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Neutrino Astronomy: a new look at the Galaxy

A stronomy N eutrino T elescope with A byss environmental RES earch. http://antares.in2p3.fr. Neutrino Astronomy: a new look at the Galaxy. Detection principles The case for the GC ANTARES status. International Conference of the 5th APC Workshop

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Neutrino Astronomy: a new look at the Galaxy

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

  2. Detection of Cherenkov light emitted by muons with a 3D array of PMT Requires a large dark transparent detection medium m Time, position, amplitudeof PMT pulses  m trajectory (~ n < 0,5 °) n Muon neutrino detection principle mwell suited for HE detection Both range and cross-section increase with energy  Large effective volume gč qč A. Kouchner - High Energy Phenomena in the Galactic Center

  3. 10-7 atmospheric muons 2400 m depth E > 1 TeV Atmosphere Sea 10-9 p, a nm p dF/dW cm-2 s-1 sr-1 m 10-11 106 muons induced from atmospheric n 10-13 10-15 Energy cut 10-17 cos qm nm Very intense atmospheric muon flux Background constraints νμatm E-3,7 log (dN/dE) νμcosm E-2 log (energy)  Signal = upward muons A. Kouchner - High Energy Phenomena in the Galactic Center

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

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

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

  7. HE expected performances (nm) • Angular resolution • Eµ> 10 TeV ~ 0.2º • E µ< 10 TeV nµ kinematics dominated • Muon effective surface A. Kouchner - High Energy Phenomena in the Galactic Center

  8. Background associated to point sources A. Heijboer ‘s thesis After quality cuts, the remaining background is due to atmospheric neutrinos only No energy cut Very low background for point-like sources !! A. Kouchner - High Energy Phenomena in the Galactic Center

  9. Assume hadronic origin of the observed g-rays from GC • p + p  p0 + p+ + p- + N +...    g + g m+ + nm m- + nm   e+ + ne + nm e- + ne + nm 2nm 1ne 0nt for 1g L. Anchordoqui, Acta Phys.Polon. B36 (2005) 495 For Ep [E1, E2] At source ! Then d/dE2 e:: =1:2:0 at sourcee:: =1:1:1 at Earth ! Inferring n flux from g observations A. Kouchner - High Energy Phenomena in the Galactic Center

  10. dF/dEnm+nm = 4.8 ×10-5E-2.2 m-2 s-1 GeV-1 (including oscillations) Neutrinos from the GC HESS observations - Energy spectrum Aharonian et al.,A&A 425, L13-L17 (2004) dF/dEg = F0 E- m-2 s-1 GeV-1 with a= 2.2 & F0 = 1.1×10-4 A. Kouchner - High Energy Phenomena in the Galactic Center

  11. anti-neutrino 3.10-3 neutrino 2.10-3 Nb events with E>En 3.10-2 ~0.03 evt / year 10-3 2.10-2 10-2 n from the GC – Expected rates PRELIMINARY Nb events per bin Most of the signal around En ~10 TeV ANTARES not large enough  Need at least 1 km3 detector ! (~1 event /year) A. Kouchner - High Energy Phenomena in the Galactic Center

  12. Extrapolated rates in a km3 detector Energy dependence of the effective surface should be taken into account The Mediterranean km3 detector layout is not fixed Realistic scaling factor 40 A. Kouchner - High Energy Phenomena in the Galactic Center

  13. Rates in Antares and a km3 detector A. Kouchner - High Energy Phenomena in the Galactic Center

  14. relative efficiency Could be used online for persistent sources like the GC Gain by a factor of ~2 - About 5 times more CPU needed per source neutrino energy (GeV) 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 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 A. Kouchner - High Energy Phenomena in the Galactic Center

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

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

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

  19. Conclusions Observation neutrino from GC likely with a Northern km3 • 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 ANTARES is a first step towards the Mediterranean km3 • 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 Latest deployments ANTARES will be the biggest NT with GC in its field of view A. Kouchner - High Energy Phenomena in the Galactic Center

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