Recent Neutrino Oscillation Results and Future
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Recent Neutrino Oscillation Results and Future
Jun Cao Institute of High Energy Physics
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There are 3 famailes of massless Neutrinos in the SM.
There are 300 neutrinos/cm3 in the universe.
Neutrinos
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Neutrino oscillation means neutrinos are massive.
Neutrino Oscillation
Solar neutrinoHomestake Exp.
Atmospheric neutrinoSuper-K exp.
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MINOS in US, first in 2006Accelerator
K2K in Japan, 2004
Accelerator
KamLAND in Japan, reactor, first in 2002
SNO in Canada, solar, in 2001
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Neutrino Mixing
1 2
1 2 3
31 3
1
2
2
3
eee eU UU U UU U U
U
1 13 13
13 13
23 23
23 23
2 12
12 12
1 0 00 00
0 00 c s0 s c 0
c s 0s c 00 0 1
c 0 s0 0s 0 c 1
i
iiU eee
23 ~ 45m2
32 ~ 2.4310-3 eV2
Atmospheric Accelerator
12 ~ 34m2
32 ~ 7.610-5 eV2
SolarReactor
013 = ?CP = ?ReactorAccelerator
In a 3- framework
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Neutrino Puzzles
10 Years ago, neutrino oscillation was well established. Is 13 non-zero? Which neutrino is heavier? (mass hierarchy) Is there CP violation? How many kinds of neutrinos? (Unitarity) Are there sterile neutrinos? What's the mass of neutrinos? Is neutrino its own anti-particle? Abnormal magnetic moment? Can we detect relic neutrino from Big Bang?Also of great interests in astrophysics, cosmology, geology, etc.
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How large is 13?PRD 62, 072002
Allowed region
Fogli et al., J.Phys.Conf.Ser.203:012103 (2010)
Gonzalez-Garcia et al., JHEP1004:056, 2010
Fogli et al., hep-ph/0506307
sin2213<0.16
sin2213~0.04
sin2213~0.04
sin2213~0.08, non-zero 2
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How to measure 13
2
4 2 21
2
3 12
213 31
221
1 sin / 4
cos si
sin
n 2 sin / 4
2
e e
m
m
P L E
L E
Reactor (disappearance) Clean in physics, only related to 13 Precision measurement
213
2 2 223 31sin sin / 4
+ ( ) + (
sin 2
CPV term matter term) +
eP m L E
Accelerator (appearance) Related with CPV and matter effect
T2K
4MeV e
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Ken Sakashita, ICHEP 2012
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T2K Indication
In Jun., 2011, 6 e events, 1.50.3 bkg expected. (1.431020 POT) 13 non-zero probability 99.3% (2.5 significance)
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T2K updated in Jul. 2012
31020 POT11 e candidates3.22 expected w/o oscillation
Ken Sakashita, ICHEP 2012
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Indication from MINOS
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MINOS updated in Jul. 2012
In 2011: antineutrino differ from neutrino (98% C.L.): CPT violation?
Most precise m2 measurement
Neutrino Anti-neutrino
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Precision Measurement at Reactors
Parameter Error Near-farReaction cross section 1.9 % 0
Energy released per fission 0.6 % 0Reactor power 0.7 % ~0.1%
Number of protons 0.8 % < 0.3%Detection efficiency 1.5 % 0.2~0.6%CHOOZ Combined 2.7 % < 0.6%
Major sources of uncertainties:
Reactor related ~2% Detector related ~2% Background 1~3%
Lessons from past experience: CHOOZ: Good Gd-LS Palo Verde: Better shielding KamLAND: No fiducial cut
Near-far relative measurementMikaelyan and Sinev, hep-ex/9908047
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Proposed Reactor Experiments
Angra, Brazil
Diablo Canyon, USA
Braidwood, USA
Double Chooz, France
Krasnoyarsk, Russia KASKA, Japan
Daya Bay, China
RENO, Korea
8 proposals, most in 2003 (3 on-going)• Fundmental parameter• Gateway to -CPV and Mass Hierachy measurements• Less expensive
