We report spatial distributions of the Fe-K$\alpha$ line at 6.4 keV and the CO($J$ = 2--1) line at 230.538 GHz in NGC 2110, which are respectively revealed by $Chandra$ and ALMA at $\approx$ 0.5 arcsec. A $Chandra$ 6.2--6.5 keV-to-3.0--6.0 keV image suggests that the Fe-K$\alpha$ emission extends preferentially in a northwest-to-southeast direction out to $\sim$ 3 arcsec, or 500 pc, on each side. Spatially-resolved spectral analyses support this by finding significant Fe-K$\alpha$ emission lines only in northwest and southeast regions. Moreover, their equivalent widths are found $\sim$ 1.5 keV, indicative for the fluorescence by nuclear X-ray irradiation as the physical origin. By contrast, CO($J$ = 2--1) emission is weak therein. For quantitative discussion, we derive ionization parameters by following an X-ray dominated region (XDR) model. We then find them high enough to interpret the weakness as the result of X-ray dissociation of CO and/or H$_2$. Another possibility also remains that CO molecules follow a super-thermal distribution, resulting in brighter emission in higher-$J$ lines. Further follow-up observations are encouraged to draw a conclusion on what predominantly changes the inter-stellar matter properties, and whether the X-ray irradiation eventually affects the surrounding star formation as an AGN feedback.

中文翻译：

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Chandra 和 ALMA 揭示 NGC 2110 中 CO 气体的 AGN X 射线辐照

我们报告了 NGC 2110 中 6.4 keV 的 Fe-K$\alpha$ 线和 230.538 GHz 的 CO($J$ = 2--1) 线的空间分布，分别由 $Chandra$ 和 ALMA 揭示\大约$ 0.5 弧秒。$Chandra$ 6.2--6.5 keV-to-3.0--6.0 keV 图像表明 Fe-K$\alpha$ 发射优先从西北到东南方向延伸至 $\sim$ 3 弧秒，即 500电脑，在每一边。空间分辨光谱分析通过仅在西北和东南地区发现显着的 Fe-K$\alpha$ 发射线来支持这一点。此外，发现它们的等效宽度为 $\sim$ 1.5 keV，表明核 X 射线辐射作为物理来源的荧光。相比之下，CO($J$ = 2--1) 排放在其中较弱。对于定量讨论，我们通过遵循 X 射线主导区域 (XDR) 模型推导出电离参数。然后我们发现它们足够高，可以将弱点解释为 CO 和/或 H$_2$ 的 X 射线解离结果。另一种可能性仍然是 CO 分子遵循超热分布，导致更高 $J$ 线的更亮的发射。鼓励进一步的后续观察得出结论，主要是什么改变了星际物质的性质，以及 X 射线辐射是否最终会影响周围的恒星形成作为 AGN 反馈。