Peruvian participation in Neutrino experiments at FERMILAB-USA

Transcription

1 Peruvian participation in Neutrino experiments at FERMILAB-USA XXVII Simposio Peruano de Física Carlos Javier Solano Salinas Laboratorio de Altas Energías, Cosmología and Astrofísica (LAECyA) Facultad de Ciencias, Universidad Nacional de Ingeniería 1

2 Outline Modern Physics Standard Model Neutrino History Neutrino oscillations Neutrino-Nucleus interaction: MINER A DUNE 2

3 MODERN PHYSICS Two scientific revolutions in first half of XX century Relativity Special Relativity We can not reach the light speed Mass is a form of energy: E = m c2 General Relativity GR encompasses gravity and describes the expanding universe and black holes. Quantum mechanics To describe anything as small as a atom requires the use of Quantum Mechanics. Uncertainty principle of Heisenberg 3

4 STANDARD MODEL One of the great intellectual achievements of the second half of the 20th century It is based on the Relativistic Theory of Quantum Fields (QFT) The first QFT was the quantum theory of Electricity and Magnetism (QED) 4

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6 NEUTRINO HISTORY Proposed by W. Pauli (1930) to explain the continuous spectrum of electrons in the β decay of neutrons n p + e- + e with ~ cm2 E. Fermi ( ) -> Beta decay theory (weak interactions, neutrinos) C. Cowman y F. Reines -> e (1956), Nobel 1995 L.Lederman, M.Schwartz, J.Steimberger --> (1962), (1975), Nobel

7 NEUTRINO REVOLUTION Neutrino revolution ( ) Neutrinos have a mass different from zero Mix of leptons! The sun seen with neutrinos Solar Neutrinos: trillons/sec Big Bang neutrinos: 10 million/s inside of us 7

8 NEUTRINO OSCILLATIONS 8

9 Neutrinos come in at least three flavors The known flavors of neutrinos: Each of them is associated with the corresponding loaded lepton: e e 9

10 The meaning of this association 10

11 In short distances neutrinos do not change flavor short journey This does not happen!! But if neutrinos have mass, and leptons are mixed, changes in the taste of neutrinos occur on long trips 11

12 Atmospheric Neutrinos Cosmic ray isotropy > 2 GeV + Gauss Law + Non-disappearance of But Super-Kamiokande (Japan) find for E > 1.3 GeV

13 Observing Neutrinos Davis y Koshiba, Nobel 2002 Super-Kamiokande, neutrino detector 13

14 Solar Neutrinos The Homestake experiment (USA) could only detect e. It found: 14

15 Solar Neutrinos 15

16 In Lab system - The experiment fix L and t These are common to all beam components 16

17 Probability for Oscillation of Neutrinos in Vacuum 17

18 Probability for Oscillation of Neutrinos in Vacuum Neutrino Oscillations With some simple algebra, the oscillation probability! 2 2 m [ev ]L [km] 2 2 P (! P( e) = sin (2 ) sin 1.27 eµ E [G ev ] Mixing angle: determines amplitude of oscillagons e e e e e e e e e e e e e e e e e e Mark Thomson DUNE

19 NEUTRINO-NUCLEUS INTERACTIONS 19

20 What are the Open Questions in Neutrino Physics? What are the masses of the neutrinos? What is the pattern of mixing among the different types of neutrinos? Are neutrinos their own antiparticles? Do neutrinos violate the symmetry CP? Are there sterile neutrinos? Do neutrinos have unexpected or exotic properties? What can neutrinos tell us about the models of new physics beyond the Standard Model? Some of these questions (like neutrino oscillations) can only be answered with experiments involving understanding how neutrinos interact with matter! What MINERvA does well is measure cross sections and differences of the interaction in different nuclei, and compare between neutrino and antineutrino interactions!!! 20

21 Motivation: We are in a period of high precision measurements of neutrino oscillation Oscillation Measures: For the NuMI / MINOS beam, a distortion in the energy distribution of is expected for E < 3 GeV -Probability of Oscillation depends on E However, the experiments measure Evis -Evis depends on the flux,, and the response of the detector Multiple interactions and type of particles produced Complications: The near/far flux are different --> The effective section is not canceled on the ratio The low effective energy section (few GeV) is not well understood - There are few data: Bubble Chamber --> small statistics and big systematic error - Data with high A (for example, Fe) is required. We must use unproven models to incorporate nuclear effects Solution : MINER A Place a fine-grained detector in a highintensity neutrino beam - NuMI Beamline 21

