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Exotic Physics searches in ANTARES

Workshop on Exotic Physics with Neutrino Telescopes Uppsala, September 20-22, 2006. Exotic Physics searches in ANTARES. Ersilio Castorina Pisa University and INFN on behalf of the ANTARES Collaboration. Outline. Current status of ANTARES MC simulation of χ Dark Matter from the Sun

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Exotic Physics searches in ANTARES

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  1. Workshop on Exotic Physics with Neutrino Telescopes Uppsala, September 20-22, 2006 Exotic Physics searches in ANTARES Ersilio Castorina Pisa University and INFN on behalf of the ANTARES Collaboration Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  2. Outline • Current status of ANTARES • MC simulation of χDark Matter from the Sun • Ongoing studies (preliminary only) : • early results for χfrom the Earth • first estimate of “slow” Magnetic Monopoles Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  3. ANTARES Astronomy with a Neutrino Telescope and Abyss environmental RESearch http://antares.in2p3.fr Project to build an undersea neutrino telescope in the Mediterranean Sea Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  4. ANTARES collaboration Erlangen NIKHEF Amsterdam, Groningen ITEP Moscow IFREMER, Brest DAPNIA, Saclay IReS, Strasbourg Mulhouse CPPM , Marseille IFREMER,Toulon COM, Marseille OCA, Nice Genova Bologna Bari IFIC Valencia Roma Pisa Catania LNS Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  5. Submarine Cable ANTARES Site The detector will be located at 2400 m depth, 40 km off the Toulon (France) coast (42º50’N, 6º10’E). The shore station is at La Seyne sur Mer, 40 km NW of the ANTARES site. Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006 Institute Michel Pacha (La Seyne sur Mer)

  6. Detector Design and Construction Status Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  7. Detector Geometry 12 lines (900 PMTs) 25 storeys / line 3 PMTs/storey Horizontal layout Depth 2400 m 40 km to shore storey 14.5 m 350 m 100 m Junction box 70 m Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006 Interconnections

  8. nm m W X N Neutrino Detection gč 43° 2400 m depth m Cherenkov lightfrom m induced by ninteraction detected by 3D PMT array Time & positionof hits allow the reconstruction of the m (~ n) trajectory nm CC interaction Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  9. Basic Dector Element: the storey Optical Beacon for timing calibration Optical Module 17” glass sphere 10” PMT Ham. R7081-20 in a cage for magnetic shielding Local Control Module electronics boards for readout of PMT signal and data acquisition (plus calibration equipment) Hydrophone RX for acoustic positioning Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  10. Construction Status Line 1 2006 MILOM 2005 • Apr 2005: Mini Instrumentation Line with OMs (MILOM) • Mar 2006: Line 1, first complete detector line • 2006: Line 2, deployed in July, to be connected TODAY ! • 2006 - 2007: installation of remaining 10 lines • 2008+: Physics with full detector! Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  11. Diagonal: larger distance, less intensity, light scattering s = 2.6 ns Horizontal s = 0.7 ns DT between hits on 2 OMs in the same storey Light source A Selection of Results: Time Calibration • The timing calibration systems of ANTARES allow: • ~100 ns in absolute timing • ≤ 1 ns in relative timing (between OMs) Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  12. + A Selection of Results: a downgoing m • Triggered hits • Hits used in fit • Snapshot hits ANTARESpreliminary m q = 172o P(c2,ndf) = 0.94 Hit altitude (relative to mid detector) [m] Hit time [ns] Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  13. Searches for Neutralino DMin ANTARES Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  14. ANTARES Science goals • Neutrinos from point-like & diffuse flux sources • Pulsars • Young SN Remnants (up to 100 ev/year/km2 ) • Microquasars (SS433: up to 250 ev/year/km2) • AGN (steady) • Gamma Ray Bursts (transient 1-100 s) + oceanography, biology, seismology … • Exotic Physics • Neutrinos from c annihilation in the Sun, the Earth and the Galactic Centre • Magnetic monopoles Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  15. From c down to n Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  16. mSUGRA Predictions & Sensitivity • Less constrained models are currently under investigation • Improvements of low E reco will affect (i.e. lower) the sensitivity Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  17. The signal is expected within a cone of a few degrees (max ~10 ) depending on mc Different atmospheric background Less restrictive cuts on events direction Different Sensitivity Annihilation in the Earth: work in progress mSUGRA flux predictions are extremely low ! Evaluate just the sensitivity (a general MSSM model could perhaps produce much more neutrinos!) Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  18. Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  19. Searches for Magnetic Monopolesin ANTARES Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  20. Exp. Upper Limits on the average monopole flux Detection of Magnetic Monopoles Monopoles are predicted by Grand Unified Theories • They can be studied through their interaction with matter: • Ionization energy loss • Radiative energy loss • Catalysis of proton decay Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  21. Detection of Magnetic Monopoles MM produce direct and d-ray induced Cherenkov light (a tiny but easily detectable fraction of the ionization energy loss!) • Direct Cherenkov emission (bth=0.74 in sea water) A monopole with gD and b=1 emits about 3·106 photons between 300 and 600 nm per cm path length Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  22. # emitted photons/cm path lenght Direct d-ray m Detection of Magnetic Monopoles • d-ray emission • Direct + d-ray Cherenkov radiation Kinetic Energy spectrum of d-rays Cherenkov Threshold for e- in water Tth= 0.25 MeV (Ph.D. Thesis by B. van Rens, NIKHEF) Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  23. ANTARES 1-year MACRO Upper limit on Monopole flux below the Cherenkov limit Simulation + dedicated Trigger & Analysis (Ph.D. Thesis by B. van Rens, NIKHEF) Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

  24. It’s indeed possible to detect DM signal (though indirectly!) Most promising sources: • Sun • Galactic Centre (though modelling still under debate) • Earth (though expected fluxes are low) It’s even easier to detect Monopole signal (if they exist!) Through Cherenkov light • direct • d-ray induced Conclusions & Outlook ANTARES has started data acquisition with the first full line Complete detector by the end of 2007 Thanks and… …stay tuned! Ersilio Castorina - Exotic Phys. with nu Telescopes , Uppsala Sept. 2006

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