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Agenda for Meeting

Agenda for Meeting. Neutrino Oscillations Overview - Mike Shaevitz (20 min) Offaxis Experiments: Capabilities and Comparisons - Mark Messier (20 min) Detector Technologies - Adam Para NuMI Offaxis Beam and Detector Performance Requirements - Stan Wojcicki (20 min)

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Agenda for Meeting

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  1. Agenda for Meeting • Neutrino Oscillations Overview - Mike Shaevitz (20 min) • Offaxis Experiments: Capabilities and Comparisons - Mark Messier (20 min) • Detector Technologies - Adam Para • NuMI Offaxis Beam and Detector Performance Requirements - Stan Wojcicki (20 min) • Plans, Schedules, and Requests for Guidance - Ed Blucher (20 min)

  2. Neutrino OscillationsNear and Far Term Prospective Michael Shaevitz Columbia University • Current Status and Present Program • Solar: Kamland, Super-K, SNO, Borexino • Atmospheric: K2K, MINOS (Icarus, Opera at CERN) • LSND: MiniBooNE • Near Term Prospects (this decade) and Possibilities • Offaxis experiments: JHF-SK (Japan), NuMI Offaxis • Reactor Experiments • Further Term Prospects and Possibilities • Superbeam experiments • Possible longbaseline to NUSL with proton decay • Neutrino Factory

  3. Neutrino Oscillations Difficult to probe small neutrino masses (<1 eV)  Use neutrino oscillations • Neutrinos have (different) mass  Dm122 = m12 – m22 , Dm232 = m22 – m32 • The Weak Eigenstates are a mixture of Mass Eigenstates Experimentally, need to measure the mass differences and the mixing parameters

  4. Why Are Neutrino Oscillation Measurements Important? • Gives a window on physics at high mass scales: unification, physics of flavor, and extra dimensions • Why are the neutrino masses so small? • Are there additional “sterile” neutrinos? • Why are their mixings so large? • Is there CP violation, T violation, or CPT violation in the leptons? • Is there a connection between the lepton and baryon sector? • Are neutrinos connected to the matter-antimatter asymmetry in the universe? • Neutrino masses and mixing are important to understanding astrophysical models of: • Supernovae, galactic structure formation, etc.

  5. Method to Measure Oscillation Parameters • Neutrino oscillation method: start with a pure nm beam at L=0, then look for a ne component as it travels a distance L. • If you see no signal and limit oscillation with Posc < P @ 90% CLthen set an excluded region in the (Dm2,sin22q) plane. • If you see an oscillation signal with Posc = P  dP then carve out an allowed region in (Dm2,sin22q) plane.

  6. Current Situation: Three Experimental Indications for Neutrino Oscillations Atmospheric NeutrinosL = 15 to 12,000 km E =300 to 2000 MeV LSND ExperimentL = 30m E = ~40 MeV Solar NeutrinosL = 108 km E =0.3 to 15 MeV Dm2 = ~ 2 to 8 10-5eV2ProbOSC = ~100% Dm2 = .3 to 3 eV2ProbOSC = 0.3 % Dm2 = ~ 1 to 7 10-3 eV2 ProbOSC = ~100%

  7. MiniBooNE Questions addressed by Current Experiments: • LSND Dm2 • Determination if osc. • Measure Dm2/sin22q • Atmospheric Dm2 • Know if nm ntorns • Measure Dm2/sin22q • Maybe see nmne • CERN observe nt • Solar Dm2 • Restrictions to one solar solution • Know if ne nm,torns • Measure Dm2 NuMI/MINOS,(K2K,CERN) SuperK,KamLAND,SNO,Borexino

  8. All solar experiments see too few solar neutrinos SNO sees expected total neutrino flux (ne+nm+nt)  ne  nm+nt mostly Solar Oscillation Experiments • New Kamland Reactor Results: • Detect too few anti-ne events from reactors around Japan • 54 events observed, 866 expected  Osc. Probability = 0.39  0.09 • Accurate measurement of Dm2Solar  7x10-5 eV2

  9. Atmospheric Oscillation Region:NuMI/MINOS Experiment • Probe for nmne appearance • Sensitivity at the level of sin2213> 0.06 @ 90%CL • From nm disappearance signal • Measure Dm232 to ~10% sin2

