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by Nicolas PICOT-CLEMENTE CNRS/CPPM, Marseille

ANTARES experiment status and first results …. by Nicolas PICOT-CLEMENTE CNRS/CPPM, Marseille. Neutrino telescope: Detection principle. 3D PMT array. p, a. n m. p. m. Cherenkov light from m. g č. n m. g. 43°. Sea floor. m. interaction.

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by Nicolas PICOT-CLEMENTE CNRS/CPPM, Marseille

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  1. ANTARES experiment status and first results … by Nicolas PICOT-CLEMENTE CNRS/CPPM, Marseille

  2. Neutrino telescope: Detection principle 3D PMTarray p, a nm p m Cherenkov light from m gč nm g 43° Sea floor m interaction Reconstruction of m trajectory(~ n)from timing and position of PMT hits n

  3. The ANTARES Collaboration • NIKHEF, Amsterdam • KVI Groningen • NIOZ Texel • ITEP,Moscow • University of Erlangen • ISS, Bucarest • IFIC, Valencia • UPV, Valencia • CPPM, Marseille • DSM/IRFU/CEA, Saclay • APC Paris • IPHC, Strasbourg • Univ. de H.-A., Mulhouse • IFREMER, Toulon/Brest • C.O.M. Marseille • LAM, Marseille • GeoAzurVillefranche • LPC, Clermont Ferrand (new) • University/INFN of Bari • University/INFN of Bologna • University/INFN of Catania • LNS – Catania • University/INFN of Pisa • University/INFN of Rome • University/INFN of Genova

  4. The ANTARES site & Infrastructure Shore Station

  5. The ANTARES detector 2500m 450 m 70 m • 900 PMTs • 12 lines + I.L. • 25 storeys / line • 3 PMTs / storey 40 km to shore Junction Box Interlink cables

  6. ANTARES Construction Milestones March 2006: First line connected. September 2006: Line 2. January 2007: Lines 3-5. December 2007: 10 Lines on the site. May 2008: Whole detector.

  7. Expected performance (MC Studies) mrec−mtrue mrec−n dominated by kinematics Effective area for n [m2] m n dominated by reconstruction • increases with energy • Earth opacity above 100 TeV • Angular resolution better than 0.3° above a few TeV, limited by: • Light scattering + chromatic dispersion in sea water: s ~ 1.0 ns • TTS in photomultipliers: s ~ 1.3 ns • Electronics + time calibration: s < 0.5 ns • OM position reconstruction: s < 10 cm (↔ s < 0.5 ns)

  8. Detector visibility CRAB CRAB VELA SS433 SS433 ANTARES (43° North) AMANDA/IceCube (South Pole) Mkn 421 Mkn 501 Mkn 501 RX J1713.7-39 GX339-4 Galactic Centre

  9. Background light under sea water …

  10. Bioluminescence and K40 desintegration g March 2006 – May 2008 g Cherenkov e- (b decay) 40K 40Ca Also used for in situ time calibrations (see Garabed Halladjian ’s talk)

  11. Atmospheric muons and neutrinos  µ p  p Expected atmospheric muons and neutrinos.

  12. Atmospheric muons Vertical muon intensity versus depth with data from Line 1. Line 1 - 2006 data

  13. Atmospheric muons Hit Elevation Hit Time Plenty circle: hit selected by the trigger. Empty square: hit used by the fit. Cross: hit saved in 2.2 ms around the event. A muon event with the 12-line detector

  14. A neutrino candidate

  15. Rate per day Reconstructed data per day compared to Montecarlo with the 5-line detector. 168 detected  during 139 days with the 5 lines

  16. ANTARES and physics

  17. What and why ? Dark matter Point sources e- M.M. Gamma-Ray Bursts Magnetic Monopoles ?

  18. The Gamma Ray Burst

  19. The Gamma Ray Burst (GRB) Count rate in unit of 1000 counts s-1 Total emitted energy: 1053 ergs Short pulses (1ms to 100 s) of g-rays (~ 1 MeV) BATSE Verydifferentsignals Burst duration 2 distinguishable classes But

