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n Physics at UCL MINOS and NEMO-III

n Physics at UCL MINOS and NEMO-III. Ruben Saakyan UCL Sheffield Particle Physics seminar 12 November 2003. Motivation. Neutrino Mixing Observed !. From KamLAND, solar n and atmospheric n. VERY approximately. Neutrino MASS What do we want to know?. Relative mass scale ( n -osc)

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n Physics at UCL MINOS and NEMO-III

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

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

  3. Neutrino MASSWhat do we want to know? • Relative mass scale (n-osc) • Mass hierarchy (n-osc and bb) • Absolute mass scale (bb +3H b) mmin~ 0 - 0.01 eV mmin~ 0.03 - 0.06 eV Dirac or Majorana preferred by theorists (see-saw) ne n1 n2 n3 Ue12 Ue22 Ue32 Mixing Only from bb From n-osc

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

  5. Why ? • Confirm SuperK with controlled n beam (K2K is first here) • Demonstrate oscillatory behaviour • Make first ever precise (10%) measurement of oscillation parameters Dm232, sin2 2q23 • Improving existing result (CHOOZ) on subdominant nm  ne (Ue3)

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

  7. FarDet~5.4kT 735km NearDet ~1kT Where and How ? 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? Mixing angle Dm2

  9. NuMI beam # protons on target 5 year plan nm CC events/8×1020 pot (~2.5 yr) Year 2005 2006 2007 2008 2009 Total Protons 2.5 3.8 5.0 6.5 7.2 25 ( × 1020) Lots of work to make it possible Low Medium High 5,080 13,800 29,600

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

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

  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 • ~26000m2 of active detector planes • <B> ~ 1.5 Tl • DE/Ehadronic  55%/E • DE/Eem 22%/E • DP/Pm  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. Reconstructed front view Timing Cosmic ray muons • 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. Veto shield Atmospheric n’s at FarDetVeto Shield Veto shield to veto vertical muons and reduce background

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

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

  18. Near Detector n target • ~1 kT • High rates ~ 3 MHz • 3.8 x 4.8 “squeezed” octagon • 1-end readout • no-multiplexing • 220 M64sQIE-based front-end • 282 steel planes • 153 scintillator planes • Use events with R<30cm • EnNear EnFar • interactions in ND ~10 – 100 n events/spill •  • ~108 – 109 events/yr • Unique opportunity • for n-scattering physics m spectrometer

  19. Construction @ FermilabNear 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 Detectorat 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, m, p 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. Pion Proton Odd Plane view Even Plane view Even Plane view Odd Plane view Strip Strip Relative Pulse Height Relative Pulse Height 3.5 GeV 3.5 GeV Plane Plane 2 GeV 2 GeV 1 GeV 1 GeV Calibration Detector Events

  22. Calibration Detector ResultsVery preliminary

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

  24. MINOS:Physics Reach nmne

  25. Summary • The MINOS Far Detector is complete and taking cosmic and atmospheric n 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 n’s – April 2005

  26. NEMO

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

  28. bb decay basics Requires Majorana mn≠ 0 In many even-even nuclei b-decay is energetically forbidden SM Qbb This leaves bb as the allowed decay mode Qbb

  29. bb Decay Basics. Rates G – phase space, exactly calculable; G0n ~ Qbb5, G2n ~ Qbb11 M – nuclear matrix element. Hard to calculate. Uncertainties factor of 2-10 (depending on isotope) Must investigate several different isotopes! <mn> is effective Majorana neutrino mass Isotopes of Interest 48Ca, 76Ge, 100Mo, 150Nd,136Xe, 116Cd, 96Zr, 82Se,130Te

  30. Currently Active Experiments CUORICINO (bolometer) NEMO-3 (Tracking calorimeter) <mn> = 0.4 eV ??? 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: • st = 250 ps • From tracker: • s||= 1cm s = 0.45mm • (using timing information • on plasma propagation) • Calibration: • Laser survey • neutron Am/Be for • s||, s, e+ signature • e-207Bi, 90Sr for • energy calibration • 60Co for time alignment Trigger: 1 scintillator hit > 150 keV + 1 track: few Geiger planes (flexible  3 – 7 Hz)

  34. How it works

  35. NEMO bb events • 3D pictures • study single electron spectra • study angular distributions • Detailed 2n information • O (105) 2n100Mo events/yr ! • 7 isotopes

  36. NEMO background events g  e+e- e- (~7 MeV) from ng

  37. 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

  38. NEMO-3 First Results100Mo 1200 h 2n: T1/2=[7.4±0.05(stat)±0.8(sys)]×1018yr (19000 events; S/B  50) 0n: 1 event in 2.8 – 3.2 MeV region T1/2 > 1023 yr 90% CL <mn> < 0.9 – 2.1 eV World’s best result for 100Mo Very preliminary (and conservative) from 3800h: T1/2 > 2.3×1023 yr <mn> < 0.6 – 1.4 eV

  39. Single State Dominance (SSD)VS Higher order State Dominance (HSD) Simkovic, Domin, Semenov nucl-th/0006084, Phys. Rev. C HSD 1+ 100Tc SSD 0+ 100Mo 0+ 100Ru • Shape of single e- spectrum • Shape of 2b spectrum • Angular distribution • ~ 20% difference in T1/2 100Mo + NEMO-like detector can test it experimentally !

  40. NEMO-3 First Results100Mo 1200 h single e- spectrum Angular distribution between two e- Preliminary: SSD is preferred

  41. NEMO-3 First Results Other Isotopes 116Cd 82Se 150Nd T1/2=[3.9±0.3(stat)±0.4(sys)]×1019 T1/2 > 1.0 × 1022 y 90% CL T1/2=[8.2±0.4(stat)±0.8(sys)]×1019 T1/2 > 4 × 1022 y 90% CL World’s best result ! T1/2=[7.0±0.7(stat)±0.7(sys)]×1018 T1/2 > 7.7 × 1020 y 90% CL

  42. NEMO-3 0nbb sensitivity5 years E = 2.8 – 3.2 MeV 100Mo 7 kg Qbb =3.034 MeV External BG: 0 Internal BG: radioactivity < 0.04 event/y/kg 2nbb = 0.11 event/y/kg  T1/2 > 3 × 1024 yr  <m> < 0.2 – 0.5 eV 82Se 1 kg Qbb =2.995 MeV External BG: 0 Internal BG: radioactivity < 0.01 event/y/kg 2nbb = 0.01 event/y/kg  T1/2 > 1 × 1024 yr  <m> < 0.6 – 1.2 eV In case of full load of 82Se (~14kg) <m> < 0.1 – 0.3 eV

  43. T1/2(2n) and Energy Resolution 82Se looks most promising candidate F ~ (sE/E)6

  44. SuperNEMO ~ 100 kg 82Se (or other) • Sensitivity <mn> ~ 0.03 eV in 5 yr • Feasible if: • BG only from 2n • (NEMO3) • b) DE/E = 5-6% • at 3 MeV (Qbb82Se) • (R&D needed) 4 supermodules, planar geometry

  45. Future bb projects comparison5yr exposure * 5 different latest NME calculations

  46. Concluding Remarks • First (preliminary) results from NEMO-III: • <mn> ≤ 0.6 eV after 3800h • 2n: SSD is preferred • NEMO-III to reach 0.1 – 0.3 eV with 10 – 14 kg 82Se upgrade • UK involvement: 1000cm3 HP Ge detector • bb excited states physics with this Ge detector • Happy to collaborate with Sheffield and Boulby

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