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The ANTARES Neutrino Telescope

The ANTARES Neutrino Telescope. Mieke Bouwhuis 27/03/2006. 1’. 1’. 1’. 1’. radio 10 -8 eV optical 10 eV x rays 10 4 eV gamma rays 10 12 eV. Broadband light source. The pulsar in the Crab nebula. The observed radiation. g. e -. e -. g. Synchrotron radiation.

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The ANTARES Neutrino Telescope

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  1. The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006

  2. 1’ 1’ 1’ 1’ radio 10-8 eV optical 10 eV x rays 104 eV gamma rays 1012eV Broadband light source The pulsar in the Crab nebula

  3. The observed radiation g e- e- g Synchrotron radiation Inverse Compton scattering But: for some sources no synchrotron radiation is seen…

  4. All particle cosmic ray spectrum relative particle flux (logarithmic units) energy (eV) No point sources found yet

  5. e, g, p and n from cosmic accelerators

  6. Pulsar Supernova Remnant (SNR) Gamma-ray Burst (GRB) Active Galactic Nucleus (AGN) Microquasar Neutrinos from high-energy sources • Neutral  point back • Weak interaction  no absorption

  7. Indirect neutrino detection Neutrino interaction (ne, nm, nt): Scattering angle median scattering angle (degrees) neutrino energy (GeV)

  8. Neutrino cross section Mean free path: cross section (cm2) ~108 m at 1 TeV neutrino energy (GeV) Very large volume needed

  9. The ANTARES neutrino telescope Mediterranean Sea, near Toulon

  10. Detection volume and medium • sea + earth = large volume Instrumented volume = 0.02 km3 Effective volume = 0.2 km3 (at 10 TeV) = 1 km3 (at 10 PeV) • water for production of Cherenkov light • water is transparent • depth of 2.5 km for shielding against atmospheric background

  11. Detection principle c(tj - t0) = lj + dj tan(qc) water properties dx = 20 cm dt = 1 ns dq = 0.2°

  12. Signals in the detector

  13. Signals in the detector 100 kHz n crosses the detector in 2 ms

  14. proton atmospheric m atmospheric n Earth sea atmosphere proton cosmic n Different types of background

  15. filter PC ANTARES data processing system • finds all correlated data • real time • data reduction by factor 104 • high efficiency (50%) • high purity (90%) • low threshold: En > 200 GeV m all raw data 10 Gb/s finds cosmic neutrinos physics data analysis 1 Mb/s shore station

  16. Angular resolution

  17. February 14, 2006

  18. March 2, 2006

  19. Line 1: data taking Physics data taking LED beacon calibration

  20. LED beacon for time calibration Line 1 MILOM ~70 m

  21. Event Display – LED beacon

  22. real data Monte Carlo 4 ms space-time correlated hits “snapshot” hit Muon trigger rate Physics event found by filter: rate (Hz) number of correlated hits

  23. 4 ms space-time correlated hits “snapshot” hit : hits used by the fit Event Display Physics event 17267 in run 21241 Physics event found by filter:

  24. zenith angle q = 179° Event Display Physics event 17267 in run 21241

  25. zenith angle q = 146° Event Display

  26. zenith angle q = 80° Event Display Upgoing!

  27. Zenith angle distribution 1394 events after 14 hours of data taking

  28. Gamma-ray bursts (GRB) • short and intense flashes of MeV gamma rays • happen unexpectedly, and take place at random locations in the sky • detected by satellites • most information from the observation of the ‘afterglow’ • mechanism:

  29. GRB warning systems

  30. Specific ANTARES features GRB features GRB warning systems • All-data-to-shore • concept • Data processing • farm • Software filters filter PC GRB duration (s) Detection of neutrinos from GRBs Combine into the “GRB method”

  31. Data taking after a GRB alert

  32. Delays and buffering

  33. ratio of effective volumes GRB method standard neutrino energy (GeV) Gain in sensitivity for GRBs

  34. Conclusions • Composition of jets → e versus p • Origin of UHE cosmic rays • Line 1 operational, 12 lines end of 2007 • Measured time resolution of ~1 ns • Expected angular resolution 0.2° • GRB method increases the sensitivity

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