Дисертації з теми "Dark Matter - Astroparticle Physics"

The striking evidence for the existence of dark matter in the Universe implies that there is new physics to be discovered beyond the Standard Model. To identify the nature of this dark matter is a key task for modern astroparticle physics, and a large number of experiments pursuing a range of different search strategies have been developed to solve it. The topic of this thesis is the complementarity of these different experiments and the issue of how to combine the information from different searches independently of experimental and theoretical uncertainties. The first part focuses on the direct detection of dark matter scattering in nuclear recoil detectors, with a special emphasis on the impact of the assumed velocity distribution of Galactic dark matter particles. By converting experimental data to variables that make the astrophysical unknowns explicit, different experiments can be compared without implicit assumptions concerning the dark matter halo. We extend this framework to include annual modulation signals and apply it to recent experimental hints for dark matter, showing that the tension between these results and constraints from other experiments is independent of astrophysical uncertainties. We explore possible ways of ameliorating this tension by changing our assumptions on the properties of dark matter interactions. In this context, we propose a new approach for inferring the properties of the dark matter particle, which does not require any assumptions about the structure of the dark matter halo. A particularly interesting option is to study dark matter particles that couple differently to protons and neutrons (so-called isospin-violating dark matter). Such isospin-violation arises naturally in models where the vector mediator is the gauge boson of a new U(1) that mixes with the Standard Model gauge bosons. In the second part, we first discuss the case where both the Z' and the dark matter particle have a mass of a few GeV and then turn to the case where the Z' is significantly heavier. While the former case is most strongly constrained by precision measurements from LEP and B-factories, the latter scenario can be probed with great sensitivity at the LHC using monojet and monophoton searches, as well as searches for resonances in dijet, dilepton and diboson final states. Finally, we study models of dark matter where loop contributions are important for a comparison of LHC searches and direct detection experiments. This is the case for dark matter interactions with Yukawa-like couplings to quarks and for interactions that lead to spin-dependent or momentum suppressed scattering cross sections at tree level. We find that including the contribution from heavy-quark loops can significantly alter the conclusions obtained from a tree-level analysis.

Diss. (sammanfattning) Stockholm : Stockholms universitet, 2010.
At the time of the doctoral defense, the following papers were unpublished and had a status as follows: Paper 5: Accepted. Paper 6: Submitted. Härtill 6 uppsatser.

While the dark matter has so far only revealed itself through the gravitational influence it exerts on its surroundings, there are good reasons to believe it is made up by WIMPs – a hypothetical class of heavy elementary particles not encompassed by the Standard Model of particle physics. The Inert Doublet Model constitutes a simple extension of the Standard Model Higgs sector. The model provides a new set of scalar particles, denoted inert scalars because of their lack of direct coupling to matter, of which the lightest is a WIMP dark matter candidate. Another popular Standard Model extension is that of supersymmetry. In the most minimal scenario the particle content is roughly doubled, and the lightest of the new supersymmetric particles, which typically is a neutralino, is a WIMP dark matter candidate. In this thesis the phenomenology of inert scalar and supersymmetric dark matter is studied. Relic density calculations are performed, and experimental signatures in indirect detection experiments and accelerator searches are derived. The Inert Doublet Model shows promising prospects for indirect detection of dark matter annihilations into monochromatic photons. It is also constrained by the old LEP II accelerator data. Some phenomenological differences between the Minimal Supersymmetric Standard Model and a slight extension, the Beyond the Minimal Supersymmetric Standard Model, can be found. Also, supersymmetric dark matter models can be detected already within the early LHC accelerator data.

Dark matter particles in the form of supersymmetric Weakly Interacting Massive Particles (WIMPs) could accumulate in the centre of the Sun because of gravitational trapping. Pair-wise annihilations of WIMPs could create standard model particles out of which neutrinos could reach the Earth. Data from the IceCube 22-string neutrino telescope have been searched for signals from dark matter annihilations in the Sun. Highly sophisticated analysis methods have been developed to discern signal neutrinos from the severe background of atmospheric particle showers. No signal has been found in a dataset of 104 days livetime taken in 2007, and an upper limit has been placed on the muon flux in the South Pole ice induced by neutrinos from the Sun, reaching down to 330 km-2y-1. The flux limit has been converted into an upper limit on the neutralino scattering cross-section, which reaches down to 2.8*10-40 cm2 for spin-dependent interactions.
Four articles are appended to the thesis:I. G. Wikström for the IceCube collaboration, Proc. of the 30th ICRC,arXiv/0711.0353 [astro-ph] (2007) 135.II. A. Gross, C. Ha, C. Rott, M. Tluczykont, E. Resconi, T. DeYoung and G. Wikström for the IceCube Collaboration, Proc. of the 30th ICRC,arXiv/0711.0353 [astro-ph] (2007) 11.III. G. Wikström and J. Edsjö, JCAP 04 (2009) 009.IV. R. Abbasi et al. (IceCube collaboration), accepted for publication in Phys. Rev. Lett., arXiv/0902.2460v3 [astro-ph.CO] (2009).
IceCube

Weak-scale supersymmetry is one of the most favoured theories beyond the Standard Model of particle physics that elegantly solves various theoretical and observational problems in both particle physics and cosmology. In this thesis, I describe the theoretical foundations of supersymmetry, issues that it can address and concrete supersymmetric models that are widely used in phenomenological studies. I discuss how the predictions of supersymmetric models may be compared with observational data from both colliders and cosmology. I show why constraints on supersymmetric parameters by direct and indirect searches of particle dark matter are of particular interest in this respect. Gamma-ray observations of astrophysical sources, in particular dwarf spheroidal galaxies, by the Fermi satellite, and recording nuclear recoil events and energies by future ton-scale direct detection experiments are shown to provide powerful tools in searches for supersymmetric dark matter and estimating supersymmetric parameters. I discuss some major statistical issues in supersymmetric global fits to experimental data. In particular, I further demonstrate that existing advanced scanning techniques may fail in correctly mapping the statistical properties of the parameter spaces even for the simplest supersymmetric models. Complementary scanning methods based on Genetic Algorithms are proposed.
At the time of the doctoral defense, the following paper was unpublished and had a status as follows: Paper 4: Submitted.

Dark matter (DM) constitutes one of the most intriguing but so far unresolved issues in physics. In many extensions of the Standard Model of particle physics, the existence of a stable Weakly Interacting Massive Particle (WIMP) is predicted. The WIMP is an excellent DM particle candidate. One of the most interesting scenarios is the creation of monochromatic gamma-rays from the annihilation or decay of these particles. This type of signal would represent a “smoking gun” for DM, since no other known astrophysical process should be able to produce it. In this thesis, the search for spectral lines with the Large Area Telescope (LAT) onboard the Fermi Gamma-ray Space Telescope (Fermi) is presented. The satellite was successfully launched from Cape Canaveral in Florida, USA, on 11 June, 2008. The energy resolution and performance of the detector are both key factors in the search and are investigated here using beam test data, taken at CERN in 2006 with a scaled-down version of the Fermi-LAT instrument. A variety of statistical methods, based on both hypothesis tests and confidence interval calculations, are then reviewed and tested in terms of their statistical power and coverage. A selection of the statistical methods are further developed into peak finding algorithms and applied to a simulated data set called obssim2, which corresponds to one year of observations with the Fermi-LAT instrument, and to almost one year of Fermi-LAT data in the energy range 20–300 GeV. The analysis on Fermi-LAT data yielded no detection of spectral lines, so limits are placed on the velocity-averaged cross-section, , and the decay lifetime, , and theoretical implications are discussed.
QC20100525
GLAST

