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p. 1 Highlight talk from Super-Kamiokande 2018 July 12th (Thu) 7th International Conference on New Frontiers in Physics ICNFP 2018 @Kolymbari, Crete, Greece Yuuki Nakano for the Super-Kamiokande collaboration (Kamioka Observatory, ICRR, The University of Tokyo) Supported by Grant-in-Aid for Young Scientists (B) 17K17880 p. 2 Contents ■ Super-Kamiokande (SK) - Detector and history - Physics targets - Summary of recent publications ■ Atmospheric neutrino - 3-fravor oscillation analysis - Tau neutrino appearance ■ Solar neutrino - Solar neutrino flux measurements - Energy spectrum and oscillation analysis ■ Future prospect and summary p. 3 Super-Kamiokande collaboration Photo in 2015 Kamioka Observatory, ICRR, Univ. of Tokyo, Japan INFN Padova, Italy ~165 people RCCN, ICRR, Univ. of Tokyo, Japan INFN Roma, Italy 45 institutes, 9 countries University Autonoma Madrid, Spain Kavli IPMU, The Univ. of Tokyo, Japan University of British Columbia, Canada KEK, Japan University of Sheffield, UK Boston University, USA Kobe University, Japan Shizuoka University of Welfare, Japan University of California, Irvine, USA Kyoto University, Japan Sungkyunkwan University, Korea California State University, USA University of Liverpool, UK Stony Brook University, USA Chonnam National University, Korea LLR, Ecole polytechnique, France Tokai University, Japan Duke University, USA Miyagi University of Education, Japan The University of Tokyo, Japan Fukuoka Institute of Technology, Japan ISEE, Nagoya University, Japan Tokyo Institute of Technology, Japan Gifu University, Japan NCBJ, Poland Tokyo University of Science, japan GIST, Korea Okayama University, Japan University of Toronto, Canada University of Hawaii, USA Osaka University, Japan TRIUMF, Canada Imperial College London, UK University of Oxford, UK Tsinghua University, Korea INFN Bari, Italy Queen Mary University of London, UK The University of Winnipeg, Canada INFN Napoli, Italy Seoul National University, Korea Yokohama National University, Japan p. 4 Super-Kamiokande (SK) ■ Detector - Located at Kamioka Japan. - 50 kton of ultra pure water tank. - 20-inch PMTs, 11,129 for ID (since SK-III). - 22.5 kton for analysis fiducial volume. - Water Cherenkov light technique. ■ History of SK ν - Long term operation since 1996 (~22 years). m 41.4 - Total live time is more than 5,500 days. - Refurbishment works toward SK-Gd have started since May 31st, 2018. 