  10. MiniBooNE With ~two years of running MiniBooNE will completely include or exclude the entire LSND signal region at the 5s level. • Expected events • 500,000 nm CC quasi-elastic • ~1000 extra ne’s if LSND correct • If MiniBooNE sees nme oscillations then need to enhance oscillation program • Three distinct Dm2 values  Indicates some unexpected physics • More than three types of neutrinos – extra “sterile” neutrino types • Neutrinos and antineutrinos have different masses • Need more long and short-baseline exps probing high Dm2 • Follow-up BooNE experiment with two detectors • Moderate short-baseline ntappearance experiments

  11. Near Term Steps of a Neutrino Oscillation Program <0.2 • Measure sin22q13 • Last unmeasured element in the mixing matrix • Sets the scale for being able to observe CP violation and matter effects • Off-axis experiments • Off-axis gives beam with narrow energy distribution that is tunable osc. max • Fermilab NuMI to Offaxis detector • Japanese JHF to SuperK experiment • Reactor Experiments • Provides complementary information to offaxis searches • Proposals being developed in US, Japan, and Europe • Determine the sign of m223 from matter effects in the earth • Only available with NuMI off axis measurements • Probe for CP Violation (d parameter) • Compare measurements for neutrinos with antineutrinos

  12. 1200m d d 3  90% CL 3 yrs Measurements of sin2213 Goal: Design experiments with sensitivity at the sin2213 0.01 level • Appearance nmne(Offaxis Exps.) • Measurement difficult: • Look for small number of events over comparable background • Disappearance nene(Reactor Exps) • Measurement difficult: • Look for slight change in overall neutrino rate

  13. By going offaxis, beam energy is reduced and spectrum becomes very sharp Allows experiment to pick an energy for the maximum oscillation signal Removes the high-energy flux that contributes to background "Not magic but relativistic kinematics" Allows experiment to use the NuMI beam for several experiments simultaneously Minos nm disappearance on-axis Offaxis nmne search Concept of the Offaxis Beam at 730 km "Off-axis"

  14. Further Term: Neutrino Superbeam Experiments If sin2213> 0.01 (x20 below current limit), design experiment to measure d (CP violation parameter) and the sign of m223 through matter effects • Need high intensity proton sources coupled with very large detectors • Current ideas for experiments: • JHF Phase II to HyperK detector • <En>  700 MeV beam using 4MW JHF to 1000kton water Cerenkov • CP violation 3s discovery reach for sin22q13>0.02 (2yr for nu’s and 6 yrs for nubars) • BNL: Upgraded AGS to NUSL • Very longbaseline with wide-band beam gives dramatically large effectsUse 1MW AGS beam with 0.5<En<5 GeV and 500 kton water Cerenkov • Fermilab: Upgraded Proton Driver and Beam • Upgrade proton driver (1-4MW) and upgraded NuMI beam combined with 500 kton detector • Possible new longbaseline beam to NUSL with large detector

  15. Neutrino Oscillation Roadmap • Stage 0: Current near term program • Solar neutrino m212 measured to 5-10% • NuMI (K2K, CERN) checks atmospheric oscillations and measures m223 to about 10% • MiniBooNE makes definitive check of LSND and measures associated m2 • Stage 1 - Observe sin2213 - Maybe also initial matter and CP violation effects • NuMI /MINOS on-axis probes sin2213> 0.06 @ 90%CL • NuMI/JHF offaxis with 20-50 kton detectors to probe sin2213> 0.01 @ 3s level • Two-detector, longbaseline reactor experiments probe at the sin2213> 0.01 level • Stage 2 - Observe CP violation and determine the sign of m223 with conventional superbeams and very large detectors (~500 ktons) - May be coupled with underground lab (NUSL...) and proton decay • Must have sin2213> 0.01 • Need to measure P(e) then P(e) or use constraints from a precision reactor e  e • Need increased rate (especially for n’s)  Need high intensity proton sources • Stage 3 - Measurements with a Neutrino Factory • Map out CP violation with precision for sin2213> 0.01 • Probe e transitions down to sin2213> 0.001

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