Solar neutrino results from Super-Kamiokande Satoru Yamada for the Super-Kamiokande collaboration Institute of cosmic ray research, University of Tokyo.

Slides:



Advertisements
Similar presentations
Recent Results from Super-Kamiokande on Atmospheric Neutrino Measurements Choji Saji ICRR,Univ. of Tokyo for the Super-Kamiokande collaboration ICHEP 2004,
Advertisements

Solar Neutrinos in Super-Kamiokande July
11-September-2005 C2CR2005, Prague 1 Super-Kamiokande Atmospheric Neutrino Results Kimihiro Okumura ICRR Univ. of Tokyo ( 11-September-2005.
Takaaki Kajita ICRR, Univ. of Tokyo Nufact05, Frascati, June 2005.
Super-Kamiokande Introduction Contained events and upward muons Updated results Oscillation analysis with a 3D flux Multi-ring events  0 /  ratio 3 decay.
G. Sullivan - Princeton - Mar 2002 What Have We Learned from Super-K? –Before Super-K –SK-I ( ) Atmospheric Solar –SNO & SK-I Active solar –SK.
Prospects for 7 Be Solar Neutrino Detection with KamLAND Stanford University Department of Physics Kazumi Ishii.
Recent Electroweak Results from the Tevatron Weak Interactions and Neutrinos Workshop Delphi, Greece, 6-11 June, 2005 Dhiman Chakraborty Northern Illinois.
M. Kowalski Search for Neutrino-Induced Cascades in AMANDA II Marek Kowalski DESY-Zeuthen Workshop on Ultra High Energy Neutrino Telescopes Chiba,
A Search for Point Sources of High Energy Neutrinos with AMANDA-B10 Scott Young, for the AMANDA collaboration UC-Irvine PhD Thesis:
21-25 January 2002 WIN 2002 Colin Okada, LBNL for the SNO Collaboration What Else Can SNO Do? Muons and Atmospheric Neutrinos Supernovae Anti-Neutrinos.
1 CC analysis update New analysis of SK atm. data –Somewhat lower best-fit value of  m 2 –Implications for CC analysis – 5 year plan plots revisited Effect.
Results and Prospects for SNO
New results from K2K Makoto Yoshida (IPNS, KEK) for the K2K collaboration NuFACT02, July 4, 2002 London, UK.
Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP Lisbon July 22, 2005.
Atmospheric Neutrino Oscillations in Soudan 2
Shoei NAKAYAMA (ICRR) for Super-Kamiokande Collaboration December 9, RCCN International Workshop Effect of solar terms to  23 determination in.
1 Super-Kamiokande atmospheric neutrinos Results from SK-I atmospheric neutrino analysis including treatment of systematic errors Sensitivity study based.
H.Sekiya, Jul 30 th 2008, Philadelphia, ICHEP2008 Recent Results from Super-Kamiokande Hiroyuki Sekiya ICRR, University of Tokyo on behalf of the Super-Kamiokande.
Coincidence analysis in ANTARES: Potassium-40 and muons  Brief overview of ANTARES experiment  Potassium-40 calibration technique  Adjacent floor coincidences.
Solar neutrino measurement at Super Kamiokande ICHEP'04 ICRR K.Ishihara for SK collaboration Super Kamiokande detector Result from SK-I Status of SK-II.
14/02/2007 Paolo Walter Cattaneo 1 1.Trigger analysis 2.Muon rate 3.Q distribution 4.Baseline 5.Pulse shape 6.Z measurement 7.Att measurement OUTLINE.
Recent results from the K2K experiment Yoshinari Hayato (KEK/IPNS) for the K2K collaboration Introduction Summary of the results in 2001 Overview of the.
Michael Smy UC Irvine Solar and Atmospheric Neutrinos 8 th International Workshop on Neutrino Factories, Superbeams & Betabeams Irvine, California, August.
The Earth Matter Effect in the T2KK Experiment Ken-ichi Senda Grad. Univ. for Adv. Studies.
Methods and problems in low energy neutrino experiments (solar, reactors, geo-) I G. Ranucci ISAPP 2011 International School on Astroparticle physics THE.
Solar Neutrino Experiments A Review The CAP'09 Congress Moncton, 7-10 June, 2009 Alain Bellerive On behalf of the SNO Collaboration Carleton University,
Dec. 13, 2001Yoshihisa OBAYASHI, Neutrino and Anti-Neutrino Cross Sections and CP Phase Measurement Yoshihisa OBAYASHI (KEK-IPNS) NuInt01,
Bruno Pontecorvo Pontecorvo Prize is very special for us: All the important works done by Super- Kamiokande point back to Bruno Pontecorvo – 1957 First.
Results from Super-Kamiokande Inside of SK detector (April 2006) Super-Kamiokande detector Atmospheric neutrino results Solar neutrino results Yasuo Takeuchi.
TAUP Searches for nucleon decay and n-n oscillation in Super-Kamiokande Jun Kameda (ICRR, Univ. of Tokyo) for Super-Kamiokande collaboration Sep.
1 DISCOVERY OF ATMOSPHERIC MUON NEUTRINO OSCILLATIONS Prologue First Hint in Kamiokande Second Hint in Kamiokande Evidence found in Super-Kamiokande Nov-12.
