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Latest Results of AMANDA

Latest Results of AMANDA. Wolfgang Rhode Universität Dortmund Universität Wuppertal for the AMANDA Collaboration. South Pole. Dark sector. Runway. AMANDA. Dome. Neutrino Telescope in the Ice. 1997: AMANDA-B10 302 OMs on 10 Strings 2000: AMANDA-II 677 OMs on 19 Strings.

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Latest Results of AMANDA

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  1. Latest Resultsof AMANDA Wolfgang Rhode Universität Dortmund Universität Wuppertal for the AMANDA Collaboration

  2. South Pole Dark sector Runway AMANDA Dome

  3. Neutrino Telescope in the Ice 1997: AMANDA-B10 302 OMs on 10 Strings 2000: AMANDA-II 677 OMs on 19 Strings

  4. Single atmospheric Muons Energy spectrum from the light deposition Depth intensity relation • Absolute Flux understood within 30% (CR-Flux*Prim. Int.) • Energy Spectrum understood within 10% (dEph/dx*PM-Efficiency) ICRC 2003: Desiati for AMANDA ICRC 2003: Geenen for AMANDA

  5. Cosmic Ray Proton Flux Measurement Energy spectrum from the light deposition (QGSJET) Ice property indepent analysis (H) = 2.70 ± 0.02 0 (H) = 0.106(7) m-2s-1sr-1TeV-1 ICRC 2003: Chirkin for AMANDA ICRC 2003: Geenen for AMANDA

  6. Iron 1 km Proton AMANDA (number of muons) log(E/PeV) 2 km Spase (number of electrons) Multiple Muons and Surface Electrons preliminary Measurement of the Cosmic Ray Composition at the Knee with SPASE-2 and AMANDA II 400 TeV – 6 PeV: Increase of the Atomic Mass ICRC 2003: Rawlins for AMANDA & SPASE

  7. B10: Observation of high-energy atm. neutrinos AMANDA B 10: 350 m/year Observation of high-energy neutrinos using Cherenkov detectors embedded deep in Antarctic ice, Ahrens et al., Nature 410, 2001, 441 Observation of high energy atmospheric neutrinos with the Antarctic muon and neutrino detector array, Ahrens et al., Phys. Rev. D. 66, 2002, 012005

  8. Atmospheric neutrinos with AMANDA II 2000:679 m horizontal Sensitivity up to the horizon. High energy selection in favor of astrophysical neutrinos. Selection optimized in declination bands. ICRC 2003: Hauschildt & Steele for AMANDA

  9. Atmospheric Neutrino Spectrum Measured with the AMANDA II Detector • Combination of • Neural network constructed energy sensitive variable • Directly measured variables • as input of regularized unfolding Spectrum up to 100 TeV compatible with Frejus data presently no sensitivity to LSND/Nunokawa prediction of dip structures between 0.4-3 TeV in future: excess studies at high energies ICRC 2003: Geenen for AMANDA

  10. Integral Method: Search for Diffuse Fluxes Assuming an E-2 spectrum: E2(E) < 8 10-7 GeV-1 cm-2 s-1 sr-1 Expected sensitivity 2000: ~ 310-7 GeV-1 cm-2 s-1 sr-1 ICRC 2003: Hill, Leuthold & Cooley for AMANDA Limits on Diffuse Fluxes of High Energy Extraterrestrial Neutrinos with the AMANDA-B10 Detector, Ahrens et al., Phys. Rev. Lett. 90, 2003, 251101

  11. Search for High Energy Neutrinos of All Flavorswith AMANDA II Flavor mixing: Signature: electromagnetic/hadronic cascade within the detector Data: 197 days (2000) Limit: 80 TeV < E < 7 PeV ICRC 2003: Kowalski for AMANDA Search for neutrino-induced cascades with the AMANDA detector, Ahrens et al., Phys. Rev. D 67, 2003, 012003

  12. B10 Limit on UHE Muon-Neutrinos E > 10 PeV: Earth opaque for nm Signature: ~ horizontal UHE nm events Background: atm. muon bundles Limit: 2.5 PeV < E < 5.6 EeV signal neural net cut parameter -> AMANDA sensitive to upward hemisphere above 1 PeV ICRC 2003: Hundertmark for AMANDA

  13. Search for extraterrestrial point sources declination averaged limit: lim  2.3•10-8 cm-2s-1 B10 A II 3 Ice ICRC 2003: Hauschildt & Steele for AMANDA Search for Point Sources of high-energy neutrinos with AMANDA, Ahrens et al., Ap. J. 583, 2003, 1040

  14. 130 days 1997 DAMA 187 days 1999 Search for Muons from WIMP Annihilation in the Center of the Earth with AMANDA B10 No WIMP signal observed ! ICRC 2003: Olbrechts for AMANDA Limits to the muon flux from WIMP annihilation in the center of the Earth with the AMANDA detector, Ahrens et al., Phys. Rev. D, 66 2002, 032006

  15. Search for High Energy Muon Neutrinos from Gamma-Ray Bursts <20° 317 BATSE triggers (1997—2000) Limitassuming WB spectrum: 4 x 10-8GeV/s/cm2/sr ICRC 2003: Hardtke, Kuehn & Stamatikos for AMANDA

  16. Count rates 0 5 10 sec Search for Neutrino Bursts from Supernovae Amanda-II Amanda-B10 B10: 60% of the Galaxy A-II: 95% of the Galaxy IceCube: up to LMC IceCube ICRC 2003: Feser for AMANDA Search for supernova neutrino bursts with the AMANDA detector, Ahrens et al., Astropart. Phys. 16, 2002, 345

  17. New AMANDA-II DAQ ICRC 2003: Wagner for AMANDA

  18. Conclusions • Improvement of the Analysis • Substantial improvement of the DAQ (2003) • Observed: atm. m and n • Not observed: HE flux excess, point sources, GRB, WIMPs, Monopoles, SN, SNR... • Best limits on additional processes • Exclusion of theoretical models • IceCube...

  19. - 80 Strings • - 4800 PMTs • 1 km3 • 2004 - 2010 South Pole Dark sector Skiway AMANDA Dome IceCube Planned Location 1 km east

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