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
…N
eutr
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JPA
RC
...
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
…N
eutr
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roje
ct
JPA
RC
...
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.
…N
eutr
ino P
roje
ct
JPA
RC
...
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
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