KM 3 Neutrino Telescope European deep-sea research infrastructure DANS symposium Maarten de Jong p travel time bending cosmic rays astronomy absorption space travel Astro-Particle Physics Energy spectrum of cosmic rays E [eV/particle] flux [(m 2 sr s GeV) -1 ] per km 2 / year 1 per m 2 / second plateau 1.5 eV = kg 1 m LHC Cosmic particle accelerator? radio images April 1993 June 1998 V ~ km/s charged particle SN1993J M81 V interstellar matter time Which particles? electronsprotons N p p neutrinos muons astronomy cosmic rays Synchroton radiation inverse Compton scattering e e p ++ p ++ ambient light 00 n Neutrino telescope: origin cosmic rays creation & composition of relativistic jets mechanism of cosmic acceleration black hole CERN in the sky Neutrino astronomy 1960 Markovs idea: range of muon detect Cherenkov light transparency of water Use sea water as target/detector How? muon wavefron t ~few km ~100 m muon travels with speed of light (300,000 km/s) ns km neutrino interaction Antares prototype completed May M position time 100 ms data filter 2 s offline reconstruction 1 Mb/s determination of muon direction 1 GB/s track optical background ~ 100 kHz ~5 neutrinos / day All-data-to-shore concept rate [Hz] cos neutrinos! Neutrinos? muon d( ) Earth 2 May :29 30 March :10 Neutrino sky map 2 Limits on neutrino fluxes, worlds best for some specific sources. part of sky invisible to Antares PSF KM3NeT Next generation neutrino telescope 200 250 M Architecture light detection data transmission data filter filtered data neutrino detector shore station analysis operation start stop 100 km 2.5 km > 1000 km 31 x 3 PMT concentrator ring increase of photocathode area by 2040% Optical module 6 m Mechanical cable connection Data cable storage Mechanical cable storage Frame Optical module Mechanical holder Storey 1Digital Optical Module=Dom 2Doms on 1 bar=Dom-bar 20Dom-bars on 1 tower=Dom tower sudden Eddie currents Temperature Earth & Sea sciences France observatory food supply Bioluminescence short lived (rare) events dominate deep-sea life permanent observatory time profile KM3NeT deep-sea infrastructure 10 km 3 > 400,000 PMTs, hydrophones, ACDP, seismometers, etc. < 100 kW, 100 GB/s two main electro-optical cables 100 km, DC, 1 cupper conductor + sea return network passive, point-to-point optical fiber with amplification new Ethernet standard Precision-Time-Protocol (White Rabbit) operation 24h/day, 365 days/year 10 years without maintenance 10kHzx400,000=4GHz 310kHzx13,000=4GHz 0.5kHzx1=500Hz neutrinos10 -3 Hz point source10 -7 Hz signal / noise data filter time Ethernet switch off-shore on shore CPU data flow data filter time Ethernet switch off-shore on shore CPU data flow data filter time Ethernet switch off-shore on shore CPU data flow Data issues operation of infrastructure real-time computing computer farm (Tier 0) control data, QA/QC information, etc. database (Oracle) offline analysis distributed data processing Grid/batch computing Monte Carlo simulations photon tracking CPU intensive GPU (80 x faster than CPU) data analyses ROOT histograms, n-tuples, trees, introspection, etc. high performance I/O Summary & outlook Neutrino astronomy is an emerging field at the intersection of particle physics and traditional astronomy several neutrino detectors operational world wide, in Europe, Antares prototype completed in 2008 Deep-sea is actively explored for large research infrastructures construction of KM3NeT is planned for the coming years synergy between different sciences interesting data challenges