1. DARK 2007 SydneySept 28 th,2007Page 1 Knowing the Universe from a Hole in the Ground Particle-Astrophysics Research at SNO & SNOLab T. Noble, Queen’s University The Past The Sudbury Neutrino Observatory ( SNO ) Current Status The Future SNOLab Physics potential Status

2. DARK 2007 SydneySept 28 th,2007Page 2 SNO Status Data acquisition, NCD phase, complete November 28, 2006 Heavy water returned by May, 2007 Analysis proceeding well. Primary focus: –NC and CC data from NCD Phase. –Low Energy Threshold Analysis (LETA) from previous phases. Analysis will continue until April 2009 Main Results: 30 year old Solar Neutrino Puzzle solved… Strong evidence for weak flavor change (> 7 sigma). Solar Neutrino Oscillations! Neutrinos have finite mass, mix… Total Flux in excellent agreement with expectations from solar models We have a good understanding of the fusion processes in the Sun…

3. DARK 2007 SydneySept 28 th,2007Page 3 Getting The Last Drop Out!

4. DARK 2007 SydneySept 28 th,2007Page 4 SNO data taking is Complete. The Experiment is Decommissioned. What is the future programme for Particle Astrophysics at this Facility?

5. DARK 2007 SydneySept 28 th,2007Page 5 SNOLAB A new International Facility for Underground Science.

6. DARK 2007 SydneySept 28 th,2007Page 6 Physics Program Direct Search for Dark Matter 85% of mass in universe + MSSM DEAP/CLEAN, PICASSO, SuperCDMS MiniClean?, LUX? Neutrino Properties –Neutrinoless double beta decay Majorana, mass scale, hierarchy EXO, SNO+ –Solar neutrinos mixing parameters, solar/stellar –Supernova neutrinos physics, new physics –Reactor neutrinos SNO+, HALO ? Geophysics –Geo-neutrinos Earth’s heat flow SNO+ –Seismology seismic wave propagation PUPS Biology ~25 letters of interest received…Initial suite of experiments recommended by an International Experiment Advisory Committee.

7. DARK 2007 SydneySept 28 th,2007Page 7 What is required to advance these areas of science? All require very low background environment –Implies deep site –Clean lab Some projects require big detector so some spaces must be large Many projects use noble liquids or gases which raise safety concerns, and require a dedicated and isolated space.

8. DARK 2007 SydneySept 28 th,2007Page 8 The Requirement for SNOLAB depth Phys.Rev. D73 (2006) 053004 Mei, D.M. and Hime, A. SNOLAB depth allows 10 -47 cm 2 cross-section sensitivity for dark matter Simplest experiment is with passive shielding afforded by rock at deep site

9. DARK 2007 SydneySept 28 th,2007Page 9 SNO: The Sudbury Neutrino Observatory

10. DARK 2007 SydneySept 28 th,2007Page 10 Existing SNO Facility SNOLAB SNOLAB Workshop 22-23 August 2007

11. DARK 2007 SydneySept 28 th,2007Page 11 Existing SNO Facility Phase I Relocate -Lab Entry -Personnel Facilities Utility Area - Chiller - Generator SNOLAB SNOLAB Workshop 22-23 August 2007

12. DARK 2007 SydneySept 28 th,2007Page 12 Existing SNO Facility Phase I Relocate -Lab Entry -Personnel Facilities Utility Area - Chiller - Generator Phase II SNOLAB SNOLAB Workshop 22-23 August 2007 * Excavation began Fall 2004, completed May 2007 * Outfitting began June 2007 * Funding announced August 07 * Construction began June 07

13. DARK 2007 SydneySept 28 th,2007Page 13 SNOLAB Underground facilities SNO Rectangular Hall Ladder Utilities

14. DARK 2007 SydneySept 28 th,2007Page 14 Laboratory Space SNOLAB Workshop 22-23 August 2007

15. DARK 2007 SydneySept 28 th,2007Page 15 0 υββ at SNOLAB SNO+ & EXO gas

16. DARK 2007 SydneySept 28 th,2007Page 16 SNO+ (SNO with Liquid Scintillator) heavy water is returned replace with liquid scintillator and use existing SNO apparatus Inexpensive, could be collecting data soon! What can be measured? low energy solar neutrinos - pep, CNO, 7 Be geo-neutrinos - anti-neutrinos from U/Th reactor neutrinos - Bruce and Darlington live for supernova potential for large mass 0υbb decay experiment with 150 Nd What are the challenges? -some re-engineering of experiment -purification of scintillator

