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Physics Working Group Aim and tasks INTERNATIONAL NEUTRINO FACTORY AND SUPERBEAM SCOPING STUDY MEETING CERN - 22-24 S

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. Organization of Physics Working Group.

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Physics Working Group Aim and tasks INTERNATIONAL NEUTRINO FACTORY AND SUPERBEAM SCOPING STUDY MEETING CERN - 22-24 S

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  1. 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 ISS Plenary#1

  2. 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 ISS Plenary#1

  3. 1. MISSION DEFINED Three subgroupsin the Physics working group • Theoretical • Phenomenological • Experimental ISS Plenary#1

  4. 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 ISS Plenary#1

  5. The neutrino mixing matrix: 3 angles and a phased n3 Dm223= 2 10-3eV2 n2 n1 Dm212= 8 10-5 eV2 Normal Hierarchy or n2 n1 Dm212= 8 10-5 eV2 Dm223= 2 10-3eV2 n3 Inverted Hierarchy q23(atmospheric) = 450 , q12(solar) = 320 , q13(Chooz) < 130 Unknown or poorly known 13,phase ,sign of Dm213 ISS Plenary#1

  6. MuEGamma Goal 10-14 Muon Physics sensitive probe for SUSY Similar plots for  e conversion with Re- ranging between (10-14 - 10-17) PRISM sensitive down to 10-18 ISS Plenary#1 Hisano et al., PL B391 (1997) 341

  7. Neutrino factory is comparable with LHC and ILC “In its scale”. Is the physics case equally strong? ISS Plenary#1

  8. 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, paint a colorful picture! ISS Plenary#1

  9. The neutrino opens the way to many new frontiers Super Beam nfactory ISS Plenary#1 Courtesy Brian Foster NuFact02 Manfred Lindner ISSWS05

  10. 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 ISS Plenary#1

  11. 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. ISS Plenary#1

  12. Goals of the plenary meeting #1Establish list of parameters and things to do ISS Plenary#1

  13. 2. Past Studies What parameters do we want to decide? What are the list of “to do”? • Ongoing Experiments • Super Beam • Beta Beam • Neutrino Factory ISS Plenary#1

  14. Ongoing Experiments “After 5 years ISS Plenary#1

  15. Near Future (Super Beam) T2K (Japan) 295km C2GT(CNGS beam)~1200km NOnA (NUMI beam) 810km They all look fornm~ ne oscillations ISS Plenary#1

  16. Super-Beam < 1MW  ~4MW • Expect to measureDm213: • 23%  10% MINOS •  2% T2K, NOvA • Find non-zero q13 • sin22q13 ~ 10-2 Super Beam Phase II • Dm213 　 1% • sin22q13  ~10-3 • mass-hierarchy up tosin22q13 ~ 10-2 • forall value of dNOvA • Search for CP violation ISS Plenary#1

  17. Near Future / ”next 10 yrs” P.Huber et al., hep-ph/0403068 NOA Super Beam: opportunity Ｘ1０ improvementover ongoing experiments Dm2=2.0x10-3eV2 ISS Plenary#1

  18. Intermediate Future/ “next 20 years” • Super Beam PhaseII • Beta Beam ISS Plenary#1

  19. Mass Hierarchy Super-NOA Long (L=810km) baseline enhances sensitivity to sgn{Dm231} for sin22q13 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/ ISS Plenary#1 New Long Baseline =1290km at Homestake

  20. Beta-Beams Detectorat Frejus Same detectors as Super Beam ! _ Store 18Ne, 6He to produce pure e and e beams ISS Plenary#1

  21. Beta beam offers clean low E ne beams • with no nm backgrounds • 1.1x1018He and 2.9x1018He decays/yr • Detector at Frejus(L=130km) 1Mt water cherenkov ~x30improvement ISS Plenary#1 Messier Nuact05

  22. Long Future/ “next 30 years” Neutrino Factory • Em=20-50GeV • 1021m’s/yr • 50kt detector • Baseline 300,700,7000km ISS Plenary#1

  23. Neutrino Factory • Provides clean intense ne nm channel (Golden) and ne  nt channel (Silver) • Provides disappearance channels nm  nm and ne  ne • NF (golden+silver)+SB solves degeneracies down to sin22q13=10-4 • Still considered as the ultimate neutrino oscillation facility • The question is cost consideration (1500M$+400M$*E/20 in Study II) ISS Plenary#1

