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Physics Working Group
Aim and tasks
INTERNATIONAL NEUTRINO FACTORY AND SUPERBEAM
SCOPING STUDY MEETING
CERN - 22-24 September 2005
Y. Nagashima
OSAKA UNIVERSITY
CONTENTS
• Mission defined
• Past studies: SB, BB, NF
• Degeneracy problem
• Summary
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Organization of Physics Working Group
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
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1. MISSION DEFINED
Three subgroups
in the Physics working group
Theoretical
Phenomenological
Experimental
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PHYSICS MOTIVATION
Two 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
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 “Neutrino Factory”
and other related facilities
The neutrino mixing matrix:
3 angles and a phase d
n e  
c12 c13
n   s12 c 23  c12 s13 s 23 e id
  
n    s12 s23  c12 s13 c23 e id
 id
s12 c13
id
c12 c 23  s12 s13 s 23 e
c12 s23  s12 s13 c 23 e id
23 (atmospheric) = 450 , 12 (solar) = 320 , 13 (Chooz) < 130
n1 
c13 s23 
n 2 

 
c13 c 23 n 3 
s13 e
n3
Dm223= 2 10-3eV2
n2
n1
Dm212= 8 10-5 eV2
Normal Hierarchy or
n2
n1
Unknown or poorly known
13 , phase d , sign of Dm213
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Dm212= 8 10-5 eV2
Dm223= 2 10-3eV2
Inverted Hierarchy
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Muon Physics
sensitive probe for SUSY
MuEGamma
Goal 10-14
Similar plots for
 e conversion with
Re- ranging between
(10-14 - 10-17)
PRISM
sensitive down to
10-18
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Hisano et al., PL B391 (1997) 341
Neutrino factory is comparable
with LHC and ILC
“In its scale”.
Is the physics case equally strong?
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Mission of the theoretical subgroup
Issue a message to global community
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
•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, paintISSaPlenary#1
colorful picture!
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The neutrino opens the way
to many new frontiers
Super Beam
n factory
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Courtesy
9
Brian Foster NuFact02
Manfred Lindner ISSWS05
Mission of the phenomenogical
and experimental subgroups
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 measurements
Make a scenario w/wo staging approach to achieve
scientific goals
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For Experimental subgroup
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.
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Goals of the plenary meeting #1
Establish list of parameters
and things to do
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What parameters do we want to decide?
What are the list of “to do”?
2. Past Studies
Ongoing Experiments
Super Beam
Beta Beam
Neutrino Factory
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Ongoing Experiments “After 5 years
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Near Future (Super Beam)
T2K (Japan)
295km
C2GT (CNGS beam) ~1200km
NOnA
(NUMI beam)
810km
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n ~ ne oscillations
15
Super-Beam < 1MW  ~4MW
Expect to measure Dm213:
23%  10%
MINOS
 2%
T2K, NOvA
Find non-zero 13
 sin2213 ~ 10-2
Super Beam Phase II
 Dm213
 1%
 sin2213  ~10-3
 mass-hierarchy up to sin2213 ~ 10-2
for all value of d NOvA
 Search for CP violation
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Near Future / ”next 10 yrs”
P.Huber et al.,
hep-ph/0403068
Super Beam: opportunity
Ｘ1０ improvement over ongoing experiments
NOnA
Dm2=2.0x10-3eV2
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Intermediate Future/ “next 20
years”
Super Beam PhaseII
Beta Beam
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Mass Hierarchy Super-NOnA
Long (L=810km) baseline enhances sensitivity to
sgn{Dm231} for sin2213 down to 0.02





