DOCSLIB.ORG

A Study of Systematic Uncertainties for a Photon-Like Low Energy Excess Search at Microboone

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

University of Tennessee, Knoxville TRACE: Tennessee Research and Creative Exchange Doctoral Dissertations Graduate School 8-2021 A Study of Systematic Uncertainties for a Photon-like Low Energy Excess Search at MicroBooNE Gray Yarbrough [email protected] Follow this and additional works at: https://trace.tennessee.edu/utk_graddiss Part of the Elementary Particles and Fields and String Theory Commons, and the Plasma and Beam Physics Commons Recommended Citation Yarbrough, Gray, "A Study of Systematic Uncertainties for a Photon-like Low Energy Excess Search at MicroBooNE. " PhD diss., University of Tennessee, 2021. https://trace.tennessee.edu/utk_graddiss/6575 This Dissertation is brought to you for free and open access by the Graduate School at TRACE: Tennessee Research and Creative Exchange. It has been accepted for inclusion in Doctoral Dissertations by an authorized administrator of TRACE: Tennessee Research and Creative Exchange. For more information, please contact [email protected]. To the Graduate Council: I am submitting herewith a dissertation written by Gray Yarbrough entitled "A Study of Systematic Uncertainties for a Photon-like Low Energy Excess Search at MicroBooNE." I have examined the final electronic copy of this dissertation for form and content and recommend that it be accepted in partial fulfillment of the equirr ements for the degree of Doctor of Philosophy, with a major in Physics. Sowjanya Gollapinni, Major Professor We have read this dissertation and recommend its acceptance: Stefan M Spanier, Nadia Fomin, David C Donovan Accepted for the Council: Dixie L. Thompson Vice Provost and Dean of the Graduate School (Original signatures are on file with official studentecor r ds.) A Study of Systematic Uncertainties for a Photon-like Low Energy Excess Search at MicroBooNE A Dissertation Presented for the Doctor of Philosophy Degree The University of Tennessee, Knoxville Gray Yarbrough August 2021 © by Gray Yarbrough, 2021 All Rights Reserved. ii Dedicated to all of those who helped me along the way iii Acknowledgments Thanks to the many people who supported me from University of Tennessee Knoxville. My advisor, Dr. Sowjanya Gollapinni, deserves particular praise for the guidance in introducing me to the MicroBooNE collaboration and her immeasurable support in my dissertation work. Also, particular thanks to my doctoral committee for their support in the dissertation process. Finally, my appreciation is immeasurable to all the professors and staff who supported me at UTK. I would also like to thank the Fermilab and MicroBooNE communities for welcoming me and supporting through my stay at the lab, both in my work and in my life. Finally, thanks to my family for their unwavering support in my career. To my mother and father, the fact that I knew I could always call on you in times of stress was a great comfort. To my grandfather, you could always be relied upon to hear my problems and make me laugh. Thank you all, truly. iv Abstract The premise of this dissertation is the study of and reduction of systematic uncertainties in the MicroBooNE experiment at the Fermi National Accelerator Laboratory. MicroBooNE is a short-baseline oscillation experiment using the innovative liquid argon time projection chamber technology to study, with unprecedented detail, neutrino interactions. The primary goal of MicroBooNE is the investigation of the MiniBooNE low energy excess (LEE) of electron neutrino events, a result which raised fundamental questions on the existence of sterile neutrinos with broad implications to the field of particle physics. The principal study of this dissertation is a study of systematics as part of the LEE search seeking an explanation to the MiniBooNE low energy excess anomaly via neutrino-induced single photon events. A detailed knowledge of uncertainties is necessary to achieve the required precision, and the work presented in this thesis allowed for an estimated three times reduction of systematic uncertainties in the single photon analysis. In addition, a study of beamline properties and systematics on the source beam for MicroBooNE, the Booster Neutrino Beam, with a method of recovering data deemed unfit due to beamline related issues has been performed. Significance of beam-related measurements depends on the protons on target collected and, as such, this result could potentially increase the neutrino data received by MicroBooNE. Overall, these studies have significantly contributed to the precision and confidence of the single photon analysis along with potential for improvements to future analyses in MicroBooNE. v Table of Contents 1 Overview of Thesis1 2 Neutrino Physics4 2.1 Standard Model..................................4 2.2 Neutrino history..................................8 2.3 Neutrino Oscillations...............................9 2.4 Neutrino Interactions............................... 