AMANDA

Latest Results of AMANDA Wolfgang Rhode Universität Dortmund Universität Wuppertal for the AMANDA Collaboration

AMANDA South Pole Dark sector AMANDA Dome Runway

Neutrino Telescope in the Ice 1997: AMANDA-B OMs on 10 Strings 2000: AMANDA-II 677 OMs on 19 Strings

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

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

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

B10: Observation of high-energy atm. neutrinos 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, AMANDA B 10: 350  /year

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

Atmospheric Neutrino Spectrum Measured with the AMANDA II Detector ICRC 2003: Geenen for AMANDA 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 TeV in future: excess studies at high energies

Integral Method: Search for Diffuse Fluxes 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, Expected sensitivity 2000: ~ 3  GeV -1 cm -2 s -1 sr -1 E 2  (E) < 8  GeV -1 cm -2 s -1 sr - 1 Assuming an E -2 spectrum:

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

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

Search for extraterrestrial point sources ICRC 2003: Hauschildt & Steele for AMANDA Search for Point Sources of high-energy neutrinos with AMANDA, Ahrens et al., Ap. J. 583, 2003, 1040 declination averaged limit:  lim  cm -2 s -1 Sourcedec.[deg]B 10A II SS M Crab Mkn Mkn Cyg. X Cas. A A II B10 3 Ice

Search for Muons from WIMP Annihilation in the Center of the Earth with AMANDA B10 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, , days DAMA 187 days No WIMP signal observed !

Search for High Energy Muon Neutrinos from Gamma-Ray Bursts ICRC 2003: Hardtke, Kuehn & Stamatikos for AMANDA 317 BATSE triggers (1997—2000) Limit assuming WB spectrum: 4 x GeV/s/cm 2 /sr  <20°

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

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

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

AMANDA South Pole Dark sector AMANDA IceCube Planned Location 1 km east Dome Skiway - 80 Strings PMTs -1 km

New Reactions e + N   e - + X electron cascade 375 TeV ≈ 300 m diameter PeV  (300 m)    decays  + N   - + X double bang event

AMANDA