Despite striking evidence for the existence of dark matter from astrophysical observations, dark matter has still escaped any direct or indirect detection until today. Therefore a proof for its existence and the revelation of its nature belongs to one of the most intriguing challenges of nowadays cosmology and particle physics. The present work tries to investigate the nature of dark matter through indirect signatures from dark matter annihilation into electron-positron pairs in two different ways, pressure from dark matter annihilation and multi-messenger constraints on the dark matter annihilation cross-section. We focus on dark matter annihilation into electron-positron pairs and adopt a model-independent approach, where all the electrons and positrons are injected with the same initial energy E_0 ~ m_dm*c^2. The propagation of these particles is determined by solving the diffusion-loss equation, considering inverse Compton scattering, synchrotron radiation, Coulomb collisions, bremsstrahlung, and ionization. The first part of this work, focusing on pressure from dark matter annihilation, demonstrates that dark matter annihilation into electron-positron pairs may affect the observed rotation curve by a significant amount. The injection rate of this calculation is constrained by INTEGRAL, Fermi, and H.E.S.S. data. The pressure of the relativistic electron-positron gas is computed from the energy spectrum predicted by the diffusion-loss equation. For values of the gas density and magnetic field that are representative of the Milky Way, it is estimated that the pressure gradients are strong enough to balance gravity in the central parts if E_0 < 1 GeV. The exact value depends somewhat on the astrophysical parameters, and it changes dramatically with the slope of the dark matter density profile. For very steep slopes, as those expected from adiabatic contraction, the rotation curves of spiral galaxies would be affected on kiloparsec scales for most values of E_0. By comparing the predicted rotation curves with observations of dwarf and low surface brightness galaxies, we show that the pressure from dark matter annihilation may improve the agreement between theory and observations in some cases, but it also imposes severe constraints on the model parameters (most notably, the inner slope of the halo density profile, as well as the mass and the annihilation cross-section of dark matter particles into electron-positron pairs). In the second part, upper limits on the dark matter annihilation cross-section into electron-positron pairs are obtained by combining observed data at different wavelengths (from Haslam, WMAP, and Fermi all-sky intensity maps) with recent measurements of the electron and positron spectra in the solar neighbourhood by PAMELA, Fermi, and H.E.S.S.. We consider synchrotron emission in the radio and microwave bands, as well as inverse Compton scattering and final-state radiation at gamma-ray energies. For most values of the model parameters, the tightest constraints are imposed by the local positron spectrum and synchrotron emission from the central regions of the Galaxy. According to our results, the annihilation cross-section should not be higher than the canonical value for a thermal relic if the mass of the dark matter candidate is smaller than a few GeV. In addition, we also derive a stringent upper limit on the inner logarithmic slope α of the density profile of the Milky Way dark matter halo (α < 1 if m_dm < 5 GeV, α < 1.3 if m_dm < 100 GeV and α < 1.5 if m_dm < 2 TeV) assuming a dark matter annihilation cross-section into electron-positron pairs (σv) = 3*10^−26 cm^3 s^−1, as predicted for thermal relics from the big bang.
Trotz vieler Hinweise auf die Existenz von dunkler Materie durch astrophysikalische Beobachtungen hat sich die dunkle Materie bis heute einem direkten oder indirekten Nachweis entzogen. Daher gehrt der Nachweis ihrer Existenz und die Enthüllung ihrer Natur zu einem der faszinierensten Herausforderungen der heutigen Kosmologie und Teilchenphysik. Diese Arbeit versucht die Natur von dunkler Materie durch indirekte Signaturen von der Paarzerstrahlung dunkler Materie in Elektron-Positronpaare auf zwei verschiedene Weisen zu untersuchen, nämlich anhand des Drucks durch die Paarzerstrahlung dunkler Materie und durch Grenzen des Wirkungsquerschnitts für die Paarzerstrahlung dunkler Materie aus verschiedenen Beobachtungsbereichen. Wir konzentrieren uns dabei auf die Zerstrahlung dunkler Materie in Elektron-Positron-Paare und betrachten einen modellunabhängigen Fall, bei dem alle Elektronen und Positronen mit der gleichen Anfangsenergie E_0 ~ m_dm*c^2 injiziert werden. Die Fortbewegung dieser Teilchen wird dabei bestimmt durch die Lösung der Diffusions-Verlust-Gleichung unter Berücksichtigung von inverser Compton-Streuung, Synchrotronstrahlung, Coulomb-Streuung, Bremsstrahlung und Ionisation. Der erste Teil dieser Arbeit zeigt, dass die Zerstrahlung dunkler Materie in Elektron-Positron-Paare die gemessene Rotationskurve signifikant beeinflussen kann. Die Produktionsrate ist dabei durch Daten von INTEGRAL, Fermi und H.E.S.S. begrenzt. Der Druck des relativistischen Elektron-Positron Gases wird aus dem Energiespektrum errechnet, welches durch die Diffusions-Verlust-Gleichung bestimmt ist. Für Werte der Gasdichte und des magnetischen Feldes, welche für unsere Galaxie repräsentativ sind, lässt sich abschätzen, dass für E_0 < 1 GeV die Druckgradienten stark genug sind, um Gravitationskräfte auszugleichen. Die genauen Werte hängen von den verwendeten astrophysikalischen Parametern ab, und sie ändern sich stark mit dem Anstieg des dunklen Materie-Profils. Für sehr große Anstiege, wie sie für adiabatische Kontraktion erwartet werden, werden die Rotationskurven von Spiralgalaxien auf Skalen von einegen Kiloparsek für die meisten Werte von E_0 beeinflusst. Durch Vergleich der erwarteten Rotationskurven mit Beobachtungen von Zwerggalaxien und Galaxien geringer Oberflächentemperatur zeigen wir, dass der Druck von Zerstrahlung dunkler Materie die Übereinstimmung von Theorie und Beobachtung in einigen Fällen verbessern kann. Aber daraus resultieren auch starke Grenzen für die Modellparameter - vor allem für den inneren Anstieg des Halo-Dichteprofils, sowie die Masse und den Wirkungsquerschnitt der dunklen Materie-Teilchen. Im zweiten Teil werden obere Grenzen für die Wirkungsquerschnitte der Zerstrahlung der dunkler Materie in Elektron-Positron-Paare erhalten, indem die beobachteten Daten bei unterschiedlichen Wellenlängen (von Haslam, WMAP und Fermi) mit aktuellen Messungen von Elektron-Positron Spektren in der solaren Nachbarschaft durch PAMELA, Fermi und H.E.S.S. kombiniert werden. Wir betrachten Synchrotronemission bei Radiound Mikrowellenfrequenzen, sowie inverse Compton-Streuung und Final-State-Strahlung bei Energien im Bereich der Gamma-Strahlung. Für die meisten Werte der Modellparameter werden die stärksten Schranken durch das lokale Positron-Spektrum und die Synchrotronemission im Zentrum unser Galaxie bestimmt. Nach diesen Ergebnissen sollte der Wirkungsquerschnitt für die Paarzerstrahlung nicht größer als der kanonische Wert für thermische Relikte sein, wenn die Masse der dunklen Materie-Kandidaten kleiner als einige GeV ist. Zusätzlich leiten wir eine obere Grenze für den inneren logarithmische Anstieg α des Dichteprofiles des dunklen Materie Halos unserer Galaxie ab.

La quête de la nouvelle physique est un défi impliquant à la fois la recherche de particules de matière noire dans les halos galactiques, et celle, aux collisonneurs, de particules dont l’existence est prédite par des théories au-delà du Modèle Standard, telles que la supersymétrie. Alors que les contraintes expérimentales sur ces particules s’intensifient, il devient capital de combiner les limites provenant de ces deux volets afin de guider la suite des recherches. Pour ce faire, il est indispensable d’évaluer et de tenir compte correctement des incertitudes astrophysiques, cosmologiques et nucléaires, pourtant souvent ignorées. La première partie de cette thèse est dédiée à l’étude de ces incertitudes et leur impact sur les contraintes obtenues en supersymétrie, ainsi que la complémentarité entre les contraintes des collisionneurs et de matière noire pour la recherche de nouvelle physique. La deuxième partie est consacrée au développement d’outils de calculs pour les détections directe et indirecte de matière noire, conçus afin de prendre correctement en compte les incertitudes astrophysiques et nucléaires, et à leur implémentation dans le code public SuperIso Relic. Enfin la troisième partie du travail concerne l’étude des implications cosmologiques d’une éventuelle découverte de nouvelles particules aux collisionneurs. Nous avons montré qu’il serait possible de tester les hypothèses du modèle cosmologique standard et d’obtenir des informations sur les propriétés de l’Univers primordial à une époque observationnellement inaccessible
The quest for new physics is a challenging task which involves, on the one hand, the search for dark matter particles from space, and on the other hand, the search at colliders for particles predicted by theories beyond the Standard Model, such as supersymmetry. With the experimental constraints on new particles getting stronger, it becomes crucial to combine the limits from both sectors in order to guide future searches. To this end, it is essential to estimate and take into account correctly the astrophysical, nuclear and cosmological uncertainties, which are most often ignored. The first part of this thesis is dedicated to the study of such uncertainties and to their impact on the constraints applied on supersymmetry. Moreover, we investigate the interplay between the constraints from colliders and dark matter searches in some detail. The second part concerns the development and the implementation in the public code SuperIso Relic of numerical tools for the calculation of direct and indirect dark matter detection constraints which were designed specifically to take correctly into account astrophysical and nuclear uncertainties. Finally, in the third part of this work, we consider the cosmological implications of a hypothetical discovery of new particles at colliders. We show that it would be possible to test the assumptions of the standard cosmological model and to obtain information on the properties of the primordial Universe at an epoch which is beyond observational reach

One of the greatest mysteries of the universe that, for the present, puzzles the mind of most astronomers, cosmologists and physicists is the question: "What makes up our universe?". This is due to how a certain substance named Dark Matter came under speculation. It is believed this enigmatic substance, of type unknown, accounts for almost three-quarters of the cosmos within the universe, could be the answer to several questions raised by the models of the expanding universe astronomers have created, and even decide the fate of the expansion of the universe. There is strong observational evidence for the dominance of non-baryonic Dark Matter (DM) over baryonic matter in the universe. Such evidence comes from many independent observations over different length scales. The most stringent constraint on the abundance of DM comes from the analysis of the Cosmic Microwave Background (CMB) anisotropies. In particular, the WMAP (Wilkinson Microwave Anisotropy Probe) experiment restricts the abundance of matter and the abundance of baryonic matter in good agreement with predictions from Big Bang Nucleosynthesis. It is commonly believed that such a non-baryonic component could consist of new, as yet undiscovered, particles, usually referred to as WIMPs (Weakly Interacting Massive Particles). Some extensions of the standard model (SM) of particle physics predict the existence of particles that would be excellent DM candidates. In particular great attention has been dedicated to candidates arising in supersymmetric theories: the Lightest Supersymmetric Particle (LSP). In the most supersymmetric scenarios, the so-called neutralino seems to be a natural candidate, being stable in theories with conservation of R-parity and having masses and cross sections of typical WIMPs. The EDELWEISS collaboration is a direct dark matter search experiment, aiming to detect directly a WIMP interaction in a target material, high purity germanium crystal working at cryogenic temperatures. It relies in the measurement of nuclear recoils that produce measurable effects in the crystal such ionization and heat. My PhD thesis is organized as follows. The first chapter aims to provide an introduction to the theoretical framework and the scientific motivation for the following work. The nature of DM has been one of the most challenging topics in contemporary physics since the first evidences of its existence had been found in the 1930s. Cosmologists and astrophysicists on one side, together with particle theorists on the other have put a lot of effort into this field: I will briefly account for their achievements and for the experimental strategies which can be set in this scenario. Since this thesis work was carried out within the EDELWEISS-II direct dark matter experiment, I will focus the next chapter on this topic, describing the main features. The second chapter is related to the set-up of the EDELWEISS-II, the current stage of the EDELWEISS experiment necessary after a first phase that achieved the best upper limit on the WIMP elastic scattering on nucleon as a function of WIMP mass in 2004. [....]

