Physics Working Group INTERNATIONAL NEUTRINO FACTORY AND SUPERBEAM SCOPING STUDY MEETING

Y.Nagashima, ISS060427

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Physics Working GroupINTERNATIONAL NEUTRINO FACTORY AND SUPERBEAM

SCOPING STUDY MEETINGRAL – 25 April, 2006

Y. NagashimaOSAKA UNIVERSITY

Status, prospects andwhat to do here

Acknowledgements: Grateful to all ISS speakers from whom I have taken material.


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Council members EU: P. Hernandez, S.King, M. Lindner, K. Long (deputy chair), M. Mezzetto US: D.Harris , W.Marciano, L. Roberts, H.MurayamaAsia: Y.Nagashima (chair), K. Nakamura, O. Yasuda

Four subgroups 　 and conveners• Theoretical : S. King• Phenomenological: O. Yasuda• Experimental: K. Long• Muon: L. Roberts (added after CERN meeting)


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This presentation is a summary of KEK and Boston meetings

Plenary meetings to date: CERN: 22 – 24 September, 2005 KEK: 23 – 26 January, 2006

Work shops: (Physics)London: 14 – 21 November, 2005Boston: 6-10 March, 2006

+ Phone meetings ~bi weekly


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Mission: Theory SubroupEstablish the neutrino physics case

• Robust arguments for peers• ‘Elevator pitch’ for decision makers

H.Murayama

If you happen to be on an elevator with a powerful senator, can you explain why you want to spend ~B$ on your project in 30 seconds ?


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H.Murayama

Many of these questions usually reside in GUT scale and beyond,


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It is very difficult to establish a one-to-one correspondence between GUT scale predictions and low energy observables.A given model, however, usually has generic predictions for low energy observables.Therefore studying neutrinos allows to gain considerable insight into phenomena which otherwise would be in accessible.Colliders can not probe this kind of physics, since any effects in scattering amplitudes are suppressed by MGUT, ~O(10-10) at LHC !

S.King, P.Huber


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•Connection with String theory (P.Langacker) Minimal see-saw unlikely. Motivates extended see-saw such as double see-saw and type II (triplet Higgs).

Top down approaches

•The Origin of Flavor

Can be tested experimentally Predicted by theory

S. KingL.Everett

E.ArgandaMore on SUSY


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Mass Hierarchy and small mixing in quarks and charged leptons suggests hidden symmetry . Symmetry broken by a VEV ~0.02 mu:mc:mt ~ md

2:ms2:mb

2

~ me2:m

2:m2 ~4: 2 : 1

Broken Flavor symmetry

Generation

Many neutrino models

H. Murayama

M.C.ChenMore on neutrino mass

Neutrino Different from quark sector ?


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* Quark-Lepton Complementarity: Minakata : A.Smirnov inNOVE03

Bottom up approaches

* Experimental test if

New reactor experiment? Gadolinium-loaded SK? Precision comparable to LBL : S. Choubey

P.HarrisonMore on mixing


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M.Fukugita, Tegmark

•Now ∑ mi < 0.4 eV

•Future (∑ mi) ~ 0.04 eV

Neutrinos in Cosmology Leptogenesis, Dark matter, Dark Energy

Mass from Large Scale Structure


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Mass varying neutrino (D.Marfatia)• The neutrino couples to light scalers• A possible candidate for Dark Energy.• Explains all existing data with one sterile neutrino, yet predicts no LSND effect• A possible signal: m2 (K2K) ≠ 　 m2 (Atmosphere)


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Mission – Phenomenological Subroup Look for new physics, survey models and determine necessary precision to: test the unitarity and/or NSI (non standard interaction)


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Status of 3+2 scheme (Note: 3+1 scheme unlikely)Can accommodate all data

Implies: Too low BG forsuperbeams, wrong near detector non-osc. assumptionEventually checked by MiniBOONE !?If confirmed: Some new interesting physics:

M. Sorel


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Unitarity triangles for lepton sectorIn see-saw mechanism: 6x6-Matrix unitary;in all realistic scenarios:Matter effects change unitarity trianglesExample: Higher Emakes sides comparable;

Easier to calculate area Easier to establish CP viol.

