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Results from the ANTARES neutrino telescope

Results from the ANTARES neutrino telescope. G. Giacomelli University of Bologna and INFN Venezia , 27/4/ 2011. Introduction.   astronomy ANTARES. Optical detection. Infrastructure Downgoing muons Preliminary n m data Exotica (Fast MMs, Nuclearites,…) Earth-Sea Science

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Results from the ANTARES neutrino telescope

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  1. Results from the ANTARES neutrino telescope G. Giacomelli University of Bologna and INFN Venezia, 27/4/ 2011 • Introduction. astronomy • ANTARES. Optical detection. Infrastructure • Downgoing muons • Preliminary nm data • Exotica (Fast MMs, Nuclearites,…) • Earth-Sea Science • Conclusions. Outlook ANTARES Results-Venezia 2011

  2. High energy neutrino astrophysics:Galactic: SN, SNRs, m-quasars, molecular clouds, ... Extra-Galactic: AGNs, GRBs, dark-GRBs, GZK, .... • Searches for New Physics: Dark matter (Sun, GC), Magnetic Monopoles, ?? • Earth-Sea Science: Oceanography,seabiology, seismology, environmental monitoring 1. Introduction Science with Deep Sea Neutrino Telescopes ANTARES Results-Venezia 2011

  3. Neutrino Astronomy • Advantages w.r.t. other messengers - -Photons: interact with CMB and matter • Protons: interact with CMB and are deflected by magnetic fields • Neutrons: are not stable • Drawback: large detectors (~GTon) are needed. photon n  p ANTARES Results-Venezia 2011

  4. CRAB CRAB VELA SS433 SS433 Sky Observable by HE Neutrino Telescopes AMANDA/IceCube (South Pole) ANTARES/KM3 (43° North) Mkn 421 Mkn 501 Mkn 501 RX J1713.7-39 GX339-4 Galactic Centre ANTARES Results-Venezia 2011

  5. 2. ANTARES Site & Infrastructure -2475m Shore Station IFREMER Toulon Centre 40 km submarine cable FOSELEV Marine ANTARES Results-Venezia 2011

  6. ANTARESOptical detection of nm gč 43° m- interaction nm ANTARES Results-Venezia 2011

  7. Buoy 2 ARS LCM 1 MB per PMT 14.5 m 3 PMTs LCM Sector LCM 448 m MLCM 2.5 km LCM 40 km cable to shore Storey SCM Junction box Seabed

  8. Storey 1 Storey 8 Storey 14 Storey 20 Storey 25 AcousticPositioning Measure every 2 min: Distance line bases to 5 storeys/line and also storey headings and tilts Radial displacement Precision ~ few cms ANTARES Results-Venezia 2011

  9. Two Events reconstructed up-going neutrino: detected in 6/12 detector lines: reconstructed down-going muon: detected in all 12 detector lines: ANTARES Results-Venezia 2011

  10. Example: Neutrino candidate height time ANTARES Results-Venezia 2011

  11. Example of a muon bundle height time ANTARES Results-Venezia 2011

  12. 2,5km 6km 3. DowngoingmuonsDepth Intensity Relation from Zenith Distribution Astropart. Phys. 34 (2010) 179 ANTARES Results-Venezia 2011 Zenith angle distribution of muon flux at 2000 m

  13. Search for deficit of downgoingmuons In the direction of the moon (diameter 0.5 degrees) Verification of the absolute pointing of the telescope Preliminary: Live time 295 days: 2.5 sigma effect Moon Shadow preliminary ANTARES Results-Venezia 2011

  14. 4. Preliminary data for Upgoing NeutrinosAngular Resolution 2007+2008 analyses: Angular resolution ~ 0.5°0.4° (ΔΘ < 1° , in 75% of cases) - Integrated over all energies (E-2 flux) - Half of data only 5 lines Full 12 line detector m n ANTARES Results-Venezia 2011

  15. Sky Map Selection optimized for Model Discover Potential (Λ >-5.4): (Live time 295 days) galactic coordinates visibility 2190 selected events Most significant cluster located at: ra=134.6°, δ=13.4° (post-trial probability to be background 2.4%) ANTARES Results-Venezia 2011

  16. Point Source Limits Quoted for E-2 flux ANTARES-best limits in the Southern sky More data (2009-2010) on tape Expect further improvement energy estimator included ANTARES Results-Venezia 2011

  17. High Energy Diffuse nm flux E2F(E)90%= 5.3×10-8 GeV cm-2 s-1 sr-1 20 TeV<E<2.5 PeV “Search for a diffuse flux of high-energy νμwith the ANTARES n telescope” Phys. Lett. B696 (2011) 16-22. ANTARES Results-Venezia 2011

  18. 5. Exotica (preliminary)Fast Intermediate Mass Magnetic Monopoles • Required in many models of spontaneous • symmetry breaking • Upgoing  masses less than ~1014 GeV • High photon yield (8.5x103 times μ) • Cherenkov threshold b >0.74 • Delta rays for b ≥ 0.5 • Track reconstruction with b free MM-Cherenkov MM-delta rays muon Monopole muon neutrino ANTARES Results-Venezia 2011

  19. 6. Earth-Sea Science Seismograph: Japan Earthquake 40 20 0 -20 -40 In laboratory Deployment Buried at site

  20. neutrino Hydrophone Array Cascade Acoustic Pressure Waves AMADEUS: Acoustic Detection of Neutrinos

  21. Biocamera 2 min Bursts: bioluminescence from Macroscopic organisms 40K

  22. 7. Conclusions - Outlook • The 12 line ANTARES detector is taking data, also with several instruments for Earth Sea Sciences studies. • The collaboration has shown capable response for solving • technical difficulties (ex.: the breaking of the connecting cable) • Compared to AMANDA-IceCube, ANTARES completes the coverage of the neutrino sky, with an angular resolution of 0.5° • First analyses of the downgoing muons allowed calibrations and measurements of the flux; comparison with MC with 30% sis err • First analyses of neutrinos with 5-12 lines for data taken in • 2007-2008 allowed a first search for cosmic point-like sources. • A search was made for a diffuse flux of H.E. muon neutrinos • ANTARES sensitivity for point sources is comparable to AMANDA • First tentative results in Earth and Sea Sciences • The technical success paves the way to KM3NeT in the Mediterranean ANTARES Results-Venezia 2011

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