[EN] Neutrino astronomy is a booming field in astroparticle physics. Due to the particular characteristics of neutrinos, these particles offer great advantages as probes for the study of the far and high-energy Universe. It is extensively accepted by the scientific community that a multi-messenger approach with the combination of information provided by neutrinos, photons and charged particles (cosmic rays) is possible to obtain a more complete image of the fundamental astrophysics processes taking place in our Universe. Since neutrinos are neutral and very weak interacting particles they can reach the Earth from astrophysical sources without deflection by magnetic fields and almost without energy losses and absorption, contrarily to the rest of messengers. The other side of the coin of neutrino properties is that detection of neutrinos is very challenging and big highly instrumented detection volumes are needed. Natural media (deep sea, lakes or ice in the Antarctica) host this kind of experiments using the water (or ice) as target material where the neutrino interaction is produced. ANTARES is the first undersea neutrino telescope, located at 2475 m depth in the Mediterranean Sea. ANTARES is optimized for optical detection of the Cerenkov light induced by relativistic muons produced by high energy neutrino interactions near the detector. The charge, position and arrival time of the photons to the optical modules which compose the detector allows the muon track reconstruction, and thus, knowing the neutrino coming direction. Some information of the event energy is also derived. ANTARES is also hosting the AMADEUS experiment which is investigating the feasibility of the acoustic detection of Ultra-High Energy (UHE) neutrinos. The framework of this thesis is the ANTARES experiment. As commonly done in the thesis developed in this experiment (and in this field), the work has been divided in two different areas. On the one hand, a part more devoted to technological aspects related to the detector and, on the other hand, a part dedicated to ANTARES data analysis. The first part of the thesis is focused in the development of a calibrator able to reproduce the acoustic signal generated in the UHE neutrino interaction with a water nucleus which, roughly speaking, generates a highly directive bipolar acoustic pulse. Having a good calibrator is crucial to test and tune the telescope response for this kind of signals. The second part of the thesis, the data analysis part, is centred in the analysis of the ANTARES data in order to constrain possible Dark Matter models. This work is focused on the detection of products resulting of the Dark Matter annihilation trapped in the centre of the Sun. Specifically, the Secluded Dark Matter (SDM) model has been tested by the detection of di-muons (co-linear muon pair) and/or neutrinos coming from Sun direction. Broadly speaking, this model is based on the idea of the existence of a mediator resulting of the Dark Matter annihilation which, subsequently, would decay into standard model particles as muons or neutrinos. These models have been proposed in order to explain some experimental "anomalies" observed, such as the electron-positron ratio spectrum detected in satellites, measured recently with high accuracy by AMS-II. The study of this thesis constitutes the first search of experimental evidences of this kind of models in neutrino telescopes.
[ES] La astronomía de neutrinos es un campo en auge dentro de la Física de Astropartículas. Los neutrinos ofrecen grandes ventajas como sondas para estudiar el Universo lejano y de alta energía. Es extensamente aceptado que mediante la combinación de la información que proporcionan los neutrinos junto a la obtenida mediante fotones de alta energía (rayos gamma) y partículas cargadas (rayos cósmicos) se podría obtener una imagen más completa de los procesos astrofísicos fundamentales que tienen lugar a lo largo de nuestro Universo.La razón fundamental por la que los neutrinos son tan altamente valorados como mensajeros es la baja interacción con el medio que los rodea. Al ser partículas sin carga interactúan muy débilmente con la materia, por ello pueden escaparse de la fuente donde se han producido y, al contrario de lo que ocurre con el resto de mensajeros, pueden llegar a la Tierra sin ser desviados por los campo magnéticos y sin prácticamente pérdida de energía. Esta misma razón que los hace tan valorados es a su vez la que los hace tan difíciles de detectar. Se impone la necesidad de construir detectores de grandes volúmenes, del orden del km3, altamente instrumentados. Se utilizan medios naturales (en el fondo del mar, en lagos o en enterrados en el hielo de la Antártida) aprovechando el agua (o hielo) como material diana donde se espera que interaccione el neutrino. ANTARES es el primer telescopio submarino de neutrinos construido en el fondo del mar Mediterráneo. Está optimizado para la detección óptica de la luz Cherenkov inducida por los muones relativistas producidos en la interacción de neutrinos de alta energía en los alrededores del detector. La información de la carga, posición y tiempo de llegada de los fotones a los fotomultiplicadores que componen el detector permite tanto la reconstrucción de la trayectoria del neutrino como el conocimiento de su energía. Además, ANTARES acoge el experimento AMADEUS mediante el cual se está investigando y testeando la detección acústica de neutrinos de muy alta energía que, al interaccionar en el agua, producen un pulso termo-acústico que se pretende registrar con una red de hidrófonos. El trabajo desarrollado en esta tesis se engloba bajo el marco del experimento ANTARES. Como es común en las tesis desarrolladas en este experimento, el trabajo se ha dividido en dos áreas diferenciadas: por un lado, una parte de enfoque más tecnológico y, por otro lado, una parte analítica de datos tomados por el telescopio. La primera parte de la tesis está centrada en el desarrollo de un calibrador capaz de reproducir la señal acústica que se emite en la interacción de un neutrino de alta energía con un núcleo de agua que, generalizando, es un pulso bipolar altamente directivo. El disponer de un buen calibrador es clave a la hora de testear la detección acústica en el telescopio y poder sintonizar y "entrenar" los los receptores para este tipo de señales. La segunda parte de la tesis se ha centrado en el análisis de datos registrados por ANTARES con el fin de contrastar posibles modelos astrofísicos para la búsqueda de materia oscura. Este trabajo ha focalizado en la detección de los productos de la aniquilación de materia oscura atrapada en el centro del Sol. Se ha testeado el modelo de Secluded Dark Matter (SDM) a través de la detección de di-muones (pareja de muones co-lineales) y neutrinos en la dirección del Sol. A grandes rasgos, este modelo se basa en la idea de la existencia de un mediador resultado de la aniquilación de materia oscura que posteriormente decaería en partículas del modelo estándar como muones o neutrinos. Estos modelos han sido propuestos con el fin de explicar ciertas 'anomalías' experimentales observadas, tales como el espectro del flujo de positrones detectado en satélites, medido recientemente con gran precisión por AMS-II. realizado en esta tesis constituye la primera búsqueda de evidencias
[CAT] L'astronomia de neutrins és un camp en auge dins la Física d'Astropartícules. Els neutrins ofereixen grans avantatges com a sondes per estudiar l'Univers llunyà i d'alta energia. Es extensament acceptat que mitjançant la combinació de la informació proporcionada pels neutrins junt a la obtinguda mitjançant fotons d'alta energia (rajos gamma) i partícules carregades (rajos còsmics) es podria obtindre una imatge més completa dels processos astrofísics fonamentals que es donen al llarg del nostre Univers. La raó fonamental per la qual els neutrins són altament valorats com a missatgers és la baixa interacció amb el medi que els envolta. Al ser partícules sense càrrega interactuen molt dèbilment amb la matèria, per això poden escapar-se de la font on s'han produït i, al contrari del que ocorre amb la resta de missatgers, poden arribar a La Terra sense desviar-se pels camps electromagnètics i sense pràcticament pèrdua d'energia. Aquesta mateixa raó que els fan tan valorats és al mateix temps la que els fa tan difícil de detectar. S'imposa la necessitat de construir detectors amb grans volums de detecció, de l'ordre del km3, altament instrumentats. S'utilitzen medis naturals (al fons de la mar, en llacs, al gel de l'Antàrtida) aprofitant l'aigua (o el gel) com a material diana on interaccionen el neutrins. ANTARES és el primer telescopi submarí de neutrins construït al fons de la mar Mediterrània. Està optimitzat per a la detecció òptica de la llum de Cherenkov induïda pels muons relativistes produïts en la interacció de neutrins d'alta energia als voltants del detector. La informació de la carrega, posició i temps d'arribada dels fotons als fotomultiplicadors que composen el detector permet tant la reconstrucció de la trajectòria del neutrí, amb gran resolució angular, com el coneixement de la seua energia. A més, ANTARES acull l'experiment AMADEUS mitjançant el qual s'està investigant i testejant la detecció acústica de neutrins de molt alta energia, que, al interaccionar a l'aigua produeixen un pols termo-acústic que es pretén registrar amb una xarxa d'hidròfons. El treball dut a terme en esta tesi s'engloba baix el marc de l'experiment ANTARES. Com es comú en les tesis desenvolupades en aquest experiment, el treball s'ha dividit en dues àrees diferenciades: per una banda una part d'enfocament mes tecnològic i, d'altra banda, una part analítica de les dades preses pel telescopi. La primera part de la tesi està centrada en el desenvolupament d'un calibrador capaç de reproduir la senyal acústica que es genera en la interacció d'un neutrí d'alta energia amb un nucli de l'aigua que, generalitzant, és un pols bipolar altament directiu. Disposar d'un bon calibrador es clau a l'hora de testejar la detecció acústica al telescopi i poder sintonitzar i "entrenar" els receptors a aquest tipus de senyals. La segona part de la tesi, amb caràcter d'anàlisi de dades, s'ha centrat en l'anàlisi de les dades registrades per ANTARES amb el fi de contrastar possibles models astrofísics per a la recerca de matèria fosca. Aquest treball es centra en la detecció dels productes d'aniquilació de matèria fosca atrapada al centre del Sol. En concret, s'ha testejat el model de Secluded Dark Matter (SDM) a través de la detecció de di-muons (parell de muons co-lineals) i neutrins en la direcció del Sol. A grans trets, aquest model es basa en la idea de l'existència d'un mediador resultat de l'aniquilació de matèria fosca que posteriorment decauria en partícules del model estàndard com muons o neutrins. Aquests models han sigut proposats amb la fi d'explicar certes "anomalies" experimentals observades, tals com l'espectre del flux de positrons detectat en satèl¿lits, mesurat recentment amb gran precisió per AMS-II. L'estudi realitzat en esta tesi constitueix la primera recerca d'evidències experimentals d'aquest tipus de models en telescopis de neutrins.
Adrián Martínez, S. (2015). Design and Development of an Acoustic Calibrator for Deep-Sea Neutrino Telescopes and First Search for Secluded Dark Matter with ANTARES [Tesis doctoral no publicada]. Universitat Politècnica de València. https://doi.org/10.4995/Thesis/10251/48877
TESIS

Big Bang Nucleosynthesis (BBN), together with the analyses of the Cosmic Microwave Background (CMB) anisotropies, confirm what our day to day experience of life attests :antimatter is far less present than matter in the Universe. In addition, these observables also permit to evaluate that there exists about one proton for every 10^{10} photons present in the Universe. This is in contradiction with expectations coming from the standard hot big bang, where no distinction between matter and antimatter is made, and where subsequent annihilations would lead to equal matter and antimatter contents, at a level 10^{−10} smaller than the observed one. The Standard Model of fundamental interactions fails to explain this result, leading us to search for ‘Beyond the Standard Model’ physics.