Z. Xing

S.GeerJ.Lopez

More on unitarity

Z.Xing


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Non Standard Interaction:

Another reason to do silver channel e

A.Friedland

More on new physics predictions S.AntuschO.Yasuda


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Lepton-flavour violating processes – clear synergy with neutrino

oscillationsNeutrino Factory could provide

copious source of muons for:

NF Frontend: 1014 muons/s

Current proton drivers: 108 muons/s

(MEG)

4 MW PD: 1011-12 muons/s

(PRISM)

Y.Kuno

Muon physics subgroup:

•Rare decays: •Flavour-change in scattering


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Y.KunoJ.Hisano

L.RobertsK.JungmannMore on muon phys.

x


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LFV in DIS processesSlepton mixing (SUSY) introduces LFV at one loop -associated LFVinteresting for Higgs-boson mediated processesUse DIS process: N -> X at neutrino factoryO(102) events for 50 GeV

Also possible with neutrino beam (in preparation)

KanemuraPhysics with High Energy Muon beam


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Mission: Experimental subgroup:

Use realistic assumptions on the performance

of accelerator and detector to: Evaluate and compare

performances ofSuperbeam Beta beam

Neutrino factoryFirst: Recent Progress on Facilities at Large 13


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Blaidwood Reactor Experiment in US 　 2-detctors

P.Fisher

K.JungmannMore on decay

Non-Accelerator Physics


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VLBNO All parameters in one experiment ?As good as any other SB experiments.Use wide band beam to measure both 1st and 2nd maximum

W.Marciano; Slides: T.Kirk Also H.Kirk, this conference


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T2KKSplit T2HK detector into two

and place one in Korea Long baseline helps to resolve degeneracy at Kamioka.T2KK reach

comparable or better than

NOvA and T2HK combined

T.Kajita, K.Nakamura

sin2213=0.05

P.Oddone


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Reminder: Studies before ISS SB outperforms NF at large 13

Very little study on Beta Beam

(Fig. from Huber, Lindner, Winter, hep-ph/0412199)

Poor knowledge on systematics


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Beta Beam studyFacilities using a Water Cherenkov detectorPrinciple advantage of betabeam: No intrinsic beam BGHigh gamma beta beambest alternative (even “low flux”)

E.Couce

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


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P. Huber et al.Comparisons: CP-13

SB still outperformsBB and NFAt large 13

E.CouceM.MezzettoE.Fernandez

More on BB


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For small 13 (<0.01)Superbeams will not address 13,

mass hierarchy, or CP violationA clear case for NF and/or -beamYet, many people take an attitude

“Wait until what SB finds, NF is useful only for small 13”

However, Will we get the funds to get a neutrino facto

ry even if all previous investments end up “unsuccessful”? (de Gouvêa: )

Investigate NF performance at high 13


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Use a Better Detector100 kton, magetised ironTwo performance assumptions:

‘Better’:

– Threshold

– Resolution

‘Baseline’:

– Threshold

– Resolution

Threshold moreimportant than

resolution

Factory Optimization

Huber, Lindner, Rolinec, Winter


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factory with better detector

Better detector threshold makes L=2000-3000 km very efficient 13-baseline for exclusion limit

“Magicbaseline”

sensitivity vs L

Better Threshold

Huber, Lindner, Rolinec, Winter


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Optimization for large 13 ? : E vs L

Mass hierarchy no problem for L >> 1000 kmCP fraction for CP violation (3“Standard”

Huber, Lindner, Rolinec, Winter, to appear

“Optimal appearance” L=1000 km/E=20 GeV looks good

W.WinterMore on NF


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Better detector: Large 13

Can compete with the superbeam upgrades (prel.)Both better Eres and threshold useful at large 13

Large +better detector prefers shorter baselines (1000-2000km); E small OK

W.


