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. ~1 TeV neutrino-induced
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. nm+nm = g + g Milagro: Galactic plane > 10 TeV preliminary 3s 5s
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. motion of the earth around the sun
preliminary
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: muons
preliminary

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