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Recent Neutrino Oscillation Results and Future

Jun Cao Institute of High Energy Physics. Recent Neutrino Oscillation Results and Future. Neutrinos. There are 3 famailes of massless Neutrinos in the SM. There are 300 neutrinos/cm 3 in the universe. Neutrino Oscillation. Solar neutrino Homestake Exp. Atmospheric neutrino

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Recent Neutrino Oscillation Results and Future

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  1. Jun Cao Institute of High Energy Physics Recent Neutrino Oscillation Results and Future

  2. Neutrinos There are 3 famailes of massless Neutrinos in the SM. There are 300 neutrinos/cm3 in the universe.

  3. Neutrino Oscillation Solar neutrino Homestake Exp. Atmospheric neutrino Super-K exp. Neutrino oscillation means neutrinos are massive.

  4. SNO in Canada, solar, in 2001 KamLAND in Japan, reactor, first in 2002 K2K in Japan, 2004 Accelerator MINOS in US, first in 2006 Accelerator

  5. Neutrino Mixing In a 3- framework 12 ~ 34 m232 ~ 7.610-5eV2 Solar Reactor 13 = ? CP = ? Reactor Accelerator 23 ~ 45 m232 ~ 2.4310-3 eV2 Atmospheric Accelerator 0

  6. Neutrino Puzzles 10 Years ago, neutrino oscillation was well established. Is 13non-zero? Which neutrino is heavier? (mass hierarchy) Is there CP violation? How many kinds of neutrinos? (Unitarity) Are there sterile neutrinos? What's the mass of neutrinos? Is neutrino its own anti-particle? Abnormal magnetic moment? Can we detect relic neutrino from Big Bang? Also of great interests in astrophysics, cosmology, geology, etc.

  7. How large is 13? PRD 62, 072002 sin2213<0.16 sin2213~0.04 Allowed region Fogli et al., hep-ph/0506307 Gonzalez-Garcia et al., JHEP1004:056, 2010 sin2213~0.04 sin2213~0.08, non-zero 2 Fogli et al., J.Phys.Conf.Ser.203:012103 (2010)

  8. How to measure 13 Accelerator (appearance) Related with CPV and matter effect T2K 4MeV ͞e Reactor (disappearance) Clean in physics, only related to 13 Precisionmeasurement

  9. Ken Sakashita, ICHEP 2012

  10. T2K Indication In Jun., 2011, 6 eevents, 1.50.3 bkg expected. (1.431020 POT) 13 non-zero probability 99.3% (2.5  significance)

  11. T2K updated in Jul. 2012 Ken Sakashita, ICHEP 2012 31020 POT 11 ecandidates 3.22 expected w/o oscillation

  12. IndicationfromMINOS

  13. MINOS updated in Jul. 2012 Anti-neutrino In 2011: antineutrino differ from neutrino (98% C.L.): CPT violation? Neutrino Most precise m2 measurement

  14. Precision Measurement at Reactors Major sources of uncertainties: • Reactor related ~2% • Detector related ~2% • Background 1~3% Lessons from past experience: • CHOOZ: Good Gd-LS • Palo Verde: Better shielding • KamLAND: No fiducial cut Near-far relative measurement Mikaelyan and Sinev, hep-ex/9908047

  15. Proposed Reactor Experiments Krasnoyarsk, Russia Braidwood, USA KASKA, Japan RENO, Korea Double Chooz, France Diablo Canyon, USA Daya Bay, China Angra, Brazil • 8 proposals, most in 2003 (3 on-going) • Fundmental parameter • Gateway to -CPV and Mass Hierachy measurements • Less expensive

  16. The Daya Bay Experiment • 6 reactor cores, 17.4 GWth • Relative measurement • 2 near sites, 1 far site • Multiple detector modules • Good cosmic shielding • 250 m.w.e@ near sites • 860 m.w.e @ far site • Redundancy 3km tunnel

  17. Double Chooz in France Daya Bay Double Chooz

  18. RENO in Korea Daya Bay 6 cores 16.5 GW 16t, 120 MWE RENO Double Chooz 16t, 450 MWE

  19. Three on-going experiments Huber et al. JHEP 0911:044, 2009

  20. Prompt signal Delayed signal, Capture on H (2.2 MeV) or Gd (8 MeV), ~30s Detecting Reactor Antineutrino Inverse beta decay Peak at ~4 MeV 0.1% Gd by weight Major backgrounds: • Cosmogenic neutron/isotopes • 8He/9Li • fast neutron • Ambient radioactivity • accidental coincidence Capture on H Capture on Gd

  21. Similar Detector Design Water • Shield radioactivity and cosmogenic neutron • Cherekov detector for muon RPC or Plastic scintillator • muon veto Three-zone neutrino detector • Target: Gd-loaded LS • 8-20 t for neutrino • -catcher: normal LS • 20-30 t for energy containment • Buffer shielding: oil • 40-100 t for shielding

  22. Similar Detector Design Water • Shield radioactivity and cosmogenic neutron • Cherekov detector for muon RPC or Plastic scintillator • muon veto Three-zone neutrino detector • Target: Gd-loaded LS • 8-20 t for neutrino • -catcher: normal LS • 20-30 t for energy containment • Buffer shielding: oil • 40-100 t for shielding Daya Bay Reflective panels

  23. DYB:Tunnel and Underground Lab.

  24. Assembly of Antineutrino Detector Daya Bay

  25. Assembly of Antineutrino Detector

  26. Muon System Installation

  27. Liquid Scintillator Hall Mineral Oil 185 ton 0.1% Gd-LS Liquid Scintillator Filling Equipment LS mixing equipment ISO tank equiped with load cell. Target mass errorr ~0.1% Daya Bay

