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Detailed spectral and morphological analysis of the shell type supernova remnant RCW 86
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Number of Authors: 2332018 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 612, article id A4Article in journal (Refereed) Published
Abstract [en]

Aims. We aim for an understanding of the morphological and spectral properties of the supernova remnant RCW 86 and for insights into the production mechanism leading to the RCW 86 very high-energy gamma-ray emission.

Methods. We analyzed High Energy Spectroscopic System (H.E.S.S.) data that had increased sensitivity compared to the observations presented in the RCW 86 H.E.S.S. discovery publication. Studies of the morphological correlation between the 0.5-1 keV X-ray band, the 2-5 keV X-ray band, radio, and gamma-ray emissions have been performed as well as broadband modeling of the spectral energy distribution with two different emission models.

Results. We present the first conclusive evidence that the TeV gamma-ray emission region is shell-like based on our morphological studies. The comparison with 2-5 keV X-ray data reveals a correlation with the 0.4-50 TeV gamma-ray emission. The spectrum of RCW 86 is best described by a power law with an exponential cutoff at E-cut = (3.5 +/- 1.2(stat)) TeV and a spectral index of Gamma approximate to 1.6 +/- 0.2. A static leptonic one-zone model adequately describes the measured spectral energy distribution of RCW 86, with the resultant total kinetic energy of the electrons above 1 GeV being equivalent to similar to 0.1% of the initial kinetic energy of a Type Ia supernova explosion (10(51) erg). When using a hadronic model, a magnetic field of B approximate to 100 mu G is needed to represent the measured data. Although this is comparable to formerly published estimates, a standard E-2 spectrum for the proton distribution cannot describe the gamma-ray data. Instead, a spectral index of Gamma(p) approximate to 1.7 would be required, which implies that similar to 7 x 10(49)/n(cm-3) erg has been transferred into high-energy protons with the effective density n(cm-3) = n/1 cm(-3). This is about 10% of the kinetic energy of a typical Type Ia supernova under the assumption of a density of 1 cm(-3).

Place, publisher, year, edition, pages
2018. Vol. 612, article id A4
Keywords [en]
astroparticle physics, gamma rays: general, ISM: supernova remnants, cosmic rays
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:su:diva-155946DOI: 10.1051/0004-6361/201526545ISI: 000429404700004OAI: oai:DiVA.org:su-155946DiVA, id: diva2:1210088
Available from: 2018-05-25 Created: 2018-05-25 Last updated: 2018-05-25Bibliographically approved

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Conrad, Jan M.Farnier, ChristianMeyer, ManuelMorå, KnutSpengler, GerritWagner, Robert M.
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Department of PhysicsThe Oskar Klein Centre for Cosmo Particle Physics (OKC)
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