Neutrino Physics & the ISS
Peter Dornan
Imperial College London
16 March 2006 P Dornan - MUTAC 2006 2
Why do Neutrino Physics?
Least understood particle Beyond the Standard Model
A trivial Addition? The Window on the Fundamental Theory?
Ultimate theory must relate quarks & leptons Cannot do this without a full understanding of the
neutrino sector Cannot do this with LHC or ILC
16 March 2006 P Dornan - MUTAC 2006 3
Neutrinos are BSM
In the SM Neutrinos are massless Lepton Flavour is Conserved Neutrino & antineutrino distinguished on the
basis of helicity Neutrino Oscillation shows
Neutrinos have mass Lepton Flavour is not Conserved Helicity cannot distinguish neutrinos from
antineutrinos
16 March 2006 P Dornan - MUTAC 2006 4
A Minor Extension of the SM?
Neutrinos are Dirac Particles Right handed Neutrinos exist
With no known interactions Or very very weak ones
Lepton Flavour is not respected But overall lepton number is conserved So Distinguish Neutrino and Antineutrino on the basis of
Lepton Number - whatever it is
Masses, Mixing Parameters - and CP Violation - just yet more parameters to feed into the theory
16 March 2006 P Dornan - MUTAC 2006 5
A Window on a Higher Theory?
now we can speculate Neutrinos are Majorana States
Neutrino and anti neutrino are not distinct Right handed neutrinos exist at very high masses -
~ unification scale
Mixing angles - and probably masses – could be related to those in the quark sector
More forms of CP violation in the lepton area than the MNS phase And this will solve the matter-antimatter mystery
16 March 2006 P Dornan - MUTAC 2006 6
Why Neutrino Physics?
These are the “Elevator” Answers For the Ultimate Theory of Particles and Forces For our Understanding of the Universe
But Improving our Knowledge demands Complex
& Challenging Experimentation. The basic tool is neutrino oscillation
From Hitoshi Murayama
When you meet your favourite senator
And want a $1B
But also to explain to immigration at O’Hare why you are coming to Fermilab
16 March 2006 P Dornan - MUTAC 2006 7
Neutrino Oscillation
Neutrinos are produced - and detected - as lepton flavour - electron, muon, tau - eigenstates
Oscillations – neutrinos produced with one flavour change to another as they pass through space
In the SM lepton flavour is conserved - no oscillations
For oscillation must have two sets of eigenstates – flavour e-states and mass e-states
16 March 2006 P Dornan - MUTAC 2006 8
`atmospheric’ `solar’ `cross/reactor’
3,2,1,, itaumuonelectronU iMNS
Oscillation defined by 3 mixing angles,
phase
ijijijij sc sin,cos
Oscillation Parametrisation
16 March 2006 P Dornan - MUTAC 2006 9
Oscillation Probability
For just two state system
E
LmP ij
ij
2
22 27.1sin2sin1
Depends upon Mixing Angle, Mass Squared Difference, L/E
More Complex for a three state systemand additional complications if neutrinos pass through matter
16 March 2006 P Dornan - MUTAC 2006 10
Oscillation Signals - Disappearance
The early evidence
Super-K Atmospheric results disappearance having travelled through the earth
SSM Prediction
Gallium Chlorine
Deficits in Solar Neutrino Flux
22323 , m
21212 ,)( me
16 March 2006 P Dornan - MUTAC 2006 11
Appearance Signals - Atmospheric
Super-K - L/E Analysis
K2K First Long Baseline
SK-I + SK+II Preliminary
L/E (km/GeV)
Dat
a/p
red
icti
on
Oscillation
No oscillation
1R- spectrum
Erec (GeV)
1 2 3 4
Nu
mb
er
of
eve
nts
16 March 2006 P Dornan - MUTAC 2006 12
Appearance Signals - Solar
The SNO Result Total Neutrino Flux as Expected
Verifies Standard Solar Model
e Detected Flux Low Electron Neutrinos have oscillated to mu or tau neutrinos
SSM Prediction Neutral Currents - Detects all Neutrinos
Charged Current - Detects Electron Neutrinos
16 March 2006 P Dornan - MUTAC 2006 13
Appearance Signals - Solar
Kamland Reactor Experiment
ceReappearan then and -
- nceDisappeara e
16 March 2006 P Dornan - MUTAC 2006 14
The Third Angle, 13
Small - only an upper limit from the Chooz Reactor Experiment
Determining just how small 13 is the next pressing problem for neutrino oscillation physics
16 March 2006 P Dornan - MUTAC 2006 15
Where are we?from: Maltoni, Schwetz, Tortola, Valle (’04)
Also know m2 > m1from matter effects in the sun
16 March 2006 P Dornan - MUTAC 2006 16
How to Proceed?
