In dieser Dissertation werden Daten aus drei Jahren vom vollständig fertiggestellten IceCube-Detektor benutzt um nach Neutrinos zu suchen, die in Dunkle-Materie-Annihilationen in fünf nahegelegen Zwerggalaxien, der M31 Galaxie und dem Virgo Galaxienhaufen produziert wurden. Um die Messung durchzuführen, wurde zunächst eine Ereignis-Selektion angewandt, die es ermöglicht, die von aus der Atmosphäre stammenden Teilchen dominierte Rate der Ereignisse von zirka 100 Hz auf 0.5 mHz zu reduzieren. Danach wird eine Maximum-Likelihood-Schätzer eingesetzt um zu bestimmen ob es ein Überschuss von Neutrinos aus der Richtung der jeweiligen Quellen gibt, der mit einen Energie-Spektrum übereinstimmt das mann für Dunkle-Materie-Annihilationen erwartet. Für die M31 Galaxie und den Virgo Galaxienhaufen wurde zusätzlich zu dieser Suche nach einer Punktquelle auch eine Suche für ein erweitertes Signal durchgeführt. In allen untersuchten Fällen ist das Ergebnis der Analyse vereinbar mit einer Messung der Hintergrund-Hypothese, und daraus wurden Limits für den über die Geschwindigkeit gemittelten Wirkungsquerschnitt für Dunkle-Materie-Annihilation für verschiedene Endprodukte bestimmt. Für hohe Dunkle-Materie-Massen gibt es ein Überschuss von Neutrinos aus drei der Zwerggalaxien. Dieser Überschuss hat einen globalen p-Wert von 4.9% und ist damit nicht statistisch signifikant. Die Suche für ein erweitertes Signal von der M31 Galaxie und dem Virgo Galaxienhaufen ergab keinen Überschuss. Die Limits auf den über die Geschwindigkeit gemittelten Wirkungsquerschnitt für Dunkle-Materie-Annihilation haben sich im Vergleich zu vorherigen IceCube-Analysen signifikant verbessert, um bis zu einer Größenordnung. Diese ist teilweise auf Grund Verbesserungen für diese Analyse besonders: eine verbesserte Ereignis-Selektion, und für die Analyse ist eine Maximum-Likelihood-Schätzer eingesetzt statt eine Analyse in ein Suchfenster. / In this thesis, three years worth of data from the completed IceCube detector is used to search for neutrinos produced in dark matter annihilations in five nearby dwarf galaxies, the M31 galaxy and the Virgo cluster. To do this, an event selection which was developed for this analysis is applied to the data sample to reduce the atmospheric background rate from approximately 100 Hz to less than 0.5 mHz. Then, an unbinned maximum likelihood method is used to determine whether there is an excess of neutrinos from the direction of the considered galaxies or galaxy cluster that has an energy spectrum that matches the spectrum expected from dark matter annihilations. For the M31 galaxy and the Virgo cluster an extended signal with a two-dimensional Gaussian shape and width up to 5 degrees is also considered. In all cases, the results of the analysis are compatible with the background-only hypothesis and limits are set on the velocity-averaged dark matter annihilation cross section for different annihilation channels. For high dark matter masses there is an excess of neutrinos from three of the five dwarf galaxies. This excess has a global p-value of 4.9%, so it is not statistically significant. The search for an extended emission from the direction of the M31 galaxy and the Virgo cluster also did not result in an excess: in both cases the global p-value is larger than 50%. The limits on the velocity-averaged dark matter annihilation cross section have improved significantly (up to an order of magnitude) with respect to the previous IceCube analysis considering these same targets. This is partially due to improvements to this analysis specifically: an improved event selection was used to select the final data sample and an unbinned maximum likelihood method was used for the final analysis instead of a binned analysis method.

