Thesis (Ph. D.)--University of Hong Kong, 1990.

Thesis (Ph. D.)--University of Chicago, Department of Physics, March 2003. / Includes bibliographical references. Also available on the Internet.

Thesis (Ph. D.)--Ohio State University, 2007. / Title from first page of PDF file. Includes bibliographical references (p. 307-319).

Orientador: Carola Dobrigkeit Chinellato / Dissertação (mestrado) - Universidade Estadual de Campinas, Instituto de Fisica Gleb Wataghin / Made available in DSpace on 2018-07-26T03:41:53Z (GMT). No. of bitstreams: 1 SouzaFilho_LuizVitorde_M.pdf: 1518149 bytes, checksum: 66f8abecc0d6ee8a9a04da771982f58d (MD5) Previous issue date: 2000 / Resumo: Neste trabalho, discutirei a utilização do tempo de chegada dos fótons Cerenkov como técnica de distinção da partícula primária em chuveiros atmosféricos extensos. Os telescópios de luz Cerenkov mostraram ser os mais eficientes instrumentos de medida em astronomia gama e suas medidas têm colaborado para a compreensão dos processos de geração de raios cósmicos em núcleos ativos de galáxias e supernovas. Na observação das fontes emissoras de raios gama, a reconstrução da energia e ângulo de incidência da partícula primária é duramente prejudicada pela detecção de chuveiros iniciados por prótons, ferros e outros núcleos. A mais utilizada técnica de distinção de primários é a Técnica de Imagem (Imaging Atmospheric Cerenkov Technique), que se baseia na forma do sinal na câmara de fotomultiplicadoras. O método aqui apresentado faz uso do tempo de chegada para caracterizar os chuveiros hadrônicos através da sua componente muônica. A teoria que descreve o desenvolvimento dos chuveiros prediz a presença de um pico antecipado na distribuição temporal devido aos fótons produzidos por múons. Modificações incluindo absorção da atmosfera, eficiência quântica das fotomultiplicadoras e refletividade dos espelhos nas simulações de Monte Carlo, viabilizaram um estudo detalhado dos perfis temporais que revelou novas características marcantes da distribuição temporal e que possibilitou o desenvolvimento de uma promissora técnica de distinção. Comprovou-se, também, a necessidade de dois enfoques diferentes na análise de chuveiros, dependendo da energia do primário. Para energias abaixo de aproximadamente 10 TeV destaca-se a pequena largura do sinal de chuveiros hadrônicos enquanto que para energias superiores a 10 TeV a separação de gamas primários só foi possível a grandes ângulos zenitais devido à detecção do pico adiantado. Além disso, mostrarei estudos sobre a eficiência dos arranjos de Davies-Cotton e parabólico no tocante à utilização do tempo de chegada, comprovando a superioridade, já esperada, dos espelhos isócronos / Abstract: The present work is a discussion of the Cerenkov photons arrival time as a technique to determine the primary particle of extensive air showers. Cerenkov telescopes have proven to be one of the most effective means of detecting sources of gamma rays and their measurements have improved our understanding on how cosmic rays are created in active galactic nuclei and supernovae. In the observations of these objects, the reconstruction of the energy and incident direction are the final goals of the data analysis. However, the precision of the reconstruction methods is strongly affected by the detection of showers initiated by protons, iron and other atomic nuclei. A method based on the shape of the image in the photomultiplier camera is the most used technique to distinguish between hadron and gamma induced showers. The so called Hillas Parameters have established the operational basis for the Imaging Atmospheric Cerenkov Technique. The method presented in this dissertation provides a way to access the information recorded in the arrival time profiles by the muonic component of the hadronic showers. The theory which describes the development of showers predicts the arrival of early Cerenkov photons due to the presence of muons in hadronic showers. The inclusion of atmospheric absorption, mirror reflectivity and photomul- tiplier quantum efficiency in the Monte Carlo programs reduced the output file size by a factor of tenallowing the simulation of a great number of events. A detailed analysis of the time profiles was carried out and revealed a new remarkable feature of the hadronic showers which resulted in the development of a promising method to distinguish primary particles. Two approaches are proposed for different ranges in energy. Hadronic showers with energies below 10 TeV show very narrow time distributions and can be eliminated by a superposition of cuts, while for energies above 10 TeV the distinction was possible only for large zenith angles through the detection of the early photons. Besides that, the properties concerning time profiles of the Davies-Cotton and Parabolic telescopes are going to be presented and, as expected, the superiority of the isochronous reflector is going to be demonstrated. / Mestrado / Física / Mestre em Física

