Physics and Technology at a Neutrino Factory Seminar University of Bonn 18 May 2006 Paul Soler...

Physics and Technology at a Neutrino Physics and Technology at a Neutrino FactoryFactory

Physics and Technology at a Neutrino Physics and Technology at a Neutrino FactoryFactory

SeminarUniversity of Bonn

18 May 2006Paul Soler

University of Glasgow

Seminar, University of Bonn. 18 May 2006

2

ContentsContents

1. Neutrino Standard Model2. Neutrino Oscillations3. Atmospheric neutrinos4. Solar neutrinos5. Three neutrino oscilllations6. Future neutrino experiments7. Physics Reach of a Neutrino Factory8. Neutrino Factory Design9. Far Detectors at a Neutrino Factory10.Near Detector at a Neutrino Factory11.NOMAD-STAR, a near detector prototype12.Near detector ideas

Thank you to many colleagues for letting me “borrow” their slides!


3

1. Neutrino Standard Model1. Neutrino Standard Model

HiggsHiggsBosonBosonHiggsHiggsBoson?Boson?

For

ceF

o rce

Car

rier

sC

arr i

ers

ZZ boson

WW boson

photon

ggluon

Generations of Generations of matter matter

tau

-neutrino

bbottom

ttop

III III

muon

-neutrino

sstrange

ccharm

II II

eelectron

ee-neutrino

ddown

upu

I I

Lep

tons

L

epto

ns

Qua

rks

Qua

rks

6 quark masses– mu , mc, mt

– md, ms, mb

3 lepton masses– me, m, m

– me, m

, m = 0

2 vector boson masses

– Mw, MZ (m, mg=0) 1 Higgs mass

– Mh

3 coupling constants– GF, , s

3 quark mixing angles– 12, 23, 13

1 quark phase–

Three neutrinos are massless no mixing, no right handed


4

2. Neutrino Oscillations2. Neutrino Oscillations If neutrinos have mass, they can mix like quarks 2 flavours ( & ) ; 2 mass eigenstates (i & j)

2

1

cossin-

sincos

seigenstate Mass seigenstateFlavour

ELmP 4sin)2(sin)(

21222

Neutrino oscillations


5

3. Atmospheric Neutrinos3. Atmospheric Neutrinos

ee

ee

)3(2)(

)(GeVE

e

Atmospheric neutrinos: neutrino production from cosmic rays in atmosphere Protons hit atmosphere: pions produced that decay (on average) into 2 muon

neutrinos for each electron neutrino produced in an interaction


6

3. Atmospheric Neutrinos3. Atmospheric Neutrinos Super-Kamiokande experiment: 50,000 tons of water, surrounded by

11,000 phototubes to detect Cherenkov light in the water.


7



8


Super-Kamiokande zenith angle distributions:

Upward-going neutrinos depleted, while upward-going electron neutrinos slightly higher than expected: proof of neutrino oscillations!


9

3. Atmospheric Neutrinos3. Atmospheric Neutrinos Super-Kamiokande L/E: Oscillation parameters

Most likely transition: -> oscillations

1)2(sin45 2

239.16.0

223 101.2 eVm


10

3. Confirmation Atmospheric Neutrinos3. Confirmation Atmospheric Neutrinos K2K: 12 GeV proton synchrotron at KEK to Kamioka mine (Japan). L=250 km,

<E>=1.4 GeV. Running. Observed: 108 events in Super-K

Expected (no oscillation): 150.9+11.6-10.0

Probability no

oscillation < 1%

K2K Front Detector

Compatible with

Super-K

atmospheric

Oscillation

parameters.

Best fit:

104.8 events


11

3. Confirmation Atmospheric Neutrinos3. Confirmation Atmospheric Neutrinos Long baseline accelerator experiments: confirms atmospheric results

+ MINOS: neutrinos from Main Injector (NuMI) at Fermilab to Soudan (Minnesotta). L=730 km, <E>=16 GeV. Started running January 2005

disappearance confirms atmospheric result. Next step: e appearance experiment


12

4. Solar Neutrinos4. Solar Neutrinos Standard Solar Model: 4 hydrogen

atoms burn in thermo-nuclear reactions to produce helium, neutrinos and energy:

Measured photon luminosity is: 3.9x1026 J s-1.Energy per reaction = 26.7 MeV= 4.3x10-12 JNumber of reactions = 3.9x1026/4.3x10-12 = 9.1x1037 s-1

Distance sun-earth = 1.5x1013 cm.

