dessa gränser kan jämföras med flödeshastigheten av neutrinos från solen för att erhålla gränser för övergångssannolikheter för annihilation av mörk materia som resulterar i neutrinos. Nedre gränser för elastisk och exotermisk inelastisk mörk materia är beräknade genom att anta Standard Halo Modellen. De exotermiska gränserna är starka och högre än de elastiska gränserna såväl som de som skulle ha erhållits i det endotermiska fallet.

We present new measures of the rotation curves of disc galaxies from z~0.2 to z~1.7, using deep exposures from both DEIMOS and LRIS spectrographs on the Keck telescopes in combination with multi-band imaging from the Hubble Space Telescope. We do this with a new modelling code, curvation, which has been optimised to extract the rotation velocity measurements from galaxies at intermediate and high redshift. To this end, we conduct a bulge-to-disc de-composition to allow us to de-project observed velocities to extract a model of the intrinsic rotation curve. We demonstrate the improved accuracy and precision of these measurements via a number of tests, but primarily in recovering an intrinsic scatter of the high redshift Tully-Fisher relation which is similar to that found locally. We show for the first time that the stellar mass Tully-Fisher relation is tightly in place at z~1, the normalisation of which has evolved less than 0.02±0.02 dex in stellar mass from z~1.7 to z~0.2. We do however see evidence for evolution in classic B-band Tully-Fisher relation, which is brighter at z~1 by 0.85±0.28 magnitudes than that at z~0.3. This trend is consistent with what was previously known about the evolving star-formation rates of disc galaxies. We then explore the potential drivers of these trends in the Tully-Fisher relation by estimating the baryonic and dark matter content of our galaxies. We also discover a surprising trend in the bulgeless disc galaxies at high redshift, which may be evolving differently from other rotationally supported galaxies. In the context of work which has been conducted at z~2, we discuss our results of a stellar mass Tully-Fisher relation which is strikingly similar over two-thirds of the age of the Universe.

I present an overview of the tools and methods of gravitational dynamics motivated by a variety of dynamics problems. Particular focus will be given to the development of dynamic phase-space configurations as well as the distribution functions of collisionless systems. Chapter 1 is a short review of the descriptions of a gravitational system examining Poisson's equations, the probability distribution of particles, and some of the most popular model groups before working through the challenges of introducing anisotropy into a model. Chapter 2 covers the work of Barber2014b which looks at the relations between quantities in collisionless systems. Analytical methods are employed to describe a model that can violate the GDSAI, a well-known result connecting the density slope to the velocity anisotropy. We prove that this inequality cannot hold for non-separable systems and discuss the result in the context of stability theorems. Chapter 3 discusses the background for theories of gravity beyond Newton and Einstein. It covers the `dark sector' of modern astrophysics, motivates the development of MOND, and looks at some small examples of these MONDian theories in practice. Chapter 4 discusses how to perform detailed numerical simulations covering code methods for generating initial conditions and simulating them accurately in both Newtonian and MONDian approaches. The chapter ends with a quick look at the future of N-body codes. Chapters 5 and 6 contain work from Barber 2012 and Barber 2014a which look at the recent discovery of an attractor in the phase-space of collisionless systems and present a variety of results to demonstrate the robustness of the feature. Attempts are then made to narrow down the necessary and sufficient conditions for the effect while possible mechanisms are discussed. Finally, the epilogue is a short discussion on how best to communicate scientific ideas to others in a lecturing or small group setting. Particular focus is given to ideas of presentation and the relative importance of formality versus personality.

We use the shear catalogue from the CFHT Stripe-82 Survey to measure the subhalo masses of satellite galaxies in redMaPPer clusters. Assuming a Chabrier initial mass function and a truncated NFW model for the subhalo mass distribution, we find that the subhalo mass to galaxy stellar mass ratio increases as a function of projected halo-centric radius r(p), from M-sub/M-star = 4.43(-2.23)(+6.63) at r(p) is an element of [0.1, 0.3] h(-1) Mpc toM(sub)/M-star = 75.40(-19.09)(+19.73) at r(p) is an element of [0.6, 0.9] h(-1) Mpc. We also investigate the dependence of subhalo masses on stellar mass by splitting satellite galaxies into two stellar mass bins: 10 < log (M-star/h(-1) M-circle dot) < 10.5 and 11 < log (M-star/h(-1) M-circle dot) < 12. The best-fitting subhalomass of the more massive satellite galaxy bin is larger than that of the lessmassive satellites: log(M-sub/h(-1) M-circle dot) = 11.14(-0.73)(+0.66) (M-sub/M-star = 19.5(-17.9)(+19.8)) versus log(M-sub/h(-1) M-circle dot) = 12.38(-0.16)(+0.16) (M-sub/M-star = 21.1(-7.7)(+7.4)).

This research uses a Bayesian approach to study the biases that may occur when kinematic data is used to estimate the mass of a galaxy. Data is simulated from the Hernquist (1990) distribution functions (DFs) for velocity dispersions of the isotropic, constant anisotropic, and anisotropic Osipkov (1979) and Merritt (1985) type, and then analysed using the isotropic Hernquist model. Biases are explored when i) the model and data come from the same DF, ii) the model and data come from the same DF but tangential velocities are unknown, iii) the model and data come from different DFs, and iv) the model and data come from different DFs and the tangential velocities are unknown. Mock observations are also created from the Gauthier (2006) simulations and analysed with the isotropic Hernquist model. No bias was found in situation (i), a slight positive bias was found in (ii), a negative bias was found in (iii), and a large positive bias was found in (iv). The mass estimate of the Gauthier system when tangential velocities were unknown was nearly correct, but the mass profile was not described well by the isotropic Hernquist model. When the Gauthier data was analysed with the tangential velocities, the mass of the system was overestimated. The code created for the research runs three parallel Markov Chains for each data set, uses the Gelman-Rubin statistic to assess convergence, and combines the converged chains into a single sample of the posterior distribution for each data set. The code also includes two ways to deal with nuisance parameters. One is to marginalize over the nuisance parameter at every step in the chain, and the other is to sample the nuisance parameters using a hybrid-Gibbs sampler. When tangential velocities, v(t), are unobserved in the analyses above, they are sampled as nuisance parameters in the Markov Chain. The v(t) estimates from the Markov chains did a poor job of estimating the true tangential velocities. However, the posterior samples of v(t) proved to be useful, as the estimates of the tangential velocities helped explain the biases discovered in situations (i)-(iv) above. / Thesis (Master, Physics, Engineering Physics and Astronomy) -- Queen's University, 2013-03-26 17:23:14.643