No description available.

No description available.

Das Thema dieser Arbeit ist die fuer das HEGRA Experiment entwickelte Rekonstruktions-Algoritmen, die Geometry und Energie von hochenergetischen kosmischen Gamma-Strahlen zu rekonstruieren, in die H.E.S.S. software Umgebung zu implementieren und das nicht-gepulste Energie-Spektrum des Krebsnebels zwischen Energien von 300 GeV und 20 TeV zu bestimmen. Dafuer wurden die ersten stereoskopischen Daten von Oktober und November 2003 mit einer 3 Teleskope-Konfiguration des H.E.S.S. Systems der Phase-I verwendet. Die Phase-I des H.E.S.S. Systems wurde im Dezember 2003 fertiggestellt, nachdem das vierte Teleskop in Betrieb genommen wurde. Die Rekonstruktionsalgorithmen wurden mit Monte Carlo Simulationen fuer die vollstaendige Phase-I des Teleskop-Systems getestet. Die Aufloesung fuer die rekonstruierte Richtung und Energie der einzelnen gamma-Ereignisse sind 0.15 Grad und 14 Prozent bei 45 Grad Zenitwinkel. Die Daten des Krebsnebels, die eine Wobble-Versetzung von +-0.5 Grad and +-1.0 Grad haben und die im Zenitwinkel-Bereich von 45 Grad bis 50 Grad fuer 4 Stunden beobachtet wurden, geben ein Signal von 50 Standardabweichungen. Das differentielle Energiespektrum des Krebsnebels zwischen 450 GeV und 20 TeV nach den Schnitten ist (dN / dE) = (3.37+-0.47)*10^{-11}*E^{-2.59+-0.12} cm^{-2} s^{-1} TeV^{-1}. Der integrierte Fluss oberhalb 1 TeV ist (2.11+-0.29)*10^{-11} cm^{-2} s^{-1}. Diese Resultate sind konsistent mit Messungen anderer Experimente, speziell von HEGRA und Whipple. Die Resultate stimmen mit den Erwartungen der synchroton self-Compton Modelle fuer den TeV Emissionbereich ueberein. Das magnetische Feld in der Region, wo die TeV gamma-Strahlen vermutlich entstehen, wird zu 0.18+-0.01 mG bestimmt. Die Resultate dieser Arbeit zeigen die Leistungsfaehigkeit des H.E.S.S. Teleskop-Systems. / The goal of this thesis is to implement the methods developed for the HEGRA experiment to reconstruct the geometry and energy of the air-showers induced by the cosmic high-energy gamma rays into the software environment of the H.E.S.S. experiment. Furthermore, using the implemented algorithms, a search for the unpulsed emission is aimed in the energy range between 300 GeV and 20 TeV from the Crab Nebula using the first stereoscopic data taken during October and November 2003 with the 3 telescope configuration of the H.E.S.S. array in Phase-I. The Phase-I of the H.E.S.S. array was completed in December 2003 by the addition of the fourth telescope. By testing the reconstruction algorithms of a complete Phase-I H.E.S.S. array with Monte Carlo simulations, it is found that the resolution of the reconstructed direction and energy of a gamma-ray event from a zenith angle of 45 degrees is around 0.15 degrees and 14 percent, respectively. The data on the Crab Nebula including runs with wobble offset of +-0.5 degrees and +-1.0 degrees is collected at zenith angles from 45 degrees to 50 degrees for a total of 4 hours and gives a background subtracted signal of about 50 standard deviations. The differential energy spectrum of the unpulsed gamma-ray emission from the Crab Nebula is found to be (dN / dE) = (3.37+-0.47)*10^{-11}*E^{-2.59+-0.12} cm^{-2} s^{-1} TeV^{-1} between 450 GeV and 20 TeV after all cuts. The integral flux above 1 TeV is (2.11+-0.29)*10^{-11} cm^{-2} s^{-1}. These results are consistent with the results published by other experiments, in particular HEGRA and Whipple. The results agree well with the expectation from synchrotron self-Compton models for TeV emission range. The magnetic field in the region, where TeV gamma rays are produced, is found to be 0.18+-0.01 mG. This result agrees with the magnetic field values deduced by the models. The results obtained for the Crab Nebula in this thesis demonstrate the performance of the H.E.S.S. array.

