Summary

Workshop on Neutrino PhysicsOct.6/7 in Hamburg

Caren HagnerVirginia Tech University

Tritium β-Decay: Mainz/Troitsk

e -33 eHe H e -33 eHe H

222i

iei mUm

CL%95eV2.2eV1.22.22.1 22

mmMainz Data (1998,1999,2001)Mainz Data (1998,1999,2001)

Future:KATRIN

eV35.0

m

Double Beta Decay

0: (A,Z) (A,Z+2) + 2e-

2: (A,Z) (A,Z+2) + 2e- + 2e(Observed for several nuclei, test of nuclear matrix elem. calculations)

d

d

u

u

e-

e-

W-

W- e

LH neutrino (L=-1) absorbed

e RH antineutrino (L=1) emitted

L=2, Majorana

Double Beta Experiments: Results

CL) (90% eV 35.0

mHeidelberg-Moskau Collaboration, Eur.Phys.J. A12 (2001) 147

IGEX Collaboration, hep-ex/0202026, Phys. Rev. C59 (1999) 2108

2.1 × 1023 0.85 – 2.1

all 90%CLall 90%CL

HM-K

IGEX

Future: 1 order of magnitude improvement

Parametrization of Neutrinomixing

Neutrino-mixing matrix: • 3 mixing angles: θ12, θ23, θ13

• 1 CP-violating Dirac-Phase: δ

Neutrino-mixing matrix: • 3 mixing angles: θ12, θ23, θ13

• 1 CP-violating Dirac-Phase: δ

In addition, if Majorana neutrinos:• 2 CP-violating Majorana-phasesIn addition, if Majorana neutrinos:• 2 CP-violating Majorana-phases

3

2

1

1212

1212

1313

1313

2323

2323

100

0

0

0

010

0

0

0

001

cs

sc

ces

esc

cs

sci

ie

θsolθ13, δθatm

Solar neutrinos

LENALENA

(Low Energy Neutrino Astrophysics)(Low Energy Neutrino Astrophysics)

Idea: A large (~30 kt) liquid scintillator Idea: A large (~30 kt) liquid scintillator underground detectorunderground detector for for

Galactic supernova Galactic supernova neutrino detectionneutrino detection

Relic supernovae Relic supernovae neutrino detectionneutrino detection

Terrestrial neutrino detection

Search for Proton Decay

Solar Neutrino Spectroscopy

Neutrino properties

P - decay event

Scintillator: PXE , non hazardous, flashpoint 145° C, density Scintillator: PXE , non hazardous, flashpoint 145° C, density 0.99, ultrapure (as proven in Borexino design studies)0.99, ultrapure (as proven in Borexino design studies)

Npe ~ 100 / MeV beta

Atmospheric neutrinos

New SuperK analysis

Preliminary!

New analysisOld analysis

• Neutrino flux (Honda 1995 Honda 2001)

• Improved event reconstruction tools

Each change slightly shifted the allowed region to lower m2

• Neutrino interaction models (several improvements, agree with K2K near data)

• Improved detector simulation

This makes life harder for everyone !

sterile neutrinos?What about LSND?

MiniBooNETaking data: data appears to be OK

First results to be presented at theWIN Conference later this month

The “box” for ->e analysisprobably will not be opened tillsometimes in 2005

The next future in neutrino oscillation experiments

• Europe: CNGS beam Opera, Icarus

• US: NuMI beam MINOS

• Japan: K2K (results) -> JPARC (JHF-SK)

Europe:CNGS

vτ - appearance

2 ways of detecting appearance

…..

- + X oscillation CC interaction

-R

h-ne- e

+--n

OPERA: Observation of the decay topology of ( à la CHORUS)In photographic emulsion (~ m granularity)A digital Cloud chamber

ICARUS: detailed TPC image

in liquid argon and kinematic

criteria ( à la NOMAD )

(~ mm granularity)A digital Bubble chamber

Decay “kink”