GADZOOKS! project at Super-Kamiokande M.Ikeda (Kamioka ICRR, U.of Tokyo) for Super-K collaboration 1 Contents GADZOOKS! project Supernova.
SNO and the new SNOLAB SNO: Heavy Water Phase Complete Status of SNOLAB Future experiments at SNOLAB: (Dark Matter, Double beta, Solar, geo-, supernova.
Study of solar neutrino energy spectrum above 4.5 MeV in Super-Kamiokande-I 1, Solar Neutrino Oscillation 2, Super-Kamiokande detector 3, Data set for.
New Results from the Salt Phase of SNO Kathryn Miknaitis Center for Experimental Nuclear Physics and Astrophysics, Univ. of Washington For the Sudbury.
Study of neutrino oscillations with ANTARES J. Brunner.
Study of neutrino oscillations with ANTARES J. Brunner.
J. Goodman – January 03 The Solution to the Solar Problem Jordan A. Goodman University of Maryland January 2003 Solar Neutrinos MSW Oscillations Super-K.
Data Processing for the Sudbury Neutrino Observatory Aksel Hallin Queen’s, October 2006.
Results from RENO Soo-Bong Kim (KNRC, Seoul National University) “17 th Lomosonov Conference on Elementary Particle Physics” Moscow. Russia, Aug ,
Search for Sterile Neutrino Oscillations with MiniBooNE
N eutrino O scillation W orkshop Conca Specchiulla, September 11 th 2006 Michael Smy UC Irvine Low Energy Challenges in SK-III.
Neutrino Oscillations at Super-Kamiokande Soo-Bong Kim (Seoul National University)
Medium baseline neutrino oscillation searches Andrew Bazarko, Princeton University Les Houches, 20 June 2001 LSND: MeVdecay at rest MeVdecay in flight.
Accelerator-based Long-Baseline Neutrino Oscillation Experiments Kam-Biu Luk University of California, Berkeley and Lawrence Berkeley National Laboratory.
Recent Results from Super-K Kate Scholberg, Duke University June 7, 2005 Delphi, Greece.
T2K Status Report. The Accelerator Complex a Beamline Performance 3 First T2K run completed January to June x protons accumulated.
CP phase and mass hierarchy Ken-ichi Senda Graduate University for Advanced Studies (SOKENDAI) &KEK This talk is based on K. Hagiwara, N. Okamura, KS PLB.
April 26, McGrew 1 Goals of the Near Detector Complex at T2K Clark McGrew Stony Brook University Road Map The Requirements The Technique.
Recent Results from RENO NUFACT2014 August. 25 to 30, 2014, Glasgow, Scotland, U.K. Hyunkwan Seo on behalf of the RENO Collaboration Seoul National University.
Solar Neutrino Results from SNO
Supernova Relic Neutrinos (SRN) are a diffuse neutrino signal from all past supernovae that has never been detected. Motivation SRN measurement enables.
September 10, 2002M. Fechner1 Energy reconstruction in quasi elastic events unfolding physics and detector effects M. Fechner, Ecole Normale Supérieure.
APS/JPS Joint Meeting Kapalua, Maui, September 2005 Michael Smy UC Irvine Relic Neutrino Detection in Large Water Cherenkov Detectors.
Jul. 24, 2010Yoshihisa OBAYASHI, Atmospheric Neutrino from SuperK2  Imaging Water Cherenkov detector  50kt Pure Water  32kt Inner Detector viewed by.
5th June 2003, NuFact03 Kengo Nakamura1 Solar neutrino results, KamLAND & prospects Solar Neutrino History Solar.
Review of experimental results on atmospheric neutrinos Introduction Super-Kamiokande MACRO Soudan 2 Summary Univ. of Tokyo, Kamioka Observatory.
News from the Sudbury Neutrino Observatory Simon JM Peeters July 2007 o SNO overview o Results phases I & II o hep neutrinos and DSNB o Update on the III.
Neutrino Interaction measurement in K2K experiment (1kton water Cherenkov detector) Jun Kameda(ICRR) for K2K collaboration RCCN international workshop.
Observation Gamma rays from neutral current quasi-elastic in the T2K experiment Huang Kunxian for half of T2K collaboration Mar. 24, Univ.
Double Chooz Experiment Status Jelena Maricic, Drexel University (for the Double Chooz Collaboration) September, 27 th, SNAC11.
30th International Cosmic Ray Conference in Merida, Mexico Michael Smy UC Irvine Low Energy Event Reconstruction and Selection in Super-Kamiokande-III.
The XXII International Conference on Neutrino Physics and Astrophysics in Santa Fe, New Mexico, June 13-19, 2006 The T2K 2KM Water Cherenkov Detector M.
Preliminary T2K beam simulation using the G4 2km detector
L/E analysis of the atmospheric neutrino data from Super-Kamiokande
Physics with the ICARUS T1800 detector
p0 life time analysis: general method, updates and preliminary result
Impact of neutrino interaction uncertainties in T2K
Davide Franco for the Borexino Collaboration Milano University & INFN
Presentation transcript:

