1. science with 40 IceCube strings IOFG 2010 Francis Halzen

2. neutrinos with 40 strings We have measured the atmospheric neutrino spectrum to an energy of 400 TeV. The data is consistent with the predicted energy dependence. IceCube can therefore search for cosmic neutrinos by (high) energy (and not just clustering), i.e. by looking for neutrinos with an energy that is not compatible with atmospheric origin.

3. preliminary ~1 TeV neutrino-induced muon 250,086 pe 65 deg 10 PeV p-value 10-3

4. sources of the Galactic cosmic rays The Milagro experiment mapped the plane of our Galaxy in > 10 TeV gamma rays identifying supernova remnants that may be the long sought- after sources of the cosmic rays. We should detect them as cosmic neutrino sources in the near future.

5. preliminary Milagro: Galactic plane > 10 TeV 3s 5s nm+nm = g + g time in years

6. muon (!) astronomy We have established that the arrival directions of the highest energy Galactic cosmic rays are not uniformly distributed in the sky. We find a large excess in the direction of Vela, the strongest gamma ray source in the sky. Note: muons with energy in excess of 20 TeV have a gyroradius of less than 0.1 pc. The Vela pulsar is at ~300 pc.

7. preliminary motion of the earth around thesun 10 TeV to several 100 TeV preliminary 20 TeV 2 KHz 3 deg shadow of the moon

8. extragalactic sources • at the highest energies we have extended the • neutrino sensitivity of IceCube to the Southern • sky. • we have established the best sensitivity to GZK • neutrinos. • we measured a correlation between the highest • energy cosmic rays and neutrinos at the 2.3s • level. • we have reached the sensitivity to confirm or • rule out gamma ray bursts as the sources.

9. northern sky: 14139 neutrinos southern sky: 23151 muons preliminary

10. observation of 117 • burst with IceCube-40 • strings • if GRB are the source: • 8 events expected, • none seen