12 2.4.1 Charge Current Quasi-Elastic Interactions............... 15 2.4.2 Deep Inelastic Interactions........................ 15 2.4.3 Resonant Interactions........................... 16 2.4.4 Coherent Interactions........................... 17 2.4.5 Neutrino-Argon Interactions Developement............... 17 2.5 Open Questions in Neutrino Physics...................... 17 2.5.1 Neutrino Mass Hierarchy......................... 18 2.5.2 Absolute Masses of Neutrinos...................... 18 2.5.3 Additional Neutrino States........................ 19 2.5.4 Majorana or Dirac Nature........................ 19 2.5.5 Charge Parity Violation......................... 20 2.6 Neutrino Experiments.............................. 22 2.6.1 Neutrino Accelerator Experiments.................... 23 2.6.2 Long Baseline Experiments....................... 26 2.6.3 Short Baseline Experiments....................... 27 vi 3 The MicroBooNE Experiment 31 3.1 Experimental Motivation............................. 31 3.2 MicroBooNE and Physics Goals......................... 33 3.3 Booster Neutrino Beam.............................. 37 3.3.1 Beam Target and Horn.......................... 38 3.3.2 Booster Neutrino Beam MicroBooNE Era............... 38 3.4 MicroBooNE Construction............................ 39 3.4.1 TPC.................................... 39 3.4.2 Light Collection.............................. 43 3.4.3 Cryogenic System............................. 43 3.4.4 Cosmic Ray Tagger............................ 44 3.4.5 Data Acquisition............................. 44 3.5 MicroBooNE Data Collection.......................... 46 4 MicroBooNE Reconstruction and Simulation 58 4.1 MicroBooNE Simulation............................. 58 4.1.1 Neutrino Flux Simulation........................ 59 4.1.2 Cosmic Generation............................ 59 4.1.3 Neutrino Interactions........................... 60 4.2 MicroBooNE Signal Processing......................... 61 4.2.1 Time Projection Chamber Signals.................... 61 4.2.2 Signal Extraction............................. 63 4.3 Reconstruction.................................. 64 4.3.1 Pandora.................................. 64 4.3.2 Optical Reconstruction.......................... 65 4.3.3 Calorimetry................................ 66 4.3.4 Particle Identification........................... 67 4.3.5 Calibration................................ 68 5 Single Photon Low Energy Excess Search 82 5.1 Goals and Hypothesis............................... 82 vii 5.2 Analysis Overview................................ 83 5.3 Single Photon Selection.............................. 83 5.4 Neutral Current π0 Selection........................... 92 6 Single Photon Systematics 99 6.1 Systematics Frameworks............................. 99 6.1.1 Covariance Matrix Construction..................... 100 6.2 Reweightable Systematic Uncertainties..................... 101 6.2.1 EventWeight Module........................... 101 6.2.2 Input Samples............................... 102 6.2.3 Flux Systematics............................. 103 6.2.4 Cross Section Systematics........................ 105 6.2.5 Total Flux and Cross Section Tables.................. 111 6.2.6 Flux and Cross Section Covariance Matrices.............. 113 6.3 Non-Reweightable Systematics.......................... 113 6.3.1 Detector Systematics Selections..................... 122 6.3.2 Detector Systematics in the Final Selections.............. 122 6.3.3 Photonocuclear Absorption Uncertainties................ 124 6.4 Systematics Constraint and Final Results.................... 128 6.4.1 Estimating the Neutral Current π0 Systematic Constraint....... 128 6.4.2 Hypothesis Testing............................ 137 6.4.3 Fitting to a Neutral Current ∆ Radiative Decay Rate Parameter... 138 7 Booster Neutrino Beam Accelerator Concepts 142 7.1 Accelerator Concept............................... 142 7.2 Fermilab Accelerator Complex.......................... 143 7.2.1 Linear Accelerator............................ 143 7.2.2 Booster.................................. 146 7.2.3 Target and Horn Details......................... 146 7.2.4 Beamline Instrumentation and Devices................. 147 viii 8 Booster Neutrino Beam Systematic Analsysis 149 8.1 Beam Position Study............................... 149 8.1.1 Target Scan Procedure.......................... 150 8.1.2 Figure of Merit Multi-Wire Study.................... 152 8.2 Hadron Production Experiment Data Fitting and BNB Flux Prediction... 163 8.2.1 HARP Data................................ 167 8.2.2 Proton Contribution to Neutrino Flux................. 167 8.2.3 Sanford-Wang Parametrization....................
Recommended publications
  • The Muon Range Detector at Sciboone Joseph Walding

