Dissertations / Theses on the topic 'Cosmic ray; detector; anisotropy'
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1
Guillian, G., J. Hosaka, K. Ishihara, J. Kameda, Y. Koshio, A. Minamino, C. Mitsuda, et al. "Observation of the anisotropy of 10 TeV primary cosmic ray nuclei flux with the Super-Kamiokande-I detector." American Physical Society, 2007. http://hdl.handle.net/2237/8844.
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Grigat, Marius [Verfasser]. "Large scale anisotropy studies of ultra high energy cosmic rays using data taken with the surface detector of the Pierre Auger Observatory / Marius Grigat." Aachen : Hochschulbibliothek der Rheinisch-Westfälischen Technischen Hochschule Aachen, 2011. http://d-nb.info/1018201106/34.
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Smith, Andrew Geoffrey Kent. "Cosmic ray anisotropy at high energies." Title page, contents and overview only, 1996. http://hdl.handle.net/2440/18616.
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Title page, contents and abstract only. The complete thesis in print form is available from the University Library.Thesis (Ph.D.)--University of Adelaide, Dept. of Physics and Mathematical Physics, 1996
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Graham, Lilian Joan. "Ultra high energy gamma ray point sources and cosmic ray anisotropy." Thesis, Durham University, 1994. http://etheses.dur.ac.uk/5594/.
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The experimental set-up at the Baksan Air Shower Array, used to detect air showers above ~0.2xl0(^14)eV, is described. An estimation of the angular resolution using the cosmic ray shadow of the Sun and the Moon gives a value of ~2.5˚ which is consistent with previous estimates from Monte-Carlo simulations. Using data from this array covering 1985-1992, a search is made for 7-ray emission from 18 candidate sources. Upper limits to the flux from these sources are stated in all cases. A periodicity search is made on data for which the excess for a single transit of a particular source is above 3(7. The results of this periodicity analysis on such days points to 4 possible observations of pulsed emission at the 95% confidence level. These are 4U0115+63 on 19.03.89, PSR19534-29 on 12.02.85, 1E2259+586 on 01.08.91 and PSR0655+64 on 12.08.89. Without confirmation from other groups however the findings are not significant enough to stand alone. A harmonic analysis has been performed on the 8 years of data and after pressure corrections and a Farley & Storey analysis to eradicate any spurious sidereal variations we find negligible evidence of 2nd or 3rd harmonic but a 1st harmonic amplitude and phase of (12.7 ±1.2) x 10(^-4) at 23.1 ± 0.3hr right ascension. When one takes into account the cosϐ effect on the sidereal anisotropy this value becomes 17.4±1.6xl0(^-4).Future developments and improvements to be undertaken at BASA, including the building of a muon detector, are outlined.
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Boghrat, Pedram. "Search for ultra high energy cosmic ray anisotropy with Auger." Diss., Restricted to subscribing institutions, 2008. http://proquest.umi.com/pqdweb?did=1750728181&sid=5&Fmt=2&clientId=1564&RQT=309&VName=PQD.
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Bultena, Sandra Lyn. "Direction measurement capabilities of the LEDA cosmic ray detector." Thesis, McGill University, 1988. http://digitool.Library.McGill.CA:80/R/?func=dbin-jump-full&object_id=63930.
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Murthy, Kavita. "Energy measurement capabilities of the LEDA cosmic ray detector." Thesis, McGill University, 1988. http://digitool.Library.McGill.CA:80/R/?func=dbin-jump-full&object_id=64058.
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梁淦章 and Kam-cheung Leung. "Muon detector array to discriminate gamma-ray eas at mountainaltitude." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 1995. http://hub.hku.hk/bib/B31213339.
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Gurtner, Maria [Verfasser]. "Cosmic ray anisotropy study with the AMANDA Neutrino Telescope / Maria Gurtner." Wuppertal : Universitätsbibliothek Wuppertal, 2013. http://d-nb.info/1046604953/34.
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Leung, Kam-cheung. "Muon detector array to discriminate gamma-ray eas at mountain altitude /." Hong Kong : University of Hong Kong, 1995. http://sunzi.lib.hku.hk/hkuto/record.jsp?B17092280.
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Simpson, K. M. "Studies of cosmic ray composition using a hybrid fluorescence detector /." Title page, contents and abstract only, 2001. http://web4.library.adelaide.edu.au/theses/09PH/09phs61261.pdf.
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Alsop, C. "A large detector for cosmic ray abundance and energy measurements." Thesis, University of Bristol, 1988. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.384391.
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Wilkinson, Christopher Richard. "The application of high precision timing in the high resolution fly's eye cosmic ray detector." Title page, contents and abstract only, 1998. http://hdl.handle.net/2440/37715.
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This thesis represents work performed by the author on the development of the High Resolution Fly's Eye (HiRes) detector for the study of extremely high energy (>10 [superscript 18] eV) cosmic rays. Chapter 1 begins with an review of this field. This chapter details the development of the field, the physics questions we seek to answer, and our current understanding based on experimental and theoretical results. It provides the basis for understanding why detectors such as HiRes are being constructed. This review leads into chapter 2, which discuses the development of cosmic ray induced extensive air showers (EAS) and the techniques used to study them. Particular emphasis is placed upon the air fluorescence technique utilised by HiRes. The two site HiRes prototype detector is then discussed in detail in chapter 3. This covers the different components that form the detector, together with details of the calibration performed to extract useful information from the data. Chapter 4 discusses the installation and subsequent testing of GPS based clock systems for the two sites that make up the HiRes prototype detector. The entire timing system was checked, and some previously hidden bugs fixed. This chapter concludes with work performed on the time to digital converter calibration for the second HiRes site. The high relative timing accuracy provided by the GPS clocks allowed the use of timing information in programs to reconstruct the arrival directions of cosmic rays. Chapter 5 covers the development of a program to use geometrical and timing information to reconstruct EAS viewed by both HiRes sites. This chapter concludes with an evaluation of the likely reconstruction accuracy of the new HiRes (stage1) detector. A well reconstructed EAS trajectory is the first step in the determination of more interesting parameters such as primary particle energy. Chapter 6 covers the collation and analysis of EAS viewed by the both sites of the prototype detector. This includes an evaluation of effects such as the atmosphere, and an estimation of the performance of the new (stage 1) HiRes detector based on results with the prototype detector. Finally the conclusions from this thesis are summarised and sugestions made for further follow up work.Thesis (Ph.D.)--Department of Physics and Mathematical Physics, 1998.
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Kirby-Gallagher, Lucy Mary. "A study of underground muons in the Soudan II Detector." Thesis, University of Oxford, 1990. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.276567.
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Bird, David John. "Arrival directions of medium energy cosmic rays in the southern hemisphere /." Title page, contents and summary only, 1991. http://web4.library.adelaide.edu.au/theses/09PH/09pb6178.pdf.
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Stassinakis, Argyrios. "A study of the atmospheric neutrino flavour content using the Soudan 2 detector." Thesis, University of Oxford, 1997. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.388755.
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Choi, HyoJeong. "Cosmic-ray interactions in charged-couple devices in the DMTPC 4-shooter detector." Thesis, Massachusetts Institute of Technology, 2013. http://hdl.handle.net/1721.1/84390.
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Thesis (S.B.)--Massachusetts Institute of Technology, Dept. of Physics, 2013.Cataloged from PDF version of thesis.
Includes bibliographical references (pages 47-48).
The Dark Matter Time Projection Chamber (DMTPC) is a low pressure (CF 4) detector that measures the two-dimensional vector direction of nuclear recoils, and it aims to directly detect dark matter. This paper explores cosmic ray interactions with the four charge-coupled devices (CCDs) of the 4-shooter detector, the largest existing prototype detector in the DMTPC project, by looking at surface runs at MIT with detector voltages off. Through this, the depth of the depletion region of each CCD is found, which can be further used in understanding not only background rejection but also in understanding the relationship between measured CCD counts and energy deposited in the detector.
by HyoJeong Choi.
S.B.