Solar neutrino results from Super-Kamiokande Satoru Yamada for the Super-Kamiokande collaboration Institute of cosmic ray research, University of Tokyo

Super Kamiokande detector - 50 kton water Cherenkov detector at 1000m underground (2700 w.e.) - 32kton inner detector: PMTs (20inch) - Fiducial volume : 22.5kton (2m from the wall) - Outer detector : 1885 PMTs (8inch) for cosmic ray muon veto 1, SK solar neutrino measurement Inner detector outer detector Water and air purification system 1000m Front-end Electronics huts electron linear accelerator for energy calib.

Super Kamiokande experiment SK-I (11146 ID PMTs) SK-II (5182 ID PMTs) SK-III (11129 ID PMTs) SK-IV (11129 ID PMTs) 1996 started on April 1998 Observed atmospheric neutrino oscillation K2K experiment 2001 Solved solar neutrino problem together with the SNO CC result Upgrade of front-end electronics and DAQ system T2K experiment - Solar neutrino measurement - Search for neutrino from supernova - Atmospheric neutrino oscillation - Neutrino from accelerator - Proton decay search - Indirect WIMP search accident Restore full coverage Frontend upgrade 1/18 Physics

ν + e - -> ν + e - (elastic scattering) ©Scientific American - High statistics for 8 B neutrino (~15evnts/day for E e > 5MeV ) - good angular resolution Solar Neutrino measurement at Super-K Goal: - Precise measurement of the solar neutrino parameters (flux, timing variation, oscillation parameters etc) - Reduce the b.g. level and measure the upturn in the solar neutrino spectrum. Measure Cherenkov ring pattern from recoiled electron Timing information -> Vertex of interaction Hit pattern -> Direction # of hit PMTs -> Energy