22 MINER A goals Precision measurement of cross sections in the 1-10 Gev region Understand the various components of cross section both CC and NC CC & NC quasi-elastic Resonance production, (1232) Resonance deep inelastic scatter (quark-hadron duality) Deep Inelastic Scattering Study A dependence of interactions in a wide range of nuclei 22

23 Beam-line NuMI Beamline Graphic courtesy B. Zwaska MINERvA MINOS 23

24 MINER A Institutions MINOS Pitt Tufts NOVA William & Mary FNAL Duluth Texas Northwestern Florida Athens MCLA (Mass.) Otterbein UNI (Peru) PUCP (Peru) CBPF (Brazil) Guanajuato (Mex) Dortmund INR, Moscow MINERVAHampton Irvine T2K MiniBooNE Rochester Valparaiso (Chile) James Madison Rutgers Theory Jefferson Lab Nuclear 24 24

25 MINER A Detector 120 planar modules. Total Mass: 200 tons. Total channels: ~32K Fully Active Fine Segmented Scintillator Target 8.3 tons, 3 tons fiducial LHe ¼ ton MINOS Near Detector (Muon Spectrometer) VetoW all Nuclear Targets with He, C, Fe, Pb, H2O,CH In same experiment reduces systematic errors between nuclei 25

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27 Tracking Scintillator Planes Strips 3 diferent orientations of strip Particule WLS fiber glued into scintillator

28 Nuclear Targets 5 Nuclear Targets: Fe Pb C 28

29 MINERvA events QE DIS showing X view Anti- QE NC

30 Latin american groups in MINER A D.A.M. Caicedo, C. Castromonte, G.A. Fiorentini, J.L. Palomino, C. Sotelo, H. da Motta Centro Brasileiro de Pesquisas Físicas, Rio de Janeiro, Brazil J. Felix, A. Higuera, Z. Urrutia, G. Zavala Universidad de Guanajuato, León Guanajuato, México J. L. Bazo, L. Aliaga, J. P. Velasquez, G. Diaz, M. J. Bustamante, A. M. Gago Pontificia Universidad Católica del Perú, Lima, Perú K. Hurtado, M. Alania, A. Chamorro, C. Romero, A. Zegarra, G. Salazar, E. Chavarria, J. Huancco, C. J. Solano Salinas Universidad Nacional de Ingeniería, Lima, Perú (since 2006 seven UNI master thesis and ~30 publications in journals with high impact factor) W. Brooks, E. Carquina, G. Maggi, C. Peña, I. Potashnikova, F. Prokoshin Universidad Técnica Federico Santa María, Valparaíso, Chile 30

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32 La UNI en Fermilab - Experimento MINERvA Kenyi Hurtado Cesar Castromonte Marcos Alania Antonio Zegarra Edgar Chavarria Gerald Salazar Julian Huancco Adolfo Chamorro Carlos Romero COLABORADORES (egresados UNI): Javier Solano Arturo Fiorentni Jose Palomino 32 Cesar Sotelo

33 La PUCP en Fermilab - Experimento MINERvA Leónidas Aliaga Carlos Pérez Carmen Araujo José Bazo Noemí Ochoa Juan Pablo Velásquez María José Bustamante José Becerra Sebastán Sánchez Gonzalo Díaz 33

34 Next steps We will continue studying neutrino-nucleus interactions Physics, now at medium energies. The experiment will stop running in 2020, but we expect to continue analysing its data some time more. In this moment we have some studies for kaon production but we are preparing samples of DIS events with hyperon production in order to study the hyperon/anti-hyperon asymmetry and polarization. Since 2016 UNI (FC) is an official institution of DUNE collaboration!!! 34

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36 What is DUNE? The Deep Underground Neutrino Experiment (DUNE) Probably the next largest global project in particle physics. It aims to "do for neutrinos what the LHC (Great Hadron did for the Higgs." It will have the potential to make great discoveries in the area of neutrinos and astrophysics. ~1000 employees, 170 institutions, +30 countries. Latin America: Mexico, Colombia, Brazil and Peru. 36

