050923ISS Plenary#11 Physics Working Group Aim and tasks INTERNATIONAL NEUTRINO FACTORY AND...

050923 ISS Plenary#1 1

Physics Working Group Aim and tasks

INTERNATIONAL NEUTRINO FACTORY AND SUPERBEAM SCOPING STUDY MEETINGCERN - 22-24 September 2005

Y. Nagashima

OSAKA UNIVERSITY

CONTENTS• Mission defined• Past studies: SB, BB, NF• Degeneracy problem• Summary


Convener: Yori Nagashima (Osaka U.)Council members: Debbie Harris (FNAL), Pilar Hernandez (U.Valencia), Manfred Lindner (Technical U. Muenchen), Ken Long (Imperial College London) Hitoshi Murayama (LBL), Lee Roberts (U. Boston), Osamu Yasuda (Tokyo Metropolitan U.)

Subgroup convener Theoretical: TBC Phenomenological: O.Yasuda Experimental: K.Long

Organization of Physics Working Group


Three subgroupsin the Physics working groupTheoreticalPhenomenologicalExperimental

1. MISSION DEFINED


PHYSICS MOTIVATIONTwo directions beyond SM, toward Unification

EW symmetry breaking, ★ HIGGS, GUT, SUSY, ED LHC, ILC Clear theoretical guide exists: Top down approach

Flavor Problem ★ Origin of generations, Mass Hierarchy, Flavor Symmetry 　 No clear theory exists. Only experimental observations: Bottom up approach Neutrino mass: Only “beyond SM evidence”! Cold Dark Matter and Dark Energy exist. Leptonic CP violation: The origin of the matter ? Precision measurement of lepton mixing matrix

and mass hierarchy “Neutrino Factory” and other related facilities


The neutrino mixing matrix:

3 angles and a phase

Normal Hierarchy or

m223= 2 10-3eV2

m212= 8 10-5 eV2

m212= 8 10-5 eV2

m223= 2 10-3eV2

Inverted Hierarchy

Unknown or poorly known 13 , phase , sign of m2

13

e

c12c13 s12c13 s13e i

s12c23 c12s13s23ei c12c23 s12s13s23e

i c13s23

s12s23 c12s13c23ei c12s23 s12s13c23e

i c13c23

1

2

3

23(atmospheric) = 450 , 12(solar) = 320 , 13(Chooz) < 130


Muon Physics

Similar plots for Similar plots for e conversion withe conversion with

RRee- ranging between- ranging between

(10(10-14-14 - 10 - 10-17-17))

PRISMPRISM sensitive down tosensitive down to

1010-18-18

MuEGammaMuEGammaGoal 10Goal 10-14-14

Hisano et al., PL B391 (1997) 341

sensitive probe for SUSY


Neutrino factory is comparable

with LHC and ILC

“In its scale”.

Is the physics case equally strong?


Mission of the theoretical subgroup

Issue a message to global community

•Describe the impact of the neutrino and other related researches towards the understanding of the matter unification, the synergy of particle physics, astro-physics and cosmology. •Draw a roadmap, paint a colorful picture!

　 Win Other Scientists’ Support It is not enough to win arguments… one must win partners.

The two are not the same. Robin Staffin, DOE, 2005 ILC Workshop at Snowmass


Super Beam

CourtesyBrian Foster NuFact02Manfred Lindner ISSWS05

The neutrino opens the way to many new frontiers

factory


Critical review of physics performance of future options :• Superbeam (SB)• Beta beam (BB)• Neutrino Factory (NF)

Define strengths and weaknesses of each facility Perform critical comparison

Step towards a consensus:Identify the need for complementary measurementsMake a scenario w/wo staging approach to achieve scientific goals

Mission of the phenomenogical and experimental subgroups


Need to define:Assumptions on accelerator performance Assumptions on detector performance Definition of baseline tools used for analyses: e.g. Nuance/Globes. Neutrino cross sections: status and what will be assumed.

For Experimental subgroup


Goals of the plenary meeting #1

Establish list of parameters and things to do


2. Past Studies

Ongoing ExperimentsSuper BeamBeta BeamNeutrino Factory

What parameters do we want to decide?What are the list of “to do”?


