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Neutrino Experiments

This talk discusses the current status of neutrino experiments, recent progress made in the last 2 years, and prospects for the near future. Topics include the mixing matrix and masses, hierarchy, CP violation, and more.

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Neutrino Experiments

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  1. Neutrino Experiments Status, recent progress, prospects Steve Brice Fermilab Steve Brice Fermilab

  2. Mixing Matrix and Masses 3s Ranges Dm221 : (7.0 - 9.1) × 10-5 eV2 TAN2q12 : 0.34 – 0.62 Dm232 : (1.9 – 2.98) × 10-3 eV2 TAN2q23 : 0.49 – 2.2 SIN2q13 ≤ 0.045 d unknown Hierarchy unknown mlightest < 2.2 eV Dirac or Majorana unknown [updated from Gonzalez-Garcia PASI 2006] Normal hierarchy Inverted hierarchy (m3)2 (m2)2 Dm221 (m1)2 ne Dm232 nm Dm231 nt (m2)2 Dm221 (m1)2 (m3)2 m2lightest m2lightest Steve Brice Fermilab

  3. Talk Overview • Intro • More than 3 neutrino types? • 12 Sector • 23 Sector • Is q23 maximal? • 13 Sector • What is the value of q13? • How are the mass eigenstates ordered? • Is CP violated? • Mass • What are the values of the neutrino masses? • Are neutrinos their own anti-particles? • Summary Philosophy:- Describe the status of the field, highlighting progress made in the last 2 years (since last EPS HEP conference), and outlining prospects for the near (~5 year) future. Connections to the parallel talks given last week will behighlighted in red Steve Brice Fermilab

  4. Theoretical developments – see next talk Cosmic ray neutrinos (e.g. IceCube) – see previous talk Neutrinos in cosmology Neutrino magnetic moment searches Recent result: A.G. Beda et al., "The first result of the neutrino magnetic moment measurement in GEMMA", arXiv:0705.4576  < 5.8 x 10^{-11} mB 90% CL BB Relic neutrinos M. Messina parallel talk Fri AM Experiments more than ~5 years distant Superbeams beyond NOnA and T2K Neutrino Factory Beta Beams C. Espinoza parallel talk Thu PM (EC Beam) T. Tabarelli parallel talk Thu PM (Beta Beam and Atmospheric) C. Orme parallel talk Thu PM (Beta Beam) Not Covered in this Talk Steve Brice Fermilab

  5. LSND • LSND: • Excess of ne events in a nm beam • 87.9 ± 22.4 ± 6.0 over background • ~4s evidence for n oscillation L/E dictates Dm2 be very different from the well established solar and atmospheric Dm2s. Z width dictates 3 light, active neutrinos and therefore only 2 independent Dm2s Therefore is the LSND result evidence for a sterile neutrino? Steve Brice Fermilab

  6. P(nm ne)= sin22q sin2(1.27Dm2L/E) target and horn decay region absorber dirt detector nm ne??? K+ p+ Booster primary beam secondary beam tertiary beam (protons) (mesons) (neutrinos) MiniBooNE Keep L/E same as LSND while changing systematics, energy & event signature Order of magnitude higher energy (~500 MeV) than LSND (~30 MeV) Order of magnitude longer baseline (~500 m) than LSND (~30 m) Steve Brice Fermilab

  7. MiniBooNE Result No ne excess in oscillation signal region but 96 ± 17 ± 20 events above background, for 300<EnQE<475MeV Two independent analyses show no evidence for nmne appearance-only oscillations. M. Sorel parallel talk Fri AM M. Maltoni parallel talk Fri AM Steve Brice Fermilab

  8. The 12 Sector 3s Ranges Dm221 : (7.0 - 9.1) × 10-5 eV2 TAN2q12 : 0.34 – 0.62 Dm232 : (1.9 – 2.98) × 10-3 eV2 TAN2q23 : 0.49 – 2.2 SIN2q13 ≤ 0.045 d unknown Hierarchy unknown mlightest < 2.2 eV Dirac or Majorana unknown [updated from Gonzalez-Garcia PASI 2006] Normal hierarchy Inverted hierarchy (m3)2 (m2)2 Dm221 (m1)2 ne Dm232 nm Dm231 nt (m2)2 Dm221 (m1)2 (m3)2 m2lightest m2lightest Steve Brice Fermilab

