Highlights of ISS and nufact 1. ISS 2. achieved goals 2.1 investigation of neutrino detectors

A. Blondel GDR neutrino 4 0ctobre 2006 Orsay

Highlights of ISS and nufact

1. ISS 2. achieved goals2.1 investigation of neutrino detectorsset of baselines2.2 study of accelerator-- Neutrino factory-- betabeam-- superbeam2.3 performance studies -- new elements -- iron calorimenter performance improvement2.4 matter effects2.5 low energy cross-sections3. conclusion: towards FP7 design studies


Detectors (NEW!)

1. Water Cherenkov (1000kton)

2. Magnetized sampling detector (100kton)

3. Liquid Argon TPC (100 kton)magnetized Liquid Argon TPC (15kton)

4. Hybrid Emulsion (4 kton)

Near detectors (and instrumentation)

( SB,BB NF )

Physics

compare performance of various options on equal footing of parameters and conventionsand agreed standards of resolutions, simulation etc.

identify tools needed to do so (e.g. Globes upgraded)

propose « best values » of baselines, beam energies etc..

Accelerator: -- proton driver (energy, time structure and consequences)-- target and capture (chose target and capture system) -- phase rotation and cooling -- acceleration and storage

evaluate economic interplays and risksinclude a measure of costing and safety assessment

Yorikiyo Nagashima

Alain Blondel

Michael Zisman coordinationPeter Dornan+ ‘wise men’Ken PeachVittorio Palladino(BENE)Steve GeerYoshitaka Kuno

The ISS:


Collaborators of the scoping study:

-- ECFA/BENE working groups (incl. CERN) (funded by CARE)-- Japanese Neutrino Factory Collaboration-- US Neutrino Factory and Muon collider Collaboration-- UK Neutrino Factory Collaboration (also part of BENE)-- others (e.g. India INO collaboration, Canada, China, Corea ...)

objectives: Evaluate the physics case for a second-generation super-beam, a beta-beam facility andthe Neutrino Factory and to present a critical comparison of their performance;

Evaluate the various options for the accelerator complex with a view to defining a baselineset of parameters for the sub-systems that can be taken forward in a subsequentconceptual-design phase;

Evaluate the options for the neutrino detection systems with a view to defining a baselineset of detection systems to be taken forward in a subsequent conceptual-design phase.


Water Cerenkov DetectorsKenji Kaneyuki, Jean-Eric Campagne

Magnetic Sampling DetectorsJeff Nelson --> Anselmo Cerverahttp://dpnc.unige.ch/users/blondel/detectors/magneticdetector/SMD-web.htm

TASD Malcolm EllisLarge Magnet Alan Bross

Liquid Argon TPC http://www.hep.yorku.ca/menary/ISS/

Scott Menary, Andreas Badertscher, Claudio Montanari, Guiseppe Battistoni (FLARE/GLACIER/ICARUS’)

Emulsion Detectors http://people.na.infn.it/~pmiglioz/ISS-ECC-G/ISSMainPage.html

Pasquale Migliozzi

Near Detectors http://ppewww.ph.gla.ac.uk/~psoler/ISS/ISS_Near_Detector.html

Paul Soler

Working groups

Detector Technology associated with detector typededicated detector technology session at ISS2 in KEK Jan06.

http://dpnc.unige.ch/users/blondel/detectors/magneticdetector/SMD-web.htm












http://people.na.infn.it/~pmiglioz/ISS-ECC-G/ISSMainPage.html










ISS detector mailing list (78)


Executive summary: I. baseline detectors

beam Far detector R&D needed

sub-GeVBB and SB (MEMPHYS, T2K)

Megaton WC photosensors!cavern and infrastructure

1-2 GeV BB and SB(off axis NUMI, high E BB, WBB)

no established baselineTASD (NOvA-like)or Liquid Argon TPCor Megaton WC

photosensors and detectorslong drifts, long wires, LEMs

Neutrino Factory (20-50 GeV, 2500-7000km)

~100kton magnetized iron calorimeter (golden)

+ ~10 kton non-magnetic ECC (silver)

straightforward from MINOSsimulation+physics studiesibid vs OPERA


Executive summaryII. beyond the baseline, (but should be studied)

beam Far detector R&D neededsub-GeV BB and SB (MEMPHYS, T2K)

Liquid Argon TPC(100kton)

clarify what is the advantage wrt WC?