Ongoing Experiments “After 5 years


Near Future (Super Beam)

T2K (Japan) 295km

C2GT (CNGS beam) ~1200km

NOA(NUMI beam) 810km

They all look for ~ e oscillations


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


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

NOA

m2=2.0x10-3eV2

Super Beam: opportunityＸ 1 ０ improvement 　 over ongoing experi

ments


Intermediate Future/ “next 20 years”

Super Beam PhaseII

Beta Beam


Mass Hierarchy Super-NOA

Long (L=810km) baseline enhances sensitivity to sgn{m2

31} for sin2213 down to 0.02

New Long Baseline=1290km at Homestake

NOvA (=NUE) phase II

SB+ 2nd detector at the 2nd oscillation maximum 50 kton detector at 710 km. 30km off axis (second max.) 6 years (3+ 3 anti )

Fermilab Proton driver study report’http://protondriver.fnal.gov/


Store 18Ne, 6He to produce pure e and e beams_

Same detectors as Super Beam !

Detector at FrejusBeta-Beams

050923 ISS Plenary#1 21Messier Nuact05

•Beta beam offers clean low E e beams　 with no backgrounds •1.1x1018He and 2.9x1018He decays/yr•Detector at Frejus(L=130km) 1Mt water cherenkov

~x30 improvement


E=20-50GeV1021 ’s/yr50kt detectorBaseline 300,700,7000kmNeutrino Factory

Long Future/ “next 30 years”


Neutrino Factory

Provides clean intense e channel (Golden)

and e channel (Silver)

Provides disappearance channels

and e e

NF (golden+silver)+SB solves degeneracies

down to sin2213=10-4

Still considered as the ultimate neutrino oscillation facility

The question is cost consideration

(1500M$+400M$*E/20 in Study II)


Figures like thiscan help us developthe neutrino physics“road map”

It would be good to develop an agreed on list of figures and experiments to beplotted, and timelinesto be used.

YEAR

sin

22 1

3

S.Geer ISSWS05

Long Future/ “Next 30 years”

Ability to resolveMass hierarchy ambiguity


Long Future / “Next 30 years”

Ability to observe non-zero 13

versus time

Fermilab Proton driver study report’http://protondriver.fnal.gov/

050923 ISS Plenary#1 26P.Huber et al., hep-ph/0412199

NF always outperforms SBexcept for very large values of sin2213 >0.01

(large uncertainties from matter effect)

050923 ISS Plenary#1 27P.Huber et al., hep-ph/0412199

Indicator for risk minimization of CP precision measurement

Sin2213=10-1 T2HK is better

Sin2213=10-3Synergy between T2HK and NF

Sin2213=10-4 NF outperforms

CP coverage is a range of fitted values of CP

050923 ISS Plenary#1 28P.Huber et al. hep-ph/0403068

Each experiment to measureat fixed suffers from correlation and degeneracy problem

T2K

CORRELATION DEGENERACYSYSTEMATIC

3. DEGENERACY PROBLEM


8-fold degeneracy P(e)=Asin2213+sin213(Bcos +Csin )+D

P(e)=Asin2213+sin213(Bcos -Csin )+D Measurement of x=P(e) and y=P(e)

at fixed E/L gives an elipse in x-y plane.

_ __ _

13 ’13 gives a different ellipse. 2-fold degeneracy

ambiguityMass hierarchy two-fold degeneracy: |m2

31|=|-m231|

degeneracy: sin2223= sin22()23


How to solve correlation and degeneracy?

Use combination of different E, Lor Golden+Silver channel

Many scenarios are proposed


Determines mass hierarchy for all values of down to sin2 213 = 0.02

Measure at 2E’s to solve correlation

Example 1

Super-NOvA SB + 2nd detector at the 2nd

oscillation maximum 50 kton detector at 710 km. 30km off axis (second max.) 6 years (3 + 3 anti )

050923 ISS Plenary#1 322nd L at MB=Magic Base Line(7500km)

Staged approachOne detector first, if /3 If not, 2nd detector at MB

Region; Single measurement OK

P.Huber et al., hep-ph/0412199

mass hierarchyremoved

Synergy of NuFact-II(300km)+T2HK

Example 2: 2 L’s to resolve degeneracy


Step towards a consensus:

Identify the need for complementary measurementMake a scenario w/wo staging approach to achieve scientific goalsEstablish the physics case for (or against! ) a NF

S.Geer’s questionIs a NF needed if sin2213 is large ?What is the minimum NF energy that will deliver the physics (cost issue)?