-

~1 mm

But also: … ee- + X

El.m. shower

stop and decay in e

Schedule

Cost to completion

all numbers in kCHF

CNGS cost estimate - Summary Dec-99 Feb-02 changesince 2002

Civil Engineering 41,570 43,720

Equipment 19,629 23,143 - 541

Infrastructure 7,336 9,701 + 165

Contingency 2,465 2,465 + 376

GRAND TOTAL 71000 79029List of possible savings (April 2002) -1429

APPROVED PROJECT COST (June 2002) 77600 0

CNGS beam

OPERA/CNGS1 an hybrid detector

supermodule

8 m

Target Trackers

Pb/Em. target

Electronic detector finds the brique of interaction ID, charge et p

Emulsion analysis vertex decay kink e/ ID, multiple scattering, kinematics

Extract selected brick  

Pb/Em. brick

8 cm Pb 1 mm

Basic “cell”

Emulsion

Schedule and Milestones

• There is still some flexibility in the installation schedule many tasks can be done in parallel :1. Detectors cabling and commissioning2. Target and Precision tracker installation3. TT planes assembly and brick wall installation4. SM2 Magnet and SM1 Target

• Data taking can run as soon as brick filling is starting

Milestones 1. november 2003 starts SM1 Magnet RPC installation2. June 2004 starts SM1 Target installation3. January 2005 BAM and BMS installation 4. July 2005 starts filling bricks

ICARUS T3000

Muon spectrometer

T600 T1200

T1200

≈3 kton of liquid Argon

Run 960, Event 4 Collection Left

25 cm

85 cm

Electronic bubble chamber

176

cm

434 cm

Run 308, Event 160 Collection Left

265 cm

142 cm

Muon decay

Shower

Hadronic interaction

Expected number of events

full mixing, 5 years run @ 4.5 x1019 pot / year

signal

(m2 = 1.3 x 10-3 eV2)

signal

(m2 = 2.0 x 10-3 eV2)

signal

(m2 = 3.0x 10-3 eV2)

BKGD

OPERA1.8 kton fiducial

4.7 7.3 11.4 0.7

ICARUS1.5 kton fiducial

4.9 7.6 11.9 0.7

Remember : proton intensity could be increased by 2.55 (at most!)

Probability of claiming a 4 discovery in 5 years

SK 90% CL

Opera no beam upgrade

Opera with foreseen beam upgrade

(1.5)Opera, no beam upgrade but half background

Opera with beam*2

Opera with beam*3

Opera with beam*4

Conclusions

• the CNGS program will start in 2006 (data available in 3 years)• the physics goal, for the appearance,

is still appealing and valid• 13 sensitivity in off peak mode is complementary

with the future Super-beam experiments (Phase 1)• it is also the way to keep alive the experimental

neutrino physics in Europe Physicists trained in this program will be also the actors

of precision measurement of the MNS mixing matrix

US:NuMI /MINOS

Precision on Δm231

Oscillation pattern

Overview of the Experiment

MINOS Physics Capabilities

MINOS Physics Reachis basically determined by the no of protonsavailable

NuMI Schedule

• The Underground (tunnel, caverns, and shafts) contractor has finished in late November of last year (2002)

• Surface Building and Outfitting contract work has begun Nov/02 and is coming to the end– Beneficial occupancy of Target Hall in October 2003– Beneficial occupancy of MINOS Hall in December 2003

• Installation of beam technical components and Near Detector should take about 1 year

• We expect first beam on NuMI target end of 12/04

How to measure themissing mixing angle

θ13?

e e (disappearance experiment)

Pth= 8.5 GWth, L = 1,1 km, M = 5toverburden: 300 mwe

Θ13: best current constraint= CHOOZ

World best constraint !

@m2atm=2.10-3 eV2

sin22θ13 < 0.2

(90% C.L)

ex

R = 1.01 2.8%(stat)2.7%(syst)

M. Apollonio et. al., Eur.Phys.J. C27 (2003) 331-374

In the future:measure the

θ13 with superbeamand/or reactor experiment

JPARC (JHF) programin Japan

Neutrino Projects in Japan1980 1990 2000 2010 2020 2030 2040

Kamiokande

KamLAND

Super-

Kamiokande

K2K

JHFnu

Hyper-

Kamiokande

FFAG-Based

Neutrino

Factory

Neutrino burst from SN1987A

Solar neutrino observation

Atmospheric neutrino oscillation

Solar neutrino oscillation

Indication of neutrino oscillation

First long baseline neutrino oscillation esperiment

Measurement of 13 ？

Neutrino CP violation？

Proton decay ？

R&d

Construct.