    The Muon Range Detector at Sciboone Joseph Walding

    The Muon Range Detector at SciBooNE Joseph Walding High Energy Physics Department, Blackett Laboratory, Imperial College, London Abstract. SciBooNE is a new neutrino experiment at Fermilab. The detector will undertake a number of measurements, principally sub-GeV neutrino cross-section measurements applicable to T2K. The detector consists of 3 sub-detectors; SciBar and the Electron-Catcher were both used in the K2K experiment at KEK, Japan, whilst the Muon Range Detector is a new detector constructed at Fermilab using recycled materials from previous Fermilab experiments. A description of the detector, its construction and software is presented here. Keywords: neutrino, neutrino detector, SciBooNE PACS: 01.30.Cc, 13.15.+g, 95.55.Vj SCIBOONE SciBooNE’s principal measurements are sub-GeV neutrino cross-section measurements applicable to T2K [1]. SciBooNE sits in the Booster neutrino beam 100 m downstream from the beam target. As well as carrying out sub-GeV cross-section measurements SciBooNE will also be used as a near detector for the MiniBooNE experiment [2]. The Muon Range Detector (MRD) is one of 3 sub-detectors that make up the SciBooNE detector [3]. It sits downstream of both SciBar and the Electron-Catcher (EC) both originally used in the K2K experiment [4] at KEK, Japan. The Muon Range Detector is made up largely from recycled materials from previous Fermilab experiments including all the PMTs, scintillator, iron absorber and data acquisition (DAQ) electronics. THE MUON RANGE DETECTOR The role of the Muon Range Detector is to confine the muons produced in charge-current quasi-elastic (CCQE) interactions, which is the dominant process in SciBooNE.
  • The History of Neutrinos, 1930 − 1985

    The History of Neutrinos, 1930 − 1985

    The History of Neutrinos, 1930 − 1985. What have we Learned About Neutrinos? What have we Learned Using Neutrinos? J. Steinberger Prepared for “25th International Conference On Neutrino Physics and Astrophysics”, Kyoto (Japan), June 2012 1 2 3 4 The detector of the experiment of Conversi, Pancini and Piccioni, 1946, 5 which showed that the mesotron is not the Yukawa particle. Detector with 80 Geiger counters. The muon decay spectrum is continuous. My thesis experiment, under Fermi, which showed that the muon decays into two neutral particles, plus the electron. Fermi, myself and others, in 1954, at a summer school in Varenna, lake Como, a few months before Fermi’s untimely disappearance. 6 Demonstration of the Neutrino In 1956 Cowan and Reines detected antineutrinos from a nuclear reactor, reacting with protons in liquid scintillator which also contained cadmium, observing the positron as well as the scattering of the neutron on cadmium. 7 The Electron and Muon Neutrinos are Different. 1. G. Feinberg, 1958. 2. B. Pontecorvo, 1959. 3. M. Schwartz (T.D. Lee), 1959 4. Higher energy accelerators, Courant, Livingston and Snyder. Pontecorvo 8 9 A C B D Spark chamber and counter arrangement. A are triggering counters, Energy spectra of neutrinos B, C and D are anticoincidence counters from pion and kaon decays. 10 Event with penetrating muon and hadron shower 11 The group of the 2nd neutrino experiment in 1962: J.S., Goulianos, Gaillard, Mistry, Danby, technician whose name I have forgotten, Lederman and Schwartz. 12 Same group, 26 years later, at Nobel ceremony in Stockholm. 13 Discovery of partons, nucleon structure, scaling, in deep inelastic scattering of electrons on protons at SLAC in 1969.
  • Searches for Dark Matter with Icecube and Deepcore

