1. Michael Smy UC Irvine Solar and Atmospheric Neutrinos 8 th International Workshop on Neutrino Factories, Superbeams & Betabeams Irvine, California, August 25 th 2006

2. Cast of Characters

3. 50kt Water Cherenkov Detector with 11,146 20”  PMTs located in Kamioka mine at 36.43 0 N latitude and 137.31 0 longitude ~2,400 m.w.e underground Super-Kamiokande April 1996-July 2001: (SK-I) Accident in November 2001 during maintenance Jan. 2003-Oct. 2005: SK-II (half PMT density) July 2006 – (SK-III) many physics topics; solar, atmospheric & accelerator ’s, proton decay Courtesy Y. Oyama

4. Super-K Is Repaired! Michael Smy, UC Irvine began in fall 2005… …now finished! Village of Dou near Atotsu Mine Entrance Mozumi Mine Entrance …despite some weather problems!

5. Sudbury Neutrino Observatory 1kt Heavy Water+ 7kt Light Water Cherenkov Detector with 9,438 8”  PMTs located in Creighton mine at 46.47 0 N latitude and 81.2 0 W longitude ~6,000 m.w.e underground November 1999-June 2001 (measurement with pure D 2 O) June 2001-October 2003 (NaCl dissolved to improve neutron eapture efficiency) ~April 2004- (with neutral current detector array) Mainly solar neutrinos

6. Other Experiments Homestake Soudan 2 MACRO SAGE Solar Solar Atmospheric Atmospheric Solar Solar

7. Neutrino Sources and Oscillations Mixing- Matrix: Michael Smy, UC Irvine

8. 2H2H p n e+e+ p I Solar Neutrinos Michael Smy, UC Irvine n e-e- p p 2H2H p 3 He p 7 Be 4 He 7 Be 4 He 8B8B p e-e- 7 Li e+e+ 4 He * 8 Be 4 He * 8 Be p 3 He 4 He p n e+e+

9. Solar Neutrino Detection - e only - D: Q = 1.445 MeV; good measurement of e energy, some direction info  (1 – 1/3 cos  ) - Cl: Q=0.8 MeV (radio-chemical) - Ga: Q=0.233 MeV (radio-chemical) - equal cross section for all active types - Q = 2.22 MeV - measures total 8 B flux from the Sun NC xx    npD ES    e−e− e−e− x - mainly sensitive to e, some  and  - strong directional sensitivity CC e−e− (n-1,p+1) (n,p)   e x Based on: K. Graham, ICHEP06 in SNO + in Cherenkov Detector

10. Solar Spectrum from Solar Model Michael Smy, UC Irvine KamLAND

11. Solar Candidates above 5 MeV Michael Smy, UC Irvine

12.  14 CC-NC separation cos  sun CC NC ES SNO Signal Extraction maximum likelihood fit of model PDF’s to data event variables R (radial position)  14 (isotropy) cos  sun and E(energy) ES separation don’t use E  “energy-unconstrained”  fit out CC spectrum! K. Graham, ICHEP06

13. Solar Problem Michael Smy, UC Irvine

14. SNO Results from NaCl Phase Flux Results CC 2176+/-78 ES 279+/-26 NC2010+/-85 #EVENTS 4722 candidate events 391 live days Neutrino Flavour Change! Day/Night Asymmetry Based on: K. Graham, ICHEP06

15. Solar Neutrino Problem Explained by SNO and Super-K as Neutrino Flavor Conversion!

16. Recoil Electron Spectrum Michael Smy, UC Irvine 8 B MC only  8 B =2.33x10 6 /cm 2 s  hep =15x10 3 /cm 2 s MC: A DN =-1.8±1.6±1.2% A DN =-6.3±4.3%(stat)

17. SNO CC Spectrum no significant sterile or NSI effects Based on: K. Graham, ICHEP06

18. Solar 95% 99.73% KamLAND Solar+KamLAND Michael Smy, UC Irvine Solar Neutrino Oscillation Parameters

19. Solar Neutrino Future Measurements SNO NCD phase will produce smaller error on NC Lower energy real-time 8 B neutrino measurement in SK-III (and SNO) studies transition from vacuum oscillation to matter-dominated oscillations Borexino (and KamLAND) measure 7 Be flux SNO+ looks at pep flux various projects to measure pp flux in real time

20. II Atmospheric Neutrinos/Neutrino Beams Michael Smy, UC Irvine

21. Atmosph. Oscillations 1489 live days of SK-I and 804 live days of SK-II only muon-like single ring events cut out low energy events and events near horizon (poor resolution in L): uncertainty in L/E is set to be <70% best fit  ↔  : sin 2 2  =1.00,  m 2 =2.3x10 -3 eV 2,  2 =83.9/83dof -decay:  2 =23.2 or 4.8  -decoher.:  2 =27.6 or 5.3  oscill. decay decoh. Michael Smy, UC Irvine

22. All SK Atmospheric Data Samples FC 1ring e-like FC mring e-like FC 1ring -like FC mring -like PC stop PC thru up-  stop P lep Sub-GeV Multi-GeV CC e CC  38 event type and mom. bins x 10 zenith bins x 2 exp.  760 bins! up-  thru up-  show. slightly slightly better constraint on mixing angle… … but solar osc. terms affects electron samples true, even if  13 =0 especially affects deviation from max. mixing include solar term best-fit : sin 2  23 = 0.52 (sin 2 2  23 = 0.9984) Best Fit:  m 2 = 2.5 x 10 -3 eV 2 sin 2 2  = 1.00  2 = 839.7 / 755 dof (18%) Preliminary Michael Smy, UC Irvine

23. Zenith angle distributions (SK-I + SK-II) Sub-GeV e-like Sub-GeV -like Multi-GeV e-like Multi-GeV -like multi-ring e-like multi-ring -like PC stoppingPC thru-going UP through non-showering UP stopping showering data MC (no osc.) MC (best-fit w/ solar terms) Preliminary Michael Smy, UC Irvine

24. Three Flavour Oscillation Analysis 1489d; Normal Hierarchy 1489d; Inverse Hierarchy

25. Sterile Admixture Limit

26. Other Atmospheric Measurements PRD 72, 052005 (2005)

27. Future Atmospheric Measurements SK-III will improve L/E measurements and  appearance analaysis MINOS distinguishes atmospheric neutrinos from antineutrinos INO, a 50kt magnet. iron experiment A. Samanta, ICTP 2006/A. Dighe, ICHEP 2006 Magnetic field ~ 1 Tesla along  y-direction P. Litchfield, Neutrino 2006

28. Conclusion we learned a lot about neutrino oscillations from solar and atmospheric neutrinos (everything we know, except  m 2 12 !) still not finished, so stay tuned