Operation

Reactor antielectron neutrino oscillation

N

600MeV Linac

3GeV PS

50G

eV P

S(0

.75M

W)

FD

Neutrino Beam Line

To SK

J-PARC Facility (JHF)

Construction2001 ～ 2006 JFY

J-PARC K2K

E(GeV) 50 (40) 12

Int.(1012ppp) 330 6

Rate(Hz)0.275

(0.353)0.45

Power(kW) 750 (770) 5.2

JAERI@Tokai-mura(60km N.E. of KEK)

Approved in Dec.2000

20072007

Detectors for the JHFnu Experiment

• Muon monitors @ ~140m– Fast (spill-by-spill) monitoring of beam

direction / Intensity• First Near detector @280m

– Neutrino intensity / spectrum / direction

• Second Near Detector @ ~2km– Almost same Espectrum as for SK

• Far detector @ 295km

1.5km

295km

0.28km

Neutrino spectra at diff. dist

dominant syst. in K2K

p

140m0m 280m 2 km 295 km

on-axis

off-axis

OA3°

OA2°OA1°

Off Axis Beam(ref.: BNL-E889 Proposal) TargetHorns

Decay Pipe

Super-K.

Quasi Monochromatic Beam x 2~3 intense than NBB

Statistics at SK (OAB 2 deg, 1 yr, 22.5 kt)~ 4500 tot ~ 3000 CC e ~0.2% at peak

~102 x (K2K)

Tuned at oscillation maximum

Near Neutrino Detectors

• Detectors at both on/off-axis– On: dir. mon. / spectrum– Off: spectrum / K component

• Full active fine grained– low energy threshold

• Muon detector w/ mag. field– Momentum meas.– Sign selection (2nd phase)

• ~1000 ton Water Cherenkov– Similar structure to the far det.

• Very similar spectrum w/ far– Small systematics in spectrum

extrapolation• Fine grained detactor

– Precise neutrino interaction meas.

• Muon detector– Catch high energy muons

@280m @~2km

Far Detector

Super-Kamiokande• 50kt water Cherenkov• 11,000 20inch PMT’s• Characteristics

– Low energy threshold– 4 coverage– Good energy resolution @ low

energies (<1GeV)– Good PID capabilities– Cheaplarge massIdeal fore app. @ low E

Hyper-Kamiokande• ~1Mt water Cherenkov• ~200,000 photo-sensors

– Need innovation to reduce cost– R&D in progress (Hybrid photo-

detector)

1st phase 2nd phase41

.4m

40m

48m

58m

Total 500m

Status of Funding Request & Schedule

• 160 Oku-Yen over 5-year period (2004 – 2008 JFY) being requested.

• Funding Agency (Ministry of Education, Culture, and Science and Technology, or “Monkasho,”) have sent this request to Ministry of Finance.

• Final decision at the end of December, 2003.– Full amount not necessarily guaranteed.

• However, 2-km detector and its hall are not included in this request.– How to get funding for the 2-km detector and civil construction?

• Additional request in later years?• KEK internal budget?• Any other sources?

• Aim at the neutrino beam line commissioning during 2008 (calendar year).

European Activities and Plans• Spain– Barcelona – E. Fernandez, F. Sanchez– Valencia – J. Burguet, J.J. Gomez Cadenas, A. Tornero

• Italy – Napoli – V. Palladino– Padova – M. Mezzetto, M. Laveder– Roma – U. Dore, P. Loverre, L. Ludovici

• France– Saclay - J. Bouchez, C. Cavata, J. Mallet, L. Mosca, F. Pierre

• Switzerland– Geneva – A. Blondell, S. Gilardoni, A. Cervera– ETH – A. Rubbia

• United Kingdom– RAL/Sussex – D. Wark– Imperial College – P. Dornan, K. Long (+ 2 to be named later)– Queen Mary Westfield – P. Harrison, C. Cormack, J. Back– Liverpool – J. Dainton, A. Mehta, C. Tournamanis

