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Highlight Talk from Super-Kamiokande 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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