ANTARES

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• ANTARES
• Astronomy with a Neutrino Telescope Abyssal
  RESearch
• A Status Report

Thierry Pradier for the ANTARES
Collaboration IPHC Strasbourg (France)
http//antares.in2p3.fr
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A short history of Neutrinos...
1930 Pauli invents the neutrino to explain
??radiation 1933 Fermi explains in details the
mechanism 1953 Experimental Observation of the
Neutrino (Reines Cowan) 1968 Solar Neutrinos
are detected (Davis) 1987 Neutrinos from SN
1987 A are detected
Birth of Neutrino Astronomy
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Neutrinos in the Universe
Big Bang
Supernovae Explosions
Sun
Terrestrial
Reactors
SNR
Atmospheric
Astrophysical
Neutrino Energy (eV)
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Using the neutrino as a new messenger...
?
?
n
p

• Exploration of Sources over cosmological
  distances
• Access to the very heart of Sources
• Weak Interaction need for Huge detection Volume
• Similarity with Gravitational Waves

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Detection Principles Target Earth !
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Typical dynamic range 1 pe , 20 pe
Detection Principles Target Earth !
?c
Shower
Good energy resolution (O(30)), poor angular
resolution (O(10))
Track
Threshold 1/3 pe
Good angular resolution (lt0.3 _at_ Egt10 TeV), poor
energy resolution (factor 2-3)
1 photo-electron
?
?e
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Charged Current (W)
??
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Detection Principles Backgrounds !
10-7
atmospheric muons
10-9
2400 m depth E gt 1 TeV
?
d?/d? cm-2 s-1 sr-1
10-11
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muons induced from atmospheric ?
10-13
10-15
10-17
cos ??
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Sources of High Energy Neutrinos Cosmic
Accelerators
Supernovae
Gamma-Ray Bursts
Cosmic Ray Astronomy
?-Ray Astronomy
Pulsars
E X T R A - G A L A C T I C
G A L A C T I C
Active Galactic Nuclei
Microquasars
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Sources of High Energy Cosmic Accelerators

• Cosmic Rays
• KASCADE, Auger
• ? Rays
• HESS
• GW ?
• Virgo/LIGO

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Connections with other messengers...
I
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I-Connection with other messengers Cosmic Rays
SNR origin
Galactic origin (several theories)
Extra Galactic Origin
1 particle per m2 per second.
1 particle per m2 per year.
1 particle per km2 per year.
Giant ASA
Ground Based Air Shower Arrays
Balloon Borne Instruments
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I-Connection with other messengersUHECRs Auger
Visible both by Antares Auger
Never visible
Always visible by both
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I-Connection with other messengersUHECRs Auger
Clusters in 2.5o
AGASA Collab., Astron.J. 120 (2000) 2190
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I-Connection with other messengersUHECRs Auger
0.11 EeV
110 EeV
Compatible with Isotropy
Auger Collab., ICRC 2007
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I-Connection with other messengersUHECRs Auger
Cosmogenic neutrino Flux
Guaranteed source of UHE ?
D. Allard et al. JCAP 0609 (2006) 005
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I-Connection with other messengers? and HESS
More than 30 TeV ? sources
Aharonian et al., (HESS Collaboration),
Astroph. J. 636(2006)
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I-Connection with other messengers? and HESS
H.E.S.S. ????R? 0.1 o
ANTARES
??????0.2??for?E???10?TeV
Source size (degrees)
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I-Connection with other messengers? and HESS
RX J1713.7-3946
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I-Connection with other messengers? and HESS
A.Kappes et al., astro-ph/0607286
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I-Connection with other messengersGWs
Virgo/LIGO