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Bisconti, Francesca [Verfasser], and J. [Akademischer Betreuer] Blümer. "Performance of the cosmic ray fluorescence detector EUSO-TA / Francesca Bisconti ; Betreuer: J. Blümer." Karlsruhe : KIT-Bibliothek, 2017. http://d-nb.info/1137264950/34.
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Tsivras, Sotirios-Ilias. "ALTO Timing Calibration : Calibration of the ALTO detector array based on cosmic-ray simulations." Thesis, Linnéuniversitetet, Institutionen för fysik och elektroteknik (IFE), 2019. http://urn.kb.se/resolve?urn=urn:nbn:se:lnu:diva-79429.
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This thesis describes a timing calibration method for the detector array of the ALTO experiment. ALTO is a project currently at the prototype phase that aims to build a gamma-ray astronomical observatory at high-altitude in the Southern hemisphere. ALTO can be assumed as a hybrid system as each detector consists of a Water Cherenkov Detector (WCD) on top of a Scintillator Detector (SD), providing an increased signal to background discrimination compared to other WCD arrays. ALTO is planned to complement the Very-High-Energy (VHE) observations by the High Altitude Water Cherenkov (HAWC) gamma ray observatory that collects data from the Northern sky. By the time the full array of 1242 detectors is installed to the proposed site, ALTO together with HAWC and the future Cherenkov Telescope Array (CTA) will serve as a state-of-the-art detection system for VHE gamma-rays combining the WCD and the Imaging Atmospheric Cherenkov Telescope (IACT) techniques. When a VHE gamma-ray or cosmic-ray enters the Earth’s atmosphere, it initiates an Extensive Air Shower (EAS). These particles are sampled by the detector array and by checking the arrival times of nearby tanks, the method reveals whether a detector suffers from a time-offset. The data analyzed in this thesis derive from CORSIKA (COsmic Ray SImulation for KAscade) and GEANT4 (GEometry ANd Tracking) simulations of cosmic-ray events within the energy range of 1–1:6TeV, which mainly consist of protons. The high flux of this particular type of cosmic-rays, gives us a tool to statistically evaluate the results generated by the proposed timing calibration method. In the framework of this thesis, I have written code in Python programming language in order to develop the timing calibration method. The method identifies detectors that suffer from time-offsets and improves the reconstruction accuracy of the ALTO detector array. Different Python packages were used to execute different tasks: astropy to read filter-present-write large datasets, numpy (Numerical Python) to make datasets comprehensiveto functions, scipy (Scientific Python) to develop our models, sympy (Symbolic Python) to find geometrical correlations and matplotlib (Mathematical Plotting Library) to draw figures and diagrams. The current version of the method achieves sub-nanosecond accuracy. The next stepis to make the timing calibration more intelligent in order to correct itself. This self correction includes an agile adaptation to the data acquired for long periods of time, in order to make different compromises at different time intervals.
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Perrett, J. C. "Measurements of scintillation and water-Cerenkov detector densities in extensive air showers produced by 10sup(16) - 5x10sup(19) eV cosmic rays." Thesis, University of Leeds, 1985. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.355950.
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Kalousis, Leonidas. "Calibration of the Double Chooz detector and cosmic background studies." Phd thesis, Université de Strasbourg, 2012. http://tel.archives-ouvertes.fr/tel-00979573.
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Double Chooz is a short-baseline experiment, located at the Chooz power plant, designed to observe the neutrino oscillation signal controlled by the θ13 mixing angle. Part of my scientific research, as a graduate student, was directed towards the development of the software needed for the calibration of the Double Chooz Inner Veto and the analysis of the data associated with this task. I was responsible for the quality tests performed in every photomultiplier prior to its installation. I completed all the necessary measurements and analysed the data, extracting the first set of gains and determining the nominal high voltage values needed to be applied in all photomultipliers. All this information served as valuable input to the detector configuration. I was also responsible for the Inner Veto photomultiplier gain analysis during the first months of data taking. I was also very actively involved in data analysis and the estimations of the various sources of background. I initiated a number of methods to isolate and study the cosmic muon events that activate the detector. Additionally I worked on the estimation of the fast neutron rate registered in the detector. The techniques I put forward played a key role and were used in the first Double Chooz publication. Finally, I developed a set of algorithms to identify and reject an instrumental background, relevant for the Double Chooz detector using topological information of the deposited charge.
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Nkosi, Godfrey Sibusiso. "A study of cosmic ray anisotropies in the heliosphere / Godfrey Sibusiso Nkosi." Thesis, North-West University, 2006. http://hdl.handle.net/10394/1627.
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Smith, Mark A. "A detector to measure 9Li production rate in liquid scintillator at the earth’s surface by cosmic ray muons." Diss., Kansas State University, 2009. http://hdl.handle.net/2097/1542.
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Doctor of PhilosophyDepartment of Physics
Glenn A. Horton-Smith
The next generation of nuclear fission reactor based neutrino experiments seeking to measure the Theta-13 mixing angle rely upon measurements made by detectors placed close to the reactor, and therefore less shielded from cosmic ray muons by the earth. 9Li production in liquid scintillator by these cosmic ray muons becomes a serious problem for these experiments that must be dealt with since the 9Li production rate is still a significant fraction of the neutrino interaction rate. This 9Li background reduces the experiment’s sensitivity to measure the Theta-13 mixing angle. This thesis discusses a small detector designed to measure the 9Li production rate in liquid scintillator at the earth’s surface by cosmic ray muons. The detector was designed, built, and finally, calibrated. The ability to find the signals necessary to actually measure the 9Li production rate is shown, establishing that this detector will be able to measure the production rate. A 90% significance level upper limit for the 9Li-like production rate, based on only 3.5 days worth of data, is reported as 213 9Li-like events per day per ton.
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Porelli, Andrea. "TAIGA-HiSCORE: a new wide-angle air Cherenkov detector for multi-TeV gamma-astronomy and cosmic ray physics." Doctoral thesis, Humboldt-Universität zu Berlin, 2020. http://dx.doi.org/10.18452/21610.
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Der TAIGA Detektor (“Tunka Advanced Instrument for cosmic ray physics and Gamma Astronomy”) testet eine neue Nachweismethode der erdgebundenen Cherenkov Gamma Astronomie fuer 10TeV bis einige PeV, und fuer kosmische Strahlung oberhalb 100TeV: die Kombination abbildender und nicht-abbildender Cherenkov Detektoren in einem hybriden System.
Im Fokus der Arbeit steht TAIGA-HiSCORE - ein Cherenkov Detektorfeld mit grosser Apertur zur Messung der Zeitstruktur der Cherenkovlichtfront in atmosphaerischen Luftschauern (EAS). Die Praezisonsvermessung der Schauerrichtung basiert auf
(1) sub-nsec Zeitsynchronisation aller Detektoren, und
(2) einer neuentwickelten Zeitkalibrationsmethode.
Die Genauigkeit wird bestimmt mit experimentellen und simulierten EAS-Daten, spezieller LED-Kalibration und dem LIDAR Laserstrahl aus der International Space Station (ISS).
Mit den HiSCORE9 Daten (2013-2014) wird die sub-nsec Zeitsynchronisation durch das White Rabbit Zeitsystem unter realen Bedingungen nachgewiesen. Eine neue, auch fuer grosse Cherenkov-Detektorfelder praktikable Zeitoffset-Kalibration aller Detektoren wurde entwickelt, und fuer HiSCORE28 (2015-2018) angewandt. Diese hybride Kalibration basiert auf EAS-Ereignissen und direkter LED-Kalibration fuer lediglich eine begrenzte Zahl von Detektoren.
Die Genauigkeit der Luftschauer-Richtungsrekonstruktion wird ueber die “Schachbrett-Methode” MC-unabhaengig bestimmt zu 0.4° an der Energieschwelle (50TeV) und <= 0.2° fuer > 100TeV.