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P.Huber

Golden

Golden + (Silver, Platinum)Improves sensitivity to CP violation at large 13

Requires its own baseline?

Now we have a good handle to make NF competitive at large 13

Need to demonstrate with realistic detectors !!


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Interactions: Physics-Detector

“Close the loop”Better detector = key component

in large 13 discussion! Need best possible detector with

1. Better low energy efficiences2. Better energy resolution?Understanding of systematics is critical.

Crosssections, Backgrounds, matter distribution, etc. At large 13, it is the limiting factor.

In addition: e detection, silver channel concepts etc.Consider what physics the near detector can do ?

Good place for new physics ?

W.Winter

J.PeltoniemiM.WarnerJ.Sobczyk

More on Matter effectscrosssectionE, and Eth


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Interactions: Physics-Accelerator

Physics: What muon energy really required? 40 GeV enough for 13, CP, mass hierarchy ?

Physics: How large can flux uncertainty be?

+ -

+silver

-

MB

W.Winter

J,CampagneL.RobertsK.Jungmann

More on flux, E spectrum phys. requirement

• Storage ring+possible NF program?


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•Avoid too many options mixed up

• Discuss different options in one section and choose one “representative” for main line of argumentation?

Need that representative here at RAL

if we are to finish in August !!!


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Our goal: ‘to understand the physics of flavour’

Requires high precision, high sensitivity measurements of neutrino oscillations

Also LVF in muons, 02 decay. Next 5 yearsNext 5 years Improve the precision on the atmospheric parametersImprove the precision on the atmospheric parametersMeasure sinMeasure sin22221313 >0.1, and find CP violation. >0.1, and find CP violation.Next 10 yearsNext 10 yearsDemonstrate visibility of sub-leading transitions: Demonstrate visibility of sub-leading transitions: Explore sinExplore sin22221313 down to 0.01 down to 0.01Solve mass hierarchySolve mass hierarchyThen, precision eraThen, precision era : : when when ??????????????


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Timescales: the challengeHep-ex/0509019

Era ofsensitivity & precision

てぃｓｇｒ

This graph is made by the same people who believe NF is good only for small13.

Hypnotized, be not !NF can be a principal actor at the era of precision


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NF roadmap: key decision points

Ambitious, science-driven scheduleIssue now is to establish vibrant R&D programme Vision for International Design Study phase:

International collaboration; coordinated effort:• Concept development – full system• Accelerator R&D • Detector R&D

Neutrino Factory roadmap

International scoping study (ISS)NuFact06 ♦International design study (IDS) ● ● ● ● ● ● ● ●

Neutrino Factory consortium formationBuildPhysics

Key decision points

Seek to instigate IDS ♦Seek to host FP7 DS and/or I3 bids ♦IDS mandate at Nufact06 ♦Submit FP7 bids ♦Form Neutrino Factory consorium ♦Initiate build phase ♦

20142010 2011 2012 20132006 2007 2008 2009 2019 20202015 2016 2017 2018

K.Long


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Summary

We have to show NF is good at large 13, too.We have to close the loop and

come up with a representative plan to achieve the goal in August.Plan a strategy to accelerate R&D, to achieve early realization of NF.


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Back up slides


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Effects of physics beyond the SM

as effective operators

Can be expanded systematically (Weinberg)

Origin of neutrino mass

•The origin of neutrino mass lies in the lowest order effect of physics and thus the most sensitive probe for new physics at high scales.