17. DARK 2007 SydneySept 28 th,2007Page 17 150 Nd Option 3.37 MeV endpoint (9.7 ± 0.7 ± 1.0) × 10 18 yr 2  half-life (measured by NEMO-III) isotopic abundance 5.6% 1% natural Nd-loaded liquid scintillator in SNO+ has 560 kg of 150 Nd compared to 37 g in NEMO-III !! Isotopic Enrichment: –SuperNEMO and SNO+, MOON and DCBA are supporting efforts to maintain an existing French AVLIS facility that is capable of making 100’s of kg of enriched Nd

18. DARK 2007 SydneySept 28 th,2007Page 18 0 : 1000 events per year with 1% natural Nd-loaded liquid scintillator in SNO+ Poor energy resolution compensated by high statistics Test = 0.150 eV maximum likelihood statistical test of the shape to extract 0 and 2 components…~240 units of  2 significance after only 1 year! Klapdor-Kleingrothaus et al., Phys. Lett. B 586, 198, (2004) simulation: one year of data

19. DARK 2007 SydneySept 28 th,2007Page 19 SNO+ Double Beta Spectrum 1 yr, 500 kg isotope, m = 150 meV

20. DARK 2007 SydneySept 28 th,2007Page 20 Statistical Sensitivity in SNO+ 500 kg isotope 56 kg isotope 3 sigma detection on at least 5 out of 10 fake data sets 2 /0 decay rates are from Elliott & Vogel, Ann. Rev. Nucl. Part. Sci. 52, 115 (2002)

21. DARK 2007 SydneySept 28 th,2007Page 21 SNO+ vs. Super-Kamiokande CC:(260) 41% (7000) 91% (30) 4.7% (10) 1.5% NC: (60) 9.3% (410) 5% (270) 42% ES: (12) 1.9% (300) 4% SN Neutrino Detection in SNO+

22. DARK 2007 SydneySept 28 th,2007Page 22 Farther in the future: EXO GAS: 200 Kg Xe TPC with Barium tagging technique

23. DARK 2007 SydneySept 28 th,2007Page 23 Dark Matter at SNOLAB DEAP/Clean, MiniClean, PICASSO & SuperCDMS

24. DARK 2007 SydneySept 28 th,2007Page 24 DEAP/CLEAN Liquid Argon Pulse Shape Discrimination of Scintillation light 1000 Kg Fiducial Spin-Independent

25. DARK 2007 SydneySept 28 th,2007Page 25 Why Argon and Pulse Shape Discrimination? Highly sensitive and inexpensive technique to scale up to tonne scales.

26. DARK 2007 SydneySept 28 th,2007Page 26

27. DARK 2007 SydneySept 28 th,2007Page 27 Deap/CLEAN Physics potential

28. DARK 2007 SydneySept 28 th,2007Page 28 Picasso Superheated Droplet Detector Detector consists of tiny (5 to 100  m) halocarbon liquid droplets (C 4 F 10 ) embedded in a gel. The droplets are superheated - maintained at a temperature higher than their boiling point.

29. DARK 2007 SydneySept 28 th,2007Page 29 When a nuclear recoil (from WIMP, or neutron interaction, or alpha) deposits a spike of heat into droplet, it rapidly evaporates. The evaporating bubble creates a sound shock wave, which can be recorded by a sensitive microphone. Detector Operation A bubble forms iff the particle creates a heat spike with enough energy E min deposited within R min Mainly sensitive to heavily ionizing particles

30. DARK 2007 SydneySept 28 th,2007Page 30 Sensitivity: Operate over this temperature range Insensitive to MIPS, β, γ

31. DARK 2007 SydneySept 28 th,2007Page 31 SNOLAB Status and Schedule

32. DARK 2007 SydneySept 28 th,2007Page 32 SNO Cavern: 2008: SNO+ SNO Utility Rm: PICASSO-IB (2kg) Ladder Labs: 2 of 2009: PICASSO IIB 2009: EXO-200-Gas 2009: Majorana (TBD) 2010: CDMS SNO Control Rm: 2007: DEAP-1 Cube Hall: 1 of 2008: DEAP/CLEAN 2009: PICASSO-III 2009: LUX Cryopit: 1 of 2008: DEAP/CLEAN 2009: LUX 2015?: EXO 2015?: 1T GERDA 2015?: CLEAN-100T 2008:HALO

