La Matière Sombre représente une des quêtes les plus importantes pour la compréhension des constituants élémentaires de l'Univers: la nature de la Matière Sombre est toujours mystérieuse. La dernière décennie a connu des développements expérimentaux remarquables dans la recherche de la Matière Sombre. Le but de ce travail est l'étude de candidats de Matière Sombre de nature supersymétrique (le neutralino) et au-delà (les particules scalaires), et de leurs aspects phénoménologiques et d'astroparticules. Le neutralino, dans l'intervalle de masses 1-100 GeV, est testé par les expériences du Grand Collisionneur d'Hadrons, de détection directe et de détection indirecte; ce travail montre que la combinaison de ces techniques est un outil décisif pour une recherche minutieuse des prédictions théoriques. Les particules scalaires sont des candidats non-standards de masses jusqu'à 1 MeV qui pourraient être produits abondamment dans le Grand Collisionneur d'Hadrons, et au même temps expliquer d'autres phénomènes tels que la masse des neutrinos et/ou le signal à 511 keV provenant du centre galactique de la Voie Lactée. / The Dark Matter problem is one of the most relevant quests for the understanding of the elementary constituents of the Universe: the nature of the Dark Matter is still unveiled. Experimental efforts aiming to detect the Dark Matter have shown a great progress in the last decade. This work is devoted to the phenomenological and astroparticle studies of Dark Matter candidates of supersymmetric nature -the neutralino- and beyond -scalar particles. The former, in the 1-100 GeV mass range, is currently being tested by the Large Hadron Collider, direct detection and indirect detection experiments; this work shows that the interplay between techniques is a decisive tool to thoroughly search for theoretical predictions. The latter is a non-standard candidate as light as 1 MeV which could be copiously produced at the Large Hadron Collider, and at the same time explain other phenomena such as neutrino masses and/or the 511 keV line from the galactic center of the Milky Way.

A utilização, em sistemas de comunicações ópticas, de formatos de modulação digitais é vista, atualmente, como uma forma promissora de aumentar a eficiência espectral, frente aos diversos efeitos de degradação do sinal em fibra óptica, sem alterar a infraestrutura já implantada. É neste contexto que surge a técnica OFDM (orthogonal frequency division multiplexing) que estabelece sobreposição espectral das subportadoras e, desta forma, permite a transmissão dos dados em forma multiplexada com grande eficiência espectral. No presente trabalho, foi proposta a simulação da técnica OFDM com modulação QAM (quadrature amplitude modulation) no software Optisystem, versões 9.0 e 10.0. O objetivo principal da pesquisa é estudar algumas configurações de sistemas OFDM óptico, com detecção direta e coerente, visando avaliar seu desempenho sistêmico frente a efeitos de propagação. Usando as figuras de mérito BER e diagrama de constelação para estabelecer a meta de ótimo desempenho, analisamos a técnica OFDM com detecção coerente em configurações aplicáveis, principalmente, para redes ópticas de acesso com alcance estendido. Para validação dos resultados, são apresentados também estudos que relacionam as degradações do sinal em fibra óptica e a técnica OFDM. Estes resultados foram comparados com os existentes na literatura, apresentando boa concordância. / The development of digital modulation formats in optical communications systems is considered to be a promising way to increase the spectral efficiency and to combat the effects of signal degradation in optical fiber without changing the infrastructure already deployed. In this context, the technique called OFDM (orthogonal frequency division multiplexing) establishes a particular spectral overlap of the subcarriers, which allows data transmission to be multiplexed with high spectral efficiency. The main objective of the research is to study some configurations of optical OFDM systems with direct detection and coherent in order to evaluate their performance against propagation effects. Using the figures of merit BER and constellation diagram to establish the goal of optimal performance, we analyze the OFDM technique with coherent detection in configurations more applicable for optical access networks with extended reach. To validate the results we also present some studies that relate the degradation of the signal in an optical fiber and the OFDM technique. These results were compared with those described in literature, showing good agreement.