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 n+ 3 anti n)
Fermilab
Proton driver study report’
http://protondriver.fnal.gov/
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New Long Baseline 19
=1290km at Homestake
Beta-Beams
Detector at Frejus
Same detectors as Super Beam !
_
Store 18Ne, 6He to produce pure ne and ne beams
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•Beta beam offers clean low E ne beams
with no n backgrounds
•1.1x1018He and 2.9x1018He decays/yr
•Detector at Frejus(L=130km) 1Mt water cherenkov
~x30 improvement
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Messier Nuact05
Long Future/ “next 30 years”
E=20-50GeV
1021 ’s/yr
50kt detector
Baseline 300,700,7000km
Neutrino Factory
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Neutrino Factory
Provides clean intense ne n channel (Golden)
and ne  n channel (Silver)
Provides disappearance channels
n  n and ne  ne
NF (golden+silver)+SB solves degeneracies
down to sin2213=10-4
Still considered as the ultimate neutrino oscillation
facility
The question is cost consideration
(1500M$+400M$*E/20 in Study II)
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Long Future/ “Next 30 years”
Ability to resolve
Mass hierarchy
ambiguity
sin2213
Figures like this
can help us develop
the neutrino physics
“road map”
It would be good to
develop an agreed on
list of figures and
experiments to be
plotted, and timelines
to be used.
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S.Geer ISSWS05
Long Future / “Next 30 years”
Ability to
observe
non-zero 13
versus time
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Fermilab
Proton driver study report’
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http://protondriver.fnal.gov/
NF always outperforms SB
except for very large values of sin2213 >0.01
(large uncertainties from matter effect)
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P.Huber et al., hep-ph/0412199
Indicator for risk minimization
of CP precision measurement
Sin2213=10-1
T2HK is better
Sin22
Synergy between
T2HK and NF
13
=10-3
NF outperforms
Sin2213=10-4
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CP coverage is a range of fitted values of dCP
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P.Huber et al., hep-ph/0412199
3. DEGENERACY PROBLEM
Each experiment to measure
at fixed
suffers from correlation and degeneracy
problem
SYSTEMATIC
CORRELATION
DEGENERACY
T2K
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P.Huber et al. hep-ph/0403068
8-fold degeneracy
P(n_en_)=Asin2213+sin213(Bcos d+Csin d)+D
P(nen)=Asin2213+sin213(Bcos d-Csin
d)+D
_
_
Measurement of x=P(nen) and y=P(nen)
at fixed En/L gives an elipse in x-y plane.
13  ’13 gives a different ellipse.  2-fold 13d degeneracy
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13  d ambiguity.
Mass hierarchy two-fold degeneracy: |Dm231|=|-Dm231|
23 degeneracy: sin2223ISS
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sin22(p/2)23
29
How to solve correlation and
degeneracy?
Use combination of different En, L
or Golden+Silver channel
Many scenarios are proposed
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Example 1
Measure at 2En’s to solve correlation
Super-NOvA

SB + 2nd detector at the 2nd
oscillation maximum

50 kton detector at 710 km.

30km off axis (second max.)

6 years (3 n + 3 anti n)
Determines mass hierarchy for
all values of d down to
sin2 213 = 0.02
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Example 2:
Synergy of
NuFact-II(300km)+T2HK
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2 L’s to resolve degeneracy
mass hierarchy
removed
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L at MB=Magic Base Line(7500km)
Staged approach
One detector first, if d~p/3
If not, 2nd detector at MB
Region; Single measurement OK
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P.Huber et al., hep-ph/0412199
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Step towards a consensus:
Identify the need for complementary measurement
Make a scenario w/wo staging approach to achieve
scientific goals
Establish the physics case for (or against! ) a NF
S.Geer’s question
Is a NF needed if sin2213 is large ?
What is the minimum NF energy that will
deliver the physics (cost issue)?
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SHEDULE
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)
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Time schedule:
taken from
An 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
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4. Summary
Issue a message to win broad community’s support
Review physics performance of future options
for precision neutrino oscillation measurements:
Define strengths and weaknesses of each facility
Perform critical comparisons
Identify the need for complementary measurements
Make a scenario and/or staging approach to achieve
scientific goals
Establish the physics case for (or against!) a NF
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On Michael Turner’s door at NSF
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The neutrino mixing matrix:
3 angles and a phase d
n3
Dm223= 2 10-3eV2
n2
n1
Dm212= 8 10-5 eV2
Normal Hierarchy or
n2
n1
23 (atmospheric) = 450 , 12 (solar) = 320 , 13 (Chooz) < 130
n3
Dm212= 8 10-5 eV2
Dm223= 2 10-3eV2
Inverted Hierarchy
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Unknown or poorly known
13 , phase d , sign of Dm213
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T2K PhaseII
Phase II:
4 MW upgrade
Phase II
HK: 1000 kt
SK: 22.5 kt
Kamioka
J-PARC
JPARC-n ~0.6GeV n
beam 0.75 MW 50 GeV PS
(2008 )
K2K ~1.2 GeV n beam
0.01 MW 12 GeV PS
(1999 2005)
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Sensitivity depends on the true value of Dm2
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Beta-beam: sensitivity
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Mezzetto
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Comparison: BB/NF
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Huber
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Neutrino Oscillation Appearance Probability
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NF operates at atmospheric n distance
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channel at neutrino factory
High energy neutrinos at NuFact allow observation of
A. Donini et al
nen
(wrong sign muons with missing energy and P). UNIQUE
Liquid Argon or OPERA-like detector at 700 or 3000 km.
Since the sind dependence has opposite sign with the wrong sign muons, this solves ambiguities
that will invariably appear if only wrong sign muons are used.
ambiguities with
only wrong sign muons (3500 km)
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associating taus to muons
equal event number curves
(no efficencies, but only OPERA mass)
muon vs taus
studies on-going
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M.Lindner;
hep-ph/0503101
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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 sin2213 is large ?
 What is the minimum NF energy that will
deliver the physics (cost issue)?
How do we best test the three-flavor framework
and how do we quantify the test ?
 How can we best articulate the physics case
for precision measurements of the neutrino
parameters if sin2213 > O(0.01), & continuing the
program if sin2213 < O(0.01) ?