1-2 GeV BB and SB(off axis NUMI, high BB)

no established baseline


platinum detectors! large coil around TASD/Larg/ECC

engineering studyfor magnet!simulations and physics evaluation;photosensors, long drift, etc…


Executive summary: III: near detector, beam instrumentation

beam BI, ND R&D needed

sub-GeV BB and SB (MEMPHYS, T2K)

T2K example…. CONCEPT for precision measurements?

concept simulationstheory

1-2 GeV BB and SB(off axis NUMI, high g BB)

NOvA example.. CONCEPT for precision measurements?

ibid


beam intensity (BCT)beam energy +polarizationbeam divergence meastshieldingleptonic detectorhadronic detector

need study--need studyneed conceptsimul+studysimul+study+Vtx det R&D


Magnetized Iron calorimeter (baseline detector, Cervera, Nelson)

Baseline

3500 Km

732 Km 108

4 x 106

2 x 108

7.5 x 106

3.4 x 105

3 x 105

CC e CC signal (sin2 13=0.01)

Event rates for 1020 muon decays (<~1 year)

(J-PARC I SK = 40)

B = 1 T = 15 m, L = 25 mt(iron) =4cm, t(sc)=1-2cm Fiducial mass = 100 kTCharge discrimination down to 1 GeV200M$


New analysis (Cervera) OLD: P> 5 GeV

NEW: L > Lhad + 75cm

(shown for three different purity levels down to << 10-4 )

old analysis

new analysis

A. Blondel GDR neutrino 4 0ctobre 2006 Orsay Location of INOLocation of INO


INO Detector ConceptINO Detector Concept


Upgrade of the proton accelerator complex at CERNProtons Accelerators for the Future (PAF) WG

PSB SPL’RCPSB

SPSSPS+

Linac4

SPL

PS

LHC / SLHC DLHC

Out

put

ener

gy

160 MeV

1.4 GeV~ 5 GeV

26 GeV40 – 60 GeV

450 GeV1 TeV

7 TeV~ 14 TeV

Linac250 MeV

SPL: Superconducting Proton Linac (~ 5 GeV)

SPL’: RCPSB injector(0.16 to 0.4-1 GeV)

RCPSB: Rapid Cycling PSB(0.4-1 to ~ 5 GeV)

PS2: High Energy PS(~ 5 to 50 GeV – 0.3 Hz)

PS2+: Superconducting PS(~ 5 to 50 GeV – 0.3 Hz)

SPS+: Superconducting SPS(50 to1000 GeV)

SLHC: “Superluminosity” LHC(up to 1035 cm-2s-1)

DLHC: “Double energy” LHC(1 to ~14 TeV)

Proton flux / Beam power

PS2 (PS2+)

PSB SPL’RCPSB

SPSSPS+

Linac4

SPL

PS

LHC / SLHC DLHC

Out

put

ener

gy

160 MeV

1.4 GeV~ 5 GeV

26 GeV40 – 60 GeV

450 GeV1 TeV

7 TeV~ 14 TeV

Linac250 MeV










PS2 (PS2+)Present chain:

weak link in Linac 2and in the PS

(old!)


Priority is given to LHC but efforts should be made to incorporate the demands of the High intensity neutrino programme the cheapest way to LHC luminosity consolidation is to -- implement the LINAC 4 and replace the CERN PS

PSB SPL’RCPSB

SPSSPS+

Linac4

SPL

PS

LHC / SLHC DLHC

Out

put

ener

gy

160 MeV

1.4 GeV~ 5 GeV

26 GeV40 – 60 GeV

450 GeV1 TeV

7 TeV~ 14 TeV

Linac250 MeV










PS2 (PS2+)

PSB SPL’RCPSB

SPSSPS+

Linac4

SPL

PS

LHC / SLHC DLHC

Out

put

ener

gy

160 MeV

1.4 GeV~ 5 GeV

26 GeV40 – 60 GeV

450 GeV1 TeV

7 TeV~ 14 TeV

Linac250 MeV










PS2 (PS2+)

Step I: replace linac 2 by Linac 4

increase injection rate no major improvement

for neutrinos~2011


PSB SPL’RCPSB

SPSSPS+

Linac4

SPL

PS

LHC / SLHC DLHC

Out

put

ener

gy

160 MeV

1.4 GeV~ 5 GeV

26 GeV40 – 60 GeV

450 GeV1 TeV

7 TeV~ 14 TeV

Linac250 MeV










PS2 (PS2+)