Une solution au problème astrophysique de la matière sombre pourrait être apportée par la détection de WIMPs, particules prédites par la supersymétrie. Sa détection directe nécessite de grandes masses de détecteurs capables d'identifier le signal d'un WIMP parmi le fond radioactif et cosmique environnant. Cette thèse se déroule dans le cadre de l'expérience EDELWEISS et la future expérience EURECA qui lui succédera. Ces expériences utilisent une technologie basée sur des détecteurs cryogéniques (bolomètres) à double voies, fonctionnant à quelques dizaines de mK. Ils sont constitués de cristaux qui sont le siège des interactions des particules, dont les dépôts d'énergie vont entraîner une élévation de température ainsi que l'ionisation du cristal, pouvant entraîner des charges ou des photons selon sa nature. Afin d'augmenter la palette de cibles pouvant faire office de bolomètres scintillants, nous avons mis en place un dispositif expérimental permettant d'étudier la scintillation de cristaux refroidis jusqu'à 3 K. Il est basé sur un cryostat à géométrie optique compacte permettant une collecte de lumière améliorée. Une méthode de comptage de photons individuels ainsi qu'un traitement statistique des données permettent de mesurer l'évolution du rendement lumineux et des constantes de temps de scintillation de cristaux entre la température ambiante et 3K. Cette thèse présente ainsi les résultats obtenus à 3 K avec ce dispositif expérimental sur deux cristaux, bien connus à température ambiante: le BGO (Bi4Ge3O12) et le BaF2. Nous présentons également les résultats sur la luminescence du saphir dopé au titane (Ti:Al2O3), sous VUV et refroidi à 8 K. / A solution to the dark matter problem in astrophysics could be found by the detection of WIMPs, particles predicted by supersymmetry. Its direct detection requires a large mass of detectors, able to identify WIMPs in the background of natural radioactivity and cosmic rays. This thesis takes place within the framework of the EDELWEISS and the future EURECA experiments. These experiments use a technology based on two channel cryogenic detectors (bolometers), working at a few tens of mK. They are made of crystals in which the energy deposited by particle interactions will produce a temperature increase (phonon signal), and where the ionization of the crystals results in either a charge or photon signal, depending on their nature. In order to broaden the range of targets for scintillating bolometers, we have built a setup to study the scintillation of crystals cooled down to 3 K. It is based on a cryostat with a compact optical geometry allowing enhanced light collection. Thanks to an individual photon counting technique and a statistical treatment of data, it allows us to measure the evolution of the the light yields and the decay time components between room temperature and 3 K. Thus this thesis presents the results obtained at 3 K on two well known room temperature crystals: BGO (Bi4Ge3O12) and BaF2. We also study the luminescence properties of titanium sapphire (Ti:Al2O3), under VUV excitation cooled down to 8 K.

The hunt for Dark Matter plays a truly critical role in contemporary physics. At both the largest and smallest scales, deep questions are being raised about the fundamental nature of the universe - questions that confirmation and then characterisation of particle dark matter will provide many answers to. This thesis presents some of the world's most sensitive searches to date for certain types of axion dark matter, axion-like particles, and two-neutrino double electron capture. These have been conducted using the Large Underground Xenon (LUX) experiment. Evidence for dark matter and physics beyond the Standard Model of particle physics is described in Chapter 1, while Chapter 2 gives an overview of proposed candidates for particle dark matter. The various experimental approaches being used to detect particle dark matter are presented in Chapter 3. Direct detection with time projection chambers plays a major role in this thesis, with particular interest in the LUX detector, that is described in its components and operations. Chapter 4 presents LUX direct searches for weakly interacting massive particles. Although I have contributed to these analyses, they are included for completeness only, as they are not part of my central work. The LUX collaboration's searches for axion dark matter and axion-like particle have delivered world-leading results on the axion-electron coupling constant. These results, that I personally led and which have been published in Physics Review Letters, are presented in Chapter 5, along with sensitivity studies, also led by me, made for the future LUX-ZEPLIN experiment. Finally, a search for two-neutrino double electron capture of 124Xe, that I performed using LUX data to extract a limit on the half life of the process, is presented in Chapter 6. Although being allowed by the Standard Model, two-neutrino double electron capture shares the matrix element calculation framework with the neutrinoless channel of the same process, becoming of great interest in the scope of neutrino physics. Conclusions follow and close the thesis.