    Searches for Dark Matter with Icecube and Deepcore

    Matthias Danninger Searches for Dark Matter with IceCube and DeepCore New constraints on theories predicting dark-matter particles Department of Physics Stockholm University 2013 Doctoral Dissertation 2013 Oskar Klein Center for Cosmoparticle Physics Fysikum Stockholm University Roslagstullsbacken 21 106 91 Stockholm Sweden ISBN 978-91-7447-716-0 (pp. i-xii, 1-112) (pp. i-xii, 1-112) c Matthias Danninger, Stockholm 2013 Printed in Sweden by Universitetsservice US-AB, Stockholm 2013 Distributor: Department of Physics, Stockholm University Abstract The cubic-kilometer sized IceCube neutrino observatory, constructed in the glacial ice at the South Pole, searches indirectly for dark matter via neutrinos from dark matter self-annihilations. It has a high discovery potential through striking signatures. This thesis presents searches for dark matter annihilations in the center of the Sun using experimental data collected with IceCube. The main physics analysis described here was performed for dark matter in the form of weakly interacting massive particles (WIMPs) with the 79-string configuration of the IceCube neutrino telescope. For the first time, the Deep- Core sub-array was included in the analysis, lowering the energy threshold and extending the search to the austral summer. Data from 317 days live- time are consistent with the expected background from atmospheric muons and neutrinos. Upper limits were set on the dark matter annihilation rate, with conversions to limits on the WIMP-proton scattering cross section, which ini- tiates the WIMP capture process in the Sun. These are the most stringent spin- dependent WIMP-proton cross-sections limits to date above 35 GeV for most WIMP models.
  • Improved Measurement of Neutral Current Coherent

    Improved Measurement of Neutral Current Coherent

    Improved measurement of neutral current coherent The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Kurimoto, Y., et al. “Improved Measurement of Neutral Current Coherent π 0 Production on Carbon in a Few-GeV Neutrino Beam.” Physical Review D, vol. 81, no. 11, June 2010. © 2010 The American Physical Society As Published http://dx.doi.org/10.1103/PhysRevD.81.111102 Publisher American Physical Society (APS) Version Final published version Citable link http://hdl.handle.net/1721.1/116670 Terms of Use Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. RAPID COMMUNICATIONS PHYSICAL REVIEW D 81, 111102(R) (2010) Improved measurement of neutral current coherent 0 production on carbon in a few-GeV neutrino beam Y. Kurimoto,5 J. L. Alcaraz-Aunion,1 S. J. Brice,4 L. Bugel,13 J. Catala-Perez,18 G. Cheng,3 J. M. Conrad,13 Z. Djurcic,3 U. Dore,15 D. A. Finley,4 A. J. Franke,3 C. Giganti,15,* J. J. Gomez-Cadenas,18 P. Guzowski,6 A. Hanson,7 Y. Hayato,8 K. Hiraide,10,† G. Jover-Manas,1 G. Karagiorgi,13 T. Katori,7 Y.K. Kobayashi,17 T. Kobilarcik,4 H. Kubo,10 W. C. Louis,11 P.F. Loverre,15 L. Ludovici,15 K. B. M. Mahn,3,‡ C. Mariani,3 S. Masuike,17 K. Matsuoka,10 V.T. McGary,13 W. Metcalf,12 G.
  • Neutrino Physics

