1. The ANTARES Deep Sea Neutrino Telescope CRIS2010, 14th Sept 2010 CRIS2010, 14th Sept 2010 Paschal Coyle Centre de Physique des Particules de Marseille

2. SN oscillations dark matter SNR AGN/GRB Science with High Energy Neutrino Telescopes High energy neutrino astrophysics: galactic: SN, SNRs,  -quasars, molecular clouds, etc... extra-gal: AGNs, GRBs, dark-GRBs, GZK, etc.... Search for New Physics: Dark matter (Sun, GC), Monopoles, ?? Earth-Sea Science: oceanography, sea biology, seismology, environmental monitoring... ~MeVGeV-100 GeVGeV-TeVTeV-PeVPeV-EeV> EeV ? ?

3.  42° interaction Sea floor Cherenkov light from  3D PMT array  - Main detection channel:  interaction giving an ultra-relativistic  ( e and tau also) - Energy threshold ~ 10 GeV - 24hr operation, more than half sky coverage The reconstruction is based on local coincidences compatible with the Cherenkov light front Detection Principle  p    p, 

4. 4  CPPM, Marseille  DSM/IRFU/CEA, Saclay  APC, Paris  LPC, Clermont-Ferrand  IPHC (IReS), Strasbourg  Univ. de H.-A., Mulhouse  IFREMER, Toulon/Brest  C.O.M. Marseille  LAM, Marseille  GeoAzur Villefranche  University/INFN of Bari  University/INFN of Bologna  University/INFN of Catania  LNS – Catania  University/INFN of Pisa  University/INFN of Rome  University/INFN of Genova  IFIC, Valencia  UPV, Valencia  UPC, Barcelona  NIKHEF,  Amsterdam  Utrecht  KVI Groningen  NIOZ Texel  ITEP,Moscow  Moscow State Univ  University of Erlangen Bamberg Observatory Bamberg Observatory  ISS, Bucarest The ANTARES Collaboration 7 countries 29 institutes ~150 scientists+engineers

5. Region of Sky Observable by Neutrino Telescopes Mkn 501 Mkn 421 CRAB SS433 Mkn 501 RX J1713.7-39 GX339-4 SS433 CRAB VELA Galactic Centre AMANDA/IceCube (South Pole) (Ice: ~2°/0.6°) ANTARES/KM3 (43° North) (water: ~0.2°/0.1°)

6. V. Bertin - CPPM - ARENA'08 @ Roma Submarine cable The ANTARES Site & Infrastructure 40 km Site 20 km from nearest land Shore Station IFREMER Toulon Centre FOSELEV Marine Shipyard

7. V. Bertin - CPPM - ARENA'08 @ Roma 70 m 450 m JunctionBox Interlink cables 40 km to shore 2500m 900 PMTs 12 lines 25 storeys / line 3 PMTs / storey The ANTARES Detector

8. 2006 – 2008: Building phase of the Detector Line 1, 2: 2006 Line 3, 4, 5: 01 / 2007 Line 6, 7, 8, 9, 10: 12 / 2007 Line 11, 12: 05 / 2008 70 m

9. Detector Status after Completion 88% of modules operational at detector completion (May 2008) Line 6 and Line 9 recovered for maintenance ROV reconnection planned oct 2010

10. 2 min Continuous baseline: Radioactivity in the sea ( 40 K) + bioluminescent bacteria Bursts: bioluminescence from Macroscopic organisms Counting Rates (short timescale) 40 K

11. In situ calibration with Potassium-40 40 K 40 Ca  e - (  decay) Cherenkov Gaussian peak on coincidence plot Peak offset Precision (~5%) monitoring of OM efficiencies Cross check of time calibration Integral under peak

12. Time evolution of K40 coincidence rate All OM pairs of Line1 during more than 2 years OM gain drop reduces efficiency Recovery after threshold retuning Recovery due to HV off during period of cable repair

13. Optical Beacons: time calibration, absorption length ~70 m ~150 m

14. Acoustic Position Alignment r = (a z - b ln[1-cz] ) v 2 Z(m) r(m) Example for Sea current v= 25 cm/s r max = 22m Measure every 2 min: Distance line bases to 5 storeys/line and also storey headings and tilts

15. Line position measurements Acoustic positioning: Hydrophone positions from July  Dec 2007 Storey 1 Storey 8 Storey 14 Storey 20 Storey 25 Radial displacement Within a lineBetween lines Acoustic positioning: Precision ~ few cms

16. Track Reconstruction Online AlgorithmOffline Algorithm Storey rotation ignored -single points Line assumed vertical (no acoustic info) Immediately available non-optimal angular resolution Uses final alignment Loose selection Full likelihood fit Multiple starting points not immediately available excellent angular resolution 12 line detector

17. Expected Performance (full detector) Neutrino effective area N det =A eff × Time × Flux For E <10 PeV, A eff grows with energy due to the increase of the interaction cross section and the muon range. For E >10 PeV the Earth becomes opaque to neutrinos. Angular resolution For E <10 TeV, the angular resolution is dominated by the -  angle. For E >10 TeV, the resolution is limited by track reconstruction uncertainties. 