  9. How to Measure the 12 Sector Probed by measuring neutrino disappearance in solar neutrino experiments En > ~5 MeV En < ~2 MeV A. De Gouvea NUSS 07 Also probed by measuring anti-neutrino disappearance with the Kamland reactor neutrino experiment For En/L = O(Dm122) L(km), E(MeV), Dm2(10-3eV2) Steve Brice Fermilab

  10. Flavor content of solar flux. SNO Solved the solar neutrino problem Charged current measurement of electron flavour coupled with neutral current measurement of all active flavours provides conclusive proof of flavour transformation S. Peeters parallel talk Fri AM Steve Brice Fermilab

  11. Kamland Use in 1000 tons of liquid scintillator to measure disappearance of ne produced by large number of Japanese reactors Clear evidence for oscillation not merely disappearance S. Enomoto WIN05 Steve Brice Fermilab

  12. State of 12 Sector 10-4 Dm221 [eV2] 10-5 Schwetz hep/ph 0606060 sin2q12 Dashed = 90% CL Solid and shaded = 99.73% CL Crucial input also from the Chlorine, Super-K, SAGE, and GALLEX solar n experiments Steve Brice Fermilab

  13. Upcoming 12 Sector Measurements • SNO • Phase 3 (NCDs) results expected soon • Kamland II (Solar Neutrino Phase) • Scintillator purification ongoing • Borexino • Detector complete • Data taking started May 16 • Kamland and Borexino plan to use neutrino scattering from electrons to measure Ev~1-2 MeV • See the change in from MSW effect • Other efforts to measure 1-2 MeV solar neutrinos • SNO+, LENA • Several collaborations looking to measure solar neutrinos below ~1 MeV using inverse beta decay • LENS(115In), MOON(100Mo), SIREN(160Gd) Shimizu DBD07 Steve Brice Fermilab

  14. The 23 Sector 3s Ranges Dm221 : (7.0 - 9.1) × 10-5 eV2 TAN2q12 : 0.34 – 0.62 Dm232 : (1.9 – 2.98) × 10-3 eV2 TAN2q23 : 0.49 – 2.2 SIN2q13 ≤ 0.045 d unknown Hierarchy unknown mlightest < 2.2 eV Dirac or Majorana unknown [updated from Gonzalez-Garcia PASI 2006] Normal hierarchy Inverted hierarchy (m3)2 (m2)2 Dm221 (m1)2 ne Dm232 nm Dm231 nt (m2)2 Dm221 (m1)2 (m3)2 m2lightest m2lightest Steve Brice Fermilab

  15. How to Measure the 23 Sector Probed by measuring muon neutrino disappearance in atmospheric neutrino experiments L(km), E(GeV), m(eV) The same oscillations can also be measured by measuring muon neutrino disappearance from beam created at accelerators Steve Brice Fermilab

  16. Atmospheric Neutrinos at SuperK “Atmospheric Neutrino Anomaly” caused by muon neutrinos oscillating away. Presumably into tau neutrinos SuperK has some evidence for tau neutrino appearance – Need CNGS confirmation K. Kaneyuki parallel talk Fri AM Kajita NuSS 2007 Steve Brice Fermilab

  17. K2K: Confirming Atmospheric Oscilllations First accelerator confirmation of atmospheric neutrino oscillations came from K2K Steve Brice Fermilab

  18. MINOS Far detector Far Detector: Soudan, Minnesota, 735 km from target 5.4 kton mass 484 steel/scintillator planes, 8x8x30 m3 Near Detector: Fermilab, 1km from target 1 kton mass 282 steel planes 153 scintillator planes, 3.8x4.8x15 m3 Near detector Steve Brice Fermilab

  19. New MINOS Result Last Thursday 2.50 POT analyzed ≈ 2x statistics of 2006 result Also improved modeling, reconstruction, and PID Comparison of new and old MINOS results A. Weber parallel talk Thu PM Steve Brice Fermilab

