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What About Dark Matter?

~85% of the matter in the Universe is Dark Matter

At most a few % of the matter is baryons

Most people believe that the lightest SUSY particle is a stable neutralino and is probably the dark matter

These are weakly interacting and heavy

Evidence of clustering

Slide 30

Wimp Capture

Wimp Capture

Slide 31

Wimp Detection

Wimp Detection

Slide 32

Neutrino Astronomy Explores Extra Dimensions

Neutrino Astronomy Explores Extra Dimensions

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Cosmic Neutrino Factory

Cosmic Neutrino Factory

Slide 34

W-B Bound

W-B Bound

Slide 35

Evading the Bound “Neutrino only” sources that are optically thick to proton photo-meson interactions and from which protons cannot escape.

Evading the Bound “Neutrino only” sources that are optically thick to proton photo-meson interactions and from which protons cannot escape.

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

Mannheim, Protheore and Rachen Model

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Neutrinos from Cosmic Rays

Neutrinos from Cosmic Rays

Slide 38

Size Perspective for KM3

Size Perspective for KM3

Slide 39

Detection Technique

Detection Technique

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Detection of ne ,nm , nt O(km) long muon tracks

Detection of ne ,nm , nt O(km) long muon tracks

Electromagnetic and hadronic cascades

Slide 41

Muon Events Measure energy by counting the number of fired PMT.

Muon Events Measure energy by counting the number of fired PMT.

(This is a very simple but robust method)

Slide 42

Determining Energy

Determining Energy

Slide 43

Double Bang Regeneration makes Earth quasi

Double Bang Regeneration makes Earth quasi

transparent for high energie nt;

(Halzen, Salzberg 1998, …)

Also enhanced muon flux due to

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