1. Stéphanie ESCOFFIER CPPM Marseille, France on behalf of the ANTARES Collaboration research goals detector setup selected results summary

2. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm2 Neutrino astronomy Cosmic sources of neutrinos micro quasars: X-ray binaries supernova remnants and shock acceleration Active Galactic Nuclei Gamma Ray Bursts Intriguing science questions: astrophysical acceleration mechanism ? origin of cosmic rays ? dark matter ? other exotic physics (magnetic monopoles) ?

3. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm3 The ANTARES Collaboration  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 IFIC, Valencia UPV, Valencia UPC, Barcelona  NIKHEF (Amsterdam)  KVI (Groningen)  NIOZ Texel  University of Erlangen  Bamberg Observatory ISS, Bucarest  ITEP, Moscow  Moscow State Univ 7 COUNTRIES 28 INSTITUTES ~ 150 SCIENTISTS AND ENGINEERS  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

4. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm4 The ANTARES detector ~60 m 350 m 14.5 m Submarine links Junction Box 40 km to shore Buoy Storey Completed in May 2008 12 lines of 75 PMTs 25 storeys / line 3 PMTs / storey ~900 PMTs

5. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm5 Optical background constant 40 K (~40 kHz) The background 2 min PMT counting rates 40 K 40 Ca e-e- Cherenkov light beta decay 40 K is used to check the time calibration of the detector bioluminescence of micro-organisms bursts from macro-organisms (Particle) Physics background cosmic rays (atmospheric μ and ν)

6. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm6 Optical background constant 40 K (~40 kHz) bioluminescence of micro-organisms bursts from macro-organisms The background 2 min PMT counting rates strongly correlated to sea currents (Particle) Physics background cosmic rays (atmospheric μ and ν)

7. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm7 Optical background constant 40 K (~40 kHz) The background 2 min PMT counting rates bioluminescence of micro-organisms bursts from macro-organisms special event in 2006: ANTARES Coll., Deep-Sea Res. I 58 (2011) 875. (Particle) Physics background cosmic rays (atmospheric μ and ν)

8. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm8 The online/precise tracking Online tracking fast, to discriminate atmospheric muons from neutrinos No detailed calibration/ no real time detector positioning needed Angular resolution: Δθ  3 o The precise tracking detailed real-time positioning of the detector detailed PMTs charge/time calibration detailed systematic knowledge of the apparatus (OMs angular acceptance, etc.) Angular resolution: up to Δθ  0.2 o arXiv 0908.0816 Astropart.Phys. 34 (2011) 652

9. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm9 Event display: a neutrino candidate Example of a reconstructed up-going muon (i.e. a neutrino candidate) detected in 6/12 detector lines: time height online tracking

10. atmospheric muon flux atmospheric neutrinos point sources  see talk by Juan Pablo Gomez diffuse ν μ flux magnetic monopoles dark matter  see talk by Juande Zornoza

11. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm11 Atmospheric muons online tracking Zenith angle distribution of reconstructed tracks from atmospheric muons with a 5 line detector. Astropart.Phys. 34 (2010) 179.  Within systematic uncertainties the measurements cannot distinguish between the models considered systematic error due to +/- 10% on absorption length = +25%/-20%; syst. err. due to -15% on PMT efficiency (QE, eff. area etc) = -15%; syst. err. due to cutoff in angular accept. = +20%/-15%; total systematic uncertainty +/- 30%. Systematic uncertainties: +30% primary flux; +25% hadronic interaction model Data MC (corsika + qgsjet) Systematics on MC corsika + qgsjet (poly) corsika + sibyll mupage

12. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm12 Muon depth-intensity relation Astropart.Phys. 34 (2010) 179.  Results are in agreement, within the systematic uncertainties, with the theoretical predictions and previous measurements 2,5km 6km

13. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm13 Atmospheric neutrinos 341 days detector live time, single- and multi-line fit elevation angle  up-going good agreement with Monte Carlo atmospheric neutrinos: 916 (30% syst. error) atmospheric muons: 40 (50% syst. error) 1062  cand. down-going 1062 neutrino candidates:  3.1 candidates/day online tracking data set: 2007-2008 data taken with 5 lines (2007) and 9, 10, and 12 lines (2008)

14. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm14 Search for point-like sources Well reconstructed Badly reconstructed uncertainties in angle reconstruction: median: 0.5  0.1 O 12-line data: 0.4  0.1 O absolute orientation:  0.1 O data set: 2007-2008 data taken with 5 lines (2007) and 9, 10, and 12 lines (2008) precise tracking arXiv:1108.0292v1 [astro-ph.HE]

15. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm15 H. Löhner, High Energy Neutrino Flux 15 Search for point-like sources Equatorial coordinates Two distinct approaches: all sky search list of candidates 24 source candidates point-like sources search  see J. Gomez’s talk arXiv:1108.0292v1 [astro-ph.HE]

16. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm16 Search for diffuse ν μ flux  no excess of high-energy events above expected flux from atmospheric background from atmospheric : ~ E -3.5 + prompt neutrinos cosmic neutrino models: ~ E -2  search for high-energy diffuse-flux tail Phys. Lett. B 696 (2011) 16. Energy estimate R based on extra light from delayed OM hits due to high-energy EM showers

17. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm17 Diffuse flux: upper limits Upper limit is E 2  (E) 90% = 4.8×10 -8 GeV cm -2 s -1 sr - 1 for 20 TeV<E<2.5 PeV Phys. Lett. B 696 (2011) 16. (334 days of equivalent live time)

18. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm18 Search for magnetic monopoles Magnetic monopoles emit 8500 more Cherenkov light than a muon  can be detected by ANTARES Two estimators to discriminate MM from atmospheric background The number of hits estimates the quantity of light The ratio of two tracking reconstruction, where χ 2 β=1 standard muon algorithm (β =1) χ 2 β modified algorithm (β free) λ=log( χ 2 β=1 /χ 2 β ) Selection optimized for the discovery potential (in a blind way)

19. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm19 Monopoles: upper limits  no excess of events above the expected atmospheric background flux Upper limit is  (E) 90% = 1.3×10 -17 cm -2 s -1 sr -1 at β≈1 (116 days of equivalent live time with 2008 data)

20. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm20 Multimessenger astronomy GCN GRB Coord. Network: γ satellites SNEWS SuperNova Early Warning System Ligo/Virgo Gravitational waves: trigger + dedicated analysis chain TaToO optical follow up Strategy higher discovery potential by observing different probes higher significance by coincidence detection higher efficiency by relaxed cuts

21. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm21 TAToO project TAToO Optical follow-up of neutrino alerts from ANTARES in order to search for and identify transient sources (GRB, AGN flares…) ν ANTARES Reconstruction “on-line” (<10ms) Trigger: multiplet / HE singlet Alert neutrino (GCN) Real time send <10s 1.9° x 1.9° Large sky coverage (>2π sr) + high duty cycle Improved sensitivity (1 neutrino may lead to a discovery !!!) No hypothesis on the nature of the source Non dependent on the availability of external triggers Advantages: Tarot and ROTSE

22. S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm22 Future plans: KM3NeT concept array of multi-PMT optical modules (OM) sensing Cherenkov light instrumented volume several km 3 sensitive to all  flavours E > 0.1 GeV angular resolution min 0.1 o for E > 10 TeV acceptance: up-going tracks, up to 10 o above horizon 

23. ANTARES completed since May 2008 complements the sky coverage of IceCube has a broad physics program new diffuse-flux limit competitive new magnetic monopoles flux limit multi-messenger observations on alert paves the way for KM3NeT