PSB SPL’RCPSB

SPSSPS+

Linac4

SPL

PS

LHC / SLHC DLHC

Out

put

ener

gy

160 MeV

1.4 GeV~ 5 GeV

26 GeV40 – 60 GeV

450 GeV1 TeV

7 TeV~ 14 TeV

Linac250 MeV










PS2 (PS2+)

Step II:

new PS2 (5-50 GeV)PS remains in operationfor injectionat 5 GeV in PS2

possible increase of SPS intensity --> CNGS

~2015

Priority is given to LHC and efforts should be made to incorporate the demands of the High intensity neutrino programmethe cheapest way to LHC luminosity consolidation is to -- implement the LINAC 4 and replace the CERN PS


PSB SPL’RCPSB

SPSSPS+

Linac4

SPL

PS

LHC / SLHC DLHC

Out

put

ener

gy

160 MeV

1.4 GeV~ 5 GeV

26 GeV40 – 60 GeV

450 GeV1 TeV

7 TeV~ 14 TeV

Linac250 MeV










PS2 (PS2+)

PSB SPL’RCPSB

SPSSPS+

Linac4

SPL

PS

LHC / SLHC DLHC

Out

put

ener

gy

160 MeV

1.4 GeV~ 5 GeV

26 GeV40 – 60 GeV

450 GeV1 TeV

7 TeV~ 14 TeV

Linac250 MeV










PS2 (PS2+)

Step III:

New SPL (or RCS) to ~5 GeV

inject directly in PS2Multi-MW oportunity

@~5 GeVno date yet (i.e. a few more years)


e physics at CNGS+?

Basic issues to solve:

1. no near detector --> no knowledge of absolute cross sections(at osc. max there are no to normalize…) difficult to measure absolute rates of e and to compare vs or different energies for CP or matter effect

2. modifications of CNGS beam line are necessary. possible? perhaps easier to build new dk tunnel -- with adequate length and near detector. then why keep the same direction?

3. can SPS and targets really handle 4x more protons?

4. 100 kton Larg or 1Mton water are large investments -- may be they deserve better!


LINAC4--> PS2: an opportunity for MultiMW physics

Eventually the PS should be phased out completely: need for a machine that bridges 1.4 (booster) to 5 GeV, or better 0.16 Linac4 to 5 GeV (PS2)

Superconducting Proton Liac or Rapid Cycling Synchrotronboth fast cycling (O(10-50 Hz). potentially a high power machine serving -- LHC -- neutrinos -- nuclear physics (Eurisol)

for neutrino physics:conventional p decay superbeam proton driver for neutrino factory


300 MeV Neutrinos

small contamination from e (no K at 2 GeV!)

A large underground water Cherenkov (400 kton) UNO/HyperKor/and a large L.Arg detector. also : proton decay search, supernovae events solar and atmospheric neutrinos. Performance similar to J-PARC IIThere is a window of opportunity for digging the cavern starting in 2009 (safety tunnel in Frejus)

CERN-SPL-based Neutrino SUPERBEAM

Fréjus underground lab.

target!


Super-beams: SPL-Frejus

TRE

CERN SPLLSM-Fréjus

Near detector

130km


CERN: -beam baseline scenario

PS

Decay

RingISOL target & Ion source

SPL

Cyclotrons, linac or FFAG

Decay ring

B = 5 T

Lss = 2500 m

SPSECR

Rapid cycling synchrotron

Nuclear Physics

,

Same detectors as Superbeam !

target!

Stacking!

neutrinos of Emax=~600MeV

eFNe e189

1810

eLiHe e63

62


Eurisol baseline Study

CERN site (use PS and SPS as are) -- could benefit from PS2Max. ion in CERN SPS is 450 GeV Z/Mion

= 150 for 6He, = 250 for 18Ne ==> EeV

2.9*1018 /yr anti-e from 6He Or 1.1*1018 /yr e from 18Ne (1017 with avail. tech.)

race track (one baseline) or triangle (2 base lines) so far study CERN--> Fréjus (130km)

longer baseline ~ 2-300km would be optimal + moderate cost: ion sources, 450 GeV equiv. storage ring (O(0.5M€))+ no need for 4MW target

Emax

=2. Q0. ion


Combination of beta beam with super beam

combines CP and T violation tests

e (+) (T) e (+)

(CP)

e (-) (T) e (-)


J-E. Campagne et al. hep/ph0603172

combine SPL(3.5 GeV) + B==> improves sensitivity by T violation!

