1. Antoine Kouchner Université Paris 7 Laboratoire APC - CEA/Saclay for the ANTARES collaboration Neutrino Astronomy: a new look at the Galaxy Astronomy Neutrino Telescope with Abyss environmental RESearch http://antares.in2p3.fr International Conference of the 5th APC Workshop High Energy Phenomena in the Galactic Center Paris, 15th - 17th June 2005 Detection principles The case for the GC ANTARES status

2. Paris - June 16, 2005 A. Kouchner - High Energy Phenomena in the Galactic Center 2   Time, position, amplitude of PMT pulses   trajectory (~ < 0,5 °) Detection of Cherenkov light emitted by muons with a 3D array of PMT Requires a large dark transparent detection medium Muon neutrino detection principle  well suited for HE detection Both range and cross-section increase with energy  Large effective volume  

3. Paris - June 16, 2005 A. Kouchner - High Energy Phenomena in the Galactic Center 3 Background constraints 10 -7 cos   atmospheric muons muons induced from atmospheric 10 6 d  /d  cm -2 s -1 sr -1 10 -9 10 -11 10 -13 10 -15 10 -17 2400 m depth E > 1 TeV Very intense atmospheric muon flux  Signal = upward muons log (energy) log (dN/dE) ν μ atm E -3,7 ν μ cosm E -2 Energy cut p    Atmosphere Sea p, 

4. Paris - June 16, 2005 A. Kouchner - High Energy Phenomena in the Galactic Center 4 Visible sky and detector latitude South Pole visible sky Mediterranean visible sky The Galactic Center cannot be seen by AMANDA/IceCube with upward muons A Mediterranean detector will see the GC 2/3 of the time 3.5  sr covered Visibility time fraction for Antares

5. Paris - June 16, 2005 A. Kouchner - High Energy Phenomena in the Galactic Center 5 The ANTARES collaboration Cable Assembly hall Power station Electro- optical Cable Shore station Institut Michel Pacha IFIC Valencia IFREMER, Brest DAPNIA, Saclay IReS, Strasbourg Mulhouse CPPM Marseille IFREMER,Toulon COM, Marseille Villefranche ITEP Moscow NIKHEF Groningen Amsterdam Genova Bari Catania Roma Erlangen LNS Pisa Bologna

6. Paris - June 16, 2005 A. Kouchner - High Energy Phenomena in the Galactic Center 6 a storey The 12 string Antares Telescope 25 storeys / line 3 PMTs / storey 900 PMTs ~70 m 350 m 100 m 14.5 m Submarine links Junction Box 40 km to shore Anchor/line socket 2005-2007  F. Montanet

7. Paris - June 16, 2005 A. Kouchner - High Energy Phenomena in the Galactic Center 7 E µ > 10 TeV ~ 0.2º E µ < 10 TeV µ kinematics dominated  Angular resolution HE expected performances (  )  Muon effective surface

8. Paris - June 16, 2005 A. Kouchner - High Energy Phenomena in the Galactic Center 8 Background associated to point sources E  >1TeV Nb selected atm.  per year (average) In the GC direction 22 300 1° 0.050.03 0.5° 0.010.007 After quality cuts, the remaining background is due to atmospheric neutrinos only A. Heijboer ‘s thesis Very low background for point-like sources !! No energy cut

9. Paris - June 16, 2005 A. Kouchner - High Energy Phenomena in the Galactic Center 9 Inferring flux from  observations 2  1 e 0  for 1   Assume hadronic origin of the observed  -rays from GC p + p                     e   e   e   e    Then d/dE 2 At source ! For E   [E 1, E 2 ] L. Anchordoqui, Acta Phys.Polon. B36 (2005) 495 e :  :  =1:2:0 at source e :  :  =1:1:1 at Earth !

10. Paris - June 16, 2005 A. Kouchner - High Energy Phenomena in the Galactic Center 10 HESS observations - Energy spectrum dF/dE  = F 0 E -  m -2 s -1 GeV -1 with  = 2.2 & F 0 = 1.1×10 -4 Aharonian et al., A&A 425, L13-L17 (2004) Neutrinos from the GC dF/dE   = 4.8 ×10 -5 E -2.2 m -2 s -1 GeV -1 (including oscillations)

11. Paris - June 16, 2005 A. Kouchner - High Energy Phenomena in the Galactic Center 11 from the GC – Expected rates ANTARES not large enough  Need at least 1 km 3 detector ! (~1 event /year) Most of the signal around E ~10 TeV ~0.03 evt / year 2.10 -2 3.10 -2 10 -2 Nb events with E>E PRELIMINARY 2.10 -3 3.10 -3 10 -3 neutrino anti-neutrino Nb events per bin

12. Paris - June 16, 2005 A. Kouchner - High Energy Phenomena in the Galactic Center 12 Extrapolated rates in a km 3 detector Energy dependence of the effective surface should be taken into account The Mediterranean km 3 detector layout is not fixed Realistic scaling factor 40

13. Paris - June 16, 2005 A. Kouchner - High Energy Phenomena in the Galactic Center 13 Rates in Antares and a km 3 detector E  >1TeV d   0.5° Not optimized PRELIMINARY ANTARES KM3 Signal events /year Bkg events /year Time for detection (4  CL) Time for detection (4  CL) GC HESS 2  10 -2 7  10 -3 247 yr6.2 yr EGRET+EHECR Crocker et al (2005) 20.4 yrweek RX J1713.7 -3946 Constantini et al (2005) 0.16 9  10 -3 15 yr0.4 yr Halzen et al (2002) 0.951.8 yr3 weeks PSR B1509- 58 HESS MSH 15-52 0.111.1  10 -2 22 yr0.6 yr

14. Paris - June 16, 2005 A. Kouchner - High Energy Phenomena in the Galactic Center 14 Increasing sensitivity for point sources M. Bouwhuis’ thesis Use prior knowledge of the source direction for both filtering and reconstruction Method originally developed for GRB alerts relative efficiency neutrino energy (GeV) Could be used online for persistent sources like the GC Gain by a factor of ~2 - About 5 times more CPU needed per source

15. Paris - June 16, 2005 A. Kouchner - High Energy Phenomena in the Galactic Center 15 Latest deployments: line 0 A 23 storey line for testing electro-optical transmission Deployed in march 2005

16. Paris - June 16, 2005 A. Kouchner - High Energy Phenomena in the Galactic Center 16 Mini instrumented line + 4 PMTs (MilOM)

17. Paris - June 16, 2005 A. Kouchner - High Energy Phenomena in the Galactic Center 17 Line connections 12-14 April, 2005

18. Paris - June 16, 2005 A. Kouchner - High Energy Phenomena in the Galactic Center 18 First test of in-situ time calibration system  OM ~ 0.7/  2 ns well within spec.  The expected angular resolution should be achieved

19. Paris - June 16, 2005 A. Kouchner - High Energy Phenomena in the Galactic Center 19 Conclusions ANTARES is a first step towards the Mediterranean km 3 Electronics tested in situ in its latest version Calibration system operational The detector should be complete late 2007 Could indicate surprise from the Galactic Center Observation neutrino from GC likely with a Northern km 3 Requires a good angular resolution (muon neutrinos) The associated background is very low The detection of a few events is significant The absence of signal will constrain the emission models Latest deployments ANTARES will be the biggest NT with GC in its field of view