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

AMANDA  IceCube Sweden: Germany: UK: Netherlands: Japan: Belgium: Uppsala Universitet Stockholm Universitet Germany: Humboldt Universität Universität Mainz DESY-Zeuthen Universität Dortmund Universität Wuppertal Universität Berlin 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

Astroparticle physics us

p gD…pn...  N ...m, casc

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

AMANDA/IceCube Amundsen-Scott South Pole Station 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]

Detection Strategies Presented in this talk: plus: 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

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

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

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

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

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

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

Average  Individual b a b-2

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

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

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