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University of Sussex/RAL

DESYOct. 6’03

Dave Wark

European Activities and Plans

• Current activities:• Cooperative analysis on HARP• A subset have joined and are participating in K2K • Active involvement in simulations • Some assistance with magnets (Saclay)

• Plans (currently evolving):• 280m – Fine-grained calorimeter, muon monitor• 2 km – Fine grained, perhaps liquid argon TPC?• HERO (?)• Simulation and analysis• Meeting at CERN on 21/22 November, all welcome

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University of Sussex/RAL

DESYOct. 6’03

Dave Wark

European Activities and Plans

• Critical weaknesses in the European group which German participation might address:• Need more really active European participants• Need more beam expertise• Need more target expertise • Need more detector expertise for 280m and 2km• The 2km detector is key to the physics objectives, but

funding is not certain – a contribution from Europe to the beam/target would help create the conditions necessary for the 2km to be realized early in the project, and thus offer an opportunity for substantial European participation in the 2km detectors.

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University of Sussex/RAL

DESYOct. 6’03

Dave Wark

Future Prospects

2013?

2004 : start construction

Future SuperBeam, VLBL, -fact for very small 13, CPV, sign of m2202x?

JHF1

sin2213>0.018?

JHF2CPVprecision meas. 13

Proton decay

JHF2Search 13 <10-3

CPVProton decay

2008

3 discovery

Hint?

The US (Fermilab) programfor off-axis neutrino beam

Possible detector architecture (active medium interspersed with particle board)

19.5 m

233 m

17 m

14.4 m

28.8 m

Liquid Scintillator Monolithic structure 1.2 m x 3 cm x 14.4 m extrusions 32 cells/extrusion 885 planes, 679,680 channels

Glass RPC’s Modular Structure 36 2.4 x 2.8 m chambers/module (12 layers)86,400 chambers, 3,686,400 channels

Comparison with JPARC

Assume transition probability at the CHOOZ limit

S.Wojcicki General Comment on US program• The total cost of the NuMI project was about $174M• Only about $50M of that amount went into Soudan

excavation and Far Detector• It makes sound financial sense to capitalize on the

investment in the NuMI beam if physics warrants it• Neutrino physics will be a frontier area in HEP for many

years to come• The focus of Fermilab activities in the medium range

future will not be a collider program. Neutrino physics appears to be an ideal center piece of medium range (2006-2018) program there.

Submit proposal(2 technologies)Request ND approval

Phase I approval of full detector

FNAL

NSFR&D: Year 1•Test beam prototype•Cosmic ray test•ND, FD engineering

R&D: Year 2•ND construction•FD engineering

R&D: Year 3•FD engineering

MRE Proposal

2003 2004 2005 2006

NSF proposal cycle

NSF funding cycle

Test beam,cosmic running

Near detectorin beam

P5 Review

FNAL reviews

Refined proposal:cost/schedule, conceptual design

PAC PAC PAC

Measuring θ13 with reactor neutrinos?

Superbeams

Reactors

One nuclear plant & two detectors

Nuclear reactor

1,2 core(s) ON/OFF : ok 4 cores ON/OFF : no !

Near detector

5-30 tons> 50 mwe

Far detector

5-30 tons> 200 mwe

D1 = 0-1 km D2 = 1-2 km

e e,,

Isotrope e flux (uranium & plutonium fission fragments) Detection tag : e + p e+ + n, <E>~ 4 MeV, Threshold ~1.8 MeV Disappearance experiment: suppression+shape distorsion between the 2 detectors 2 IDENTICAL detectors (CHOOZ, KamLAND, BOREXINO/CTF type)

• Minimise the uncertainties on reactor flux & spectrum (2 % in CHOOZ)• Cancel cross section uncertainty (1.9 %) • Challenge: relative normalisation between the two detectors < 1% !

Sites Summary

Reactor Site Distances 1 / 2

(km)

Pth

(GW)

Overburden

(mwe)

Target mass

(m3)

Chooz France100-

200/1050 8.4 (2) 50 / 300 ~11.5

Diablo Canyon

US (Cal) <1/~2 6.1 (2) 200 / 800 30-40 ?