  24. Long Future/ “Next 30 years” sin22q13 YEAR Ability to resolve Mass hierarchy ambiguity 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. ISS Plenary#1 S.Geer ISSWS05

  25. Long Future / “Next 30 years” Ability to observe non-zero q13 versus time Fermilab Proton driver study report’ http://protondriver.fnal.gov/ ISS Plenary#1

  26. NF always outperforms SB except for very large values of sin22q13 >0.01 (large uncertainties from matter effect) ISS Plenary#1 P.Huber et al., hep-ph/0412199

  27. Indicator for risk minimization of CP precision measurement T2HK is better Sin22q13=10-1 Synergy between T2HK and NF Sin22q13=10-3 NF outperforms Sin22q13=10-4 ISS Plenary#1 CP coverage is a range of fitted values of dCP P.Huber et al., hep-ph/0412199

  28. Each experiment to measure at fixed suffers from correlation and degeneracy problem SYSTEMATIC CORRELATION DEGENERACY 3. DEGENERACY PROBLEM T2K ISS Plenary#1 P.Huber et al. hep-ph/0403068

  29. P(nenm)=Asin22q13+sin2q13(Bcos d+Csin d)+D P(nenm)=Asin22q13+sin2q13(Bcos d -Csin d)+D Measurement of x=P(nenm) and y=P(nenm) at fixed En/L gives an elipse in x-y plane. _ _ _ _ 8-fold degeneracy q13 q’13 gives a different ellipse.2-foldq13-d degeneracy • q13- dambiguity. • Mass hierarchy two-fold degeneracy:|Dm231|=|-Dm231| • q23degeneracy:sin22q23= sin22(p/2-q)23 ISS Plenary#1

  30. How to solve correlation and degeneracy? Use combination of different En, L or Golden+Silver channel Many scenarios are proposed ISS Plenary#1

  31. 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 ofddown to sin2 2q13 =0.02 ISS Plenary#1

  32. Example 2: 2 L’s to resolve degeneracy Synergy of NuFact-II(300km)+T2HK mass hierarchy removed Region; Single measurement OK 2nd L at MB=Magic Base Line(7500km) Staged approach One detector first, if d~p/3 If not, 2nd detector at MB ISS Plenary#1 P.Huber et al., hep-ph/0412199

  33. ISS Plenary#1

  34. 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 sin22q13 is large ? • What is the minimum NF energy that will deliver the physics (cost issue)? ISS Plenary#1

  35. 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) ISS Plenary#1

  36. 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 ISS Plenary#1

  37. 4. Summary • Issue a message to win broad community’s support • Review physics performance of future options forprecision 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 ISS Plenary#1

  38. On Michael Turner’s door at NSF ISS Plenary#1

  39. ISS Plenary#1

  40. The neutrino mixing matrix: 3 angles and a phased n3 Dm223= 2 10-3eV2 n2 n1 Dm212= 8 10-5 eV2 Normal Hierarchy or n2 n1 Dm212= 8 10-5 eV2 Dm223= 2 10-3eV2 n3 Inverted Hierarchy q23(atmospheric) = 450 , q12(solar) = 320 , q13(Chooz) < 130 Unknown or poorly known 13,phase ,sign of Dm213 ISS Plenary#1

  41. T2K PhaseII Phase II: 4 MW upgrade Phase II HK: 1000 kt JPARC- ~0.6GeV n beam 0.75 MW 50 GeV PS (2008 ) SK: 22.5 kt Kamioka J-PARC K2K~1.2 GeV n beam 0.01 MW 12 GeV PS (1999 2005) ISS Plenary#1

  42. ISS Plenary#1

  43. ISS Plenary#1

  44. ISS Plenary#1

  45. ISS Plenary#1

  46. Sensitivity depends on the true value of Dm2 ISS Plenary#1

  47. Mezzetto Beta-beam: sensitivity ISS Plenary#1

  48. Huber Comparison: BB/NF ISS Plenary#1

  49. Neutrino Oscillation Appearance Probability ISS Plenary#1

  50. ISS Plenary#1

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