)7.26(224 4 MeVeHep e

2110213

37

2104.6

)105.1(4

101.92

4

cmsR

NneutrinosofFlux e

(64 billion neutrinos per second in 1 cm2 !!!!)


13

4. Solar Neutrinos4. Solar Neutrinos pp cycle: 98.5% of the total sun’s power

comes from these reactions CNO cycle: catalysed by C, N and O only

produces 1.5% of power output Low energy (<0.42 MeV) pp reaction (flux

6.0x1010 cm-2 s-1) most abundant 8B neutrinos (<14 MeV): only 10-4 total


14

4. Solar Neutrinos4. Solar Neutrinos Ray Davis’ Chlorine experiment inside Homestake mine in Lead, South Dakota:

100,000 gallons (615 tons) cleaning fluid (C2Cl4) eArCle3737

Expect about 1.5 Ar atoms/day

3737eeClAr

Extract Ar and count in proportional counter:

2.82 keV K-shell x-rays

Observation about 1/3 the expected number of solar neutrinos


15

4. Solar Neutrinos4. Solar Neutrinos Results Super-Kamiokande experiment:

– Proof that neutrinos come from sun: angular correlation

– Neutrino flux is 46.5% that expected from the solar model

Confirmation Solar NeutrinoPuzzle!


16

4. Solar Neutrinos4. Solar Neutrinos Sudbury Neutrino Observatory (Sudbury, Ontario, Canada).

1000 tonnes D2O, 6500 tonnes H2O, 10,000 PMTs

Acrylic Vessel

104 8” PMTs

Phototube SupportStructure (PSUP)

6500 tonnes H2O

Surface: 2 km1000 tonnes D2O


17

4. Solar Neutrinos4. Solar Neutrinos First results with D2O:

– Charged current (CC):– Elastic scattering (ES):– Neutral current (NC):

CC 1967.7 +61.9 +60.9

+26.4 +25.6ES 263.6 +49.5 +48.9NC 576.5#E

VE

NT

S

eppde ee xx

xx pnd

About 35% electron neutrinosmake it to earth (from CC) but flux of all neutrino species (fromNC and ES) as expected:

(0.35+-0.02 SSM)

Neutrinos change species in flight: Neutrino Oscillations!

(1.01+-0.12 SSM)

(Threshold>2.225 keV)

(Threshold>1.442 keV)


18

4. Solar Neutrinos4. Solar Neutrinos

All results consistent with oscillations:

+ e CC rate is 0.31 SSM

+ ES rate consistent with Super-Kamioka

+ NC rate (all ) as expected Neutral currents detected

through neutron capture on 35Cl (increases NC sensitivity)

12610.011.0 1059.1

scmFluxCC

12633.028.0 1021.2

scmFluxES

1261047.021.5 scmFluxNC

036.0306.0

/

NCCC

CC 1339.6 +63.8 +61.5

+23.9 +20.1ES 170.3 +69.8 +69.0NC 1344.2

Confirmation of results with with salt data:


19

4. Solar Neutrinos4. Solar Neutrinos Global picture of solar neutrinos after

SNO results: Large Mixing Angle (LMA) solution of

neutrino oscillationse

Interpretation solar neutrino results: MSW resonant neutrino oscillations in the sun

Before SNO After SNO

4.25.32 e25222

12 101.7 eVmmmevv


20

4. Confirmation Solar Neutrinos4. Confirmation Solar Neutrinos KAMLAND reactor experiment in Kamioka

mine (Japan) confirms Large Mixing Angle (LMA) solution of solar neutrino problem.

- Observed/Expected= 0.611+-0.085+-0.041- Average distance (L) to reactors 175+-35 km


21

4. Confirmation Solar Neutrinos4. Confirmation Solar Neutrinos Spectral distortions in KAMLAND: no distortions fit 0.4% CL- Best fit to:

- Therefore:1.3446.0tan 12

10.007.012

2 256.0

5.0212 109.7 eVm

E

LmP ee 4

sin2sin1cos)(2122

122

134

Independent confirmation of solarNeutrino oscillation parameters!


