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NNN2018 Summary M NNN2018 Summary M. Nakahata Kamioka Observatory, ICRR, Kavli IPMU, Univ. of Tokyo Disclaimer: Impossible to summarize all wonderful talks in short time given to me. Apologies for skipping many brilliant talks. 1 This year is the 20th Anniversary of Neutrino Oscillations NEUTRINO 1998 June 5, 1998@Takayama Kajita-san 2 Discoveries in last 20 years 1998 1999 2000 2001 2002 2003 2004 2005 2006 2007 Evidence for Evidence for Evidence for Evidence for (K2K) (MINOS) atmospheric solar ν osc. solar ν osc. reactor ν osc. Evidence for νµ ν osc. (SK) (SK vs. SNO CC) (SNO CC vs. NC) （KamLAND） disappearance by artificial ν 2008 2009 2010 2011 2012 2013 2014 2015 2016 2017 2018 (OPERA, 5.1σ) σ (Daya Bay) (RENO) (Double Chooz) (SK, 3.8 ) Indication of νe ν ν τ appearance appearance Observation of ̅e disappearance in reactor (T2K) 3 4 What we know now after the 20 years m2 NO m2 IO C. Giunti 2 2 m3 m2 2 m1 νe νµ ντ 2 m2 2 m 2 m1 3 Note: differences between global fit groups should be resolved. 5 Next Questions in Neutrino Physics M. Messier Which mass ordering? Normal or Inverted? S. Zhou Is CP violated? θ23 octant or full mixing? What is the absolute mass of neutrinos? Is neutrino mass Dirac or Majorana? Is there sterile neutrinos? 6 Mass ordering at present Global analyses Super-K atmospheric ν S. Mine C. Giunti IO NO T2K L. Kormos NO is favored over IO at ~3σ level. IO NO NOvA G. Pawloski IO NO 7 Mass Ordering in near future JUNO A. Garfagnini ∆χ2 ~10 JUNO only ∆χ2 ~14 2 (if accuracy of ∆m µµ is Phys.Rev. D88 (2013) 013008. constraint to be 1% by long baseline exp.) Data taking will start in 2021. KM3NeT(ORCA)/PING ORCA σ C. Nielsen J. Hignight ~4 level for full mixing. 8 Mass Ordering, eventually DUNE A. Sousa 9 CP violation now T2K L. Kormos NOvA G. Pawloski CP conserving values of Excludes CP=π/2 of IO at CP lie outside 2σ region. >3σ but CP conserving values still allowed. 10 CP violation now With same horizontal axis Similar shape for IO. T2K More statistics are necessary to discuss further. NOvA 11 Future δCP measurement DUNE Hyper-Kamiokande A. Sousa A. Pritchard J. Walker C. Marshall DUNE Hyper-K Baseline 1300 km 295 km Beam energy Several GeV ~0.6 GeV Earth Matter effect Large Small (sensitive to mass ordering) (less effect from mass ordering) Detector 40 kton Liquid Ar TPC 190 kton water Cherenkov Complementary measurements. 12 Hot news from DUNE and Hyper-K A. Sousa A. Pritchard The protoDUNE SP at CERN taking beam and cosmic-ray data. Hyper-K construction will begin in April 2020. 13 Future δCP measurement DUNE Hyper-Kamiokande A. Sousa A. Pritchard Precision of δCP measurement (10 years) ~16o (~7o) for δCP=±90o (0o ) ~22o (~7o) for δCP=±90o (0o ) 14 S. Zhou 15 Sign doors at Kamioka 16 The first door at Kamiokande Sheldon Lee Glashow Aug.30, 1984 I shall decay when the proton returns! Paul Langacker August 5, 1985 Decay or not decay? That is the question. 17 Yoichiro Nambu’s sign My interpretation Kamiokande era It would take a hundred years to discover proton decay, if you keep taking data with Kamiokande. You must make a much bigger detector. A hundred years at Kamiokande = a few years at Hyper-Kamiokande 18 Proton decay current results S. Mine SNO+ limit on 3ν decay mode M. Askins 19 Proton decay sensitivity of HK A. Pritchard pe+π0 pνK+ 3σ discovery sensitivity: 3σ discovery sensitivity: τ/BR=10^{35} years τ/BR=3x10^{34} years 20 Double beta decay Unique method to investigate Majorana feature of neutrino mass. A. Gando 21 Summary of “multi-messenger signals” from exploding 17 Msun star Nakamura, Horiuchi, Tanaka, Hayama, Takiwaki, KK (MNRAS) 2016 53 51 49 46 Energetics: Eneutrino ~10 