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SUSYmotivated prediction


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Production

Detection

Transition

New interactions can happen in three places


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Neutrino Oscillation Appearance Probability


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13 & beam experiments

Appearance probability :

dependences in sin(223), sin(23), sign(m231), -CP phase in [0,2]

13 & reactor experiments• <E> ~ a few MeV only disappearance experiments

sin2(213) measurement independent of -CP

• 1-P(e e) = sin2(213)sin2(m231L/4E) + O(m2

21/m231)

weak dependence in m221

• a few MeV e + short baselines negligible matter effects (O[10-4] ) sin2(213) measurement independent of sign(m2

13)


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Conclusions (Reactors ： T.Lasserre NO-VE 06)

A further increase of the mass: sin2(213)<0.01 Movable detectors : Daya-bay, Braidwood Motionless detectors: Angra , Triple Chooz Shape only uncorrelated background dominates !!! 1000 mwe: Daya Bay, Angra Need more mass 450 mwe: Braidwood , Triple Chooz Need more mass + x >5 times better bkg

rejection

Several projects of reactor experiment in the pipelines First generation : sin2(213)~0.02-0.03

Rate + Shape Near/Far normalization error dominates (<1% error) Motionless detectors: Double Chooz, KASKA, RENO

A new reactor neutrino experiment dedicated to 13 is now being accepted as an important milestone of the neutrino oscillation program Reactor & Beam programs provide complementary measurements of 13 An early value of 13 will help to define the optimum CP- program

Towards the Second Generation: sin2(213)<0.02 Movable detectors : Daya-bay, Braidwood and motionless Triple Chooz Multi-detector phased programs better cross checks But what is the systematic error induced by moving ‘100 tons’ detectors?


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Ongoing Experiments “After 5 years


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Expect to measure m213:

23% 10% MINOS 2% T2K, NOvAFind non-zero 13 sin2213 ~ 10-2

Super-Beam < 1MW ~4MW

m213 　　　 1%

　 sin2213 ~10-3

　 mass-hierarchy up to sin2213 ~ 10-2 for all value of NOvA　 Search for CP violation

Super Beam Phase II


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Near Future / ”next 10 yrs” P.Huber et al., hep-ph/0403068

NOA

Super Beam: opportunityＸ 1 ０ improvement 　 over ongoing experi

ments


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Kajita EP2010


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3 sensitivity to sin2213

Better Eres Better threshold Better Eres+thresh

Optimization: Better detector versus higher muon energy?

Interactions: Detector-Accelerator

(Huber, Lindner, Rolinec, Winter, to appear)


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Mass hier., CP violation Better threshold (especially)

Better energy resolution Smaller matter density uncertainty (for large 13)

Standard Optimal Detector (better threshold + energy resolution)


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New physics tests:

Test unitarity and small ad-mixtures of “new physics” by: detection Pee+Pe+Pe = 1? (Donini, Meloni, Migliozzi, 2002; Autiero et al, 2004)

Neutral currents (hard) (Barger, Geer, Whisnant, 2004) Spectral signature on probability level

Example: Damping effects(Blennow, Ohlsson, Winter, hep-ph/0502147)

More complicated: Hamiltonian-level effects(e.g., Blennow, Ohlsson, Winter, hep-ph/0508175)

Example: Oscillation-NSI confusion theorem(Huber, Schwetz, Valle, 2002)

See other talks inthis workshop for

specific possible effects!E.g. Hisano, Kanemura,

Sato, Sorel, Xing

P.Huber


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Beyond the ISS: timescales

Mezzetto

50

30

20

50

30

20


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Timescales: the challenge

Era ofsensitivity & precision

Hep-ex/0509019


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Conclusions:International scoping study:

Has become establishedIs raising, and beginning to address, key issuesReport will lay the foundations for the more detailed design-study phase

International Design Study of the Neutrino FactoryRequired to follow the ISS to:

• Prepare reference (baseline) design by ~2011• Prepare first conceptual design by ~2013

In parallel, design studies for alternative facilities must be carried forward:

To allow best possible facility to be identified

The ISS, together with MICE, MERIT, and EMMAAn exciting R&D programme …With a first-rate scientific goal

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Physics Working Group INTERNATIONAL NEUTRINO FACTORY AND SUPERBEAM SCOPING STUDY MEETING

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