22

5. Three Neutrino Oscillations5. Three Neutrino Oscillations

Neutrino oscillations well established!! CHOOZ reactor experiment (France) set limits on disappearance : <E>~6MeV, L~1km

Three neutrino flavour mixing: Pontecorvo-Maki-Nakagawa-Sakata (PMNS) matrix

Similar mixing matrix to CKM matrix

3

2

1

U

e

ijijijij sandcwhere

cs

sc

iδecs

sccs

sc

U

sin,cos

0

010

0

00

010

001

0

0

001

100

0

0

1313

1313

2323

23231212

1212

)%90(1.02sin)%90(05.0)( 132 CLCLP

i

iiU where ,,e and 3,2,1iMixing of states:


23

5. Three Neutrino Oscillations5. Three Neutrino Oscillations

Oscillations, if not negligible:212m

xE

mx

E

mx

E

mJ

xE

mcx

E

msxP

ee

4sin

44cos

~

4sin2sin

4sin2sin)(

213

212

213

2122

1222

23

2132

1322

23)(

where is for ,

13231213 2sin2sin2sin~ cJ (Jarlskog coefficient for CP violation)

13≠0

Oscillations of three neutrino families, if: 223

213

223

212 , mmmm

with

x

E

msxP

ee 4sin2sin)(

2232

1322

23)(

x

E

mcxP

ee 4sin2sin)(

2232

1322

23)(

x

E

mcxP

4sin2sin)(

2232

2324

13)(

ijijc cosijijs sin


24

5. Neutrino oscillation global fits5. Neutrino oscillation global fits

Consistent picture emerging Global fit provides 23, 12, m12

2 and m232

13 not known, mass hierarchy not known,CP violation phase not known!!


25

6. Future Neutrino Experiments6. Future Neutrino Experiments First, need to determine13: possibly using neutrino “super-beams”

Do ->e oscillations and fit sub-leading oscillations sin213 to:

Decay Pipe

Target

Horns

Detector

x

E

msxP

ee 4sin2sin)(

2232

1322

23)(

Off-axis: narrower energy band:

cos2

22

pE

mmE

Possible super-beams: 1-4 MW proton intensity to generate beam of neutrinos. Off-axis for better determination neutrino energy. For example: MINOS off-axis (~700 km) or Japanese T2K (Tokai to SuperK, ~250 km)


26

6. Future Neutrino Experiments6. Future Neutrino Experiments Japanese JPARC (Tokai) Hadron Facility: T2K (Tokai to SuperK, ~295 km)

.).%90(10sin 213

2 LCatDiscovery of e appearance: 13 & m2

13


27

6. Search for 6. Search for 1313 and CP Violation and CP Violation For CP violation need to compare with Make CP asymmetry parameter:

Three neutrino oscillations in matter (through earth): mass heirarchy and CP phase accessible due to

)( eP )( eP

)()(

)()(

ee

eeCP PP

PPA

BB

xB

xE

A

EB

m

A

mx

E

mJ

xE

A

A

mcx

B

EB

msxP

ee

2sin

4sin

24cos

~

4sin2sin

2sin

22sin)(

213

212

213

2212

1222

232

213

1322

23)(

1324

13

2

13213 2sin2cos

2

1 mAmE

Bwith where is for ,


28

7. Physics Reach of a Neutrino Factory7. Physics Reach of a Neutrino Factory Matter-antimatter asymmetry

of the universe: baryogenesis (CP violation in quark sector), leptogenesis (CP violation in lepton sector)

e

e

e

e

Conceptual design: neutrinos produced from muon decay in storage ring. Rate calculable by kinematics of decay (Michel spectrum)

Neutrino factory: very long baseline oscillation experiments to measure 13, mass hierarchy and leptonic CP violation


29

7. Physics Reach of a Neutrino Factory7. Physics Reach of a Neutrino Factory

ee

Disappearance Appearance eee

e

e

ee

Far detector (3000-7000 km) can search for “wrong-sign” muons in appearance mode (gold channel), disappearance of “right-sign” leptons, either e or and possible appearance of (silver channel)

Can detect sign of m232 due to matter effects and determine CP violating

phase if it is large enough.

Gold channel

Silver channel

Platinum channel

Silver channel


30

7. Physics Reach of a Neutrino Factory7. Physics Reach of a Neutrino Factory Far detector (3000-7000 km) can

search for “wrong-sign” muons in appearance mode (for example, Large Magnetic Detector)

Background: charm production, charge misidentification.