  20. Current State of 23 Sector Steve Brice Fermilab

  21. Opera A hybrid emulsion and tracking detector Goal: Verify that the nm are oscillating into nt m spectrometer: Dipolar magnet + RPC chambers Precision tracker: Drift tubes n Hall B brick (56 Pb/Em. “cells”) 8 cm (10X0) Pb target 1.8 kton CNGS: Beam <En> ≈ 17 GeV Baseline 732 km Expected event rate: ~3600 n NC+CC /kton/year ~16 nt CC /kton/year (for sin22q23=1, Dm322=2.5x10-3 eV2) module Target Trackers Pb/Em. target brick wall scintillator strips G. Wilquet parallel talk Thu PM A. Murst Guler parallel talk Thu PM (Assoc. Charm Prod.) Steve Brice Fermilab

  22. Opera Latest Tracking tested with CNGS runs in Aug and Oct 2006 Brick installation started Sep 2006 (~20000 currently stored) May 2007 cosmic ray test with 15000 bricks. Tested chain: Prediction / Brick Extraction / Development / Scanning Worked well Sep 2007 CNGS neutrino beam on 50000-60000 bricks. Full (170,000 Bricks) planned for Mar 2008. Sato DBD07 Steve Brice Fermilab

  23. The 13 Sector 3s Ranges Dm221 : (7.0 - 9.1) × 10-5 eV2 TAN2q12 : 0.34 – 0.62 Dm232 : (1.9 – 2.98) × 10-3 eV2 TAN2q23 : 0.49 – 2.2 SIN2q13 ≤ 0.045 d unknown Hierarchy unknown mlightest < 2.2 eV Dirac or Majorana unknown [updated from Gonzalez-Garcia PASI 2006] Normal hierarchy Inverted hierarchy (m3)2 (m2)2 Dm221 (m1)2 ne Dm232 nm Dm231 nt (m2)2 Dm221 (m1)2 (m3)2 m2lightest m2lightest Steve Brice Fermilab

  24. How to Measure the 13 Sector Probed by measuring the disappearance of reactor produced electron anti-neutrinos. Need to work at an L/E matched to the atmospheric Dm2 (C.F. Kamland measurement at solar Dm2) L(km), E(MeV), m(10-3eV) Steve Brice Fermilab

  25. How to Measure the 13 Sector (cont) Also probed by measuring electron neutrino appearance from accelerator produced muon neutrinos Need to have an L and E such that interference between solar and atmospheric scales can bee seen L(km), E(GeV), m(eV) Matter effect Steve Brice Fermilab

  26. Current State of q13 Sector 10-2 Dm231 [eV2] 10-3 sin2q13 Schwetz hep/ph 0606060 Steve Brice Fermilab

  27. How to Improve on Chooz • Increase statistics: • Use more powerful nuclear reactors • Utilize larger target mass, hence larger detectors • Suppress background: • Go deeper underground to gain overburden for reducing cosmogenic background • Reduce systematic uncertainties: • Reactor-related: • Optimize baseline for best sensitivity and smaller reactor-related errors • Near and far detectors to minimize reactor-related errors • Detector-related: • Use “Identical” pairs of detectors to do relative measurement • Comprehensive program in calibration/monitoring of detectors • Interchange near and far detectors (optional) Peng DBD07 G. Mention parallel talk Thu AM Steve Brice Fermilab

  28. Double Chooz 0.28 km 1.05 km Near Far Suekane DBD07 I. Gil Botella parallel talk Thu AM Steve Brice Fermilab

  29. Daya Bay V. Vorobel parallel talk Thu AM Steve Brice Fermilab

  30. Double Chooz Latest • Final stages of R&D • Detector construction starts this year • First data taking expected to start in 2008 with far detector • Get down to sin22q13 < 0.06 in 1.5 years • Start taking data with both detectors in 2010 • Get down to sin22q13 < 0.025 in 3 years Suekane DBD07 Daya Bay Latest • Oct 2006: Passed DOE scientific review • Apr 2007 • Passed DOE CD-1 review • Passed final nuclear safety review in China • Began to receive 3 year project funding from Chinese agencies • Jun 2007: Began civil construction • Oct 2007: Anticipate DOE CD-2/3a review • May 2009: Start data taking with 2 detectors at Daya Bay near hall • Apr 2010: Start data taking with 8 detector final configuration Peng DBD07 Other reactor efforts ongoing: Angra (Brazil), RENO (Korea) Steve Brice Fermilab

