The cubic-kilometer sized IceCube neutrino observatory is burieddeep in the glacial ice at the Earth’s South Pole. Its low-energyextension array DeepCore enables physicists to search indirectlyfor light Dark Matter (DM) particles with masses as low as tensof GeV/c2 situated within our home galaxy, the Milky Way. GeVneutrinos could be produced through DM particle annihilations,propagating to the Earth where they could be detected by IceCube. This licentiate thesis presents a search for Weakly Interacting Mas-sive Particles (WIMPs) with masses as low as 30 GeV/c2 in theGalactic center (GC) using the 79-string configuration of the IceCubeneutrino detector. Data from 319.7 live-days have been analyzedusing a cut-and-count analysis approach, and found to be consistentwith the background-only hypothesis with expected backgroundfrom atmospheric muons and neutrinos. Thus, upper limits wereset on the velocity averaged DM annihilation cross-section. The Precision IceCube Next Generation Upgrade (PINGU) as apossible future neutrino detector within DeepCore would reducethe neutrino energy detection threshold to a few GeV. In additionto the data analysis with DeepCore, a sensitivity study has beenconducted to investigate the performance of PINGU for indirectDM searches in the GC and the Sun. In the Sun WIMPs could begravitationally captured through elastic scattering off nucleons. Inthis thesis, we derive PINGU sensitivities for the velocity averagedDM annihilation cross-section of WIMPs in the GC, and for theSpin-Dependent (SD) and Spin-Independent (SI) WIMP-protonscattering cross-sections, under the assumption of thermodynamicequilibrium between the WIMP capturing and annihilation rate inthe Sun. / IceCube

The Large Hadron Collider (LHC) is the most powerful and complex particle accelerator ever built. The ATLAS detector is a general-purpose particle detector at the LHC, designed to cover a wide range of physics measurements.This thesis presents two physics studies performed using data of proton-proton collisions collected with the ATLAS detector at √s = 8 TeV. The identication of jets originating from b quarks (b-tagging) is a crucial tool for many physics analyses at the LHC. A new technique to calibrate the efficiency of b-tagging algorithms using high transverse momentum jets is described. This technique allows to perform the calibration using jets with transverse momenta up to 1200 GeV, while the current calibration methods only reach approximately 300 GeV. The results of the calibration are presented.  The second study presented in this thesis is a search for Dark Matter (DM) production in association with a pair of heavy flavour quarks. A reinterpretation of the results of the ATLAS search for DM at √s = 8 TeV has been done based on simplied models. A set of simplied models with various DM masses, masses of the exchange particle, that mediates the interaction between DM and the regular matter, and couplings is considered. This study aims to choose benchmark models to be used in future searches at √s = 13 TeV. Additionally an accomplished technical project on the development of the b-tagging ATLAS software is presented.

