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

2. 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

3. Astroparticle physicsus

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 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]

7. 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

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
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

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

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

13. 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

14. Average  Individual b a
b-2

15. 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

16. 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
+ -

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