    Neutrino Physics

    Neutrino Physics Steve Boyd University of Warwick Course Map 1. History and properties of the neutrino, neutrino interactions, beams and detectors 2. Neutrino mass, direct mass measurements, double beta decay, flavour oscillations 3. Unravelling neutrino oscillations experimentally 4. Where we are and where we're going References K. Zuber, “Neutrino Physics”, IoP Publishing 2004 C. Giunti and C.W.Kim, “Fundamentals of Neutrino Physics and Astrophysics”, Oxford University Press, 2007. R. N. Mohaptara and P. B. Pal, “Massive Neutrinos in Physics and Astrophysics”, World Scientific (2nd Edition), 1998 H.V. Klapdor-Kleingrothaus & K. Zuber, “Particle Astrophysics”,IoP Publishing, 1997. Two Scientific American articles: “Detecting Massive Neutrinos”, E. Kearns, T. Kajita, Y. Totsuka, Scientific American, August 1999. “Solving the Solar Neutrino Problem”, A.B. McDonald, J.R. Klein, D.L. Wark, Scientific American, April 2003. Plus other Handouts Lecture 1 In which history is unravelled, desperation is answered, and the art of neutrino generation and detection explained Crisis It is 1914 – the new study of atomic physics is in trouble (Z+1,A) Spin 1/2 (Z,A) Spin 1/2 Spin 1/2 electron Spin ½ ≠ spin ½ + spin ½ E ≠ E +e Ra Bi “At the present stage of atomic “Desperate remedy.....” theory we have no arguments “I do not dare publish this idea....” for upholding the concept of “I admit my way out may look energy balance in the case of improbable....” b-ray disintegrations.” “Weigh it and pass sentence....” “You tell them. I'm off to a party” Detection of the Neutrino 1950 – Reines and Cowan set out to detect n 1951 1951 1951 I.
  • Dstau: Study of Tau Neutrino Production with 400 Gev Protons from the CERN-SPS

    Dstau: Study of Tau Neutrino Production with 400 Gev Protons from the CERN-SPS

    Prepared for submission to JHEP DsTau: Study of tau neutrino production with 400 GeV protons from the CERN-SPS Shigeki Aoki,a Akitaka Ariga,b;1 Tomoko Ariga,b;c Sergey Dmitrievsky,d Elena Firu,e Dean Forshaw,b Tsutomu Fukuda,f Yuri Gornushkin,d Ali Murat Guler,g Maria Haiduc,e Koichi Kodama,h Masahiro Komatsu,f Muhtesem Akif Korkmaz,g Umut Kose,i Madalina Miloi,e Antonio Miucci,b Motoaki Miyanishi,f Mitsuhiro Nakamura,f Toshiyuki Nakano,f Alina Neagu,e Hiroki Rokujo,f Osamu Sato,f Elizaveta Sitnikova,d Yosuke Suzuki,f Tomoki Takao,f Svetlana Vasina,d Mykhailo Vladymyrov,b Thomas Weston,b Junya Yoshida,j Masahiro Yoshimoto.k The DsTau Collaboration aKobe University, Kobe, Japan bAlbert Einstein Center for Fundamental Physics, Laboratory for High Energy Physics, University of Bern, Bern, Switzerland cKyushu University, Fukuoka, Japan dJoint Institute for Nuclear Research, Dubna, Russia eInstitute of Space Science, Bucharest, Romania f Nagoya University, Nagoya, Japan gMiddle East Technical University, Ankara, Turkey hAichi University of Education, Kariya, Japan iCERN, Geneva, Switzerland jAdvanced Science Research Center, Japan Atomic Energy Agency, Tokai, Japan kGifu University, Gifu, Japan E-mail: [email protected] Abstract: In the DsTau experiment at the CERN SPS, an independent and direct way to measure tau neutrino production following high energy proton interactions was proposed. As the main source of tau neutrinos is a decay of Ds mesons, produced in proton-nucleus arXiv:1906.03487v1 [hep-ex] 8 Jun 2019 interactions, the project aims at measuring a differential cross section of this reaction. The experimental method is based on a use of high resolution emulsion detectors for effective registration of events with short lived particle decays.
  • HARP Targets Pion Production Cross Section and Yield Measurements: Implications for Miniboone Neutrino Flux

