BRUN, F.; LEMOINE-GOUMARD, M.; MARANDON, V.; JOGLER, T.; KATSUTA, J.

doi:10.1016/j.nuclphysbps.2017.06.007

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BRUN, F.
Centre d'Etudes Nucléaires de Bordeaux Gradignan [CENBG]

LEMOINE-GOUMARD, M.
Centre d'Etudes Nucléaires de Bordeaux Gradignan [CENBG]

MARANDON, V.

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Nucl.Part.Phys.Proc., Nucl.Part.Phys.Proc., 2016-07-04, Ischia. 2017, vol. 291-293, p. 30-35

Résumé en anglais

The supernova remnant (SNR) W49B originated from a core-collapse supernova that occurred between one and four thousand years ago, and subsequently evolved into a mixed-morphology remnant, which is interacting with molecular clouds (MC). SNR/MC associations are particularly interesting for probing the acceleration of hadrons in SNRs and consequently the origin of Galactic cosmic rays. The molecular material in the vicinity of the source acts as an efficient target material for accelerated particles, leading to an enhanced γ -ray emission, making these kinds of sources of particular interest for γ ray observatories. W49B has been detected in γ -rays at high energies and very high energies with the Fermi Large Area Telescope ( Fermi -LAT) and the High Energy Stereoscopic System (H.E.S.S.), respectively. The latest results obtained on W49B with these instruments are presented in this contribution. In particular, the spectrum shows a break at low energies, similar to previous observations by the Fermi -LAT in other SNRs and interpreted as the signature of a pion-decay γ -ray emission. The implications of these results on the population of particles at the origin of the γ -ray emission are discussed.< Réduire

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W49B

Supernova remnant

Cosmic-rays

ISM

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The Fermi-LAT and H.E.S.S. views of the supernova remnant W49B

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