1. The ANTARES Neutrino Telescope and its Dark Matter Capabilities
Jürgen Hößl, Universität Erlangen, on behalf of the ANTARES Collaboration
Edinburgh, September 2004

2. ANTARES NeutrinoTelescope
buoy
350 m
12 lines
25 storeys / line
3 PMTs / storey
40 km to
shore
100 m
Junction
box
muon
65 – 70 m

3. ANTARES Site Shore Station Institut Michel Pacha -2500m
Submarine Cable
La Seyne sur Mer
Institut Michel Pacha
Shore Station

4. 2/3 of time: Galactic Centre
Sky Coverage
ANTARES
43o North
2/3 of time: Galactic Centre
Dateien
AMANDA
South Pole
Dateien
0.5 p sr instantaneous common view
1.5 p sr common view per day

5. Angular Resolution sq < 0.2o m n n m for high energies:
(Quality of water!)

6. ANTARES Collaboration
Erlangen
NIKHEF
Amsterdam
ITEP
Moscow
Sheffield
Leeds
IFREMER, Brest
DAPNIA, Saclay
IReS, Strasbourg Mulhouse
CPPM Marseille
IFREMER,Toulon
COM, Marseille
OCA, Nice
Genova
Bologna
Bari
IFIC
Valencia
Pisa
Roma
Catania
LNS

7. Scientific Programme Neutralino search
Annihilation at centre
of Earth, Sun, Galaxy
cc  n ....
Search for galactic/extragalactic
n sources
SN remnants, Galactic microquasars
AGN, GRB, …
+ oceanography, biology, seismology

8. Cosmic Particle Accelerators
Gamma Ray
Bursts
Supernova
Remnants
Pulsars,
Plerions
Active Galactic
Nuclei
(Quasars, Blazars)
Microquasars

9. Dark Matter Microwave background Gravitational lenses
Rotation of galaxies
Gravitational lenses

10. Search for Neutralino Annihilation
Gravitational capture of c in Earth, Sun,
Galactic Centre c c
WIMP loses energy by elastic interaction
if v< vescape =>capture
capture + annihilation balance
=> constant density in core
Annihilation:
Wm m c c+ c
bcm m - ~ b c
bcm m +
hard spectrum ( if Mc<MW)
soft spectrum

11. Dark Matter Sensitivity
search cone
around source
(depends on
Neutralino mass)
number of atmos-
pheric background
events
90 % upper limit
on signal events
mSUGRA
parameter scan
comparison
muon/neutrino
flux prediction
muon /neutrino
flux limit

12. WIMP Annihilation in Sun

13. WIMP Annihilation at Centre of the Earth
- mass of Earth << mass of Sun
possibly dramatic reduction of capture rate in Earth due to
depletion of neutralino density by solar capture
Large uncertainties
(J.Lundberg and J.Edsjö, astro-ph/ )
only small capture rate in the Earth
annihilation rate and neutrino flux from Earth
smaller than from Sun
for ANTARES:
search from Earth not competitive with search from Sun

14. WIMP Annihilation at Galactic Centre (GC)
possibility to probe DM profile in Galactic Centre (contrary to direct searches)
- uncertainties about DM profile:
standard parametrisations give low neutrino fluxes from GC
(e.g. Navarro, Frenk and White, Astrophys. J. 462(1996) 563 )
from G. Bertone et al.
astro-ph/

15. WIMP Annihilation at Galactic Centre (GC)
but: possible enhancement of annihilation flux by orders of
magnitude in the presence of a black hole (spike)
(e.g. P. Gondolo and J. Silk, Phys. Rev. Lett. 83(1999)1719 )
EGRET g signal
neutrino flux:
from G. Bertone et al.
astro-ph/
orders of magnitude flux uncertainties!

16. Mini Instrumentation Line Feb 2003
Prototype Sector Line
Dec 2002
12m
100m
100m
LASER Beacon
LED beacon
Mini Instrumentation Line Feb 2003
Status ANTARES
to shore
Oct 2001
Dec 2002

17. Prototype Sector Line: Nov 2002

18. PSL & MIL Operation in 2003 Lot of data during 3 months of operation
Sea operations: - deployment/connections/recovery
without problems
Line operations: - power distribution
- data transfer to shore (130 GByte)
- remote control
minor problems:
- distribution of the onshore synchronised clock signal failed due
to broken fibre: manufacturer used inappropriate cable
water leakage in Mini Instrumentation Line after 2 months under
high pressure: mismatch of o-ring/hole size
Lot of data during 3 months of operation

19. Optical Background Less than 1% burst fraction 10% burst fraction
bursts
baseline
10min
10min
K + bioluminescence 40

20. Long Term Background

21. ANTARES Summary and Future
_________________
Operation
of Sector
Line
Deployment of lines 1 to 12
and operation
Mini Instrumentation Line with Optical Modules: deployment and operation
Sector Line connection
in 2007
12 string detector
complete
Mini Instrumentation Line deployment
Sector Line deployment
Junction box deployment

22. The End