1. Physics at UCL MINOS and NEMO-III Ruben Saakyan UCL Sheffield Particle Physics seminar 12 November 2003

2. Motivation Neutrino Mixing Observed ! From KamLAND, solar and atmospheric VERY approximately

3. Neutrino MASS What do we want to know? Relative mass scale ( -osc) Mass hierarchy ( -osc and  ) Absolute mass scale (    ) Dirac or Majorana 1  3 e U e1 2 U e2 2 U e3 2 Mixing Only from  From -osc m min ~ 0 - 0.01 eV m min ~ 0.03 - 0.06 eV preferred by theorists (see-saw)

4. MINOS outline  MINOS basics  Construction status and schedule  Atmospheric ’s  Physics reach

5. Why ?  Confirm SuperK with controlled beam (K2K is first here)  Demonstrate oscillatory behaviour  Make first ever precise (10%) measurement of oscillation parameters  m 23 2, sin 2 2    Improving existing result (CHOOZ) on subdominant   e (U e3 )

6. Who ? Main Injector Neutrino Oscillation Study 32 institutions 175 physicists

7. Where and How ? FarDet ~5.4kT NearDet ~1kT 735km Two functionally identical magnetized steel/scintillator sandwich calorimeters

8. How ? (Part II) Expected event spectrum (from NearDet) Observed event spectrum (from FarDet) Ratio: survival probability as a Function of energy Shape: Oscillations? Decay? Other? m2m2 Mixing angle

9. NuMI beam Low Medium High 5,080 13,800 29,600  CC events/8×10 20 pot (~2.5 yr) Year 2005 2006 2007 2008 2009 Total Protons 2.5 3.8 5.0 6.5 7.2 25 ( × 10 20 ) Lots of work to make it possible # protons on target 5 year plan

10. Construction @ Fermilab. The Beam 677 m decay pipe Near Detector Target Horns in fabrication Tunneling is finished Decay pipe is finished and encased in concrete October’03: Target Hall outfitting complete Beneficial occupancy of Near Detector hall – January 2004 NuMI beamline completed Dec 2004 Jan-Mar 2005 – Beam commissioning Apr 2005 – Start of physics running

11. 1” thick steel planes Extruded plastic scintillator strips XY orientation of scint planes WLS fiber + Hamamatsu multianode PMTs: M16 (Far) and M64 (Near) = 1.5 Tl (Far and Near) Front-ends VA(IDE) – M16 QIE – M64 Software trigger Detector Technology

12. MINOS Far Detector 8 m octagonal 1” steel plates 2 Supermodules 15 m each 5.4 kT total mass 484/485 scintillator/steel planes 2-ended readout 8X optical multiplexing ~1000 Km of scintillator ~2000km of WLS + clear fiber ~26000m 2 of active detector planes ~ 1.5 Tl  E/E hadronic  55%/  E  E/E em  22%/  E  P/P    12% (by curvature)  6% (by range)

13. Far Detector at Soudan Completed July 2003 Magnetized and running Half the detector has been running since mid 2002 Fully commissioned Taking atmospheric neutrino data, Soudan 2 exposure by the end of next year

14. Cosmic ray muons Reconstructed front view Timing Cosmic ray muons are used for calibration (and physics!) 2.6ns/plane timing resolution permits direction determination Veto shield tags incoming “parallel” muons which can mimic neutrino events

15. Atmospheric ’s at FarDet Veto Shield Veto shield Veto shield to veto vertical muons and reduce background

16. Upward muons Downward Upward Timing allows measurement of 1/  Good separation of downward (cosmic ray) and upward (neutrino induced) muons

17. Atmospheric events at FarDet 700 MeV muon Atmospheric interactions have been observed B-field allows to measure muons up to 70 GeV B-field gives charge info: distinguish and bar Potential to test CPT Num of events in 5 years bar Contained vertex with  620 400 Upgoing  280 120

18. Near Detector ~1 kT High rates ~ 3 MHz 3.8 x 4.8 “squeezed” octagon 1-end readout no-multiplexing 220 M64s QIE-based front-end 282 steel planes 153 scintillator planes Use events with R<30cm E Near  E Far target  spectrometer interactions in ND ~10 – 100 events/spill  ~10 8 – 10 9 events/yr Unique opportunity for -scattering physics