39.3 m Nobel prize p. 5 Physics targets in SK Super- ■ Neutrinos Kamiokande - Astrophysical neutrinos → Solar neutrino → Supernova (relic) neutrino - Atmospheric neutrino - Accelerator (Long baseline) PPNP 67, 651 (2012) ■ Other physics - Proton decays - Dark matter search → From galactic center, Sun, Earth - Other exotic models Solar ν Supernova ν Atmospheric ν and proton decay < ~20 MeV ~20-~100 MeV ~100 MeV GeV TeV PeV p. 6 Recent publications from SK ■ Atmospheric neutrino - 3-fravor oscillation analysis: Phys. Rev. D 97, 072001 (2018). - Tau neutrino cross section: arXiv:1711.0943 [hep-ex]. - Atmospheric neutrino flux: Phys. Rev. D 94, 052001 (2016). ■ Solar neutrino - Energy spectrum measurement: Phys. Rev. D 94, 052010 (2016). - Day/night flux asymmetry: Phys. Rev. Lett. 112, 091805 (2014). ■ Proton decay (nucleon decay) - Anti-lepton plus meson: Phys. Rev. D 96, 012003 (2017). - p→e+π0 and p→μ+π0: Phys. Rev. D 95, 012004 (2017). - Invisible particle & charged lepton: Phys. Rev. Lett. 115, 121803 (2015). - Dinucleon decay into π: Phys. Rev. D 91, 072009 (2015). ■ Others (Dark matter search, Sterile ν and Lorentz invariance…) More detail: http://www-sk.icrr.u-tokyo.ac.jp/sk/publications/index.html p. 7 Atmospheric neutrino ■ Feature of atmospheric neutrino - Primary cosmic-ray interacts with nuclei in atmosphere. → π, K are produced and then μ, e are produced with neutrinos. - Travel length: O(~10) km - 13,000 km (zenith angle dependence). - Wide energy range : Sub-GeV to over TeV. Proton, Helium… Flux is precisely measured ν 흊 + 흊ഥ SK 흁 흁 흊풆 + 흊ഥ풆 ν Proton Helium… Isotropic flux of cosmic ray p. 8 Category of neutrino events Fully contained (FC) Partially contained (PC) Up-going μ (UPMU) ν μ e μ ν Also μ, multi-ring (decay electron) FC PC UPMU p. 9 Atmospheric neutrino in SK ■ Oscillation probability and sub-leading effects - SK has sensitivity to all PMNS parameters. ퟐ → Atmospheric ν oscillation is dominated by 흂흁 → 흂흉 ∆풎ퟐퟑ, 휽ퟐퟑ . - Sub-leading effects are expected in 흊풆 sample. → Resonant oscillation due to matter effect in the Earth. → Sensitive to mass hierarchy, 휽ퟐퟑ octant and CP phase. Due to solar term. 흂흁 → 흂흁 흂흁 → 흂풆 Flux normalization changes by CP phase. Resonant oscillation due to finite 휽ퟏퟑ. Enhancement of 흊풆 when normal hierarchy. (흊ഥ풆 when inverted) Sub-GeV Multi-GeV Sub-GeV Multi-GeV p. 10 Momentum Up-going μ PC sample Black point: Data SK-I~IV 5326 days Light Blue: MC Normal hierarchy p. 11 Neutrino oscillation analysis ■ Oscillation analysis (Only SK data) - Data set: SK-IV 2519 days → SK-I~IV: 5326 days (328 퐤퐭퐨퐧 ∙ 퐲퐞퐚퐫). ퟐ ퟐ ퟐ ퟐ ퟐ ퟐ - Scan 흌 for , 퐬퐢퐧 휽ퟐퟑ, 횫풎 → 횫흌 = 흌푵푯 − 흌푰푯 = −4.33 (SK only). ퟐ 퐬퐢퐧 휽ퟐퟑ ퟐ IH 퐬퐢퐧 휽ퟏퟑ = ퟎ. ퟎퟐퟏퟗ ± ퟎ. ퟎퟎퟏퟐ NH ퟐ ∆풎ퟑퟐ ퟐ ∆풎ퟑퟏ IH NH *Other experiments results → before Neutrino2018* p. 12 Neutrino oscillation analysis ■ Oscillation analysis with external constraint - Introduce constraint from T2K public data and reactor results. ퟐ ퟐ ퟐ - Normal hierarchy is slightly preferred, 횫흌 = 흌푵푯 − 흌푰푯 = −ퟓ. ퟐ. ퟐ ퟐ ∆풎ퟑퟐ 퐬퐢퐧 휽ퟐퟑ 휹퐂퐏 ퟐ ∆풎ퟑퟏ IH IH IH NH NH NH ퟐ 퐬퐢퐧 휽ퟏퟑ = ퟎ. ퟎퟐퟏퟗ ± ퟎ. ퟎퟎퟏퟐ (fix) ퟐ ퟐ [ −ퟑ ퟐ] ퟐ Mass hierarchy 흌 ∆풎ퟑퟐ,ퟑퟏ × ퟏퟎ 퐞퐕 퐬퐢퐧 휽ퟐퟑ 휹퐂퐏 +ퟎ.ퟎퟓ +ퟎ.ퟎퟑퟗ +ퟎ.ퟖퟏ Normal 639.43 ퟐ. ퟓퟎ−ퟎ.ퟏퟐ ퟎ. ퟓퟓퟎ−ퟎ.ퟎퟓퟕ ퟒ. ퟖퟖ−ퟏ.ퟒퟖ +ퟎ.ퟏퟑ +ퟎ.ퟎퟑퟓ +ퟏ.ퟎퟓ Inverted 644.70 ퟐ. ퟒퟎ−ퟎ.ퟎퟔ ퟎ. ퟓퟓퟎ−ퟎ.ퟎퟓퟏ ퟒ. ퟓퟒ−ퟎ.