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LMC N132D: A mature supernova remnant with a power-law gamma-ray spectrum extending beyond 8 TeV
Univ Namibia, Namibia.
Dublin Inst Adv Studies, Ireland;Max Planck Inst Kernphys, Germany;RAU, Armenia.
Max Planck Inst Kernphys, Germany.
Aix Marseille Univ, France.
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2021 (Engelska)Ingår i: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 655, artikel-id A7Artikel i tidskrift (Refereegranskat) Published
Abstract [en]

Context. Supernova remnants (SNRs) are commonly thought to be the dominant sources of Galactic cosmic rays up to the knee of the cosmic-ray spectrum at a few PeV. Imaging Atmospheric Cherenkov Telescopes have revealed young SNRs as very-high-energy (VHE, >100 GeV) gamma-ray sources, but for only a few SNRs the hadronic cosmic-ray origin of their gamma-ray emission is indisputably established. In all these cases, the gamma-ray spectra exhibit a spectral cutoff at energies much below 100 TeV and thus do not reach the PeVatron regime. Aims. The aim of this work was to achieve a firm detection for the oxygen-rich SNR LMC N132D in the VHE gamma-ray domain with an extended set of data, and to clarify the spectral characteristics and the localization of the gamma-ray emission from this exceptionally powerful gamma-ray-emitting SNR. Methods. We analyzed 252 h of High Energy Stereoscopic System (H.E.S.S.) observations towards SNR N132D that were accumulated between December 2004 and March 2016 during a deep survey of the Large Magellanic Cloud, adding 104 h of observations to the previously published data set to ensure a > 5 sigma detection. To broaden the gamma-ray spectral coverage required for modeling the spectral energy distribution, an analysis of Fermi-LAT Pass 8 data was also included. Results. We unambiguously detect N132D at VHE with a significance of 5.7 sigma. We report the results of a detailed analysis of its spectrum and localization based on the extended H.E.S.S. data set. The joint analysis of the extended H.E.S.S and Fermi-LAT data results in a spectral energy distribution in the energy range from 1.7 GeV to 14.8 TeV, which suggests a high luminosity of N132D at GeV and TeV energies. We set a lower limit on a gamma-ray cutoff energy of 8 TeV with a confidence level of 95%. The new gamma-ray spectrum as well as multiwavelength observations of N132D when compared to physical models suggests a hadronic origin of the VHE gamma-ray emission. Conclusions. SNR N132D is a VHE gamma-ray source that shows a spectrum extending to the VHE domain without a spectral cutoff at a few TeV, unlike the younger oxygen-rich SNR Cassiopeia A. The gamma-ray emission is best explained by a dominant hadronic component formed by diffusive shock acceleration. The gamma-ray properties of N132D may be affected by an interaction with a nearby molecular cloud that partially lies inside the 95% confidence region of the source position.

Ort, förlag, år, upplaga, sidor
EDP Sciences, 2021. Vol. 655, artikel-id A7
Nyckelord [en]
gamma rays, general, cosmic rays, ISM, supernova remnants
Nationell ämneskategori
Astronomi, astrofysik och kosmologi
Forskningsämne
Fysik, Astropartikelfysik
Identifikatorer
URN: urn:nbn:se:lnu:diva-108308DOI: 10.1051/0004-6361/202141486ISI: 000712071700009Scopus ID: 2-s2.0-85118591240Lokalt ID: 2021OAI: oai:DiVA.org:lnu-108308DiVA, id: diva2:1616268
Tillgänglig från: 2021-12-02 Skapad: 2021-12-02 Senast uppdaterad: 2025-05-09Bibliografiskt granskad

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Becherini, YvonneBylund, TomasKukec Mezek, GasperPunch, MichaelSenniappan, Mohanraj

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Becherini, YvonneBylund, TomasKukec Mezek, GasperPunch, MichaelSenniappan, Mohanraj
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Institutionen för fysik och elektroteknik (IFE)
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Astronomy and Astrophysics
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