10 year exposure

issues:

-- 18Ne flux?-- low energy --> cross-section accuracy? (assume 2%) -- energy reconstruction OK-- near detector concept?

sensitivity sin2213 ~2-5 10-4

3 sensitivity to sin2213


Better beta beams:

main weakness of He/He beta-beam is low energy (450 GeV proton equiv. storage ring produces 600 MeV neutrinos)

Solution 1: Higher (Hernandez et al) Use SPS+ (1 TeV) or tevatron ==> reach expensive!

Solution 2: use higher Q isotopes (C.Rubbia)

8B --> 8Be e+ e

or 8Li --> 8Be e-

anti- e


A possible solution to the ion production shortage:

Direct production in a small storage ring, filled [Gas + RF cavity] for ionization cooling

For 8B or 8Li production, strip-inject 6Li / 7Li beam, collide with gas jet (D2 or 3He)

reaction products are ejected and collected

goal: >~ 1021 ions per year


Advantages of 8B5+ (e Q=18MeV ) or 8Li3+ (anti-e Q=16MeV)vs 18Ne, 6He (Q~=3 MeV)

The storage ring rigidity is considerably lower for a given E

==> for ~1 GeV end point beam for 8B5+ : 45 GeV proton equiv. storage ringfor 8Li3+: 75 GeV proton equiv. storage ring

Two ways to see it: 1. Beta-beams to Fréjus (Emax =600 MeV) could be accelerated with PS2 into a 50 GeV proton-equivalent storage ring (save €)2. Beta beams of both polarities up to end-point energy of ~6 GeV can be produced with the CERN SPS (up to 2000km baseline)

A new flurry of opportunities


EC: A monochromatic neutrino beam

Decay T1/2 BR EC/ ECI B(GT) EGR GR QEC E E

148Dy 148Tb* 3.1 m 1 0.96 0.96 0.46 620 2682 2062

150Dy 150Tb* 7.2 m 0.64 1 1 0.32 397 1794 1397

152Tm2- 152ET* 8.0 s 1 0.45 0.50 0.48 4300 520 8700 4400 520

150Ho2- 150Dy* 72 s 1 0.77 0.56 0.25 4400 400 7400 3000 400

Electron Capture: N+e- N’+e

rates are low but very useful for cross-section measurementsBurget et al

A. Blondel GDR neutrino 4 0ctobre 2006 Orsay SPSC 2004 Villars Alain Blondel, 24/09/04

-- Neutrino Factory --CERN layout

e+ e _

interacts

giving

oscillates e interacts giving

WRONG SIGN MUON

1016p/s

1.2 1014 s =1.2 1021 yr

3 1020 eyr3 1020 yr

0.9 1021 yr

A. Blondel GDR neutrino 4 0ctobre 2006 Orsay NUFACT05 – highlights Alain Blondel CERN seminar 13/9/2005

NB: This works just as well

INO ~7000 km (Magic distance)


NON MAGNETIC

MAGNETIC

A. Blondel GDR neutrino 4 0ctobre 2006 Orsay Alain Blondel

NUFACT Accelerator baseline

40Beam durationb) (s)

2 ± 1Bunch length, rms (ns)

3,5a)No. of bunch trains

50Repetition rate (Hz)

4Beam power (MW)

10 ± 5Energy (GeV)

Valueproton driver parameter

a)Values ranging f rom 1–5 possibly acceptable.b)Maximum spill duration for liquid-metal target.

1021/ yr0.1/

decays per straightangular divergence

100ns trains of both signs of muons separated by

20GeV40GeV

stored muon energy upgradable to

yescooling

phase rotation and bunching

L Hg+ 20T solenoid

Target+capture

ValueNuFact Parameter

RF

Goals achieved!

NEUTRINO FACTORY -- paradoxically quite mature option. ISS (International Scoping Study) revisited accelerator and detector options in 2005-2006.


Overall comparisons from ISS (nearly final plots)

sign m2

CP phase

NuFACT does it all…(+ univ. test etc…)but when can it do it and at what cost?


