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Point to sun e-e- sun e 4p 4 He + 2e e + 25 MeV Atomic electron! Earth
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Astroparticle physics with large neutrino detectors
Existing detectors Physics motivation Antares project KM3NeT proposal
M. de Jong
Super-Kamiokiande detector
50 kT water Cherenkov detector
Point to sun
e-
sun e
4p 4He + 2e+ + 2e + 25 MeV
Atomic electron!
Earth
Super Nova 1987A
Time correlation
All particle cosmic ray spectrum
= E-2.7 (m
2 s
r s
GeV
)-1
E (GeV)
1 / km2 /year
Where do they come from?
Pierre Auger Observatory
Emax = 1021 eV > 5 x 1019 eV (GZK)
1 GeV 1010 GeV
Neutrino detection
Neutral point back Weak interaction no absorption
Need huge detector
XN
1.5deg.θE TeV
1960 Markov’s idea:
Range of muon:
Detect Cherenkov light:
Transparency of water:
R 1 km at 200 GeV
Use sea water as target/detector
c90 AN sin θcm 2 d
λ 50 100 m
Amanda neutrino sky map
Atmospheric muonshorizon
No point sources discovered yet
Active Galaxy(e.g. M87)
Black hole with108 x mass of sun
104 ly
extra-galactic
Microquasar(SS433 etc.)
Black hole with mass of sun
1 ly
galactic
Neutrino source candidates
Supernova remnant(Crab nebula)
Neutrino production Acceleration:
Decay:
0accp (p) X
ee
ee
0X qq
Astrophysics– Neutrino astronomy– Composition of jets– Engine of cosmic accelerators
Particle physics– Origin of UHE cosmic rays– Massive particles (GUT)– Dark matter– Neutrino properties (, )
Physics motivation
Diffuse neutrino fluxes
atmospheric neutrinos
W&B
MPR
DUMAND
+ NT-200
AMANDA-II/ANTARES
IceCube/KM3NeT
NT-200AMANDA-B10
GRB
Antares detector
Equipped volume 0.1 km2 x 0.4 km (=800 x SuperK)
42° 50’ N 6° 10’ E
Atlas
Detection principle
c(tj - t0) = lj + dj tan(c)
+ N + X
= 0.2 deg.x = 20 cmt = 1 ns
mediumproperties
“All-data-to-shore” conceptpo
sitio
n
time
10 ms
DataFilter
2 s
offline reconstruction
1 MB/s
determination of trajectory
1 GB/s
events
GRB alert systems
GRBs are detected by satellites
Distribution of GRB alerts that follow the detection of a GRB within tens of seconds
Possibly messages will followwith the location of the burst
Data taking in case of a GRB alert
GRB alert
DataFilterDataFilterDataFilterDataFilterDataFilterDataFilterDataFilterDataFilterDataFilterDataFilterDataFilter
alert trigger
events from the known direction
looks for correlations in thedata for the given direction
write all data to disk, including all data in memory
all data
100 DataFilter nodes with each 1 GB RAM
location of the GRB
detector
data filtered offline100 s of unfiltered data
prior to the alert+
few minutes of unfiltered data after the alert
disk
disk
specialised data filter
Effective volume
log10 E (GeV)
effe
ctiv
e vo
lum
e (k
m3 )
Detection efficiencies
clustering and reconstruction using direction information
standard clustering and reconstruction
Improved detection efficiency
GRB detection Source tracking Monopole detection Periodic signals
“All-data-to-shore” options:
KM3NeT
Main objectives– Equipped volume 1 km3 (25 x Antares)– Cost/Volume x 0.5– 4 Field Of View– Angular resolution 0.1 deg.
FP6 Design Study proposal March 2004– NIKHEF leading partner IT– PMT & readout developments– Detector parts assembly in the Netherlands
KM3NeT
Summary
Water Cherenkov: Large neutrino detectors Antares: “All-data-to-shore” concept KM3NeT initiative 2004 - 2008 Astroparticle physics with neutrinos