Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the...
-
Upload
melina-williamson -
Category
Documents
-
view
216 -
download
0
Transcript of Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the...
![Page 1: Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005.](https://reader035.fdocuments.us/reader035/viewer/2022062500/56649ef25503460f94c0409e/html5/thumbnails/1.jpg)
Antares Neutrino Telescope
Jean-Pierre ErnenweinUniversité de Haute Alsace
(On behalf of the ANTARES collaboration)
Rencontres de Moriond, 13/03/2005
![Page 2: Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005.](https://reader035.fdocuments.us/reader035/viewer/2022062500/56649ef25503460f94c0409e/html5/thumbnails/2.jpg)
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
![Page 3: Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005.](https://reader035.fdocuments.us/reader035/viewer/2022062500/56649ef25503460f94c0409e/html5/thumbnails/3.jpg)
13/03/2005 JP Ernenwein - Rencontres de Moriond 3
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 :
![Page 4: Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005.](https://reader035.fdocuments.us/reader035/viewer/2022062500/56649ef25503460f94c0409e/html5/thumbnails/4.jpg)
13/03/2005 JP Ernenwein - Rencontres de Moriond 4
(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,
![Page 5: Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005.](https://reader035.fdocuments.us/reader035/viewer/2022062500/56649ef25503460f94c0409e/html5/thumbnails/5.jpg)
13/03/2005 JP Ernenwein - Rencontres de Moriond 5
(Potential) Sources of Neutrinos for ANTARES
X ray
OpticalRADIO
e (Compton, Synchrotron)
M 87
p/A + p/ e e
Hadronic interactions
![Page 6: Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005.](https://reader035.fdocuments.us/reader035/viewer/2022062500/56649ef25503460f94c0409e/html5/thumbnails/6.jpg)
13/03/2005 JP Ernenwein - Rencontres de Moriond 6
ANTARES detection principleNeutrino detection principle
č
43°2500 mdepth
p
p,
interaction
Cherenkovlight from
3D PMT array
Measurement :Time & position
of hits
(~ ) trajectory
![Page 7: Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005.](https://reader035.fdocuments.us/reader035/viewer/2022062500/56649ef25503460f94c0409e/html5/thumbnails/7.jpg)
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
![Page 8: Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005.](https://reader035.fdocuments.us/reader035/viewer/2022062500/56649ef25503460f94c0409e/html5/thumbnails/8.jpg)
13/03/2005 JP Ernenwein - Rencontres de Moriond 8
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
![Page 9: Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005.](https://reader035.fdocuments.us/reader035/viewer/2022062500/56649ef25503460f94c0409e/html5/thumbnails/9.jpg)
13/03/2005 JP Ernenwein - Rencontres de Moriond 9
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
![Page 10: Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005.](https://reader035.fdocuments.us/reader035/viewer/2022062500/56649ef25503460f94c0409e/html5/thumbnails/10.jpg)
13/03/2005 JP Ernenwein - Rencontres de Moriond 10
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
![Page 11: Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005.](https://reader035.fdocuments.us/reader035/viewer/2022062500/56649ef25503460f94c0409e/html5/thumbnails/11.jpg)
13/03/2005 JP Ernenwein - Rencontres de Moriond 11
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
![Page 12: Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005.](https://reader035.fdocuments.us/reader035/viewer/2022062500/56649ef25503460f94c0409e/html5/thumbnails/12.jpg)
13/03/2005 JP Ernenwein - Rencontres de Moriond 12
ANTARES Effective AreasAeff = surface of a perfect detector (100% efficiency)
Aeff for Neutrinos : absorption in earth is accounted for computations
![Page 13: Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005.](https://reader035.fdocuments.us/reader035/viewer/2022062500/56649ef25503460f94c0409e/html5/thumbnails/13.jpg)
13/03/2005 JP Ernenwein - Rencontres de Moriond 13
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
![Page 14: Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005.](https://reader035.fdocuments.us/reader035/viewer/2022062500/56649ef25503460f94c0409e/html5/thumbnails/14.jpg)
13/03/2005 JP Ernenwein - Rencontres de Moriond 14
Point-like sources sensitivity
Test of Micro Quasar C. Distefano et al model :
Amanda has the required sensitivity.
Antares will reach this sensitivity.
MACRO
![Page 15: Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005.](https://reader035.fdocuments.us/reader035/viewer/2022062500/56649ef25503460f94c0409e/html5/thumbnails/15.jpg)
13/03/2005 JP Ernenwein - Rencontres de Moriond 15
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
![Page 16: Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005.](https://reader035.fdocuments.us/reader035/viewer/2022062500/56649ef25503460f94c0409e/html5/thumbnails/16.jpg)
13/03/2005 JP Ernenwein - Rencontres de Moriond 16
Submarine cable connection
March 2003
![Page 17: Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005.](https://reader035.fdocuments.us/reader035/viewer/2022062500/56649ef25503460f94c0409e/html5/thumbnails/17.jpg)
13/03/2005 JP Ernenwein - Rencontres de Moriond 17
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
![Page 18: Antares Neutrino Telescope Jean-Pierre Ernenwein Université de Haute Alsace (On behalf of the ANTARES collaboration) Rencontres de Moriond, 13/03/2005.](https://reader035.fdocuments.us/reader035/viewer/2022062500/56649ef25503460f94c0409e/html5/thumbnails/18.jpg)
13/03/2005 JP Ernenwein - Rencontres de Moriond 18
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