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Julia Becker for the IceCube collaboration

Julia Becker for the IceCube collaboration. Neutrino Physics at the South Pole: Recent results from the AMANDA experiment. Sweden: Uppsala Universitet Stockholm Universitet. UK: Imperial College Oxford University. Netherlands: Utrecht University. Japan: Chiba University.

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Julia Becker for the IceCube collaboration

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  1. Julia Becker for the IceCube collaboration Neutrino Physics at the South Pole:Recent results from the AMANDA experiment

  2. Sweden: Uppsala Universitet Stockholm Universitet UK: Imperial College Oxford University Netherlands: Utrecht University Japan: Chiba University Belgium: Université Libre de Bruxelles Vrije Universiteit Brussel Universiteit Gent Université de Mons-Hainaut New Zealand: University of Canterbury Antarctica: Amundsen Scott South Pole Station AMANDA  IceCube Germany: Humboldt Universität Universität Mainz DESY-Zeuthen Universität Dortmund Universität Wuppertal Universität Berlin

  3. Astroparticle physics us

  4. p gD…pn...  N ...m, casc

  5. Diffuse Neutrino Spectra • Atmospheric Bg • Extragalactic: • AGN (1) (Becker/Biermann /Rhode) • AGN (3 and 4) (Mannheim /Protheroe/Rachen) • GRBs (2) (Waxman/Bahcall)

  6. AMANDA/IceCube 677 PMTs on 19 strings Cherencov light South Pole Dome road to work AMANDA Summer camp 1500 m Amundsen-Scott South Pole Station 2000 m [not to scale]

  7. Detection Strategies • Presented in this talk: • Diffuse search • Steady Point sources • Transient objects (AGN flares & GRBs) • WIMPs • plus: • SN in our galaxy • Cosmic Ray Composition • Atmospheric muon spectrum • Search for magnetic monopoles • Galactic Plane

  8. Diffuse energy spectrum • Unfolding the energy spectrum • Data follow atmospheric prediction • Energy spectrum up to 100 TeV • Limit on E-2 extragalactic flux:

  9. Diffuse limits and sensitivities • Unfolded spectrum • 4yr sensitivity • All flavor limits: • Cascades • Ultra High Energies • IceCube

  10. Single sources 3329 events (2000-2003), mostly atm. neutrinos, < 5% atm. muons no point source signal seen so far • Improved background rejection by new pattern recognition method • Blindness strategy: Event selection optimized with randomized RA • Sensitivity (90% C.L.):~ above 10 GeV

  11. Stacking of sources (year 2000) single source sensitivity (4yrs)

  12. AGN flares Mkn421, year 2000 • Sliding window:12 sources tested, no significant excess • Multi-wavelength: 3 of the 12 sources, no excess

  13. GRBs – average spectrum years #(GRB) selection criteria limit/sens. 97-00 312 BATSE 4e-8 00-03 139 BATSE& IPN 3e-8 01 - diffuse search 2.7e-6 Preliminary 00 74 BATSE 9.5e-7

  14. Average  Individual b b-2 a

  15. GRBs – Individual Spectra Model Sensitivity [GeV/s/cm2] Limit [GeV/s/cm2] isotropic 0.157 0.150 beamed 0.041 0.039 average (WB) 0.036 0.035 • Waxman/Bahcall: average spectrum • Single spectrum approach • GRB030329: • Individual par. (model 1,2) • average par. (model 3)

  16. Indirect WIMP search excluded by CDMS Results (2001) for solar WIMPs • Dark matter accumulates in high density regions • Earth and Sun: annihilation of WIMPs in the center • If  flux from there WIMPS • Signal expectation: use Monte Carlo (DARKSUSY) • No significant excess above background, limit on muon flux hard channel: ccW W + -

  17. Summary • AMANDA is an operating UHE neutrino telescope • Different search strategies: • Diffuse search, spectrum up to 100 TeV • Steady point sources (single sources & stacking) • Transient sources (flares and GRBs) • Dark matter search • …and more… • Analyses show so far no signal above atmospheric flux • Constraints on current models possible • Future: IceCube

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