  31. Off Axis Beams Far Detector Near Detector Dm2=3x10-3eV2 L=295km Decay Pipe q Target Horns nm • Increases flux on osc. max. • Reduces high-E tail, and thus NC backgrounds • Reduces ne contamination from K and m decay OA2° Steve Brice Fermilab

  32. NOnA Far detector: 18 kton, fully active segmented detector 12 km off NuMI beamline axis 810 km baseline optical fibre Steve Brice Fermilab

  33. NOnA Near Detector 186 liquid scintillator planes in target 10 in muon ranger, 1m steel Same cell size as far detector Readout from one side per plane with APDs plus faster electronics than far detector Requires some additional excavation in NuMI tunnel in order for detector to be at proper 14 mrad angle Steve Brice Fermilab

  34. T2K Beam from JPARC to SuperK M. Zito parallel talk Thu AM Steve Brice Fermilab

  35. T2K Near Detector (@280m Offaxis) Near Detector @ 280m Built inside UA1/NOMAD magnet for pm measurement Sandwich calorimeters/trackers and TPCs for precision beam spectrum and composition measurement. Particular attention paid to measuring p0 from neutral current interactions Magnet coils FGDs Magnet yoke TPCs ECAL beam tracker p0 detector Steve Brice Fermilab

  36. NOnA Latest • Accelerator upgrades merged with NOnA detector project Dec 20 2006 (upgrades for a 700kW source) • Cap on total project cost of $260M put in place late Dec 2006 • DOE CD1 approval announced May 11 • Currently working to get cost below $260M • Hoping to start detector construction in 2010 and have 700kW source on same timescale T2K Latest • JPARC Linac beam commissioning Dec 2006 • First horn prototype operated successfully with 8.5x105 pulses • JPARC Rapid Cycling Synchrotron Beam Commissioning Sep 2007 • JPARC Main Ring Beam Commissioning: May, 2008 • Hoping for first data April 2009 • Ramp up to 750kW source by 2012 Steve Brice Fermilab

  37. An Aside on GeV Neutrino Cross Sections Compilation of nm CC Quasi-Elastic Cross-Section Measurements The CCQE xsec is the best known!! Background xsecs for NOna and T2K are known much more poorly If NOnA and T2K are to perform as we hope then the xsecs need to be better constrained A. Bodek parallel talk Thu PM Steve Brice Fermilab

  38. Cross-Sections with MiniBooNE • By almost 2 orders of magnitude • MiniBooNE has the largest ~1 GeV • neutrino data set ever taken. • A range of Cross-Section measurements • are planned:- • CC Quasi-elastic (MA, osc signal channel) • NC elastic (compare to CC QE) • CC p+ (disapp. osc. bkgd, coh. prod.) • NC p0 (osc bkgd., coh. prod.) • CC p0 (compare to NC channel) First CCQE paper completed (arXiv:0706.0926 [hep-ex]) Cross-Sections are also being published by the K2K collaboration A. Blondel parallel talk Thu PM (HARP) M. Wascko/B. Roe parallel talk Fri AM Steve Brice Fermilab

  39. Cross-Sections with SciBooNE • Idea: Put well developed • K2K SciBar detector into • the well understood FNAL • Booster Neutrino Beamline • Precision measurement of xsecs for T2K • BNB beam well matched to T2K beam • Low cost (<$1M) SciBooNE Timeline • 2005, Summer - Collaboration formed • 2005, Dec - Proposal • 2006, Jul - Detectors move to FNAL • 2006, Sep - Groundbreaking • 2006, Nov - EC Assembly • 2007, Feb - SciBar Assembly • 2007, Mar - MRD Assembly • 2007, Mar - Cosmic Ray Data • 2007, Apr - Detector Installation • 2007, May - Commissioning • 2007, Jun - Neutrino Data Run M. Wascko parallel talk Fri AM Steve Brice Fermilab

  40. Cross-Sections with MINERnA High granularity detector in NuMI beamline Large physics program including xsec measurements at a few GeV “Chewy center (active target), with a crunchy shell of muon, hadron, and EM absorbers” The nSNS experiment is planning to measure cross-sections of 10-50 MeV neutrinos produced by stopped pions and muons at SNS. Necessary input to supernova calculations Steve Brice Fermilab