ퟗퟕ p. 13 Tau neutrino appearance ■ Tau neutrino in atmospheric sample - Detection of 흂흉 is critical for verifying 3-flavor mixing scheme. → Search for hadronic decay of 흉 lepton. - More than 3.5 GeV, Up-going sample has a chance. - Hard to identify event by event but can be statistically seen. 3.5 GeV 흂흁 → 흂흉 ~ퟏ 퐞퐯퐞퐧퐭/퐲퐞퐚퐫 ∙ 퐤퐭퐨퐧 Example of 흂흉 event (흂흉CC) Sub-GeV Multi-GeV p. 14 Signal and cross section ■ Analysis and its results - Event selection is performed using Neural Network. → Discriminate tau signal from background: Efficiency 76%. - 2D fit with signal scale parameter is evaluated. α = 0: no τ contribution α = 1: MC expected - α = 1.47±0.32 (stat.+syst.) → 4.6σ from 0 (NH assumed). SK-I~IV 흊흉 5326 days 흊ഥ흉 (0.94±0.20) ×10-38 cm2 Excess in up-going sample 338.1±72.7 events p. 15 Solar neutrino ■ Production of solar neutrino - Solar neutrinos are produced via nuclear fusions in the core. - Several processes makes electron-neutrino. → pp, pep, 7Be, 8B, hep and CNO - Standard solar model predicts their fluxes (SK can detect 8B/hep). SK Astrophys. J. 621 85 (2005). p. 16 Motivations of solar neutrino ■ Goal of solar neutrino measurement in SK (1) Test the transition of solar ν oscillation btw vacuum and matter. → Lowering threshold & reducing BG to test MSW up-turn. (2) Day-night flux asymmetry → Regeneration of 흊풆 due to the Earth’s matter effect is expected. (~2.5σ indication, update of this analysis is in progress). Super-Kamiokande p. 17 8B solar neutrino measurement ■ 8B solar neutrino signals − − - Elastic scattering (흊푿 + 풆 → 흊푿 + 풆 ). (1) Timing → Vertex position & real-time measurement (2) Ring pattern → Direction of the incoming neutrino (3) # of hit PMTs → Energy (~6 p.e./MeV) - ~20 events/day in SK-IV (SK-I~IV 5695 days: ~93k events). SK-IV 2860days +ퟑퟔퟑ ퟓퟓ, ퟕퟐퟗ−ퟑퟔퟏ (stat. only) Background Solar ν signals p. 18 8B solar neutrino flux ■ Flux measurements - SK has measured the 8B solar neutrino flux for 22 years. → Fluxes are consistent within uncertainties among all SK phases. SK flux/SNO NC flux = 0.4432±0.0084 (stat.+syst.). ■ Correlation of the flux with the solar activity - Solar activity is strongly correlated with sunspot numbers. - No correlation with the 11-years solar activity is observed. SK-II SK-I SK-III SK-IV 흌ퟐ = ퟐퟏ. ퟓퟕΤퟐퟏ DATA/MC = 0.4432±0.0084 (stat.+syst.) Prob. = 41.4% 8B flux= 2.33±0.04 [×106 cm-2sec-1] Sun spot number: http://www.sidc.be/silso/datafiles Source: WDC-SILSO, Royal Observatory of Belgium, Brussels. p. 19 Recoil electron energy spectrum SK-I SK-II 4.5 MeV 6.5 MeV 1496 days 791 days SK-III SK-IV 4.0 MeV 3.5 MeV 548 days 2860 days p. 20 Combined spectrum ■ Energy spectrum vs. MSW predictions - Introduce quadratic function to test the MSW prediction. ퟐ - Quadratic fit is consistent with solar 횫풎ퟐퟏ within 1.2σ, ퟐ while it disfavors KamLAND 횫풎ퟐퟏ by 2.0σ. Red point: Statistically added. Total # of bins of SK I-IV is 83, 80 dof 훘ퟐ Solar global 77.38 Solar+KamLAND 79.71 