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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Measurements of resonant scattering in the Perseus Cluster core with Hitomi SXS
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Measurements of resonant scattering in the Perseus Cluster core with Hitomi SXS

机译：用Hitomi SXS测量Perseus团簇核中的共振散射

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Thanks to its high spectral resolution (～5?eV at 6?keV), the Soft X-ray Spectrometer (SXS) on board Hitomi enables us to measure the detailed structure of spatially resolved emission lines from highly ionized ions in galaxy clusters for the first time. In this series of papers, using the SXS we have measured the velocities of gas motions, metallicities and the multi-temperature structure of the gas in the core of the Perseus Cluster. Here, we show that when inferring physical properties from line emissivities in systems like Perseus, the resonant scattering effect should be taken into account. In the Hitomi waveband, resonant scattering mostly affects the Fe?xxv Heα line (w)—the strongest line in the spectrum. The flux measured by Hitomi in this line is suppressed by a factor of ～1.3 in the inner ～30?kpc, compared to predictions for an optically thin plasma; the suppression decreases with the distance from the center. The w line also appears slightly broader than other lines from the same ion. The observed distortions of the w line flux, shape, and distance dependence are all consistent with the expected effect of the resonant scattering in the Perseus core. By measuring the ratio of fluxes in optically thick (w) and thin (Fe?xxv forbidden, Heβ, Lyα) lines, and comparing these ratios with predictions from Monte Carlo radiative transfer simulations, the velocities of gas motions have been obtained. The results are consistent with the direct measurements of gas velocities from line broadening described elsewhere in this series, although the systematic and statistical uncertainties remain significant. Further improvements in the predictions of line emissivities in plasma models, and deeper observations with future X-ray missions offering similar or better capabilities to the Hitomi SXS, will enable resonant scattering measurements to provide powerful constraints on the amplitude and anisotropy of cluster gas motions.
机译：由于具有高光谱分辨率（在6？keV时约为5？eV），Hitomi板上的软X射线光谱仪（SXS）使我们能够测量星系团中高电离离子的空间分辨发射线的详细结构。第一次。在这一系列论文中，我们使用SXS测量了珀尔修斯星团核心中气体运动的速度，金属性和气体的多温度结构。在这里，我们表明，当从像Perseus这样的系统中的线发射率推断物理性质时，应考虑共振散射效应。在Hitomi波段中，共振散射主要影响Fe？xxvHeα线（w），即光谱中最强的线。与光学薄等离子体的预测值相比，Hitomi在这条线上测得的通量在内部〜30？kpc处被抑制了约1.3倍。抑制随着距中心的距离而减小。 w线也比相同离子的其他线略宽。 w线通量，形状和距离相关性的观察到的扭曲都与英仙座核中共振散射的预期效果一致。通过测量光学粗线（w）和细线（禁止Fe 2 x xx，Heβ，Lyα）中的通量比，并将这些比值与蒙特卡洛辐射转移模拟的预测值进行比较，可以获得气体运动的速度。尽管系统和统计上的不确定性仍然很明显，但该结果与本系列其他地方描述的通过线展宽直接测量气体速度是一致的。等离子体模型中线发射率的预测的进一步改进以及对未来X射线任务提供与Hitomi SXS相似或更好功能的更深入的观察，将使共振散射测量能够对团簇气体运动的幅度和各向异性提供强大的约束。

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