• Excitation of BH/NS
• Acceleration of Jet

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I-Connection with other messengersGWs
Virgo/LIGO
Maximum hGW for a NS/BH ?Q at 1 kpc
Th. Pradier, AA to be submitted
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I-Connection with other messengersGWs
Virgo/LIGO
Detection efficiency for Virgo alone, with SNR
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N. Arnaud et al., Phys.Rev. D65 (2002) 042004
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I-Connection with other messengersGWs
Virgo/LIGO
Never Visible by Antares
Always Visible by Antares
Angular resolution of Virgo 2 LIGOs Network
F. Cavalier et al., Phys.Rev. D74 (2006) 082004
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The ANTARES Neutrino Telescope
II
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II-ANTARES ...and other Neutrino Telescopes in
the World...
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II-Antares Observable Skies with Antares/Amanda
IceCube, AMANDA (Southe Pole) 2? sr
ANTARES (43o N) 3.5? sr
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II-ANTARES The Collaboration
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II-ANTARES The detector
350 m
100 m
12 lines 3x25 PMTs/line
60-70 m
-2500 m
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II-ANTARES The basic element a Storey
Optical Beaconwith blue LEDs timing calibration
? astro-ph/0703355
Titanium frame support structure

• Optical Module 10 Hamamatsu PMT in
• 17 glass sphere
• photon detection
• NIM A555 (2005) 132

Hydrophone acoustic positioning
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II-Antares Physics Performances
Opacity of Earth to Neutrinos
?
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II-Antares Physics Performances

• Spectral resolution

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

• Angular resolution

• Eµ gt 10 TeV ? 0.2º
• E µ lt 10 TeV ? µ-? interaction

Median angle ()
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II-Antares Pointing Calibration Shadow of the
Moon
C. Distefano et al., NEMO Collab. NIM A567 (2006)
495-497
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II-Antares Physics Performances
Antares Limit
WB Limit
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II-Antares Physics Performances
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ANTARES Milestones
III
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III-Antares Milestones 2003 Immersion
Connection of a Protoype Line
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III-Antares Milestones 2003 Immersion
Connection of a Protoype Line
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III-ANTARES MilestonesCurrent Lines taking data

• 2005 2006
• Mini Instrumentation Line Oms (MILOM)
• 12 April 2005 ? 6 April 2007
• Line 1 running since 2 March 2006,first
  complete detector line
• Line 2 running since Sept 2006

L2

• 2006 now
• Lines 3,4,5 connected January 2007
• 5 Lines taking data !
• Lines 6,7 deployed
• Lines 8,9 deployed in July

Full completion early 2008 !
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ANTARES in Operation...
IV
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IV-ANTARES OperationTime Calibration
Led Beacon blue LEDs synchronizedflash lt 0.5
ns Intense lightPMT TTS negligible
Timing resolution of electronics lt0.5ns within
spec
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IV-ANTARES OperationTime Calibration
All timing measurements in good agreement with
expectations
Line 1
150 m
MILOM
70 m
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IV-ANTARES OperationCoincidence rates from 40K
decay
e-
40Ca
?Cherenkov
40K
Simulation 12 Hz 4 Hz (sys)
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IV-ANTARES OperationDetector Positioning
Acoustic distance measurement of hydrophones
from fixed emitters on MILOM anchor autonomous
transponders

• Hydrophone

hydrophones
storey positions fit
Acoustic positioning and tilt-meters ? Line
shape
AutonomousTransponder
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ANTARES first Results...
V
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V-ANTARES ResultsEvent Displays

• Hits are plotted for each line height (z) versus
  time (t)
• Characteristic pattern depending on zenith angle
  and
• distance of closest approach

upward
downward
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V-ANTARES ResultsEvent Displays Atmospheric
muons
Hit altitude (relative to mid detector) m
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V-ANTARES ResultsEvent Displays Atmospheric
muons
Antares preliminary

• 21240 / 12527
• ?? 146o

Hit altitude (relative to mid detector) m
µ
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V-ANTARES ResultsEvent Displays Atmospheric
muons Bundles
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V-ANTARES Results(Atmospheric) Neutrino Candidate
?55o
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Soon...
? ?
ANTARES/KM3NeT
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The End...
...