The Super-Kamiokande Collaboration

Super-Kamiokande and IceCube- two complementary approaches to neutrino astronomy..thanks to many for providing slides (knowingly or not )IceCube Counting House

Kamioka Mountain

Lutz KpkeJohannes Gutenberg University MainzCCAPP, Columbus, Ohio, April, 4, 2011OutlineIntroduction, detector principles and sensitivitiesNeutrino oscillation physicsHigh energy neutrino astronomyCore collapse supernovae

Main objectives of Super-Kamiokande and IceCube:Determine properties, interactions and QM of neutrinosTest extensions of our standard field theory larger symmetry groups (e.g. Proton Decay) additional symmetries (e.g. Super-Symmetry) symmetry violations (CPT, Lorentz etc. )Discover origin of cosmic rays and nature of cosmic catalcysms

1. Introduction and detectorsNobel Prize 2002A professor denounced me as being no good at physics. That made me furious. So I took the entrance exam for the physics department.

Moisei Alexandrovich MarkovMid 1950s: proposal for deep underground and underwater neutrino observatoriesMasatoshi Koshiba Grandfathers of astronomyMarkov warned the soviet leaders in 1947 about dangerous political-ideological moves that threaten to separate soviet science from thre rest

This was a brave (almost suicidal) move, as he and other scientists were charged of not sufficiently quoting Russian scientists and uncritically receiving western physical theories and propagandizing them in our countryStalin, however, chose the atomic bomb over ideology which saved their lives

Later, Markov became active in promoting disarmament

3Fluxes of cosmic neutrinos

under-groundoptical:- deep water- deep ice air showers radio acousticsKamiokande also uses neutrinos from accelerator beams (e.g. T2K)Super-Kamiokande199619971998199920002001200220032004200520062007200820092010

11146 PMTs(40% coverage)

5.0 MeV5182 PMTs(19% coverage)

7 MeV11129 PMTs(40% coverage)

5 MeVTotal energy threshold

Acrylic (front)+ FRP (back)

ElectronicsUpgradeSK-ISK-IISK-IIISK-IV~4.5 MeV < 4.0 MeV achieved goal120 collaborators, 31 institutions, 6 countries Will provide data for a long time (2025)!

supernovae, proton decay

The IceCube Observatory

1000 m1000 m1450 m80 sparsely instrumented strings 17 m vertical sensor distance 125 m horizontal string distance

6 densely instrumented strings (DeepCore) 7-10 m sensor distance 60 m horizontal string distance

5160 sensors + autonomous DAQ in iceDecember 2010: IceCube fully deployed !!!

250 collaborators, 36 institutions, 9 countries IceCube accumulated exposure

for 100 TeVThe interesting time is now !Factor 300 since 2000data available 7Complementary approaches

Imaging detector: 40% PMT coverage

precision detector: Calibration uncertainties O(%) Sparse sampling detector < 1% PMT coverage

discovery instrument: Systematic uncertainties O(10-20%)

~125 m~17 mBoth detect all neutrino species ( e ) ,but are optimized for very different energy ranges and neutrino fluxes Size comparison and energy coverage

IceCube: 1000 Mton

DeepCore: 15 MtonSuper-K: 0.05 Mton1 MeV10 MeV 100 MeV 1 GeV10 GeV 100 GeV 1 TeV 10 TeV 100 TeVIceCubeDeepCore extensionSuper-Ksolar SN proton decay atmospheric neutrinos (extra)galactic 9II. Neutrino Oscillations

10000 20000 30000 40000 km/GeVeprobability0.2 0.4 0.6 0.8 1.0frequency:mi2-mj2 E / LSchematically: e

mixing angles:12,23,13Neutrinos

propagating mass eigenstate weak interactions eigenstatesunknown CP violationonly limit 13< 10o knownwould like improved precision at the end one would like to understandwhy neutrinos mix differently than quarks Present knowledge (Lisl, Neutel2011): 12 = (33.6+1.2-1.0)o (~ 3%) 23 = (40.4+5.2-3.5)o (~ 11%) 13 < 13o m22-m12 = (7.54+0.25-0.21) x 10-5 [eV2] (~ 3%) m32-m22 = (2.36+0.12-0.10) x 10-3 [eV2] (~ 5%)

normal invertedMore specific questions that can be answered in neutrino oscillation experimentsCan we see appearance of ? ( Opera)How large is 13?Is there CP-violation in the neutrino sector?What is the neutrino hierarchy?

