ANTARES : la pche aux neutrinos cosmiques

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Astronomy Neutrino Telescope with Abyss
environmental RESearch
http//antares.in2p3.fr/
ANTARES Status report

• RD and site properties studies
• Detector design
• High energy performances
• Lower energy studies
• Results from a prototype line
• Construction plans

Antoine Kouchner University Paris 7 Laboratoire
APC and CEA/Saclay for the ANTARES collaboration
HENA Workshop Paris, June 17th 2003
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The ANTARES collaboration

• NIKHEF, Amsterdam

• University of Sheffield
• University of Leeds

• ITEP, Moscou

• IFIC, Valencia

• Universitat, Erlangen

Particle physicists, oceanographers,
astronomers
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The ANTARES immersion site
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Electro-optical cableOctober 10th 2001
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The ANTARES Fleet
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Sea floor survey with Cyana
Obstacle Average density 1 big object per ha
Ex historic compass
Accuracy reached for deployments 5m all objects
around detector located ?No concern
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Water transparency

• Scattering absorption
• ?
• Angular resolution effective detection surface

- Blue light (470 nm) labs 60
? 8 m lscat eff 265 ? 30 m - UV
light (370 nm) labs 26 ? 2 m
lscat eff 120 ? 4 m
Timing of photons (pulsed by LED sources)
Errors ? different measurements
Photons arrival time
(ns)
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Demonstrator immersion
November 1999 - June 2000
Castor
Real time sonar display
Line (descending)
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Acoustic positioning
2 cm
Relative positioning ? 5 cm confirmed with
tilt-meters
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The Antares detector
Shore station
12 equipped lines 75 PMTs / line 5 sectors /
line 5 floors / sector 3 PMTs / floor
Optical module
14,5 m
Octagonal geometry
2475 m
Compass, tilt meter
float
Electro-optic submarine cable 40km
350 m active
Electronics containers
Readout cables
100 m
Junction box
anchor
Acoustic beacon
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Junction box deployment December 2002
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The optical module
Mu metal magnetic shield
Active PMT base (ISEG)
PMT 10 Hamamatsu
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The ARS front-end digitizer
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Storey layout electronics
to the cable
Calibration Beacon
Block of Electronics LCM
Optical Module in the glass sphere
to the cable
Hydrophone
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Scientific Motivations
Medium Energy 10 GeV lt E? lt 1 TeV
Low Energy 10 GeV lt E? lt 100 GeV
High Energy E? gt 1 TeV
? from galactic and extra-galactic sources
neutralino search
? oscillations
Oceanography - measurements of oceanographic
parameters of deep sea - studies of
bioluminescence


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HE expected performances

• Angular resolution

• Em gt 10 TeV ? 0.2º
• Em lt 10 TeV ? n-m interaction dominated

Log(Emrec) GeV

• Spectral resolution

• 10 GeV lt Em lt 100 GeV muon path
• Em gt 1 TeV ? E estimated by a factor 2-3

Log(Emtrue) GeV
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Effective areas (rate/flux)
For n induced muons at the detector 0.01-0.07 km2
For neutrinos when entering earth 1-20 m2
known sources fit quality
Earth Opacity
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Diffuse flux sensitivity
Includes full simulation of tracks and energy
reconstruction
MPR98
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Point-like sources - Sky coverage
One year limit for an E-2 spectrum
ANTARES (43o N) 3.5p sr
After 1 year Antares can improve limit
for Southern hemisphere or discover something
ANTARES
Cowen, Neutrino 2002
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Galactic microquasars
Promising sources detectable by Antares after one
year !
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Extra-galactic fireball GRBs
Source localization and duration ? Low
background ? Soften quality cuts
Compact Object Explosion
Relativistic ejecta
Robust background estimate based on BATSE 4th
catalog burst duration / intensity 6 x 10-3 Bkg
events / year all GRB sources
Shock wave
Fermi acceleration
Different models for neutrino emission WB, MPR,
Guetta et al. 0.5 10 signal events / year
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Search for Dark Matter
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Atmospheric n oscillations
Looking for nm ? nX
Survival probability 1- sin2 2q sin2(1,27 L/E
Dm2) Dm2 squared masses difference eV2
L oscillation length km E nm energy
GeV q mixing angle
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Prototype sector line
Buoy
Optical module - 10 PMT and active base - LED
calibration system
acoustic Rx 2
Local control module - Front end
electronics - positioning monitoring tools
- clock
LED beacon
Master local control module - Processor
5 storeys ? 1Gb/s ethernet to SCM
String control module - power supply
- DWDM
acoustic Rx1
acoustic Rx/Tx
Junction box
Bottom String Socket
Interlink cable
To shore
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Sector line 20 décembre 2002
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(No Transcript)
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Pre-immersion tests

• Acoustic system in a pool

acoustic Rx/Tx transducer

• Calibration in dark room

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Dark room results

• Data
• Without walk correction
• With walk correction

• MC
• Reflects the PMT time transit spread

?t /?21.5 ns
?t /?21.4 ns
?t /?21.3 ns
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Counting rate monitoring
5 mins
50 m
No short time correlation along the line Long
term monitoring foreseen until September
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Counting rate monitoring
Z O O M
20 s
Baseline 60 kHz, correlated spikes seen within
triplets
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Line movement orientation
As an example 40 days monitoring
These measurements allow a 10 cm accuracy on
line position estimate
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Conclusion outlook
ANTARES has successfully met essential milestones
Collaboration forming
1996 1997 1998 1999 2000
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2001 2002 2003 2004 2005