science with 40 IceCube strings

IOFG 2010Francis Halzen

neutrinos with 40 strings

We have measured the atmospheric neutrinospectrum to an energy of 400 TeV. The data isconsistent with the predicted energy dependence.IceCube can therefore search for cosmic neutrinosby (high) energy (and not just clustering), i.e. bylooking for neutrinos with an energy that is notcompatible with atmospheric origin.

250,086 pe65 deg10 PeVp-value 10-3

~1 TeV neutrino-inducedmuon

preliminary

sources of the Galactic cosmic rays

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

= = time in years

3

5

Milagro: Galactic plane > 10 TeVpreliminary

muon (!) astronomy

We have established that the arrival directions ofthe highest energy Galactic cosmic rays are notuniformly distributed in the sky. We find a largeexcess in the direction of Vela, the strongest gammaray source in the sky.

Note: muons with energy in excess of 20 TeVhave a gyroradius of less than 0.1 pc. The Velapulsar is at ~300 pc.

20 TeV2 KHz3 deg

10 TeVto several100 TeV

motion of the earth around the sun

shadow of the moon

preliminary

preliminary

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 2.3 level.• we have reached the sensitivity to confirm or rule out gamma ray bursts as the sources.

preliminary

northern sky: 14139 neutrinos

southern sky: 23151 muons

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