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The ANTARES N eutrino Telescope and its Dark Matter Capabilities

The ANTARES N eutrino Telescope and its Dark Matter Capabilities. Jürgen Hößl, Universität Erlangen, on behalf of the ANTARES Collaboration. Edinburgh, Septemb er 200 4. ANTARES NeutrinoTelescope. buoy. 350 m. 12 lines 25 storeys / line 3 PMTs / storey. 40 km to shore. 100 m.

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The ANTARES N eutrino Telescope and its Dark Matter Capabilities

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  1. The ANTARES Neutrino Telescope and its Dark Matter Capabilities Jürgen Hößl,Universität Erlangen,on behalf of theANTARES Collaboration Edinburgh, September 2004

  2. ANTARES NeutrinoTelescope buoy 350 m • 12 lines • 25 storeys / line • 3 PMTs / storey 40 km to shore 100 m Junction box muon 65 – 70 m

  3. ANTARES Site -2500m Submarine Cable La Seyne sur Mer Institut Michel Pacha Shore Station

  4. Sky Coverage ANTARES 43o North 2/3 of time: Galactic Centre AMANDA South Pole 0.5 p sr instantaneous common view 1.5 p sr common view per day

  5. Angular Resolution m n n m for high energies: sq < 0.2o (Quality of water!)

  6. ANTARESCollaboration Erlangen NIKHEF Amsterdam ITEP Moscow Sheffield Leeds IFREMER, Brest DAPNIA, Saclay IReS, Strasbourg Mulhouse CPPM Marseille IFREMER,Toulon COM, Marseille OCA, Nice Genova Bologna Bari Pisa IFIC Valencia Roma Catania LNS

  7. Scientific Programme Neutralino search Annihilation at centre of Earth, Sun, Galaxy cc  n .... Search for galactic/extragalactic n sources SN remnants, Galactic microquasars AGN, GRB, … + oceanography, biology, seismology

  8. Cosmic Particle Accelerators Gamma Ray Bursts Supernova Remnants Pulsars, Plerions Active Galactic Nuclei (Quasars, Blazars) Microquasars

  9. Dark Matter Microwave background Gravitational lenses Rotation of galaxies

  10. c c c c c c c c c c c c c c c c c c c c c c c c c Wm m c c+ c Wm m Search for Neutralino Annihilation Gravitational capture of c in Earth, Sun, Galactic Centre WIMP loses energy by elastic interaction if v< vescape =>capture capture + annihilation balance => constant density in core Annihilation: bcm m + + c - ~ b bcm m - - c + soft spectrum hard spectrum ( if Mc<MW)

  11. Dark Matter Sensitivity search cone around source (depends on Neutralino mass) number of atmos- pheric background events 90 % upper limit on signal events mSUGRA parameter scan comparison muon/neutrino flux prediction muon /neutrino flux limit

  12. WIMP Annihilation in Sun

  13. WIMP Annihilation at Centre of the Earth • - mass of Earth << mass of Sun • possibly dramatic reduction of capture rate in Earth due to • depletion of neutralino density by solar capture Large uncertainties (J.Lundberg and J.Edsjö, astro-ph/0401113) only small capture rate in the Earth annihilation rate and neutrino flux from Earth smaller than from Sun for ANTARES: search from Earth not competitive with search from Sun

  14. WIMP Annihilation at Galactic Centre (GC) • possibility to probe DM profile in Galactic Centre (contrary to direct searches) • - uncertainties about DM profile: • standard parametrisations give low neutrino fluxes from GC • (e.g. Navarro, Frenk and White, Astrophys. J. 462(1996) 563 ) from G. Bertone et al. astro-ph/0403322

  15. WIMP Annihilation at Galactic Centre (GC) but: possible enhancement of annihilation flux by orders of magnitude in the presence of a black hole (spike) (e.g. P. Gondolo and J. Silk, Phys. Rev. Lett. 83(1999)1719 ) EGRET g signal neutrino flux: from G. Bertone et al. astro-ph/0403322 orders of magnitude flux uncertainties!

  16. Prototype Sector Line Dec 2002 Mini Instrumentation Line Feb 2003 to shore Oct 2001 Dec 2002 100m 12m LED beacon 100m 100m LASER Beacon Status ANTARES

  17. Prototype Sector Line: Nov 2002

  18. PSL & MIL Operation in 2003 • Sea operations: - deployment/connections/recovery • without problems • Line operations: - power distribution • - data transfer to shore (130 GByte) • - remote control • without problems • minor problems: • - distribution of the onshore synchronised clock signal failed due • to broken fibre: manufacturer used inappropriate cable • water leakage in Mini Instrumentation Line after 2 months under • high pressure: mismatch of o-ring/hole size Lot of data during 3 months of operation

  19. Optical Background Less than 1% burst fraction 10% burst fraction bursts baseline 10min 10min 40 K + bioluminescence

  20. Long Term Background

  21. ANTARES Summary and Future _________________ 2002 2003 2004 2005 2006 2007 Operation of Sector Line Deployment of lines 1 to 12 and operation Mini Instrumentation Line with Optical Modules: deployment and operation Sector Line connection in 2007 12 string detector complete Mini Instrumentation Line deployment Sector Line deployment Junction box deployment

  22. The End

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