Among the possible mechanism which could be responsible for the creation of such a matter asymmetry, leptogenesis is particularly attractive because it only relies on the same ingredients previously introduced to generate neutrino masses. Unfortunatelly, this elegant proposal suffers from a major difficulty :it resists to any tentative of being probed by our low energy observables. In this thesis, we tackle the problem the other way around and propose a way to falsify this mechanism. Considering the type-I leptogenesis mechanism, i.e. a mechanism based on the asymmetric decay of right-handed neutrinos, in a left-right symmetric framework, we show that the observation of a right-handed gauge boson W_R at future colliders would rule out any possibility for such mechanism to be responsible of the matter asymmetry present in our Universe.

Another intriguing question that analyses of the anisotropies of the CMB confirmed is the presence of a non-baryonic component of matter in our Universe, i.e. the dark matter. As hinted by observations of galactic rotation curves, it should copiously be present in our galactic halo, but is notoriously difficult to detect directly. We can take advantage on the fact that antimatter almost disappeared from our surroundings to detect the contamination of cosmic rays from standard sources the annihilation products of dark matter would produce.

The second subject tackled in this work is the study of the imprints the Inert Doublet Modem (IDM) could leave in (charged) cosmic rays, namely positrons, antprotons and antideuterons. This model, first proposed to allow the Bout-Englert-Higgs particle to evade the Electroweak Precision Test (EWPT) measurements, introduces an additional scalar doublet which is inert in the sense that it does not couple directly to fermions. This latter property brings an additional virtue to this additional doublet :since it interacts weakly with particles, it can play the role of dark matter. This study will be done in the light of the data recently released by the PAMELA, ATIC and Fermi-GLAST collaborations, which reported e^± excesses in two different energy ranges.
Doctorat en Sciences
info:eu-repo/semantics/nonPublished

Dunkle Materie bindet etwa 24 % der gesamten Energie im Universum. Bis heute ist jedoch dessen Ursprung nicht bekannt. Untersuchungen von Galaxien und kosmologischen Messungen deuten auf Dunkle Materie hin. Ein Kandidat für Dunkle Materie ist das sogenannte Weakly Interactive Massive Particle (WIMP), welches nur der Schwerkraft und der schwachen Wechselwirkung unterliegt. Eines dieser supersymmetrischen Teilchen ist das Neutralino. Das Ziel dieser Arbeit ist es, nach Dunkler Materie in dieser Form zu suchen. Aufgrund seiner Nähe sowie der hohen Dichte an Dunkler Materie bietet das Zentrum unserer Galaxie besondere Möglichkeiten zur Suche nach diesen Teilchen. Es wird vermutet, dass Neutralinos miteinander wechselwirken, dabei in Teilchen des Standard Modells zerfallen und so Photonen mit hohen Energien entstehen. Die Suche nach hochenergetischen Gammastrahlen in der Nähe des Galaktischen Zentrums kann folglich das Rätsel der Dunklen Materie lösen. Das Gammastrahlenobservatorium VERITAS hat das Galaktische Zentrum für etwa 108 Stunden beobachtet. Diese Daten wurden mittels einer unbinned Likelihood-Analyse auf die Existenz von Dunkler Materie untersucht. Da VERITAS das Galaktische Zentrum bei geringer Elevation beobachtet, können nur Gammastrahlen in einem Energiebereich zwischen 4 und 70 TeV detektiert werden. Die Analysemethode modelliert sowohl die räumliche Verteilung der Dunklen Materie als auch das Gammastrahlenspektrum. Der Beitrag der Gammastrahlen, welcher nicht von Dunkler Materie erzeugt wird, ist mittels einer punktförmigen Quelle modelliert. Zum Schluss wird der Untergrund mit realen Daten außerhalb des Galaktischen Zentrums abgeschätzt. Im Energiebereich zwischen 4 und 100 TeV wurden keine Signale der Dunklen Materie gefunden. Obere Grenzwerte für den Wechselwirkungsquerschnitt der WIMPs ergeben ⟨σv⟩ < (6.6 − 7.6) × 10−25 cm^3 oberhalb von 70 TeV in einem 95-prozentigen Erwartungsintervall.
Dark matter accounts for 24% of the universe’s energy, but the form in which it is stored is currently unknown. Understanding what form this matter takes is one of the major unsolved mysteries of modern physics. Much evidence exists for dark matter in the measurements of galaxies, dwarf galaxies, galaxy clusters, and cosmological measurements. One theory posits dark matter is a new undiscovered particle that only interacts via gravity and the weak force, called a weakly interacting massive particle (WIMP). One WIMP candidate is a supersymmetric particle called a neutralino. The objective of this thesis is to search for these dark matter particles, and attempt to measure their mass and cross section. Dark matter particles appear to concentrate in most galaxy-scale gravitational wells. One region of space that is both nearby and assumed to have a high density of dark matter is the center of our own galaxy. The neutralino is expected to annihilate into Standard Model particles, which may decay into photons. Therefore, a search for gamma rays near the Galactic Center may uncover the presence of dark matter. 108 hours of VERITAS gamma-ray observations of the Galactic Center are used in an unbinned likelihood analysis to search for dark matter. The Galactic Center’s low elevation results in VERITAS observing gamma rays in the 4–70 TeV energy range. The analysis used in this thesis consists of modeling the halo of dark matter at the Galactic Center, as well as the spectrum of gamma rays produced when two WIMPs annihilate. A point source is added to model the non-dark-matter gamma-ray emission detected from the Galactic Center. Background models are constructed from data of separate off-Galactic-Center observations. No dark matter signal is found in the 4–100 TeV mass range. Upper limits on the WIMP’s velocity-averaged cross section have been calculated, which above 70 TeV result in new limits of ⟨σv⟩ < (6.6 − 7.6) × 10−25 cm3 at the 95% confidence level.

Thesis (Ph. D.)--Massachusetts Institute of Technology, Dept. of Physics, 2012.
This electronic version was submitted by the student author. The certified thesis is available in the Institute Archives and Special Collections.
Cataloged from student-submitted PDF version of thesis.
Includes bibliographical references (p. 147-150).
N-body simulations have revealed a wealth of information about dark matter halos but their results are largely empirical. Here we attempt to shed light on simulation results by using a combination of analytic and numerical methods. First we generalize an analytic model of halo formation, known as Secondary Infall, to include the effects of tidal torque. Given this model we compare its predictions for halo profiles to simulation results and infer that angular momentum plays an important role in setting the structure of dark matter profiles at small radii. Next, we focus on explaining the origin of universality in halos. We find evidence that diffusion -- which can potentially lead to universality -- occurs during halo evolution and is partially sourced by external torques from large scale structure. This is surprising given that the halo is nonlinear and typically thought to be unaffected by neighboring structures. Last, we describe promising ways to analytically describe the evolution of nonlinear halos using a Fokker-Planck formalism.
by Phillip Gregory Zukin.
Ph.D.

De nombreuses mesures cosmologiques et astrophysiques tendent à montrer que notre galaxie serait englobée par un halo de matière sombre non-baryonique. La détection directionnelle vise à mesurer la direction du recul nucléaire issu d'une interaction avec une particule de matière sombre. Cela permettrait de mettre en évidence la forte dépendance angulaire de la distribution de reculs due à la rotation du système solaire autour du centre galactique. Cette thèse aborde la détection directionnelle par une approche multi-thématique : phénoménologie, expérimentale et analyse de données. L'objectif des études phénoménologiques est de montrer l'apport d'un détecteur directionnel en terme de recherche de matière sombre. Grâce au développement de méthodes statistiques dédiées, on montre qu'un détecteur tel que celui proposé par la collaboration MIMAC, devrait permettre de découvrir la matière sombre avec une grande significance jusqu'à des sections efficaces 2 à 3 ordres de grandeur en dessous des limites actuelles. La mise en place d'une méthodologie d'analyse de données directionnelles constitue un second objectif de cette thèse car la reconstruction 3D des traces mesurées est un point clef de cette nouvelle stratégie de détection. On présente ainsi une nouvelle méthode d'analyse basée sur une approche par vraisemblance, permettant d'optimiser l'estimation des paramètres de chaque événement mesuré: position dans le détecteur et direction. Dans le cadre de la discrimination du bruit de fond électronique, on a mis en place une étude basée sur la topologie de la trace et utilisant une analyse par arbres de décision boostés qui nous permet d'obtenir des facteurs de rejet environ 20 fois supérieurs à ceux obtenus avec des analyses séquentielles. Du point de vue expérimental, on présente une méthode originale de la mesure de vitesse de dérive des électrons permettant d'obtenir des incertitudes de l'ordre du pourcent et de contraindre simultanément les coefficients de diffusion longitudinale. On termine enfin sur l'analyse des données obtenues auprès du champ de neutrons AMANDE permettant de valider la stratégie de détection du projet MIMAC.

Le Modèle Standard de la physique des particules a été renforcé par la récente découverte du très attendu boson de Higgs. Le modèle standard cosmologique a lui relevé le défi de la haute précision des observations cosmologiques et des expériences d'astroparticules. Toutefois, ces deux modèles standards sont encore confrontés à plusieurs problèmes théoriques, comme le problème de naturalité dans le secteur de Higgs du Modèle Standard, ainsi que des problèmes observationnels à l'image des nombreuses preuves de l'existence d'un genre inconnu de matière, appelé Matière Noire, qui représenterait la majeure partie du contenu en matière de l'Univers. Les tentatives visant à résoudre ces problèmes ont conduit au développement de nouveaux modèles physiques au cours des dernières décennies. La supersymétrie est un de ces modèles qui traite du problème du réglage fin dans le secteur de Higgs et fournit de bons candidats à la Matière Noire. Les expériences actuelles de physique des hautes énergies et de haute précision offrent de nombreuses possibilités pour contraindre les modèles supersymétriques. C'est dans ce contexte que cette thèse s'inscrit. En considérant le Modèle Standard Supersymétrique Minimal (MSSM), l'extension supersymétrique la plus simple du Modèle Standard, et son candidat à la Matière Noire, le neutralino, il est montré que les contraintes obtenues en collisionneur pourraient fournir des informations sur une période de l'Univers jeune, l'ère inflationnaire. Il est également démontré que la Détection Indirecte de Matière Noire, en dépit de plusieurs inconvénients, peut se révéler être une technique efficace pour explorer les modèles de Matière Noire supersymétrique. Au-delà du MSSM il est montré que des caractéristiques uniques du candidat à la Matière Noire dans le NMSSM peuvent être explorées aux collisionneurs. L'étude d'un modèle supersymétrique avec une symétrie de jauge étendue, le UMSSM, est également développée. Les caractéristiques d'un autre candidat de la matière noire de ce modèle, le sneutrino droit, sont analysées. Des contraintes plus générales telles que celles provenant d'observables de basse énergie sont finalement prise en compte
The Standard Model of particle physics has been strengthened by the recent discovery of the long-awaited Higgs boson. The standard cosmological model has met the challenge of the high precision observations in comology and astroparticle physics. However these two standard models face both several theoretical issues, such as the naturalness problem in the Higgs sector of the Standard Model, as well as observational issues, in particular the fact that an unknown kind of matter called Dark Matter accounts for the majority of the matter content in our Universe. Attempts to solve such problems have led to the development of New Physics models during the last decades. Supersymmetry is one such model which addresses the fine-tuning problem in the Higgs sector and provides viable Dark Matter candidates. Current high energy and high precision experiments give many new opportunities to probe the supersymmetric models. It is in this context that this thesis is written. Considering the Minimal Supersymmetric Standard Model (MSSM), the simplest supersymmetric extension of the Standard Model of particle physics, and its conventional Dark Matter candidate, the neutralino, it is shown that collider constraints could provide informations on the very early Universe at the inflation area. It is also demonstrated that the Indirect Detection of Dark Matter, despite several drawbacks, can be a powerful technique to probe supersymmetric Dark Matter models. Beyond the MSSM it is shown that unique characteristics of the Dark Matter candidate in the NMSSM could be probed at colliders. The study of a supersymmetric model with an extended gauge symmetry, the UMSSM, is also developed. The features of another Dark Matter candidate of this model, the Right-Handed sneutrino, are analysed. More general constraints such as those coming from low energy observables are finally considered in this model