Eine wichtige Zufallsentdeckung war mit HiSCORE28 moeglich: der Laser des ISS-CATS-Lidars wurde in richtungsrekonstruierten Daten von HiSCORE28 nachgewiesen. Mit den “ISS Ereignissen” gelang es, sowohl die Rekonstruktionsgenauigkeit von HiSCORE, als auch das “absolute pointing” zu messen (<=0.1°) - besonders wichtig, da eine starke Gamma-Quelle im Datensatz bisher nicht nachgewiesen wurde. Im Schlussteil der Arbeit wird ein Methode zur Punktquellensuche im gesamten Gesichtsfeld von TAIGA-HiSCORE vorgestellt.The TAIGA (Tunka Advanced Instrument for cosmic ray physics and Gamma Astronomy) detector is a new ground-based Cherenkov detection technology for gamma-astronomy from 10TeV up to several PeV, and cosmic rays (CR) above 100TeV. The main topic of this work is TAIGA-HiSCORE, the wide-aperture air Cherenkov timing array. The focus is on precision extensive air shower (EAS) arrival direction reconstruction, achieved by (1) sub-nsec time-synchronization between the array stations, and (2) a newly developed array time calibration procedure. The performance is verified using simulated and experimental data from EAS, dedicated LED calibration, and a LIDAR laser beam from the International Space Station (ISS). The analysis of the HiSCORE 9 data (2013-14), collected with a data acquisition system (DAQ) based on the White Rabbit (WR) timing system, allows to verify the sub-nsec time synchronization between the array stations. The analysis of HiSCORE 28 data (2015-2018) addresses the problem of achieving an easy-to-perform time calibration for large area ground-based Cherenkov array. A new "hybrid" calibration method is developed, which makes use of EAS data, and requires direct LED calibration of only a few array stations. The "chessboard" method is applied on the reconstructed data to obtain a MC-independent estimation of the detector angular resolution, found to be 0.4° at threshold (~50TeV) and <= 0.2° above 100TeV. A serendipitous discovery was made in this work: a signal from the CATS-LIDAR on-board the ISS was found in the HiSCORE 28 data. These "ISS-events" are used to verify the detector performance, in particular the absolute angular pointing (<= 0.1°), particularly important since a strong gamma point source has not yet been detected by the TAIGA-HiSCORE. The final part of the work presents a first preliminary approach to a wide aperture point source analysis, developed for the TAIGA-HiSCORE in stand-alone operation.
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Smith, Mark A. "A detector to measure ⁹Li production rate in liquid scintillator at the earth's surface by cosmic ray muons." Manhattan, Kan. : Kansas State University, 2009. http://hdl.handle.net/2097/1542.
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Ngobeni, Mabedle Donald. "Aspects of the modulation of cosmic rays in the outer heliosphere / by Mabedle Donald Ngobeni." Thesis, North-West University, 2006. http://hdl.handle.net/10394/97.
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A time-dependent two-dimensional (2D) modulation model including drifts, the solar wind
tennination shock (TS) with diffusive shock acceleration and a heliosheath based on the
Parker (1965) transport equation is used to study the modulation of galactic cosmic rays
(GCRs) and the anomalous component of cosmic rays (ACRs) in the heliosphere. In
particular, the latitude dependence of the TS compression ratio and injection efficiency of the
ACRs (source strength) based on the hydrodynamic modeling results of Scherer et al. (2006)
is used for the first time in a modulation model. The subsequent effects on differential
intensities for both GCRs and ACRs are illustrated, comparing them to the values without a
latitude dependence for these parameters. It is found that the latitude dependence of these
parameters is important and that it enables an improved description of the modulation of
ACRs beyond the TS. With this modeling approach (without fitting observations) to the
latitude dependence of the two parameters, it is possible to obtain a TS spectrum for ACRs at
a polar angle of B = 55" that qualitatively approximates the main features of the Voyager 1
observations. This positive result has to be investigated further. Additionally, it is shown that
the enhancement of the cosmic ray intensity just below the cut-off energy found for the ACR
at the TS in an A < 0 magnetic polarity cycle in the equatorial plane with the latitude
independent scenario, disappears in this region when the latitude dependence of the
compression ratio and injection efficiency is assumed. Subsequent effects of these scenarios
are illustrated on the global anisotropy vector of both GCRs and ACRs as the main theme of
this work. For this purpose the radial and latitudinal gradients for GCRs and ACRs were
accurately computed. The radial and latitudinal anisotropy components were then computed
as a function of energy, radial distance and polar angle. It is also the first time that the
anisotropy vector is comprehensively calculated in such a global approach to cosmic ray
modeling in the heliosphere, in particular for ACRs. It is shown that the anisotropy vector
inside (up-stream) and outside (down-stream) the TS behaves in a complicated way, so care
must be taken in interpreting it. It is found that the latitude dependence of the two mentioned
parameters can alter the direction (sign) of the anisotropy vector. Its behaviour beyond the TS
is markedly different from inside the TS, mainly because of the slower solar wind velocity,
with less dependence on the magnetic polarity cycles.Thesis (M.Sc. (Physics))--North-West University, Potchefstroom Campus, 2007.
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Greim, Roman Verfasser], Stefan [Akademischer Betreuer] Schael, and Christopher Henrik V. [Akademischer Betreuer] [Wiebusch. "Measurement of the charged cosmic ray flux at solar minimum with the PERDaix detector / Roman Greim ; Stefan Schael, Christopher Wiebusch." Aachen : Universitätsbibliothek der RWTH Aachen, 2016. http://d-nb.info/1130589935/34.
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Köhli, Markus Otto [Verfasser], and Ulrich [Akademischer Betreuer] Schmidt. "The CASCADE 10B thermal neutron detector and soil moisture sensing by cosmic-ray neutrons / Markus Otto Köhli ; Betreuer: Ulrich Schmidt." Heidelberg : Universitätsbibliothek Heidelberg, 2019. http://d-nb.info/1193252415/34.
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Köhli, Markus [Verfasser], and Ulrich [Akademischer Betreuer] Schmidt. "The CASCADE 10B thermal neutron detector and soil moisture sensing by cosmic-ray neutrons / Markus Otto Köhli ; Betreuer: Ulrich Schmidt." Heidelberg : Universitätsbibliothek Heidelberg, 2019. http://nbn-resolving.de/urn:nbn:de:bsz:16-heidok-269692.
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Greim, Roman [Verfasser], Stefan Akademischer Betreuer] Schael, and Christopher Henrik V. [Akademischer Betreuer] [Wiebusch. "Measurement of the charged cosmic ray flux at solar minimum with the PERDaix detector / Roman Greim ; Stefan Schael, Christopher Wiebusch." Aachen : Universitätsbibliothek der RWTH Aachen, 2016. http://d-nb.info/1130589935/34.
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Porelli, Andrea [Verfasser]. "TAIGA-HiSCORE: a new wide-angle air Cherenkov detector for multi-TeV gamma-astronomy and cosmic ray physics / Andrea Porelli." Berlin : Humboldt-Universität zu Berlin, 2020. http://d-nb.info/1215095546/34.
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Tao, Li. "Measurement of the cosmic lepton and electron fluxes with the AMS detector on board of the International Space Station. Monitoring of the energy measurement in the calorimeter." Thesis, Université Grenoble Alpes (ComUE), 2015. http://www.theses.fr/2015GRENY016/document.
