Neutrino Astronomy

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No observational evidence (from baryons or high energy photons)

Cores of AGNs (rather than in the jets) by photo-meson interactions or via p−p collisions in a collapsing galactic nucleus or in a cacooned black hole.

The most optimistic predictions of the AGN core model have already been ruled out by AMANDA

Slide 36

Mannheim, Protheore and Rachen Model

Slide 37

Neutrinos from Cosmic Rays

~50 events/km2/yr

Slide 38

Size Perspective for KM3

50 m

1500 m

2500 m

300 m

AMANDAII

Slide 39

Detection Technique

neutrino

muon or tau

Cerenkov

light cone

detector

interaction

The muon radiates blue light in its wake

Optical sensors capture (and map) the light

See Talks in this Session

Slide 40

Detection of e , , 

O(km) long muon tracks

direction determination

by cherenkov light timing

 17 m

Slide 41

Eµ= 10 TeV

Eµ= 6 PeV

Measure energy by counting the number of fired PMT.

(This is a very simple but robust method)

Muon Events

Slide 42

Determining Energy

10 TeV m

6 PeV m

375 TeV Cascade

Slide 43

 Double Bang

E << 1PeV: Single cascade

(2 cascades coincide)

E ≈ 1PeV: Double bang

E >> 1 PeV: partially contained

(reconstruct incoming tau track and cascade from decay)

Regeneration makes Earth quasi

transparent for high energie ;

(Halzen, Salzberg 1998, …)

Also enhanced muon flux due to

Secondary µ, and nµ

(Beacom et al , astro/ph 0111482)

Learned, Pakvasa, 1995

Slide 44

Tau Cascades

E << 1PeV: Single cascade

(2 cascades coincide)

E ≈ 1PeV: Double bang

E >> 1 PeV: partially contained

(reconstruct incoming tau track and cascade from decay)

Slide 45

Slide 46

Neutrino ID (solid) Energy and angle (shaded)