A new formalism is presented for calculating the mean intensity spectrum and angular power spectrum of gamma-rays or neutrinos from extragalactic annihilating dark matter, taking into account the dependence of the relative motions of the annihilating particles on the annihilation cross section. To model the large scale dark matter distribution of mass and relative velocities, the halo distribution model is comprehensively summarized, and extended to include a universal radial profile of the particles' velocity variance, based on results from N-body computer simulations of dark matter halos. A velocity variance profile, associated with the NFW density profile, is proposed by enforcing a power-law profile of the pseudo phase-space density. This allows the large-scale velocity distribution to be described by virialized, gravitationally bound dark matter halos, as opposed to thermal motions used to describe the velocity distribution in the early Universe. The recent particle motion history of the Universe is presented for the described model. Sample extragalactic gamma-ray intensities from dark matter annihilation are shown for dark matter annihilating with p-wave, according to a relative-velocity-weighted annihilation cross section sigmav = a + bv^2, for constants a and b, with examples taken from supersymmetric models. For thermally produced dark matter, the p-wave suppresses the signal intensity. If b/a > 10^6, the p-wave hardens the intensity spectrum by an estimated factor of 1 + (6b/a)delta_I (E_gamma), and increases the angular power spectrum by a factor also depending on new coefficients (delta_Cl)^(1) (E_gamma ) and (delta_Cl)^(2) (E_gamma ). The energy-dependence of the new p-wave coefficients delta_I , (delta_Cl)^(1) (E_gamma ), and (delta_Cl)^(2) (E_gamma ) are shown for various annihilation spectra. Sample intensity spectra are also presented for Sommerfeld-enhanced annihilation. The intensity of neutrinos from dark matter annihilation is also considered. The variations between the dark matter annihilation signals for different particle phenomenologies suggest that particle physics constraints are possible from an observed indirect detection signal. Calculations of the annihilation signal from the galactic halo are also shown. The extragalactic signal's intensity is found to be consistent in magnitude with the galactic intensity?within the uncertainty of the models of the dark matter distribution?when looking out from the galactic plane. This suggests that the total cosmic signal may have significant contributions from both components.

Made available in DSpace on 2015-05-14T12:14:07Z (GMT). No. of bitstreams: 1 arquivototal.pdf: 9808595 bytes, checksum: 235eec9737496afa4dfbdf1feafbc21f (MD5) Previous issue date: 2013-02-04 / Coordenação de Aperfeiçoamento de Pessoal de Nível Superior - CAPES / The Dark matter (DM) problem constitutes a key question at the interface among Particle Physics, Astrophysics and Cosmology. The observational data which have been accumulated in the last years point to an existence of non baryonic amount of DM. Since the Standard Model (SM) does not provide any candidate for such non-baryonic DM, the evidence of DM is a major indication for new physics beyond the SM. We will study in this work one of the most popular DM candidates, the so called WIMPs (Weakly Interacting Massive Particles) from a direct and indirect detection perspective. In order to approach the direct and indirect dection of DM in the context of Particle Physics in a more pedagogic way, we will begin our discussion talking about a minimal extension of the SM. Later we will work on the subject in a 3-3-1 model. Next, we will study the role of WIMPs in the Big Bang Nucleosynthesis. Lastly, we will look for indirect signals of DM, by looking for gamma-ray excess observed by the NASA Satelite, called Fermi-LAT, in the Galactic Center. Through an analyses of the data events observed by Fermi-LAT and some background models, we will constrain the annihilation cross section-mass relation. As a result of this PhD 9 articles have been done. Two of them are still under the publication process. / O problema da matéria escura (ME) constitui uma questão chave na interface entre física de partículas, astrofísica e cosmologia. O acúmulo de dados observacionais nos últimos anos apontam para uma enorme quantidade de ME não bariônica. Uma vez que o Modelo Padrão (MP), não fornece um candidato para este tipo de matéria, a evidência de ME é uma forte indicação de física nova, além do MP. Estudaremos neste trabalho um dos candidatos à ME mais populares, os chamados WIMPS (partículas massivas que interagem fracamente) sob o ponto de vista de detecção direta e indireta de ME. Para que possamos abordar os meios de detecção direta e indireta de ME no contexto de Física de Partículas de forma didática, iniciaremos nossa discussão apresentando uma extensão mínima do MP. Posteriormente trataremos do assunto no contexto de um modelo 3-3-1. Adiante verificaremos qual o papel da ME no cenário da Nucleossíntese Primordial. Por ´ultimo procuraremos por sinais indiretos de ME, na busca por excessos em raios gama observados pelo satélite da NASA, chamado Fermi-LAT, no centro da nossa galáxia. Através de uma análise dos eventos observados pelo Fermi-LAT e de alguns modelos de background astrofísico iremos impor vínculos com relação à massa e seção de choque de aniquilação. Ao longo desse doutorado foram publicados 9 artigos. Um destes ainda sob o processo de publicação.