  41. The Masses 3s Ranges Dm221 : (7.0 - 9.1) × 10-5 eV2 TAN2q12 : 0.34 – 0.62 Dm232 : (1.9 – 2.98) × 10-3 eV2 TAN2q23 : 0.49 – 2.2 SIN2q13 ≤ 0.045 d unknown Hierarchy unknown mlightest < 2.2 eV Dirac or Majorana unknown [updated from Gonzalez-Garcia PASI 2006] Normal hierarchy Inverted hierarchy (m3)2 (m2)2 Dm221 (m1)2 ne Dm232 nm Dm231 nt (m2)2 Dm221 (m1)2 (m3)2 m2lightest m2lightest Steve Brice Fermilab

  42. How to Measure the Masses Direct kinematic search: Look for a distortion at the end-point of a b decay spectrum. Low endpoint energy optimal therefore use tritium (18.6keV) (Also an effort to use 187Re with 7x lower endpoint) Existing limit from tritium endpoint measurement: mn < 2.2eV 95% CL (Mainz and Troitsk groups) Steve Brice Fermilab

  43. Improve mn by x10 (2.2 0.2 eV) • Stronger Tritium source (x80) • Longer measuring peroid (100 1000 days) • Better spectrometer (DE=0.93eV) • Smaller systematics, reduced energy losses Katrin Main spectrometer Gaseous tritium source Transport section Pre-spectrometer Detector 2005 vacuum tests of pre-spectrometer 2006 electromagn. tests of pre-spectrometer, main spectrometer on site 2007 source demonstrator, inner electrode mounting 2008 commissioning of WGTS, tritium loops, em. test of spectrometers 2009 system integration & first tritium runs regular data taking for 5-6 years Spectrometer being transported Nov 2006 G. Drexlin Steve Brice Fermilab

  44. How to Measure the Masses (cont) Search for 0n double b decay: In many even-even nuclei, b decay is energetically forbidden.This leaves bb as the allowed decay mode. 2nbb decay has been observed in several nuclei, but 0nbb has not yet. 0νββ 2νββ (Te1+Te2 ) / Qββ If observed it would imply a massive Majorana neutrino G0n = phase space factor (~Q5) M0n = nuclear matrix element a,b are the Majorana phases Steve Brice Fermilab

  45. 0nbb Decay Measurements Survey of some past and present experiments A. Nucciotti arXiv:0707.2216 [nucl-ex] Timescales: t1/2(U,Th) ~ Tuniverse t1/2(2nbb) ~ 1010Tuniverse t1/2(0nbb) ~ 1017Tuniverse Soldner-Rembold parallel talk Thu AM (NEMO-3) Steve Brice Fermilab

  46. Ge Claim • Heidelberg-Moscow (in Gran Sasso) • Enriched Ge detectors • Operating 1990-2003 • Total exposure ~71.7 kg·y • Longest running 0nbb expt. by far • Part of collaboration claim: • T1/2 = (0.7 – 4.2)·1025 y (3 σ) • mbb ≈ 0.44 eV Steve Brice Fermilab

  47. Combining 0nbb and Oscillation Knowledge Switch “bases” from (m1,m2,m3)to (Dm212,Dm322,mlightest) Dm212,Dm322 come from oscillation experiments Majorana phases a,b completely unknown mlightest could be constrained by 0nbb decay Ge claim Very interesting distinction between the normal and inverted mass hierarchies Normal hierarchy: At least one neutrino has mi>√(Dm322)≈0.05eV Inverted hierarchy: At least two neutrinos have mi>√(Dm322)≈0.05eV Steve Brice Fermilab

  48. Future 0nbb Prospects A sample of the proposed experiments A. Nucciotti arXiv:0707.2216 [nucl-ex] I. Bandac parallel talk Thu AM (CUORE) K. Kroeninger parallel talk Thu AM (GERDA) Steve Brice Fermilab

  49. Summary • The last decade has been revolutionary in neutrino physics • The next decade promises an even more rapid development of our understanding • The masses and mixings are giving us hints of physics well beyond the Standard Model • Can we develop these hints? • In the upcoming era of LHC physics the neutrino realm will provide a unique and independent source of knowledge Steve Brice Fermilab

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