Le travail présenté dans cette thèse porte sur la recherche de neutrino stérile à l'aide de désintégrations β dans les expériences SOX et TRISTAN. Le neutrino stérile est une particule hypothétique, solidement établi théoriquement, qui ne prendrait part à aucune interaction fondamentale, gravité mise à part. Étant entendu que le neutrino stérile se mélange avec les neutrinos actifs connus, l'existence de ces premiers peut être étudiée directement en laboratoire. L'expérience SOX a été conçue pour explorer l'existence d'un neutrino stérile d'une masse autour de l'électronvolt (eV). Un neutrino stérile avec une telle masse permettrait d'expliquer plusieurs anomalies observées à courte distance de sources (quelques mètres) lors de mesures d'oscillations de neutrinos de basses énergies (quelques MeV). SOX avait pour projet d'utiliser le détecteur de neutrinos solaire déjà existant Borexino, et d'observer un signal d'oscillation vers le stérile à l'intérieur même du volume actif du détecteur. La source radioactive de 5.5 PBq et positionnée à 8.5 m du centre du détecteur, émettrait des antineutrinos électroniques via la désintégration β du ¹⁴⁴Ce et du ¹⁴⁴Pr. Une des clés de l'observation de cette oscillation, est la connaissance précise de l'activité de la source. Une telle activité peut être déterminée en mesurant la chaleur dégagée par la source. C'est la raison pour laquelle l'INFN Genova et la TUM ont développé conjointement un calorimètre dédié. La chaleur dégagée par la radioactivité est alors captée par un échangeur puis transmise à un circuit d'eau étroitement contrôlé. Le calorimètre a été assemblé, optimisé puis étalonné avec succès. La perte de chaleur du circuit fut déterminée lors des mesures d'étalonnage grâce à un chauffage électrique. Des variations des conditions expérimentales et une isolation thermique sophistiquée ont permis d'opérer avec des pertes de chaleur négligeables. Il a ainsi été démontré que la puissance thermique de la source pouvait être estimée, en 5 jours seulement, avec une précision supérieure à 0,2%. Malheureusement, le programme SOX a dû être annulé. Le projet TRISTAN, quant à lui, tend à démontrer l'existence d'un neutrino stérile avec une masse de l'ordre du kilo-électronvolt (keV). Si le neutrino stérile à l'eV tente d'apporter une réponse aux différentes anomalies observées lors de mesures d'oscillation, le neutrino stérile au keV, en tant que potentiel candidat matière noire. Le projet TRISTAN cherche à mesurer l'empreinte de ce nouvel état de masse sur le spectre du tritium dans le cadre de l'expérience KATRIN. Cette dernière vise à déterminer la masse effective du neutrino (actif) en mesurant l'extrémité du spectre de tritium avec une excellente résolution et un faible taux de comptage. Une fois la mesure achevée, le détecteur de KATRIN sera modifié afin d'effectuer une mesure différentielle et intégrale de l'ensemble du spectre en tritium: c'est le projet TRISTAN. Le détecteur actuel sera remplacé par un nouveau détecteur de silicium à dérive (SDD) de 3500 pixels permettant une résolution de 3% à 6 keV et pouvant supporter un taux de comptage montant jusqu'à 10⁸ coups par seconde, activité maximum attendue. Un prototype a été testé avec succès et une première mesure de tritium a été réalisé au spectromètre de masse neutrino Troitsk afin d'étudier les erreurs systématiques et de développer des méthodes d'analyses pertinentes. Un premier ajustement cohérent du spectre tritium différentiel acquis lors de cette installation, a démontré la faisabilité du projet. TRISTAN lui-même est toujours en cours de développement mais les caractérisations du détecteur et les études de systématiques sont plus qu'encourageantes pour la poursuite du projet. La première investigation de neutrino stérile avec le détecteur de TRISTAN sur le site de KATRIN est prévue après la mesure de masse, en cours à Karlsruhe, aux alentours de 2024. / The work presented in this thesis is about the sterile neutrino search with the two experiments SOX and TRISTAN based on the β-decay. Sterile neutrinos are theoretically well motivated particles that do not participate in any fundamental interaction except for the gravitation. With the help of these particles one could elegantly explain the origin of the neutrino mass, dark matter and the matter-antimatter asymmetry in the universe. As sterile neutrinos can mix with the known active neutrinos, they could be discovered in laboratory searches. The SOX experiment was designed to search for a sterile neutrino with a mass in the eV-range. This particular mass range is motivated by several anomalous observations at short-baseline neutrino experiments that could be explained by an additional oscillation with a length in the order of meters that arises from an eV-scale sterile neutrino. For SOX it was planned to use the existing Borexino solar neutrino detector to search for an oscillation signal within the detector volume. The neutrinos are emitted from a 5.5 PBq electron-antineutrino source made of the β-decaying isotopes ¹⁴⁴Ce and ¹⁴⁴Pr, located at 8.5 m distance from the detector center. For the analysis of the signal it is crucial to know the source activity. This parameter is determined by measuring the decay heat of the source with a thermal calorimeter that was developed by TUM and INFN Genova. The decay heat is measured through the temperature increase of a well-defined water flow in a heat exchanger that surrounds the source. The calorimeter was assembled, optimized and characterized. Heat losses were determined through calibration measurements with an electrical heat source. Adjustable measurement conditions and an elaborate thermal insulation allowed an operation with negligible heat losses. It was proven that the power of a decaying source can be measured with <0.2% uncertainty in a single measurement that lasts ~5 days. Unfortunately the SOX experiment was canceled after a technological problem rendered the source production with the required activity and purity impossible. The TRISTAN project is an attempt to discover sterile neutrinos with masses in the order of keV. In contrast to eV-scale sterile neutrinos that are motivated by several anomalies observed in terrestrial experiments, the existence of sterile neutrinos with masses in the keV range could resolve cosmological and astrophysical issues, as they are dark matter candidates. The TRISTAN project is an extension of the KATRIN experiment to search for the signature of keV-scale sterile neutrinos in the tritium β-spectrum. KATRIN itself is attempting to determine the effective neutrino mass by measuring the end point of the tritium spectrum at low counting rates. The KATRIN setup will be modified after the neutrino mass measurements are finished to conduct a differential and integral measurement of the entire tritium spectrum. This project is called TRISTAN. The current detector will be replaced by a novel 3500-pixel silicon drift detector system that has an outstanding energy resolution of a few hundred eV and can handle rates up to 10⁸ counts per second as they occur when the entire spectrum is scanned. Prototype detectors were successfully tested and first tritium data was taken at the Troitsk ν-mass spectrometer to study systematic effects and develop analysis methods. A successful fit of the differential tritium spectrum proved the feasibility of this approach. TRISTAN itself is still at an early stage, but the detector development and systematic studies are well on track and delivered so far encouraging results. The sterile neutrino search is scheduled after the KATRIN neutrino mass program is finished in ~2024.