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Le Spectromètre Magnétique Alpha (AMS) est un détecteur de particules installé à bord de la Station Spatiale Internationale ; il enregistre des données depuis mai 2011. L'expérience a pour objectif d'identifier la nature des rayons cosmiques chargés et des photons et de mesurer leur flux dans la gamme d'énergie du GeV au TeV. Ces mesures permettent d'affiner les modèles de propagation de rayons cosmiques, d'effectuer une recherche indirecte de matière noire, et de chercher l'antimatière primordiale (anti-hélium). Dans ce mémoire, les données des premières années ont été utilisées pour mesurer les flux d'électrons et de leptons (électrons + positons) dans la gamme d'énergie de 0.5 GeV à 700 GeV. L'identification d'électrons nécessite une séparation électrons/protons de l'ordre de 104, obtenue par l'utilisation conjointe des estimateurs de différents sous-détecteurs d'AMS, en particulier du calorimètre électromagnétique (ECAL), du trajectomètre et du détecteur à radiation de transition (TRD). Dans cette analyse, les nombres d'électrons et de leptons sont estimés par un ajustement des distributions de l'estimateur du calorimètre et vérifiés en utilisant l'estimateur du TRD : 11 millions leptons ont été sélectionnés et analysés. Les incertitudes systématiques sont déterminées en variant les coupures de sélection et la procédure d'ajustement. L'acceptance géométrique du détecteur et les efficacités de sélection sont estimées grâce aux données de simulation. Les différences observées sur les échantillons de contrôle issus des données permettent de corriger la simulation. Les incertitudes systématiques associées à ces corrections sont établies en variant les échantillons de contrôle. Au total, à 100 GeV (resp. 700 GeV), l'incertitude statistique du flux de leptons est 2% (30%) et l'incertitude systématique est 3% (40%). Comme les flux se comportent globalement en loi de puissance en fonction de l'énergie, il est important de maitriser la calibration en énergie. Nous avons contrôlé in situ la mesure en énergie du calorimètre en comparant les électrons des données de vol et les données de tests en faisceaux, en utilisant en particulier la variable E/p ou p est la quantité de mouvement mesurée par le trajectomètre. Une deuxième méthode de calibration absolue à basse énergie, indépendante du trajectomètre, basée sur l'effet de la coupure géomagnétique a été développée. Deux modèles de prédiction de la coupure géomagnétique, l'approximation Störmer et le modèle IGRF, ont été testés et comparés. Ces deux méthodes ont permis de contrôler la calibration en énergie à 2% et de vérifier la stabilité des performances du calorimètre dans le tempsThe Alpha Magnetic Spectrometer (AMS) is a particle detector installed on the International Space Station; it starts to record data since May 2011. The experiment aims to identify the nature of charged cosmic rays and photons and measure their fluxes in the energy range of GeV to TeV. These measurements enable us to refine the cosmic ray propagation models, to perform indirect research of dark matter and to search for primordial antimatter (anti-helium). In this context, the data of the first years have been utilized to measure the electron flux and lepton flux (electron + positron) in the energy range of 0.5 GeV to 700 GeV. Identification of electrons requires an electrons / protons separation power of the order of 104, which is acquired by combining the information from different sub-detectors of AMS, in particular the electromagnetic calorimeter (ECAL), the tracker and the transition radiation detector (TRD). In this analysis, the numbers of electrons and leptons are estimated by fitting the distribution of the ECAL estimator and are verified using the TRD estimator: 11 million leptons are selected and analyzed. The systematic uncertainties are determined by changing the selection cuts and the fit procedure. The geometric acceptance of the detector and the selection efficiency are estimated thanks to simulated data. The differences observed on the control samples from data allow to correct the simulation. The systematic uncertainty associated to this correction is estimated by varying the control samples. In total, at 100 GeV (resp. 700 GeV), the statistic uncertainty of the lepton flux is 2% (30%) and the systematic uncertainty is 3% (40%). As the flux generally follows a power law as a function of energy, it is important to control the energy calibration. We have controlled in-situ the measurement of energy in the ECAL by comparing the electrons from flight data and from test beams, using in particular the E/p variable where p is momentum measured by the tracker. A second method of absolute calibration at low energy, independent from the tracker, is developed based on the geomagnetic cutoff effect. Two models of geomagnetic cutoff prediction, the Störmer approximation and the IGRF model, have been tested and compared. These two methods allow to control the energy calibration to a precision of 2% and to verify the stability of the ECAL performance with time
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Kraus, Manuel [Verfasser], Stefan [Akademischer Betreuer] Funk, and Stefan [Gutachter] Funk. "The Cosmic-Ray Electron Anisotropy Measured with H.E.S.S. and Characterization of a Readout System for the SST Cameras of CTA / Manuel Kraus ; Gutachter: Stefan Funk ; Betreuer: Stefan Funk." Erlangen : Friedrich-Alexander-Universität Erlangen-Nürnberg (FAU), 2018. http://d-nb.info/1159771219/34.
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Halliday, Robert Paul. "Electronics and Timing for the AugerPrime Upgrade and Correlation of Starburst Galaxies with Arrival Directions of Ultra High Energy Cosmic Rays." Case Western Reserve University School of Graduate Studies / OhioLINK, 2019. http://rave.ohiolink.edu/etdc/view?acc_num=case1553599216169462.
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Reichhart, Lea. "ZEPLIN-III direct dark matter search : final results and measurements in support of next generation instruments." Thesis, University of Edinburgh, 2013. http://hdl.handle.net/1842/7914.
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Astrophysical observations give convincing evidence for a vast non-baryonic component, the so-called dark matter, accounting for over 20% of the overall content of our Universe. Direct dark matter search experiments explore the possibility of interactions of these dark matter particles with ordinary baryonic matter via elastic scattering resulting in single nuclear recoils. The ZEPLIN-III detector operated on the basis of a dualphase (liquid/gas) xenon target, recording events in two separate response channels { scintillation and ionisation. These allow discrimination between electron recoils (from background radiation) and the signal expected from Weakly Interacting Massive Particle (WIMP) elastic scatters. Following a productive first exposure, the detector was upgraded with a new array of ultra-low background photomultiplier tubes, reducing the electron recoil background by over an order of magnitude. A second major upgrade to the detector was the incorporation of a tonne-scale active veto detector system, surrounding the WIMP target. Calibration and science data taken in coincidence with ZEPLIN-III showed rejection of up to 30% of the dominant electron recoil background and over 60% of neutron induced nuclear recoils. Data taking for the second science run finished in May 2011 with a total accrued raw fiducial exposure of 1,344 kg days. With this extensive data set, from over 300 days of run time, a limit on the spin-independent WIMP-nucleon cross-section of 4.8 10-8 pb near 50 GeV/c2 WIMP mass with 90% confidence was set. This result combined with the first science run of ZEPLIN-III excludes the scalar cross-section above 3.9 10-8 pb. Studying the background data taken by the veto detector allowed a calculation of the neutron yield induced by high energy cosmic-ray muons in lead of (5.8 0.2) 10-3 neutrons/muon/(g/cm2) for a mean muon energy of 260 GeV. Measurements of this kind are of great importance for large scale direct dark matter search experiments and future rare event searches in general. Finally, this work includes a comprehensive measurement of the energy dependent quenching factor for low energy nuclear recoils in a plastic scintillator, such as from the ZEPLIN-III veto detector, increasing accuracy for future simulation packages featuring large scale plastic scintillator detector systems.
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Peixoto, Carlos Jose Todero. "Reconstrução de chuveiros atmosféricos extensos detectados pelo Observatório Pierre Auger utilizando métodos robustos." [s.n.], 2008. http://repositorio.unicamp.br/jspui/handle/REPOSIP/277465.