18. reconstructed up-going neutrino: detected in 6/12 detector lines: Event Displays reconstructed down-going muon: detected in all 12 detector lines:

19. Coincidences between adjacent storeys (low E muons) Energy threshold ~ 4 GeV (track length) Delay between storeys ΔtΔt Pedestal = random background (K40, bio) Integral under peak ~ event rate ~ muon flux Peak offset, width and shape = f (muon angular distribution, OM angular acceptance, …) µ

20. Event rate as function of floor depth By repeating the analysis for every detector storey the muon flux reduction with depth is directly measured Systematic errors mainly in normalization (+50/-35%), otherwise ~3% Published in Astrop. Phys 33 (2010) 86-90

21. Depth Intensity Relation from Zenith Distribution Zenith angle distribution of muon flux at 2000 m accepted for publication in Astroparticle Physics 11 july 2010, arXiv:1007.1777 2,5km 6km

22. Livetime:168 days 276 upward events (multi-line fit) 5-Line Data: Zenith Distribution down up horizontal p   p,  

23. Candidate List Search Search applied to 24 pre-selected sources 276 neutrino candidates

24. Candidate List Search Largest excess (4.1 events) at HESS J1023-575: post-trial prob=3.4% (1.8sigma, 1-sided) Nevents p-value (Pre-trial) 1.0 0.08235 1.6 0.00773 4.1 0.00142 0.0 0.5 0.172 0.0 1.6 0.04894 0.0 1.1 0.102 0.0

25. All Sky Search Most significant cluster 4.2 events decl =-9.5 degree, RA=222.15 degree This value or higher expected in 31% of toy Monte Carlo experiments 276 neutrino candidates

26. Coming Very Soon….2007+2008 data Live time: 295 days 2040 upgoing events + significantly better angular resolution Zenith distribution Scrambled skymap

27. Point Search Limits and Sensitivity 6 months of half detector already similar sensitivity to many years of MACRO, SK 2007-2008 data will give best sensitivity in Southern Sky 2009-2010 data in the pipeline Assumes E -2 flux spectrum

28. Diffuse Flux Search # of PMTs with prompt and late photons R= ---------------------------------------------------- # of all PMTs contributing to the event (See presentation of Simone Biagi- later today) <

29. Diffuse Flux Search

30. Transients with ANTARES Requires Satellite trigger (Swift, Fermi) Low backgrounds due to direction and time coincidences Full sky search (see all GRBs) 24hr/24hr Sliding time window around events Sensitive to dark bursts optical follow up to identify source  Fast online reconstruction Rolling searchTriggered search

31. GRB Neutrino Spectrum II. Or use of the Swift, Fermi LAT γ-ray spectrum:  p-γ interaction model  neutrino spectrum I. The so-called Waxman–Bahcall GRB flux, issued from average GRB parameters measured by BATSE to determine an all-sky neutrino flux from the GRB population. Guetta et al, Astropart. Phys. 20 (2004) 429 Waxman and Bahcall, PRL 78 (1997) 2292 20 GRB with measured redshift 37 GRB with no redshift z = 2 For all GRB in 2008: A special case, the GRB080916C

32. Opacity constraints  lower limit on the boost Lorentz factor (600-900)  sensitivity ~50 above the W&B fireball model (Г=600) analysis of the ANTARES data on- going (unblinding requested) Sensitivity of ANTARES to GRB080916C (LAT) Discovered by the Fermi-LAT (redshift z=4.35) One of the most powerful GRB (E iso ~8.8x10 54 ergs) Abdo et al, Science 323 (2009) 1688

33. Optical Follow-Up with TAROT FoV 1.86°x1.86° 10s pointing V<17 (10s) V<19 (100s) TAROT La Silla Doublets (15min, 3°*3°) or Singlet (high-energy) triggers

34. Dark Matter: Spin Dependent Earth       Sun WIMPs gravitational trapped via elastic collisions in the sun Antares “soft” annihilation : χχ -> bb M  = 1 TeV “hard” annihilation : χχ -> W+W- : neutrino : anti-neutrino M  = 1 TeV

35. Limits from 5-line data

36. Extremely high energy deposition Direct Cherenkov light for  > 0.74 light from δ-rays for  > 0.51 Dedicated reconstruction (  free) likelihood ratio  free to  =1 Expected Sensitivity using 2008 data AMANDA II 137 days M.M. with  0.65 MAGNETIC MONOPOLES

37. Summary  ANTARES infrastructure completed since May 29th 2008 Detector operation and calibration understood Maintenance capability demonstrated  Exciting physics program ahead  many thousands of neutrinos already reconstructed  Unexplored regions of sensitivity in southern hemisphere  astronomical sources, dark matter, oscilllations, ……  Multi-messenger approach strongly pursued  Real-time readout and in-situ power capabilities facilitates a large program of synergetic multi-disciplinary activities: acoustics, biology, oceanography, seismology……  Major step towards the KM3NeT multi-disciplinary deep-sea research infrastructure (Piera Sapienza talk)

38. The KM3NeT Challenge 12 lines, 900 PMTs ~250 lines, ~30000 PMTs –Maximise physics potential Substantial improvement over ICECUBE Instrumented volume ~5 km3 Angular resolution ~0.1 degrees (E>10 TeV) –Build in a reasonable time  4 years New deployment techniques Speed-up integration time Sub contract part of the production … –At a reduced cost Factor 2 reduction cf ANTARES Simplified architecture Reduced maintenance Multi-line deployments … (See presentation Piera Sapienza later today)

39. Sensitive to Cosmic Ray Composition Preliminary

40. Transient Sources GRB neutrinos: Relatvistic Jets (Fireball Modèl) Meszaros & Rees, Waxman SN neutrinos: mildy relativistic choked jet, no prompt optical counter-part Razzaque & al,, Ando & Beacom