ANTARES

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ANTARES

• Underwater Neutrino Telescope

Andreas Horneffer Slava Rychkov Tamas
Novak Abdeslem Rrhioua
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Goals I Astrophysics

• High-energy neutrino astronomy
• X-ray binaries
• supernovae
• AGNs
• gamma-ray bursters
• Cosmic ray puzzle

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Goals II Particle physics Cosmology

• Atmospheric neutrino oscillations ?? ?
  ??, ?e
• Search for dark matter WIMP decays,
  annihilations

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Detection I Cherenkov light from ? and ?

• Main event ?? N ? ? X (CC)

• Background atmospheric ?

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Detection II EM and hadronic showers
? N ? ? X (NC) ?e e ? ?e e (CC,NC)
Showers are point-like ? poor angular resolution
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Detector design

• 900 PMTs on 12 strings (0.1 km² effective area)

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Typical event simulation
E? 1.2 TeV
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Angular resolution
3 _at_ 100 GeV 0.3 _at_ 10 TeV
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Energy resolution
Within factor 6 _at_ 100 GeV 2.5 _at_
10 TeV
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Sensitivity / event rates

• Atmospheric ?? 240 events/year _at_ 1 TeV
• Cosmological diffuse flux 10 events/year

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Conclusion complementarity
ANTARES
BAIKAL, Russia
AMANDA, South Pole
NESTOR, Greece