A utilização, em sistemas de comunicações ópticas, de formatos de modulação digitais é vista, atualmente, como uma forma promissora de aumentar a eficiência espectral, frente aos diversos efeitos de degradação do sinal em fibra óptica, sem alterar a infraestrutura já implantada. É neste contexto que surge a técnica OFDM (orthogonal frequency division multiplexing) que estabelece sobreposição espectral das subportadoras e, desta forma, permite a transmissão dos dados em forma multiplexada com grande eficiência espectral. No presente trabalho, foi proposta a simulação da técnica OFDM com modulação QAM (quadrature amplitude modulation) no software Optisystem, versões 9.0 e 10.0. O objetivo principal da pesquisa é estudar algumas configurações de sistemas OFDM óptico, com detecção direta e coerente, visando avaliar seu desempenho sistêmico frente a efeitos de propagação. Usando as figuras de mérito BER e diagrama de constelação para estabelecer a meta de ótimo desempenho, analisamos a técnica OFDM com detecção coerente em configurações aplicáveis, principalmente, para redes ópticas de acesso com alcance estendido. Para validação dos resultados, são apresentados também estudos que relacionam as degradações do sinal em fibra óptica e a técnica OFDM. Estes resultados foram comparados com os existentes na literatura, apresentando boa concordância. / The development of digital modulation formats in optical communications systems is considered to be a promising way to increase the spectral efficiency and to combat the effects of signal degradation in optical fiber without changing the infrastructure already deployed. In this context, the technique called OFDM (orthogonal frequency division multiplexing) establishes a particular spectral overlap of the subcarriers, which allows data transmission to be multiplexed with high spectral efficiency. The main objective of the research is to study some configurations of optical OFDM systems with direct detection and coherent in order to evaluate their performance against propagation effects. Using the figures of merit BER and constellation diagram to establish the goal of optimal performance, we analyze the OFDM technique with coherent detection in configurations more applicable for optical access networks with extended reach. To validate the results we also present some studies that relate the degradation of the signal in an optical fiber and the OFDM technique. These results were compared with those described in literature, showing good agreement.

Deux problématiques sont abordées dans cette thèse: la formation de galaxies spirales et la détection de la matière noire (MN).Nous étudions trois simulations cosmologiques hydrodynamiques de haute résolution zoomées sur des halos de propriétés similaires à celui de la Voie Lactée que nous réalisons avec le code à grille adaptative RAMSES. Nous analysons les distributions d'étoiles et de gaz et constatons qu'une de nos galaxies simulées possèdent des propriétés intéressantes par rapport à la Voie Lactée. Nous obtenons un disque stellaire étendu et une courbe de rotation plate avec la vitesse de rotation et la densité locale de MN en accord avec les observations. En ce qui concerne la distribution de MN, nous analysons l'interaction avec les baryons et nous montrons explicitement comment le profil de densité de MN est aplatie par les processus de feedback.Dans le cadre de cette simulation, nous étudions les incertitudes astrophysiques sur la détection directe en analysant les quantités importantes comme la densité locale de MN, sa distribution de vitesse et la vitesse d'échappement locale. De plus, nous considérons plusieurs sélections de distribution de MN et d'étoiles et estimons ainsi la variabilité du taux de détection.Dans le cadre cohérent de la simulation, nous calculons les signaux d'annihilation et de désintégration de MN en rayons gamma ainsi que le fond diffus, que nous modélisons en utilisant les explosions de supernovae comme sources de rayons cosmiques qui produisent les rayons gamma par spallation sur la distribution de gaz. Les configurations de la matière noire et des baryons induisent une situation défavorable à la détection indirecte de la MN. / The thesis tackles two topics: the formation of spiral galaxies and the detection of dark matter (DM).We study three high resolution cosmological hydrodynamical simulations of Milky Way-sized halos including a comparison with the corresponding DM-only runs performed with the code RAMSES. We analyze the stellar and gas distribution and find one of our simulated galaxies with interesting Milky Way like features with regard to several observational tests. We obtain an extended disk and a flat rotation curve with a circular velocity and a DM density in the solar neighborhood that are in agreement with observations. Following observational procedures, we rederive the stellar-to-halo mass ratio and obtain competitive values for this criterion. Concerning the DM distribution, we explicitly show the interaction with the baryons and show how the DM is first contracted by star formation and then cored by feedback processes.In the framework of the simulation, we analyze the astrophysical uncertainties relevant for direct detection by studying the involved quantities like the local DM density, the DM velocity distribution and the local escape velocity . Furthermore, we consider various selections of DM and star distributions and estimate the variability of the detection rate.Within the self-consistent framework of the simulation, we calculate the DM annihilation and decay gamma ray (GR) signals as well as the diffuse GR background, that we model using the supernovae explosions as cosmic ray sources which produce GRs by spallation on the gas distribution. The cored DM profile and the high central baryonic densities induce a challenging configuration for indirect DM detection.

