Y.Nagashima, ISS 060427 1 Physics Working Group INTERNATIONAL NEUTRINO FACTORY AND SUPERBEAM SC OPING STUDY MEETING RAL – 25 April, 2006 Y. Nagashima OSAKA UNIVERSITY Status, prospects and what to do here nowledgements: Grateful to all ISS speakers from I have taken material.
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Physics Working Group INTERNATIONAL NEUTRINO FACTORY AND SUPERBEAM SCOPING STUDY MEETING
Physics Working Group INTERNATIONAL NEUTRINO FACTORY AND SUPERBEAM SCOPING STUDY MEETING RAL – 25 April, 2006 Y. Nagashima OSAKA UNIVERSITY. Status, prospects and what to do here. Acknowledgements: Grateful to all ISS speakers from whom I have taken material. Council members - PowerPoint PPT Presentation
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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
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
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 ♦
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
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?