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Orientador: Carlos Ourivio EscobarTese (doutorado) - Universidade Estadual de Campinas, Instituto de Fisica Gleb Wataghin
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Resumo: Desde os primeiros Raios Cósmicos de alta energia detectados por Pierre Auger na década de 30, toda a comunidade de Física de Radiação Cósmica procura técnicas matemáticas e métodos estatísticos mais adequados para analisar estes eventos. Estes processos de análise são imprescindíveis na estimativa da energia da partícula primária, bem como no cálculo do ângulo de chegada q . A estimativa desta energia e do ângulo q é o final de toda uma rede de trabalho e o começo de uma nova linha de pesquisa na busca pelas possíveis fontes que produziram tais eventos. Ao longo deste trabalho refizemos o princípio de reconstrução dos "chuveiros de Auger", os chamados "Chuveiros Atmosféricos Extensos" ( C.A.E.), utilizando um conceito relativamente novo de estatística, hoje denominada Estatística Robusta. O Método dos Mínimos Quadrados ou Least Square -LS, apresentado por Gauss e Legendre, possuía limitações que eles próprios já reconheciam e tentaram resolver, sem sucesso. Desde fins do século XVIII e come¸ co do século XIX, os métodos estritamente paramétricos, em especial o Método dos Mínimos Quadrados e a média aritmética, foram questionados quando utilizados para descrever distribuições pouco comportadas ou com grandes utuações. Algumas das principais questões estavam relacionadas a como tratar pontos muito distantes da distribuição principal (os chamados outliers) e como estes influenciavam a própria distribuição. A saída convencional mais utilizada foi a rejeição dos outliers e de pontos que apresentassem grandes desvios em relação a média. Porém, a perda de informações sobre a própria distribuição tornava-se inevitável. O modelo paramétrico mostrou-se apenas uma aproximação da realidade, uma vez que as flutuações, apesar de serem consideradas, não são "bem-vindas"; são vistas apenas como um erro inerente à observação. Então, no fim do século XIX apareceram as primeiras tentativas de extrair informação das flutuações, classificando-as e as considerando parte integral da descrição da distribuição. Se um método estatístico for capaz de descrever os dados observados, incluindo e classificando as flutuações inerentes, este passa a ser conhecido como "Método Robusto" ou "Estatística Robusta", onde a nomenclatura "Robusta" está relacionada à capacidade do método ou modelo de "resistir" às flutuações fornecendo uma descrição da realidade com razoável independência destas mesmas flutuações. Com base em dois métodos robustos, Mínima Mediana Quadrada (Least Median Square - LMS) e Mínimos Quadrados "Aparados" (Least Trimmed Square - LTS), aplicamos estes nos ajustes da Função Distribuição Lateral de Chuveiros (Lateral Distribution Function - LDF) extraindo o valor de S 1000, parâmetro necessário para estimar a energia da partícula primária. Os valores para S1000 calculados a partir de estatística convencional (Mínimos Quadrados) e estatística robusta (LMS e LTS) são comparados. O valor de S1000, para chuveiros de mesma energia, depende do ângulo q dos primários, já que o CAE sofre atenuação na atmosfera, atenuação esta tanto maior quanto maior, for q . Para levar em conta a atenuação no cálculo do espectro de energia, em que todos os ângulos de chegada são considerados (até 60 graus), é introduzido o parâmetro S38, onde 38 graus é a mediana dos dados do Auger. A atenuação é calculada usando-se o método do Constant Intensity Cut (CIC) o qual depende da validade de várias hipóteses. As três hipóteses supostas pela Colaboração Auger são apresentadas neste trabalho. Correlacionamos, assim, todos os novos valores de S38 com os valores da chamada "Energia Híbrida", obtida diretamente do programa de análise da Colaboração Auger. Esta correlação nos permite recorrigir a energia com base em detecção híbrida, que é a grande vantagem do Observatório Pierre Auger. Esta correlação nos permite estabelecer a escala de energia ou calibração do detector de superfície com base na determinação calorimétrica da energia feita pelo detector de flurescência, que é o grande avançoo trazido para o campo pelo Obvservatório Pierre Auger. Com os novos resultados de energia, refizemos os cálculos de minimização para a correlação de radiação cósmica com fontes extra-galácticas obtendo correlações que não estão em correspondência biunívoca com aquelas obtidas pelo método convencional de análise. Por fim fazemos uma análise das próprias estações outliers tentando extrair alguma informação relacionada à performance do detector de superfície. Os apêndices incluídos após as conclusões foram colocados neste trabalho apenas por motivos didáticos como consulta rápida para o leitor leigo em métodos de detecção de radiação cósmica
Abstract: Since the first ultra high-energy cosmic rays detected by Pierre Auger (the 30s) the entire community of Physics of Cosmic Rays search for mathematical techniques and more appropriate statistical methods to analyze these events. These analysis processes are essential for the estimate of the energy of the primary particle as well as in the calculation of the angle of arrival q . The estimate of the energy and the angle q is the end of a long chain of analysis and the beginning of a new line of research in the search for the possible sources that produced such events. Throughout this work we re-analysed the reconstruction chain of the "Auger showers", the socalled "Extensive Air Showers - EAS", using a relatively new concept of statistics, known as Robust Statistics. The Least Square Method - LS, presented by Gauss and Legendre had limitations already recognized by themselves who tried to overcome them without success. Since the end of the eighteenth century and beginning of the nineteenth century, strictly parametric methods, especially the Least Squares and the arithmetic average, were questioned when used to describe distributions with bad behavior or with large uctuations. Some of the main issues were related to how to deal with points far way from the main distribution (the so-called outliers) and how it in uenced the main distribution. The more conventional way out used was the rejection of the outliers and points that produced large deviations from average. But the loss of information about the distribution was inevitable. The parametric model proved to be only an approximation of reality, since uctuations, despite being considered, are not "welcome"; are seen only as an error inherent in observation. Then, at the end of the nineteenth century there appeared the first attempts to extract information from uctuations sorting them out and considering them as an integral part of the description of the distribution. Whether a statistical method is able to describe observed data, including and sorting the uctuations inherent, then becomes known as "Robust Method" or "Robust Statistic", where the nomenclature "Robust" is related the ability of the method or model to "Resist" the uctuations by providing a description of reality with reasonable independence these same uctuations. Based on two robust methods: Least Median Square - LMS and Least Trimmed Square - LTS; we apply these to adjust the Lateral Distribution Function - LDF extracting the value of S1000, parameter needed to estimate the energy of the primary particle. The values for S1000 calculated from conventional statistic (Least Square) and robust statistic (LMS and LTS) are compared. The parameter S1000 is dependent on the angle of arrival of the shower, then we apply a correction factor called S38. This correlates S1000 and and, currently, there are several ways to calculate this factor. The three hypotheses most used by Auger Collaboration are presented in this work. We then correlate all new values of S38 with the values of the so-called "Hybrid Energy", obtained directly from analysis software of the Auger Collaboration. This relationship allows us to correct the energy based on hybrid detection that is great advantage of the Pierre Auger Observatory. This relationship allows us to establish the energy scale or calibration of the surface detector on the basis of the calorimetric determination of the energy done by the uorescence detector which is the great advancement brought to the field by the Pierre Auger Observatory. With the new results for the energy we reanalysed the the correlation with extra-galactic sources of cosmic ray getting new correlations, which are absent in the conventional methods of analysis. Finally we make an analysis of the surface stations outliers by themselves trying to extract some information relevant for their performance. Appendices included after the conclusions were placed in this work only for a rapid consultation by lay readers in methods of detection of cosmic rays
Doutorado
Teorias Especificas e Modelos de Interação ; Sistematica de Particulas ; Raios Cosmicos
Doutor em Ciências
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Ahmad, Salleh. "Développement et réalisation d'un circuit de microélectronique pour le détecteur spatial de rayons cosmiques JEM-EUSO." Thesis, Paris 11, 2012. http://www.theses.fr/2012PA112327.