Orientadores: José Augusto Chinellato, Márcio Aparecido Müller / Dissertação (mestrado) - Universidade Estadual de Campinas, Instituto de Física Gleb Wataghin / Made available in DSpace on 2018-08-19T10:08:45Z (GMT). No. of bitstreams: 1 Theodoro_VanessaMenezes_M.pdf: 42012954 bytes, checksum: 1cd4d5a5b5ebfd4b0836da1f0709faa6 (MD5) Previous issue date: 2011 / Resumo: O Observatório Pierre Auger foi construído para detectar raios cósmicos de altas energias. Um dos principais objetivos das pesquisas realizadas pelo Observatório Auger, é o estudo da composição de massa dos raios cósmicos primários. O conteúdo muônico dos chuveiros atmosféricos extensos, produzidos a partir das interações dessas partículas primárias no alto da atmosfera, é um dos parâmetros mais sensíveis para o estudo da composição de massa. Ao nível do solo, as partículas detectadas com os 1600 tanques Cherenkov, que constituem o detector de superfície do Observatório, são essencialmente uma mistura de fótons, elétrons e pósitrons, que formam a componente eletromagnética; e os múons da componente muônica dos chuveiros extensos. A contribuição relativa dessas componentes depende do estágio de desenvolvimento do chuveiro e da distância radial ao eixo do mesmo. Nas regiões mais afastadas do eixo do chuveiro, num determinado estagio de seu desenvolvimento, um chuveiro iniciado por um núcleo de ferro, pode sob as mesmas condições que um chuveiro com primário de próton, induzir até 40% mais múons. Um dos métodos possíveis para estimar a contribuição muônica é o uso da estrutura temporal do sinal Cherenkov no detector de superfície. Esses sinais digitalizados em FADCs, mostram que múons induzem picos de sinais acima de um contínuo eletromagnético formado de pequenos picos. De forma que essa estrutura de sinal característica das componentes dependem da distância radial ao eixo do chuveiro. Esse trabalho tem como objetivo contribuir para a identificação e discriminação das componentes muônicas e eletromagnética dos chuveiros, a partir de um desenvolvimento matemático sobre o método de análise ¿Muon Jump¿. O método de jumps é baseado nas estruturais temporais dos sinais das componentes registrados pelos tanques Cherenkov do Observatório Auger e digitalizados em unidades FADCs. Usando essa característica estrutura temporal dos sinais, poderemos estimar o sinal de cada componente, definindo filtros de separação nas distribuições temporais dos sinais das frentes dos chuveiros e nas distribuições das derivadas desses sinais. Partindo dos diferentes sinais depositados por múons e partículas eletromagnéticas nos tanques Cherenkov, fizemos um estudo de contaminação desse sinal muônico pela componente eletromagnética, de forma individual e em frentes de chuveiros atmosféricos. Com isso, definimos o conceito de um filtro a ser aplicado nas distribuições de sinais, que nos permitisse separar de forma eficiente os sinais produzidos pelas partículas / Abstract: The Pierre Auger Observatory was built to detect high-energy cosmic rays. Studies of the mass composition of the highest energy cosmic rays is a major focus of research developed by the Pierre Auger Observatory. The muon content of the extensive air showers produced from the interactions of these primary particles with the atmosphere, is one of the most sensitive parameters to the mass composition. At the ground level, the detected particles by the Surface Detector of the Auger Observatory consists of 1660 water-Cherenkov detectors, are essentially a mixture of photons, electrons and positrons, the electromagnetic component, and muons, the muonic component. The relative contribution of these components depends on the stage developmental stage and on the radial distance of the showers. Far enough from the shower axis at a given development stage, a shower initiated by a iron primary may induce up to 40% more muons than a proton primary under the same conditions. The time structure of the Cherenkov signal profile in the surface detectors of particles reaching ground is used to estimate the muonic contribution. The Cherenkov signals are digitized as FADCs traces, and show that muons induce peaks signal above a continuous electromagnetic formed of small peaks. So this characteristic structure of the muonic and eletromagnetic peaks depend on the radial distance from the shower axis. The goals of my work is to contribute to the identification and discrimination of the eletromagnetic and muonic components, from a mathematical model to apply filters in the signal distributions of the particles. This method is based on the Jump method. Using the detailed time structure of signs, we can estimate the sign of each component, defining a set of separation filters to make an efficient selection of the muonic signal. The different signals deposited by muons and electromagnetic particles in Cherenkov tanks, allowed us to study the electromagnetic contamination in individual muonic signals and in the showers fronts / Mestrado / Física / Mestra em Física

