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2013-03-15 - Article/Dans un journal avec peer-review - Anglais - 15 page(s)

Kohnen Georges , IceCube Collaboration , "Search for Galactic PeV Gamma Rays with the IceCube Neutrino Observatory" in Physical Review. D, Particles and Fields, 87, 062002

  • Edition : American Physical Society, Lancaster (PA)
  • Codes CREF : Physique des particules élémentaires (DI1221), Astrophysique (DI1455)
  • Unités de recherche UMONS : Physique nucléaire et subnucléaire (S824)
  • Instituts UMONS : Institut de Recherche sur les Systèmes Complexes (Complexys)
  • Centres UMONS : Algèbre, Géométrie et Interactions fondamentales (AGIF)

Abstract(s) :

(Anglais) Gamma-ray induced air showers are notable for their lack of muons, compared to hadronic showers. Hence, air shower arrays with large underground muon detectors can select a sample greatly enriched in photon showers by rejecting showers containing muons. IceCube is sensitive to muons with energies above ~500??GeV at the surface, which provides an efficient veto system for hadronic air showers with energies above 1 PeV. One year of data from the 40-string IceCube configuration was used to perform a search for point sources and a Galactic diffuse signal. No sources were found, resulting in a 90% C.L. upper limit on the ratio of gamma rays to cosmic rays of 1.2×10-3 for the flux coming from the Galactic plane region (-80°?l?-30°; -10°?b?5°) in the energy range 1.2–6.0 PeV. In the same energy range, point source fluxes with E-2 spectra have been excluded at a level of (E/TeV)2dF/dE~10-12–10-11??cm-2?s-1?TeV-1 depending on source declination. The complete IceCube detector will have a better sensitivity (due to the larger detector size), improved reconstruction, and vetoing techniques. Preliminary data from the nearly final IceCube detector configuration have been used to estimate the 5-yr sensitivity of the full detector. It is found to be more than an order of magnitude better, allowing the search for PeV extensions of known TeV gamma-ray emitters.

Identifiants :
  • arXiv : arXiv:1210.7992
  • DOI : 10.1103/PhysRevD.87.062002