Takaaki Kajita Takaaki Kajita ICRR and IPMU, Univ. of Tokyo - - PowerPoint PPT Presentation

Takaaki Kajita Takaaki Kajita ICRR and IPMU, Univ. of Tokyo

Introduction Introduction

• It is already more than 10 years since we knew neutrinos have

masses.

• Since then, all the tests suggested that the dominant oscillation

channel observed in atmospheric and long baseline experiments is   experiments is .

• Small but finite neutrino masses are believed to be related to

the physics at the very high energy scale and the early Universe.

• Present:

 Precise measurements of m23

2 and sin2223

(J.Valle)

• Near future:

 Measurement of 13 N t l

3 e  

13

• Next goals

 CP violation and mass hierarchy

3

2

• r
• r
• r

hierarchy.

2 1

Outline Outline

• Introduction (Done)
• Measurements of m

2 and sin22

• Measurements of m23

2 and sin2223

 Atmospheric neutrino experiments  LBL experiments

• 13

13

 status of 13 search  Future possibilities with atmospheric ’s  Future possibilities with atmospheric  s  Near future LBL 13 experiments d  ( h )

• Beyond 13 (short)
• Summary

Many thanks to many people, especially; A.Habig, M.Messier, N.Mondal, R.Wendel, C.Ishihara, F.Dufour, K.Okumura, A.Ichikawa, J.Maricic

Measurements of Measurements of m23

2 and sin2223 23 23

Atmospheric neutrino experiments Atmospheric neutrino experiments

Frejus (700 ) Kamiokande (1000 ) There are many experiments that contributed to the atmospheric neutrino studies. NUSEX (700ton) (1000ton) IMB (3300ton) (130ton)

Soudan‐2 Soudan 2 (1kton)

R lt f S K

MACRO

Results from Super‐K are discussed, due to the dominant

MINOS

Super‐K (22.5kton) statistics. Super‐K‐I+II+III: 173 kton・yr

MINOS (5.4kton)

y

Super‐K‐III data included to the final physics analysis for the first time.

Atmospheric neutrino data from Super Atmospheric neutrino data from Super‐K

R Wendell July 4

e‐like

‐like

R.Wendell, July 4

Super‐K‐I+II+III (2806 days (173kton・yr) for FC+PC, 3109 days for up‐) 

gy energ

＋ DATA ＋ DATA ― MC (no osc.) ― MC (best‐fit)

L/E distribution update with SK L/E distribution update with SK‐I+II+III I+II+III

Preliminary

Neutrino decay (4.4) Neutrino decoherence (5.4)

Long baseline experiments Long baseline experiments

NO A T2K

(2009 ‐)

CNGS

(running)

NOvA

(~2013‐)

K2K MINOS

(running) Next talk…

K2K

(finished) (running)

The MINOS experiment The MINOS experiment

A Habig July 2 A,Habig, July 2

735km

5 4 kton MINOS far detector 1 kton near detector

735km

Monte Carlo

5.4 kton MINOS far detector 1 kton near detector

Unoscillated Oscillated Oscillated

NuMI beam line

MuMI MuMI beam history beam history

A,Habig, July 2

MINOS MINOS  result result

A.Habig (MINOS collab.) July 2 g y PRL 101, 131802 (2008)

848 CC  candidates  1065±60(syst) no‐osc. prediction With oscillation fit

Decay and decoherence models are disfavored at 3.7 and 5.7, resp.

Clear energy dependent  deficit. Completely consistent with .

P( P( ) and ) and P( P( ) identical? ) identical?

A.Habig, July 2 g, y

MINOS is the first LBL experiment that can separate  and anti‐ interactions. 6.4% of CC interactions in the Far detector are anti‐. 82% efficiency, 97% purity 82% efficiency, 97% purity “ Best fit” region region

 Dedicaed ani‐neutrino running starting in September!

13

 13

13 global fit

global fit

arXiv:0808.2016 arXiv:0806.2649

◆SNO and KamLAND slight tension. ◆CHOOZ: dominant contribution. Still not clear…. Any further hint from newer Any further hint from newer atmospheric and LBL data ?

MINOS MINOS e appearance search appearance search

M Sanchez (MINOS) Fermilab seminar Feb 2009 M.Sanchez (MINOS), Fermilab seminar Feb. 2009 A.Habig, TAUP2009

35 e candidate events are selected at the Far detector. Expected background: 27±5(stat)±2(syst) (1.5 )

“signal “

 

G.L.Fogli et al, arxiv:0905.3549 Also; A. Palazzo, July 2

Interesting data! Can atmospheric neutrinos help?

