1. 1 IceCube Christian Spiering for the IceCube Collaboration EPSC, Cracow July 2009

2. 2 The IceCube Collaboration USA: Bartol Research Institute, Delaware University of California, Berkeley University of California, Irvine Pennsylvania State University Clark-Atlanta University Ohio State University Georgia Tech University of Maryland University of Alabama, Tuscaloosa University of Wisconsin-Madison University of Wisconsin-River Falls Lawrence Berkeley National Lab. University of Kansas Southern University and A&M College, Baton Rouge University of Alaska, Anchorage Sweden: Uppsala Universitet Stockholm Universitet UK: Oxford University Belgium: Université Libre de Bruxelles Vrije Universiteit Brussel Universiteit Gent Université de Mons-Hainaut Germany: DESY-Zeuthen Universität Mainz Universität Dortmund Universität Wuppertal Humboldt Universität MPI Heidelberg RWTH Aachen Japan: Chiba University New Zealand: University of Canterbury 33 institutions, ~250 members Netherlands: Utrecht University Switzerland: EPFL

3. 3 AMANDA IceCube The Amundsen-Scott Station South Pole Station Building Astronomy Sector skiway

4. 4 IceCube 05/06: 8 Remaining: 22 IceCube Strings 5 DeepCore Strings  complete in January 2011 IceCube Observatory

5. 5 IceCube/Amanda Selected results cosmic ray (CR) spectrum,  CR composition  CR anisotropies  shadow of the moon  atmospheric neutrinos (oscillations, effects of quantum gravity, … )  neutrino point sources  gamma ray bursts  multimessenger approaches  diffuse fluxes  dark matter  magnetic monopoles  supernova bursts  atmosphere physics  glaciology  new technologies for highest energies (radio, acoustics)  IceCube high energy extension plans 

6. 6 Shadow of the Moon Cosmic Rays  Absolute pointing  1°  Angular resolution  1° 0.5° 8 months IceCube 40 strings Downward muons, max. 28° above horizon, median energy of primary parent ~ 30 TeV

7. 7 Large-scale anisotropy of downgoing muons IceCube (40 strings 2008) anisotropies on the per-mille scale (skymap in equatorial coordinates) 90 -90 24h 0 0 90 -90 12 TeV 126 TeV

8. 8 MILAGRO Compare to Northern hemisphere Tibet air shower array Simulation (Lallement et al. Science 2005) Compton-Getting effect ? Heliosphere effect ? Nearby pulsars ? Interstellar magnetic field ? First observation on Southern hemi- sphere adds important piece of information.

9. 9 Search for neutrino point sources Amanda 2000-2006 6595 Events

10. 10 5 δ=90º 24h 0h Max Significance δ=54º, α=11.4h 3.38σ 95 of 100 background maps (data randomized in RA) have a point with significance ≥ 3.38  Amanda 2000-2006 significance map 0 2.5 5

11. 11 First look above horizon (IceCube 2007, 22 strings) PeV-EeV range Southern hemisphere Northern hemisphere Sensitivity of ¼ IceCube, 1 year ~ 2 x sensitivity of Amanda 7 years  enter new territory !

12. 12 Northern hemisphere TeV - PeV Background: atmospheric neutrinos Southern hemisphere PeV - EeV Background: atmospheric muons Reduced by 10 -5 using energy cut 175.5 days livetime, 6796 up-going events, 10981 down-going events Preliminary All-sky map (6 months IceCube 2008, 40 strings)

13. 13 Hottest location at r.a.=114.95°, dec.=15.35° Pre-trial -log 10 (p-value) = 4.43 all-sky p-value is 61%  not significant Preliminary All-sky map (6 months IceCube 2008, 40 strings)

14. 14 Point Sources limits/sensitivities AMANDA 7 yr 40-string Discovery Potential: 5 σ in 50% of trials 40-string Sensitivity: Flux excluded at 90%cl ANTARES IC22 SK MACRO 80-string Sensitivity: Based on 40-string analysis 40 string results preliminary

15. 15 Diffuse Neutrino Fluxes IceCube EHE analysis WB bound GZK Auger IceCube atm. Integral limits (E -2 flux) from Baikal, Amanda IceCube

16. 16 t ~ -10  -100st ~ 0  t90 t ~ t90  ? Waxman & Bahcall, PRL 78:2292 (1997) Waxman & Bahcall, ApJ 541:707 (2000) Razzaque et al., PRD 68 (2003) Neutrinos from GRB

17. 17 t ~ -10  -100st ~ 0  t90 t ~ t90  ? Waxman & Bahcall, ApJ 541:707 (2000) Neutrinos from GRB AMANDA limit from 408 bursts 1997-2003 Waxman-Bahcall GRB prediction 10 -10 10 -7 10 -8 10 -9 10 4 10 6 10 5 10 7 10 8 neutrino energy E (GeV) E 2  flux (GeV  cm -2  s -1  sr -1 )

18. 18 Neutrinos from naked-eye GRB080319B  Duration: 70 s, z=0.94  Brightest GRB (optical) ever  Large number of  -ray, x-ray, UV and optical, observations Pi of the Sky  Detector was in maintenance mode 9 out of 22 strings.  Signal expectation: 0.1 events (  = 300)  No events at GRB position/time after cut  Limit Full-IceCube expectation ~ 1 event

19. 19 Indirect Dark Matter Search Sun Detector Earth Amanda skymap around Sun

20. 20 Indirect Dark Matter Search

21. 21 Indirect Dark Matter Search ….. apply to spin-dependent cross section Models with strong spin-dependent coupling are the least constrained by direct DM searches. W.r.t. spin-dependent coupling, Amanda & IceCube are ~100 times more sensitive than direct search experiments (Sun is mostly hydrogen) Effect of DeepCore

22. 22