  20. The Gamma Ray Burst (GRB) If time and position coïncidences g, n Very clear signal, with low background in ANTARES Short pulses (1ms to 100 s) of g-rays (~ 1 MeV). Should appeared with extreme conditions during violent and far astrophysics phenomenons (0.03 < z < 6.29). • Collapse of massive star and black hole formation surrounded by an accretion disk. • Binary systems. Burst duration , … 2 distinguishable classes

  21. The Gamma Ray Burst (GRB) alert location of GRB save The acquisition system All data detector 100111011 100111011 All data before, during and after GRB analysis

  22. The Gamma Ray Burst analysis Angular resolution ~ 2.6° Use of a specific trigger, of an improve reconstruction and of somecuts (Nhits, Totampl, qzen,…) Prompt GRB range Excellent signal over noise ratio remaining after analysis ~ 10. With an angular resolution ~ 2.6°. Analysis for the 5-line detector is ready.

  23. The point-like source search

  24. Point-like source search InHadronic modelsTeVnshould be produced in roughly equal numbers to TeVg-rays. VHE ray sources represent prime targets for neutrino telescopes. Sources coming from different catalogues (HESS, Magic, ...) • 50 Galactic sources among: • Pulsar Wind Nebulae (PWN) • Supernovae Remnants (SNRs) • g-Ray Binaries.... Galactic coordinates 69 sources selected in ANTARES field of view • 19 extragalactic sources : • Quasars, • ...

  25. Point-like source search 25 47 GoldenSources • Sources closer than the ANTARES angular resolution (0.3º above a few TeV) are considered as a single point-like source. • PWN are excluded because generally treated as leptonic emitters (exceptions for Crab & VelaX). Added selection criteria have been taken into account for the 5Line data analysis: Find correlations with those neutrinos 26 GoldenSources

  26. Point-like source sensitivity Point-like source analysis results for the 5-lines detector will arrive soon !

  27. The dark matter

  28. Dark matter search WIMP ANTARES  Sun • Accretion into the sun • Self-annihilation • En MWIMPs

  29. Dark matter search PRELIMINARY LKPs (Lightest KK Particles), non-baryonic and neutral particles corresponds to the first KK-resonance level of the hypercharge boson B(1) • Self annihilation channel( avec UED: B(1)) : B(1) B(1)ff, hh*,  , p, p, e+, e- , 

  30. The magnetic monopoles

  31. Magnetic monopole search Dirac in 1931 : e- M.M. the smallest magnetic charge, called the Dirac charge. t’Hooft and Polyakov in 1974 : Non perturbative solutions which looks like Dirac M.M. in non-abelian gauge theories. Généralisation Those solutions appear each time a compact and connected group is broken into a connected sub-group. Transition example with the minimal GUT group: MM with charge g=gD, not affected by the second transition. radius ~ 10-28 cm mass ~ 1016 GeV

  32. Magnetic monopole signal in sea water Direct Cherenkov emission  > 0.74 : Direct Cherenkov photons from a MM with g=gD. nsea water ~1.35 x 8500 Cherenkov photons from delta-rays. Number of photons emitted by a MM with the minimal charge gD, compared to a muon of same velocity : 8500 times more ! Cherenkov photons from a muon. Indirect Cherenkov emission  > 0.51 : The energy transferred to electrons is sufficiently important to pull out electrons (d-rays). These can emit Cherenkov light.

  33. Magnetic monopole search Expecting sensitivity with a C.L. of 90% for the 5-line detector after 127 days of data taking with some preselection cuts (not interesting for slow M.M. with b < 0.75). 127 PARKER MACRO PRELIMINARY AMANDA II 127

  34. A new project with an optical follow-up

  35. Neutrino detection with an optical follow-up Principle: Neutrinos are used this time as triggers for an optical telescope. Conditions: • 2 n from the same direction (< 3°) in 15 minutes. • 1 H.E. nwith the best reconstruction. Number of expected alert per month: 1 or 2. A collaboration with TAROT: Two 25 cm telescopes located at Calern (South France) and La Silla (Chile). 1h of optical data taking after the alert. Implementation of an online analysis program in progress. First alert very soon …

  36. Conclusion The detector isnowcomplete and isworkingverywell. • Resultsfromdifferentanalysis on the 5-line detector data will arrive verysoon. • Analysiswith the 10 and 12-line detector are in progress.

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