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Extreme Universe Space Observatory on Japanese Experiment Module (JEM-EUSO) est conçu comme l’expérience de rayons cosmiques de prochaine génération pour observer les particules hautement énergétiques au-dessus de 10²⁰ eV. Le projet est mené par RIKEN et soutenu par une collaboration de plus de 200 membres provenant de 13 pays. Cet observatoire, sous la forme d'un télescope fluorescent, sera arrimé à la Station Spatiale internationale (ISS) pour un lancement prévu en 2017. En observant les gerbes atmosphériques produites dans la troposphère, à une altitude de 400 km, cet observatoire de rayons cosmique offrira une grande surface de détection, qui est au moins 100 fois supérieur que le plus grand détecteur de rayons cosmiques jamais construit. La surface focale de JEM-EUSO sera équipée d'environ 5000 unités de photomultiplicateur multianode 8x8 pixels (MAPMT). Un circuit intégré (ASIC), connu sous le nom SPACIROC, a été proposé pour la lecture du MAPMT. Cet ASIC de 64 voies propose des fonctionnalités comme le comptage de photons, la mesure des charges et le transfert de données à haute vitesse. Par-dessus tout, cet ASIC doit peu consommé afin de respecter la contrainte de puissance de JEM-EUSO. Réalisé en utilisant la technologie AMS Silicium-Germanium (SiGe) 0,35 µm, cet ASIC intègre 64 canaux de comptage de photons rapides (Photon Counting). La résolution de temps pour le comptage de photons est de 30 ns, ce qui permettra d’atteindre la valeur maximale comptage qui est de l'ordre de 10⁷ photons / s. Le système de mesure de charge est basé sur le Time-Over-Threshold qui offre 8 canaux de mesure. Chaque canal de mesure est une somme des 8 pixels du MAPMT et il est prévu que ce système est capable de mesurer jusqu'à 200 pC. La partie numérique fonctionne en continu et gère la conversion des données de chaque voie des blocs de Photon Counting et Time-Over-Threshold. Les données numériques sont transmises par l'intermédiaire de liaisons parallèles dédiées et ces opérations sont effectuées pendant une fenêtre de communication ou « Gate Time Unit » (GTU) de fréquence 400 kHz. Le taux de transfert des données d’ASIC avoisine les 200 Mbps ou 576 bits / GTU. La dissipation de puissance est strictement inférieure à 1 mW par canal ou 64 mW pour l'ASIC. Le premier prototype de SPACIROC a été envoyé pour fabrication en Mars 2010 au Centre Multi Projet (CMP). Des puces nues et packagés ont été reçues en Octobre 2010, ce qui a débuté la phase de caractérisation de cet ASIC. Après une phase de test réussie, des puces SPACIROC ont été intégrés dans l'électronique frontale d'un instrument pour détecter les sursauts gamma - Ultra Fast Flash Observatoire (UFFO) qui va être lancé en 2013. Vers la fin de l'année 2012, des cartes électroniques frontales conçues autour des puces SPACIROC ont été fabriqués pour le projet EUSO-Balloon. Ce projet de vol en ballon stratosphérique à une altitude de 40 km servira comme le démonstrateur technologique et l'ingénierie d'un instrument miniaturisé JEM-EUSO. La deuxième génération de cet ASIC a été envoyée à la fonderie en Décembre 2011. Ce second prototype, SPACIROC2, a été testé à partir de mai 2012. Les principales améliorations sont les suivantes: la consommation d'énergie a été revue à la baisse, ainsi que l'amélioration de la résolution temporelle de Photon Counting et l'extension de la gamme dynamique pour le module Time-Over-Threshold. Les mesures en cours ont montré que SPACIROC2 présente un bon comportement général et apporte des améliorations par rapport à son prédécesseurExtreme Universe Space Observatory on Japanese Experiment Module (JEM-EUSO) is conceived as the next generation cosmic rays experiment for observing the highly energetic particles above 5.10¹⁹ eV. The project is lead by RIKEN and supported by an active collaboration of more than 200 members from 13 countries. This observatory, in the shape of a wide field-of-view UV telescope, will be attached to the International Space Station (ISS) for a planned launch in 2017. Observing the Air Showers generated in troposphere from an altitude of 400 km, this space based cosmic rays experiment will offer a very large instantaneous detection surface, which is at least 100 times bigger than the largest land based cosmic rays observatory. The detection surface of JEM-EUSO will be equipped with around 5000 units of 8x8 pixels Multianode Photomultiplier (MAPMT). A radiation hardened mixed signal application-specific integrated circuit (ASIC), known as SPACIROC, has been proposed for reading out the MAPMT. This ASIC features 64-channel analog inputs, fast photon counting capabilities, charge measurements and high-speed data transfer. Above all, the power dissipation of this ASIC is required to be very low in order to comply with the strict power budget of JEM-EUSO. By taking the advantages of high speed AMS 0.35 µm Silicon-Germanium (SiGe) process, this ASIC integrates 64 fast Photon Counting channels. The photon counting time resolution is 30 ns, which allows the theoretical counting rate in the order of 10⁷ photons/s. The charge measurement system is based on Time-Over-Threshold which offers 8 measurement channels. Each measurement channel is composed of 8 pixels of the MAPMT and it is expected that this system will measure up to 200 pC. The digital part is then required to operate continuously and handles data conversion of each Photon Counting and Time-Over-Threshold channel. For the first version of this ASIC, one channel measurement channel for the dynode is also available. The digital data are transmitted via dedicated parallel communication links and within the defined Gate Time Unit (GTU) of 400 kHz frequency. The ASIC data output rate is in the vicinity of 200 Mbps or 576 bits/GTU. The power dissipation is kept strictly below 1 mW per channel or 64 mW for the ASIC. The first prototype of SPACIROC was sent for tapeout in March 2010 through Centre Multi Projet (CMP) prototyping services. The packaged ASICs and bare dies have been received in October 2010 which marked the characterization phase of this chip. After successful testing phase, SPACIROC chips were integrated into the front-end electronics of an instrument pathfinder for detecting the gamma ray bursts – Ultra Fast Flash Observatory (UFFO) which is foreseen to be launched in 2013. Towards the end of 2012, front-end board designed around SPACIROC chips have been fabricated for the EUSO-Balloon project. This balloon borne project will serve as a technical and engineering demonstrator of a fully miniaturized JEM-EUSO instrument which will be flown to the stratosphere at the altitude of 40 km. The second tapeout of this ASIC was done in December 2011. This second prototype, SPACIROC2, was tested from May 2012. The main improvements are as follows: lower power consumption due to better power management, enhancement in Photon Counting time resolution and extension the Time-Over-Threshold maximum input rate. The ongoing tests have shown that SPACIROC2 exhibits a good overall behavior and improvement compared to its predecessor
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Bellido, Caceres Jose Alfredo. "Anisotropy studies of the HiRes EHECR." Thesis, 2002. http://hdl.handle.net/2440/79723.
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In this thesis I present studies of the EHtrCR (E > 10¹⁸ eV) arrival directions using the data from the HiRes cosmic ray detector. The aims are to look for evidence of any cosmic ray anisotropy in any particular direction, especially in the directions of a priori, selected source candidates (Cygnus X-3, Virgo A, the AGASA triplet and the supergalactic plane). To perform these anisotropy studies it was necessary to determine in advance the uncertainties of the reconstructed cosmic ray arrival directions. The early chapters of my thesis give an introduction to cosmic ray physics and a review of anisotropy studies undertaken by several groups. In Chapter 4, I describe in some detail the High Resolution Fly's Eye (HiRes) detector. In Chapters 5, 6, and 7, I present details of the geometry reconstruction of the arrival directions of cosmic rays (monocular and stereo events) and estimations of the uncertainties in the reconstructed arrival directions. In Chapter 8, I present the results of the arrival direction anisotropy analysis. Finally in Chapter 9, I present a summary and conclusions.Thesis (Ph.D.) -- University of Adelaide, Dept. of Physics and Mathematical Physics, 2002
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Chen, Chi-Jung, and 陳紀榮. "Developing a multi-channel cosmic ray detector system." Thesis, 2011. http://ndltd.ncl.edu.tw/handle/26579469891957068806.
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碩士國立聯合大學
電子工程學系碩士班
99
Particle Astrophysics is very important in universe study by watchingγ ray, cosmic ray and neutrinos; We have developed a cosmic ray detector system in a cost-effective way, and with a friendly web interface which can be used by the researchers to monitor, process the data by internet. Meanwhile, we also try to promote this system to high school for fundamental education of particle astrophysics. With auto-calibration of system parameter and aging warning of detector, the users can maintain the system with a minimum cost. It’s very important in promotion.
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Simpson, Kenneth Mark. "Studies of Cosmic Ray Composition using a Hybrid Fluorescence Detector." 2001. http://hdl.handle.net/2440/37751.
