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

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

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

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

5. 5 Neutrino Mixing  23 ~ 45   m 2 32 ~ 2.43  10 -3 eV 2 Atmospheric Accelerator  12 ~ 34   m 2 32 ~ 7.6  10 -5 eV 2 Solar Reactor 0   13 = ?  CP = ? Reactor Accelerator In a 3- framework

6. 6 Neutrino Puzzles 10 Years ago, neutrino oscillation was well established.  Is  13 non-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. 7 How large is  13 ? PRD 62, 072002 Allowed region Fogli et al., J.Phys.Conf.Ser.203:012103 (2010) Gonzalez-Garcia et al., JHEP1004:056, 2010 Fogli et al., hep-ph/0506307 sin 2 2  13 <0.16 sin 2 2  13 ~0.04 sin 2 2  13 ~0.08, non-zero 2 

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

9. 9 Ken Sakashita, ICHEP 2012

10. 10 T2K Indication In Jun., 2011,  6 e events, 1.5  0.3 bkg expected. (1.43  10 20 POT)   13 non-zero probability 99.3% (2.5  significance)

11. 1 T2K updated in Jul. 2012 3  10 20 POT 11 e candidates 3.22 expected w/o oscillation Ken Sakashita, ICHEP 2012

12. 12

13. 13 Indication from MINOS

14. 14 MINOS updated in Jul. 2012 In 2011: antineutrino differ from neutrino (98% C.L.): CPT violation? Most precise  m 2 measurement Neutrino Anti-neutrino

15. 15 Precision Measurement at Reactors ParameterErrorNear-far Reaction cross section1.9 %0 Energy released per fission0.6 %0 Reactor power0.7 % ~0.1% Number of protons0.8 % < 0.3% Detection efficiency1.5 % 0.2~0.6% CHOOZ Combined2.7 %< 0.6% 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

16. 16 Proposed Reactor Experiments Angra, Brazil Diablo Canyon, USA Braidwood, USA Double Chooz, France Krasnoyarsk, Russia KASKA, Japan Daya Bay, China RENO, Korea 8 proposals, most in 2003 (3 on-going) Fundmental parameter Gateway to -CPV and Mass Hierachy measurements Less expensive

17. 17 The Daya Bay Experiment 6 reactor cores, 17.4 GW th 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

18. 18 Double Chooz in France Daya Bay Double Chooz

19. 19 RENO in Korea 6 cores 16.5 GW 16t, 450 MWE 16t, 120 MWE Daya Bay RENO Double Chooz

20. 20 Three on-going experiments Experiment Power (GW) Detector(t) Near/Far Overburden (m.w.e.) Near/Far Sensitivity (3y,90%CL) Daya Bay17.440 / 80250 / 860~ 0.008 Double Chooz 8.5 8 / 8120 / 300~ 0.03 RENO16.516 / 16120 / 450~ 0.02 Huber et al. JHEP 0911:044, 2009

21. 21 Detecting Reactor Antineutrino Delayed signal, Capture on H (2.2 MeV) or Gd (8 MeV), ~30  s Prompt signal Peak at ~4 MeV Capture on H Capture on Gd Inverse beta decay Major backgrounds:  Cosmogenic neutron/isotopes  8 He/ 9 Li  fast neutron  Ambient radioactivity  accidental coincidence 0.1% Gd by weight

22. 2 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

23. 23 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 PMTCoveragepe yieldpe yield/Coverage Daya Bay192 8"~6%163 pe/MeV 1.77 RENO354 10"~15%230 pe/MeV 1 Double Chooz390 10"~16%200 pe/MeV 0.81

24. 24 DYB:Tunnel and Underground Lab.

25. 25 Assembly of Antineutrino Detector J. Cao (IHEP)Daya Bay 25

26. 26 Assembly of Antineutrino Detector

27. 27 Muon System Installation

28. 28 Liquid Scintillator Hall Daya Bay 28 LS mixing equipment 185 ton 0.1% Gd-LS Liquid Scintillator Mineral Oil Filling Equipment ISO tank equiped with load cell. Target mass errorr ~0.1%

29. 29 Detector Installation

30. 30 Neutrino Selections 0.7-12 MeV 6-12 MeV Prompt candidate Delayed candidate Correlated Events in 1-200  s Reactor Neutrinos (Prompt) Neutrons (Delayed )

