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Antares /KM3NeT. M. de Jong. Neutrino astronomy. p. n. g. neutrinos. Why neutrinos: no absorption no bending ‘remote microscope’. Scientific motivation: origin cosmic rays birth & composition relativistic jets mechanism of cosmic particle acceleration dark matter. - PowerPoint PPT Presentation
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neutrinos g
np
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
Detector operation
date
onlin
e ne
utrin
o co
unt complete direction information
zenith angle only
main cable repairtwelve linesoperational!
%90detector construction
completed
Neutrino detection
L cos q
num
ber o
f eve
nts
Antares: angular resolution 0.5±0.1 degrees
upward going muons good quality events
neutrinosneutrinos
dataMonte Carlo totalMonte Carlo neutrinoMonte Carlo muon
Neutrino sky map (2007‒2008)
2°
Limits on neutrino fluxes, world’s best for some specific sources.
part of sky invisible to Antares
PSF
Nikhef analyses in Antares Point source search, A. Heijboer et al.– 1st 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
31 x 3” PMTETeL, Hamamatsu, ...
concentrator ring
increase of photocathode area by 20‒40%
Optical module
6 m
Mechanical cable connection
Data cable storage
Mechanical cable storage
Frame
Optical module
Mechanical holder
Needs new deployment technique
Storey
1 Digital Optical Module = Dom2 Dom’s on 1 bar = Dom-bar
20 Dom-bar’s on 1 tower = Dom tower
NIOZ operations
1st 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
Atmospheric muon rates
5 10 15 20 25 30 35 4010-2
10-1
1
number of Lx
Rate
[kHz
]
L0L1L2
70% of L0s contribute to L1s
Angular resolution
angle [degrees]
prob
abili
typr
obab
ility
E-2 muon
E-2 neutrino
Antares labs
bar 0 m
standard
SeaWiet
Dt [ns]
R = 10 mR = 20 mR = 30 mR = 40 mR = 50 m
Sky map of event PDFs
Event reconstruction4D-PDF
cos q
f
-1 +100
2p
p
2D-PSF
comparison with IceCube
3s limit
sind
Galactic centre
5s discovery
E2 F [G
eV-1
cm-2
s-1]
IceCubeKM3NeT
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
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
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