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Population study of Galactic supernova remnants at very high gamma-ray energies with HESS
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.
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2018 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 612, article id A3Article in journal (Refereed) Published
Abstract [en]

Shell-type supernova remnants (SNRs) are considered prime candidates for the acceleration of Galactic cosmic rays (CRs) up to the knee of the CR spectrum at E approximate to 3 x 10(15) eV. Our MilkyWay galaxy hosts more than 350 SNRs discovered at radio wavelengths and at high energies, of which 220 fall into the H.E.S.S. Galactic Plane Survey (HGPS) region. Of those, only 50 SNRs are coincident with a H.E.S.S source and in 8 cases the very high-energy (VHE) emission is firmly identified as an SNR. The H.E.S.S. GPS provides us with a legacy for SNR population study in VHE gamma-rays and we use this rich data set to extract VHE flux upper limits from all undetected SNRs. Overall, the derived flux upper limits are not in contradiction with the canonical CR paradigm. Assuming this paradigm holds true, we can constrain typical ambient density values around shell-type SNRs to n <= 7 cm(-3) and electron-to-proton energy fractions above 10 TeV to epsilon(ep) <= 5 x 10(-3). Furthermore, comparisons of VHE with radio luminosities in non-interacting SNRs reveal a behaviour that is in agreement with the theory of magnetic field amplification at shell-type SNRs.

Place, publisher, year, edition, pages
EDP Sciences, 2018. Vol. 612, article id A3
Keywords [en]
gamma rays: general, ISM: supernova remnants
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Physics, Astroparticle Physics
Identifiers
URN: urn:nbn:se:lnu:diva-76469DOI: 10.1051/0004-6361/201732125ISI: 000429404700003Scopus ID: 2-s2.0-85045517455OAI: oai:DiVA.org:lnu-76469DiVA, id: diva2:1232113
Available from: 2018-07-10 Created: 2018-07-10 Last updated: 2019-08-29Bibliographically approved

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Becherini, YvonneFarnier, ChristianProkhorov, DmitryPunch, Michael

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Becherini, YvonneFarnier, ChristianProkhorov, DmitryPunch, Michael
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