    HARP Targets Pion Production Cross Section and Yield Measurements: Implications for Miniboone Neutrino Flux

    HARP targets pion production cross section and yield measurements: Implications for MiniBooNE neutrino flux A Dissertation Submitted to the Graduate School of the University of Cincinnati in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Department of Physic of the College of Arts and Sciences July 2015 by Don Athula Abeyarathna Wickremasinghe M.Sc., University of Cincinnati, 2011 M.Sc., Norwegian University of Science and Technology (NTNU), 2008 B.Sc., University of Peradeniya, 2002 Committee Chair: Professor Randy A. Johnson © 2015 Don Athula A. Wickremasinghe All Rights Reserved HARP targets pion production cross section and yield measurements: Implications for MiniBooNE neutrino flux Don Athula Abeyarathna Wickremasinghe Abstract The prediction of the muon neutrino flux from a 71.0 cm long beryllium target for the MiniBooNE experiment is based on a measured pion production cross section which was taken from a short beryllium target (2.0 cm thick - 5% nuclear interaction length) in the Hadron Production (HARP) experiment at CERN. To verify the extrapolation to our longer target, HARP also measured the pion production from 20.0 cm and 40.0 cm beryllium targets. The measured production yields, d2N π± (p; θ)=dpdΩ, on targets of 50% and 100% nuclear interaction lengths in the kinematic rage of momentum from 0.75 GeV/c to 6.5 GeV/c and the range of angle from 30 mrad to 210 mrad are presented along with an update of the short target cross sections. The best fitted extended Sanford-Wang (SW) model parameterization for updated short beryllium target π+ production cross section is presented.
  • RECENT RESULTS from ICECUBE on NEUTRINO OSCILLATIONS 1 Introduction Neutrino Oscillations Were Discovered by Super-Kamiokande In

    RECENT RESULTS from ICECUBE on NEUTRINO OSCILLATIONS 1 Introduction Neutrino Oscillations Were Discovered by Super-Kamiokande In

    RECENT RESULTS FROM ICECUBE ON NEUTRINO OSCILLATIONS J. P. A. M. de Andre,´ for the IceCube Collaborationa Department of Physics and Astronomy, Michigan State University, East Lansing, MI, USA The IceCube Neutrino Observatory, located at the South Pole, is the world's largest neutrino 2 2 detector. IceCube is well placed to probe the existence of sterile neutrinos with ∆m41 ≈ 1 eV , which is a region of particular interest for the various anomalies motivating the existence of sterile neutrinos, by looking for muon neutrino disappearance around 1 TeV. In addition to that, using data from a more densely instrumented region of the detector, DeepCore, IceCube can be used to precisely measure regular neutrino oscillations and, by looking at distortions on those oscillations, further probe the existence of sterile neutrinos. We will discuss recent results from IceCube on neutrino oscillations, both related to searches for sterile neutrino and to precision measurement of the atmospheric mixing angles. 1 Introduction Neutrino oscillations were discovered by Super-Kamiokande in 1998 1 through the measurement of atmospheric neutrinos, and SNO in 2002 2 through the measurement of solar neutrinos. The parameters describing the standard three flavor neutrino oscillation have been measured with varying precision by many different experiments (see Ref. 3 and references therein) with the 2 exception of the CP-violating phase (δCP ) and the mass ordering (the sign of ∆m32). The am- plitude of the neutrino oscillation is determined by the elements of the mixing matrix, described by the mixing angles (θ12, θ13, and θ23) and δCP , while its oscillation period in vacuum depends 2 2 on j∆m32jL=E and j∆m21jL=E, where E is the neutrino energy, L is the distance between its 2 production and interaction points, and ∆mji is the difference between the square of the masses of νj and νi.
  • Pos(Nufact2017)067 Mass Range

