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.

4

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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13

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

Thanks !