1. Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005

2. 13/03/2005JP Ernenwein - Rencontres de Moriond2 ANTARES collaboration IFIC Valencia IFREMER,Toulon & Brest DAPNIA, Saclay IReS, Strasbourg GRPHE, Mulhouse CPPM Marseille IGRAP, Marseille COM, Marseille ITEP Moscow NIKHEF Amsterdam Genova Bari Catania Roma Erlangen LNS Pisa Bologna

3. 13/03/2005JP Ernenwein - Rencontres de Moriond3 The messenger of ANTARES  : absorbed (interaction with C.B.) p : magn. field + GZK effect –Weakly interacting  Source exploration on cosmological distances –Access to the heart of sources –Weakly interacting  large detection volume required Neutrino :

4. 13/03/2005JP Ernenwein - Rencontres de Moriond4 (Potential) Sources of Neutrinos for ANTARES GALACTIC SOURCES Dark Matter : annihilation of neutralinos inside massive objects (Sun, Earth, Galactic Center) EXTRA GALACTIC SOURCES Active Galactic Nuclei M 87, HST SN 1987A, HST Supernova remnants, Gamma Ray Bursts Micro Quasars, Pulsars, Crab Nebula Galactic Center,

5. 13/03/2005JP Ernenwein - Rencontres de Moriond5 (Potential) Sources of Neutrinos for ANTARES X ray OpticalRADIO e   (Compton, Synchrotron) M 87 p/A + p/              e e Hadronic interactions 

6. 13/03/2005JP Ernenwein - Rencontres de Moriond6 ANTARES detection principle Neutrino detection principle   43° 2500 m depth p    p,   interaction Cherenkov light from  3D PMT array Measurement : Time & position of hits  (~ ) trajectory

7. 13/03/2005JP Ernenwein - Rencontres de Moriond7 © F. Montanet 12 lines 25 storeys / line 3 PMTs / storey 900 PMTs ~70 m 100 m 350 m 14.5 m Submarine links Junction Box 40 km to shore Anchor/line socket to be deployed by 2005-2007 a storey 2500m depth

8. 13/03/2005JP Ernenwein - Rencontres de Moriond8 Detector design Optical Beaconstiming calibration with blue LEDs Vacuum valve Photomultiplier Magnetic Shield Optical gel LED Glass Sphere Base (electronics) penetrator Optical Module : 10’’ PMT + time calibration LED. STOREY Local Control Module (Ti cylinder) Housing of electronics (PMT, compass, acoustics …) Inner rack Ti tube penetrator

9. 13/03/2005JP Ernenwein - Rencontres de Moriond9 Off the coast of Toulon (France) in mediterranean Sea (42º50’N, 6º10’E), at 2500 m depth. ANTARES location and sky view 0.5  sr instantaneous common view IceCube, AMANDA (South Pole) 2  sr 2/3 time see Galactic Center ANTARES (42.5 o N) 3.5  sr

10. 13/03/2005JP Ernenwein - Rencontres de Moriond10  kinematics reconstruction ANTARES angular resolution E µ >10 TeV Electronics simulation + light absorption & scattering + light background ( 40 K + bacteria bioluminescence ~ 60 kHz) : Angular resolution < 0.2° abs ~ 26/60 m @ 370/470 nm eff ( scattering )~ 100/300 m @ 370/470 nm WATER on A NTARES site

11. 13/03/2005JP Ernenwein - Rencontres de Moriond11 10 GeV < E  < 100 GeV : method = muon path E  >1 TeV : method = quantity of light  E estimated by a factor 2-3 ANTARES Energy resolution

12. 13/03/2005JP Ernenwein - Rencontres de Moriond12 ANTARES Effective Areas A eff = surface of a perfect detector (100% efficiency) A eff for Neutrinos : absorption in earth is accounted for computations

13. 13/03/2005JP Ernenwein - Rencontres de Moriond13 Performances :Diffuse Fluxes Neutrino oscillations  e :  :  = 1:1:1 Detectors sensitive to HE cascades  sensitive to HE of any flavour ANTARES HE cascade sensitvity estimate in progress not yet included in limits

14. 13/03/2005JP Ernenwein - Rencontres de Moriond14 Point-like sources sensitivity Test of Micro Quasar C. Distefano et al model : Amanda has the required sensitivity. Antares will reach this sensitivity. MACRO

15. 13/03/2005JP Ernenwein - Rencontres de Moriond15 10min Rate (kHz) time Prototype Sector Line 5 storeys Junction box Connected in March 2003 40 K + bacteria burst correlation between burst fraction and sea current velocity observed Sea operation OK Remote control OK Water leak in 1 LCM Broken fiber in EMC

16. 13/03/2005JP Ernenwein - Rencontres de Moriond16 Submarine cable connection March 2003

17. 13/03/2005JP Ernenwein - Rencontres de Moriond17 light transmissiometer water current profiler Conductivity- Temperature probe Year 2005 : Line 0, MILOM Line 0 : 23 storeys with spheres but without PMTs inside purpose : test of new version of EMC cable & test of LCMs penetrators (failures in PSL) MILOM Mini Instrumented Line with Optical Modules 4 PMTs & positionning devices & calibration devices Connection : april 2005

18. 13/03/2005JP Ernenwein - Rencontres de Moriond18 Next Steps : Line 1... Line 1 is currently at the integration step Line 1 will be deployed and connected in autumn 2005 The 11 next lines will be deployed and connected during year 2006 / beginning of 2007 Line 0 : validation of the new EMC cable