2, Recent SK solar neutrino analysis (SK-III phase) SK-III period: 2006/8/5-2008/8/18 (live time : 548 days, E≥6.5 MeV, 289 days, E< 6.5MeV) 2006/8/5-2007/1/24 : livetime days 2007/1/ /4/17 livetime days (RR sample  210.7day ) 2008/4/ /8/18 : livetime 94.8 days (RR sample 87.5day )  RR sample : Radon Reduced sample for which high background rate periods are rejected from the normal run Reduce Low energy BG ~70% Improved Systematics ~50% Data set Improvements in SK-III solar v analysis

Improvement of water circulation and purification system 12t/h 36t/h 60t/h 12t/h 35t/h stagnation of water 2, Optimized water flow in the tank 1, Improved water quality Doubled circulation rate Increased purification power Circulation 60t/h 32t/h 28t/h Increased RO 2-1, Reduction of background → Lower Rn concentration in fiducial volume

Vertex distribution of final sample Fiducial volume of each energy region is shown as red box: 12.3kt (4.5-5MeV), 13.3kt(5-5.5MeV), and 22.5kt(5.5-20MeV) Event/day/grid With upgrade of water system, water with higher radioactivity stays near bottom region. -> by applying tighter fiducial volume cut, low b.g. rate can be achieved for MeV region

Comparison of background rate between SK-I and III In lower energy region with tighter fiducial volume cut, SK-III has a lower b.g. rate due to lower radon concentration in water around the central region of the detector. Solar angular distribution for each energy range.

New cut for low energy events Background events coming from radioactive sources in FRP cover of PMTs or wall have small clusters in space and timing distribution, when compared with neutrino events near the wall. Cluster(space)Cluster(timing) -> Use variables related with cluster size for b.g. reduction.

Background 8 B neutrino MC cut Cluster size (cm) Hits in 20ns/ total # of hits after correction New cut for low energy events(cont ’ d) Horizontal axis : Cluster size * concentration in timing distribution

Timing Calibration improvement Before After Z [m] R 2 <150m 2 Z> -7.5m (8.9kt) R 2 <180m 2 Z> -7.5m (13.3kt) R 2 [m 2 ] After x (cm) z (cm) 10cm Before rr R (192days) 5-20 MeV Improve systematics (vertex shift) Reduce low energy BG New hit timing correction is installed. Electronics linearity is corrected by this correction Z R SK detector , Improved systematics Laser pulse width 4ns -> 0.2ns

Angular reconstruction in tank Energy [MeV] SK-I angular res.(MC) SK-III LINAC with New Fitter SK-III LINAC with Old Fitter Degree Improving direction fitter Made likelihood functions for different energy bins from MC Calibration&MC tuning: black sheet reflectivity Data /MC cos  PMT Q(reflected light)/Q(direct light) e-e-  PMT Photon Path Updated in ±1%

MC improvement fig_4.eps Top-bottom asym.(TBA) parameter is newly installed in SK-III MC’s water transparency parameters DATA MC w/ TBA MC w/o TBA water parameters are carefully tuned MC hit timing distribution of LINAC is perfectly matched to DATA Barrel topbottom Red: with TBA Black: w/o TBA(uniform)

Energy scale fig_5.eps Difference between MC and DATA is within +/- 0.5% Volume average Electron beam energy [MeV]

Table of systematic uncertainties 15 SK-III (Preliminary) SK-I Energy scale+/-1.4 +/-1.6 Energy resolution+/-0.2 8B spectrum shape+/ /-1.0 Trigger efficiency+/ /-0.3 Vertex shift+/-0.54+/-1.3 Reduction+/ /-1.6 Small cluster hits cut+/-0.5 Spallation cut+/-0.2 External event cut+/-0.25+/-0.5 Background shape+/-0.1 Angular resolution+/ /-1.2 Signal extraction method +/-0.7 Cross section+/-0.5 Live time calculation+/-0.1 Total+/ /-3.2% Due to Improvement of detector MC, reconstruction tools and calibration, systematic errors were reduced from +3.5/-3.2%(SK-I) To +-2.1%(SK-III). -> ~60% Timing calibration Improvement of reduction tools and MC Improvement Direction fitter

3, Solar neutrino results i n SK-III SK-I : black bars and points SK-III : color bars For lower energy region, SK-III has lower b.g. level than SK-I. Reduction step

Solar neutrino flux for E=5-20MeV SK-I:2.38+/-0.02(sta.)+/-0.08(sys.) ×10 6 cm -2 s -1 SK-II:2.41+/-0.05(sta.)+/-0.16(sys.) ×10 6 cm -2 s -1 (re-fitted by Winter06 spectrum) SK-III result is Consistent with SK-I and II. Systematic error is reduced.