SYSTEMATICS - related topics


[2700-3600 ] [1800-2700 ]

NB: 3sigma = 60 means that +-1 sigma = +-3.50


for NUFACT:

work on systematic errors on matter effect

A preliminary study was made by

E. Kozlovskaya, J. Peltoniemi, J. Sarkamo,

The density distribution in the Earth along the CERN-Pyhäsalmi baseline and its effect on neutrino oscillations. CUPP-07/2003

the uncertainties on matter effects are at the level of a few%

J. Peltoniemi


Errors in density

1.5%1.8%Oceanic 9000 km

1.7%2.0%Continental 9000 km

1.7%2.6%Oceanic 2500 km

2.9%4.7%Continental 2500 km

“best”“a priori”location length

Errors are ~2 sigma(errors not really Gaussian)

Recommendations

Avoid:

• Alps

• central Europe

• thick crust (e.g. Fenoscandia)

• Europe to Japan

Recommendations

Best profiles:

• Western Europe to Eastern US

• Atlantic Islands (Canaries, Maderia, Azores) to Portugal, western Spain, NW France, southern Ireland, western England

Such a study, in collaboration with geophysicistswill be needed for candidate LBL sites

ISS-3 at RAL Warner


near detector constraints for CP violation

= ACP sin2 solar term…

sinsin (m212 L/4E) sin sin P(e) - P(e)

P(e) + P(e)

Near detector gives e diff. cross-section*detection-eff *flux and ibid for bkg

BUT: need to know and diff. cross-section* detection-eff

with small (relative) systematic errors.

knowledge of cross-sections (relative to each-other) required knowledge of flux!

interchange role of e and for superbeam

ex. beta-beam or nufact:


Bsig

need to know this:

sig

e

sig

sig

e

sig

/

/

experimental signal= signal cross-section X efficiency of selection + Background

and of course the fluxes… but the product flux*sig is measured in the near detector

this is not a totally trivial quantity as there is somethig particular in each of these cross-sections:

for instance the effects of muon mass as well as nuclear effects are different for neutrinos and anti-neutrinos

while e.g. pion threshold is different for muon and electron neutrinos


3.5 GeV SPL

beam

-- low proton energy: no Kaons e background is low--region below pion threshold (low bkg from pions)

but:low event rate and uncertainties on cross-sections


Uncertainties in the double ratio (Sobczyk at RAL meeting)

1. problem comes from compound of Fermi motion and binding energy with the muon mass effect.

)(

)(,

)(

)(

ee

RR

the double ratio calculation is very insensitive to variations of parameters … but


)(

)()(

)(

e

eDR

at 250 MeV (first maximum in Frejus expt) prediction varies from 0.88 to 0.94according to nuclear model used. (= +- 0.03?)

Hope to improve results with e.g. monochromatic k-capture beam


EP2010:

« pursue an internationally coordinated, staged program in neutrino physics »

CERN-SG: Studies of the scientific case for future neutrino facilities and the R&D into associated technologies are required tobe in a position to define the optimal neutrino programme

based on the information available in around 2012;Council will play an active role in promoting a coordinated Europeanparticipation in a global neutrino programme.

Towards a high-intensity neutrino programme


Conclusions

CERN priority to LHC makes it unlikely to raise a new neutrino programme until at least 2016. However opportunities are open by the upgrades of the LHC acclerator complex

-- upgrade of CNGS … tempting and politically attractive. but is it feasible? worth it given the time scales?

-- SPL would offer a powerful low energy beam-- beta-beam offers extremely clean e beam new ideas to improve flux/energy/cost…. -- baseline detector for sub-GeV neutrinos is WaterCherenkov-- in few GeV range, Larg, TASD etc… competitive -- near detector and monitoring systems should not be forgotten


-- neutrino factory still the ultimate contender, especially if 13

is very small. Requires magnetic detectors

-- design studies of Superbeam/betabeams/ NuFact and of the associated detector systems will be necessary for a choicearound 2010/2012; organization ongoing.

Conclusions (ctd)


2010 will be a time of major decisions in particle physics

•LHC will be completed first results will appear

•I LC GDE

•I t is crucial that infrastructure needed for future neutrino expts be on the map

=> although 2012 is the eventual target date we should be sure to have interim reportsby 2010.

