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The supernova remnant W49B as seen with HESS and Fermi-LAT
North-West University, South Africa.
University of Hamburg, Germany.
Max Planck Institute for Nuclear Physics, Germany ; Dublin Institute for Advanced Studies, Ireland ; National Academy of Sciences of the Republic of Armenia, Armenia.
Max Planck Institute for Nuclear Physics, Germany.
Vise andre og tillknytning
2018 (engelsk)Inngår i: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 612, artikkel-id A5Artikkel i tidsskrift (Fagfellevurdert) Published
Abstract [en]

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). Gamma-ray observations of SNR-MC associations are a powerful tool to constrain the origin of Galactic cosmic rays, as they can probe the acceleration of hadrons through their interaction with the surrounding medium and subsequent emission of non-thermal photons. We report the detection of a gamma-ray source coincident with W49B at very high energies (VHE; E > 100 GeV) with the H.E.S.S. Cherenkov telescopes together with a study of the source with five years of Fermi-LAT high-energy gamma-ray (0.06-300 GeV) data. The smoothly connected, combined source spectrum, measured from 60 MeV to multi-TeV energies, shows two significant spectral breaks at 304 +/- 20 MeV and 8.4(-2.5)(+2.5) GeV; the latter is constrained by the joint fit from the two instruments. The detected spectral features are similar to those observed in several other SNR-MC associations and are found to be indicative of gamma-ray emission produced through neutral-pion decay.

sted, utgiver, år, opplag, sider
EDP Sciences, 2018. Vol. 612, artikkel-id A5
Emneord [en]
gamma rays: general, ISM: supernova remnants, ISM: clouds
HSV kategori
Forskningsprogram
Fysik, Astropartikelfysik
Identifikatorer
URN: urn:nbn:se:lnu:diva-76472DOI: 10.1051/0004-6361/201527843ISI: 000429404700005Scopus ID: 2-s2.0-85045418660OAI: oai:DiVA.org:lnu-76472DiVA, id: diva2:1232103
Tilgjengelig fra: 2018-07-10 Laget: 2018-07-10 Sist oppdatert: 2019-08-29bibliografisk kontrollert

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Becherini, YvonneFarnier, ChristianProkhorov, DmitryProkoph, HeikePunch, Michael

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