Thesis (Ph. D.)--Massachusetts Institute of Technology, Dept. of Physics, 2012.
Cataloged from PDF version of thesis.
Includes bibliographical references (p. 253-273).
In this thesis, we build new Effective Field Theory tools to describe the propagation of energetic partons in hot and dense media, and we propose two new reactions for dark matter in the early universe. In the first part, we analyze the transverse momentum broadening in the absence of radiation of an energetic parton propagating through quark-gluon plasma via Soft Collinear Effective Theory (SCET). We show that the probability for picking up transverse momentum ki is given by the Fourier transform of the expectation value of two transversely separated light-like path-ordered Wilson lines. We evaluate the result for the strongly coupled plasma of N = 4 SYM theory by using gauge/gravity duality, and for the weakly coupled QCD plasma by using perturbation theory. In the second part, we introduce two new dark matter reactions, called "semi-annihilation" and "assimilation". The semi-annihilation reaction takes the schematic form [psi]i[psi]j -> [psi]k[psi], where [psi]i are stable dark matter particles and # is an unstable state. They lead to non-trivial dark matter dynamics in the early universe, and they might also take place today in the Milky Way, enriching the (semi-)annihilation final state spectrum observed in indirect detection experiments. The "assimilation" reaction efficiently destroy singlet dark matter particles, but dark matter number is stored in new quasi-stable heavy states which carry the baryon asymmetry. The subsequent annihilation and late-time decay of these heavy states yields (symmetric) dark matter as well as (asymmetric) standard model baryons.
by Francesco D'Eramo.
Ph.D.

This thesis explores methods of detecting dark matter particles, with some emphasis on several dark matter models of current interest. Detection in this context means observation of an experimental signature correlated with dark matter interactions with Standard Model particles. This includes recoils of nuclei or electrons from dark matter scattering events, and direct or indirect observation of particles produced by dark matter annihilation.
Physics

L'un des problèmes les plus intéressants de la physique moderne est celui de la matière noire de l'Univers, qui reste de nature insaisissable. L'existence de la matière noire est inférée par des preuves indirectes telles que les mesures des courbes de rotation des galaxies, des dispersions de vitesse des galaxies dans les amas galactiques et les effets de lentille gravitationnelle. Ces observations fournissent des preuves sur l'existence d'une matière invisible dominant notre Univers. Il n'existe cependant aucune indication claire sur sa nature. Les observations actuelles en font le constituant dominant de l'Univers, par opposition à la matière baryonique "normale". Deux solutions sont proposées pour résoudre ce mystère. La première est basée sur une modification de la loi de la gravité comme dans la dynamique newtonienne modifiée qui pourrait expliquer les divergences entre prédictions et observations de la dynamique des masses dans l'Univers. L'autre idée consiste à proposer l'existence d'une nouvelle particule massive qui n'interagit pas avec la lumière (appelée WIMP pour "Weakly Interactive Massive Particle"), mais pouvant influencer la matière lumineuse par gravité. Plusieurs théories proposent l'existence de telles nouvelles particules. La plus célèbre de ces théories est la supersymétrie, qui est une extension du Modèle Standard de la Physique des Particules. Si l'un des partenaires supersymétriques des bosons neutres est une particule stable et le plus léger de tous les superpartenaires, il devient alors un candidat idéal pour la matière noire. La supersymétrie est en général le cadre le plus favorable pour l'existence de la matière noire
The early history of modern physics have been full of problems fixed with un-orthodox yet brilliant solutions. From the Hydrogen electron orbit, black bodyradiation and the ultraviolet catastrophe, to the perihelion precession of Mercury.Quantum Mechanics and General Relativity not only solved these problems butthey opened the path to new observations and predictions about the Universe welive in and the introduction of new problems to be solved.One of the more modern problems we are facing today in physics is the largediscrepancy among measurements of the visible mass in the Universe and the pre-dictions of laws of gravity. An indisputable mass of evidence from different partsof observational cosmology is showing again and again that the observed lumi-nous mass in the Universe constitutes a tiny fraction of the matter that actuallyexists. The proposed solutions of this problem comes in two completely differentflavors. One proposed solution is that the laws of gravity are not the same in thelimit of tiny accelerations. Theories of modified gravitational dynamics proposea non-linear term in Newton law of gravity that becomes relevant at small accel-erations which in turn can explains the missing matter. The other solution to themissing matter is the introduction of new type of matter that does not interact withlight, making it invisible yet inferred to exist by its gravitational effect. The newmatter becomes a new elementary particle to be added to list of already knownelementary particles. While there are many candidates to this new elementaryparticle the favored one is called a WIMP or Weakly Interacting Massive Particle

We are at the dawn of a data-driven era in astrophysics and cosmology. A large number of ongoing and forthcoming experiments combined with an increasingly open approach to data availability offer great potential in unlocking some of the deepest mysteries of the Universe. Among these is understanding the nature of dark matter (DM)—one of the major unsolved problems in particle physics. Characterizing DM through its astrophysical signatures will require a robust understanding of its distribution in the sky and the use of novel statistical methods.

The first part of this thesis describes the implementation of a novel statistical technique which leverages the “clumpiness” of photons originating from point sources (PSs) to derive the properties of PS populations hidden in astrophysical datasets. This is applied to data from the Fermi satellite at high latitudes (|b| ≥ 30°) to characterize the contribution of PSs of extragalactic origin. We find that the majority of extragalactic gamma-ray emission can be ascribed to unresolved PSs having properties consistent with known sources such as active galactic nuclei. This leaves considerably less room for significant dark matter contribution.

The second part of this thesis poses the question: “what is the best way to look for annihilating dark matter in extragalactic sources?” and attempts to answer it by constructing a pipeline to robustly map out the distribution of dark matter outside the Milky Way using galaxy group catalogs. This framework is then applied to Fermi data and existing group catalogs to search for annihilating dark matter in extragalactic galaxies and clusters.

In the last years, the standard model of cosmology has been corroborated by a wide number of astrophysical observations. Despite its undeniable success, nowadays there is little knowledge about the true nature of dark matter and dark energy. In this thesis we use a different approach to give an intriguing answer to these open problems, in the light of the corpuscular model of gravity. We give a general overview on the reasons behind the need for a corpuscular theory of the gravitational interaction. Then, we show that if the same picture is extended to cosmological spaces, dark energy naturally emerges as a quantum state of the gravitational dynamics, and it is described as a Bose-Einstein condensate of very soft and virtual gravitons without the necessity of introducing an exotic dark fluid. Besides, the cosmic condensate responds locally to the presence of baryonic matter, and the back-reaction manifests itself in the emergence of a dark force that mimics a dark matter behavior. In particular, at galactic scales the MOND formula for the acceleration is recovered. Then, a first attempt of estimating the back-reaction is proposed within the framework of Bootstrapped Newtonian gravity, that allows for an effective field description where Newtonian theory is “bootstrapped" introducing post-Newtonian corrections, providing a useful tool for calculations. Finally, we show that a logarithmic potential arises as a solution of the Bootstrapped field equation, in accordance with MOND prediction.

Thesis: Ph. D., Massachusetts Institute of Technology, Department of Physics, 2017.
Cataloged from PDF version of thesis.
Includes bibliographical references (pages 153-178).
In this thesis, I study the expected direct and indirect detection signals of dark matter. More precisely, I study three aspects of dark matter; I use hydrodynamic simulations to extract properties of weakly interacting dark matter that are relevant for both direct and indirect detection signals, and construct viable dark matter models with interesting experimental signatures. First, I analyze the full scale Illustris simulation, and find that Galactic indirect detection signals are expected to be largely symmetric, while extragalactic signals are not, due to recent mergers and the presence of substructure. Second, through the study of the high resolution Milky Way simulation Eris, I find that metal-poor halo stars can be used as tracers for the dark matter velocity distribution. I use the Sloan Digital Sky Survey to obtain the first empirical velocity distribution of dark matter, which weakens the expected direct detection limits by up to an order of magnitude at masses by Lina Necib.
Ph. D.

Thesis (S.B.)--Massachusetts Institute of Technology, Dept. of Physics, 2012.
Cataloged from PDF version of thesis.
Includes bibliographical references (p. 39).
We study a new form of dark matter interaction which may significantly affect the thermal relic abundance of dark matter. This new interaction takes the form C+D --> C+[phi], where D is the dark matter species present today, [phi] is a standard model species, and C is a very heavy exotic particle. In particular, C was present during the period when freeze-out occurred for dark matter species D, but subsequently decayed into standard model particles. We refer to this process as a catalytic reaction, since C acts as a catalyst for the destruction of D. We further postulate that there is a matter-antimatter asymmetry in C, so that C+C --> D+[phi] is suppressed. We find that the catalytic reaction produces very different dynamics than the standard annihilation reaction. We also find that the catalytic reaction can significantly affect the relic abundance of dark matter even if it has a much smaller cross section than the annihilation reaction. Possible physical origins for this catalytic reaction are discussed.
by Fei Lin.
S.B.