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This thesis describes several aspects of cosmic ray composition studies using the Utah Fly's Eye and High Resolution Fly's Eye (HiRes) detectors. The Fly's Eye detector utilises the atmospheric fluorescence technique to measure the development of cosmic ray cascades as they pass through the atmosphere. This is complementary to the surface array technique, as used by the Akeno experiment in Japan, which measures the electromagnetic and muon content of air showers at a single observation level. For some time it was thought that Fly's Eye and Akeno gave inconsistent composition results. In Chapter 4 I show that the inconsistency is due, for the most part, to a difference in the assumptions made about hadronic interactions. In Chapter 5 I present analysis of the composition between 10^17 and 10^18 eV using the prototype High Resolution Fly's Eye (HiRes) detector in coincidence with the Michigan Muon Array (MIA). The hybrid nature of these measurements gives us more information about cosmic ray showers than either technique on its own. The consistency or otherwise of the composition measured by the two detectors is discussed. Finally, in Chapter 6, I discuss a method of extracting the total proton-proton cross section from the cosmic ray data. This information is of interest because it is derived at centre of mass energies much higher (by at least an order of magnitude) than those currently accessible by collider experiments. I present a preliminary calculation of the cross section using the HiRes/MIA hybrid data set.Thesis (Ph.D.)--Department of Physics and Mathematical Physics, 2001.
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Simpson, Kenneth Mark. "Studies of cosmic ray composition using a hybrid fluorescence detector." Thesis, 2001. http://hdl.handle.net/2440/37751.
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This thesis describes several aspects of cosmic ray composition studies using the Utah Fly's Eye and High Resolution Fly's Eye (HiRes) detectors. The Fly's Eye detector utilises the atmospheric
fluorescence technique to measure the development of cosmic ray cascades as they pass through the atmosphere. This is complementary to the surface array technique, as used by the Akeno experiment in Japan, which measures the electromagnetic and muon content of air showers at a single observation level. For some time it was thought that Fly's Eye and Akeno gave inconsistent composition results. In Chapter 4 I show that the inconsistency is due, for the most part, to a difference in the assumptions made about hadronic interactions. In Chapter 5 I present analysis of the composition between 10^17 and 10^18 eV using the prototype High Resolution Fly's Eye (HiRes) detector in coincidence with the Michigan Muon Array (MIA). The hybrid nature of these measurements gives us more information about cosmic ray showers than either technique on its own. The consistency or otherwise of the composition measured by the two detectors is discussed. Finally, in Chapter 6, I discuss a method of extracting the total proton-proton cross section from the cosmic ray data. This information is
of interest because it is derived at centre of mass energies much higher (by at least an order of magnitude) than those currently accessible by collider experiments. I present a preliminary calculation of the cross section using the HiRes/MIA hybrid data set.Thesis (Ph.D.) -- Dept. of Physics and Mathematical Physics, 2001
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Simpson, K. M. (Kenneth Mark). "Studies of cosmic ray composition using a hybrid fluorescence detector." 2001. http://web4.library.adelaide.edu.au/theses/09PH/09phs61261.pdf.
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Chang, CHIH-CHIA, and 張智嘉. "Using Cosmic Ray Muon Detector to measure the muon lifetime." Thesis, 2009. http://ndltd.ncl.edu.tw/handle/13654337684435055675.
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碩士輔仁大學
物理學系
97
We use the quarknet muon detector to measure the muon lifetime and flux. The detector is made by Fermilab, USA. In the muon lifetime study, we find the results in our lab are similar as the PDG world average, ~2.2 micro seconds. One day, we take the detector to Yu-San mountain and repeat the muon lifetime data taking. We find that the muon lifetime is too small. We wonder that some other high energy charged pion particles may affect our results. In the flux study, we find that the flux would become smaller while the angle between the scintillator plane and the horizontal increases. The behavior can be described by the cosine square function. Besides, the flux in the higher story is larger than that in the lower story. The quarknet project in Taiwan becomes better and better this year. We hope to distribute the knowledge of cosmic ray related issues to high school students and teachers. Hopefully, this thesis would help people to learn this.
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Whelan, Benjamin James. "A magnetic spectrometer analysis method for ultra high energy cosmic ray data." Thesis, 2012. http://hdl.handle.net/2440/72154.
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Since their discovery at the beginning of the 20th Century, cosmic rays have been the subject of much research. However, fundamental questions, such as the origin of the most energetic of these particles, await an answer. The unambiguous identification of cosmic ray sources is made difficult by the deflections that these charged particles suffer in their propagation through cosmic magnetic fields.This problem is compounded by the extremely low flux of the highest energy cosmic rays at Earth, the arrival directions of which may be expected to retain information about their point of origin. However, the advent of ultra high energy cosmic ray detectors possessing collecting areas of thousands of square kilometres, such as the Pierre Auger Observatory, means that the number of cosmic rays detected at the highest energies maybe sufficient to enable directional cosmic ray astronomy in the near future. The 'magnetic spectrometer analysis', described in this thesis, is designed for the analysis of ultra high energy cosmic ray data sets.The analysis is designed to identify energy ordering in the arrival directions of a cosmic ray data set, and reconstruct the source directions of such events. A brief history of the discovery of cosmic rays is presented in Chapter1, along with an introduction to the physics of extensive air showers and methods of detecting them. The current knowledge of the properties of the cosmic ray flux atultra high energies is reviewed in Chapter 2, and a summary of ultra high energy cosmic ray detectors, both past and present, is presented in Chapter3. The propagation of cosmic rays through magnetic fields, and the methods of measuring those fields, is briefly reviewed in Chapter 4. In addition, the Galactic magnetic field models that are used for the production of simulated cosmic ray data sets are described there. Numerical integration is employed in the generation of the simulated data sets,and the method of doing so, as well as considerations that must be made for such simulations, is described in Chapter 5. The magnetic spectrometer analysis method is introduced in Chapter 6 in addition to a discussion of related analyses found in the literature. The results of applying the magnetic spectrometer analysis to simulated cosmic ray data sets are presented in Chapter 7. Finally, the results of an application of the magnetic spectrometer analysis to real data collected by the Pierre Auger Observatory are described in Chapter 8, followed by a discussion of those results and concluding remarks.Thesis (Ph.D.) -- University of Adelaide, School of Chemistry and Physics, 2012
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Charara, Youssef Mohamad. "Characterization of the Cosmic Ray Telescope for the Effects of Radiation (CRaTER) detector." 2009. http://etd.utk.edu/2009/Spring2009Dissertations/ChararaYoussefMohamad.pdf.
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Bird, David John 1965. "Arrival directions of medium energy cosmic rays in the southern hemisphere / David John Bird." 1991. http://hdl.handle.net/2440/22483.
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Bibliography : leaves i-xxxi, 168, [99], xx leaves : ill ; 30 cm.
Title page, contents and abstract only. The complete thesis in print form is available from the University Library.
Thesis (Ph.D.)--University of Adelaide, Dept. of Physics and Mathematical Physics, 1991
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Saraiva, J. G. "Calibration and performance of the tile calorimeter of ATLAS with cosmic ray muons." Doctoral thesis, 2010. http://hdl.handle.net/10451/2454.