Astrophysical observations indicate the existence of dark matter through its gravitational interaction, but since its other interactions remain undetected, its particle nature is still unknown. There are several dark matter candidates, one being a hypothetical particle called axion that can have three types of non-gravitational couplings: electromagnetic, electric dipole moment (EDM), and gradient. This dissertation presents experimental approaches and axionlike dark matter search results from two table-top experiments: Cosmic Axion Spin Precession Experiment (CASPEr-electric) sensitive to EDM and gradient couplings, and Search for Halo Axions with Ferromagnetic Toroids (SHAFT) sensitive to electromagnetic coupling. CASPEr-electric is a resonant search for axionlike dark matter through the induced nuclear spin precession. The experimental approach is measuring nuclear magnetic resonance (NMR) of the heavy atom in a ferroelectric crystal. Experimental setup is characterized using pulsed NMR calibration measurements. Recorded search data that is sensitive to axionlike dark matter is analyzed by optimal filtering and then setting a detection threshold based on the histogram of power spectral density modeled as a Gaussian distribution. The candidates above the threshold are all rejected through statistical fluctuations and scan/re-scan measurements. CASPEr-electric places the upper bounds on the EDM and gradient couplings of axionlike dark matter in the Compton frequency range from 39.1 MHz to 40.2 MHz. SHAFT is a broadband search for axionlike dark matter through the induced oscillatory magnetic field. The resultant magnetic flux is measured with a precision magnetometer called superconducting quantum interference device (SQUID), coupled to a coil placed on the inner surface of a ferromagnetic toroid. After analyzing the search data, all candidates are rejected and SHAFT places a limit on electromagnetic coupling of axionlike dark matter between 3 kHz and 3 MHz Compton frequencies. Finally, coupling limits placed by CASPEr-electric and SHAFT are evaluated in the wider parameter space, and possible future directions that both experiments could take to improve their sensitivities to axionlike dark matter are discussed. / 2022-09-27T00:00:00Z

京都大学 / 0048 / 新制・課程博士 / 博士(理学) / 甲第18074号 / 理博第3952号 / 新制||理||1569(附属図書館) / 30932 / 京都大学大学院理学研究科物理学・宇宙物理学専攻 / (主査)教授 谷森 達, 教授 鶴 剛, 准教授 市川 温子 / 学位規則第4条第1項該当 / Doctor of Science / Kyoto University / DFAM

