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, Paul K H Yeung Institute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwa-no-ha, Kashiwa, Chiba 277-8582, Japan E-mail: pkh91yg@icrr.u-tokyo.ac.jp Search for other works by this author on: Oxford Academic Shiu-Hang Lee Department of Astronomy, Kyoto University , Kitashirakawa, Oiwake-cho, Sakyo-ku, Kyoto, Kyoto 606-8502, Japan Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo , Kashiwa 277-8583, Japan Search for other works by this author on: Oxford Academic Tsunefumi Mizuno Hiroshima Astrophysical Science Center, Hiroshima University , 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima 739-8526, Japan Search for other works by this author on: Oxford Academic Aya Bamba Department of Physics, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan Research Center for the Early Universe, School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan Trans-Scale Quantum Science Institute, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan Search for other works by this author on: Oxford Academic
https://orcid.org/0000-0003-3476-022X Publications of the Astronomical Society of Japan, Volume 76, Issue 3, June 2024, Pages 490–497, https://doi.org/10.1093/pasj/psae025
Published:
03 May 2024
Article history
Received:
23 August 2023
Accepted:
20 March 2024
Published:
03 May 2024
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Paul K H Yeung, Shiu-Hang Lee, Tsunefumi Mizuno, Aya Bamba, Examining a hadronic γ-ray scenario for the radiative shell and molecular clouds of the old GeV supernova remnant G298.6−0.0, Publications of the Astronomical Society of Japan, Volume 76, Issue 3, June 2024, Pages 490–497, https://doi.org/10.1093/pasj/psae025
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Abstract
Based on the 13.7yr Fermi-LAT data, Yeung, Bamba, and Sano (2023, PASJ, 75, 384) claimed detection of two γ-ray sources (namely Src-NE and Src-NW) associated with the supernova remnant (SNR) G298.6−0.0, and interpreted it as an old GeV SNR interacting with molecular clouds (MCs). In this follow-up study, we refine the flux measurements below 2 GeV with Fermi-LAT event types of better angular reconstruction. Then, we report our γ-ray spectral fittings and cosmic-ray phenomenology in a hadronic scenario, considering both the shell and MC regions of SNR G298.6−0.0. We confirm that the γ-ray spectra of both Src-NE and Src-NW exhibit spectral breaks, at |$1.50_{-0.50}^{+0.60}$| and |$0.68_{-0.11}^{+0.32}\:$|GeV, respectively. Src-NW has a harder broad-band photon index than Src-NE, suggesting an appreciable difference between the physical separations of their respective emission sites from SNR G298.6−0.0. The cosmic-ray spectrum responsible for Src-NE starts with a minimum energy |$E_\mathrm{CR,min}=1.38_{-0.16}^{+0.47}\:$|GeV, and has a proton index |$\Gamma _\mathrm{CR}=2.57_{-0.21}^{+0.18}$| below the exponential cutoff energy |$E_\mathrm{CR,max}=240_{-150}^{+240}\:$|GeV. Accordingly, we argue that Src-NE is dominated by the SNR shell, while only a minor portion of lower-energy emission is contributed by the MCs interacting with the SNR. The cosmic-ray population for Src-NW starts at a higher energy such that the ECR, min ratio of Src-NW to Src-NE is ≳2. The high ECR, min, as well as the high cosmic-ray energy density required (∼26 eV cm−3), supports the interpretation that Src-NW is predominantly the γ-ray emission from the farther MCs being bombarded by protons that had earlier escaped from SNR G298.6−0.0. By comparing the high-energy features of G298.6−0.0 with those of analogical SNRs, especially SNRW 28 and SNRW 44, we further constrain the age of SNR G298.6−0.0 to be 10–30 kyr, under the assumption of a purely hadronic scenario.
© The Author(s) 2024. Published by Oxford University Press on behalf of the Astronomical Society of Japan.
This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model)
Subject
miscellaneous sociology of astronomy surveys
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