Qt = P sin2 cut eliminates backg at 10-6

Large Magnetic Detector

iron (4 cm) + scintillators (1cm)

beam20 m

20 m

B=1 T

40KT40KT

e

e

50%

50%

wrongwrongsignsign

muonmuon

e

detectordetector

not detected

De

e

De e

NC

CC

Hadron decay

Other Detectors: liquid argon TPC, water Cherenkov, emulsion can search for either e, or appearance


31

7. Physics Reach of a Neutrino Factory7. Physics Reach of a Neutrino Factory Determine 13 and CP phase simultaneously: need ~1021 muons/year Optimal CP phase sensitivity ~6000 km but

can obtain >5 sensitivity for ~1000-8000 km


32

7. Physics Reach of a Neutrino Factory7. Physics Reach of a Neutrino Factory

P. Huber et al.2006


33

8. Neutrino Factory Design8. Neutrino Factory Design

Proton Driver

– primary beam on production target Target, Capture, Decay

– create , decay into Bunching, Phase Rotation

– reduce E of bunch Cooling

– reduce transverse emittance Acceleration

– 130 MeV 20-50 GeV Decay Ring

– store for ~500 turns; long straight section

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

Optimization in progress at International Scoping Study: report Autumn 2006


34

8. Neutrino Factory Design8. Neutrino Factory Design 1. Proton Drivers Technology depends on host laboratory: JPARC, Brookhaven, Fermilab, CERN, RAL

In Japan: upgrade of JPARC to 4 MW

Brookhaven: AGS upgrade

201.25 MHz DTL

BOOSTER

High Intensity Sourceplus RFQ

800 MHz Superconducting Linac

To RHIC

400 MeV

116 MeV

1.5 GeV

To Target Station

AGS1.5 GeV - 28 GeV

0.4 s cycle time (2.5 Hz)

0.2 s 0.2 s

805 MHz CCL

Fermilab: 8 GeV superconducting LINAC

~ 700m Active Length8 GeV Linac8 GeV

neutrino

MainInjector

@2 MW

SY-120Fixed-Target

Neutrino

“Super- Beams”

NUMI

Off-

Axis


35


At RAL: 5-30 GeV synchrotrons

At CERN, Superconducting Proton LINAC (SPL): 3.5 GeV

H-

RFQ RFQ1 chop. RFQ2DTL-CCDTL-SCL 0.65 0.8 1

dump

Source Front End Normal Conducting Superconducting

95 keV 3 MeV 180 MeV 3.5 GeV

40MeV 90MeV

10 m 83 m ~ 350 m

Stretching andcollimation line

3.5 GeV to PS &Accumulator Ring(Neutrino Facility)

Debunching

400 MeV

chopp.

LINAC 4

352 MHz 704 MHz

900 MeV

1

1 - 2 GeV toEURISOL

SPL CDR2 Preliminary Layout 15.3.2005Work in progress!

1. Proton Drivers


36


Probably optimum energy is between 5 and 15 GeV

Need hadron production data (HARP experiment at CERN) to verify models on which prediction is based.


37

8. Neutrino Factory Design8. Neutrino Factory Design HARP at CERN: Pion production yields from protons on different targets to optimize neutrino factory energies Proton energies: 2-15 GeV First results on Al target (<210 mrad) Useful for K2K expt.

Pion production


38

8. Neutrino Factory Design8. Neutrino Factory Design 2. Target, capture, decay

Carbon (solid) targets can withstand up to 1 MW beams

Above 1 MW need to do something different: Hg jets in 20 T solenoid field for pion capture

MERIT experiment at CERN: Hg in 20 T solenoid field

MARS simulations indicate 10 GeV protons on Hg seem to provide best pion yield


39

8. Neutrino Factory Design8. Neutrino Factory Design 3. Bunching, phase rotation

Preferred RF cavities:

Bunching and phase rotation: bunch width 2 ns

Phase rotation achieves monochromatic beam of pions


40

8. Neutrino Factory Design8. Neutrino Factory Design 4. Muon ionization cooling: needed to achieve 1021 /yr

Principle Practice Study II

~ 20% cost of neutrino factory


41

8. Neutrino Factory Design8. Neutrino Factory Design Muon Ionization Cooling Experiment (MICE) at RAL: demonstration experiment of ionization cooling


42


5. AccelerationFixed Field Alternating Gradient (FFAG)

developments in Japan


43

8. Neutrino Factory Design8. Neutrino Factory Design 6. Decay rings:

148(133)

solid/liquid

80 μ+

80 μ+

80 μ+

80 μ+

80 μ+

127(!30)

127(130)

127(130)

127(130)

