Reflectivity around the gold M-edges of x-ray reflector of the Soft X-ray Telescope onboard ASTRO-H
Reflectivity around the gold M-edges of x-ray reflector of the Soft X-ray Telescope onboard ASTRO-H
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ASTRO-H 软 X 射线望远镜 X 射线反射镜金色 M 边缘周围的反射率
DOI：
10.1117/12.2231173
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发表时间：
2016
期刊：
影响因子：
--
通讯作者：
Sho et al.
中科院分区：
文献类型：
--
作者：
Kurashima;Sho et al.
X射线天文学卫星ASTRO-H配备了两个等效的软X射线望远镜（SXT-I和SXT-S），覆盖0.3{12 keV的能带。SXT的X射线反射器通过复制技术（Okajima等人在本卷中）涂有金单层。在2-4 keV波段的一系列金M吸收边导致SXT的能量响应中的复杂结构。在同一条谱带中，Si、Ar和S的发射谱线具有重要的天体物理意义。由于SXS具有前所未有的高光谱分辨率，我们在同步辐射装置KEK PF BL 11-B上以非常精细的能量间距测量了金M边周围的反射率，其中2100 eV至4100 eV带中的2 eV间距覆盖了整个吸收边系列（M-I至M-V），与反射器的掠入射角为0.5、0.8、1.0、1.2、1.4度，并且在2200 eV至2350 eV带中具有0.25 eV的更精细间距，其中包括两个最深的M-IV和M-V边缘。在所得的反射率曲线，我们已经清楚地确定了与所有的M-边缘的精细结构。利用这些数据，我们计算了原子散射因子f1作为X射线能量的函数，我们已经建立了可以应用于朱雀光谱的镜响应函数。结果发现，与朱雀星云4U 1630 -472（一个黑洞瞬变）和蟹状星云M边附近的数据相比，谱模型与朱雀星云官方响应的差异显著减小。
The X-ray astronomy satellite ASTRO-H are equipped with two equivalent soft X-ray telescopes (SXT-I and SXT-S) which cover the energy band 0.3{12 keV. The X-ray reflectors of the SXTs are coated with a gold monolayer by means of the replication technique (Okajima et al. in this volume). A series of gold M absorption edges in the 2-4 keV band causes complex structures in the energy response of the SXTs. In the same band, there are astrophysically important emission lines from Si, Ar and S. Since the SXS has unprecedentedly high spectral resolution, we have measured the reflectivity around the gold M-edges in an extremely fine energy pitch at the synchrotron radiation facility KEK PF BL11-B, with the 2 eV pitch in 2100 eV to 4100 eV band that covers the entire series of the absorption edges (M-I through M-V) at grazing incident angles to the reflectors of 0.5, 0.8, 1.0, 1.2, 1.4 degree, and with a finer pitch of 0.25 eV in the 2200 eV to 2350 eV band where the two deepest M-IV and M-V edges are included. In the resultant reflectivity curves, we have clearly identified the fine structures associated with all the M-edges. Using these data, we calculated atomic scattering factor f1 as a function of X-ray energy, with which we have built the mirror response function which can be applied to the Suzaku spectra. As a result, we have found that discrepancy of the spectral model to the Suzaku data of 4U1630-472 (a black hole transient) and the Crab nebula around the M-edges are significantly reduced from those with the official Suzaku response.