Made available in DSpace on 2015-05-14T12:14:15Z (GMT). No. of bitstreams: 1 arquivototal.pdf: 4811188 bytes, checksum: e6a9d4d69f963d42f294d99b19a7c9fb (MD5) Previous issue date: 2014-07-30 / Coordenação de Aperfeiçoamento de Pessoal de Nível Superior - CAPES / Dark Matter (DM) is a key piece for our understanding of the universe evolution. Its existence has been confirmed by gravitational effects on the known matter, and we do not know its constitution just yet. The assumption that DM is composed of particles demands an extension of the Standard Model of Elementary Particles (SM). There are many experiments searching for neutral, stable, weakly interacting particles so called WIMPs, but no conclusive positive signal has been observed so far. That being said, we propose a Majorana fermion to be our DM candidate in one of the simplest minimal extensions of the SM, which adds to the scalar sector a neutral scalar that mixes to the Higgs boson. Further, we study another model which supplements the former by adding a charged scalar, which mediates interactions between the DM particle and leptons. In both models, we compute the relic density, the scattering cross section off nucleon (Direct Detection), and its annihilation rate in Standard Model particles (Indirect Detection) using the numerical package micrOMEGAs. In conclusion, we interestingly find that such models have regions of the parameter space yielding the right abundance while compatible with direct and indirect detection limits. Lastly, we investigate the possibility having the Majoron risen in our extensions as dark radiation in the light of the recent CMB spectrum analyses. / A Matéria Escura (ME) é uma peça fundamental para nosso entendimento sobre a evolução do universo. Sua existência foi confirmada pelos efeitos gravitacionais que exerce sobre a matéria que conhecemos e até hoje não sabemos sua constituição. Assumir que ela seja constituída de partículas implica na necessidade de estender o Modelo Padrão das Partículas Elementares (MP). Há vários experimentos buscando partículas neutras, estáveis e pouco interagentes conhecidas como WIMPs, mas até agora nenhum sinal positivo é conclusivo. Em vista disso, propomos um férmion de Majorana como candidato à ME em uma das extensões mais simples do MP, adicionando ao setor escalar um escalar neutro singleto que se mistura com o bóson de Higgs. Em seguida, estudamos outro modelo que acrescenta ao anterior um escalar carregado singleto mediando interações entre as partículas de ME e os léptons. Nos dois modelos, computamos a abundância relíquia, a seção de choque de espalhamento com nucleons (detecção direta) e a taxa de aniquilação de ME em partículas do MP (detecção indireta) usando o pacote numérico micrOMEGAs. Em conclusão, mostramos que esses modelos têm uma interessante região de parâmetros que fornece a abundância relíquia correta estando de acordo com os limites das detecções direta e indireta. Finalmente, investigamos a possibilidade de o majoron que aparece em nossas extensões ser radiação escura, à luz de recentes análises do espectro da radiação CMB.

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.

Cette étude porte sur l'impact des fuites de CO2 provenant d'un réservoir géologique de stockage de CO2 sur un aquifère d'eau douce. Elle se distingue des autres études, réalisées sur le même thème, par la recherche et l'application, depuis l'échelle du laboratoire jusqu'à celle d'un site pilote, de nouveaux outils de monitoring et d'approche isotopique destinés à la détection précoce de fuite de CO2. Afin de tester ces outils, des échantillons solides et liquides provenant de l'aquifèrestratégique de l'Albien du Bassin de Paris ont été prélevés, analysés et utilisés pour une étude expérimentale en batch. Cette expérience permet de contraindre et de comprendre précisément les interactions eau-roche-CO2 et les réponses isotopiques. Une application grandeur nature en Norvège a permis de mettre en place ce programme isotopique et de suivre l'évolution de la composition isotopique en distinguant les processus et phénomènes naturels et les processus reliés à l'injection de CO2. Ces deux cas d'étude appliqués au contexte de détection de fuite de CO2 ont permis de choisir les outils isotopiques les meilleurs comme indicateurs indirects de la présence de CO2, dans le cas particulier des systèmes étudiés. L'efficience de ces outils isotopiques réside dans l'enregistrement de la trace laissée par la présence de CO2 au cours d'interactions eau/roche/CO2. L'utilisation de tels outils nécessite une méthodologie rigoureuse abordée dans ce manuscrit et nécessite d'être adaptée aux spécificités des sites envisagés. / This study deals with the impact of CO2 leakages out of geological storage into overlying freshwater aquifers. Compared to other existing studies, the major added value of this study lies, on the one hand, in the research of new monitoring tools and isotopic approach in the context of CCS aiming at early and sensitive detection of CO2 leakage and, on the other hand, in the application of these tools at the (limited) laboratory scale as well as at field scale. In order to test these tools, solid and liquid materials were sampled out of the major strategic drinking water Albian aquifer in the Paris Basin (France). We have then precisely characterized and used them within a batch experiment. This experiment yields interesting results which help understanding and constraining precisely the water-rock-CO2 interactions as well as the isotopic responses. A real scale application of the method was then performed in Norway. It was an opportunity to develop this isotopic program and to track the isotopic evolution composition, while differentiating the natural processes and the system response tothe CO2 injection. When applied to the detection of CO2 leakage context, the two case studies open the way for choosing the “best” isotopic tools as indirect indicators of CO2 presence in these specific systems. The efficiency of these isotopic tools comes from the recording of the CO2 footprint all along the water-rock-CO2 interactions. Using such tools imposes a rigorous methodology, which is tackled inthis manuscript. Furthermore, future application will require adapting to the specifics of a proposed site.