Quadratic best-fit 75.80 All SK phase are combined without regard to energy resolution or systematic uncertainty in this figure. p. 21 ퟐ ퟐ Constraint on 퐬퐢퐧 휽ퟏퟐ, ∆풎ퟐퟏ(SK vs. SNO) ■ Oscillation parameters from SK and SNO - SK result uniquely selects the LMA-MSW region by more than 3σ. ퟐ ퟐ - SK (SNO) gives the best constrain on ∆풎ퟐퟏ (퐬퐢퐧 휽). SNO SK+SNO SK Filled region 3σ p. 22 ퟐ ퟐ Constraint on 퐬퐢퐧 휽ퟏퟐ, ∆풎ퟐퟏ(solar vs. KamLAND) 2 sin 휃12 = 0.310 ± 0.014 2 +1.20 −5 2 ∆푚21 = 4.82−0.60 × 10 eV 2 +0.034 sin 휃12 = 0.316−0.026 2 +0.19 −5 2 ퟐ ∆푚 = 7.54 × 10 eV Constraint with 퐬퐢퐧 훉ퟏퟑ = ퟎ. ퟎퟐퟏퟗ ± ퟎ. ퟎퟎퟏퟒ 21 −0.18 2 from short baseline reactor. sin 휃12 = 0.310 ± 0.012 2 +0.19 −5 2 ∆푚21 = 7.49−0.17 × 10 eV SK+SNO (dash-line) Combined KamLAND Solar global Filled region 3σ ퟐ 2σ tensition in ∆풎ퟐퟏ between the solar global and KamLAND.
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    IUPAP Report 41a A Report on Deep Underground Research Facilities Worldwide (updated version of August 8, 2018) Table of Contents INTRODUCTION 3 SNOLAB 4 SURF: Sanford Underground Research Facility 10 ANDES: AGUA NEGRA DEEP EXPERIMENT SITE 16 BOULBY UNDERGROUND LABORATORY 18 LSM: LABORATOIRE SOUTERRAIN DE MODANE 21 LSC: LABORATORIO SUBTERRANEO DE CANFRANC 23 LNGS: LABORATORI NAZIONALI DEL GRAN SASSO 26 CALLIO LAB 29 BNO: BAKSAN NEUTRINO OBSERVATORY 34 INO: INDIA BASED NEUTRINO OBSERVATORY 41 CJPL: CHINA JINPING UNDERGROUND LABORATORY 43 Y2L: YANGYANG UNDERGROUND LABORATORY 45 IBS ASTROPHYSICS RESEARCH FACILITY 48 KAMIOKA OBSERVATORY 50 SUPL: STAWELL UNDERGROUND PHYSICS LABORATORY 53 - 2 - __________________________________________________INTRODUCTION LABORATORY ENTRIES BY GEOGRAPHICAL REGION Deep Underground Laboratories and their associated infrastructures are indicated on the following map. These laboratories offer low background radiation for sensitive detection systems with an external users group for research in nuclear physics, astroparticle physics, and dark matter. The individual entries on the Deep Underground Laboratories are primarily the responses obtained through a questionnaire that was circulated. In a few cases, entries were taken from the public information supplied on the lab’s website. The information was provided on a voluntary basis and not all laboratories included in this list have completed construction, as a result, there are some unavoidable gaps. - 3 - ________________________________________________________SNOLAB (CANADA) SNOLAB 1039 Regional Road 24, Creighton Mine #9, Lively ON Canada P3Y 1N2 Telephone: 705-692-7000 Facsimile: 705-692-7001 Email: [email protected] Website: www.snolab.ca Oversight and governance of the SNOLAB facility and the operational management is through the SNOLAB Institute Board of Directors, whose member institutions are Carleton University, Laurentian University, Queen’s University, University of Alberta and the Université de Montréal.