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Tese de doutoramento, Física, Universidade de Lisboa, Faculdade de Ciências, 2011The installation of the ATLAS detector in the experimental cavern, took place from 2005 until 2009. During this period, technicians, engineers and physicists have been intensivelyworking on the preparation of the detector for its main objective: probing the new frontiers of high energy physics with the LHC, the particle collider with the largest center of mass energy (14 TeV nominal) and very high luminosities(1034cm−2s−1 nominal). The context of this thesis was this challenging environment that involved all ATLAS members in the preparation of the detector for collisions during the period of the detector commissioning with cosmic ray muons and with calibration and monitoring systems. In 2008 during a short period of time single beam data was available and was used to study the detector response. This large effort was fundamental to prepare the detector for the first collisions at the LHC that started in November 2009. Before collisions started, the only high energy particles available for studieswith the LHC detectors were the muons produced by the interaction of cosmic particles in the atmosphere. These cosmic ray muons are the only detectable particles reaching the earth surface in quantities large enough to study the performance of the different sub-systems of the ATLAS detector. Thework I have developed duringmy PhDand thatwill be detailed in this document is centered on the energy calibration and synchronization of the Tile Calorimeter, the barrel hadronic calorimeter of ATLAS, using cosmic ray muons. The two main topics of study are now summarized: Contribution to the energy calibration of the Tile Calorimeter A electromagnetic energy scale was set in testbeam using high energy particles for 12% of the Tile Calorimeter modules. My contribution was centered in the validation of the global energy scale algorithm and the detector’s energy response uniformity in φ using the TileMuonFitter. The results presented in this document have shown that both the energy scale application, from testbeam to all modules in the experimental cavern, and the energy uniformity in φ are better than 5%. A difference between radial layers A and D of 3% is measured and it is something not completely understood and must be studied later using e.g. isolated muons from collisions. The used data stream and method, still have shown that a full coverage in φ can be achieved for these measurements. These results obtained with an independent method are consistent with an earlier analysis, reported in the readiness paper of the Tile Calorimeter [18]. Calorimeters are not designed and developed for the detection of muons however they play an important role on the commissioning of the LHC detectors and physics program. Before reaching the muon chambers the muons produced in collisions will lose energy in the calorimeter volume. Corrections on the energy loss in the calorimeters are necessary to improve the precision of the muon momentum measurement. This correctionmus be applied to anymuons crossing the calorimeter volume and in particular in fundamental processes used on the final calibration of the detectorwhich includes complex objects as the Z boson decaying to two muons. Lepton isolation techniques are used in the so called golden-channel for the Higgs boson discovery, the decay to four leptons H→ZZ→4l, for the rejection of QCD background. The Tile Calorimeter performance with muons can have an important impact in physics beyond the standard model, such as Super-Symmetry, for instance on the search for stable massive particles, since some of these massive particles are characterized by having an energy loss in the calorimeter similar to muons. The work developed with cosmic muons can also be applied later using muons produced in collisions to monitor the EM scale during the LHC operation. So the work developed with cosmic ray muons is not only important for the commissioning of the detector but can also be relevant for the physics of the LHC to be done with the ATLAS detector. Understanding the response of the Tile Calorimeter to muons as well as to have under control the EM energy scale are fundamental to achieve the best performance of the ATLAS detector. Synchronization of the Tile Calorimeter The Tile Calorimeter synchronization was established during 2008 combining measurements with the laser system and high energy particles: cosmic ray muons and muons from single beam. Thework presented in this thesis uses both types ofmuons, butwith different objectives inmind. Using the single beamdataweremeasured corrections to the velocity of propagation of light in the clear fibers, a parameter used in the laser synchronization. The measured value of 18.5 cm/ns resulted in the update of this parameter in the laser calibration system. The work done with cosmic muons consisted in the determination of the time offsets of the Tile Calorimeter measured both for towers and individual cells. The time offsets were calculated as the residuals after the synchronization made with the laser system. The final results have shown that the cosmic ray muons and single beam data agree within less than 2 ns. The timing is fundamental for the operation of the detector and all systems must be internally synchronized and externally synchronized with the LHC clock ( f = 1 25 ns given by the bunch crossing). The timing plays an important role in the energymeasurement due to the stringent operation conditions of the LHC that require the online signal reconstruction for the Tile Calorimeter channels to be done without iterations. The time of each channel must be known with a precision of the order of a few nanoseconds so that the correct parameters are chosen for the online reconstruction method. Time is also used to select particles that come from p-p collisions, to provide quality factors on the selection of events, and it is the most sensitive quantity for the discovery of slow long lived particles, also called stable massive particles, that are predicted in models beyond the Standard Model. This thesis is divided in 7 chapters. The first is introductory and presents the Large Hadron Collider, the ATLAS detector and its physics goals. In Chapter 2 the Tile Calorimeter is described in some detail presenting the geometry, calibration systems and performance features obtained from the last testbeam results. The following chapters are dedicated to the commissioning of the Tile Calorimeter with cosmic ray muons. The third chapter presents the motivations for the work developed, focusing on the energy scale and synchronization of the Tile Calorimeter. These quantities are of course important in the overall detector performance and have also a larger importance in specific physics channels. Chapter 4 introduces the commissioning and gives a brief overview of the activities during this stage, it is mostly descriptive but also reporting with some detail the activities in which I contributed during the development of my thesis work. The main contributions to the Tile Calorimeter commissioning is included in the next two chapters. Chapter 5 presents the results on the energy scale and uniformity in φ using the TileMuonFitter. Chapter 6 is dedicated to the methods and results for synchronization with cosmic ray muons data. Finally in Chapter 7 conclusions are given.
Fundação para a Ciência e Tecnologia (SFRH/BD/27416/2006)
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Medina, Hernandez Carlos Francisco. "Analysis of calorimeter/ITC cosmic ray datafrom the ATLAS detector, and preparation for supersymmetry searches." 2009. http://hdl.handle.net/10106/1688.
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Pu-KaiWang and 王莆凱. "The R＆D of Compact Scintillator Array Detector for Cosmic Ray measurement in sounding rocket or CubeSat missions." Thesis, 2018. http://ndltd.ncl.edu.tw/handle/h9k4b4.
Full textAbstract:
碩士國立成功大學
物理學系
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The developement of CubeSat and sounding rocket is a total game changer to the space program, and it makes building a space instrument to be more achievable and affordable. Therefore, it give us a great opportunity to build a small cosmic ray detector which has ca- pabilities to measure flux, direction, energy and charge of cosmic rays at the height that scientific balloon can't reach. It might open a new door for the cosmic ray physics. In this thesis, I will show the idea and the detailed design of Compact Scintillator Array Detector (ComSAD). A series of functional and environmental tests will be conducted to demonstrate that this is suitable for a cosmic ray reach in Space.
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Lau, Koon Hang. "A Cerenkov-ΔΕ-Cerenkov Detector for High Energy Cosmic Ray Isotopes and an Accelerator Study of ⁴⁰Ar & ⁵⁶Fe Fragmentation." Thesis, 1985. https://thesis.library.caltech.edu/8692/1/Lau_KH_1985.pdf.
Full textAbstract:
This thesis has two major parts. The first part of the thesis will describe a high energy cosmic ray detector -- the High Energy Isotope Spectrometer Telescope (HEIST). HEIST is a large area (0.25 m2sr) balloon-borne isotope spectrometer designed to make high-resolution measurements of isotopes in the element range from neon to nickel (10 ≤ Z ≤ 28) at energies of about 2 GeV/nucleon. The instrument consists of a stack of 12 NaI(Tl) scintilla tors, two Cerenkov counters, and two plastic scintillators. Each of the 2-cm thick NaI disks is viewed by six 1.5-inch photomultipliers whose combined outputs measure the energy deposition in that layer. In addition, the six outputs from each disk are compared to determine the position at which incident nuclei traverse each layer to an accuracy of ~2 mm. The Cerenkov counters, which measure particle velocity, are each viewed by twelve 5-inch photomultipliers using light integration boxes.
HEIST-2 determines the mass of individual nuclei by measuring both the change in the Lorentz factor (Δγ) that results from traversing the NaI stack, and the energy loss (ΔΕ) in the stack. Since the total energy of an isotope is given by Ε = γM, the mass M can be determined by M = ΔΕ/Δγ. The instrument is designed to achieve a typical mass resolution of 0.2 amu.
The second part of this thesis presents an experimental measurement of the isotopic composition of the fragments from the breakup of high energy 40Ar and 56Fe nuclei. Cosmic ray composition studies rely heavily on semi-empirical estimates of the cross-sections for the nuclear fragmentation reactions which alter the composition during propagation through the interstellar medium. Experimentally measured yields of isotopes from the fragmentation of 40Ar and 56Fe are compared with calculated yields based on semi-empirical cross-section formulae. There are two sets of measurements. The first set of measurements, made at the Lawrence Berkeley Laboratory Bevalac using a beam of 287 MeV/nucleon 40Ar incident on a CH2 target, achieves excellent mass resolution (σm ≤ 0.2 amu) for isotopes of Mg through K using a Si(Li) detector telescope. The second set of measurements, also made at the Lawrence Berkeley Laboratory Bevalac, using a beam of 583 MeV/nucleon 56Fe incident on a CH2 target, resolved Cr, Mn, and Fe fragments with a typical mass resolution of ~ 0.25 amu, through the use of the Heavy Isotope Spectrometer Telescope (HIST) which was later carried into space on ISEE-3 in 1978. The general agreement between calculation and experiment is good, but some significant differences are reported here.