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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >An X-ray spectroscopic study of the hot interstellar medium toward the galactic bulge
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An X-ray spectroscopic study of the hot interstellar medium toward the galactic bulge

机译：星际热介质向银河凸起的X射线光谱研究

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摘要

We present a detailed spectroscopic study of the hot gas toward the galactic bulge along the 4U 1820-303 sight line by a combination analysis of emission and absorption spectra. In addition to the absorption lines of OVII Kα, OVII Kβ, OVIII Kα, and NeIX Kα by Chandra LTGS, as shown by previous studies, Suzaku clearly detected the emission lines of OVII, OVIII, NeIX, and NeX from the vicinity. We used simplified plasma models with constant temperature and density. An evaluation of the background and foreground emission was carefully performed, including the stellar X-ray contribution based on the recent X-ray observational results and the stellar distribution simulator. If we assume that one plasma component exists in front of 4U 1820-303 and the other one at the back, the obtained temperatures are T = (1.7±0.2) × 10 ~6 K for the front-side plasma and T = (3.9 _(-0.3)~(+0.4)) × 10 ~6 K for the back-side. This scheme is consistent with a hot and thick ISM disk, as suggested by extragalactic source observations and an X-ray bulge around the galactic center.
机译：我们通过发射和吸收光谱的组合分析，对沿4U 1820-303视线朝向银河凸起的热气体进行了详细的光谱学研究。如先前的研究所示，除了钱德拉·LTGS的OVIIKα，OVIIKβ，OVIIIKα和NeIXKα的吸收线外，朱雀还清晰地从附近检测到OVII，OVIII，NeIX和NeX的发射线。我们使用具有恒定温度和密度的简化等离子体模型。仔细进行了背景和前景发射的评估，包括基于最新X射线观测结果和恒星分布模拟器的恒星X射线贡献。如果我们假设一个等离子体成分存在于4U 1820-303的前面，而另一个位于背面，则对于正面等离子体，获得的温度为T =（1.7±0.2）×10〜6 K，T =（3.9背面为_（-0.3）〜（+0.4））×10〜6K。如银河外源观测和银河中心周围的X射线凸起所表明的，该方案与一个热而厚的ISM盘一致。

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