    Pos(Nufact2017)067 Mass Range

    Neutrino cross-section measurement prospects with SBND PoS(NuFact2017)067 Nicola McConkey∗ for the SBND Collaboration University of Sheffield E-mail: [email protected] SBND (Short-Baseline Near Detector) is a 112ton liquid argon time projection chamber (LArTPC) neutrino detector under construction in the Fermilab Booster Neutrino Beam. Together with MicroBooNE and ICARUS-T600 detectors, SBND will search for short baseline neutrino oscillations in the 1eV2 mass range. SBND will also perform detailed studies of the physics of neutrino-argon interactions, thanks to a data sample of millions of electron and muon neutrino interactions. Finally SBND plays an important role in the on-going R&D effort to develop the LArTPC technology, testing several technologies that can be used in a future kiloton-scale neu- trino detectors for a long-baseline experiment. We will discuss the detector design, its current status, and the physics program, with a particular focus on the neutrino cross-section measure- ment prospects. The 19th International Workshop on Neutrinos from Accelerators-NUFACT2017 25-30 September, 2017 Uppsala University, Uppsala, Sweden ∗Speaker. c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). https://pos.sissa.it/ Neutrino cross-section measurement prospects with SBND Nicola McConkey Table 1: Parameters of the three SBN detectors. Detector Baseline (m) Active LAr mass (tonnes) SBND 110 112 MicroBooNE 470 87 ICARUS T-600 600 476 1. Introduction Over the past 20 years there have been several experimental anomalies observed in neutrino PoS(NuFact2017)067 experiments with baselines of the order of <1km, which are referred to as short baseline exper- iments.
  • ANNUAL REPORT (APRIL 2016 – MARCH 2017) Editorial Board MIYOKI, Shinji YOSHIKOSHI, Takanori TAKENAGA, Yumiko FUKUDA, Hironobu

    ANNUAL REPORT (APRIL 2016 – MARCH 2017) Editorial Board MIYOKI, Shinji YOSHIKOSHI, Takanori TAKENAGA, Yumiko FUKUDA, Hironobu

    INSTITUTE FOR COSMIC RAY RESEARCH THE UNIVERSITY OF TOKYO ANNUAL REPORT (APRIL 2016 – MARCH 2017) Editorial Board MIYOKI, Shinji YOSHIKOSHI, Takanori TAKENAGA, Yumiko FUKUDA, Hironobu c Institute for Cosmic Ray Research, The University of Tokyo 5-1-5, Kashiwanoha, Kashiwa, Chiba 277-8582, Japan Telephone: (81) 4-7136-3102 Facsimile: (81) 4-7136-3115 WWW URL: http://www.icrr.u-tokyo.ac.jp/ TABLE OF CONTENTS Preface Research Divisions ......................................................................................... 1 Neutrino and Astroparticle Division 2 High Energy Cosmic Ray Division 28 Astrophysics and Gravity Division 52 Observatories and a Research Center ......................................................................... 65 Norikura Observatory 66 Akeno Observatory 72 Kamioka Observatory 75 Kagra Observatory 76 Research Center for Cosmic Neutrinos 77 Appendix A. ICRR Workshops and Ceremonies ............................................................. 79 Appendix B. ICRR Seminars .............................................................................. 82 Appendix C. List of Publications .......................................................................... 82 (a) Papers Published in Journals (b) Conference Papers (c) ICRR Reports Appendix D. Doctoral Theses ............................................................................. 89 Appendix E. Public Relations ............................................................................. 89 (a) ICRR News (b) Public Lectures (c) Visitors Appendix F. Inter-University
  • Neutrino Experiments