Thesis (Ph. D.)--Massachusetts Institute of Technology, Dept. of Physics, 2011.
Cataloged from PDF version of thesis.
Includes bibliographical references (p. 181-188).
The products of interactions between galaxies with a high mass ratio and low orbital angular momentum are studied. The interactions scatter the material from the smaller galaxy into structures with distinctive dynamics and morphology, including high local densities and a simple density profile related to properties of the participating galaxies. The role of the larger galaxy's tides in creating these structures and their relation to a well-studied class of mathematical objects motivates us to name them "tidal caustics". We study the densities achievable in tidal caustics for a typical merger of this type using an example from the Andromeda galaxy to determine whether they are sufficient to produce a detectable gamma-ray signal from self-interactions in the dark matter component, for likely particle models of dark matter. We find that the expected signal is an order of magnitude too low to be detected with current instruments. We also study the constraints that can be placed on the properties of the participating galaxies by observing the surface brightness profiles of the tidal caustics. We find that the local gravity and gravity gradient of the larger galaxy, and the energy spread and initial phase space density of the smaller galaxy, can be jointly constrained by fitting this profile. The constraints are degenerate but model-independent. We find that measurements of multiple caustics and the velocity of the material in each caustic along the line of sight give information about the orbital angular momentum and the deviations from spherical symmetry in the larger galaxy, though this information is somewhat model-dependent. We discuss the main technical difficulty in fitting the surface brightness profile: determining the inclination angle of the caustic. We demonstrate that a simple model can successfully recover the necessary parameters for some cases, and that a simple modification to this model will improve its success rate.
by Robyn Ellyn Sanderson.
Ph.D.

Well motivated theoretical models predict the annihilation of dark matter (DM) into standard model particles, a phenomenon which could be a significant source of photons in the gamma-ray sky. With its unprecedented sensitivity and its broad energy range (20 MeV to more than 300 GeV) the main instrument on board the Fermi satellite, the Large Area Telescope (LAT), might be able to detect an indirect signature of DM annihilations. In this work we revisit several interesting claims of extended dark matter emission made from analyses of Fermi-LAT data: First, based on three years of Fermi Large Area Telescope (LAT) gamma-ray data of the Virgo cluster, evidence for an extended emission associated with dark matter pair annihilation in the bb̄ channel has been reported by Han et al. (arxiv:1201.1003). After an in depth spatial and temporal analysis, we argue that the tentative evidence for a gamma-ray excess from the Virgo cluster is mainly due to the appearance of a population of previously unresolved gamma-ray point sources in the region of interest. These point sources are not part of the LAT second source catalogue (2FGL), but are found to be above the standard detection significance threshold when three or more years of LAT data is included. Second, we confirm the detection of a spatially extended excess of 2-5 GeV gamma rays from the Galactic Center (GC), consistent with the emission expected from annihilating dark matter or an unresolved population of about 10³ milisecond pulsars. However, there are significant uncertainties in the diffuse galactic background at the GC. We have performed a revaluation of these two models for the extended gamma ray source at the GC by accounting for the systematic uncertainties of the Galactic diffuse emission model. We also marginalize over point source and diffuse background parameters in the region of interest. We show that the excess emission is significantly more extended than a point source. We find that the DM (or pulsars population) signal is larger than the systematic errors and therefore proceed to determine the sectors of parameter space that provide an acceptable fit to the data. We found that a population of order a 10³ MSPs with parameters consistent with the average spectral shape of Fermi-LAT measured MSPs was able to fit the GC excess emission. For DM, we found that a pure τ⁺τ⁻ annihilation channel is not a good fit to the data. But a mixture of τ⁻τ⁻ and bb̄ with a (σν) of order the thermal relic value and a DM mass of around 20 to 60 GeV provides an adequate fit. We also consider the possibility that the GeV excess is due to nonthermal bremsstrahlung produced by a population of electrons interacting with neutral gas in molecular clouds. The millisecond pulsars and dark matter alternatives have spatial templates well fitted by the square of a generalized Navarro-Frenk-White (NFW) profile with inner slope γ = 1.2. We model the third option with a 20-cm continuum emission Galactic Ridge template. A template based on the HESS residuals is shown to give similar results. The gamma-ray excess is found to be best fit by a combination of the generalized NFW squared template and a Galactic Ridge template. We also find the spectra of each template is not significantly affected in the combined fit and is consistent with previous single template fits. That is, the generalized NFW squared spectrum can be fit by either of order 10³ unresolved MSPs or DM with mass around 30 GeV, a thermal cross section, and mainly annihilating to bb̄ quarks. While the Galactic Ridge continues to have a spectrum consistent with a population of nonthermal electrons whose spectrum also provides a good fit to synchrotron emission measurements. We also show that the current DM fit may be hard to test, even with 10 years of Fermi-LAT data, especially if there is a mixture of DM and MSPs contributing to the signal, in which case the implied DM cross section will be suppressed.

Hierarchical structure formation in the standard Λ+cold dark matter (CDM) model produces gravitationally bound clumpy halos with abundant substructure. These subhalos are the remnants of dark matter halos that have been accreted by their host halo over cosmic time, and have survived tidal destruction. Understanding halo substructure is extremely important, as subhalos are believed to host satellite galaxies, boost the dark matter annihilation signal, cause tidal heating of fragile structures such as stellar streams and disks, and are potentially responsible for interesting phenomena in gravitational lensing. Most importantly, the demographics of subhalos contain information of the Universe, thus providing a stringent testbed for the cosmological model.

This thesis provides a comprehensive study of dark matter subhalos, using a combination of cosmological N-body simulations and semi-analytic modeling. We start with developing a new, semi-analytic model describing halo assembly and subhalo evolution. The model combines Monte-Carlo techniques of generating halo merging histories and simple analytical descriptions for the evolution of subhalos, thus offering extremely fast computation, the agility to experiment with different cosmologies, and the control of specific physical processes. The model accurately predicts the distributions of subhalo mass and structural parameters in cosmological simulations, and outperforms simulations in terms of mass resolution and statistical power. Taking advantage of the speed and agility of the model, we present universal fitting formulae for subhalo mass and maximum circular velocity (^&ngr;max) functions that are valid for a broad range in host halo mass, redshift and CDM cosmology.

The remainder of the dissertation makes use of the model, together with a number of state-of-the-art N-body simulations, to study the statistics of halo substructure. Recent high-resolution CDM simulations reveal ~10 massive Galactic subhalos whose central potential wells are too deep to be consistent with those of the ~10 brightest Milky-Way (MW) satellite galaxies. This inconsistency, dubbed the `too-big-to-fail' problem (TBTF), has become a persistent challenge to the standard ACDM cosmology. However, the number of well resolved Galactic halos in simulations is too small to fully capture the halo-to-halo variance in substructure content, which hinders the interpretation of the inconsistency. Unleashing the power of the semi-analytic model, we generate thousands of MW-size halos with well-resolved subhalo populations, and explicitly demonstrate that a reliable assessment of TBTF requires such large samples. We argue that existing statistics used to address TBTF suffer from the look-elsewhere effect and/or disregard certain aspects of the data on the MW satellite population. We devise a new statistic that is not hampered by these shortcomings, and, using data of the MW satellites with vmax > 15 km s^-1, demonstrate that 1.4^+3.3-1.1% of MW-size host halos have a subhalo population in statistical agreement with that of the MW. We also discuss how the severity of TBTF depends on halo mass and cosmology.

We conclude the thesis with a study of unprecedented statistical power regarding the halo-to-halo variance of substructure. First, we study the mass fraction (f_sub) in subhalos as a function of host halo mass, formation redshift, and halo-centric distance. We note that recent measurements of f_sub from gravitational lensing are much higher than the average but within the 90th percentile of the f_sub distribution. Second, we quantify the deviation of the occupation statistics of subhalos from Poissonian statistics, which is widely assumed in halo occupation distribution (HOD) models. In particular, we clearly reveal the sub-Poissonian statistics at [special characters omitted] ≤ 3, aside from the already-known super-Poissonity at [special characters omitted] » 1, with [special characters omitted] the average number of subhalos. we also quantify the effect of the sub-Poissonity on the galaxy clustering predictions from HOD models. We further show that the extent of nonPoissonity depends on subhalo selection and on halo formation time - selecting subhalos by their mass or vmax at accretion yields weaker super-Poissonity for large [special characters omitted] but stronger sub-Poissonity for small [special characters omitted], compared to selecting by their present-day mass or vmax; earlier-formed halos exhibit less non-Poissonity than later-formed ones. Finally, we use the occupation statistics of the most massive satellites of the MW to put constraint on the mass and formation redshift of the MW halo. In particular, the `^&ngr;_max gap' of MW satellites between ~ 30 km s^-1 and 60 km s^-1 favors a low-mass, late-formed MW halo, with 0.25 < M_vir/10¹² h^-1M[special characters omitted] < 1.4 and 0.1 < z_f < 1.4 at 90% confidence.

Through their connection with dark matter structures, galaxies act as tracers of the underlying matter distribution in the Universe. Their observed spatial distribution allows us to precisely measure large scale structure and effectively test cosmological models that explain the content, geometry, and history of the Universe. Current observations from galaxy surveys such as the Baryon Oscillation Spectroscopic Survey have already probed vast cosmic volumes with millions of galaxies and ushered in an era of precision cosmology. The next surveys will probe over an order of magnitude more. With this unprecedented statistical power, the bottleneck of scientific discovery is in the methodology.

In this dissertation, I address major methodological challenges in constraining cosmology with the large-scale distribution of galaxies. I develop a robust framework for treating systematic effects, which significantly bias galaxy clustering measurements. I apply new innovative approaches to probabilistic parameter inference that challenge and test the in- correct assumptions of the standard approach. Furthermore, I use precise predictions of structure formation from cosmology and observations of galaxies during the last eight billion years to develop detailed models of how galaxies are impacted by their host dark matter structures. These models provide key insight into the galaxy-halo connection, which bridges the gap between cosmology theory and observations. They also answer crucial questions of how galaxies form and evolve. The developments in this dissertation will help unlock the full potential of future observations and allow us to precisely test cosmological models, General Relativity and modified gravity scenarios, and even particle physics theory beyond the Standard Model.