Search for non Search for non‐zero zero 13

13 in atmospheric neutrinos

in atmospheric neutrinos

0.1 0.2 0.3 0.4 0.5

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1 10

Eν (GeV) cosΘν Δm2=0.002eV2, sin2θ23=0.5, sin2θ13=0.05

P(νe → νµ)

) (

e

P    

Super‐K‐I+II+III data

0.1 0.2 0.3 0.4 0.5

• 1
• 0.9
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1 10

Eν (GeV) cosΘν Δm2=0.002eV2, sin2θ23=0.5, sin2θ13=0.05

P(νe → νµ)

0.1 0.2 0.3 0.4 0.5

• 1
• 0.9
• 0.8
• 0.7
• 0.6
• 0.5
• 0.4
• 0.3
• 0.2
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1 10

Eν (GeV) cosΘν Δm2=0.002eV2, sin2θ23=0.5, sin2θ13=0.05

P(νe → νµ)

cos

0.1 0.2 0.3 0.4 0.5

• 1
• 0.9
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• 0.7
• 0.6
• 0.5
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• 0.3
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1 10

Eν (GeV) cosΘν Δm2=0.002eV2, sin2θ23=0.5, sin2θ13=0.05

P(νe → νµ)

1‐ring

0.1 0.2 0.3 0.4 0.5

• 1
• 0.9
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• 0.7
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1 10

Eν (GeV) cosΘν Δm2=0.002eV2, sin2θ23=0.5, sin2θ13=0.05

P(νe → νµ)

E(GeV) (Normal hierarchy and m12

2=0 assumed)

 Electron appearance in the multi‐GeV upward going events. No evidence for electron appearance…

Allowed Allowed 13

13 region from SK atmospheric

region from SK atmospheric

Normal

CHOOZ limit Preliminary 68, 90, 99%CL CHOOZ li it

Inverted

CHOOZ limit

No evidence for non‐zero 13 with an analysis that assumes m12

2=0.

Future Future 13

13 analysis of the atmospheric neutrino data

analysis of the atmospheric neutrino data

◆Super‐K‐I+II+III searched for finite 13 based on the 1 mass scale dominance. ◆No evidence for finite 13 have been found. ◆However, the solar term effects are relevant in atmospheric neutrino exp’s.

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10

• 1

1 10 0.5 0.6 0.7 0.8 0.9 1 1.1 1.2 1.3 1.4 1.5 Eν (GeV) cosΘν

Ψ(νe)/Ψ0(νe)

sin2θ23=0.5, sin2θ13=0.04, solar on

, p p ◆Furthermore, the analyses in arXiv:0806.2649 and others indicate the potential importance of the full 3 flavor analysis.

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10

• 1

1 10 0.5 0.6 0.7 0.8 0.9 1 1.1 1.2 1.3 1.4 1.5 Eν (GeV) cosΘν

Ψ(νe)/Ψ0(νe)

sin2θ23=0.5, sin2θ13=0.04, solar on

s223=0.4 s213=0.04  =/4 Solar term

0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18 50 100 150 200 250 300 350 CP phase sin2θ13 0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18 50 100 150 200 250 300 350 CP phase sin2θ13

Sensitivity Sorry, only SK 80 years sensitivity …

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• 1

1 10 0.5 0.6 0.7 0.8 0.9 1 1.1 1.2 1.3 1.4 1.5 Eν (GeV) cosΘν

Ψ(νe)/Ψ0(νe)

sin2θ23=0.5, sin2θ13=0.04, solar on

cp /4 Effect f  Interference

0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18 50 100 150 200 250 300 350 CP phase sin2θ13 0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18 50 100 150 200 250 300 350 CP phase sin2θ13

90%CL 99%CL nith) sin213=0.04 sin213=0.02

sin213

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10

• 1

1 10 0.5 0.6 0.7 0.8 0.9 1 1.1 1.2 1.3 1.4 1.5 Eν (GeV) cosΘν

Ψ(νe)/Ψ0(νe)

sin2θ23=0.5, sin2θ13=0.04, solar on

• f 13

Interference (CP)

0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18 50 100 150 200 250 300 350 CP phase sin2θ13 0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18 50 100 150 200 250 300 350 CP phase sin2θ13

90%CL 99%CL cos(zen Test ( 13) point 0.1

• 1
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• 0.6
• 0.4
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10

• 1

1 10 0.5 0.6 0.7 0.8 0.9 1 1.1 1.2 1.3 1.4 1.5 Eν (GeV) cosΘν

Ψ(νe)/Ψ0(νe)

sin2θ23=0.5, sin2θ13=0.04, solar on

0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18 50 100 150 200 250 300 350 CP phase sin2θ13 0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18 50 100 150 200 250 300 350 CP phase sin2θ13

 2 CP phase 

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10

• 1

1 10 0.5 0.6 0.7 0.8 0.9 1 1.1 1.2 1.3 1.4 1.5 Eν (GeV) cosΘν

Ψ(νe)/Ψ0(νe)

sin2θ23=0.5, sin2θ13=0.04, solar on

In any case, interesting to see the data!

Future study of atmospheric Future study of atmospheric s: INO : INO

50 kton INO detector

Naba K Mondal, NuHorizons 09

• D. Indumathi, NuGoa (2009)

Location of INO Location of INO ・3 modules ・Each module = 16×16×12m3 ・140 layers of 6cm thick iron ・Magnetized to 1.2 Tesla Funding for the current plan period ending in March 2012 has been allocated. g p p g Expect to start the experiment with the first module by 2013.