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Physics Motivation
Minimal Standard Model (SM)Baryon Number, Lepton Flavour & Lepton Number - conserved !
neutrinos massless - no oscillations !
Hence: processes such as e,  e,  eee, K0Le, Z0e & n-oscillations
& 0n-decay are sensitive tools to probe physics beyond the Standard Model
• Discovery of n-oscillations (Super-K)
• g-2 Results (BNL)
• Evidence for 0n-decay (Heidelberg/Moscow)
• Proton Decay ??? (Kolar Goldfield)
}
Further Stimulate the search for LFV
in the charged Lepton Sector
Extensions to SM -( with n-oscillations) - Predict LFV rates too small to be observed
Extensions beyond SM - Predict LFV & BNV at a measurable level
(e.g. see Barbieri & Hall, Hisano et al.)
Super Symmetry (SUSY-GUTs)
SU(5) 1013<Br( e) < 1015
SO(10) 1011<Br( e) < 1013
Process
  e+ 
 N  e N

Current SUSY
Limit
level
10-11
10-13
~10-12
10-15
10-6
10-9
!!! Just below Present Experimental Bound <1.2·10-11 !!!
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Physics Motivation cont.
e.g. Prediction Br(e) vs. parameter space in SUSY SU(5)
see J. Hisano et al. Phys. Lett. B391 (1997) 341
MuEGamma
Goal 10-14
Similar plots for
 e conversion
with
Re- ranging between
(10-14 - 10-17)
over most of the parameter
ranges
MECO(BNL)-goal single
event sensitivity of 2.10-17
*tan()
*
- ratio of vac. expec. values of Higgs Fields
- Higgs Fields mixing parameter
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Physics Motivation cont.
LFV and n -oscillations
10
Br(e  )
-4
10
MSW large an gle
MS W small an gle
-5
bound
10
Phys. Rev. D59 (1999)
ge
-12
10
-7
Br ( 
10
-8
MuEGamma
Goal 10-14
-13
10
10
o
-14
st
s
10
J ust so
-10
SU(5) grand unified
model with heavy,
right-handed
neutrinos (Majorana)
Solar -n Results from
Super-Kamiokande
favour
Ju
-9
10
M
Possible
solutions to
solar n oscil.
SW
s
~
lar mal l
ge
a
a n n gle
g le
sm
a ll
M
e)
M SW larg e angle
small mass
ma
ss
la r
-6
10
D m 2 (eV 2 )
Mega Limit
-11
an
g le
10
J. Hisano and
D. Nomura
Experimental
SW
Dm2(eV2)
10
10
From the model of:
-10
-3
MSW Large-angle
Mixing
-15
10
10
-11
10
-3
10
-2
-1
10
2
sin 2 
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10
12
10
13
10
14
M nR2 (GeV)
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MEG @ PSI
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BR = 2 X 10-13
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