When studying astrophysical structures with sizes ranging from dwarf galaxies to galaxy clusters, it becomes clear that there are vast amounts of unobservable gravitating mass. A compelling hypothesis is that this missing mass, which we call dark matter, consists of elementary particles that can be described in the same manner as those of the standard model of particle physics. This thesis is dedicated to the study of particle dark matter in astrophysical systems. The solar composition problem refers to the current mismatch between theoretical predictions and observations of the solar convection zone depth and sound speed profile. It has been shown that heat transfer by dark matter in the Sun may cool the solar core and alleviate the problem. We discuss solar capture of a self-interacting Dirac fermion dark matter candidate and show that, even though particles and antiparticles annihilate, the abundance of such a particle may be large enough to influence solar physics. Currently, direct and indirect methods are employed in searches for dark matter. In this context, we study inelastic dark matter, where a small mass splitting separates two dark matter particles and scattering takes one into the other. This affects the scattering kinematics, which in turn affects direct detection and solar capture rates. We also discuss the information contained in a direct detection signal and how it can be used to infer a minimal solar capture rate of dark matter. When comparing simulated dark matter halos with collisionless dark matter with dark matter halos inferred from observations, problems appear in the smallest structures. A proposed solution is self-interacting dark matter with long range forces. As the simplest models are under severe constraints, we study self-interactions in a model of inelastic dark matter. / <p>QC 20170309</p>

Bandlimited optical intensity channels, arising in applications such as indoor infrared communications and visible light communications (VLC), require that all signals satisfy a bandwidth constraint as well as average, peak and non-negative amplitude constraints. However, the signaling designed for conventional radio frequency (RF) electrical channels cannot be applied directly, since they take energy constraints into consideration instead of amplitude constraints. In addition, conventional transmission techniques optimized for broad-band optical channels such as fiber optics, terrestrial/satellite-to-satellite free-space optical (FSO) communications are typically not bandwidth efficient. In this thesis, a two-dimensional signal space for bandlimited optical intensity channels is presented. A novel feature of this model is that the non-negativity and peak amplitude constraints are relaxed. The signal space parameterizes the likelihood of a negative or peak amplitude excursions in the output. Although the intensity channel only supports non-negative amplitudes, the impact of clipping on system performance is shown to be negligible if the likelihood of negative amplitude excursion is small enough. For a given signal space, a tractable approximation approach using a finite series is applied to accurately compute the likelihood of clipping under average and peak optical power constraints. The uncoded asymptotic optical power and spectral efficiencies using two-dimensional lattice constellations are computed. The Monte-Carlo (MC) simulation results show that for a given average or peak optical power, schemes designed in the presented signal space haver higher spectral efficiency than M-ary pulse amplitude modulation (PAM) using previously established techniques. / Thesis / Master of Applied Science (MASc)