2 of 5 interleaved 80 μˉ

bunch trains of 2nd ring

80 full and 127 (or 130) empty RF buckets

> 100ns intervals


44

9. Far Detector Designs9. Far Detector Designs

Baseline option: wrong signmuon golden channel

Large Magnetic Iron Detectoro 40-100 ktono B field ~1 To Transverse resolution ~1 cmo Readout: scintillator (liquid or solid) or RPC

Optimised for small 13 Strong cut on muon momentum > 5 GeV/cProblems below muon momentum < 3 GeV/c (cannot see second maximum)

iron (4 cm) scintillators (1cm)

beam

20 m

10 m

10 m

B=1 T

1cm transverse resolution


45

9. Far Detector Designs9. Far Detector Designs Attempting optimisation of segmented magnetic detector:

o Iron free regions: improve momentum and charge determinationIron (4cm) + active Iron (4cm) + active (1cm) (1cm)

air + active (1cm)air + active (1cm)

hadron showerhadron shower muonmuon

1m

o Combining iron-free regions with liquid scintillator to improve electron ID and to reduce momentum threshold.

? Iron (2cm) + active Iron (2cm) + active (4cm) (4cm)

air + active (1cm)air + active (1cm)

hadron showerhadron showermuonmuon

Liquid scintillator

iron


46

9. Far Detector Designs9. Far Detector DesignsVery large liquid argon detectors:

FLARE in USA

R&D very challenging and very difficult to put a magnetic field around it.

100 kton detector with double phase readout: 20 m drift

HV

S igna l Liq. Ar

Cathode (- 2 MV)

Extraction grid

Charge readout plane

Scint. (UV) and Č light readout by

PMTs

E ≈ 3 kV/cm

Electronics racks

Field shaping electrodes

E ≈

1 k

V/c

m

Gas Ar

p ≈ 3 atm

p < 0.1 atm

20 m

dri

ft

GLACIER in Europe


47

9. Far Detector Designs9. Far Detector Designs

High precision tracking (x<1m, <1mrad): kink decay for identification a la OPERA

Emulsion walls in between iron-scintillator magnetic detectors for tau ID?

Electronic det:e/ separator

&“Time stamp”

Rohacell® plateemulsion filmstainless steel plate

spectrometertarget shower absorber

Emulsion detectors:

8.3kg

10 X0

1 brick:10.2x12.7x7.5 cm57 Em. Plates + 2CS56 Pb (1 mm)


48

10. Near Detector at a Neutrino Factory10. Near Detector at a Neutrino Factory To achieve physics goals of neutrino factory, need to establish near

detector for near/far ratio. Long baseline neutrino oscillation systematics:

– Flux control and measurement for the long baseline search.– Neutrino beam angle and divergence– Beam energy and spread– Control of muon polarization– Measurement of charm backgrounds

Near detector neutrino physics:– Cross-section measurements: DIS, QES, RES scattering– sin2W - sin2W ~ 0.0001– Parton Distribution Functions, nuclear shadowing S from xF3 - S~0.003 _– Charm production: |Vcd| and |Vcs|, D0/ D0 mixing– Polarised structure functions– polarization– Beyond SM searches General Purpose Detector(s)!!


49

10. Near Detector at a Neutrino Factory10. Near Detector at a Neutrino Factory Near detector(s) are some distance (d~30-1000 m)

from the end of straight section of the muon storage ring. Muons decay at different points of straight section: near detector is

sampling a different distribution of neutrinos to what is being seen by the far detector

storage ring

shielding

the leptonic detector

the charm and DIS detector

Polarimeter

Cherenkov d

Different far detector baselines:+ 730-7500 km, 20 m detector: ~30-3 rad

If decay straight is L=100m and d =30 m, at 8 rad, lateral displacement of neutrinos is 0.25-1.0mm to subtend same angle.


50

10. Near Detector Aims10. Near Detector Aims

e

e

e

e

Neutrino beams from decay of muons:

Spectra at d=30 m

Number CC interactions

Polarisation dependence

P=+1: gone!

Need to measure polarization!!

