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U·M·I University Microfilms International a Bell & Howell Lntormanon Company 300 North Zeeb Road INFORMATION TO USERS This manuscript has been reproduced from the microfilm master. UMI films the text directly from the original or copysubmitted. Thus, some thesis and dissertation copies are in typewriter face, while others may be from any type of computer printer. The quality of this reproduction is dependent upon the quality of the copy submitted. Broken or indistinct print, colored or poor quality illustrations and photographs, print bleedthrough, substandard margins, and improper alignment can adverselyaffect reproduction. In the unlikely.event that the author did not send UMI a complete manuscript and there are missing pages, these will be noted. Also, if unauthorized copyrightmaterial had to be removed, a note will indicate the deletion. Oversize materials (e.g., maps, drawings, charts) are reproduced by sectioning the original, beginning at the upper left-hand corner and continuing from left to right in equal sections with small overlaps. Each original is also photographed in one exposure and is included in reduced form at the back of the book. Photographs included in the original manuscript have been reproduced xerographically in this copy. Higher quality 6" x 9" black and white photographic prints are available for any photographs or illustrations appearing in this copy for an additional charge. Contact UMI directly to order. U·M·I University Microfilms International A Bell & Howell lntormanon Company 300 North Zeeb Road. Ann Arbor. M148106-1346 USA 313/761-4700 800/521-0600 Order Number 9416065 A treatise on high energy muons in the 1MB detector McGrath, Gary G., Ph.D. University of Hawaii, 1993 V·M·I 300N. Zeeb Rd. Ann Arbor, MI48106 A TREATISE ON HIGH ENERGY MUONS IN THE 1MB DETECTOR A DISSERTATION SUBMITTED TO THE GRADUATE DIVISION OF THE UNIVERSITY OF HAWAII IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY IN PHYSICS DECEMBER 1993 By Gary G. McGrath Dissertation Committee: John G. Learned, Chairperson Sandip Pakvasa Michael W. Peters Victor J. Stenger R. Brent Tully III ACKNOWLEDGEMENTS Foremost, I would like thank my wife, Jami, for the unending support, encouragement, and love she has given me over the last four years. She has always been the person who best understands what my work means to me, and the hopes and aspirations we share are one of my greatest motivations. For that, I would like to dedicate this thesis to her. I also wish to express how much the support and encouragement of my parents, Gerald and Grace, has meant to this work. Their support has been invaluable, as they are always there when I need them. It allowed me to make it to the graduate level and motivated me to continue on, and so I am grateful. Three people have been most responsible for my academic pursuit: John Learned, Bob Svoboda, and Ralph Becker-Szendy. I would like to thank all three of them for the endless hours they have given me. Bob first introduced me to 1MB as an undergraduate and suggested that I consider U.H. for my graduate work. Beyond that, he did much of the work that this neutrino oscillation analysis is founded on. He has always offered advice and help that I could count on, and I can not imagine where I would be today if it where not for him. Once I arrived here, Ralph took me in under his wing, showed me the ropes, and endured hours of stupid questions. He set an example of the kind of student I hoped to be, and remains a great friend to this day, always willing to go beyond reasonable limits to help - he sometimes just likes to go beyond reasonable limits. Finally, John has offered me his guidance and experience to not only teach me the technical aspects of physics, but to show me the subtleties I would otherwise miss. He is extremely generous and an example of the kind of physicist I aspire to be. For all of their help and guidance through the years, I am indebted. iv Several other people have expended much effort to answer my questions and lend me ideas. Sandip Pakvasa and Andy Acker have helped me immensely in my neutrino oscillation work, as they were always willing to answer my questions. Whenever I had hardware questions or ideas, Jeff Bolesta or Shige Matsuno usually had the answers and offered to help. Greg Grajew and Vic Stenger performed the tedious work of laboring through the uncorrected versions of this thesis. There are numerous people who make up the backbone of the University that allows the physicists to perform their work, and I would like to thank two in particular: Caroline Chong and Diane Ibaraki, Caroline has always gone out of her way to see that things go smoothly, regardless