Physics working group workshop #1

14-21 November 2005 Imperial College London

Plenary Meetings #2 KEK; 23-25 January 2006

#3 RAL; 27-29 April 2006 #4 Irvine; 21-23 August 2006 (just

before NuFact06)

SHEDULE


Time schedule: taken fromAn International Scoping Study of a Neutrino Factory and super-beam facility

http://www.hep.ph.ic.ac.uk/%7Elongkr/UKNF/Scoping-study/ISS-www-site/WG1-PhysPhen/Council/2005-08-29/PhysPhen-council-2005-08-29-WG1-plan.pdf


Issue a message to win broad community’s supportReview physics performance of future options

for precision neutrino oscillation measurements:Define strengths and weaknesses of each facility Perform critical comparisonsIdentify the need for complementary measurementsMake a scenario and/or staging approach to achieve scientific goals

Establish the physics case for (or against!) a NF

4. Summary


On Michael Turner’s door at NSF


23(atmospheric) = 450 , 12(solar) = 320 , 13(Chooz) < 130

The neutrino mixing matrix:

3 angles and a phase

Normal Hierarchy or

m223= 2 10-3eV2

m212= 8 10-5 eV2

m212= 8 10-5 eV2

m223= 2 10-3eV2

Inverted Hierarchy

Unknown or poorly known 13 , phase , sign of m2

13


JPARC-JPARC- ~0.6GeV ~0.6GeV beam beam 0.75 MW 50 GeV PS 0.75 MW 50 GeV PS

(2008 (2008 ))KamiokaKamioka J-PARCJ-PARC

SK: 22.5 ktSK: 22.5 kt

Phase II:Phase II:4 MW upgrade4 MW upgradePhase IIPhase II

HK: 1000 ktHK: 1000 kt

K2K ~1.2 GeV K2K ~1.2 GeV beam beam 0.01 MW 12 GeV PS 0.01 MW 12 GeV PS

(1999 (1999 2005)2005)

T2K PhaseII


Sensitivity depends on the true value of m2


Beta-beam: sensitivity Mezzetto


Comparison: BB/NF Huber


Neutrino Oscillation Appearance ProbabilityNeutrino Oscillation Appearance Probability


NF operates at atmospheric distance

optimum


channel at neutrino factory

High energy neutrinos at NuFact allow observation of e(wrong sign muons with missing energy and P). UNIQUE

Liquid Argon or OPERA-like detector at 700 or 3000 km.

Since the sin dependence has opposite sign with the wrong sign muons, this solves ambiguitiesthat will invariably appear if only wrong sign muons are used.

ambiguities with only wrong sign muons (3500 km)

equal event number curvesmuon vs taus

associating taus to muons (no efficencies, but only OPERA mass)

studies on-going

A. Donini et al

050923 ISS Plenary#1 53M.Lindner; hep-ph/0503101


Wish-List for Study S.Geer ISSWS05

There have been a series of neutrino physics studies in Europe, Japan and the US, aimed at understanding future needs and options. Lots has been done, but there are still some questions to be nailed … for example:

Is a NF needed if sin2213 is large ?

What is the minimum NF energy that will deliver the physics (cost issue)? How do we best test the three-flavor frameworkand how do we quantify the test ? How can we best articulate the physics case for precision measurements of the neutrino parameters if sin213 > O(0.01), & continuing the program if sin2213 < O(0.01) ?


Minimal Standard Model (SM)-Minimal Standard Model (SM)-

Baryon Number, Lepton Flavour & Lepton Number - conserved !Baryon Number, Lepton Flavour & Lepton Number - conserved !

neutrinos massless - no oscillations !neutrinos massless - no oscillations !

Hence: processes such as Hence: processes such as ee, , e, e, eee, K eee, K00LLe, Ze, Z00e & e & -oscillations-oscillations

& 0& 0-decay -decay are sensitive tools to probe physics beyond the Standard Model are sensitive tools to probe physics beyond the Standard Model

• Discovery of Discovery of -oscillations -oscillations (Super-K)(Super-K)

• g-2 Resultsg-2 Results (BNL) (BNL)

• Evidence for 0Evidence for 0-decay -decay (Heidelberg/Moscow)(Heidelberg/Moscow)

• Proton Decay ??? Proton Decay ??? (Kolar Goldfield)(Kolar Goldfield)

Extensions to SMExtensions to SM -( with -( with -oscillations) - Predict LFV rates-oscillations) - Predict LFV rates too small to be observed too small to be observed

Extensions beyond SMExtensions beyond SM - Predict LFV & BNV at a measurable level - Predict LFV & BNV at a measurable level

(e.g. see Barbieri & Hall, Hisano et al.)(e.g. see Barbieri & Hall, Hisano et al.)

Super Symmetry (SUSY-GUTs)Super Symmetry (SUSY-GUTs)

SUSUr(r(ee) )

SOSOr(r(ee) )

!!! Just below Present Experimental Bound <1.2·10!!! Just below Present Experimental Bound <1.2·10 -11-11 !!! !!!

