Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine...
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Transcript of Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine...
![Page 1: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/1.jpg)
Super-Kamiokande – Neutrinos from MeV to TeV
Mark Vagins
University of California, Irvine
EPS/HEP2005 - LisbonJuly 22, 2005
![Page 2: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/2.jpg)
The Collaboration
1 Kamioka Observatory, ICRR, Univ. of Tokyo, Japan2 RCCN, ICRR, Univ. of Tokyo, Japan3 Boston University, USA4 Brookhaven National Laboratory, USA5 University of California, Irvine, USA6 California State University, Dominguez Hills, USA7 Chonnam National University, Korea8 Duke University, USA9 George Mason University, USA10 Gifu University, Japan11 University of Hawaii, USA12 Indiana University, USA13 KEK, Japan14 Kobe University, Japan15 Kyoto University, Japan16 Los Alamos National Laboratory, USA17 Louisiana State University, USA
18 University of Maryland, College Park, USA19 University of Minnesota, Duluth, USA20 Miyagi University of Education, Japan21 SUNY, Stony Brook, USA22 Nagoya University, Japan23 Niigata University, Japan24 Osaka University, Japan25 Seoul National University, Korea26 Shizuoka Seika College, Japan27 Shizuoka University, Japan28 Sungkyunkwan University, Korea29 RCNS, Tohoku University, Japan30 University of Tokyo, Japan31 Tokai University, Japan32 Tokyo Institute for Technology, Japan33 Warsaw University, Poland34 University of Washington, USA
~140 collaborators 34 institutions 4 countries
(as of Jan. 2005)
+Tsinghua Univ., China(June, 2005~)
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Super-Kamiokande
The Location
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40m
41.4m
40m
41.4m
The Detector 50000 tons ultra-pure water
1 km overburden = 2700 m.w.e.
22500 tons fiducial volume
![Page 5: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/5.jpg)
SK-I: 40% PMT Coverage SK-II: 19% PMT Coverage
April 1996 July 2001 December 2002 September 2005
![Page 6: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/6.jpg)
The Neutrino Sources
Solar (Low E) Atmospheric (High E)
5 MeV 20 MeV 100 MeV 10 TeV+P = 1 – sin22sin2(1.27 )
m2L
E
![Page 7: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/7.jpg)
8B ’s
hep ’s
SK-I: 5 MeV
SK-II: 7 MeV
SK-III: 4 MeV
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12 MeVsolar
Result of -eelastic
scattering:points back
in solardirection
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603 MeVatmospheric
muon
Note sharpedge of ringfrom muon
produced by-nucleoninteraction
![Page 10: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/10.jpg)
492 MeVatmosphericelectron
Note diffuseedge of ring
from electronproduced bye-nucleoninteraction
![Page 11: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/11.jpg)
Tau candidate event (~3 GeV)
(Still Fully Contained)
![Page 12: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/12.jpg)
Upward-Going Muons
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Upward-goingatmospheric induced
muon
Note activityin outer
detector: not contained
Parent energy between 2 GeV and 40 TeV!
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Atmospheric Results
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No Oscillation(sin2223=1.0, m2
23=2.5X10-3 eV2)
1489 days of data
![Page 16: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/16.jpg)
No Oscillation(sin2223=0.98, m2
23=3.1X10-3 eV2)
627 days of data
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Solar Results
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SK-I: 8B Solar Neutrino Flux
8B flux = 2.35 0.02 0.08 [x106/cm2/s] Data / SSMBP2004 = 0.406 0.004(stat.) +0.014 -0.013 (syst.)
22400 230
solar events
PLB539 (2002) 179
Electron total energy: 5.0-20MeV
May 31, 1996 – July 15, 2001 (1496 days )
Data / SSMBP2000 = 0.465 0.005(stat.) +0.016 -0.015 (syst.)