erg, Ekinetic ~10 erg, Ephoton ~ 10 erg, EGW ~ 10 erg Matzner & McKee’99 (Mej, Eexp, Rstar) Popov’93 (Mej, Eexp, Rstar) Odrzywolek+’04 (15 Msun model) K. Kotake High frequency variation by SASI might be observed. K. Kotake E. O’Sullivan Supernova burst detectors in the world now Liquid scintillator Water, Ice Super-Kamiokande Other Borexino LVD Baksan target mass SNO+ 0.3 kt 0.3 kt 1 kt 32 kt 1 kt KamLAND HALO Pb 76 t MicroBooNE NOvA surface Daya Bay 1 kt IceCube Ar 1 gt 90 t surface 14 kt 0.16 kt 24 Supernova in Future Large Volume Detectors JUNO(China) DUNE/LBNF (US) Hyper-Kamiokande (20kton Liq. Sci.) (40 kton Liq. Ar) (220 kton Water) ν ν 40 → - 40 50~80k e̅ p for 10 kpc SN. Precise measurement e + Ar e + K* is the dominant 2~3k events for LMC, of average energy and ~10 events for M31. luminosity for all interaction. neutrino flavors. ~4000 events for 10kpc Precise measurement of SN. ~60 events from time variation (e.g. SASI). ~1% for <E> for νe̅ neutronization burst for 3~4k ν+e gives ~1 deg. ~10% for <E> for νe IO case (~0 for NO). ~5% for <E> for νX pointing accuracy. A. Pritchard A. Garfagnini A. Sousa E. O’Sullivan 25 Diffuse supernova ν in SK-Gd M. Smy Similar sensitivity expected at JUNO too. 26 Multi-messenger Astronomy Opening a new window J. Kiryluk On 22 September 2017 IceCube Chandra detected a ~290-TeV neutrino from Cassiopeia A H.E.S.S. a direction , as reported by Fermi- LAT on September 28 2017, consistent with the flaring g-ray blazar TXS 0506+056. 27 High energy neutrino astronomy by IceCube J. Kiryluk Spectrum index depends on event type. J. Hignight Chandra Cassiopeia A EHE IceCube spectrum 28 High Energy Neutrino Astrophysics: Future KM3NeT/ARCA IceCube Upgrade C. Nielsen ARA IceCube-Gen2 N. Whitehorn J. Hignight 29 Anomalies Anomalies (problems) are important for future discoveries, e.g. “solar neutrino problem” in the Homestake experiment and atmospheric ν anomaly in Kamiokande. 30 Reactor Anomaly H. Band Composition of the reactor core change with time. 239Pu yield is consistent with model. 235U yield disagree with the model at ~3σ level. This result suggests that this isotope may be the primary source of the anomaly. Daya Bay RENO 31 New Solar Neutrino Problem? M. Smy (averaged) vacuum matter effect is oscillation dominant Borexino (pp) dominant all solar (pp) Borexino (7Be) Borexino (pep) Borexino (8B) 2 Δm 21 MSW: solar+KamLAND best fit 2 sin θ12=0.308 2 -5 2 Δm 21=7.50x10 eV KamLAND Homestake MSW: solar best fit Super-K 2 +SK+SNO solar sin θ12=0.311 2 2 -5 2 (CNO) +SNO sin θ12 Δm 21=4.85x10 eV MeV 2 Tension in Δm 21 between reactor and solar neutrinos. In future, spectrum and day/night measurements by A. Garfagnini E. O’Sullivan Hyper-K and JUNO should solve the issue. SNO+ and Borexino has potential to measure CNO neutrinos. E. O’Sullivan 32 LSND/MiniBooNE anomaly B. Russell Analysis of MicroBooNE data is on-going. We hope to see phase 1 results in near future. SBND: Detector construction on-going. Plan to begin taking data in 2020 ICARUS: Currently instrumenting and commissioning the detector Plan to begin taking data in 2019 33 New underground sites A. Garfagnini S. Nakayama JUNO Hyper-K 650 m underground ~700 m underground LBNF/DUNE J. Tang CJPL 2400 m underground 1475 m underground 34 Development for possible future large volume detectors G. D. Orebi Gann Development of water-based LS More interesting plots. See Dr. Gann’s presentation ANNI V. Fischer 35 Conclusion • Fantastic neutrino physics in last 20 years. • We expect another interesting ~20 years. • Let’s continue to enjoy neutrino physics. • Hope to discover proton decays and double beta decays sometime in future. 36.
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