31. 31 Daya Bay Results 2011-8-15 2011-11-5 2011-12-24 Mar.8, 2012, with 55 day data sin 2 2  13 =0.092  0.016(stat)  0.005(syst) 5.2 σ for non-zero θ 13 Jun.4, 2012, with 139 day data sin 2 2  13 =0.089  0.010(stat)  0.005(syst) 7.7 σ for non-zero θ 13

32. 32 Side-by-side Comparison  0.2%  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) This check shows that syst. are under control, and will eventually "measure" the syst. error Data set: 2011.9 to 2012.5

33. 3  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% Functional Identical Detectors DiameterIAV1IAV2IAV3IAV4IAV5IAV6 Surveyed(mm)3123.123121.713121.773119.653125.113121.56 Variation (mm)1.32.02.31.81.52.3  "Same batch" of liquid scintillator 5x40 t Gd-LS, circulated 200 t LS, circulated 4-m AV in pairs Assembly in pairs 20 t filling tank

34. 34 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)

35. 35 Daya Bay Results (2012.6) R = 0.944 ± 0.007 (stat) ± 0.003 (syst)sin 2 2θ 13 =0.089±0.010(stat)±0.005(syst)

36. 36 Double Chooz Results  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 sin 2 2  13 =0.086  0.041(Stat)  0.030(Syst), 1.7σ for non-zero θ 13 sin 2 2  13 =0.109  0.030(Stat)  0.025(Syst), 3.1σ for non-zero θ 13

37. 37 Double Chooz Results (2012.6)

38. 38 RENO  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: sin 2 2  13 =0.113  0.013(Stat)  0.019(Syst), 4. 9σ for non-zero θ 13

39. 39 RENO Results (2012.4) R = 0.920 ± 0.009(stat) ± 0.014 (syst) sin 2 2θ 13 =0.113±0.013(stat)±0.019(syst) 4.9  for non-zero value of  13

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

41. 41 Global Picture 2012.3 Exclusion of non-zero  13 by S. Jetter (2010) 2011.6 2011.7 2011.11

42. 42 Global Picture 2012.4 2012.6 (7.7  ) 2012.6 Exclusion of non-zero  13 by S. Jetter A consistent picture (2010) 2011.6 2011.7 2011.11 2012.3

43. 43 Future  13  Daya Bay  Installation of remaining two detectors this summer  Full data taking this fall  Current precision of sin 2 2  13 12.5%, 3 year ： 4-5%  RENO  Continue data taking  3 year precision of sin 2 2  13 : ~10%  Double Chooz  Near site detector installation underway  Full data taking(by the end of) next year  3 year precision of sin 2 2  13 : ~15%  Direct measurement  m 2 31, Reactor spectrum, Reactor anomaly, cosmogenic n/isotope yield, non-standard interaction,...

44. 4 Next Step: Daya Bay-II Experiment Daya Bay 60 km Daya Bay II  20 kton LS detector  3%/  E ̅ resolution  Rich physics  Mass hierarchy  Precision measurement of 4 oscillation parameters to <1%  Supernovae neutrino  Geoneutrino  Sterile neutrino  Atmospheric neutrinos  Exotic searches 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

45. 45 The reactors and possible sites Daya BayHuizhouLufengYangjiangTaishan StatusOperationalPlanned Under construction Power17.4 GW 18.4 GW 45 Daya Bay Huizhou Lufeng Site 2 Site 1 Yangjiang Taishan

46. 46  30% chance to determine Mass Hierachy T2K+NOvA

47. 47 LBNE Approved 10 kT LAr detector on ground

48. 48 Hyper-K

49. 49  Phased Icecube Next Generation Upgrade PINGU

50. 50 Indian Neutrino observatory: INO  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 three 17kt modules, each 16  16  14.4m 3 150 iron plates, each 5.6 cm thick

51. 51 2020-2022 Projected Sensitivity to MH

52. 52 Summary  Daya Bay experiment discovered the new oscillation and proved  13 is quite large.  We can measure the MH and CPV in our lifetime!  Six results from 3 reactor exp., 2 accelerator exp., and fit from solar+KamLAND are consistent.  Precision on sin 2 2  13 will be improved to 4-5%  In the next 10 years, we will see data from the next generation of neutrino oscillation experiments  Mass hierarchy, maybe CPV  Precision measurement of mixing parameters up to < 1% level  unitarity test of the mixing matrix

53. Thanks !