E.g. With 50 kg 109 interactions/yr

Need high granularity


51

mixing: doubly Cabbibo suppressedSM very small, new physics

10. Near Detector Measurements 10. Near Detector Measurements

Charm mesons produced: Charm is background for oscillation signal Measure of Vcd and strange quark content nucleon

Measure charm vs pt (background to oscillations) 6-7% of cross-section at 20 GeV3% CC events:

about 30 million charm states per year

...,,,, 00 csDDDD

McFarland

00 DD

Charm production:


52

10. Near Detector Measurements 10. Near Detector Measurements

Measurement cross-sections Measurement flux Other physics:

— Structure functions— S from xF3 - S~0.003

— QCD sum rules— sin2W

— polarization: spin transfer from

quarks to

Other physics:


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High granularity in inner region that subtends to far detector. Very good spatial resolution: charm detection Low Z, large Xo Electron ID Does the detector have to be of same/similar technology as far detector?

11. NOMAD-STAR: 11. NOMAD-STAR: near detector prototypenear detector prototype

Does not need to be very big (eg. R~50-100 cm)

Possibilities:— silicon vertex detector in a

magnet with calorimetry, electron and muon ID

(eg. NOMAD-STAR??)— Liquid argon calorimeter:

problems with rate

NOMAD-STAR (Silicon TARget)


54

11. NOMAD-STAR11. NOMAD-STAR R&D in NOMAD for short baseline detector based on silicon:

NOMAD-STAR (NIMA 413 (1998), 17; NIMA 419 (1998), 1; NIMA 486 (2002), 639; NIMA 506 (2003), 217.)

Total mass: 45 kg of B4C target (largest density for lowest X0)


55

Aim of NOMAD-STAR: reconstruct short lived particles in a neutrino beam

to determine capabilities detection: use impact parameter signature of charm decays to mimic

impact parameter ~ 62 m, normal charged current (CC) interactions ~30 m

signal very similar to charm signal

11. NOMAD-STAR11. NOMAD-STAR


56

Longest silicon microstrip detector ladders ever built: 72cm, 12 detectors, S/N=16:1

Detectors: Hamamatsu FOXFET p+ on n, 33.5x59.9 mm2, 300 m thick, 25 m pitch, 50 m readout

VA1 readout: 3 s shaping



57

CC event

Primary vertex

Secondary vertex



58

Increase noise in some ladders affected some efficiencies: compensated by clustering algorithm with cuts as function of ladder


Noise(e-)

1500

2500


59

Vertex resolution: y = 19 m Impact parameter resolution: 33 m

Double vertex resolution: 18 m from Ks reconstruction

Pull:~1.02

x~33 m


x~18 m z~280 m


60

Charm event selection:


Efficiency very low: 3.5% for D0, D+ and 12.7% for Ds

+ detection because fiducial volume very small (72cmx36cmx15cm), only 5 layers and only one projection.

From 109 CC events/yr, about 3.1x106 charm events, but efficiencies can be improved.


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Passive target can provide target mass, but affects vertex and tracking reconstruction efficiency due to scatters

Improve efficiency by having 2D space point measurement and more silicon planes.

For example: 52 kg mass can be provided by 18 layers of Si 500 m thick, 50 x 50 cm2 (ie. 4.5 m2 Si) and 15 layers of B4C, 5 mm thick

Optimal design: fully pixelated detector (could benefit from Linear Collider developments in MAPS, DEPFET or Column Parallel CCD). With pixel size: 50 m x 400 m 200 M pixels, ~0.4 X0

Could also use 3D detectors or double sided silicon strips (with long ladders of 50 cm x 50 m 360 k pixels).

International Scoping Study (ISS) for a neutrino factory (July 2005 to August 2006): aim to define the scope of physics parameters, neutrino factory machine technology and detector technology needed to launch a full design study 2007-2010. Near and far detector technologies are being considered.

Opportunity for another application of DEPFET detectors

12. Near Detector Ideas 12. Near Detector Ideas


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Conclusions The present series of neutrino experiments measure solar and

atmospheric neutrino parameters

The next series of experiments (off-axis) will aim to measure 13 and will provide a first attempt at measuring leptonic CP violation

The neutrino factory is the ultimate tool for the study of neutrino properties.

The Neutrino Factory International Scoping Study is defining the physics programme and is performing a first attempt at optimising the parameters for the machine in conjunction with the detectors.

An intense R&D programme is being carried out in the key technologies needed for a neutrino factory.

There exists a baseline far detector consisting of a segmented magnetic detector to measure the wrong-sign muon signal.

A near detector needs to measure the charm background for the far detector, and it should include a silicon vertex detector to identify charm candidates.

Neutrino factories offer a varied and exciting physics programme. We should aim to build one before the end of the next decade.

Physics and Technology at a Neutrino Factory Seminar University of Bonn 18 May 2006 Paul Soler...

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