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Antares/KM3NeT M. de Jong

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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

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Antares Operation and physics analyses

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

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Neutrino detection cos number of events Antares: angular resolution 0.50.1 degrees upward going muonsgood quality events neutrinos data Monte Carlo total Monte Carlo neutrino Monte Carlo muon

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Neutrino sky map (20072008) 2 Limits on neutrino fluxes, worlds best for some specific sources. part of sky invisible to Antares PSF

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Nikhef analyses in Antares Point source search, A. Heijboer et al. 1 st point source search to be published soon AntaresAuger 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

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

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31 x 3 PMT ETeL, Hamamatsu,... concentrator ring increase of photocathode area by 2040% Optical module

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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 2Doms on 1 bar=Dom-bar 20Dom-bars on 1 tower=Dom tower

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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

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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

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

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

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Sensitivity E 2 [GeV cm -2 s -1 ] ratio sin( )

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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 22 2D-PSF

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

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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

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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 (200250 M) new ways in event reconstruction explored deployment prototype model before end 2011

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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 2627 March