1. Status report on the Antares project Luciano Moscoso (DSM/DAPNIA, CEA/Saclay F-91191 Gif-sur-Yvette) (On behalf of the ANTARES collaboration) http://antares.in2p3.fr See also my poster exhibition

2. 16/08/2004L. Moscoso - ICHEP04 - Beijing 2 ANTARES collaboration IFIC Valencia CPPM Marseille DAPNIA, Saclay GRPHE, Mulhouse IReS, Strasbourg IFREMER,Toulon & Brest IGRAP, Marseille COM, Marseille ITEP Moscow Sheffield Leeds NIKHEF Amsterdam Genova Bari Catania Roma Erlangen LNS Pisa Bologna

3. 16/08/2004L. Moscoso - ICHEP04 - Beijing 3 Scientific aims of ANTARES Neutrinos from galactic sources – – Pulsars, Supernova Remnants – – Microquasars – – Intense activity in Galactic centre reported by TeV  -ray telescopes Neutrinos from extragalactic sources – – Active Galactic Nuclei – – Gamma Ray Bursts Dark Matter – – annihilation of neutralinos in the Sun or Galactic Centre. Magnetic Monopoles + oceanography, biology, seismology …

4. 16/08/2004L. Moscoso - ICHEP04 - Beijing 4 © 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

5. 16/08/2004L. Moscoso - ICHEP04 - Beijing 5 Sky View AMANDA South Pole 0.5  sr instantaneous common view 1.5  sr common view per day ANTARES 43 o North 2/3 of time: Galactic Centre

6. 16/08/2004L. Moscoso - ICHEP04 - Beijing 6 Water quality parameters light scattering : eff ~ 300 m (470 nm) eff ~ 100 m (370 nm) water transparency:  abs ~ 60  8 m (470 nm)  abs ~ 26  2 m (370 nm) counts time (ns)

7. 16/08/2004L. Moscoso - ICHEP04 - Beijing 7 Angular resolution for high energies:    < 0.2 o (Quality of water!) Good quality of sea water  Extremely powerful pointing Very competitive with other projects Only few % of event/year background for any point-like source  Simulated events, including: TTS due to electronics, scattering of light, light absorption and light background

8. 16/08/2004L. Moscoso - ICHEP04 - Beijing 8 Point-like sources sensitivity: fluxes Amanda has and Antares will reach the sensitivity to test the C. Distefano et al model.

9. 16/08/2004L. Moscoso - ICHEP04 - Beijing 9 Diffuse fluxes Neutrino oscillations  e :  :  = 1:1:1 Detectors are sensitive to HE cascades  sensitive to HE neutrinos of any flavour Estimates of the Antares sensitivity to cascades have started Energy estimate is compulsory for this study. Quantity of light  muon energy For Antares:  (Log E) = 0.3

10. 16/08/2004L. Moscoso - ICHEP04 - Beijing 10 Prototype Lines operated in 2003 Prototype Sector Line (PSL) Dec 2002 Mini Instrumentation Line (MIL) Feb 2003 Dec 2002 March 2003

11. 16/08/2004L. Moscoso - ICHEP04 - Beijing 11 Submarine cable connection March 2003

12. 16/08/2004L. Moscoso - ICHEP04 - Beijing 12 Monitoring of storey position and orientation data from July 2003 Example: heading

13. 16/08/2004L. Moscoso - ICHEP04 - Beijing 13 ) Examples for PMT rates (short time) 10min Rate (kHz) time rates due to : radioactive 40 K and bioluminescence

14. 16/08/2004L. Moscoso - ICHEP04 - Beijing 14 Long time rate variation (spring 2003) baseline rate: rate averaged during 15 min burst fraction: percentage of time with rate > 1.2 baserate correlation between burst fraction and sea current velocity observed baseline rate (kHz) burst fraction time (days) time April - May - June 2003

15. 16/08/2004L. Moscoso - ICHEP04 - Beijing 15 PSL & MIL operations 2003   Sea operations   Deployment   Connection   Recovery PSL Dec 02 Mar 03 Jul 03 MIL Feb 03 Mar 03 May 03 Junction box operates fine Very functional 130 Gb on disk The dark side… Mismatch O- ring/hole dimensions Water leak in 1 LCM Broken fiber in EMC Inappropriate protective tube used by manufacturer New connector New EMC  Line operations  Power distribution  Remote-control  Acquisition and digital transfer

16. 16/08/2004L. Moscoso - ICHEP04 - Beijing 16 Muon tracks Clock failure precluded an accurate time measurement compulsory for cosmic ray trajectory reconstruction. Nevertheless, cosmic ray reconstruction was already performed with our previous prototype in 2000 (cf A. Kouchner PhD thesis and L. Thompson, Neutrino2000, Sudbury). Therefore we focus our attention on the reliability of individual components. New analysis

17. 16/08/2004L. Moscoso - ICHEP04 - Beijing 17 Next steps: end 2004: re-deployment of prototype line deployment of improved instrumentation line 2005-2007: deployment of the full detector