Low-energy solar n + e- n + e- candidatecolor: timeEe = 9.1MeVcosqsun = 0.95~ 6 hits / MeV (SK-I, III, IV)SK-III resolution 10 MeV electrons: vertex: 55 cm direction: 23o energy: 14%

Timing information: vertex position

Ring pattern: direction

Number of hit PMTs: energySK-IV up to Nov. 2010

13

Three-Flavor Analysis (including SK-I+II+III) 68, 95, 99.7% C.L. 13 = 9.1+2.9-4.7o ( < 14o at 95%C.L.), but consistent with 0 !Solar -results

arXiv:1010.0118KamLANDtan212

Solar globalKamLANDSolar+KamLANDPreliminary tan212sin213m212 [eV2]

Zenith angle distributions atmospheric sSuper-Kamiokande I+II+III, 2806 days oscillation (fit)no oscillatione-like

m-likeClear deficit !No e deficit ! determine 23 m223 limit 13, observe ?

99% C.L.90% C.L.68% C.L.best fitFull 3-flavor oscillation resultsSK-I+II+IIINormal hierarchy Super-K preliminary

0.84000.4Inverted hierarchy 3003.5x10-31.5x10-311.5x10-3No significant hierarchy differenceor constraint on CP at 90% CL !0.4030003.5x10-3SK: best constraint on 23 Minos: sharper constraint on m23

Minos 90%CL16

99% C.L.90% C.L.68% C.L.best fitFull 3-flavor oscillation results (SK I-III)0.4No significant hierarchy difference or constraint on CP at 90% CL !03000SK: best constraint on 23 Minos: sharper constraint on m23

Super-K preliminary1.5x10-33.5x10-3Minos 90%CL similar, but less constraint for inverse hierarchyNormal hierarchy 17

e or or hadronsEnergy threshold: 3.5 GeV

events at Super-KNegligible primary flux Any observed oscillation induced ! but: complicated event topologyGOAL : test the null hypothesis of no appearance

Fitted excess inconsistent with no appearance at 3.8s Exotic Oscillations (IceCube)Quantum gravity effects: Lorentz invariance violation and quantum decoherencestandard oscillations 1/Equantum gravity oscillations E (or E2)

Muon neutrino survival probabilityconventionaloscillationsDeepCoreVLI oscillations,c/c = 10-27 e.g. VLI: speed of light = f(neutrino flavor): parameters: c/c, sin 2, Phase

excludedsin 2 Log c/c-27-25III. High energy astronomy

highest energy event255000 photo-electrons!if muon bundle: E ~ 1016 eVWaxman-Bahcall limitIdea: constrain possible neutrino flux from extragalactic cosmic ray intensity neutrinos must be created in cosmic ray beam dumps

Extragalactic flux

IceCube sensitivityAssume p (and pp, pn) interaction in surrounding materialpions and kaons neutrinos Assume optically thin sourcesExtrapolate to lower energy assuming flux ~ 1/E2WB upper limit () depends on many assumptions WB: expect flux 1/5? there are also many specific models (AGN, GRB, galactic sources )IceCube sky map (50% of detector)

hottest spot post-trial value 18%

no discovery yet ! Live time 375 days, 14121 upgoing events, 22779 downgoing eventsLimits for point sources with flux 1/E2 Factor1000in 15 years !

Complementarity in dark matter searches

direct detectionindirect detectionProduction at LHC colliderDirect searches profit from coherent interaction on nucleon ( A2) telescopes profit from large detection volumespin-independent cross sectionallowed modelsspin-dependent cross sectionSensitivity direct searchesSensitivity IceCube (Super-K)e.g. Cohen, Phalen, PiercePhys. Rev. D81, 116001 (2010)

Excluded by direct detection experiments for spin-dependent interactionIceCube/Amandalimit (W+,W-)Dark matter sensitivity spin dependent Super-K (2009)Prel. limit (W+,W-) IceCube/DeepCoresensitivity (W+,W-)IceCube: sensitivity 100 x direct search experiments (sun mostly hydrogen!)Non-excluded even if SI- limits improved by 1000MSSM scanpreliminary

continuing to higher energies look for excess of , e etc on top of atmospheric neutrinosSpectrum of atmospheric 100 TeV=1014 eV study energies above O(50) TeV

Extraterrestric - diffuse fluxWaxman-Bahcall boundIceCube 40 strings: 5 excluded the Waxman-Bahcall bound has been crossed EGADS Schedule2009-10: Excavation of new underground experimental hall, construction of stainless steel test tank and PMT-supporting structure (all completed, June 2010)

