Suzaku observations of Fe K-shell lines in the supernova remnant W51C and hard X-ray sources in the proximity
Suzaku observations of Fe K-shell lines in the supernova remnant W51C and hard X-ray sources in the proximity
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朱雀对超新星遗迹 W51C 中的 Fe K 壳线和附近的硬 X 射线源的观测
DOI：
10.1093/pasj/psac026
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发表时间：
2022
影响因子：
2.3
通讯作者：
Fujita Yutaka
中科院分区：
文献类型：
--
作者：
Shimaguchi Aika;Nobukawa Kumiko K;Yamauchi Shigeo;Nobukawa Masayoshi;Fujita Yutaka
在本文中，我们研究了超新星遗迹 W 51 C 中的 Fe K 壳线和附近的硬 X 射线源。我们分别测量了6.40 keV和6.68 keV处的FeiKα和FexxvHeα线的强度，发现6.68 keV线的强度与先前研究预期的背景水平一致，而6.40 keV线的强度在2.0σ的显着性水平上更高。鉴于伽马射线发射的存在以及与残余物在空间上重合的高电离率点，我们得出结论，增强的 6.40 keV 线很可能源自低能宇宙射线和分子云之间的相互作用。此外，我们发现紧凑 Hiiregion G49.0−0.3 的 6.68 keV 线发射增强，显着性水平为 3.4σ。光谱分析表明，6.68 keV 线的热等离子体的温度和丰度分别为 keV 和 Z= 0.5 ± 0.2 太阳。这些值可以通过 O 型恒星的星风产生的热等离子体来解释。
In this paper, we investigate the Fe K-shell lines in the supernova remnant W 51 C and hard X-ray sources in the proximity. We measure the intensities of the FeiKα and FexxvHeα lines at 6.40 and 6.68 keV, respectively, and find that the intensity of the 6.68 keV line is consistent with the background level expected from previous studies, while that of the 6.40 keV line is higher at the significance level of 2.0σ. Given the presence of gamma-ray emission and high ionization rate point spatially coincident with the remnant, we conclude that the enhanced 6.40 keV line most likely originates from the interaction between low-energy cosmic rays and molecular clouds. Also, we discover an enhanced 6.68 keV line emission from the compact Hiiregion G49.0−0.3 at a significance level of 3.4σ. Spectral analysis reveals that the temperature and abundance of the thermal plasma with the 6.68 keV line iskeV andZ= 0.5 ± 0.2 solar, respectively. These values are explained by the thermal plasma generated by the stellar winds of O stars.