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The Daya Bay Experiment• 6 reactor cores, 17.4 GWth • Relative measurement
– 2 near sites, 1 far site• Multiple detector modules• Good cosmic shielding
– 250 m.w.e @ near sites– 860 m.w.e @ far site
• Redundancy
3km tunnel
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Double Chooz in FranceDaya Bay
Double Chooz
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RENO in Korea6 cores16.5 GW
16t, 450 MWE
16t, 120 MWE
Daya BayRENO
Double Chooz
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Three on-going experiments
ExperimentPowe
r(GW)
Detector(t)Near/Far
Overburden (m.w.e.) Near/Far
Sensitivity(3y,90%CL
)Daya Bay 17.4 40 / 80 250 / 860 ~ 0.008Double Chooz 8.5 8 / 8 120 / 300 ~ 0.03RENO 16.5 16 / 16 120 / 450 ~ 0.02
Huber et al. JHEP 0911:044, 2009
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Detecting Reactor Antineutrino
e nep 2e e
Delayed signal, Capture on H (2.2 MeV) or Gd (8 MeV), ~30s
Prompt signal Peak at ~4 MeV
Capture on H
Capture on Gd
Inverse beta decay
Major backgrounds: Cosmogenic neutron/isotopes
8He/9Li fast neutron
Ambient radioactivity accidental coincidence
0.1% Gd by weight
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Similar Detector Design Water Shield radioactivity and
cosmogenic neutron Cherekov detector for muon
RPC or Plastic scintillatormuon veto
Three-zone neutrino detectorTarget: Gd-loaded LS
8-20 t for neutrino-catcher: normal LS
20-30 t for energy containmentBuffer shielding: oil
40-100 t for shielding
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Similar Detector Design Water Shield radioactivity and
cosmogenic neutron Cherekov detector for muon
RPC or Plastic scintillatormuon veto
Three-zone neutrino detectorTarget: Gd-loaded LS
8-20 t for neutrino-catcher: normal LS
20-30 t for energy containmentBuffer shielding: oil
40-100 t for shielding
Daya Bay Reflective panels
PMT Coverage pe yield pe yield/CoverageDaya Bay 192 8" ~6% 163 pe/MeV 1.77RENO 354 10" ~15% 230 pe/MeV 1Double Chooz 390 10" ~16% 200 pe/MeV 0.81
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DYB:Tunnel and Underground Lab.
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Daya Bay
Assembly of Antineutrino Detector
J. Cao (IHEP) 25
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Assembly of Antineutrino Detector
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Muon System Installation
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Liquid Scintillator Hall
Daya Bay 28
LS mixing equipment
185 ton 0.1% Gd-LSLiquid Scintillator
Mineral Oil
Filling Equipment
ISO tank equiped with load cell. Target mass errorr ~0.1%
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Detector Installation
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Neutrino Selections
0.7-12 MeV 6-12 MeV
Prompt candidate Delayed candidate
Correlated Events in 1-200 sReactor Neutrinos
(Prompt)Neutrons (Delayed )
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Daya Bay Results
2011-8-15
2011-11-5
2011-12-24
Mar.8, 2012, with 55 day datasin2213=0.0920.016(stat)0.005(sys
t)5.2 σ for non-zero θ13
Jun.4, 2012, with 139 day datasin2213=0.0890.010(stat)0.005(sys
t)7.7 σ for non-zero θ13
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Side-by-side Comparison 0.2% detector-related uncertainty (relative measurement) Expected ratio of neutrino events: R(AD1/AD2) = 0.982
The ratio is not 1 because of target mass, baseline, etc. Measured ratio: 0.987 0.004(stat) 0.003(syst)
This check shows that syst. are under control, and will eventually "measure" the syst. error
Data set: 2011.9 to 2012.5
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Why systematics is so small? c.f. An et al. NIM. A 685 (2012) 78
Idea of "identical detectors" throughout the procedures of design / fabrication / assembly / filling.