2010-11: Assembly of main water filtration system (completed), tube prep, mounting of PMTs, installation of electronics and DAQ computers

2011-13: Experimental program, long-term stability assessmentAt the same time, material aging studies will be carried out in Japan, and transparency and water filtration studies will continue in the USThe goal is to be able to state conclusively whether ornot gadolinium loading of Super-Kamiokande will besafe and effective. Target date for decision = mid-201228

IV. Core collapse supernova detection Milky Way: 2 1 core collapse supernovae per century

with 3 supernovae/century, probability of observation:

25 % within 10 years45% within 20 years

Goal: get most of physics out of this precious event Relic neutrinos neighboring galaxies?Energy release E

R=1010 m star collapses via a Rcore=106 m core to a RNS =104 m neutron star E EEkin 10-2 EEem 10-4 Eindividual neutrino energy ~ E /Ndominant reaction: e+ p e+ + n

cross section: E2 (count events - SK) Cherenkov light: E3 (count s - IceCube)8.8 M progenitor O-Me-Mg core (1s after bounce) rates strongly dependent on energies

track length ~ 0.57 cm x Ee+ (MeV) N300-600nm ~ 180 x Ee+ (MeV)29

Interaction vertices in IceCubeview from aboveDark noise: ~ 540 Hz/DOM can be reduced somewhat

dominant reaction: e+ p e+ + n

cross section: E2 (events - SK) Cherenkov light: E3 (s - IceCube)

Idea: track coherent increase of total rate due to neutrinos on top of low dark noise

Effective volume: ~30 m3/MeV of e+Effective volume overlap small O(1%)30Expected rate distribution (IceCube)

Lawrence Livermore model, 10 kpc distance (~ distance to center)IceCube Monte Carlo with time dependent energy spectra incorporatednormal neutrino hierarchyinverted neutrino hierarchyTotani et al. Astrop. Phys. 496, 216 (1998)preliminarybackground levelclear differences in model shapes for normal and inverted hierarchy!31

More exotic signals to hope for quark star formation black hole formation no explosion!

normal invertedHierarchy Dasgupta et al., Phys. Rev. Lett. D 81, 103005 (2010)anti- peak!Sumiyoshi et al., ApJ 667, 382 (2007)black holeformation>40 solar mass progenitor

no oscillationsnormal hierarchy inverted hierarchy32How does IceCube compare?Due to noise background, the answer depends on the signal/noise assumption which is a function of distance, model and time within bursttake this plot with a big grain of salt !

example: comparison of initial 0.38 sLawrence Livermore model!60% milky waycoverage equivalent mass background free detector (Mton) 0.25 MtonSuper-K IceCube 1 Mton

0.1 Mton

0.01 Mtondistance [kpc] 0 10 20 30 40 50 60Super-K: 10% chance to see SN in Andromeda33Super-K and IceCube make a good team .IceCube: Mton scale detector for close supernovae study fine details of neutrino light curve

Super-K: energy, direction + some type separation low background handle for relic neutrinos

Aim for combined analyses!!discuss at workshop Talk M. Smydirectional information 25o/NThe future (Super-Kamiokande)T2K 300 km base line experiment J-PARC Super-K; first interactions 2010!Goal: test 13 down to 5x10-3 dependent on CP-phase ; reach 13 ~ 4o by mid 2011T2K 13 sensitivity1020 1021 1022Protons on target4.0o1.5oJuly 2011 goal?

Gd loading test facilityLarge n capture Gd+nG* Gd+

8 MeV total E200 ton tank 250 PMTsAdd gadolinium to water for efficient antineutrino tagging talk Michael Smy Goal: Determine by mid-2012 if Gadolinium loading will be safe and effectiveOne candidate for e appearance!

Not significant

29% probability forbackground fluctuationO0.5 GeV

0.3 backgroundevents expected Earth quake, but no Tsunami damage; Super-Kamiokande is fineProblems: Power, some outer structuresEarth quake damage at J-PARC

Dump south37 the future (IceCube)Find extra-terrestrial neutrinos!

Soon results from DeepCore extension with (10) GeV energy threshold:

bridge gap to Super-K to study atmospheric oscillations, Wimps, galactic sources

Think about even denser in-fill with O(1) GeV threshold?

Dream about future ice lab for low energy physics and proton decay?

