ANTARES and KM3NeT John Carr Centre de Physique de Particules
de Marseille IN2P3 / MICINN meeting Madrid, 12 Jan 2009
Slide 2
ANTARES Collaboration CPPM, Marseille CPPM, Marseille APC Paris
APC Paris Univ. de H.-A., Mulhouse Univ. de H.-A., Mulhouse
DSM/IRFU/CEA, Saclay IFREMER, Toulon/Brest IFREMER, Toulon/Brest
C.O.M. Marseille C.O.M. Marseille LAM, Marseille LAM, Marseille
GeoAzur Villefranche GeoAzur Villefranche University/INFN of Bari
University/INFN of Bari University/INFN of Bologna University/INFN
of Bologna University/INFN of Catania University/INFN of Catania
LNS Catania LNS Catania University/INFN of Pisa University/INFN of
Pisa University/INFN of Rome University/INFN of Rome
University/INFN of Genova University/INFN of Genova IFIC, Valencia
IFIC, Valencia UPV, Valencia UPV, Valencia NIKHEF, Amsterdam
NIKHEF, Amsterdam KVI Groningen KVI Groningen NIOZ Texel NIOZ Texel
ITEP, Moscow ITEP, Moscow University of Erlangen University of
Erlangen ISS, Bucharest ISS, Bucharest Spokesman Paschal Coyle,
Marseille Deputy Spokesman Juanjo Hernandez, Valencia Technical
Coordinator Marco Circella, Bari 8% 47% 11% 9% 22% 1% 2%
Slide 3
Current Operating Neutrino Telescopes ANTARES: Mediterranean
Sea BAIKAL: Siberia AMANDA/ICECUBE: South Pole
Slide 4
Motivation for Astronomy Search for cosmic-ray accelerators
Active galactic nuclei Supernova remnants Gamma-ray bursts
Microquasars Unknown objects Search for Exotic Particles Dark
Matter : WIMPs/Neutralinos Magnetic Monopoles Nuclearites Unknown
imagined particles Particle Physics Neutrino Oscillations High
Energy Cross-sections Tests of Lorentz Invariance
Slide 5
Sky Coverage of Neutrino Telescopes Indicative sky coverage
assuming 100% efficiency in downward hemisphere Mediterranean
SeaSouth Pole Galactic Centre seen by northern hemisphere neutrino
telescope
Slide 6
12 lines 25 storeys / line 3 PMTs / storey 900 PMTs ~70 m 100 m
350 m Link cable Junction Box cable to shore Anchor/line socket
2500m depth ANTARES Detector Calibration systems: Acoustic
positioning Optical beacons storey
Slide 7
ANTARES Infrastructure Toulon La Seyne Submarine cable (45km)
Site 20 km from nearest land Shore Station IFREMER Toulon Centre
FOSELEV Marine Shipyard
Slide 8
Detector on seabed Junction Box Line bases Line storeys L11 L9
L10 L12 L8 L6 L4 L2 L3 L5 L1 IL07 seismometer 100 m N Junction box
Submarine cable to shore L7
Slide 9
Data Taking 1 line 2 lines 5 lines 10 lines 12 lines
Slide 10
Time Calibration Optical fibres Laser On shore laser system In
sea LED beacon system LED beacon RMS 0.74ns RMS 0.60ns
Slide 11
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 1 min:
Distance line bases to 5 storeys/line and also storey headings and
tilts
Slide 12
Line position measurements
Slide 13
Data zenith angle distribution Data Atmospheric Neutrino Monte
Carlo Atmospheric Muon Monte Carlo June 2007 Dec 2007 5 lines 140
active days 168 neutrinos 224 neutrinos Dec 2007 May 2008 10 lines
109 active days
Slide 14
Sky map of neutrino events (June 2007 Dec 200, 5 lines,140
active days)
Slide 15
Search for events in 3 cone around 25 sources No significant
excess !
Slide 16
Flux limits on point source search Limit on flux with E 2
spectrum
Conclusion ANTARES completely operational - demonstrates the
feasibility of undersea neutrino telescope France-Spain
co-operations important - IFIC-CPPM optical beacon calibration
systems - UPV-CPPM acoustic positioning - IFIC-APC Point Sources
ANTARES biggest detector in northern hemisphere - already best
results for point sources KM3NeT - next generation neutrino
telescope in Mediterranean Sea - expect significant funding
decisions in 2009