Minimal Standard Model (SM)-Minimal Standard Model (SM)-

Baryon Number, Lepton Flavour & Lepton Number - conserved !Baryon Number, Lepton Flavour & Lepton Number - conserved !

neutrinos massless - no oscillations !neutrinos massless - no oscillations !

Hence: processes such as Hence: processes such as ee, , e, e, eee, K eee, K00LLe, Ze, Z00e & e & -oscillations-oscillations

& 0& 0-decay -decay are sensitive tools to probe physics beyond the Standard Model are sensitive tools to probe physics beyond the Standard Model

• Discovery of Discovery of -oscillations -oscillations (Super-K)(Super-K)

• g-2 Resultsg-2 Results (BNL) (BNL)

• Evidence for 0Evidence for 0-decay -decay (Heidelberg/Moscow)(Heidelberg/Moscow)

• Proton Decay ??? Proton Decay ??? (Kolar Goldfield)(Kolar Goldfield)

Extensions to SMExtensions to SM -( with -( with -oscillations) - Predict LFV rates-oscillations) - Predict LFV rates too small to be observed too small to be observed

Extensions beyond SMExtensions beyond SM - Predict LFV & BNV at a measurable level - Predict LFV & BNV at a measurable level

(e.g. see Barbieri & Hall, Hisano et al.)(e.g. see Barbieri & Hall, Hisano et al.)

Super Symmetry (SUSY-GUTs)Super Symmetry (SUSY-GUTs)

SUSUr(r(ee) )

SOSOr(r(ee) )

!!! Just below Present Experimental Bound <1.2·10!!! Just below Present Experimental Bound <1.2·10 -11-11 !!! !!!

ee++ ee++

NN ee NN

1010-9-91010-6-6

1010-13-131010-11-11

1010-15-15~10~10-12-12

SUSY level

Current Limit

Process

Further Stimulate the search for LFVFurther Stimulate the search for LFV in the charged Lepton Sectorin the charged Lepton Sector}

Physics Motivation


Physics Motivation cont.e.g. Prediction Bre.g. Prediction Br((ee)) vs. parameter space in SUSY SU(5) vs. parameter space in SUSY SU(5)

see J. Hisano et al. Phys. Lett. B391 (1997) 341see J. Hisano et al. Phys. Lett. B391 (1997) 341

Similar plots for Similar plots for

e conversione conversion with with

RRee- ranging between- ranging between

((1010-14-14 - 10 - 10-17-17)) over most of the parameter over most of the parameter rangesranges

MECO(BNL)-goal single MECO(BNL)-goal single event sensitivity of event sensitivity of 2.102.10-17-17

*tan() - ratio of vac. expec. values of Higgs Fields* - Higgs Fields mixing parameter



Mega Limit

Physics Motivation cont.10

(GeV)M R2

141312101010

bound

Experimental

-1-2-3 11010

MSW small angle

MSW large anglesmall mass

J ust so

MSW large angle

sin 22

m

2(e

V )2

e

)

Br(

10

10

10

10

10

10

10

10

-3

-4

-5

-6

-7

-8

-9

-10

10

-11

10

10

10

10

10

10

-10

-11

-12

-13

-14

-15

m2(e

V2)

Br(

e

)

Possible solutions to

solar -oscil.

MS

W la

rge

angl

e

MS

W la

rge

angl

eM

SW

sm

all a

ngle

MS

W s

mal

l ang

leV

acVac


LFV and LFV and -oscillations -oscillationsLFV and LFV and -oscillations -oscillationsFrom the model of: From the model of:

J. Hisano and J. Hisano and D. NomuraD. Nomura

Phys. Rev. D59 (1999)Phys. Rev. D59 (1999)

SU(5) grand unified SU(5) grand unified model with heavy, model with heavy, right-handed right-handed neutrinos (Majorana)neutrinos (Majorana)

Solar -Solar - Results from Results from Super-KamiokandeSuper-Kamiokande

favourfavour

MSW Large-angle MSW Large-angle Mixing Mixing

From the model of: From the model of:

J. Hisano and J. Hisano and D. NomuraD. Nomura

Phys. Rev. D59 (1999)Phys. Rev. D59 (1999)

SU(5) grand unified SU(5) grand unified model with heavy, model with heavy, right-handed right-handed neutrinos (Majorana)neutrinos (Majorana)

Solar -Solar - Results from Results from Super-KamiokandeSuper-Kamiokande

favourfavour

MSW Large-angle MSW Large-angle Mixing Mixing


MEG @ PSI

Discovery Potential: 4 Events BR = 2 X 10-13

050923ISS Plenary#11 Physics Working Group Aim and tasks INTERNATIONAL NEUTRINO FACTORY AND...

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