37 Peruvian DUNE institutions Initially the peruvian official institutions are: Universidad Nacional de Ingeniería (UNI): C. J. Solano Salinas, C. Castromonte, O. Pereyra (and we expect more in a near future) Pontificia Universidad Católica del Perú (PUCP): A. M. Gago, J. L. Bazo, J. Jones And, as UNI, we are just working with (future DUNE institutions): Comisión Nacional de Investigación y Desarrollo Aeroespacial (CONIDA): L. Otiniano Universidad Nacional Mayor de San Marcos (UNMSM): T. Vargas, R. Tovar 37

38 Primary goals of DUNE It will try to answer some open questions in particle physics and astrophysics. Neutrino oscillations: Accurate measurement of oscillation parameters Determine the correct ordering of the neutrino masses. It will provide evidence, a favor against, on the violation of the symmetry of charge-parity (CP) conjugation in the lepton sector. Proton decay Never observed experimentally but predicted by several Great Unification theories (GUT s): Physics of neutrinos produced in the explosion of Supernovas Sensible to electron neutrinos (νe) produced by the collapse of a Supernova. 38

39 Near detector to characterize the beam Overview of DUNE South South Dakota Dakota Chicago Chicago & & ee FD FD Barrel'' Barrel'' RPCs' RPCs' Magnet' Coils' Magnet' Coils' Barrel' ECAL' Barrel' ECAL' STT'Module' STT'Module' Backward'ECAL' Backward'ECAL' End' End' RPCs' RPCs' Forward' ECAL' Forward' ECAL' End' End' RPCs' RPCs' ND ND Mark Mark Thomson Thomson DUNE DUNE Beam of muon neutrinos/antineutrinos generated in the LBNF. Max energy of 2,5 GeV and 1,2 MW of power. A Near Detector to characterize the neutrino beam. An underground Far Detector : liquid argon temporary projection chamber (LArTPC). 4 x 17 kton, with fiducial mass (usable) > 40 kton. 39

40 The Near Detector of DUNE Designed to characterize the neutrino beam and perform some high precision studies. It will provide data on cross sections and on the flow of neutrinos. It allows the use of several targets: argon, carbon, calcium, iron. Highly granulated interior, magnetic field of 0.4 T. ~10 ~1077 interactions/year interactions/year 40

41 The Far Detector of DUNE Time Projection Chambers of liquid argon (LArTPC's) 4 independent modules (cryostats) of ~ 17 kton built in stages. ~ 40 kton of total (usable) fiducial volume of liquid argon. DUNE Design = The liquid argon is at the same time Far detector: 40-kt LAr-TPC target and medium of detection. Dimensions of each cryostat: 15.1 (width) x 14.0 (height) x 62 (length) m3. First module planned for Near detector: Multi-purpose high-resoluti Barrel' Barrel' STT'Module' STT'Module' Backward'ECAL' Backward'ECAL'

42 LArTPC Technology Liquid Argon TPC Basics A modular implementation of Single-Phase TPC Record ionization in LAr volume 3D image E Cathode planes Anode planes e 180kV C A Steel Cryostat A Mark Thomson DUNE w ire # 3.6 m 14.4 m 32 C w ire # A C w ire # 12 m A time / ms time /time ms / ms 42

43 LArTPC Technology Benefits of an imaging detector e.g. for electron neutrino appearance e± $ γ separagon is vital «True for both photons from 0! γγ or single photons Single electron 0 gg Calorimetry to tag electrons/ gammas using de/dx before EM shower evolves e γ! e+e Mark Thomson DUNE

44 LArTPC (J. Huancco simulations) 44

45 Current status of DUNE experiment DUNE is moving forward with big steps Excavation of the caverns: 2017 Construction of the prototype (ProtoDUNE) at CERN: 2018 Construction of the Far Detector (cryostat # 1): 2019 Installation of the Far Detector (cryostat # 1): 2021 Start of operations with the Far Detector (cryostat # 1): 2024 DUNE intend to take data for at least 20 years! 45

46 Summary Crucial and exciting moment for neutrino Physics. DUNE will develop a quite broad program in order to answer fundamental questions in particle physics: Neutrino oscillation: hierarchy of the masses and violation of CP. Decay of the proton, neutrinos of the supernova explosion. Surprises: non-standard interactions, sterile neutrinos, etc. Since DUNE is in the training stage, it is an optimal time to try to participate in this experiment! 46

47 Thanks! 47