Angular distribution for E= MeV Solar neutrino in this energy region was measured with 4σ significance. RED: best fit curve Blue: back ground 232. ±59. event 2.14 + (stat.) ×10 6 cm -2 sec -1 For MeV region,

8 B Energy spectrum of SK-III data Consistent with SK-I result No distortion 4.5MeV (total energy) 4.0MeV(kinetic energy)

Day/Night flux SK-I: A DN = -1.8±1.6 % SK-II: A DN = -3.6±3.5±3.7% SK-III: A DN = -4.1 ±1.3% combined: ADN=-2.3±1.3%(stat) sys : under study Δm 2 = 6.0x10 -5 eV 2 tan 2 θ= 0.44 (Solar best fit parameter)

Seasonal variation the eccentricity correction is not applied. SK-I,II,III χ 2 = 3.6 (only stat) With dof = 7 Probability 89% Consistent with the eccentricity of the orbit

2-flavor SK-I/II/III with flux constraint 22 4, Oscillation results SK-I 1496 days, spectrum MeV + D/N : E ≥ 5.0MeV SK-II 791 days, spectrum MeV + D/N : E ≥ 7.5MeV SK-III 548 days, spectrum MeV + D/N : E ≥ 5.0MeV B8 rate is constrained by SNO(NCD+LETA) NC flux = (5.14+/-0.21) 10 6 cm -2 s -1 Hep is constrained by SSM flux with uncertainty(16%) Only LMA (i.e. LOW excluded) Best fit value (preliminary) Δm 2 = 6.1×10-5 eV 2 tan 2 θ = 0.48 Φ B8 = 5.2×10 6 cm -2 s -1 SK-I/IISK-I/II/III 95% C.L.

Global oscillation analysis Data set SK-I/II/III SNO : CC flux(Phase-I & II & III) NC flux(Phase-III & LETA combined) ( = (5.14+/-0.21) 10 6 cm −2 s −1 ) Day/Night asymmetry(Phase-I & II) Radiochemical : Cl, Ga New Ga rate: SNU (All Ga global) (Phys.Rev.C80:015807,2009.) Cl rate: 2.56+/-0.23 (Astrophys. J. 496 (1998) 505) Borexino 7 Be rate: 48 +/- 4 cpd/100tons (PRL 101: , 2008) KamLAND : 2008

95% C.L. Best fit value (preliminary) Solar global Solar+KamLAND 24 2-flavor global analysis Solar global Δm 2 = 6.2×10 -5 eV 2 tan 2 θ = 0.48 Φ B8 = 5.3±0.2×10 6 cm -2 s -1 Solar global + KamLAND Δm 2 = 7.6×10 -5 eV 2 tan 2 θ = 0.3 Φ B8 = 5.1±0.1×10 6 cm -2 s -1

3-flavor global analysis: θ 12 - Δm , 95, 99.7% C.L. Solar global KamLAND Solar+KamLAND 25 Solar global Δm 2 = 6.2×10 -5 eV 2 sin 2 θ 12 = 0.31 sin 2 θ 13 = Φ B8 = 5.3±0.2×10 6 cm -2 s -1 Best fit value (preliminary) Solar global+KamLAND Δm 2 = 7.7×10 -5 eV 2 sin 2 θ 12 = 0.31 sin 2 θ 13 = Φ B8 = ×10 6 cm -2 s Free parameters : θ 12,θ 13,Δm 12

68, 95, 99.7% C.L. Solar global KamLAND Solar+KamLAND 3-flavor global analysis: θ 12 - θ 13 Solar global sin 2 θ 13 < C.L. Solar global + KamLAND sin 2 θ 13 < C.L.