What Questions remain to be answered Many!
What must we measure? Everything we can
What can we measure? Quite a lot
With the right ingenuity - and investment
16 March 2006 P Dornan - MUTAC 2006 17
Unanswered – Non Oscillation Expts
Are Neutrinos Dirac or Majorana? Neutrinoless double-beta decay
What is the Absolute Mass? Tritium Decay Spectrum Neutrinoless double-beta decay Cosmological data
16 March 2006 P Dornan - MUTAC 2006 18
Unanswered – Oscillation Expts
Is 23 maximal?
How small is 13? CP Violation in the lepton sector? Mass hierarchy?
m3 < or > m2
Is the MNS approach correct? CPT violation? The ultimate accuracy on the mixing angles and the
mass differences What accuracy is needed?
(LSND? Sterile neutrino(s)? )
16 March 2006 P Dornan - MUTAC 2006 19
Mass Hierarchy?
Normal Inverted
Require matter interactions to distinguish.
Long Baseline
Noa > T2K
Leads to degeneracies in superbeam expts.
Critical for Neutrinoless double beta decay
16 March 2006 P Dornan - MUTAC 2006 20
CP Violation
Vitally important for our understanding of nature and the universe
Arises from phases which flip sign on the change particle antiparticle In SM Non-zero phase in the CKM quark mixing matrix
Describes observed CP violating effects Does not explain the matter antimatter asymmetry
Standard MNS matrix has one phase, , (like CKM)
BUT, if neutrinos are Majorana additional phases and potential for substantial CP violation
16 March 2006 P Dornan - MUTAC 2006 21
e Appearance in a Beam - SuperBeam
e Disappearance in a e Beam - Reactor
13 and - Leptonic CP Violation
leads to CP Violation
No term
16 March 2006 P Dornan - MUTAC 2006 22
The Imminent Future
Two long base line experiments using a beam MINOS
Numi Beam from FNAL to Soudan 735 km Two Detectors – near and far – magnetized Fe-scintillator Look for disappearance 23, m2
23
e Appearance 13 (~factor 2 better than Chooz)
OPERA CNGS Beam from CERN to Gran Sasso 732 km
One Far Detector – Emulsion Look for Appearance
16 March 2006 P Dornan - MUTAC 2006 23
In 3 – 10 Years - 13
Main aim is 13 - but will also improve other parameters
Two off-axis Superbeam Experiments T2K Noa
One or more Reactor Experiments Double Chooz
and maybe Braidwood, Daya Bay, Angra dos Deis ……
16 March 2006 P Dornan - MUTAC 2006 24
Possible Reactor Experiments
Experiment Where
Baseline
(km)
Overburden (m.w.e.)
Detector size
(t) sin2(213)
Sensitivity
(90% C.L.)Near Far Near Far Near Far
Angra dos Reis Brazil 0.3 1.5 200 1700 50 500 < ~0.01
Braidwood US 0.27 1.51 450 450 65x2 65x2 <~0.01
Double Chooz France 0.2 1.05 50 300 10 10 < ~0.03
Daya Bay China 0.3 1.8-2.2
300 1100 50 100 < ~0.01
Diablo Canyon US 0.4 1.7 150 750 50 100 < ~0.01
KASKA Japan 0.4 1.8 100 500 8 8 < ~0.02
Kr2Det (Krasnoyarsk)
Russia 0.1 1.0 600 600 50 50 < ~0.03
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“neardetector”
“fardetector
Reactor Measurements of 13
No Dependence on , No matter effects
16 March 2006 P Dornan - MUTAC 2006 26
600MeV Linac
3GeV PS
50G
eV P
S(0
.75M
W)
FD
Neutrino Beam Line
To SK
Long baseline neutrino oscillation experiment from Tokai to Kamioka ( T2K )
J-PARC (50 GeV PS) Construction: 2001~2007 Operation: 2008~
T2K (Approved in Dec-03) Construction: 2004~2008 Experiment: 2009 ~
JAERI@Tokai-mura(60km N.E. of KEK)
(~100xK2K)
Super-K50kton
Phase 2 4MW, Mton, CPV
Phase 1 (0.75MW + SK) x disappearance
Precise m2, sin22
e appearance Finite 13 ?
