HARP Targets Pion Production Cross Section and Yield Measurements: Implications for Miniboone Neutrino Flux
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Arxiv:1812.08768V2 [Hep-Ph] 3 Dec 2019
IPPP/18/113/FERMILAB-PUB-18-686-A-ND-PPD-T Testing New Physics Explanations of MiniBooNE Anomaly at Neutrino Scattering Experiments 1, 2, 3, Carlos A. Argüelles, ∗ Matheus Hostert, y and Yu-Dai Tsai z 1Dept. of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 2Institute for Particle Physics Phenomenology, Department of Physics, Durham University, South Road, Durham DH1 3LE, United Kingdom 3Fermilab, Fermi National Accelerator Laboratory, Batavia, IL 60510, USA (Dated: December 5, 2019) Heavy neutrinos with additional interactions have recently been proposed as an explanation to the MiniBooNE excess. These scenarios often rely on marginally boosted particles to explain the excess angular spectrum, thus predicting large rates at higher-energy neutrino-electron scattering experiments. We place new constraints on this class of models based on neutrino-electron scattering sideband measurements performed at MINERνA and CHARM-II. A simultaneous explanation of the angular and energy distributions of the MiniBooNE excess in terms of heavy neutrinos with light mediators is severely constrained by our analysis. In general, high-energy neutrino-electron scattering experiments provide strong constraints on explanations of the MiniBooNE observation involving light mediators. Introduction – Non-zero neutrino masses have been the experiment has observed an excess of νe-like events established in the last twenty years by measurements of that is currently in tension with the standard three- neutrino flavor conversion in natural and human-made neutrino prediction and is beyond statistical doubt at the sources, including long- and short-baseline experiments. 4:7σ level [5]. While it is possible that the excess is fully The overwhelming majority of data supports the three- or partially due to systematic uncertainties or SM back- neutrino framework. -
Miniboone Anomaly and Nuclear Physics 4
1. MiniBooNE 2. Beam 3. Detector MiniBooNE Anomaly and Nuclear physics 4. Oscillation 5. Discussion PRL121(2018)221801 outline 1. MiniBooNE neutrino experiment 2. Nucleon correlations 3. Pion puzzle 4. NC single photon production 5. Conclusions Teppei Katori Queen Mary University of London ECT* workshop, Trento, Italy, April 15, 2019 Teppei Katori, [email protected] 15/04/19 1 1. MiniBooNE 2. Beam 3. Detector 4. Oscillation 5. Discussion 1. MiniBooNE neutrino experiment 2. Nucleon correlations 3. Pion puzzle 4. NC single photon production 5. Discussions Teppei Katori, [email protected] 15/04/19 2 1. MiniBooNE 2. Beam 3. Detector 4. Oscillation 5. Discussion Teppei Katori, [email protected] 15/04/19 3 1. MiniBooNE 2. Beam 3. Detector 4. Oscillation 5. Discussion The most visible particle physics result of the year Teppei Katori, [email protected] 15/04/19 4 https://physics.aps.org/articles/v11/122 PHYSICAL REVIEW LETTERS 120, 141802 (2018) signature of dark matter annihilation in the Sun [5,6]. 1. MiniBooNE Despite the importance of the KDAR neutrino, it has never MiniBooNE 2. Beam been isolated and identified. 3. Detector 86 m 4. Oscillation In the charged current (CC) interaction of a 236 MeV νμ background KDAR 12 − NuMI 5. Discussion (νμ C → μ X), the muon kinetic energy (Tμ) and closely beam decay pipe related neutrino-nucleus energy transfer (ω E − E ) horns ν μ target distributions are of particular interest for benchmarking¼ absorber neutrino interaction models and generators, which report widely varying predictions for kinematics at these tran- 5 m 675 m sition-region energies [7–14]. -
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. -
Icecube Sterile Neutrino Searches