Identifying the relic particles that constitute the cold dark matter in our Universe is an outstanding problem in astro-particle physics. Direct detection experiments are among the most promising methods of detecting particle dark matter through non-gravitational interactions. In this thesis, the usual assumptions made when calculating the event rate at direct detection experiments are examined. Varying astrophysical parameters and the dark matter velocity distribution leads to significant changes in acceptance regions and exclusion curves for scenarios in which the tail of the velocity distribution is sampled; this includes 'light dark matter' (mass less than 10 GeV) and 'inelastic dark matter'. The DAMA and CoGeNT collaborations both report an annual modulation in their event rate that they attribute to dark matter. Two analyses of these experiments are performed. In the first, it is shown that these experiments can be compatible with each other and with the constraints from other direct detection experiments. This requires some isospin violation in the couplings of dark matter to protons and neutrons and a small inelastic splitting to boost the modulation fraction. The second analysis provides a comparison of the modulation signals free from all astrophysical parameters, under the assumption that dark matter scatters elastically. Again it is found that some isospin violation and a boosted modulation fraction is required in order that DAMA and CoGeNT are consistent with all experiments. A boosted modulation fraction may arise from a velocity distribution different from the Maxwell-Boltzmann distribution, which is usually assumed. Finally, a supersymmetric theory in which the dark matter candidate is a mixture of left- and right-handed sneutrino is considered. This theory has many novel signatures at colliders, indirect detection and direct detection experiments.

The Standard Model of particle physics can account for neither the dark matter dominating the universe's matter density, nor the baryon asymmetry that leads to the visible matter density. This dissertation explores models of new physics that connect dark matter to baryogenesis and can naturally account for the observed quantities of both types of matter. Special emphasis is given to models incorporating new weak-scale physics, as such models often predict signatures at present and upcoming experiments and can potentially be connected to solutions of the hierarchy problem. In one class of models we study, the dark matter abundance is determined by a dark matter asymmetry connected to the baryon asymmetry. In such models, the separate dark matter, baryon, and lepton number global symmetries observed today are individually broken at or above the weak scale and lead to mixing of dark matter and Standard Model fields in the early universe. This can happen generically, with dark matter-visible matter mass mixing induced by large background energies or moduli in the early universe, and can also arise at the electroweak phase transition. Mass mixing models of asymmetric dark matter can readily accommodate dark matter masses ranging from 1 GeV to 100 TeV and expand the scope of possible relationships between the dark and visible sectors. We also consider models of symmetric dark matter in which the annihilation of dark matter particles in the early universe generates the observed baryon asymmetry. This process, called “WIMPy baryogenesis”, naturally accommodates weak-scale dark matter and explains the observed dark matter density with only order-one couplings. WIMPy baryogenesis is a new model of baryogenesis at the weak scale, avoiding problems with high reheat temperatures in supersymmetric theories, and yielding observable consequences in ongoing and future experiments for some models
Physics

A model of dark matter excitations is studied in an attempt to explain the anomalously large 511 keV photon line emission observed by the SPI spectrograph on INTEGRAL to be originating from the galactic bulge of the Milky Way. The proposed dark matter WIMP has a near degenerate mass partner a few MeV heavier. Scattering between dark matter particles leads to excitations, with the subsequent decays producing an electron-positron pair. In this way, the kinetic energy of the massive dark matter particles can be efficiently converted into electron-positron pairs moving slow enough to produce the narrow annihilation line observed. With a sufficiently large mass gap, kinematic considerations and the cuspy dark matter density profile constrain excitations to the galactic bulge where the escape velocity, and thus the fraction of dark matter particles above the kinematic cutoff, is large.
Un model d'excitations matière sombre est etudié dans une tentative d'explication de la ligne d'emission anormalement large observé par le spectrographe SPI sur INTEGRAL originaire du bulbe galactique de la Voie Lactée. La matière sombre WIMP proposée possède un partenaire ayant une masse de quelques MeV supplémentaires. La diffusion entre les particules de matière sombre mène aux excitations et à la désintégration ultérieure en une paire électron-positron. De cette façon, l'énergie cinétique des particules de matière sombre peut être convertie en paires électron-positron se déplaçant suffisement lentement pour produire l'étroite ligne d'annihilation observée. Avec un espacement en masse suffisement grand, les considérations cinématique et un profil de densité de la matière sombre cuspy contraignent les excitations au bulbe galactique, où la vitesse d'échappement, et donc la fraction de particules matière sombre au-dessus du seuil cinétique, est grande.

Dark matter has a long history, but it was not until modern times that we have a chance of detecting it. This thesis focuses on the velocity distribution and its effect on indirect WIMP detection. Recently a new velocity distribution, based on data from SDSS and GAIA, was proposed. For this reason simulation of capture, annihilation and resulting flux of neutrinos from the Sun and Earth has been made both for the new and Maxwell-Boltzmann velocity distribution. The newly proposed velocity can reduce the annihilation rate in Earth by two thirds. For the Sun the effect depends on the mass of the WIMPs. For 50 GeV WIMPs the newly proposed velocity distribution could increase the annihilation rate by 5%, while for 3 TeV WIMPs it could decrease the annihilation rate by 28%. For Earth and high mass WIMPs the low velocity tail is the important part and the low resolution of this region in the new velocity distribution result in some uncertainties.

Thesis (S.B.)--Massachusetts Institute of Technology, Dept. of Physics, 2010.
Cataloged from PDF version of thesis.
Includes bibliographical references (p. 67).
Alpha background, specifically from radon and its progeny in the uranium and thorium chains, has been a major issue in dark matter detectors. This work focuses on alpha background presence in the DMTPC experiment by examining the energy distribution and the rate of alpha tracks in detector's fiducial volume. It was found that the rate and the energy distribution of alpha tracks are inconsistent with radon buildup in the detector. This was verified by replacing stainless steel materials with copper that is known to have lower uranium concentration. The alpha background was reduced 5 fold confirming that the origin of alphas is from early uranium decay chain, not radon buildup in the detector.
by Hayk Yegoryan.
S.B.

Thesis (Ph. D.)--Massachusetts Institute of Technology, Dept. of Physics, 2012.
Cataloged from PDF version of thesis.
Includes bibliographical references (p. 113-118).
Recent work in astrophysics has show that most of the matter in the universe is non-luminous. This work investigates two searches for non-luminous matter: hot dark matter formed from cosmic relic neutrinos from the Big Bang, and directional detection of cold dark matter. The cosmic neutrino background is investigated through the KATRIN experiment, using neutrino capture on tritium to search for a signal. A sensitivity at KATRIN of about 10⁴ events per year, or a local overdensity of relic neutrinos of about 3 x 10⁹ is found. Directional detection of cold dark matter provides a unique way to distinguish a dark matter signal from terrestrial backgrounds, using the expected direction of a dark matter wind based on astrophysical parameters. This work presents a new technique for directional dark matter detection--a drift chamber readout using a CCD camera. The backgrounds of this detector are investigated and enumerated, and a dark matter search sets a limit at mX =100 GeV of 3.7 x 10?³³ cm².
by Asher C. Kaboth.
Ph.D.

Under the umbrella of Theoretical Physics, progress in ‘Beyond the Standard Model’ (BSM) physics proceeds broadly along two main avenues of investigation. The first is concerned with constructing theories that attempt to explain observations, or address theoretical problems, which cannot be explained within the tremendously successful Standard Model (SM) of particle physics. The second involves looking for new ways to observe or test BSM physics, and such tests are usually developed with current experimental hints, or attractive theoretical models, in mind. This thesis contains material which falls under both approaches. Part I is concerned with Supersymmetry (SUSY). We review the basics of SUSY, and the current state of this field, and then present a novel model for SUSY at the TeV scale. This model has a Higgs sector similar to the SM and possesses a continuous U(1)_R symmetry, dramatically suppressing contributions to flavour-changing neutral currents, which can be problematic in SUSY models. After this we demonstrate that if more than one SUSY-breaking sector is present then this could lead to a rich spectrum of states with mass roughly twice the gravitino mass. In particular, if SUSY-breaking in a hidden sector arises dynamically then multiple ‘Goldstini’ and ‘Modulini’ states can arise, which couple to visible sector fields via the ‘Goldstino Portal’. We also demonstrate a new phenomenon which can occur in the context of multiple hidden sectors. If one sector breaks SUSY then this can ‘stimulate’ other sectors into also breaking SUSY, even if they are incapable of doing so on their own. Part II focusses on the matter in our Universe. We review our current understand- ing of how the visible matter in our Universe came into existence, and our current understanding of the nature of dark matter (DM). Following this we describe how DM could potentially be indirectly observed through its effects on cold white dwarf stars. Alternatively, if DM were detected by independent means, then observed cold white dwarfs could be used to place limits on the DM density in globular clusters, giving clues as to how these clusters of stars formed. We then present a new model for the co-generation of both the visible and dark matter in our Universe. This proceeds by generating a particle anti-particle asymmetry in the dark sector, which is then shared with the visible sector. This model predicts the existence of a light, m ≲ 5 eV, scalar particle which derivatively couples to DM, and provides a final state for the symmetric DM component to annihilate away into. Work completed during the period of this D.Phil is contained in [1–8], however only material in [3–6, 8] is presented in this thesis.

Several astrophysical observations, both on a galactic and cosmological scales, showing that there’s a “missing mass” in the observable Universe, can be explained assuming a non-luminous kind of matter, hence called “dark matter”. One of the most promising candidates is the Weakly Interacting Massive Particle (WIMP), a non-relativistic massive particle, gravitationally and weakly interacting with baryonic matter. The present work is specifically focused on the physics potential besides WIMP search of dark matter detectors filled with Liquid argon, like DarkSide and DEAP-3600. Liquid argon is an optimal target thanks to its high scintillation and ionization yields. DEAP-3600 is a single-phase detector, exploiting the scintillation channel only, while DarkSide-20k and Argo, future tonne scale experiments from the DarkSide program, are dual-phase Time Projection Chambers (TPCs), looking at both scintillation and ionization signals. The large mass (3.3 tons) of the DEAP-3600 target has allowed me to perform an analysis to search for Multi Interacting Massive Particles (MIMPs), a dark matter candidate alternative to WIMPs, at masses above 10^{ 16} GeV and with argon-dark matter spin-independent cross-section of about 10^{ −22 }cm^{ 2} , fully setting up the upcoming unblinding of three years of data taking. Going from the present to the future dark matter detectors, DarkSide-20k and Argo will be characterized by an extraordinary sensitivity at low energy recoils. This is mainly consequence of the high energy resolution of the chosen photodetectors, Silicon Photomultipliers (SiPMs). Custom SiPMs have been designed for the dark matter search in DarkSide-20k; hence, SiPMs have been here characterized, with a focus on their correlated noises, namely afterpulses and optical crosstalks. The same sensitivity at low energy brings also to a strong potential in detecting supernova neutrinos via coherent elastic neutrino-nucleus scattering (CEvNS) in argon by exploiting the ionization signal. The related sensitivity study is here performed showing that the neutrino emission will be detected for any galactic supernova, with a good accuracy in reconstructing the main parameters of the burst, namely the total energy of neutrinos and their average energy.