16 March 2006 P Dornan - MUTAC 2006 27
T2K prediction
90%C.L. sensitivities
sin2213
CHOOZexcluded
Off axis 2.5deg, 40GeV 5yr
x 20m2(e
V2)
(m223) < 1×10-4 eV2
(sin2223) ~ 0.01
For 5yr running
16 March 2006 P Dornan - MUTAC 2006 28
Noa
Upgrade of FNAL NuMi program.
Off-axis configuration, and larger proton intensity (6.5x1020 proton/year).
Very Long Baseline (810km) and sizeable matter effects
Complementary to T2K program (mass hierarchy).
<En> ~ 2.22GeV 30Kton “fully” active detector. Liquid scintillator.
16 March 2006 P Dornan - MUTAC 2006 29
Noa
Sensitivity similar to T2K.– improve with antineutrinorun.
● Sensitivity to masshierarchy.
● Synergies with T2K &reactor experiments:different matter effects anddifferent degeneracies.
16 March 2006 P Dornan - MUTAC 2006 30
The Precision Era - after T2K and Nova
Around 2012 - 2015 We shall have good measurements of
12, 23, m212, m2
23
Probably have a measurement of 13
Possibly know the mass hierarchy
So can now plan for the ultimate neutrino measurements Refine all parameters Check consistency Measure CP Violation
This is the aim of the ISS
16 March 2006 P Dornan - MUTAC 2006 31
CP Violation
16 March 2006 P Dornan - MUTAC 2006 32
Neutrino source – options:
Second generation super-beam CERN, FNAL, BNL,
J-PARC II
Beta-beam
Neutrino Factory
16 March 2006 P Dornan - MUTAC 2006 33
The International Scoping Study
International scoping study of a future Neutrino Factory and super-beam facility
Motivation
Organisation Status
Physics Group Accelerator Group Detector Group
ISS: next steps
16 March 2006 P Dornan - MUTAC 2006 34
ISS: motivation
Neutrino Factory – prior to launch of ISS Several studies at the turn of the century
US Studies I, II, IIa ECFA/CERN Study NuFact-J Study
established feasibility & R&D programme MUCOOL, MICE, MERIT….
But there have been advances since then Also appreciation of the need for an integrated
accelerator-detector-physics approach and an international approach
16 March 2006 P Dornan - MUTAC 2006 35
ISS: motivation
Goal: timely completion of conceptual design Significant international effort taking several years
Requires successful bids to provide the resources
Preparation for design study Review physics case
Critical comparison of options Review options for accelerator complex:
Prepare concept-development and hardware-R&D roadmaps for design-study phase
Review options for neutrino-detection systems Emphasis: identify concept-development and hardware-R&D
roadmaps for design-study phase Establish the Cost Drivers & Optimize
Physics/$ - where there are alternatives Absolute scientific value - where only one method
16 March 2006 P Dornan - MUTAC 2006 36
ISS: organisation
16 March 2006 P Dornan - MUTAC 2006 37
Meetings
Plenary meetings to date: CERN: 22 – 24 September 2005
Attendance: 92 Americas: 15 Asia: 12 Europe 65
KEK: 23 – 26 January 2006 Attendance: 67 Americas: 11 Asia: 28 Europe 28
Working groups: Physics:
Workshops: Imperial: 14 – 21 November 2005 Boston 6 – 10 March 2006 Phone meetings
Accelerator: Workshops: BNL: 07 – 12 December 2005 Phone meetings
Detector: Phone meetings Detector/Physics parallel at Physics workshops
16 March 2006 P Dornan - MUTAC 2006 38
Acknowledgments
This will be a very brief review of the activity in the ISS
From the meetings - very many people have contributed so - it is hard to acknowledge everyone - so I apologise for failing to mention many of the contributors
All plots and contributors can be found on the web
16 March 2006 P Dornan - MUTAC 2006 39
Physics Group
Theory subgroup : What is the new physics Need to distinguish between alternative theories Establish the case for high-precision, high-sensitivity neutrino-
oscillation programme Phenomenological subgroup
Review models of neutrino oscillations Identify measurables that distinguish them and assess the
precision required Experimental subgroup:
Use realistic assumptions on the performance of accelerator and detector to: Evaluate performance of the super-beam, beta-beam and Neutrino
Factory alone or in combination Make meaningful comparisons
Muon physics subgroup: Lepton-flavour violating processes – clear synergy with neutrino
oscillations – possibly the next major discovery
16 March 2006 P Dornan - MUTAC 2006 40
Some Theoretical Ideas