EPJ Web of Conferences 207, 04005 (2019) https://doi.org/10.1051/epjconf/201920704005 VLVnT-2018 IceCube Sterile Neutrino Searches 1, B.J.P. Jones ∗ For the IceCube Collaboration 1University of Texas at Arlington, 108 Science Hall, 502 Yates St, Arlington, TX Abstract. Anomalies in short baseline experiments have been interpreted as evidence for additional neutrino mass states with large mass splittings from the known, active flavors. This explanation mandates a corresponding signa- ture in the muon neutrino disappearance channel, which has yet to be observed. Searches for muon neutrino disappearance at the IceCube neutrino telescope presently provide the strongest limits in the space of mixing angles for eV- scale sterile neutrinos. This proceeding for the Very Large Volume Neutrino Telescopes (VLVnT) Workshop summarizes the IceCube analyses that have searched for sterile neutrinos and describes ongoing work toward enhanced, high-statistics sterile neutrino searches. 1 Introduction Sterile neutrinos are hypothetical particles that have been invoked to explain anomalies in short baseline accelerator decay-at-rest [1] and decay-in-flight experiments [2], reactor neu- trino fluxes [3, 4] and radioactive source experiments [5]. In low-energy, short baseline exper- iments that are sensitive to νe appearance, matter effects can be neglected and an oscillation of the form: 2 2 2 ∆m L Pν ν = sin 2θµe sin (1) µ→ e 4E is predicted. A large ∆m2 thus introduces an oscillation at a small characteristic L/E, with 2 the effective mixing parameter, sin 2θµe governing the amplitude of oscillation. To introduce flavor-change at similar L/E as exhibited in the MiniBooNE and LSND experiments, mixing 2 3 parameters sin 2θµe of 10− or larger are required, with favored parameter space in the one- to-few eV2 mass splittings. -
Current Status of Neutrino Anomalies
Current Status of Neutrino Anomalies Srubabati Goswami Physical Research Laboratory, Ahmedabad, India Anomalies 2020 !1 Is it a monument, a madrasa or a market square? Charminar holds many mysteries within its fold https://www.thehindu.com/society/history-and-culture/the-very-many-mysteries-of-hyderabads-charminar/ article24311906.ece !2 Neutrino: many questions ❖ What Unknown oscillation parameters - hierarchy, octant of 2-3 mixing angle and CP phase ❖ Absolute neutrino masses — beta decay, cosmology ❖ Nature of neutrinos - Dirac or Majorana — neutrino less double beta decay ❖ Are there more than three flavours — sterile neutrinos ❖ Origin of neutrino masses and mixing — seesaw , flavour symmetry — physics beyond Standard Model !3 Neutrino Connections Baryogenesis via Collider leptogenesis Physics Dark Matter Higgs/Vacuum Cosmology stability Neutrinos Astrophysics/ CLFV Multimessenger Nucl. Physics/ interactions !4 Plan of talk New physics Neutrino Neutrinoless Ultra high In neutrino Oscillation double Energy neutrinos Parameters oscillation beta decay NSI Sterile Nus !5 Neutrino Oscillations Solar Atmospheric Reactor Accelerator !6 New result from Borexino !7 First detection of CNO neutrinos R(CNO) = 7.2 +2.9 -1.7 cpd/100ton Null hypothesis(CNO=0) rejected at 5.1 sigma. G. Ranucci , Neutrino 2020 !8 Three Neutrino Paradigm ❖ Measurement of non-zero in reactor experiments three neutrino picture !9 NOvA Results Joint analysis of disappearance and Appearance data in both neutrino and antineutrino channel ❖ P Preference for Neutrino 2020 !10 -
“ Chamber” Neutrino Physi Years After Gargamelle
35 years after Gargamelle: the Renaissance of the “ Bubble chamber” neutrino physics Carlo Rubbia CERN, Geneva, Switzerland INFN-Assergi, Italy C. Rubbia, CERN, 0ct09 111 A Gargamelle neutrino event QuickTime™ and a decompressor are needed to see this picture. Charm production in a neutrino interaction The total visible energy is 3.58 GeV. C. Rubbia, CERN, 0ct09 Slide: 2 The path to massive liquid Argon detectors CERN 1 2 Laboratory work CERN CERN 3 T600 detector 4 2001: First T600 module 5 20 m Cooperation with industry C. Rubbia, CERN, 0ct09 Slide: 3 T600 in hall B (CNGS2 -2009) QuickTime™ and a decompressor are needed to see this picture. C. Rubbia, CERN, 0ct09 Slide: 4 Thirty years of progress........ LAr is a cheap liquid Bubble diameter ≈ 3 mm (≈1CHF/litre), vastly (diffraction limited) produced by industry Gargamelle bubble chamber ICARUS electronic chamber “Bubble” size 3 x 3 x 0.3 mm3 T300 real event Medium Heavy freon Medium Liquid Argon Sensitive mass 3.0 ton Sensitive mass Many ktons Density 1.5 g/cm3 Density 1.4 g/cm3 Radiation length 11.0 cm Radiation length 14.0 cm Collision length 49.5 cm Collision length 54.8 cm dE/dx 2.3 MeV/cm dE/dx 2.1 MeV/cm C. Rubbia, CERN, 0ct09 Slide: 5 Summary of LAr TPC performances l Tracking device ØPrecise event topology ØMomentum via multiple scattering l Measurement of local energy deposition dE/dx T300 real event Øe / γ separation (2%X 0 sampling) ØParticle ID by means of dE/dx vs range l Total energy reconstruction of the events from charge integration ØFull sampling, homogeneous calorimeter with excellent accuracy for contained events RESOLUTIONS Low energy electrons: σ(E)/E = 11% / √ E(MeV)+2% Electromagn. -