    Neutrino Experiments

    Neutrino Experiments 1. Neutrinos and n observatories 2. Establishing n oscillation & mixing 3. Present questions and experiments Sofia Andringa, LIP July 2017 17th JINR-ISU Baikal Summer School on Physics of Elementary Particles and Astrophysics What are neutrinos? 1, 2, 3 n Neutrino n sources detection 1. Neutrinos and n observatories Discovery of neutrino oscillations the elementary particles g . g . W,Z Neutrino masses not to scale: == ZERO in the Standard Model what are neutrinos? 1930: an “undetected particle” ensuring energy conservation in b-decays (Pauli) Dear Radioactive Ladies and Gentlemen, (...) I have hit upon a desperate remedy to save (...) the law of energy conservation. (...) emitted together with the electron, in such a way that the sum of the energies (...) is constant. (...) electrically neutral particles (...) s n (Z,A) –> (Z+1,A) + b mass not larger than 0.01 proton mass(...) o r t c M(Z,A) = M(Z+1,A) + E e (...) the question concerning experimental proof of l e n –> p + e⁻ + v such a neutron, if it has something like about 10 times n i the penetrating capacity of a g -ray. y t i s n e t n I Electron kinetic energy (MeV) “inverse beta decay” 1934: Fermi, “attempt at a theory of b rays” weak interaction (GF~10⁻⁵ GeV ⁻ ²) cross-section ~ 10⁻⁴⁴ cm² for E ~ MeV mean free path of 10¹⁹ m in water or 1 out of 10¹⁹ interact in 1m of water need both a large number of neutrinos and a large number of targets (electron anti-)neutrinos detected 25 years after first proposal the Reines and Cowen experiment delayed coincidences in liquid scintilator Reines nobel lecture(1995) to detect neutrinos from nuclear reactors electron / muon / neutrino p -> mn -> enn are all the neutrinos the same? 3 types of detectable neutrinos Electron neutrino (1956) Muon neutrino (1962) (by Lederman, Steinberg & Schwartz, at BNL) following suggestion by B.
  • Search for Antineutrino Charged Current Coherent Pion Production at Sciboone Hide-Kazu TANAKA

    Search for Antineutrino Charged Current Coherent Pion Production at Sciboone Hide-Kazu TANAKA

    Search for Antineutrino Charged Current Coherent Pion Production at SciBooNE Hide-Kazu TANAKA Massachusetts Institute of Technology, Department of Physics, 77 Massachusetts Avenue, Cambridge, MA 02139-4307 Abstract. The SciBooNE experiment (Fermilab) recently published results of a search for charged current coherent pion production 12 −12 + in neutrino mode: muon neutrinos scattering on carbon, nm C → m Cp . The results of this study are that no evidence for coherent pion production is observed, and SciBooNE set 90% confidence level upper limits on the cross section ratio of charged current coherent pion production to the total charged current cross section. Recently proposed new coherent pion models predict a production of charged current coherent pion events just below the SciBooNE’s upper limit. Motivated by this, we performed a search for charged current coherent pion production using SciBooNE’s collected antineutrino data since antineutrino data are expected to be more sensitive to look at coherent pion production than neutrino data. This paper describes preliminary results of a search for antineutrino charged current coherent pion production at the SciBooNE experiment. Keywords: neutrino-nucleus cross-section, coherent pion production PACS: 01.30.Cc, 13.15.+g, 25.30.Pt INTRODUCTION The unknown neutrino mixing angle q13 is one of the most important goals in current neutrino experiments. For the next generation of long baseline neutrino oscillation experiments, T2K and NOvA, the precise measurement of neutrino-nucleus cross sections in the few GeV energy range is an essential ingredient in the interpretation of neutrino oscillation signals. Charged current single charged-pion production (CC-1p) is a dominant background process for nm → nX oscillation measurements.