For example: Inner Acrylic Vessel, designed D=31205 mm Variation of D by geometry survey=1.7mm, Var. of volume: 0.17% Target mass var. by load cell measurement during filling: 0.19%
Functional Identical Detectors
Diameter IAV1 IAV2 IAV3 IAV4 IAV5 IAV6Surveyed(mm
)3123.12 3121.71 3121.77 3119.65 3125.11 3121.56
Variation (mm)
1.3 2.0 2.3 1.8 1.5 2.3 "Same batch" of liquid scintillator
5x40 t Gd-LS, circulated
200 t LS, circulated4-m AV in pairs Assembly in pairs
20 t filling tank
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Daily Rate: Evidence of Deficit
Predictions are absolute, multiplied by a global normalization factor from the fitting.(to account for the absolute flux and absolute detection eff. uncertainty)
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Daya Bay Results (2012.6)
R = 0.944 ± 0.007 (stat) ± 0.003 (syst)sin22θ13=0.089±0.010(stat)±0.005(syst)
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Double Chooz Results
Far detector starts data taking at the beginning of 2011 First results in Nov. 2011 based on 85.6 days of data
Updated results on Jun.4, 2012, based on 228 days of data sin2213=0.0860.041(Stat)0.030(Syst), 1.7σ for non-zero θ13
sin2213=0.1090.030(Stat)0.025(Syst), 3.1σ for non-zero θ13
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Double Chooz Results (2012.6)
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RENO
Data taking started on Aug. 11, 2011 First physics results based on 228 days data taking (up to
Mar. 25, 2012) released on April 3, 2012, revised on April 8, 2012:
sin2213=0.1130.013(Stat)0.019(Syst), 4. 9σ for non-zero θ13
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RENO Results (2012.4)
R = 0.920 ± 0.009(stat) ± 0.014 (syst)sin22θ13=0.113±0.013(stat)±0.019(syst)
4.9 for non-zero value of 13
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Global PictureExclusion of non-zero 13
(2010)
2011.6
2011.7
2011.11
by S. Jetter
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Global Picture
2012.3
Exclusion of non-zero 13
by S. Jetter
(2010)
2011.6
2011.7
2011.11
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Global Picture
2012.4
2012.6 (7.7)
2012.6
2012.6
2012.6
Exclusion of non-zero 13
by S. Jetter
A consistent picture
(2010)
2011.6
2011.7
2011.11
2012.3
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Future 13 Daya Bay
Installation of remaining two detectors this summer Full data taking this fall Current precision of sin2213 12.5%, 3 year: 4-5%
RENO Continue data taking 3 year precision of sin2213 : ~10%
Double Chooz Near site detector installation underway Full data taking(by the end of) next year 3 year precision of sin2213 : ~15%
Direct measurement m231, Reactor spectrum, Reactor
anomaly, cosmogenic n/isotope yield, non-standard interaction, ...
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Next Step: Daya Bay-II Experiment
Daya Bay60 km
Daya Bay II 20 kton LS detector 3%/E resolution Rich physics
Mass hierarchy Precision measurement
of 4 oscillation parameters to <1%
Supernovae neutrino Geoneutrino Sterile neutrino Atmospheric neutrinos Exotic searches
Talk by Y.F. Wang at ICFA seminar 2008, Neutel 2011; by J. Cao at Nutel 2009, NuTurn 2012 ; Paper by L. Zhan, Y.F. Wang, J. Cao, L.J. Wen, PRD78:111103,2008; PRD79:073007,2009
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The reactors and possible sitesDaya Bay Huizhou Lufeng Yangjiang Taishan
Status Operational Planned Planned Under construction Under constructionPower 17.4 GW 17.4 GW 17.4 GW 17.4 GW 18.4 GW
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Daya BayHuizhou Lufeng
Site 2
Site 1
Yangjiang
Taishan
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30% chance to determine Mass Hierachy
T2K+NOvA
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LBNE
Approved 10 kT LAr detector on ground
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Hyper-K
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Phased Icecube Next Generation Upgrade
PINGU
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Indian Neutrino observatory: INO 50kt magnetized iron plate
interleaved by RPC for Sign sensitive atmospheric
neutrinos (stage I) long baseline neutrino beams (stage II)
Features: Far detector at magic baselines:
� CERN to INO: 7152 km� JPARC to INO: 6556 km� RAL to INO: 7653 km
Muons fully contained up to 20 GeV
Good charge resolution, B=1.5 T Good tracking/Energy/time
resolutionthree 17kt modules, each 161614.4m3
150 iron plates, each 5.6 cm thick
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2020-2022
Projected Sensitivity to MH
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Summary Daya Bay experiment discovered the new oscillation
and proved 13 is quite large. We can measure the MH and CPV in our
lifetime! Six results from 3 reactor exp., 2 accelerator exp.,
and fit from solar+KamLAND are consistent. Precision on sin2213 will be improved to 4-5% In the next 10 years, we will see data from the next
generation of neutrino oscillation experiments Mass hierarchy, maybe CPV Precision measurement of mixing parameters up
to < 1% level unitarity test of the mixing matrix
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Thanks !