Die vorliegende Arbeit beschreibt einen semi-analytischen Ansatz zur Modellierung der Dichteverteilung von DM im Galaktischen Halo. Aus den verschiedenen Substrukturmodellen wird die γ-Strahlungsintensität, welche die Erde erreicht, berechnet. Eine Spannbreite plausibler γ-Strahlungsintensitäten aufgrund der Paarvernichtung Galaktischer DM wird vorgeschlagen, welche die Vorhersagen verschiedener früherer Studien umfasst, und es werden die durchschnittlichen Massen, Abstände und ausgedehnten Strahlungsprofile der γ-strahlungsintensivsten DM-Verdichtungen berechnet. Schließlich werden die DM-Modelle für eine umfassende Berechnung der Nachweismöglichkeit Galaktischer Substrukturen mit CTA verwendet. Die instrumentelle Sensitivität zum Nachweis der γ-strahlungsintensivsten DM-Substruktur wird für eine mit CTA geplanten großflächigen Himmelsdurchmusterung außerhalb der Galaktischen Ebene berechnet. Die Berechnung wird mit CTA Analyse- Software und einer Methode durchgeführt, welche auf einer Likelihood beruht. Eine alternative, ebenfalls Likelihood-basierte Analysemethode wird entwickelt, mit welcher DM-Substrukturen als äumliche Anisotropien im Multipolspektrum des Datensatzes einer Himmelsdurchmusterung nachgewiesen werden können. Die Analysen ergeben, dass eine Himmelsdurchmusterung mit CTA und eine anschließende Suche nach γ-Strahlung von DM-Substrukturen Wirkungsquerschnitte für eine Paarvernichtung in der Größenordnung von (σv) > 1 × 10−24 cm3 s−1 für eine DM-Teilchenmasse von mχ ∼ 500 GeV auf einem Vertrauensniveau von 95% ausschließen kann. Diese Sensitivität ist vergleichbar mit Langzeitbeobachtungen einzelner Zwerggalaxien mit CTA. Eine modellunabhängige Analyse ergibt, dass eine Himmelsdurchmusterung mit CTA Anisotropien im diffusen γ-Strahlungshintergrund oberhalb von 100 GeV für relative Schwankungen von CPF > 10−2 nachweisen kann. / In the current understanding of structure formation in the Universe, the Milky Way is embedded in a clumpy halo of dark matter (DM). Regions of high DM density are expected to emit enhanced γ-radiation from the DM relic annihilation. This γ-radiation can possibly be detected by γ-ray observatories on Earth, like the forthcoming Cherenkov Telescope Array (CTA). This dissertation presents a semi-analytical density modeling of the subclustered Milky Way DM halo, and the γ-ray intensity at Earth from DM annihilation in Galactic subclumps is calculated for various substructure models. It is shown that the modeling approach is able to reproduce the γ-ray intensities obtained from extensive dynamical DM simulations, and that it is consistent with the DM properties derived from optical observations of dwarf spheroidal galaxies. A systematic confidence margin of plausible γ-ray intensities from Galactic DM annihilation is estimated, encompassing a variety of previous findings. The average distances, masses, and extended emission profiles of the γ-ray-brightest DM clumps are calculated. The DM substructure models are then used to draw reliable predictions for detecting Galactic DM density clumps with CTA, using the most recent benchmark calculations for the performance of the instrument. A Likelihood-based calculation with CTA analysis software is applied to find the instrumental sensitivity to detect the γ-ray-brightest DM clump in the projected CTA extragalactic survey. An alternative Likelihood-based analysis method is developed, to detect DM substructures as anisotropies in the angular power spectrum of the extragalactic survey data. The analyses predict that the CTA extragalactic survey will be able to probe annihilation cross sections of ⟨σv⟩ > 1 × 10−24 cm3 s−1 at the 95% confidence level for a DM particle mass of mχ ∼ 500 GeV from DM annihilation in substructures. This sensitivity is compatible with long-term observations of single dwarf spheroidal galaxies with CTA. Independent of a particular source model, it is found that the CTA extragalactic survey will be able to detect anisotropies in the diffuse γ-ray background above 100 GeV at a relative amplitude of CP_F > 10−2.