Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005

Antares Neutrino Telescope

Jean-Pierre ErnenweinUniversité de Haute Alsace

(On behalf of the ANTARES collaboration)

Rencontres de Moriond, 13/03/2005

13/03/2005 JP Ernenwein - Rencontres de Moriond 2

ANTARES collaboration

IFICValencia

IFREMER,Toulon & BrestDAPNIA, SaclayIReS, StrasbourgGRPHE, MulhouseCPPM Marseille IGRAP, MarseilleCOM, Marseille

ITEPMoscow

NIKHEFAmsterdam

Genova

BariCatania

Roma

Erlangen

LNS

Pisa Bologna


The messenger of ANTARES

: absorbed (interaction with C.B.)

p : magn. field +GZK effect

– Weakly interacting Source exploration on cosmological distances

– Access to the heart of sources – Weakly interacting large detection volume required

Neutrino :


(Potential) Sources of Neutrinos for ANTARES

GALACTIC SOURCES

Dark Matter : annihilation of

neutralinos inside massive objects

(Sun, Earth, Galactic Center)

EXTRA GALACTIC SOURCES

Active Galactic Nuclei

M 87, HST

SN 1987A, HST

Supernova remnants,

Gamma Ray Bursts

Micro Quasars,

Pulsars,

Crab Nebula

Galactic Center,


(Potential) Sources of Neutrinos for ANTARES

X ray

OpticalRADIO

e (Compton, Synchrotron)

M 87

p/A + p/ e e

Hadronic interactions


ANTARES detection principleNeutrino detection principle

č

43°2500 mdepth

p

p,

interaction

Cherenkovlight from

3D PMT array

Measurement :Time & position

of hits

(~ ) trajectory

13/03/2005 JP Ernenwein - Rencontres de Moriond 7© F. Montanet

• 12 lines• 25 storeys / line• 3 PMTs / storey• 900 PMTs

~70 m

100 m

350 m14.5 m

Submarine links

JunctionBox

40 km toshore

Anchor/line socket

to be deployed by 2005-2007

a storey

2500m depth


Detector design

Optical Beacons

timing calibration with

blue LEDs

Vacuum valve

Photomultiplier

Magnetic Shield

Optical gel

LED

Glass Sphere

Base (electronics)

penetrator

Optical Module : 10’’ PMT + time calibration LED.

STOREY

Local Control Module (Ti cylinder)

Housing of electronics (PMT, compass, acoustics …)

Inner rackTi tubepenetrator


Off the coast of Toulon (France) in mediterranean Sea (42º50’N, 6º10’E), at 2500 m depth.

ANTARES location and sky view

0.5 sr instantaneous common view

IceCube, AMANDA (South Pole) 2 sr

2/3 time see Galactic Center

ANTARES (42.5o N) 3.5 sr


kinematics reconstruction

ANTARES angular resolution

Eµ >10 TeV

Electronics simulation + light absorption & scattering + light background (40K + bacteria bioluminescence ~ 60 kHz) :

Angular resolution < 0.2°

abs ~ 26/60 m @ 370/470 nm

eff (scattering)~ 100/300 m @ 370/470 nm

WATER on ANTARES site


10 GeV < E < 100 GeV : method = muon path E>1 TeV : method = quantity of light

E estimated by a factor 2-3

ANTARES Energy resolution


ANTARES Effective AreasAeff = surface of a perfect detector (100% efficiency)

Aeff for Neutrinos : absorption in earth is accounted for computations


Performances :Diffuse FluxesNeutrino oscillations e:: = 1:1:1

Detectors sensitive to HE cascades sensitive to HE of any flavour

ANTARES HE

cascade sensitvity

estimate in progress

not yet included

in limits


Point-like sources sensitivity

Test of Micro Quasar C. Distefano et al model :

Amanda has the required sensitivity.

Antares will reach this sensitivity.

MACRO


10min

Rate (kHz)

time

Prototype Sector Line

Profiler for Sea currant

(ADCP)

Probe for salinity and temperature (CTD)

Probe for Sound velocity

J unction Box

LED Beacon

Laser Beacon

Seismograph

hydrophones hydrophone

5 Storeys of Optical Modules

Anchor with electronics containers Link Cables

5 storeys

Junction box

Connected in March 2003

40K + bacteria

burst

correlation between burst fractionand sea current velocity observed

Sea operation

OK

Remote control

OK

Water leak in 1 LCM

Broken fiber in EMC


Submarine cable connection

March 2003


light transmissiometer

water current profiler

Conductivity- Temperature probe

Year 2005 : Line 0, MILOMLine 0 :

23 storeys with spheres but

without PMTs inside

purpose :

test of new version of EMC

cable

&

test of LCMs penetrators

(failures in PSL)

MILOM

Mini Instrumented Line with Optical Modules

4 PMTs

& positionning

devices

&

calibration devices

Connection : april 2005


Next Steps : Line 1 ...

Line 1 is currently at the integration step

Line 1 will be deployed and connected in autumn 2005

The 11 next lines will be deployed and connected during year 2006 / beginning of 2007

Line 0 : validation of the new EMC cable

Documents

Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005