We investigate the connection between X-ray and radio-loud AGNs and the physical properties of their evolved and massive host galaxies, focussing on the mass-related quenching channel followed by $\mathcal{M}^\star (\simeq 10^{10.6} M_\odot)$ galaxies in the rest-frame NUVrK colour diagram at $0.2 10^{11}M_\odot$) galaxies, ruling out their feedback as a primary driver of $\mathcal{M}^\star$ galaxy quenching, we found that (2) X-ray AGNs affected by heavy obscuration of their soft X-ray emission are mostly hosted by $\mathcal{M}^\star$ galaxies that are in the process of quenching. This is consistent with a quenching scenario that involves mergers of (gas-poor) $\mathcal{M}^\star$ galaxies $after$ the onset of the quenching process, i.e., a scenario where $\mathcal{M}^\star$ galaxy mergers are not the cause but rather an aftermath of the quenching mechanism(s). In that respect, we discuss how our results may support a picture where the slow quenching of $\mathcal{M}^\star$ galaxies happens due to halo-halo mergers along cosmic filaments.

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关于 M* 星系的缓慢淬灭：严重模糊的 AGN 使图片变得清晰

我们研究了 X 射线和无线电响度 AGN 之间的联系及其演化和巨大宿主星系的物理特性，重点关注与质量相关的淬灭通道，然后是 $\mathcal{M}^\star (\simeq 10^{ 10.6} M_\odot)$ 星系在静止帧 NUVrK 颜色图中 $0.2 10^{11}M_\odot$) 星系，排除它们的反馈作为 $\mathcal{M}^\star$ 星系的主要驱动力在淬灭过程中，我们发现（2）X 射线 AGN 受其软 X 射线发射的严重遮挡影响，主要由处于淬灭过程中的 $\mathcal{M}^\star$ 星系承载。这与涉及（贫气）$\mathcal{M}^\star$ 星系在淬灭过程开始后$ 合并的淬灭情景一致，即，$\mathcal{M}^\star$ 星系合并不是原因，而是淬灭机制的后果。在这方面，我们讨论了我们的结果如何支持 $\mathcal{M}^\star$ 星系的缓慢淬灭是由于沿着宇宙细丝的晕晕合并而发生的图片。