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SK-II: 8B Solar Neutrino Flux
SK-I 8B flux = 2.35 0.02 0.08 [x106/cm2/s]
![Page 23: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/23.jpg)
Seasonal Variation: SK-I + SK-II
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SK-I Day / Night Variation
ADN=(Day-Night)
(Day+Night)/2
![Page 25: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/25.jpg)
SK-II Day / Night asymmetry
= 0.014+/-0.049(stat.) (sys.)ADN= (Day-Night)
(Day+Night)/2
SK-I D/N Asymmetry: -0.021+/-0.020+0.013- 0.012
Preliminary
+0.024- 0.025
![Page 26: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/26.jpg)
SK-I: Energy Spectrum
Energy correlated systematic error
No strong distortion seen
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SK-II: Energy Spectrum
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Oscillation parameters from solar neutrino and KamLAND experiments (SK-I data only)
Solar 95%
99.73% KamLAND
Solar+KamLAND
12
12
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Ongoing Work:
• ATM MaVaN Analysis for SK-I/II• ATM L/E Analysis for SK-II• Solar SK-II Oscillation Analysis• Three Flavor Analyses • Improved Relic Supernova Neutrino Analysis• Tau Appearance Paper (soon!)• Full SK-I Solar Paper (very soon!) • Gadolinium Enrichment Studies for SK-III• Many others…
Next Up:
• Drain Super-Kamiokande-II and Restore 40% PMT Coverage• Resume Data-Taking with SK-III by June 2006
Beacom & Vagins,
PRL93 (2004)171101
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L/E Analysis
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L/E Analysis Motivation
E
Path length
L
Neutrino energy
Use only high resolution L/E events
A first dip can be observed
P = (cos2sin2x exp(– ))2m2
Neutrino oscillation :
P = 1 – sin22sin2(1.27 )
m2LE
Neutrino decoherence :
P = 1 – sin22 x (1 – exp(–))
21
Neutrino decay :
LELE
![Page 33: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/33.jpg)
L/E Distribution
Null oscillation MC
Best-ft expectation
1489.2 days FC+PC
First dip is seen as expected by neutrino oscillation
Best fit expectation w/ systematic errors
![Page 34: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/34.jpg)
Test for neutrino decay & neutrino decoherence
Oscillation
Decay
Decoherence
2min=37.9/40 d.o.f
2min=49.1/40 d.o.f 2 =11.3
2min=52.4/40 d.o.f 2 =14.5
2 =11.4 for decay
3.4
2 =14.6 for decoherence
3.8
The first dip the data cannot be explained by other models
![Page 35: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/35.jpg)
Comparison of the allowed parameter regionsbetween zenith angle analysis and L/E analysis
L/E analysis
Zenith angle analysis
K2K
Soudan 2
MACRO
90% allowed regions
![Page 36: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/36.jpg)
Mass Varying Neutrinos (MaVaN)
![Page 37: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/37.jpg)
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Tau Appearance
![Page 39: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/39.jpg)
Result: a = 1.82 ± .61b = 0.96
Expected #:35.2 fitted #:64 ± 21 Signal Eff: 44%Total number of tau = 145(total exp’d =79)
Partially Polarized Distribution
Likelihood Analysis
![Page 40: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/40.jpg)
GADZOOKS!
![Page 41: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/41.jpg)
Here’s what the coincident signals in Super-K with GdCl3 will look like (energy resolution is applied):
![Page 42: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/42.jpg)
Oh, and as long as we’re collecting e’s…
GADZOOKS!
GADZOOKS! will collect this much reactor neutrino data in two weeks.
KamLAND’s first 22
months of data
Hyper-K with GdCl3 will collect six KamLAND years of data in one day!
![Page 43: Super-Kamiokande – Neutrinos from MeV to TeV Mark Vagins University of California, Irvine EPS/HEP2005 - Lisbon July 22, 2005.](https://reader033.fdocuments.in/reader033/viewer/2022051619/56649ddf5503460f94ad88f3/html5/thumbnails/43.jpg)
This summer I’ll employ some excellent large-scale hardware to find out if the GdCl3 technique will work:
K2K’s 1 kiloton tank will be used for “real world” studies of
• Gd Water Filtering – UCI built and maintains this water system • Gd Light Attenuation – using real 20” PMTs• Gd Materials Effects – many similar detector elements as in Super-K
We are nearly ready for this effort…