of whether it is possible or not. Not only has Diane helped me with the many technical computer problems I encountered, but she went out of her way to see that I have the computer resources I need. Much of this analysis would not be technically possible if she had not found a way. The 1MB collaboration represents physicists from all over, and it would be difficult to thank them all individually. It should be noted that none of this work could have begun without the careful work that has gone into the detector over the last decade. The comments, suggestions, and guidance I received from my collaborators is invaluable, and I am sincerely grateful. I would just like to mention Steve Dye, Wojciech Gajewski, Todd Haines, Peter Halverson, and Clark McGrew in particular for the many times they went out of their way to offer me suggestions and ideas. This work was funded by the United States Department of Energy, High Energy Physics Division. v ABSTRACT The Irvine-Michigan-Brookhaven proton decay detector records upward­ going muon data at a rate of rv 0.5 ILlday and downward-going muon data at a rate of 2.7 ILls. After separating the upward-going data from the downward­ going data, both data sets are examined for consistency with expectation and searched for physical effects. The upward-going muon data is used to search for vp. +-+ Ve and vp. +-+ V T neutrino oscillation effects that are consistent with the parameters suggested by the atmospheric neutrino flavor anomaly that is found in the contained data. Three different techniques provide the search, but uncover no evidence. Hence, the upward-going data limits the preferred parameter space for both types of 22() oscillations. For vp.+-+ V e oscillations, the 90% C.L. limits are sin 2:: 0.38 for large 8m2 and 8m2 2:: 1.8 x 10-2 at large mixing angles, while the limits for 22() 2 2 3 vp. +-+ VT oscillations are sin 2:: 0.42 for large 8m and 8m :::: 1.7 x 10- at large mixing angles. Although the upward-going data remains consistent with the neutrino oscillation hypothesis, it greatly limits the possible parameters. In addition to the neutrino oscillation analysis, the downward-going muon data is used to search for point sources and to study the origins of underground muons. Although the testing of 13 sources chosen a priori uncovered no candi­ dates, two features stand out in these data: at least two possible point sources and a large scale anisotropy. A survey of the entire sky finds two excesses at 0 IMBm1=(a rv 164 , 8 rv 53°) and IMBm2=(a rv 106°, 8 rv 68°), with ran­ dom chance probabilities (including trials penalties) of p = 2.0 X 10-5 and 4 p = 7.9 X 10- respectively, although neither direction is associated with any popular v or -y-ray sources. In addition, there is an anisotropy in the data favor­ ing the a = 270° and 8 = 30° direction, with an approximate magnitude of 10-2 • This magnitude is surprisingly large, but it does not seem to be attributable to systematics in the data. Vl TABLE OF CONTENTS ACKNOWLEDGEMENTS iii ABSTRACT ... .V LIST OF TABLES ix LIST OF FIGURES .x 1. INTRODUCTION 1 A. Neutrino History ... 1 B. Observation Techniques 5 C. Nuclear Reactor Experiments. 6 D. Accelerator Experiments. .. 9 E. Solar Neutrino Experiments 11 F. Atmospheric Neutrino Experiments 13 G. Downward-Going Muon History 15 H. Muon Astronomy . 17 2. THE 1MB DETECTOR 19 A. Introduction .. 19 B. General Overview 19 C. Overburden 21 D. Photo Detection 22 E. Trigger .... 23 F. Read Out 24 G. Absolute Event Time 26 3. MONTE CARLO PREDICTIONS 27 A. Introduction ....... 27 B. Atmospheric Neutrino Flux 29 C. Neutrino Oscillations ... 34 1. Vacuum Oscillations 35 2. Matter Effects . 36 Vll 3. Event Weighting 38 D. Neutrino Interaction Cross Sections 40 E. Lepton Propagation 44 F. Detector Response 46 4. NEUTRINO OSCILLATION ANALYSIS 47 A. Introduction 47 B. Event Classification 48 1. Contained . 48 2. Downward-Going . 49 3. Upward-Going 50 4. Stopping 51 5. Showering 55 C. Upward-Going Muon Comparison Techniques 57 1. Absolute Rate 57 2. SiT Ratio . 58 3. Zenith Angle Distribution 60 D. Preferred Region for Contained Events 63 5. DOWNWARD-GOING MUON ANALYSIS 64 A. Introduction 64 B. Direction Fitting 65 C. Resolution 66 D. Cone Searching 71 E. Background Calculations . 73 F. Flashers 78 G. Data Cuts 80 H. Absolute Event Time 81 1. Live-Time 83 J. Effective Area 85 K. Equatorial Coordinates 86 L. Radio Burst Correlated Signal 88 M. Galactic and 811Ilergalactic Coordinates 90 viii N. Moon Coordinates . 91 6. NEUTRINO OSCILLATION RESULTS 94 A. Introduction .......... 94 B. Contained Event Preferred Region 94 C. Upward-Going Muon Exclusions 97 1. Absolute Rate 97 2. SiT Ratio .. 101 3.
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