19. Construction @ Fermilab Near Detector All NearDet planes assembled and ready to install Beneficial occupancy of NearDet Hall – Jan 04 Installation starts January 04 Installation complete – Oct 04

20. Calibration Detector at CERN Both ND and FD too big to be calibrated in test beam CalDet is the same but smaller T7 and T11 beamlines at CERN PS in 2001, 2002, 2003 October 2003: Data taking programme complete Understand detector response to p, e, ,  of 0.5 – 10 GeV (particle ID) Calibrate out Near/Far readout differences Debug detector subsystems Refine topology and pattern recognition software  60 planes (1m×1m) 12 ton  24 strips/plane, XY orientation in consecutive planes  FarDet and/or NearDet readout

21. Calibration Detector Events Proton Even Plane view Odd Plane view Pion Even Plane view Odd Plane view Strip Relative Pulse Height 3.5 GeV 2 GeV 1 GeV Plane 2 GeV 1 GeV

22. Calibration Detector Results Very preliminary

23. MINOS: Physics Reach    2.3 yr * 3.7 yr * 5.0 yr * * Times according to 5 year proton intensity plan

24. MINOS: Physics Reach   e

25. Summary  The MINOS Far Detector is complete and taking cosmic and atmospheric data  Beam work and Near Detector construction at FNAL is on schedule. First beam – end 2004.  Calibration Detector programme at CERN complete  Physics running with NuMI ’s – April 2005

26. NEMO

27. NEMO Outline   decay basics  The NEMO-III detector  First results  Sensitivity by 2008  Towards NEMO-NEXT

28.  decay basics Q  In many even-even nuclei  -decay is energetically forbidden This leaves  as the allowed decay mode Requires Majorana m ≠ 0 SM Q 

29.  Decay Basics. Rates G – phase space, exactly calculable; G 0 ~ Q  5, G 2 ~ Q  11 M – nuclear matrix element. Hard to calculate. Uncertainties factor of 2-10 (depending on isotope) Must investigate several different isotopes! is effective Majorana neutrino mass Isotopes of Interest 48 Ca, 76 Ge, 100 Mo, 150 Nd, 136 Xe, 116 Cd, 96 Zr, 82 Se, 130 Te

30. Currently Active Experiments = 0.4 eV ??? CUORICINO (bolometer) NEMO-3 (Tracking calorimeter) Heidelberg-Moscow exp is still running ???

31. Neutrino Ettore Majorana Observatory 40 physicists and engineers  13 Laboratories/Universities  7 Countries

32. UK NEMO team (so far)  Phil Adamson, Leo Jenner, Ruben Saakyan, Jenny Thomas (all UCL)  Received approval from PPRP 27 Jan 03  Main involvement: data analysis.. ..and some hardware tasks: PMT helium tests, light injection optimization  Expect to participate in shifts at Frejus

33. From scintil detector:   = 250 ps From tracker:  || = 1cm   = 0.45mm (using timing information on plasma propagation) Calibration: Laser survey neutron Am/Be for  ||,  , e + signature e - 207 Bi, 90 Sr for energy calibration  60 Co for time alignment Trigger: 1 scintillator hit > 150 keV + 1 track: few Geiger planes (flexible  3 – 7 Hz)

34. How it works

35. NEMO  events  3D pictures  study single electron spectra  study angular distributions  Detailed 2  information  O (10 5 ) 2 100 Mo events/yr !  7 isotopes

36. NEMO background events  e + e - e - (~7 MeV) from n 

41. Data taking  June 2002: start with all 20 sectors, iron shielding, neutron shielding but…  …still a lot of debugging (both tracking detector and calorimeter)  14 February 2003: start of routine data taking

42. NEMO-3 First Results 100 Mo 1200 h 2 : T 1/2 =[7.4±0.05(stat)±0.8(sys)]×10 18 yr (19000 events; S/B  50) 0 : 1 event in 2.8 – 3.2 MeV region T 1/2 > 10 23 yr 90% CL < 0.9 – 2.1 eV World’s best result for 100 Mo Very preliminary (and conservative) from 3800h: T 1/2 > 2.3×10 23 yr < 0.6 – 1.4 eV

43. Single State Dominance (SSD) VS Higher order State Dominance (HSD) Simkovic, Domin, Semenov nucl-th/0006084, Phys. Rev. C 100 Mo 100 Tc 100 Ru 0+0+ 1+1+ 0+0+ SSD HSD 1.Shape of single e - spectrum 2.Shape of 2  spectrum 3.Angular distribution 4.~ 20% difference in T 1/2 100 Mo + NEMO-like detector can test it experimentally !

