X-ray spectra of galaxy clusters are dominated by the thermal emission from the hot intracluster medium. In some cases, besides the thermal component, spectral models require additional components associated, e.g., with resonant scattering and charge exchange. The latter produces mostly underluminous fine spectral features. Detection of the extra components therefore requires high spectral resolution. The upcoming X-ray missions will provide such high resolution, and will allow spectroscopic diagnostics of clusters beyond the current simple thermal modeling. A representative science case is resonant scattering, which produces spectral distortions of the emission lines from the dominant thermal component. Accounting for the resonant scattering is essential for accurate abundance and gas motion measurements of the ICM. The high resolution spectroscopy might also reveal/corroborate a number of new spectral components, including the excitation by non-thermal electrons, the deviation from ionization equilibrium, and charge exchange from surface of cold gas clouds in clusters. Apart from detecting new features, future high resolution spectroscopy will also enable a much better measurement of the thermal component. Accurate atomic database and appropriate modeling of the thermal spectrum are therefore needed for interpreting the data.
Resonant scattering at the center of the galaxy cluster PKS 0745-191 with XRISM
Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA)（日本宇宙航空研究开发机构宇宙科学研究所）；Department of Astronomy, Graduate School of Science, The University of Tokyo（东京大学理学研究科天文学专攻）；Lawrence Livermore National Laboratory（劳伦斯利弗莫尔国家实验室）；SRON Netherlands Institute for Space Research（荷兰空间研究研究所）；Faculty of Physics, Tokyo University of Science（东京理科大学理学部）；Department of Physics & Astronomy, Waterloo Centre for Astrophysics, University of Waterloo（滑铁卢大学天体物理中心物理与天文系）；NASA / Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）；IRAP, CNRS, Université de Toulouse, CNES, UT3-UPS（图卢兹大学/法国国家科学研究中心/法国国家空间研究中心天体物理与行星学研究所）；Department of Astronomy, University of Maryland（马里兰大学天文学系）
GEMINI 3D spectroscopy of BAL+IR+Fe II QSOs: II. IRAS 04505-2958 an explosive QSO with hypershell and a new scenario for galaxy formation and galaxy end
从BAL + IR + Fe II类星体的研究（使用深双子座GMOS-IFU光谱）的新结果：红外天文台04505-2958。具体来说，我们详细研究了外流（OF）过程及其相关结构，主要是在两个大星系尺度：（i）两个斑点/壳（S1，S2）在半径r = 1.1和2.2 kpc的;（ii）外部超巨星壳（S3）在r = 11 kpc。此外，还讨论了在r = 80 kpc时两个非常扩展的超巨星壳层（S4，S5）的存在.从GMOS研究中获得了以下主要结果：（i）对于外部超巨星壳层S3，电离气体的运动学GMOS图显示出与在NGC 5514中观察到的爆炸外部超巨星壳层原型非常相似的特征。(ii)这个超巨星壳层S3-的主要节点K1、K2和K3 -显示了与星暴+ OF/激波存在相关的恒星星族和发射线比率。(iii)内壳层S1和S2的结构、OF成分和性质与Mrk 231核壳层中检测到的非常相似。(iv)壳层S1+S2和S3在PA = 131处对齐：即表明OF过程处于具有双极结构的吹出阶段。此外，壳体S4和S5（80-100 kpc尺度）在PA = 40时对齐，即：垂直于内部OF的双极OF。最后讨论了BAL + IR + Fe II类星体中与HyNe有关的UHE宇宙射线和中微子/暗物质的产生。
High-resolution X-ray spectroscopy of the low and high states of the Seyfert 1 galaxy NGC 4051 with Chandra LETGS
方法.本文分析了Chandra低能透射光栅光谱仪的两个观测结果。我们研究了光谱响应突然通量减少的一个因素，这发生在第二次观察。结果我们检测到一个高度电离的吸收组件的流出速度为-4670公里/秒，在塞弗特1星系中观察到的最高流出速度的组件之一。该光谱包含一个相对论O VIII Ly α线，和四个吸收组件跨越范围的电离参数XI在0.07和3.19之间。在低态出现了产生CVI和CV辐射复合连续谱的发射分量。黑体温度随着第二次观测中观测到的通量的下降而下降。结论.对于所有的吸收器组件，我们排除了电离参数线性响应通量的减少了5倍。吸收体的可变性表明，四个检测到的组分中至少有三个位于0.02-1 pc的范围内。删节
