1. CEA DSM Irfu The ANTARES Neutrino Telescope A status report Niccolò Cottini on behalf of the ANTARES Collaboration 44 th Rencontres de Moriond February 2009

2. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini2 The ANTARES Collaboration Since 1996 7 countries 22 laboratories 200 physicists, engineers, sea scientists

3. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini3 Outline of the talk Neutrino astronomy –The potential sources The ANTARES detector –Construction milestones Detector operations –The data taking campaign The first physics analyses –Atmospheric muons –Atmospheric neutrinos –Search for cosmic neutrino sources –Indirect dark matter detection

4. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini4 The Neutrino Astronomy

5. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini5 Neutrino astronomy p  Galaxy Local galaxy group   p/A + p/     +  0  +      e e  : interact with CMB and matter Protons: deflection by magnetic fields : weakly interacting –huge target needed (100Mton - Gton)

6. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini6 Potential sources GALACTIC Supernova remnants Pulsars Microquasars EXTRAGALACTIC GRBs AGNs Indirect dark matter search See Damien Dornic’s talk See Vincent Bertin’s talk

7. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini7 Detection principle  43° interaction Sea floor Cherenkov light from  3D PMT array  Main detection channel: charged  interaction giving an ultrarelativistic  Energy threshold: 10 GeV ANTARES 12 lines MC

8. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini8 The ANTARES detector

9. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini9 The ANTARES site 42°50’ latitude Nord 6°10’ longitude Est Galactic Center –visible 75% of the day Galactic coordinates

10. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini10 Toulon La Seyne Submarine cable (~40km) Shore Station The ANTARES site

11. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini11 The ANTARES detector ~60 m 100 m 350 m 14.5 m Link cable Junction Box Cable to shore 2500m depth

12. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini12 The ANTARES detector Storey 45°

13. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini13 Hydrophone 17’’ glass sphere 10’’ PMT A detector storey DAQ Slow Control Titanium frame LED Beacon ~10 cm resolution ~0.6 ns resolution

14. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini14 2006 – 2008: deployments of the detector lines Line 1: 03 / 2006 Line 2, 3, 4, 5: 01 / 2007 Line 6, 7, 8, 9, 10: 12 / 2007 Line 11, 12: 05 / 2008 ~60 m

15. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini15 Detector layout See Kay Graf’s talk Acoustic storey … and several instruments for environment studies with the ANTARES infrastructure

16. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini16 Detector operations

17. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini17 The detected signal Muon (Cherenkov) –2 µs crossing time 40 K decay –Continuous background  30 kHz * Bioluminescence –Continuous background  30 kHz * –Occasional bursts ~MHz Simulation 2 min * 10’’ PMT, 0.3 p.e. threshold 792 days

18. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini18 The Trigger Front end chip digitizes charge and time of a light signal All data transmitted through multiplexed Gigabit links –the whole data flow can not be written to disk Computer farm running a software trigger: –look in all directions for light signals compatible with a muon track –when found, write a Physics Event Other triggers exist: cluster of storeys, GRBs, Galactic Center, …  “ALL DATA TO SHORE” SCHEME:

19. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini19 Track reconstruction  =35 o

20. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini20 Number of triggers 10 or more lines (2008)5 lines (2007) Data taking ongoing… …accumulating neutrinos

21. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini21 The first physics analyses

22. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini22 atmospheric  atmospheric  Atmosphere Sea Earth cosmic 

23. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini23 Muon flux at the detector Atmosphere Earth Sea 10 7 atmospheric  per year* 10 3 atmospheric per year* cosmic  Line 1: 03 / 2006 Line 2, 3, 4, 5: 01 / 2007 Line 6, 7, 8, 9, 10: 12 / 2007 Line 11, 12: 05 / 2008 Performance paper submitted First physics analyses completed Ongoing analysis Data taking * Reconstructed tracks in 12 line detector

24. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini24 Atmospheric muon studies with 5 lines Systematic uncertainty ± 30% Main contributions –optical module response –absorption length of the light in water See Claire Picq’s talk data CORSIKA (QGSJET01) + NSU model MC uncert.

25. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini25 Selection of neutrino events with 5 lines Upgoing events dominated by the tail of badly reconstructed atmospheric muons Upgoing eventsDowngoing events Data,  MC, MC (x100) Likelihood ratio  : maximum likelihood of the track fit MC

26. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini26 Data,  MC, MC (x100) Selection of neutrino events with 5 lines Purity = ~90%; Efficiency = ~30% y = s(x) / [ s(x) + b(x) ] 

27. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini27 Detection of atmospheric neutrinos with 5 lines Data : 185 (1,1 / j), 93% purity ANTARES 5 lines (164 days live time) MC : Test of detector response to a known neutrino signal A preliminary step before searching for cosmic sources Bartol flux (20% uncertainty on the absolute  flux) Mainly optical module response and calibration uncertainties (preliminary) Data MC Uncertainties

28. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini28 Search for point like neutrino sources with 5 lines See Katia Fratini’s talk No discovery 90% CL flux limit Definition of a potential source list Analysis optimization by MC, for E -2 flux Data unblinding: 94 neutrino events

29. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini29 Preliminary analysis of 10 line data 208 neutrinos Preliminary quality cuts Dec 2007 – Apr 2008 : 100 days live time

30. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini30 A neutrino event on 12 lines

31. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini31 Conclusion ANTARES today –Successful end of construction phase Technology proven Data taking ongoing –First physics outputs Atmospheric  and, cosmic neutrino sources, dark matter Neutrino oscillations, magnetic monopoles, VHE neutrino interactions, … On the road for the next step –KM3Net… KM3 See Christopher Naumann’s talk

32. CEA DSM Irfu 05 / 02 / 2009Niccolò Cottini32 Vue de la salle de contrôle d’ANTARES A view from ANTARES control room