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Astroparticle physics with large neutrino detectors

Astroparticle physics with large neutrino detectors. Existing detectors Physics motivation Antares project KM3NeT proposal. M. de Jong. Super-Kamiokiande detector. 50 kT water Cherenkov detector. 4p  4 He + 2e + + 2 n e + 25 MeV. e -. q. sun. Earth. n e. Atomic electron!.

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Astroparticle physics with large neutrino detectors

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  1. Astroparticle physics with large neutrino detectors • Existing detectors • Physics motivation • Antares project • KM3NeT proposal M. de Jong

  2. Super-Kamiokiande detector 50 kT water Cherenkov detector

  3. 4p  4He + 2e+ +2ne+ 25 MeV e- q sun Earth ne Atomic electron! Point to sun

  4. Super Nova 1987A Time correlation

  5. All particle cosmic ray spectrum Pierre Auger Observatory Where do they come from? F (m2 sr s GeV)-1 F= E-2.7 Emax = 1021 eV > 5 x 1019 eV (GZK) 1 / km2 /year E (GeV) 1 GeV 1010 GeV

  6. m nm N q X Neutrino detection • Neutral  point back • Weak interaction  no absorption Need huge detector

  7. 1960 Markov’s idea: • Range of muon: • Detect Cherenkov light: • Transparency of water: Use sea water as target/detector

  8. Amanda neutrino sky map atmospheric neutrinos horizon Atmospheric muons No point sources discovered yet

  9. Neutrino source candidates Supernova remnant (Crab nebula) Microquasar (SS433 etc.) Active Galaxy (e.g. M87)  1 ly  104 ly Black hole with  mass of sun Black hole with 108 x mass of sun galactic extra-galactic

  10. Neutrino production • Acceleration: • Decay:

  11. Physics motivation • Astrophysics • Neutrino astronomy • Composition of jets • Engine of cosmic accelerators • Particle physics • Origin of UHE cosmic rays • Massive particles (GUT) • Dark matter • Neutrino properties (nt, s)

  12. NT-200 AMANDA-B10 + NT-200 AMANDA-II/ANTARES IceCube/KM3NeT Diffuse neutrino fluxes DUMAND MPR W&B atmospheric neutrinos GRB

  13. Antares detector 42° 50’ N 6° 10’ E Atlas Equipped volume 0.1 km2 x 0.4 km (=800 x SuperK)

  14. medium properties dx = 20 cm dt = 1 ns dq = 0.2 deg. Detection principle nm+ N m+ X c(tj - t0) = lj + dj tan(qc)

  15. “All-data-to-shore” concept time 1 GB/s position 2 ms 10 ms DataFilter 1 MB/s events offline reconstruction determination of m trajectory

  16. GRB alert systems GRBs are detected by satellites Distribution of GRB alerts that follow the detection of a GRB within tens of seconds Possibly messages will follow with the location of the burst

  17. DataFilter DataFilter DataFilter DataFilter DataFilter DataFilter DataFilter DataFilter DataFilter DataFilter DataFilter 100 s of unfiltered data prior to the alert + few minutes of unfiltered data after the alert disk Data taking in case of a GRB alert GRB alert all data detector write all data to disk, including all data in memory alert trigger 100 DataFilter nodes with each 1 GB RAM location of the GRB disk events from the known direction specialised data filter data filtered offline looks for correlations in the data for the given direction

  18. Effective volume clustering and reconstruction using direction information standard clustering and reconstruction effective volume (km3) Improved detection efficiency log10 En (GeV) Detection efficiencies

  19. “All-data-to-shore” options: • GRB detection • Source tracking • Monopole detection • Periodic signals

  20. KM3NeT

  21. KM3NeT • Main objectives • Equipped volume 1 km3 (25 x Antares) • Cost/Volume x 0.5 • 4p Field Of View • Angular resolution 0.1 deg. • FP6 Design Study proposal March 2004 • NIKHEF leading partner IT • PMT & readout developments • Detector parts assembly in the Netherlands

  22. Summary • Water Cherenkov: Large neutrino detectors • Antares: “All-data-to-shore” concept • KM3NeT initiative 2004 - 2008 • Astroparticle physics with neutrinos

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