  • Retrospect of GALLEX/GNO

    Retrospect of GALLEX/GNO

    10th Int. Conf. on Topics in Astroparticle and Underground Physics (TAUP2007) IOP Publishing Journal of Physics: Conference Series 120 (2008) 052013 doi:10.1088/1742-6596/120/5/052013 Retrospect of GALLEX/GNO Till Kirsten Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany E-mail: [email protected] Abstract. After the completion of the gallium solar neutrino experiments at the Laboratori Nazionali del Gran Sasso (GALLEX, GNO), we shortly summarize the major achievements. Among them are the first observation of solar pp-neutrinos and the recognition of a substantial (40%) deficit of sub-MeV solar neutrinos that called for νe transformations enabled by non- vanishing neutrino masses. We also inform about a recent complete re-analysis of the GALLEX data evaluation and reflect on the causes for the termination of GNO. From our gallium data we extract the e-e survival probability Pee for pp-neutrinos after subtraction of the 8B and 7Be contributions based on the experimentally determined 8B- (SNO/SK) and 7Be- (Borexino) neutrino fluxes as Pee(pp only) = 0.52 ± 0.12. 1. Introduction The Gallium solar neutrino experiments at the Laboratori Nazionali del Gran Sasso have been terminated for external non-scientific reasons. This triggers a short retrospect of the achievements of GALLEX and GNO (Section 2). In Section 3 we report on a recent update that is based on data that were impossible to acquire before completion of the low rate measurement phase (solar runs). After some reflections on the causes for the termination of the gallium experiments at Gran Sasso (Section 4), I give a first quantitative estimate of the separate pp solar neutrino production (Section 5).
  • Current Research on Neutrinos

    Current Research on Neutrinos

    UNIT1: Experimental Evidences of Neutrino Oscillation Atmospheric and Solar Neutrinos Stefania Ricciardi HEP PostGraduate Lectures 2016 University of London 1 Neutrino Sources • Artificial: SUN – nuclear reactors First detected neutrinos – particle accelerators • Natural: – Sun Atmosphere – Atmosphere – SuperNovae – fission in the Earth core (geoNeutrinos) – Astrophysical origin (Old supernovae, AGN, etc.) Expected, but undetected so far,: – relic neutrinos from BigBang (~300/cm3 ) SuperNovae Neutrinos are everywhere! 2 Neutrino Flux vs Energy The Sun is the most intense detected source with a flux on Earth of of 6 1010 n/cm2s Abundant Detection of solar but challenging and atmospheric detection neutrino has provided the first compelling evidence of neutrino oscillations Below detection threshold of current experiments 3 D.Vignaud and M. Spiro, Nucl. Phys., A 654 (1999) 350 Atmospheric Neutrinos 4 Neutrino Production in the Atmosphere Absolute n flux has ~10% uncertainty But muon/electron neutrino ratio is known with ~3% uncertainty. Expected: (n n ) 2 (ne n e) 5 6 Cosmic Flux Isotropy We expect an isotropic Flux of neutrinos at high energies (earth magnetic field deviate path of low-momentum secondaries only : East-West effects) For En > a few GeV, and a given n flavour (Up-going / down-going) ~ 1.0 with <1 % uncertainty Note the baseline (= distance nproduction-ndetection) spans 3 order of magnitudes! 7 Atmospheric neutrino detectors Neutrinos in 100 MeV – 10 GeV energy. Flux ~ 1 event/(cm2 sr sec) Quasi-elastic interaction region Small cross-section Massive Detector (kTons) Background from charged cosmic rays deep underground location:mines, caverns under mountains, provide >1 Km rock overburden necessary to reduce the muon flux by 5-6 orders of magnitude 2 detection techniques: - Calorimetric - iron and tracking detectors (Nusex, Frejus, Soudan) - Cherenkov - water (Kamiokande, IMB) First detectors built to search for proton-decay.