Suzaku and Fermi view of the supernova remnant 3C 396
| Autor: | Nergis Cesur, A. Sezer, Shota Kisaka, Ryo Yamazaki, Shuta J. Tanaka, Yutaka Ohira, Tulun Ergin |
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| Rok vydání: | 2020 |
| Předmět: |
High Energy Astrophysical Phenomena (astro-ph.HE)
Physics 010308 nuclear & particles physics Astrophysics::High Energy Astrophysical Phenomena Molecular cloud Astronomy Bremsstrahlung FOS: Physical sciences Astronomy and Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics 01 natural sciences Pulsar wind nebula Spectral line Luminosity Supernova Space and Planetary Science 0103 physical sciences Astrophysics - High Energy Astrophysical Phenomena Supernova remnant 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics Fermi Gamma-ray Space Telescope |
| Zdroj: | Monthly Notices of the Royal Astronomical Society, 492, 1, pp. 1484-1491 Monthly Notices of the Royal Astronomical Society, 492, 1484-1491 |
| ISSN: | 0035-8711 |
| Popis: | 3C 396 is a composite supernova remnant (SNR), consisting of a central pulsar wind nebula (PWN) and a bright shell in the west, which is known to be interacting with molecular clouds (MCs). We present a study of X-ray emission from the shell and the PWN of the SNR 3C 396 using archival Suzaku data. The spectrum of the SNR shell is clearly thermal, without a signature of a non-thermal component. The abundances of Al and Ca from the shell are slightly enhanced, which indicates the presence of metal-enriched supernova ejecta. The PWN spectra are well described by a power-law model with a photon index of $\sim$1.97 and a thermal component with an electron temperature of $\sim$0.93 keV. The analysis of about 11-years of Fermi data revealed an 18 sigma-detection of gamma-ray emission from the location overlapping with the position of 3C 396 / 4FGL J1903.8+0531. The spectrum of 3C 396 / 4FGL J1903.8+0531 is best-fitted with a log-parabola function with parameters of $\alpha$ = 2.66 and $\beta$ = 0.16 in the energy range of 0.2$-$300 GeV. The luminosity of 3C 396 / 4FGL J1903.8+0531 was found to be $>$10$^{35}$ erg s$^{-1}$ at 6.2 kpc, which rules out the inverse Compton emission model. Possible scenarios of gamma-ray emission are hadronic emission and bremsstrahlung processes, due to the fact that the SNR is expanding into dense MCs in the western and northern regions of the SNR. Comment: 9 pages, 5 figures; accepted for publication in MNRAS |
| Databáze: | OpenAIRE |
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