Les travaux de recherche documentés dans cette thèse s'inscrivent dans le cadre de la Collaboration UA9 au CERN. L'objectif principal de la collaboration est l'étude de la collimation et de l'extraction de faisceaux de particules de haute énergie. La thèse est principalement consacrée au développement des détecteurs et aux installations expérimentales correspondantes qui ont été mises en œuvre au SPS et au LHC au CERN. En ce qui concerne la nature de l'interaction des particules chargées avec une structure monocristalline, un cristal courbé peut être utilisé pour orienter le faisceau de particules de haute énergie au moyen de la canalisation de particules entre les plans atomiques du cristal. Un tel phénomène est étudié de manière approfondie par la Collaboration UA9. Un des principaux objectifs de la recherche présentée dans cette thèse est de développer des dispositifs sensibles pour mesurer le flux et les caractéristiques de faisceau des particules déviées par le cristal au SPS et au LHC. Pour cette thèse nous avons étudié les détecteurs Cherenkov (CpFM) et les détecteurs à pixel (Timepix). Depuis 2015, le CpFM (détecteur de Cherenkov pour la mesure du flux de protons) a été souvent modifié afin d'améliorer la précision pour le comptage des particules. La plage de fonctionnement du dispositif varie de 1 à 1000 particules par faisceau de particules (~3 ns) avec une résolution inférieure à 20% par proton. Fonctionnant dans le vide primaire de l’accélérateur et à des doses de rayonnement élevées, le détecteur a montré une grande stabilité et ayant la possibilité d’effectuer des études de contamination par faisceau. À son tour, le détecteur Timepix a été étalonné sur la ligne de faisceaux d'extraction de l'accélérateur SPS, fonctionnant dans le vide secondaire (Roman Pot). Une partie importante de la thèse est consacrée à la caractérisation et à l'étalonnage de ces détecteurs avec les développements des logiciels pour l'acquisition et l'analyse de données. Dans cette thèse, nous proposons également la mesure du moment dipolaire magnétique (MDM) de baryons à courte durée de vie. Le MDM est une caractéristique importante de l'interaction des particules avec un champ magnétique externe. Pour cette thèse, nous nous concentrons sur la mesure le MDM du baryon LambdaC+, qui pourrait fournir des informations sur le facteur gyromagnétique (g) du quark charme. Une valeur différente de g=2 indiquera une structure composite possible du c-quark et clairement la présence de physique au-delà du Modèle Standard (SM). Jusqu'ici, aucune mesure expérimentale du moment dipolaire magnétique des baryons avec des quarks lourds n'a été effectuée en raison d'une courte durée de désintégration de ces particules (environ 60 um). La proposition faite dans cette thèse est de produire des baryons charmés par interaction forte entre les protons extraits (à l’aide d’un premier cristal courbé) et une cible. Après la cible, un deuxième cristal courbé à grand angle (de plusieurs mrad) est utilisé pour canaliser les baryons et induire une rotation du vecteur de polarisation des baryons charmés. Cette configuration s'appelle une configuration à double cristal et l'expérience est proposée au LHC. Dans cette thèse, je me suis concentré principalement sur tous les tests et la validation nécessaires au SPS avant la mise en œuvre au LHC. Une configuration expérimentale possible pour les mesures MDM au niveau du SPS est également proposée avec une estimation de l'erreur absolue de la valeur mesurée du facteur g pour le baryon LambdaC+. / The