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VHE gamma-rays from the other side of the Milky-Way: SNR G349.7+0.2

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Abstract

Young massive star clusters as sites of strong stellar winds and supernova explosions may accelerate charged particles at high energies and produce gamma-rays. These sources may also contribute to the production of cosmic rays in our galaxy. At TeV energies several candidates have already been detected: Cygnus OB2, Westerlund 1 \& 2, W43, Pismis 22 and W49A. Our study addresses the issue of very young star clusters where no supernova has occurred yet. During the lifetime of a massive star (M$ > 20 M_{\odot}$), supersonic stellar winds do indeed release as much energy as a supernova explosion. As supernova remnants are already known as gamma-ray emitters our purpose is to avoid any ambiguity on the origin of a possible gamma ray emission and to fully assume a stellar wind contribution. In this work we first present a catalogue of potential gamma-ray emitting clusters and discuss the criteria used to built the catalogue. We hence model the expected energetic particle spectrum including escapes and losses. We deduce gamma-ray luminosities produced by Inverse Compton and pion decay emission of each cluster and their associated HII regions. We finally compare these gamma-ray luminosities with HESS-II and CTA Cherenkov telescopes sensitivities.
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Dates and versions

in2p3-00856159 , version 1 (30-08-2013)

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  • HAL Id : in2p3-00856159 , version 1

Cite

C. Trichard, D. Fernandez, V. Marandon, A. Fiasson, Matthieu Renaud, et al.. VHE gamma-rays from the other side of the Milky-Way: SNR G349.7+0.2. 33rd International Cosmic Ray Conference (ICRC2013), Jul 2013, Rio de Janeiro, Brazil. ⟨in2p3-00856159⟩
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