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We introduce an elastic constitutive model of gravity that enables the interpretation of cosmological observations in terms of established ideas from Solid Mechanics and multiscale modeling. The behavior of physical space is identified with that of a material-like medium called "cosmic fabric," which exhibits constitutive behavior. This cosmic fabric is a solid hyperplate that is broad in the three ordinary spatial dimensions and thin in a fourth hyperspatial dimension. Matter in space is treated as fabric inclusions that prescribe in-plane (three-dimensional) strain causing the transverse bending of the fabric into the fourth hyperspatial dimension. The linearized Einstein-Hilbert action, which governs the dynamics of physical space, is derived from postulating Hooke’s Law for the fabric, and the Schwarzschild metric is recovered from investigating matterabric interactions. At the continuum length scale, the Principle of Relativity is shown to apply for both moving and stationary observers alike, so that the fabric’s rest reference frame remains observationally indistinguishable at such a length scale. Within the Cosmic Fabric paradigm, the structural properties of space at different hierarchical length scales can be investigated using theoretical notions and computational tools from solid mechanics to address outstanding problems in cosmology and fundamental physics. For example, we propose and offer theoretical support for the "Inherent Structure Hypothesis", which states that the gravitational anomalies currently attributed to dark matter may in fact be manifestations of the inherent (undeformed) curvature of space. In addition, we develop a numerical framework wherein one can perform numerical "experiments" to investigate the implications of said hypothesis.

I investigate the observational signatures of the formation of dark matter cores in dwarf galaxies. I adopt the paradigm where the energy from star formation feedback is injected into the orbits of dark matter particles, forming a constant density core consistent with observations of dwarf galaxies. Using physically motivated constraints I show there is ample feedback energy available given the average stellar mass of dwarf galaxies to form cores in $10^{8}$--$10^{11}$\thinspace M$_{\odot}$ halos, and predict the maximum core size as a function of stellar mass. I describe how observational features of the old stellar content of dwarf galaxies are due to this core formation paradigm. As both dark matter and stars are collisionless fluids, the stars responsible for the feedback form in the centres of dwarf galaxies and have their orbits grown by subsequent star formation. This will naturally lead to age and metallicity gradients, with the younger and more metal rich stellar population near the dwarf centres. This process also prevents the destruction of globular clusters by driving them out of the dwarf nucleus --- the decrease in central dark matter density reduces the strength of dynamical friction --- and increases the likelihood of being stripped onto the stellar halos of larger galaxies. It also offers a model for forming multiple populations in globular clusters, with the only assumption being that the source of the polluted gas resides within the dwarf progenitor. As the orbit of a globular cluster grows, it will experience multiple accretion events with each pass through the gas-rich galaxy centre. The simple accretion model exhibits two traits revealed from observations --- a short accretion timescale and a sensitive dependence on mass --- without requiring an exotic initial stellar mass function or the initial globular cluster mass function to be 10--25 times larger than at present. / Dissertation / Doctor of Philosophy (PhD)

Longstanding evidence from observational astronomy indicates that non-luminous "dark matter" constitutes the majority of all matter in the universe, yet this mysterious form of matter continues to elude experimental detection. This dissertation presents a search for dark matter at the Large Hadron Collider using 139 fb\(^{-1}\) of proton-proton collision data at a centre-of-mass energy of \(\sqrt{s} = 13\,\)TeV, recorded with the ATLAS detector from 2015 to 2018. The search targets a final state topology in which dark matter is produced from the proton-proton collisions in association with a pair of W bosons, one of which decays to a pair of quarks and the other to a lepton-neutrino pair. The dark matter is expected to pass invisibly through the detector, resulting in an imbalance of momentum in the plane transverse to the beam line. The search is optimized to test the Dark Higgs model, which predicts a signature of dark matter production in association with the emission of a hypothesized new particle referred to as the Dark Higgs boson. The Dark Higgs boson is predicted to decay to a W boson pair via a small mixing with the Standard Model Higgs boson discovered in 2012. Collisions that exhibit the targeted final state topology are selected for the search, and an approximate mass of the hypothetical Dark Higgs boson is reconstructed from the particles in each collision. A search is performed by looking for a deviation between distributions of the reconstructed Dark Higgs boson masses and Standard Model predictions for the selected collisions. The data is found to be consistent with the Standard Model prediction, and the results are used to constrain the parameters of the Dark Higgs model. This search complements and extends the reach of existing searches for the Dark Higgs model by the ATLAS and CMS collaborations. / Graduate