Flavour symmetry:
Quarks and charged leptons do not carry the same hidden quantum numbers
All neutrinos carry the same hidden quantum numbers Allows differences in mass hierarchies and mixing matrices to
be explained through symmetry breaking Random sampling of many such models indicates that large
θ13 is favoured
16 March 2006 P Dornan - MUTAC 2006 41
Some Theoretical Ideas
Quark-lepton complementarity
Intriguing Relations Coincidence fundamental
GUTs motivate relationships between the quark and lepton mixing matrices
Measurable relations Need Precision
41212 CKMMNS
42323 CKMMNS
16 March 2006 P Dornan - MUTAC 2006 42
16 March 2006 P Dornan - MUTAC 2006 43
16 March 2006 P Dornan - MUTAC 2006 44
A Possible Neutrino Sum Rule
cos26.35 1312
%10313
%10313
20
5.012
16 March 2006 P Dornan - MUTAC 2006 45
Towards a performance comparison
A Major Goal of the ISS Now many options Must be reduced if there is to be a realistic design for
a ‘precision era’ neutrino facility Requires justifiable assumptions:
Accelerator: flux, energy spectrum Detector: Ethresh, ERes (background, x-sect.
uncertainty…)
and optimised facility (accelerator, baseline, & detectors)
Already a very substantial amount of work
16 March 2006 P Dornan - MUTAC 2006 46
Cases under Consideration
Off axis super-beam: T2HK taken as example
Plan to explore different options (essentially vary E and L)
Beta beam: Low : = 100 and L = 130 km
High flux (~1018 decays per year) and high flux (1019 dpy) High : = 350 and L = 700 km
High flux (~1018 decays per year) and high flux (1019 dpy) Also Beta beam abd superbeam combination
Neutrino Factory Performance studied as a function of:
E and L Ethresh and ERes
16 March 2006 P Dornan - MUTAC 2006 47
Sample - CP sensitivity v. sin2213
Work in progress
But highlights the importance of 13 in defining a strategy
Huber, Lindner, Rolinec, Winter
16 March 2006 P Dornan - MUTAC 2006 48
CPT & the MNS Theory
In the Quark sector the CP violation parameters are determined in many ways
Can we do the same in the neutrino sector?
With 3 flavours and CPT CP violation related in
e ->
->
e ->
Needs tau modes
Murayama
16 March 2006 P Dornan - MUTAC 2006 49
Beta beam, super beam comparison
High θ13: Beta beam & super beam alone:
sensitivity good Poor sign(m23
2) sensitivity
T2HK
Low-E βB
High-E βB
2 MW
4 MW
Low Flux
High Flux
Low Flux
High Flux
T2HK
Low-E βB
High-E βB
2 MW
4 MW
Low Flux
High Flux
Low Flux
High Flux
Preliminary! Need to include bettertreatment ofbackgroundand sys. err.
Couce
16 March 2006 P Dornan - MUTAC 2006 50
Neutrino Factory: optimisation
Study performance as a function of muon energy and baseline
Detector: 100 kton, magnetised iron Importance of threshold
sensitivity
Can trade muon energy against detector threshold and resolution
16 March 2006 P Dornan - MUTAC 2006 51
ISS status: Accelerator Group
Subsystems & subgroups Proton driver Target and capture Front end
Bunching and phase rotation
Cooling
Acceleration Decay ring
Decay Channel
Linear Cooler
Buncher
1-4 MWProtonSource
Hg-Jet Target
Pre-Accelerator
Acceleration
DecayRing ~
1 km5-10 GeV
10-20GeV
1.5-5 GeV
Decay Channel
Linear Cooler
Buncher
1-4 MWProtonSource
Hg-Jet Target
Pre-Accelerator
Acceleration
DecayRing ~
1 km5-10 GeV
10-20GeV
1.5-5 GeV
16 March 2006 P Dornan - MUTAC 2006 52
Accelerator Group – mission
Two phase approach: Phase 1:
Study alternative configurations; arrive at baseline specifications
Develop tools required for end-to-end simulations ‘Top-down’ cost evaluation required to guide choices
Phase 2: Focus on selected option(s)
Begin to consider engineering issues Through initial engineering studies, identify R&D required in
‘International Design Study’ phase
Presently working through Phase 1 Highlights
16 March 2006 P Dornan - MUTAC 2006 53
Proton driver:
Key issues for Neutrino Factory proton driver: Beam current limitations Creation of short bunches Repetition rate limitations Space charge limitations Tolerances
Largely driven by downstream constraints
Survey carried out:
1. SPL 3.5 GeV 50 Hz 4 MW2. JPARC 50 GeV 0.33 Hz 0.6 -> 4 MW3. AGS 24 GeV 0.5 Hz 0.2 -> 4 MW4. FNAL SCL 8 GeV 10 Hz 0.5 -> 2 MW5. RAL RCS 5 GeV 50 Hz 4 MW6. RAL RCS 15 GeV 25 Hz 4 MW7. RAL FFAG 10 GeV 50 Hz 4 MW8. KEK/Kyoto 3 GeV 1 kHz 1 MW9. A. Ruggiero FFAG 12 GeV 100 Hz 18 MW10. A. Ruggiero FFAG 1 GeV 1 kHz 10 MW