  28. Detector Installation

  29. Neutrino Selections 0.7-12 MeV 6-12 MeV Prompt candidate Delayed candidate Reactor Neutrinos (Prompt) Neutrons (Delayed ) Correlated Events in 1-200 s

  30. Daya Bay Results 2011-11-5 Mar.8, 2012, with 55 day data sin2213=0.0920.016(stat)0.005(syst) 5.2 σ for non-zero θ13 2011-12-24 2011-8-15 Jun.4, 2012, with 139 day data sin2213=0.0890.010(stat)0.005(syst) 7.7 σ for non-zero θ13

  31. Side-by-side Comparison Data set: 2011.9 to 2012.5 This check shows that syst. are under control, and will eventually "measure" the syst. error • 0.2%detector-related uncertainty (relative measurement) • Expected ratio of neutrino events: R(AD1/AD2) = 0.982 • The ratio is not 1 because of target mass, baseline, etc. • Measured ratio: 0.987  0.004(stat)  0.003(syst)

  32. Functional Identical Detectors • "Same batch" of liquid scintillator 5x40 t Gd-LS, circulated 20 t filling tank 200 t LS, circulated 4-m AV in pairs Assembly in pairs • Why systematics is so small?c.f. An et al. NIM. A 685 (2012) 78 • Idea of "identical detectors" throughout the procedures of design / fabrication / assembly / filling. • For example: Inner Acrylic Vessel, designed D=31205 mm • Variation of D by geometry survey=1.7mm, Var. of volume: 0.17% • Target mass var. by load cell measurement during filling: 0.19%

  33. Daily Rate: Evidence of Deficit Predictions are absolute, multiplied by a global normalization factor from the fitting.(to account for the absolute  flux and absolute detection eff. uncertainty)

  34. Daya Bay Results (2012.6) R = 0.944 ± 0.007 (stat) ± 0.003 (syst) sin22θ13=0.089±0.010(stat)±0.005(syst)

  35. Double Chooz Results sin22q13=0.0860.041(Stat)0.030(Syst), 1.7σ for non-zero θ13 sin22q13=0.1090.030(Stat)0.025(Syst), 3.1σ for non-zero θ13 Far detector starts data taking at the beginning of 2011 First results in Nov. 2011 based on 85.6 days of data Updated results on Jun.4, 2012, based on 228 days of data

  36. Double Chooz Results (2012.6)

  37. RENO sin22q13=0.1130.013(Stat)0.019(Syst), 4. 9σ for non-zero θ13 Data taking started on Aug. 11, 2011 First physics results based on 228 days data taking (up to Mar. 25, 2012) released on April 3, 2012, revised on April 8, 2012:

  38. RENO Results (2012.4) sin22θ13=0.113±0.013(stat)±0.019(syst) R = 0.920 ± 0.009(stat) ± 0.014 (syst) 4.9  for non-zero value of 13

  39. Global Picture Exclusion of non-zero 13 (2010) 2011.6 2011.7 2011.11 by S. Jetter

  40. Global Picture Exclusion of non-zero 13 (2010) 2011.6 2011.7 2011.11 2012.3 by S. Jetter

  41. Global Picture A consistent picture Exclusion of non-zero 13 (2010) 2011.6 2012.6 2011.7 2012.6 2012.6 2011.11 2012.6 (7.7) 2012.3 2012.4 by S. Jetter

  42. Future 13 • Daya Bay • Installation of remaining two detectors this summer • Full data taking this fall • Current precision of sin221312.5%, 3 year：4-5% • RENO • Continue data taking • 3 year precision of sin2213 : ~10% • Double Chooz • Near site detector installation underway • Full data taking(by the end of) next year • 3 year precision of sin2213 : ~15% • Direct measurement m231, Reactor  spectrum, Reactor  anomaly, cosmogenic n/isotope yield, non-standard interaction, ...

  43. Next Step: DayaBay-II Experiment • 20 kton LS detector • 3%/E̅resolution • Rich physics • Mass hierarchy • Precision measurement of 4 oscillation parameters to <1% • Supernovae neutrino • Geoneutrino • Sterile neutrino • Atmospheric neutrinos • Exotic searches 60 km Daya Bay II Daya Bay Talk by Y.F. Wang at ICFA seminar 2008, Neutel 2011; by J. Cao at Nutel 2009, NuTurn 2012 ; Paper by L. Zhan, Y.F. Wang, J. Cao, L.J. Wen, PRD78:111103,2008; PRD79:073007,2009

  44. The reactors and possible sites Site 2 Lufeng Huizhou Daya Bay Site 1 Taishan Yangjiang

  45. T2K+NOvA 30% chance to determine Mass Hierachy

  46. LBNE Approved 10 kT LAr detector on ground

  47. Hyper-K

  48. PINGU Phased Icecube Next Generation Upgrade

  49. Indian Neutrino observatory: INO three 17kt modules, each 161614.4m3 150 iron plates, each 5.6 cm thick • 50kt magnetized iron plate interleaved by RPC for • Sign sensitive atmospheric neutrinos (stage I) • long baseline neutrino beams • (stage II) • Features: • Far detector at magic baselines: • CERN to INO: 7152 km • JPARC to INO: 6556 km • RAL to INO: 7653 km • Muons fully contained up to 20 GeV • Good charge resolution, B=1.5 T • Good tracking/Energy/time resolution

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