九头蛇座A中的气体运动：XRISM对跨喷流膨胀腔的星系团际介质运动学的约束
Gas Motions in Hydra-A: XRISM Constraints on ICM Kinematics Across Jet-Inflated Cavities
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中文总结 AI 辅助
该研究利用XRISM观测九头蛇座A，结合空间光谱混合技术研究其大气运动学，分析了不同区域的速度弥散、动能等，发现喷流在不同尺度驱动气体运动效率不同，还观测到中央指向西南象限的整体流动。
中文摘要 AI 辅助
我们报告了对九头蛇座A的X射线大气的中部和北部区域进行的两次深度XRISM观测，这些区域覆盖了由中央星系的活动星系核（AGN）喷流膨胀形成的气泡。我们使用空间光谱混合技术，将钱德拉的高空间分辨率与XRISM的高光谱分辨率相结合，以研究大气运动学。北部区域的大气速度弥散为$\sigma_v = 140^{+30}_{-20}$ km s$^{-1}$，与中部区域（$\sigma_v = 162 \pm 10$ km s$^{-1}$）相当。我们表明，大规模茧状激波前沿的运动可能是导致向北方向较大弥散的原因。中央指向东北象限的速度弥散为$\sigma_v = 260 \pm 50$ km s$^{-1}$，是测量到的最高弥散之一。该区域包含一个先前被确定为富含金属的X射线亮特征，可能由上一代空洞尾流中上升的气体组成。所有其他象限区域的弥散较低（$\sigma_v \leq 120$ km s$^{-1}$），与之前对其他天体的XRISM结果一致。中心的动能与空洞的焓相当，而在北部，动能大约小一个数量级。因此，喷流在较小尺度（$r < 95$ kpc）上有效地驱动气体运动，而在较大尺度（沿喷流向北$95 - 317$ kpc）上效率较低。在中央指向的西南象限还观测到朝向我们视线的$-100 \pm 30$ km s$^{-1}$的整体流动，可能是由于晃动。
英文摘要
We report on two deep XRISM observations of the central and northern regions of Hydra-A's X-ray atmosphere covering the bubbles inflated by jets from the central galaxy's active galactic nucleus (AGN). We use spatial-spectral mixing that combines Chandra's high spatial resolution with XRISM's high spectral resolution to investigate atmospheric kinematics. The atmospheric velocity dispersion in the northern region, $σ_v = 140^{+30}_{-20}$ km s$^{-1}$, is comparable to that in the central region ($σ_v = 162 \pm 10$ km s$^{-1}$). We show that the motion of the large-scale cocoon shock front could be responsible for the large dispersion toward the north. The velocity dispersion in the northeast quarter of the central pointing, $σ_v = 260 \pm 50$ km s$^{-1}$, is among the highest dispersions measured. This region contains an X-ray-bright feature previously identified as metal-rich, possibly consisting of gas uplifted in the wake of previous-generation cavities. The dispersions in all other quarter regions are low ($σ_v \leq 120$ km s$^{-1}$) and consistent with previous XRISM results from other objects. The kinetic energy at the center is comparable to the enthalpies of the cavities, while in the north, it is roughly an order of magnitude smaller. The jet thus drives gas motion efficiently at smaller scales ($r < 95$ kpc) and inefficiently at larger scales ($95-317$ kpc toward the north along the jet). A bulk flow toward our line of sight of $-100 \pm 30$ km s$^{-1}$ in the southwest quarter of the central pointing is also observed, possibly due to sloshing.