16 March 2006 P Dornan - MUTAC 2006 54
RAL 4 MW FFAG Proton Driver
•RAL design
•5 bunches per pulse
•50 Hz repetition rate
•10 GeV
•Isochronous FFAG with insertions
• RF system naturally gives 2 ns rms pulse• need to add 6th harmonic to get 1 ns rms
Issue:
Bunch length at injection
16 March 2006 P Dornan - MUTAC 2006 55
Target and capture
Issues for target and capture system: Optimum proton-driver energy Optimum target material Constraints on target operation at 4 MW
Proton bunch intensity Proton bunch length Repetition rate
Possible materials Liquid mercury preferred for high-power operation Solid tantalum may be an option Carbon probably OK up to 1 MW
16 March 2006 P Dornan - MUTAC 2006 56
Target and capture: proton energy
Different simulations disagree MARS Geant4
Preliminary conclusion: Proton driver energy
in range 5 – 15 GeV
120G
eV10
0GeV
75G
eV50G
eV
40G
eV
30G
eV
20G
eV
15G
eV
10G
eV
4GeV
2.2G
eV
3GeV
5GeV
6GeV
8GeV
0
0.001
0.002
0.003
0.004
0.005
0.006
0.007
0.008
0.009
1 10 100 1000
Proton Energy (GeV)
Pio
ns
per
Pro
ton
.GeV
(es
t. P
has
e R
ota
tor)
pi+/(p.GeV)
pi-/(p.GeV)
pi+/(p.GeV)
pi-/(p.GeV)
16 March 2006 P Dornan - MUTAC 2006 57
Target and capture
MERIT experiment at CERN High-power liquid-mercury jet
target engineering demonstration
16 March 2006 P Dornan - MUTAC 2006 58
Front-end
Review and compare performance of existing schemes (CERN, KEK, US) Conclusions will require cost model to be developed
Evaluate trade-offs between degree of cooling and downstream acceptance Figure of merit (muons per proton) Need to define options for acceptance downstream of cooling
channel Small, medium, and large?
Optimisations: Minimise RF required Optimum choice of materials for absorber in cooling channel
Evaluate cost optimum
16 March 2006 P Dornan - MUTAC 2006 59
Front end: new configurations
• “Guggenheim” cooling channel• provides longitudinal cooling• solves problems with
injection, absorber heating• can taper parameters
(A. Klier)
(D. Neuffer)
• cool while doing phase rotation• cost savings• 150 atm hydrogen (room temp)• 24 MV/m RF• performance looks promising
16 March 2006 P Dornan - MUTAC 2006 60
Cooling: hardware R&D programme
Complementary programmes: MuCool:
Design, prototype, and test – using an intense proton beam – cooling channel components
MICE: Design, construct, commission,
and operate – in a muon beam – a section of cooling channel and measure its performance in a variety of modes
Both programmes well advanced
16 March 2006 P Dornan - MUTAC 2006 61
Acceleration: FFAG development Increasing effort on
scaling and non-scaling FFAG
PRISM: Phase rotated intense muon source
Under construction in OsakaCommissioning 2007
Proof of principle ‘non-scaling’ FFAGDecay ring
EMMA :Electron model of muon acceleration
16 March 2006 P Dornan - MUTAC 2006 62
Decay ring
Issues: Racetrack or triangle geometry
20 GeV or 50 GeV or 20 GeV-upgradable
How to handle both muon charges (1 ring or 2)
Length of µ bunch train (constrains circumference)
RF to maintain bunch structure
Beam loading (~MW µ beams)
Shielding from µ decays
16 March 2006 P Dornan - MUTAC 2006 63
Decay Ring - Options
Isosceles Triangle (G Rees) Circumference = 1170 m length of each production straight = 301 m (2 x 0.26 efficiency) 5 bunch trains per cycle angles of triangle depend on ring and target sites
designed for apex angle = 22.4o 27, 34.5, 45, 52 also possible (±1o)
Racetrack geometry (C Johnstone), C = 1371 m both 20 GeV and 50 GeV use same lattice production straight
496 m long (36% production efficiency) quad focusing - maximum beta = 155 m, 167 m
16 March 2006 P Dornan - MUTAC 2006 64
ISS status: Detector Group
Detector options and subgroups Large water Cherenkov
ISS activity focuses on consideration of R&D required: Photo tubes Front-end electronics
Liquid argon Emulsion Magnetic sampling calorimeter Near detector
Further instrumentation issues: Flux, muon-polarisation measurement
16 March 2006 P Dornan - MUTAC 2006 65
Detector technology: summary
Magnetised liquid argon: Golden, platinum, and silver channels accessible
Magnetised sampling calorimeter: Golden channel accessible
Sampling fraction: Can totally active ‘get’ some silver or platinum sensitivity
Hybrid detector system?