research work documented in this thesis is done in a frame of the UA9 Collaboration at CERN. The main goal of the collaboration is the investigation of the high-energy particle beam collimation and extraction. The thesis is mainly devoted to the developments of detectors and the consequent experimental setups implemented at the SPS or LHC circulating machines at CERN. Regarding the nature of the charged particle interaction with a monocrystalline structure, a curved crystal can be used for the steering of the high-energy particle beam by means of the particle channeling between atomic planes of the crystal. Such a phenomenon is intensively studied by the UA9 Collaboration. Therefore, one of the main goals of the presented research is to develop sensitive devices for measuring the flux and the beam characteristics of the particles deflected by the crystal at the circulating machines. The detectors studied for this thesis are Cherenkov (CpFM) and pixel (Timepix). Since 2015, the CpFM (Cherenkov detector for proton Flux Measurement) has undergone various modifications to improve the particle counting characteristics. The range of the device operation varies from 1 to 1000 particles per bunch (~3 ns) with the particle resolution of less than 20% per single proton. Working in the primary vacuum of the accelerator and at high radiation doses, the detector showed high stability with the possibility to perform beam contamination studies. In turn, the Timepix detector has been calibrated at the extraction beamline and SPS accelerator, working in the secondary vacuum of the Roman Pot. A significant part of the thesis is devoted to the characterization and calibration of these detectors with the software developments for data acquisition and analysis. In this thesis, we also make a proposal for the measurement of the magnetic dipole moment (MDM) of short-lived baryons. The MDM is an important characteristic of the particle interaction with an external magnetic field. For the thesis, we concentrate on the measurement of the LambdaC+ MDM, which could provide information on the gyromagnetic (g) factor of the charm quark. Any discrepancy from g=2 will indicate a possible composite structure of the c-quark and clearly physics beyond the Standard Model (SM). So far, no experimental measurements of this value of baryons with heavy flavoured quarks have been carried out due to a short decay length of these particles (about 60 um). The proposal made in this thesis is to produce charm baryons by a strong interaction of the extracted proton beam (using a first bent crystal) impinging onto a target followed by the second large angle bent crystal (of several mrad) to channel the baryons and to rotate their polarization vector. This configuration is called a double-crystal setup and the experiment is proposed to take place at the LHC. In this thesis, I concentrate mainly on all the tests and validation needed at the SPS prior to the implementation at the LHC. A possible experimental configuration for the MDM measurements at the SPS is also proposed with an estimation of the absolute error of the measured g-factor value for the LambdaC+ baryon.

In dieser Arbeit wird mit Hilfe von Daten, die mit dem High Energy Stereocopic System (H.E.S.S.) in Namibia aufgenommen wurden, indirekt nach dunkler Materie im Halo der Milchstraße gesucht / An indirect search for the presence of dark matter particles in the halo of the Milky Way with data that were recorded with the High Energy Stereoscopic System (H.E.S.S.) is discussed in this work