DeepCore(IceCube veto)IceCubeSuper-K38SummarySK-IV is running with the lowest energy threshold ever! 100% efficiency at Etotal~ 4.5MeVFull 3-flavor atmospheric and solar oscillation results More stringent proton decay limitsR&D for Gadolinium in Super-K is underway (results 2012)Very efficient data taking for T2K beam

High sensitivity gradient for IceCubes analysesSensitivity has crossed Waxman-Bahcall boundComplementarity to direct dark matter searchesMton scale experiment for close supernovaeOne year of data from low energy extension DeepCoreIdeas about future extensions being gathered

39

40The Super-Kamiokande Collaboration1 Kamioka Observatory, ICRR, Univ. of Tokyo, Japan2 RCCN, ICRR, Univ. of Tokyo, Japan3 IPMU, Univ. of Tokyo, Japan4 Boston University, USA5 Brookhaven National Laboratory, USA6 University of California, Irvine, USA7 California State University, Dominguez Hills, USA8 Chonnam National University, Korea9 Duke University, USA10 Gifu University, Japan11 University of Hawaii, USA12 Kanagawa, University, Japan13 KEK, Japan14 Kobe University, Japan15 Kyoto University, Japan16 Miyagi University of Education, Japan17 STE, Nagoya University, Japan18 SUNY, Stony Brook, USA19 Niigata University, Japan20 Okayama University, Japan21 Osaka University, Japan22 Seoul National University, Korea23 Shizuoka University, Japan24 Shizuoka University of Welfare, Japan25 Sungkyunkwan University, Korea26 Tokai University, Japan27 University of Tokyo, Japan28 Tsinghua University, China29 Warsaw University, Poland30 University of Washington, USAFrom PRD81, 092004 (2010)~120 collaborators31 institutions, 6 countriesAutonomous University of Madrid, Spain (Nov.2008~)

USA:University of Alaska, AnchorageUniversity of Alabama, Tuscaloosa Bartol Research Institute, Delaware University of California, BerkeleyLawrence Berkeley National Lab.Clark-Atlanta UniversityGeorgia TechUniversity of California, IrvineLawrence Berkeley National LaboratoryUniversity of MarylandOhio State University Pennsylvania State UniversitySouthern University and A&M College, Baton RougeUniversity of Wisconsin-MadisonUniversity of Wisconsin-River FallsSweden:Stockholm UniversitetUppsala UniversitetUK: Oxford UniversityBelgium: Universit Libre de Bruxelles Vrije Universiteit Brussel Universiteit Gent Universit de MonsGermany: RWTH AachenUniversitt BochumUniversitt BonnDESY-ZeuthenUniversitt DortmundHumboldt UniversittMPI Heidelberg Universitt MainzUniversitt WuppertalJapan: Chiba UniversityNew Zealand: University of Canterbury36 institutions, ~250 members http://icecube.wisc.eduSwitzerland: EPFLIceCube CollaborationBarbados:University of the West Indies41PAS CITER TOUS LES PAYS MAUS JUSTE UW HALZENcamera at 2450 m depth

Ice and freeze-in properties in itself interesting .42General theoretical lessons on sAt least two neutrinos have (very small) massesMasses are probably small, because s are of Majorana type (masses inverse proportional to large scale of lepton number violation)Mass ~MR empirically close to 1014-1015 GeV ~ MGUTDecays of right handed neutrinos produce baryogenesis via leptogenesis0.025 m2 (normal hierarchy): m2/m3~0.2 (close to c ~ 0.22 ?)very small 13 and maximal 23 (45o) theoretically hard

Operas nutau candidate

nu tau candidate opera

44Search for p e+ + p0 SK-I+II+III+IV

proton / B > 1.21 x1034 yr SK-I-IV combined (205.7 kton/year): no candidates!Signal MCDataPreliminary should reach 2 x 10-34 by 2017 if no candidates are found

Nucleon decay limits, status 2010 Proton is stable in the standard model GUT. SUSY models allow p decay, but predict different channels and lifetimes!46limited by number of protons (SK: 7.5 x 1033) and neutrons (SK: 6.0 x 1033) background and time !! Lifetime sensitivity 2010202020303x10342x1034pe+01x1034

Phys Lett B587:105-116 (2004)Comparison with an SO(10) ModelSuper-K data are providing strong constraints to these models But need sensitivity ~ 1036 years to rule out minimal SUSY ??? 47

Expected significancedepends on detection technique as well as model and neutrino properties > 25 in Galaxy

~ 3-10 in Magellanic cloudspreliminary48