Uniform Distribution of the Extremely Overionized Plasma Associated with the Supernova Remnant G359.1-0.5
Uniform Distribution of the Extremely Overionized Plasma Associated with the Supernova Remnant G359.1-0.5
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DOI：
10.3847/1538-4357/ab80ba
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发表时间：
2020-03
期刊：
影响因子：
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通讯作者：
Hiromasa Suzuki;A. Bamba;R. Enokiya;H. Yamaguchi;P. Plucinsky;H. Odaka
中科院分区：
文献类型：
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作者：
Hiromasa Suzuki;A. Bamba;R. Enokiya;H. Yamaguchi;P. Plucinsky;H. Odaka
我们报告了我们对超新星遗迹（SNR）G359.1−0.5的特殊重组等离子体和相互作用的CO云的详细分析结果。结合钱德拉和朱雀的数据，我们估计电离状态的等离子体的背景光谱的仔细处理。平均光谱显示出电子温度（约0.17 keV）与初始温度（>16 keV）的显著大偏差，表明等离子体处于高度复合主导状态。另一方面，重组时间尺度（净）与其他重组SNR相当（约4.2 × 1011 cm−3 s）。我们还搜索了等离子体参数的空间变化，但没有发现显著差异。利用NANTEN 2获得的12 CO（J = 2-1）数据，我们发现了一个新的、合理的相互作用CO云候选者，其视线速度为1.20 km s-1。这表明SNR位于1.4kpc的距离，这是银河系中心的前景，正如以前报道的那样。相关的CO云与附近的GeV/TeV辐射没有明显的空间重合，这表明GeV/TeV辐射的起源可能与G359.1−0.5无关。
We report on the results of our detailed analyses on the peculiar recombining plasma of the supernova remnant (SNR) G359.1−0.5, and the interacting CO clouds. Combining Chandra and Suzaku data, we estimated the ionization state of the plasma with a careful treatment of the background spectrum. The average spectrum showed a remarkably large deviation of the electron temperature (∼0.17 keV) from the initial temperature (>16 keV), indicating that the plasma is in a highly recombination-dominant state. On the other hand, the recombination timescale (net) is comparable to those of the other recombining SNRs (∼4.2 × 1011 cm−3 s). We also searched for spatial variation of the plasma parameters, but found no significant differences. Using 12CO(J = 2–1) data obtained with NANTEN2, we found a new, plausible candidate for the interacting CO cloud, which has a line-of-sight velocity of ∼ −20 km s−1. This indicates that the SNR is located at a distance of ∼4 kpc, which is the foreground of the Galactic center, as previously reported. The associated CO cloud does not show clear spatial coincidence with the nearby GeV/TeV emission, indicating that the origins of the GeV/TeV emission are likely unrelated to G359.1−0.5.