44. NEMO-3 First Results 100 Mo 1200 h single e - spectrum Angular distribution between two e - Preliminary: SSD is preferred

45. NEMO-3 First Results Other Isotopes T 1/2 =[8.2±0.4(stat)±0.8(sys)]×10 19 T 1/2 > 4 × 10 22 y 90% CL World’s best result ! T 1/2 =[7.0±0.7(stat)±0.7(sys)]×10 18 T 1/2 > 7.7 × 10 20 y 90% CL T 1/2 =[3.9±0.3(stat)±0.4(sys)]×10 19 T 1/2 > 1.0 × 10 22 y 90% CL 82 Se 150 Nd 116 Cd

46. 82 Se 1 kg Q  =2.995 MeV External BG: 0 Internal BG: radioactivity < 0.01 event/y/kg  = 0.01 event/y/kg  T 1/2 > 1 × 10 24 yr  < 0.6 – 1.2 eV NEMO-3 0  sensitivity 5 years 100 Mo 7 kg Q  =3.034 MeV External BG: 0 Internal BG: radioactivity < 0.04 event/y/kg  = 0.11 event/y/kg  T 1/2 > 3 × 10 24 yr  < 0.2 – 0.5 eV E = 2.8 – 3.2 MeV In case of full load of 82 Se (~14kg) < 0.1 – 0.3 eV

47. T 1/2 (2 ) and Energy Resolution F ~ (  E /E) 6 82 Se looks most promising candidate

48. SuperNEMO  Sensitivity ~ 0.03 eV in 5 yr ~ 100 kg 82 Se (or other) 4 supermodules, planar geometry Feasible if: a)BG only from 2 (NEMO3) b)  E/E = 5-6% at 3 MeV (Q  82 Se) (R&D needed)

49. Future  projects comparison 5yr exposure ExperimentSource and Mass Sensitivity to T 1/2 (y) Sensitivity to (eV) * Majorana $50M 76 Ge, 500kg3×10 27 0.02 – 0.06 CUORE $25M 130 Te, 750kg(nat) 2×10 26 0.03 – 0.10 EXO $50M-100M 136 Xe 1 ton 8×10 26 0.03 – 0.10 SuperNEMO $20M 82 Se (or other) 100 kg 2×10 26 0.03 – 0.07 * 5 different latest NME calculations

50. Concluding Remarks  First (preliminary) results from NEMO-III: ≤ 0.6 eV after 3800h 2 : SSD is preferred  NEMO-III to reach 0.1 – 0.3 eV with 10 – 14 kg 82 Se upgrade UK involvement: 1000cm 3 HP Ge detector  excited states physics with this Ge detector Happy to collaborate with Sheffield and Boulby

51. Concluding Remarks II  SuperNEMO sounds very promising. Sensitivity ~ 0. 03 eV with 100kg 82 Se  Feasibility tested with NEMO-III  Boulby is a great potential site for SuperNEMO  Opportunity for UK leadership  3-5 December in Orsay: 1 st meeting to form SuperNEMO collaboration – ALL WELCOME

52. BACKUP

53. beam systematics Pointing at right place ? Do we know the spectrum and rates ? What about spectra differences at Near and Far sites ? Beam Monitors GPS and laser survey Near Det Far Det MIPP – a hadron production expt

54. MINOS Calibration Cosmic muons strip-to-strip calibration   Muon Energy Unit (MEU) relative calibration between ND and FD (stopping muons) Light Injection PMT gain drift PMT/electronic non-linearity Calibration Detector Converts MEU to GeV Topology and pattern recognition Energy Calibration goal: 5% absolute 2% relative between ND and FD

55. Pure materials: Source foils measured with the NEMO-3 detector 208 Tl < 2  Bq/kg 214 Bi < 2  Bq/kg neutrons < 10 -9 n cm -2 s -1 Radon in the detector 222 Rn ~ 20 mBq/m 3 220 Rn ~ 1.6 mBq/m 3 to be improved with new anti-radon system