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
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. -
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. -
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. -
Measurement of the Cosmic Ray and Neutrino-Induced Muon Flux at the Sudbury Neutrino Observatory
Lawrence Berkeley National Laboratory Lawrence Berkeley National Laboratory Title Measurement of the Cosmic Ray and Neutrino-Induced Muon Flux at the Sudbury Neutrino Observatory Permalink https://escholarship.org/uc/item/6nk6379r Author Aharmim, B. Publication Date 2009-08-01 Peer reviewed eScholarship.org Powered by the California Digital Library University of California Measurement of the Cosmic Ray and Neutrino-Induced Muon Flux at the Sudbury Neutrino Observatory ! ! ! ! The SNO Collaboration ! ! ! ! ! ! This work was supported by the Director, Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. DISCLAIMER This document was prepared as an account of work sponsored by the United States Government. While this document is believed to contain correct information, neither the United States Government nor any agency thereof, nor The Regents of the University of California, nor any of their employees, makes any warranty, express or implied, or assumes any legal responsibility for the accuracy, completeness, or usefulness of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by its trade name, trademark, manufacturer, or otherwise, does not necessarily constitute or imply its endorsement, recommendation, or favoring by the United States Government or any agency thereof, or The Regents of the University of California. The views and opinions of authors expressed herein do not necessarily state or reflect those of the United States Government or any agency thereof or The Regents of the University of California. Measurement of the Cosmic Ray and Neutrino-Induced Muon Flux at the Sudbury Neutrino Observatory B. -
Miniboone, LSND, and Future Very-Short Baseline Experiments
1 MiniBooNE, LSND, and Future Very-Short Baseline Experiments Mike Shaevitz - Columbia University BLV2011 - September, 2011 - Gatlinburg, Tennessee Neutrino Oscillation Summary 2 ! µ " ! Sterile " ! e New MiniBooNEνµ consistent OPERA : νµ→ντ ⇒ & ICARUS Confirmed by K2K and Minos accelerator neutrino exps New θ13 Information! νe→νµ / ντ ⇒ Confirmed by Kamland reactor neutrino exp Possible Oscillations to Sterile Neutrinos 3 Sterile neutrinos – Partners to the three standard neutrinos – Have no weak interactions (through the standard W/Z bosons) – Would be produced and decay through mixing with the standard model neutrinos – Are postulated in see-saw models to explain small neutrino masses – Can affect oscillations through mixing Cosmological Constraints NS = # of Thermalized Sterile ν States Oscillation Patterns with Sterile Neutrinos 3 + 1 3 + 2 68%, 95%, 99% CL 4 LSND νµ →νe Signal + + " # µ ! µ + e ! e! µ Saw an excess of: Oscillations? ! e 87.9 ± 22.4 ± 6.0 events. With an oscillation probability of (0.264 ± 0.067 ± 0.045)%. LSND in conjunction with the atmospheric and solar oscillation results needs more than 3 ν’s 3.8 σ evidence for oscillation. ⇒ Models developed with 1 or 2 sterile ν’s The MiniBooNE Experiment 5 at Fermilab LMC + ? K+ µ 8GeV π+ νµ νµ→νe Booster magnetic horn decay pipe absorber 450 m dirt detector and target 25 or 50 m • Goal to confirm or exclude the LSND result - Similar L/E as LSND – Different energy, beam and detector systematics – Event signatures and backgrounds different from LSND • Since August 2002 have