1. Antares/KM3NeT M. de Jong

2. neutrinos  p Scientific motivation: – origin cosmic rays – birth & composition relativistic jets – mechanism of cosmic particle acceleration – dark matter neutrino telescope Why neutrinos: – no absorption – no bending – ‘remote microscope’ Neutrino astronomy 10,000 sparser than Super-K

3. Antares Operation and physics analyses

4. Detector operation date online neutrino count complete direction information zenith angle only main cable repair twelve lines operational! detector construction completed

5. Neutrino detection  cos  number of events Antares: angular resolution 0.5±0.1 degrees upward going muonsgood quality events neutrinos data Monte Carlo total Monte Carlo neutrino Monte Carlo muon

6. Neutrino sky map (2007‒2008) 2° Limits on neutrino fluxes, world’s best for some specific sources. part of sky invisible to Antares PSF

7. Nikhef analyses in Antares  Point source search, A. Heijboer et al. – 1 st point source search to be published soon  Antares‒Auger correlation, J. Petrovic et al. – approved unblinding of data (December 2010)  GRB: muon neutrino, M. Bouwhuis et al. – approved unblinding of data (January 2011)  GRB: electron neutrino, C. Reed & E. Presani – approved unblinding of part of data (January 2011 ) Nikhef is leading analysis efforts

8. KM3NeT convergence on the design ¶ ¶ unanimous decision of the institute board, d.d. 25 January 2011

9. 31 x 3” PMT ETeL, Hamamatsu,... concentrator ring increase of photocathode area by 20‒40% Optical module

10. 6 m Mechanical cable connection Data cable storage Mechanical cable storage Frame Optical module Mechanical holder Needs new deployment technique Storey 1Digital Optical Module=Dom 2Dom’s on 1 bar=Dom-bar 20Dom-bar’s on 1 tower=Dom tower

12. NIOZ operations  1 st deployment test SeaWiet line December 2010  new set of deployment tests last & this week  deployment & unfurling successful, but some problems with detachment of launcher  data from 2 autonomous lines with 3” PMTs will become available next week after 1 year of operation

13. Atmospheric muon rates 5 10 152025303540 10 -2 10 -1 1 number of Lx Rate [kHz] L0 L1 L2 70% of L0s contribute to L1s

14. Effective area E [GeV] A [m 2 ] ratio TeV PeV Antares abs bar 0 m standard SeaWiet

15. Angular resolution angle [degrees] probability E -2 muon E -2 neutrino Antares abs bar 0 m standard SeaWiet

16. Sensitivity E 2  [GeV cm -2 s -1 ] ratio sin(  )

17.  t [ns] R = 10m R = 20m R = 30m R = 40m R = 50m Sky map of event PDFs Event reconstruction 4D-PDF cos   +1 0 0 22  2D-PSF

18. comparison with IceCube 3  limit sin  Galactic centre 5  discovery E 2  [GeV -1 cm -2 s -1 ] IceCube KM3NeT

19. Nikhef contributions to KM3NeT  Technical design ‒multi-PMT optical module ‒data acquisition system design “All-data-to-shore” has become a standard fibre-optics network & transceivers online data filter – HV PMT-base, vertical electro/fibre-optics cable, power system,... – deployment procedures (NIOZ)  Science ‒Monte Carlo simulation tools ‒Event reconstruction & physics analyses Nikhef is a main contributor

20. Summary & outlook  Antares ‒taking data routinely (24h/day) ‒superior angular resolution compared to ice ‒new MoU in preparation (5 years)  KM3NeT ‒established technical convergence ‒cost estimates remain stable (200‒250 M€) ‒new ways in event reconstruction explored ‒deployment prototype model before end 2011

21. personal remarks  site issue – top-down requires one of the host countries to cover 50% (?) of cost – natural way takes time for some of us to come to terms with the outcome – multi-site may be steered by funding prospects  technical design – established convergence provides necessary focus simulations & prototyping efforts are now made in a coherent way [re-]evaluation by early 2012  science – strong case for neutrino astronomy beyond IceCube (and Antares) world-wide collaboration between IceCube, Antares and KM3NeT “Beyond deep core” IceCube workshop, Amsterdam 26‒27 March