Le Modèle Standard de la physique des particules est une théorie robuste à l'échelle électro-faible. Cependant, ce dernier possède des lacunes. Par exemple il ne permet pas d'expliquer la matière sombre, qui est une des problématiques majeures de la physique moderne. Près de 85% de la matière présente dans l'Univers n'est pas expliquée par le Modèle Standard. On l’appelle la matière sombre. Cette thèse présente une catégorie de modèles s'adressant à la problématique de la matière sombre. Ceux-ci s'appuient sur le paradigme du WIMP, qui nous enseigne qu'une particule neutre avec une section efficace électro-faible et une masse électro-faible explique à peu près l'abondance relique observée. Néanmoins, une analyse plus approfondie révèle que cette correspondance n'est en fait pas très précise puisque des masses multi-TeV pour la matière sombre sont nécessaires pour les modèles les plus simples, ce qui est 1-2 ordres de grandeur plus grand que l’échelle électro-faible. Cependant, avec un secteur sombre étendu, il est possible de maintenir la masse de la matière sombre proche de l’échelle électro-faible tout en gardant la densité relique observée. Ma thèse présente des modèles effectifs simples de matière sombre fermionique du type WIMP, ou le candidat de matière sombre est issu du mélange entre un singlet du Modèle Standard et d'un n-plet de SU(2)×U(1). La particule de matière sombre est supposée avoir une masse de l'ordre de l'échelle électro-faible, et le mélange est généré par des opérateurs de dimensions supérieures impliquant le doublet de Higgs. Lorsque la symétrie électro-faible est brisée, le boson de Higgs acquiert sa valeur moyenne dans le vide et des matrices de masse non-diagonales sont générées dans le secteur sombre. Cela engendre un mélange entre les états du secteur sombre, et les états physiques ainsi que leur masse sont obtenus en diagonalisant les matrices de masse. Pour des valeurs appropriées des paramètres, il est toujours possible d’accommoder le mélange afin de reproduire la densité relique mesurée. On parle de "well-tempered mixing" ou mélange correctement ajusté en français. Afin de stabiliser la particule de matière sombre, on doit ajouter une symétrie sous laquelle le secteur sombre est impair et le Modèle Standard est pair. Pour n impair, le n-plet est un multiplet de Majorana d'hypercharge nulle. Pour n pair, on considère un bi-multiplet d'hypercharge opposée ± 1/2 de sorte à ce qu'il forme un spineur de Dirac. On se focalise sur les contraintes liées à la densité relique et à la détection directe pour les configurations singlet-triplet, singlet-quadruplet et singlet-quintuplet. Notons que les contraintes de la détection indirecte sont moins fortes que celles issues de la détection directe. On impose une masse électro-faible pour la matière sombre afin qu'elle puisse être produite au LHC. Les résultats montrent qu'il est toujours possible de trouver un espace des paramètres, avec une masse électro-faible pour la matière sombre et redonnant la densité relique observée, qui passe les contraintes de détection directe et a fortiori indirecte. Dans la région de validité de la théorie effective, la détection directe est moins contraignante pour les grandes représentations du n-plet à cause du très faible mélange. / The Standard Model of particles physics is a well-tested theory at the electroweak scale. However this is not the end of the story. For instance, it does not solve the dark matter problem, which is one of the major issues of the modern physics. About 85% of the matter in the Universe is not describe by the Standard Model. It is called dark matter. This thesis presents a category of models responding to the dark matter problem. These models are based on the WIMP-paradigm, stating that a neutral particle with an electroweak cross-section and with an electroweak-scale mass roughly explains the observed relic abundance. Nevertheless, a closer look reveals that this correspondence is quantitatively not very precise since multi-TeV dark matter masses are required for the simplest models, which is 1-2 orders of magnitude larger than the electroweak scale. However, with an extended dark sector, it is possible to maintain the dark matter particle mass close to the electroweak scale and to keep the observed relic density. My thesis discloses simple effective models of fermionic WIMP dark matter, where the dark matter candidate is a mixture of a Standard Model singlet and an n-plet of SU(2)×U(1). The dark matter is assumed to be aroundthe electroweak scale, and the mixing is generated by higher-dimensional operators involving the Higgs doublet. Upon electroweak symmetry breaking, the Higgs takes its vacuum expectation value and non diagonal mass matrices are generated for the dark matter sector. This causes mixing between dark matter sector states, and physical states and masses are obtained by diagonalising the mass matrices. For suitable parameters, it is always possible to adjust the mixing to reproduce the observed relic density. This is reffered to as a well-tempered mixing. In order to stabilise the dark matter particle, we need to add a discrete symmetry under which the dark matter sector is odd and the Standard Model is even. For n odd, the n-plet is a Majorana multiplet with zero hypercharge. For n even, we consider a bi-multiplet with opposite hypercharges of ± 1/2 such as to form a Dirac spinor. We focus on the observed relic density and the direct detection constraints for the singlet-triplet, singlet-quadruplet and singlet-quintuplet configurations. Note that bounds from indirect detection are less stringent than those from direct detection. We impose electroweak mass for the dark matter particle such that it could be produced by the LHC. Results show that it is always possible to find a choice of parameters reproducing the observed relic density with an electroweak dark matter mass which conforms to the direct and a fortiori indirect detection constraints. In the region of validity of the effective theory, direct detection is less constraining for higher representations of the n-plet due to the tiny mixing.

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.