1, SK-IV Electronics and DAQ system were updated at the beginning of SK-IV phase) Improvements of front-end electronics 5 times wider dynamic range for charge measurement (>2000pC) 5 times wider dynamic range for charge measurement (>2000pC) Larger amount of data can be sent to Online system via 100Base/T Ethernet Larger amount of data can be sent to Online system via 100Base/T Ethernet Low power consumption ( < 1W/ch ) Low power consumption ( < 1W/ch ) 5, SK-IV status 2,Fine water temperature control for inlet water -> Lower radon concentration in fiducial volume SK-I/II/III DAQ system SK-IV system All the hit data is sent to the online system and event building is done by software -> capable of lower energy threshold Hardware trigger was used. Only Triggered hit data was sent to online system. Improvements of online-DAQ system

Background level in SK-IV Same level of b.g. level as SK-III have been achieved in SK-IV phase. SK3SK4 SK MeV MeV

6, Summary - Results of solar measurement in SK-III phase have been reported. - There are improvements for b.g. level and systematic uncertainty in SK-III data analysis due to -- Water system modification -- Improvement of reconstruction tools -- Precise calibration and upgrade of detector simulation - Solar flux, energy spectrum and oscillation results are upgraded including SK-III data - Measurement in SK-IV phase is on-going, after upgrading front-end electronics and DAQ system.

Definition of SK  2 oscillated/unoscillated of 8 B ( hep ) flux Stat.+Energy-uncorrelated sys ,  andδs are chosen to minimize the spectrum fit  2. Spectrum fit Time variation Energy correlated sys. B 8 rate is constrained by SNO NC flux hep rate is constrained by SSM flux and uncertainty.

Select period with stable event rate 07 Jan. 07.Jan. 08. Sep.

M. Ikeda, phD thesis 8 B flux comparison Theory experiment

Contribution of SK-III result Δm 2 [×10 -5 ev 2 ] tan 2  Δχ 2 95% C.L. tan 2  =0.44 Δm2 = 6.0×10 -5 eV 2

Definition of  2 s for global analysis Ga/Cl Ga/Cl/Borexino ,  andδs are chosen to minimize (SK spectrum+SNO flux fit)  2. SK spectrum+SNO flux fit SK Time variation SNO CC flux Day/Night asymmetry

1D plot – this time analysis sin 2  13  2 95%C.L. solar global : sin 2  13 <0.060 KamLAND : sin 2  13 <0.075 solar global+KamLAND : sin 2  13 < sin 2   = f_7.ps preliminary

Sensitivity calculation Ratio (data/ssm)    = 1 : expected curve  = 0 : flat  SK-IV, 5years, cor-E is same as SK-I 13.3kton ( 5.5MeV), (sin 2 ,  m 2 ) = (0.30,7.9x10 -5 ) E (MeV) 29

Sensitivity of the upturn measurement Year Sigma level for up-turn (1)Enlarge fiducial volume to 22.5kton with low B.G. (2)Half energy correlated systematic error as SK-1. The black line shows the 13.3kton ( 5.5MeV) fiducial volume with the same energy correlated error as SK-1 (1) and (2) (1) (2) In the case of (sin 2 ,  m 2 ) = (0.30,7.9x10 -5 ) First target : 2 sigma level up-tern discovery for 3 years observation. (or exclude the up-tern) First target : 2 sigma level up-tern discovery for 3 years observation. (or exclude the up-tern) Need to enlarge fiducial volume with low BG as large as possible Need to enlarge fiducial volume with low BG as large as possible Also the reduction of the energy correlated systematic error is important. Also the reduction of the energy correlated systematic error is important. 30

Oscillation parameter dependence Year The correlated error is half as SK kton ( 5.5MeV) Solar KamLAND 31

Flux measurement in SK Solar KamLAND BS05(GS98) BS05(AGS98) 8 B flux from SK-I (10 6 /cm 2 /sec) If theta12 is determined, the precise 8 B flux measurement in SK may be possible to contribute the improvement of the Solar Model. (SK-I error is applied)