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The ANTARES Neutrino Telescope A status report

The ANTARES Neutrino Telescope A status report

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The ANTARES Neutrino Telescope A status report

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  1. The ANTARES Neutrino TelescopeA status report Niccolò Cottini on behalf of the ANTARES Collaboration 44th Rencontres de Moriond February 2009

  2. The ANTARES Collaboration • Since 1996 • 7 countries • 22 laboratories • 200 physicists, engineers, sea scientists Niccolò Cottini

  3. Outline of the talk • Neutrino astronomy • The potential sources • The ANTARES detector • Construction milestones • Detector operations • The data taking campaign • The first physics analyses • Atmospheric muons • Atmospheric neutrinos • Search for cosmic neutrino sources • Indirect dark matter detection Niccolò Cottini

  4. The Neutrino Astronomy Niccolò Cottini

  5. Local galaxy group Galaxy p/A+p/g p+ p0+ ...  g g  nmm  nm nee Neutrino astronomy • g: interact with CMB and matter • Protons: deflection by magnetic fields • n: weakly interacting • huge target needed (100Mton - Gton)   p Niccolò Cottini

  6. Potential sources GALACTIC EXTRAGALACTIC Indirect dark matter search GRBs Supernova remnants See Damien Dornic’s talk See Vincent Bertin’s talk Pulsars AGNs Microquasars Niccolò Cottini

  7. ANTARES 12 lines MC 3D PMTarray Cherenkov light from m 43° Sea floor m nm interaction Detection principle Main detection channel: charged nm interaction giving an ultrarelativistic m Energy threshold: 10 GeV Niccolò Cottini

  8. The ANTARES detector Niccolò Cottini

  9. Galactic coordinates The ANTARES site 42°50’ latitude Nord 6°10’ longitude Est • Galactic Center • visible 75% of the day Niccolò Cottini

  10. The ANTARES site Toulon Shore Station La Seyne Submarine cable (~40km) Niccolò Cottini

  11. 350 m 14.5 m 100 m ~60 m The ANTARES detector 2500m depth Cable to shore Junction Box Link cable Niccolò Cottini

  12. The ANTARES detector 45° Storey Niccolò Cottini

  13. A detector storey LED Beacon DAQSlow Control ~0.6 ns resolution 17’’ glass sphere 10’’ PMT Titanium frame Hydrophone ~10 cm resolution Niccolò Cottini

  14. 2006 – 2008: deployments of the detector lines Line 1: 03 / 2006 Line 2, 3, 4, 5: 01 / 2007 Line 6, 7, 8, 9, 10: 12 / 2007 Line 11, 12: 05 / 2008 ~60 m Niccolò Cottini

  15. Detector layout Acoustic storey See Kay Graf’s talk … and several instruments for environment studies with the ANTARES infrastructure Niccolò Cottini

  16. Detector operations Niccolò Cottini

  17. Muon (Cherenkov) 2 µs crossing time 40K decay Continuous background  30 kHz * The detected signal Simulation 2 min • Bioluminescence • Continuous background  30 kHz * • Occasional bursts ~MHz 792 days * 10’’ PMT, 0.3 p.e. threshold Niccolò Cottini

  18. m The Trigger • Front end chip digitizes charge and time of a light signal • All data transmitted through multiplexed Gigabit links • the whole data flow can not be written to disk • Computer farm running a software trigger: • look in all directions for light signals compatible with a muon track • when found, write a Physics Event • Other triggers exist: cluster of storeys, GRBs, Galactic Center, … “ALL DATA TO SHORE” SCHEME: Niccolò Cottini

  19. Track reconstruction =35o Niccolò Cottini

  20. Number of triggers 5 lines (2007) 10 or more lines (2008) Data taking ongoing… …accumulating neutrinos Niccolò Cottini

  21. The first physics analyses Niccolò Cottini

  22. Atmosphere Sea Earth atmospheric n atmospheric m cosmic n Niccolò Cottini

  23. Muon flux at the detector 107 atmospheric m per year* 103 atmospheric n per year* Atmosphere Sea Earth cosmic n * Reconstructed tracks in 12 line detector Line 1: 03 / 2006 Line 2, 3, 4, 5: 01 / 2007 Line 6, 7, 8, 9, 10: 12 / 2007 Line 11, 12: 05 / 2008 Performance paper submitted First physics analyses completed Ongoing analysis Data taking Niccolò Cottini

  24. data CORSIKA (QGSJET01) + NSU model MC uncert. Atmospheric muon studies with 5 lines • Systematic uncertainty ± 30% • Main contributions • optical module response • absorption length of the light in water See Claire Picq’s talk Niccolò Cottini

  25. Likelihood ratio Data, m MC, n MC (x100) Selection of neutrino events with 5 lines L: maximum likelihood of the track fit MC Upgoing events Downgoing events Upgoing events dominated by the tail of badly reconstructed atmospheric muons Niccolò Cottini

  26. m n Selection of neutrino events with 5 lines Data, m MC, n MC (x100) y = s(x) / [ s(x) + b(x) ] Purity = ~90%; Efficiency = ~30% Niccolò Cottini

  27. Data MC Uncertainties Detection of atmospheric neutrinos with 5 lines • Test of detector response to a known neutrino signal • A preliminary step before searching for cosmic sources ANTARES 5 lines (164 days live time) Data : 185 n (1,1 / j), 93% purity Mainly optical module response and calibration uncertainties (preliminary) MC : Bartol flux (20% uncertainty on the absolute n flux) Niccolò Cottini

  28. Search for point like neutrino sources with 5 lines • Definition of a potential source list • Analysis optimization by MC, for E-2 flux • Data unblinding: 94 neutrino events No discovery 90% CL flux limit See Katia Fratini’s talk Niccolò Cottini

  29. Preliminary analysis of 10 line data Preliminary quality cuts 208 neutrinos Dec 2007 – Apr 2008 : 100 days live time Niccolò Cottini

  30. A neutrino event on 12 lines Niccolò Cottini

  31. KM3 Conclusion • ANTARES today • Successful end of construction phase • Technology proven • Data taking ongoing • First physics outputs • Atmospheric m and n, cosmic neutrino sources, dark matter • Neutrino oscillations, magnetic monopoles, VHE neutrino interactions, … • On the road for the next step • KM3Net… See Christopher Naumann’s talk Niccolò Cottini

  32. Vue de la salle de contrôle d’ANTARES A view from ANTARES control room Niccolò Cottini