1. The ANTARES Project Sino-French workshop on the Dark Universe Stephanie Escoffier Centre de Physique des Particules de Marseille On behalf of the ANTARES collaboration Marseille, September 19-23, 2005

2. Sino-French workshop on the Dark Universe Neutrino Astronomy Galactic and Extra-galactic Point Sources of High Energy Neutrinos Pulsar Young Super Nova Remnants Microquasar Galactic Centre (visibilty 67% of the day) Active Galactic Nuclei Gamma Ray Bursts Neutralino annihilations in the Sun, in the Earth, in the Galactic Center  Dark Matter searches

3. Sino-French workshop on the Dark Universe Site Location: La Seyne sur Mer Water Properties transparency:  abs ~ 60  8 m (blue)  abs ~ 26  2 m (UV) light scattering : eff ~ 300 m (blue) eff ~ 100 m (UV) For  > 90º the loss in transmission is < 1.5% in 1 year. Biofouling  = 0°  = 90° 42º50’N, 6º10’E

4. Sino-French workshop on the Dark Universe   43° 2500 m depth Cherenkov light from  induced by interaction detected by 3D PMT array Time & position of hits allow the reconstruction of the  (~ ) trajectory interaction Neutrino detection

5. Sino-French workshop on the Dark Universe Expected Angular Resolution Dominated by reconstruction Dominated by kinematic angle   Reconstruction resolution limited only by phototube TTS and light diffusion in water true  rec  Simulated events, including: TTS scattering of light light absorption light background

6. Sino-French workshop on the Dark Universe Point-like sources: expected sensitivity After 1 year, Antares can improve limit for Southern hemisphere… or discover something ! 90% c.l. Muon flux limits (cm -2 s -1 ) Declination (degrees) AMANDA B-10 130 days E >10 GeV, angular resolution ~ 3.9 deg (2003). MACRO 1388 events in ~6 y > 1.5 GeV, angular resolution ~ 0.5 deg SK 2369 upward-going stopping and through-going muons in 4.6 y, > 3 GeV, angular resolution of about 2° (ICRC 2003). AMANDA II sensitivity 197 days (2004) southern skynorthern sky ANTARES sensitivity 1 yr E -2 neutrino spectrum AMANDA II

7. Sino-French workshop on the Dark Universe Detector Geometry 70 m 12 lines (900 PMTs) 25 storeys / line 3 PMTs/storey 350 m 100 m 14.5 m Junction box Readout cables 40 km to shore 2500 m storey Horizontal layout

8. Sino-French workshop on the Dark Universe Hydrophone RX Cage (magnetic shield) Local Control Module Optical Beacons for timing calibration (blue LEDs) Line storey elements 10” PMT in the glass sphere

9. Sino-French workshop on the Dark Universe The excellent angular resolution of ANTARES relies on the global timing resolution and on an accurate knowledge in real time of the OMs positions In-situ calibration systems: – Clock calibration system – LEDs in Optical Modules – Optical Beacons – Laser Beacons Strings Light sources Light shells Optical modules Timing calibration goals of ANTARES: ~1 ms in absolute timing (internal clock w.r.t. UTC) ≤ 0.5 ns in relative timing (between OMs) ANTARES Time Calibration System

10. Sino-French workshop on the Dark Universe  test of deployment and mechanical structure of a full line (23 storeys)  equipped with water leak sensors and instruments for attenuation measurements Recovery showed: no water leaks in electronic containers optical transmission losses due to an interface problem between EMC penetrators and the LCM cylinder  solution proposed, under validation 2005: Line O

11. Sino-French workshop on the Dark Universe 2005: the MILOM Led Beacon Laser Beacon 50 m 14.5 m 100 m 1 OM 3 OMs ADCP Sound Velocimeter CT (Conductivity Temperature) CSTAR (Light Transmission meter) Acoustic Positioning Module (Rx) Acoustic Positioning Module (RxTx) Buoy Acoustic positioning system  Receiver at 1 storey  Transceiver (transmitter + receiver) at anchor Instrumentation components  current profiler (ADCP)  sound velocimeter  water properties (CSTAR, CT) Optical components  Equipped with final electronics  3 + 1 optical modules at two storeys Time calibration system  Two LED beacons at two storeys  Laser Beacon attached to anchor Deployed in March, connected in April, still taking data

12. Sino-French workshop on the Dark Universe MILOM Clock Calibration Slope due to an increase of the average temperature in the on-shore cable ~1 ns JB MEOC 4o km

13. Sino-French workshop on the Dark Universe Optical Beacons Calibration Time difference between signals between 2 OMs in a storey Time difference between the OMs and the internal PMT of the LED beacon (low TTS) 14.5 m Mean of the distribution of time difference of hits on 2 adjacent OMs  stability of calibrations

14. Sino-French workshop on the Dark Universe Resolution of ~3 cm on a distance measurement of ~84 m Acoustic Positioning System ANTARES required precision on 3D position of the OMs is ~10 cm. Sound velocimeter

15. Sino-French workshop on the Dark Universe Measurement of the water current profile using the Doppler effect V average =.093 m s -1 Preferred directions: ~ West  East

16. Sino-French workshop on the Dark Universe Measurement of water temperature JB

17. Sino-French workshop on the Dark Universe Baseline and Burst Fraction The burst fraction is the time ratio during which the counting rate exceeds the baseline by more than 20%

18. Sino-French workshop on the Dark Universe Conclusions The MILOM has been a big step forward in understanding the behaviour of all the ANTARES devices. Timing calibration systems have been successfully tested in the sea. Line 1 construction has started and is expected to be running in January 2006. The full 12-string detector operation can be expected in 2007.

19. Sino-French workshop on the Dark Universe 2003 Prototype Lines Prototype Sector Line (PSL) Dec 2002 Junction Box Dec 2002 Cables linked by IFREMER Nautile March 2003 Mini Instrumentation Line (MIL) Feb 2003 Acoustic Doppler Sea Current Profiler 5 storeys of optical modules GENISEA sound velocimeter Conductivity- Temperature-Depth sensors Hydrophone Rx/Tx hydrophones seismograph Laser beacon Anchor with String Control Module LED beacon Faulty fiber carrying Master clock signal. No synchro between storeys

20. Sino-French workshop on the Dark Universe Internal LED Calibration Sample timing LED distribution from two different OM internal LEDs By firing the LED system with the clock, the PMT transit time can be measured and monitored LED