朱雀卫星观测的Sgr B分子云的X射线正面图
An X-Ray Face-on View of the Sgr B Molecular Clouds Observed with Suzaku
摘要：
作为银河系中心漫射X射线（GCDX）的应用研究，我们提出了一种新的方法来推导Sgr B分子云（MC）沿视线的位置。GCDX是由约7 keV和1 keV的温度的热等离子体发射，和非热连续辐射，包括6.4 keV线从中性铁。前者是银河系中心等离子体发射（GCPE），在经度上均匀分布，而后者是汤姆逊散射和MCs在外部X射线照射下产生的荧光（X射线反射星云发射：XRNE）。我们检查了靠近Sgr B MC络合物的GCPE和XRNE的Suzaku X射线光谱，发现光谱具有两个不同的吸收峰，N_H（Abs 1）>10^23 H cm^-2和N_H（Abs 2）~6 x 10^22 H cm^-2。Abs 1正比于6.4 keV的线通量，因此是由于MC，而Abs 2是典型的星际吸收朝向银河系中心。假设GCPE等离子体在Sgr A* 周围呈球形扩展，具有均匀的密度和相同的两个温度分量的角分布，我们从Abs 1和没有Abs 1时GCPE谱的通量比定量估计了MCs的视线位置。结果表明，在GCPE中，Sgr B MCs位于Sgr A* 的近侧。
英文摘要：
We present a new methodology to derive the positions of the Sgr B molecular clouds (MCs) along the line of sight, as an application study of the Galactic center diffuse X-rays (GCDX). The GCDX is composed of hot plasma emission of about 7 keV and 1 keV temperatures, and non-thermal continuum emission including the 6.4 keV line from neutral irons. The former, the Galactic center plasma emission (GCPE), is uniformly distributed over 1 degree in longitude, while the latter is clumpy emission produced by Thomson scattering and fluorescence from MCs irradiated by external X-rays (the X-ray reflection nebula emission: XRNE). We examined the Suzaku X-ray spectra of the GCPE and XRNE near to the Sgr B MC complex, and found that the spectra suffer from two different absorptions of N_H (Abs1) >10^23 H cm^-2 and N_H (Abs2) ~6 x 10^22 H cm^-2. Abs1 is proportional to the 6.4 keV-line flux, and hence is due to the MCs, while Abs2 is typical of interstellar absorption toward the Galactic center. Assuming that the GCPE plasma is spherically-extended around Sgr A* with a uniform density and the same angular distribution of the two temperature components, we quantitatively estimated the line-of-sight positions of the MCs from the flux ratio the GCPE spectrum suffered by Abs1 and that with no Abs1. The results suggest that the Sgr B MCs are located at the near side of Sgr A* in the GCPE.
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