Kashiwasaki

Japon ~0.4/1.3 24.3 (7) 250 / 500 ~8

Penly France 0.4/1.8 8.3 (2) 200 / 200 20 ?Cruas France 1./1.8 11.7 (4) 150 / 400 20 ?

Krasnoyarsk

Russie 0.1/1 1.6 (1) 600 50

Angra Brésil ?/? ~ 4 (1) ? ?Texono Taiwan ?/~2 4.1 (1) ? / 800 ?

Site review at the Munich meeting this week (9-11/10/2003)

Reactor potential: sin2(213)<0.02-0.03, 90% C.L. CHOOZ : sin2(213)<0.2 discovery potential !Reactor & accelerator have a SIMILAR potential and are complementary

Technology / design well known (Chooz, Borexino, KamLAND) few R&D needed

Detector cost is strongly dependent on the site: Example: @Chooz, 2x10 tons, cost<10 Meuros. (Civil engineering included)

Strong links between Germany & France (Bugey, LENS, Borexino, …)Case under study: French target vessels & German scintillator (MPIK)

Our Goal @CHOOZ: Construction starts in 2005 (civil engineering ) Start data taking in 2007 !

Summary & outlook

2003 2004 2005 2006 2007 2008 2009

Site Data takingProp. Construction

year

design

< sin2(213) < ~0.04 < sin2(213) < 0.025-003

Status and perspectivesof

accelerator based neutrino programs

in Europe

V. Palladino/INFN Workshop

Neutrinophysik06.-07. Oktober 2003

DESY, Hamburglonger term aspects beyond present CNGS

Conventional beam decay channel … (0.1-1% e)

SuperBeam, if MW power ……. need Very Large Detector (water C, Li-Ar) the same as p-decay

Neutrino Factory storage ring ….. & e

manipulate & (& accelerator complex! )accelerate needs Large Magnetic Detector parents ! (SuperMINOS, Li-Ar in B )

BetaBeam storage ring … pure e (& EU accelerator complex)

detectors as SuperBeams

What options do we have? NB: beam + detector configurations

possible, in all cases, for CP, T & CPT studies

50-500 Ktons ie new lab

30-100 KtonsLNGS ! new lab ?

novel

beams

Superbeam Conventional SuperBeam: the CERN scheme

Few 100 MeV

e e appearance

Concept of a Neutrino Factory

Neutrino Factory: CERN Scheme

e e

e e

Disappearance e e deficit

deficit

Appearance e e excess excess

Appearance … Wrong Charge Signature

e excess Golden excess Silver

! Magnetic detector

MultiGeV

Incoming muon beam

Diffusers 1&2

Beam PIDTOF 0

CherenkovTOF 1

Trackers 1 & 2 measurement of emittance in and out

Liquid Hydrogen absorbers 1,2,3

Downstreamparticle ID:

TOF 2 Cherenkov

Calorimeter

RF cavities 1 RF cavities 2

Spectrometer solenoid 1

Matching coils 1&2

Focus coils 1 Spectrometer solenoid 2

Coupling Coils 1&2

Focus coils 2 Focus coils 3Matching coils 1&2

10% cooling of 200 MeV/c muons requires ~ 20 MV of RF single particle measurements =>

measurement precision can be as good as out/ in ) = 10-3

never done before either….

MICE

Japanese Approach

• Circular machine-acceleration based• FFAG (Fixed Field Alternating Gradient

synchrotron)– Large transverse and longitudinal acceptance– A fixed field allows quick acceleration

• Low Frequency RF (~1 MV/m)– Large aperture

• No phase rotation / cooling

NufactJ report is available at http://www-prism.kek.jp/nufactj/

Neutrino TelescopesPhysics motivation

origin and acceleration of cosmic rays understand cosmic cataclysms find new kind of objects?

neutrino properties , cross sections, oscillations (ANTARES) mass hierarchy from SN (ICECUBE) dark matter (neutralino annihilation)

new (rare) particles

tests of relativitiy .. effects of extra dimension etc. .Neutrino background radiation Z0hadrons

Summary

neutrino telescopes clue to understand cosmic accelerators

with some luck also important results for particle physics

with very much luck extremely interesting ....

Very important contributions by DESY to AMANDA and IceCube

end