Future study of atmospheric Future study of atmospheric ’s: ’s: INO INO

If m23

2 is positive

resonance for  Very important to

. Indumathi, NuGoa (2009)

EXAMPLE: mass hierarchy If m23 is positive, resonance for   If m23

2 is negative, resonance for anti‐

measure the charge of leptons  INO

INO/2006/01 Project report

13 (sin213) Significance (1.12Mtonyr) 7 deg (0 015) 1 6 

Normal Inverted

7 deg (0.015) 1.6  9 (0.025) 2.5 11 (0.036) 3.5 13 (0.05) 4.5

Near future Near future LBL LBL 13

13 experiments

experiments

J-PARC (750kW design)

NO NO A T2K T2K

Need much higher sensitivity experiments

Ash Ri er Ash Ri er

( g )

NO NOA

(~ (~2013 2013 -

• )

)

T2K T2K

(2009 (2009 -

• )

)

Ash River

Duluth International Falls

Ash River

Duluth International Falls

15 kton totally active detector

295km

Minneapolis Minneapolis

810km 295km

Fermilab Fermilab

Super-Kamiokande (22 5 kton fid vol)

NuMI beam

(22.5 kton fid. vol)

NuMI beam intensity upgrade to 700 kW

T2K setup (@J T2K setup (@J‐PARC) PARC)

Target station Horn (test)

A.Ichikawa, July 2 M.Besnier, July 2 Target Station Target Station Target Target‐Horn System Horn System

M

Preparation Section Preparation Section 295 km to 295 km to Super Kamiokande Super Kamiokande

Final Final Focus Focus Section Section Muon Muon Monitoring Pit Monitoring Pit

280m 280m 110m 110m 2km detector (LoI submitted ) SCFM at Arc Section SCFM at Arc Section Decay Volume Decay Volume Beam Dump Beam Dump Near Neutrino Detector Near Neutrino Detector

Near detector

Most of the setup are ready. (Full horns and near detectors will be ready soon.)

T2K first beam and the next T2K first beam and the next

First beam signals in muon monitor (April 2009)

• Neutrino beam line OK!
• Intensity: ~4x1011 p/bunch, 1 bunch/spill (~0.1% of design

i t it ) intensity)

• Will try 100kW in JFY2009.
• Physics run from 2010
• Physics run from 2010
• Continuous effort for higher intensity

Sensitivities Sensitivities

T2K 13 sensitivity (5×1021 POT,

If sin2213 =0.08

M.Messier

13 =0 assumed)

A.Ichikawa, July 2

Values of CP  for 0.008 at 0.008 at CP

CP=0/

=0/ which hierarchy is resolved at > 95% CL. (normal hierarchy)

BG subtraction: BG subtraction: 10% error

B d Beyond 13

Studies in US and Asia Studies in US and Asia

Future LBL possibilities Future LBL possibilities

(assuming sin (assuming sin22 is larger than 0 01) is larger than 0 01)

1300 km (1000 1250 k )

(assuming sin (assuming sin 213

13 is larger than 0.01)

is larger than 0.01)

295 km (1000‐1250 km) 1.0 ‐ 2.3 MW proton beam 1.66 MW proton beam (J PARC upgrade) 295 km (J‐PARC upgrade)

Megawatt class super-beam + + Megaton class (water) detector

0 54Mt d t t i K i k 100kton modular water Ch.  Total mass = 300 ktons Or, 50‐100 kton LAr. 0.54Mton detector in Kamioka, or 0.27 Mton water Cherenkov detector in Kamioka and Korea.

CP violation sensitivities CP violation sensitivities

10-1

13

J‐PARC to Kamioka + Korea Fermilab to DUSEL

J.Maricic, July 2

10-2 10-1 normal OA=1.0 (new syst) OA=2.5 (new syst)

sin22

1 66MW

10

1 2 3 4 5 6

1MW beam assumed (sensitivity will be improved with higher 1.66MW assumed

• 2

10-1 i t d

Thick: 3

p o ed t g e beam power)

10-2 inverted

Thin: 2

1 2 3 4 5 6



M hi h I th th iti iti h t i 22 0 01 Mass hierarchy: In these exp. the sensitivities reach to sin2213 ~ 0.01.

 These experiments should be very interesting, if sin2213 > 0.01.

Summary Summary

• Since the discovery of neutrino oscillations, our

understanding on the neutrino masses and mixing understanding on the neutrino masses and mixing angles have been improving substantially.

• Dominant   oscillation is already studied rather
• Dominant  oscillation is already studied rather

accurately by atmospheric and LBL experiments. (2009) Th i t ti h i i th b d i t

• There are many interesting physics in the sub‐dominant
• scillations (13, CP violation, mass hierarchy, …).
• The next generation experiments will find evidence for

non‐zero 13, if sin2213 > 0.01. (2010 ‐)

• The subsequent big goals are CP violation, mass
• hierarchy. The world community is working hard for the

best strategy for these measurements. (20XX ‐)