Context: The majority (~85%) of the matter in the universe is composed of dark matter, a mysterious particle that does not interact via the electromagnetic force yet does interact with all other matter via the gravitational force. Many direct detection experiments have been devoted to finding interactions of dark matter with baryonic matter via the weak force. It is still possible that dark matter interacts with itself via a strong scale force and has a self-scattering cross-section of ~0.5 cm²g ^-1. In fact such a strong scale scattering force could resolve several outstanding astronomical mysteries: a discrepancy between the cuspy density profiles seen in ΛCDM simulations and the cored density profiles observed in low surface brightness galaxies, dwarf spheroidal galaxies, and galaxy clusters, as well as the discrepancy between the significant number of massive Milky Way dwarf spheroidal halos predicted by ΛCDM and the dearth of observed Milky Way dwarf spheroidal halos. Need: While such observations are in conflict with ΛCDM and suggest that dark matter may self-scatter, each suffers from a baryonic degeneracy, where the observations might be explained by various baryonic processes (e.g., AGN or supernove feedback, stellar winds, etc.) rather than self-interacting dark matter (SIDM). If dark matter lags behind the effectively collisionless galaxies then this is clear evidence that dark matter self-interacts. The expected galaxy-dark matter offset is typically >25 kpc (for cross-sections that would explain the other aforementioned issues with ΛCDM), this is larger than the scales of that are plagued by the baryonic degeneracies. Task: To test whether dark matter self-interacts we have carried out a comprehensive survey of the dissociative merging galaxy cluster DLSCL J0916.2+2951 (also known as the Musket Ball Cluster). This survey includes photometric and spectroscopic observations to quantify the position and velocity of the cluster galaxies, weak gravitational lensing observations to map and weigh the mass (i.e., dark matter which comprises ~85% of the mass) of the cluster, Sunyaev-Zel'dovich effect and X-ray observations to map and quantify the intracluster gas, and finally radio observations to search for associated radio relics, which had they been observed would have helped constrain the properties of the merger. Using this information in conjunction with a Monte Carlo analysis model I quantify the dynamic properties of the merger, necessary to properly interpret constraints on the SIDM cross-section. I compare the locations of the galaxies, dark matter and gas to constrain the SIDM cross-section. This dissertation presents this work. Findings: We find that the Musket Ball is a merger with total mass of 4.8^+3.2_-1.5×10 ¹⁴M_sun. However, the dynamic analysis shows that the Musket Ball is being observed 1.1^+1.3_-0.4 Gyr after first pass through and is much further progressed in its merger process than previously identified dissociative mergers (for example it is 3.4^+3.8 _-1.4 times further progressed that the Bullet Cluster). By observing that the dark matter is significantly offset from the gas we are able to place an upper limit on the dark matter cross-section of σ_SIDMm ^-1_DM < 8 cm²g^-1. However, we find an that the galaxies appear to be leading the weak lensing (WL) mass distribution by 20.5" (129 kpc at z=0.53) in southern subcluster, which might be expected to occur if dark matter self-interacts. Contrary to this finding though the WL mass centroid appears to be leading the galaxy centroid by 7.4" (47 kpc at z=0.53) in the northern subcluster. Conclusion: The southern offset alone suggests that dark matter self-interacts with ~83% confidence. However, when we account for the observation that the galaxy centroid appears to trail the WL centroid in the north the confidence falls to ~55%. While the SIDM scenario is slightly preferred over the CDM scenario it is not significantly so. Perspectives: The galaxy-dark matter offset measurement is dominated by random errors in each cluster. Thus measuring this offset in other dissociative mergers holds the promise of reducing our uncertainty and enabling us to: 1) state confidently whether dark matter self-interacts via a new dark sector force, or 2) constrain the dark matter cross-section to such a degree that SIDM cannot explain the aforementioned mysteries. To this end we have established the Merging Cluster Collaboration to observe and simulate an ensemble of dissociative merging clusters. We are currently in the process of analyzing six dissociative mergers with existing data, and carrying out multi-wavelength observations of a new sample of 15 radio relic identified dissociative mergers. (Abstract shortened by UMI.)

It is now largely accepted that dark matter, and more specifically, Weakly Interacting Massive Particles (WIMPs), constitute the majority of the mass in our Universe. Within this thesis are presented: (i) an overview of the motivation and evidence for the existence of dark matter; (ii) a detailed discussion of direct detection techniques and a worldwide review of WIMP search experiments; and (iii) new experimental measurements and complementary detailed numerical simulations, carried out by the author, to determine the performance of DRIFT experimental technology. Collectively, this work explores the capability of DRIFT technology to detect dark matter, and in doing so, to resolve one of the key open questions of contemporary science. The DRIFT programme consists of an array of direct dark matter search detectors located in the Boulby mine. An important limitation to the experiment is the neutron and gamma-ray background. Experimental work presented here has determined the U and Th content of the cavern rock to be 66±6 ppb and 145±13 ppb respectively, clarifying ambiguities in previous estimations. Through the use of a Monte Carlo simulation the neutron and gamma-ray background experienced by DRIFT has been determined and the experimental implications assessed. In addition, the activity of the main neutron calibration source used to calibrate DRIFT modules has been measured and was found to be 11600 n s−1±5% on the date of exposure, resolving an earlier discrepancy. Analysis of experimental data has confirmed that the technology employed by DRIFT detectors has the capability to provide directional information of recoiling nuclei at the low energies of interest to dark matter searches. A Monte Carlo simulation has then been employed to determine the WIMP-nucleon sensitivity achievable using DRIFT detectors of the present performance, also examining what would be achievable if this was supplemented by a realistic active neutron veto detector. It is found that a CS2-filled DRIFT type detector running at a 500 NIP threshold ( 16 keV and 27 keV for C and S recoils respectively) for 300 kg years, and surrounded by the proposed veto scheme, would expect to observe a background of six un-vetoed events. The minimum positive signal above this background (90% C.L.) would correspond to a WIMP-nucleon sensitivity limit of 1.75×10−9 pb. This identifies the realistic limit of what can be achieved using gaseous CS2 as a target medium. An investigation into the limits achievable using a similar array in which DRIFT modules act as self-vetoing detectors is also examined providing insight into the future development and operation of the DRIFT programme.

In this work, we consider two different models of dark matter and set limits on results of experiments. One is a dynamic dark matter scenario where we put limits on parameters observable by experiments DAMA and XMASS through nuclear recoil of detector atoms (direct detection). The second is a case of dark matter annihilation into positrons and electrons and the signal this would produce on measured values of positron flux and ratio of electron to positron (indirect detection). The values of these quantities as measured by FERMI and PAMELA experiments are observed and an explanation using a dark matter annihilation is presented vs astrophysical sources of particles.

We explore a dynamic dark matter scenario with an ensemble of dark matter particles that starts at m₀ and spans a comb of particles separated by j^δΔ m. We verify the model by using Δm = ∞ and comparing the predictions to a non dynamic model for the same mass m0. We then observe the wider set of possibilities available with the dynamic dark matter model compared with the single mass case vis a vis constraints set by NaI and Xe detectors published by the DAMA and XMASS collaborations and check for validity of model against these measurements.

The Fermi experiment has measured the cosmic ray electron+positron spectrum and positron fraction [фe+/(фe⁺+e⁻)], and PAMELA has measured the positron fraction with better precision. While the majority of cosmic ray electrons and positrons are of astrophysical origin, there may also be a contribution from dark matter annihilation in the galactic halo. The upcoming results of the AMS experiment will show measurements of these quantities with far greater precision. One dark matter annihilation scenario is where two dark matter particles annihilate directly to e ⁺ and e⁻ final states. In this article, we calculate the signature “bumps” in these measurements assuming a given density profile (NFW profile). If the dark matter annihilates to electrons and positrons with a cross section σv ∼ 10⁻²⁶ cm³/s or greater, this feature may be discernible by AMS. However, we demonstrate that such a prominent spectral feature is already ruled out by the relative smoothness of the positron + electron cosmic ray spectrum as measured by Fermi. Hence we conclude that such a feature is undetectable unless the mass is less than ∼40 GeV.

It is almost a century now since data implying the presence of nonluminous matter in the Universe surfaced: in 1932 Oort [1] observed that the number of stars near the sun was 30´50% less than the number necessary to explain their velocities; then, in 1933, Zwicky [2] pointed out that the velocity dispersion of galaxies in the Coma cluster required 10 to 100 times more mass than the one accounted for the luminous galaxies themselves. The same Zwicky called this unseen matter dunkle materie (dark matter). These observations were practically ignored for almost four decades until a large number of new evidences corroborating the claim of Oort and Zwicky emerged. Nowadays evidences advocating the existence of Dark Matter (DM) range from the galactic scale, where DM is needed to explain the observed stellar dynamics, to cosmological scales, DM being one of the pillars of the ΛCDM model. However, despite its central role, the nature of the DM remains unknown. This ignorance, which mostly stems from our inability to detect nongravitational interactions between dark and baryonic matter, together with the fact that DM is one of the few phenomenological flaws of the Standard Model (SM) has driven a huge activity in the theoretical community.1 However, if the lack of information about the DM properties makes quite easy is to come up with plausible theoretical solutions it also makes very hard to proof or disproof them. Thus it is crucial to keep pushing the experimental frontiers in parallel with the theoretical efforts. In the following we summarize the (few) experimental informations we have about the DM, and the experimental endeavors that the community is undergoing in the attempt to unveil some of its key features. [...]