1 / 27

Neutrinophysics Projects

Neutrinophysics Projects. VIDMAN. KATRIN. Majorana Cuoricino/Cuore NEMO,…. Dirac or Majorana neutrino?. GERDA. OPERA. MINOS/ICARUS. BOREXINO. KamLAND. Kaska, Braidwood, Daya Bay,…. DCHOOZ. neutrino factory?. Superbeams: T2K NOvA. Beta Beams?. cosmology. absolute neutrino mass.

guy-shaw
Télécharger la présentation

Neutrinophysics Projects

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Neutrinophysics Projects VIDMAN KATRIN MajoranaCuoricino/CuoreNEMO,… Dirac or Majorananeutrino? GERDA OPERA MINOS/ICARUS BOREXINO KamLAND Kaska, Braidwood, Daya Bay,… DCHOOZ neutrino factory? Superbeams:T2K NOvA Beta Beams? cosmology absolute neutrino mass tritium β-decay ββ- decay 23 neutrino mixing, Δm2 v- oscillation 12 13 Majorana-CP Dirac-CP CP-violation

  2. Neutrino Mixing + Majorana CP-Phases (not observable in v-oscillations)

  3. Super Kamiokande results From L/E sin22θ > 0.90 and 1.9×10-3 < Δm2 < 3.0×10-3 eV2 (90% CL)best fit: sin22θ = 1.02 , Δm2 = 2.4×10-3 eV2 (PRL 93 (2004) 101801) sin22θ > 0.92 and 1.5×10-3 < Δm2 < 3.4×10-3 eV2 (90% CL)best fit: sin22θ = 1 and Δm2 = 2.1×10-3 eV2 (hep-ex/0501064v2) Final SK-I

  4. OPERA sin2(2θ13) < 0.06 • Neutrinobeams: • CNGS beam: 2006 Ev = 17 GeV, P = 0.3 MW • K2K beam (Japan): existing Ev = 1.3 GeV, P = 0.005 MW • T2K Superbeam (Japan): 2009 Ev = 0.7 GeV, P = 0.75-4 MW • NuMI beam (USA): just started Ev = 3.5 GeV, P = 0.4 MW vτ appearance ve appearance LNGS 732 km

  5. 1 mm t n Pb Emulsion layers Detektor Precision Tracker (PT):Universität Hamburg Aktive Target:200.000 lead –emulsion - bricks= 1.800 tons 8.3kg

  6. Automatic Scanning: Nagoya and Europe R&D efforts Bari, Bern, Bologna, Lyon, Münster, Napoli, Roma, Salerno sq ~ 2mrad sx ~ 0.5mm European station S-UTS prototype at Nagoya Final version of the european system ready and working at 20 cm2/hour (15 stations under installation)

  7. OPERA Hamburg: precision tracker Precision Tracker eines Supermoduls (SM) Total (2 SM): ~ 10000 Drifttubes

  8. vτ→vμsensitivity full mixing, 5 years run @ 4.5 x1019 pot / year (…) with CNGS beam upgrade (X 1.5) Start CNGS beam summer 2006 (next SPSC meeting 4 July)

  9. Outlook: Dm231 and sin2q23 Plot by Huber, Lindner, Rolinec, Schwetz, Winter

  10. Neutrino Mixing CHOOZ limit: sin2(213) < 0.2

  11. How to measure theta13, CPV (anti-v) with Synergy Reactor experiments: Neutrino superbeams: Sensitive to θ13 , δCP, mass hierarchybut degeneracies & correlations pure measurement of θ13

  12. Next Generation Experiments: q13 Sensitivity coming long baseline experiments 1 reactor +2 detectors NOvA T2K next generation long baseline experiments T2K NOvA • Compare: • 5 years each • 5% flux uncertainty NOnA

  13. T2K

  14. CP-Violation

  15. Effect of θ13 in reactor experiments: sin22θ13

  16. Reactor Experiments (Proposals) Double-Chooz Braidwood Daya bay Kaska Angra

  17. Double-CHOOZ Frankreich: Saclay, APC, Subatech, Deutschland: MPI-Kernphysik Heidelberg TU München, Univ. Tübingen, Univ. Hamburg, interested RWTH Aachen Russland: Kurchatov Institut, USA: Univ. Alabama, Univ. Notre Dame, Univ. Kansas, Univ. Tennessee, Univ. Lousiana, Drexel University, Argonne Double-Chooz sensitivity for (m2 = 2.0-2.5 10-3 eV2): sin2(213) < 0.025-0.03, 90% C.L. Current limit: Chooz : sin2(213) < 0.2

  18. Double Chooz Detector Target: 12.7 m3Gd (0.1%) loaded scintillator γ catcher: scintillator (not loaded) buffer: not scintillating Inner myon veto: water or scintillator 7m 7m

  19. Far and Near Detectors Distance Reactor-detector Required overburden (m.w.e) 100 45-53 150 55-65 200 67,5-80 300 m.w.e • 60 m.w.e. overburden • 12 m compacted earth • 3 meter high density material DAPNIA 3,5m (under the crane) Ø4,2m DAPNIA Muon Veto Buffer Target Gamma Catcher

  20. Double Chooz Sensitivity Near detector starts Far detector starts 2004 2005 2006 2007 2008 2009 2003 Site Proposal & design Construction ? Data taking • 1% background in Near & Far D. • Syst. uncert.: • σabs = 2.0% • σrel = 0.6% • σscl = 0.5% • σshp = 2.0% • σΔm2= 20% m2=2.4 10-3 eV2 3 years (efficiencies included) sin2(213)<0.024

  21. Double Chooz: deformation in energy spectrum Yield Near – Far: time ~ 3.5 years sin22Q = 0.05 Dm2 = 2 x10-3 eV2

  22. KASKA (Kashiwazaki, Japan) Tohoku Univ., Niigata Univ., Rikkyo Univ., KEK, Kobe Univ., Tokyo Institute of Technology, Tokyo Metropolitan Univ. 7 Reactors P = 24.3 GWth 3 Detectors 2 near: 8 tons – 300-400 m – 100 mwe 1 far: 8 tons - 1.3-1.8 km - 500 mwe Sensitivity after 3 years 0.5% systematic error sin2(213) < 0.026 (90% C.L.) Outlook 2004-05: R&D, 2006-07: Construction, running in 2008

  23. Neutrino Mixing

  24. Solar-v & KamLAND: Δm212 and θ12 tan2θ = 0.40+0.10-0.07 , Δm2 = 7.9+0.6-0.5 ×10-5 eV2 (1σ)

  25. Status BOREXINO • Detector + DAQ ready (air runs) (but not yet filled with scintillator) • Waiting for permission to handle scintillator from authorities

  26. LENA(Low Energy Neutrino Astrophysics) A large (~30 kt) liquid scintillator underground detector Npe ~ 100 / MeV beta ~ 12000 PMs (20 inch) P - decay event Scintillator: PXE , non hazardous, flashpoint 145° C, density 0.99, ultrapure (as proven in Borexino design studies)

  27. Relic supernovae neutrino detection Solar Neutrino Spectroscopy LENA (Low Energy Neutrino Astrophysics) Search for Proton Decay Detector for NeutrinoSuperbeam Galactic supernova neutrino detection Neutrino properties Terrestrial neutrino detection

More Related