TARGET DATE I 2010

Barry Barish, CERN SPC sept05

ILC


Regional Oversight Committees

Nufact study

Accelerator

Detectors

Physics

Betabeam study

Accelerator

Detectors

Physics

Superbeam study(or studies)

Accelerator

Detectors

Physics

Neutrino Oscillation Physics Working Group

-- exact structure of each study to be decided by proponents

-- Regional Oversight Committees will possibly converge to a single international committee for a future precision neutrino facility


I SS- - > I DS aspirational time line:

ISS report: end of 2006will include a description of the R&D and ressources necessary to produce I nterimDesignReport in 2010 and CDR in 2012

Next « ISS » meeting second half of february 2007 19- 21 feb @ CERN

2006- 2007 preparation of funding proposals

Review of where we stand at NUFACT07

mid- 2008 (NUFACT08) funded engineering phase begins

2010 IDS interim report

2012 CDR

Meanwhile a European Oversight Committee should be put in place to coordinateneutrino- beam requests.


FP7 design studies under ESGARD

Design studies : ~2M€ each mostly calculation or engineering work (personnel)3 years?

SLHCNUFACT+SuperBeam SC-SPS -beam

call: february 2007 --> application likely in sept. 1st 2007

funding mid 2008?


Integrated Activities - IA ~10 M€, (also called Integrated Infrastructure Initiatives - I3)Joint Research Activities , Network Activities, Trans-national access

HE-HIProtons

SC RF New acceleration techniques

M-MW p driver

Target & Collection

M.MW p driver& muon RLA (200-800 MHz)power sources

(CLIC)(sLHC,DLHC) (ILC)

Muon cooling

FFAG

Call expected not earlier than April 07


to this, a design study of magnetic detectors (neutrino factory) should be added.

100kton magnetized iron detectormagnetized Liquid Argon, Fine grain scintillator or Emulsion detector

+ near detector and instrumentation


7.Test Beam Facility for Neutrino 7.Test Beam Facility for Neutrino Detector R&DDetector R&D Request test beam in East Area at the CERN PS, with a fixed dipole magnet for dedicated Neutrino Detector R&D

Liquid Argon tests, beam telescopes for

silicon pixel and SciFi tests, calorimetry …

Neutrino detector test facility: community resource forneutrino detector R&D


8. Total Neutrino Detector R&D 8. Total Neutrino Detector R&D ProgrammeProgramme

Estimated total funds needed to take forward R&D plans

Some fraction of these funds(~30-50%) to be requested from EU

Water Cherenkov R&D in different bid


Agenda

20 septembre BENE steering group25 octobre OPEN BENE steering group at CERN 30 October at CERN meeting of the CARE task force to define JRAs 14 november BENE0615-17 november CARE06

February 26-28 ISS-IDS meeting @ CERN


Intensity increase to CNGS?

can one launch an off axis programme similar to T2K and NUMI-off-axis?

-- present neutrino beam optimized for High energy (tau appearance) ==> factor >~10 less flux at off axis energy than T2K-- no near detector!

A.Rubbia et al, A. Ball et al, have proposed a low energy version of CNGS with different target and more compact optics,run off axis (E

~800 MeV for C2GT, 1.5-2 GeV GeV for Larg

A. Ball et al(C2GT) CERN-PH-EP-2006-002A. Rubbia, P. Sala JHEP 0209 (2002) 004[arXiv:hep-ph/0207084].A. Meregaglia and A. Rubbia hep-ph/0609106


target and horn

1.5 Mton of water in the Golf of Taranto for 25 1019 pot = 5yrs

C2GT off axis2d maximum

detectormodule

--> sensitivity (90%) to sin213= 0.0076


hep-ph/0609106 Imagine: 100 kton Larg detectorat 0.750 off-axis 850 km (1st max) --> search

or 1.50 off-axis 1050 km 2d maxCP violation and matter effect

or sharing 1st and 2d maximum

assume all of 50 GeV 200 kW PS2 accelerated to 400 GeV==> CNGS+ = 30 1019 pot/year

<-- sensitivity sin 2213 ~ 10-3

(2026)

5years 5 years


thanks to and running, sensitivity to and matter effects

example (90%)for‘known hierarchy’(assume that hierarchy is given by comparison with another expt)


SPL (2.2 GeV) superbeam 20m decay tunnelsingle open horn, L Hg target

Low energy --> low Kaon ratebetter controlled e

contamination


2 years run to 440 ktonFrejusEMeVsmall cross-sectionslimited sensitivity( sin 2213 ~ 210-3)

near detector design?

Main technical issues-- 50 Hz horn operation-- handling of 4 MW in target and environment.

Highlights of ISS and nufact 1. ISS 2. achieved goals 2.1 investigation of neutrino detectors

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Transcript of Highlights of ISS and nufact 1. ISS 2. achieved goals 2.1 investigation of neutrino detectors