16 March 2006 P Dornan - MUTAC 2006 66
Liquid argon
Detector concepts
Various configurations being studied in ISS: Glacier T2K-LAr (near det.) NuMI LArTPC
16 March 2006 P Dornan - MUTAC 2006 67
Emulsion detector – MECC
Stainless steel or Lead Film Rohacell
DONUT/ OPERA type target + Emulsion spectrometer + TT + Electron/pi discriminator
B
Assumption: accuracy of fi lm by fi lm alignment = 10 micron (conservative)
13 lead plates (~2.5 X0) + 4 spacers (2 cm gap) (NB in the future we plan to study stainless steel as well. May be it will be the baseline solution: lighter target)
The geometry of the MECC is being optimized
3 cm Electronic detectors/ ECCStainless steel or Lead Film Rohacell
DONUT/ OPERA type target + Emulsion spectrometer + TT + Electron/pi discriminator
BB
Assumption: accuracy of fi lm by fi lm alignment = 10 micron (conservative)
13 lead plates (~2.5 X0) + 4 spacers (2 cm gap) (NB in the future we plan to study stainless steel as well. May be it will be the baseline solution: lighter target)
The geometry of the MECC is being optimized
3 cm Electronic detectors/ ECC
16 March 2006 P Dornan - MUTAC 2006 68
Magnetic sampling calorimeter
Concept: Magnetised iron?
Sampling fraction?
Air toroid Cost
~ $300M
Basic Detector Concept
7.5 mm
15.0 mm
Considered Extremely Fined Grained
Electro
n
Mu
on
16 March 2006 P Dornan - MUTAC 2006 69
Near detector
Measurement of cross sections in DIS, QE and RES.
Coherent Different nuclear targets: H2, D2
Nuclear effects, nuclear shadowing, reinteractions
With modest size targets can obtain very large statistics
What is lowest energy we can achieve? E.g. with LAr can go down to ~MeV
Measurement of cross sections in DIS, QE and RES.
Coherent Different nuclear targets: H2, D2
Nuclear effects, nuclear shadowing, reinteractions
With modest size targets can obtain very large statistics
What is lowest energy we can achieve? E.g. with LAr can go down to ~MeV
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Timescales: the challenge
16 March 2006 P Dornan - MUTAC 2006 71
ISS – Summary The ISS was launched at NuFact05 and is now half way
through its one year programme Conclude at NuFact06 and a report early fall
It has demonstrated a strong desire to have an internationally coordinated effort for future neutrino research (c.f linear collider) New ideas Many clarifications
It has brought together accelerator & detector scientists with their experimental and theoretical physics colleagues in a very productive way
It has built up a momentum which must be used as a springboard for the next phase
16 March 2006 P Dornan - MUTAC 2006 72
ISS – Immediate Future
Next Plenary Meeting RAL, UK, April 24 – 29 Preceded by an Accelerator Group Workshop
Final Meeting Irvine, Aug 21 – 22 Just before NuFact06
Still much to be done – more help always welcome
Visit the website http://www.hep.ph.ic.ac.uk/iss/ Transparencies from all the meetings etc. Join the mailing lists Help to establish the best way forward