33. DARK 2007 SydneySept 28 th,2007Page 33 Phase I (Cube Hall, Ladder Labs) –Excavation 100% complete. –Outfitting began June 2007, complete early 2008. Phase II (Cryopit) –Funding announced Aug 2007. –Excavation had started in anticipation and will be in parallel with outfitting of Phase I. –Ready for occupancy mid 2008. Surface Facility –Operational since 2005. SNOLAB Workshop: Aug 22/23 2007 Sudbury On –Initial assignments of space underground. –See: www.snolab.ca SNOLAB Status

34. DARK 2007 SydneySept 28 th,2007Page 34 Excavation Status

35. DARK 2007 SydneySept 28 th,2007Page 35 CUBE HALL

36. DARK 2007 SydneySept 28 th,2007Page 36 CUBE HALL

37. DARK 2007 SydneySept 28 th,2007Page 37 LADDER LABS

38. DARK 2007 SydneySept 28 th,2007Page 38 Shotcrete linear complete: Hand Troweled surface to enhance cleanliness. SNOLAB Workshop 22-23 August 2007

39. DARK 2007 SydneySept 28 th,2007Page 39 Personnel Area

40. DARK 2007 SydneySept 28 th,2007Page 40 Cryopit Top Access

41. DARK 2007 SydneySept 28 th,2007Page 41 Surface Facilities Complete and in use

42. DARK 2007 SydneySept 28 th,2007Page 42 IT Server Room Control Rooms Meeting Rooms Clean Room Laboratories

43. DARK 2007 SydneySept 28 th,2007Page 43 Schedule 2007 2008 2009 2006

44. DARK 2007 SydneySept 28 th,2007Page 44 The Bottom Line –SNOLAB is nearing completion –All the capital funding for the facility is in place –The operations funding is coming together –Funding for experiments has started to flow –Exciting experimental program being developed, and on track for start in early 2008. SNOLAB is Open for Business

45. DARK 2007 SydneySept 28 th,2007Page 45

46. DARK 2007 SydneySept 28 th,2007Page 46

47. DARK 2007 SydneySept 28 th,2007Page 47 Low Energy Solar Neutrinos p + p  2 H + e + + e p + e − + p  2 H + e 2 H + p  3 He +  3 He + 3 He  4 He + 2 p 3 He + p  4 He + e + + e 3 He + 4 He  7 Be +  7 Be + e −  7 Li +  + e 7 Be + p  8 B +  7 Li + p   +  8 B  2  + e + + e p-p Solar Fusion Chain complete our understanding of neutrinos from the Sun pep, CNO, 7 Be, pp CNO Cycle 12 C + p → 13 N +  13 N → 13 C + e + + e 13 C + p → 14 N +  14 N + p → 15 O +  15 O → 15 N + e + + e 15 N + p → 12 C + 

48. DARK 2007 SydneySept 28 th,2007Page 48 Vacuum vs Matter Enhanced Survival Probability vacuum oscillation matter enhanced oscillation transition region solar pp pep 8 B 3-5% flux measurement compare  SNO+ /  SSM (  SSM =1.5%) confirm MSW model improve  12 precision sensitive to new physics

49. DARK 2007 SydneySept 28 th,2007Page 49 muon rate in KamLAND: 26,000 d −1 compared with SNO: 70 d −1 these plots from the KamLAND proposal 11 C Cosmogenic Background

50. DARK 2007 SydneySept 28 th,2007Page 50 SNO+ AV Hold Down AV Hold Down Ropes Existing AV Support Ropes

51. DARK 2007 SydneySept 28 th,2007Page 51 Phase 1a: (published in ’05 PLB, NIM) 20g 2kgd Bckg: 480 /kg/d Phase Ib: (ongoing) 2.6 kg 336 kgd Bckg: 80/kg/d Spin Dependent Sector Phase II: 25 kg 3600 kgd Bckg: 0.8 /kg/d Ladder Lab Phase III: 100 kg 28000 kgd Bckg: 0.08 /kg/d Picasso phased approach (Bckg.values: integrated from 6 keV – 1 MeV ) Phase Ia Phase Ib Phase II Phase III

52. DARK 2007 SydneySept 28 th,2007Page 52 A number of extremely fundamental questions can be addressed by the scientific program of SNOLAB: What is Dark Matter? Is there a new symmetry of nature (Supersymmetry or …) that will reveal itself at higher energies? Why is the Universe dominated by matter, and how did this asymmetry come about? What are the neutrino masses, and how have they contributed to the structure and evolution of the Universe? How were the heavy elements formed in Supernovae, and what is the role of neutrinos in that process. How do cosmic accelerators work? What is the mechanism responsible for neutrino oscillations in the sun (MSW matter oscillations or ?)

53. DARK 2007 SydneySept 28 th,2007Page 53 LADDER LABS