AI 中文总结
该研究通过VLT/MUSE数据对12个近邻AGN对候选体开展电离气体空间分辨分析，揭示其电离特性、运动学特征及AGN活动衰减证据，为理解星系并合与AGN的相互作用提供观测依据。
AI 中文摘要
研究AGN对及其宿主星系对于理解星系并合与超大质量黑洞吸积、反馈等关键内部过程的相互作用至关重要。我们将Big Multi-AGN Catalog（The Big MAC）与甚大望远镜（VLT）的多单元光谱探测器（MUSE）公共数据档案交叉匹配，得到12个近邻宇宙（红移z≲0.1）中的AGN对候选体，其投影距离r_p≤20千秒差距（kpc）。利用存档的VLT/MUSE数据，我们对这12个AGN对候选体开展电离气体运动学与电离特性的空间分辨研究。我们将光学发射线分解为两个高斯分量，尝试区分与星系盘旋转相关的气体和非圆周运动气体，还利用空间分辨的BPT诊断法识别主导电离机制。研究发现，12个系统中有4个的两个核均归类为赛弗特星系（Seyfert）或低电离核发射线区（LINER）；另有3个核在光学诊断中归类为恒星形成区或复合区，但在其他波段被识别为AGN。运动学方面，24个核中有16个检测到规则旋转的电离气体盘，9个系统检测到由电离气体示踪的明显潮汐特征，18个核普遍存在电离气体外流。最后，基于光学发射线比值和假设的AGN光电离模型，我们发现3个核（Mrk 739A、NGC 7592B和J1544+0446A）在过去数万年（10^4年）内存在AGN活动衰减的证据。
英文摘要
Studying AGN pairs and their host galaxies is essential for understanding the interplay between galaxy mergers and key internal processes such as supermassive black hole fueling and feedback. We cross-match between the Big Multi-AGN Catalog (The Big MAC) and the public data archive of the VLT/MUSE, and obtain 12 AGN pair candidates in the local universe ($z\lesssim0.1$) with a projected distance $r_{\rm p}\leq 20\rm\,kpc$. Using the archival VLT/MUSE data, we present a spatially resolved study of the ionized gas kinematics and ionization properties of these 12 AGN pair candidates. By decomposing the optical emission lines into two Gaussian components, we try to separate gas associated with disk rotation from non-circular motions. We further identify dominant ionization mechanisms using spatially resolved BPT diagnostics. We find that both nuclei in 4 of the 12 systems are classified as Seyfert or LINER. In addition, three nuclei are classified as star-forming or composite in the optical diagnostics, but are identified as AGNs at other wavelengths. Kinematically, regularly rotating ionized gas disks are detected in 16 of 24 nuclei. Prominent tidal features traced by ionized gas are also detected in 9 systems. Ionized gas outflows are widespread and are detected in 18 nuclei. Finally, for three nuclei (Mrk 739A, NGC 7592B, and J1544+0446A), we find evidence for fading AGN activity over the past several $10^{4}\rm\, yr$, based on optical emission-line ratios and an assumed AGN photoionization model.
Comments20+15 pages, 5+11 figures, 5+1 tables, accepted for publication in ApJS
