论文标题
目录为220偏移和双重AGN：主要合并和分离以下4 kpc的AGN激活增加
A Catalog of 220 Offset and Dual AGNs: Increased AGN Activation in Major Mergers and Separations under 4 kpc
论文作者
论文摘要
在银河合并期间，气体和灰尘被驱动到合并星系的中心，触发增强的恒星形成和超级质量黑洞（SMBH）的生长。理论预测，这种增强的活动在SMBH分离处达到峰值$ <$ 20 kpc；如果在此阶段有足够的材料积聚在一个或两个SMBH上，以使它们成为活性银河核（AGN），它们分别被称为偏移和双AGN。为了更好地研究这些系统，我们已经构建了ACS-AGN合并目录，这是一个均匀选择的大量目录（$ n = 220 $），由$ \ textit {hst} $观察到$ 0.2 <z <2.5 $，分离$ <$ <$ 20 kpc。使用此目录，我们回答了许多有关SMBH的问题 - 合并期间的星系共同进化。首先，我们确认AGN分数在SMBH对分离$ <$ <$ 10 kpc;具体而言，我们发现该分数在$ 4 kpc的一对分离时大大增加。其次，我们发现合并中的AGN在主要合并中优先发现，并且合并中发现的AGN的比例遵循对数关系，随着合并质量比的增加而降低。第三，我们没有发现合并（也不是主要或次要合并亚群）触发最发光的AGN。最后，我们发现核柱密度，AGN光度和宿主星系星形成速率在这些系统中不依赖于SMBH对分离或合并质量比，这些值的分布也与总体AGN总体的分布没有显着差异。
During galaxy mergers, gas and dust is driven towards the centers of merging galaxies, triggering enhanced star formation and supermassive black hole (SMBH) growth. Theory predicts that this heightened activity peaks at SMBH separations $<$20 kpc; if sufficient material accretes onto one or both of the SMBHs for them to become observable as active galactic nuclei (AGNs) during this phase, they are known as offset and dual AGNs, respectively. To better study these systems, we have built the ACS-AGN Merger Catalog, a large catalog ($N=220$) of uniformly selected offset and dual AGN observed by $\textit{HST}$ at $0.2<z<2.5$ with separations $<$20 kpc. Using this catalog, we answer many questions regarding SMBH -- galaxy coevolution during mergers. First, we confirm predictions that the AGN fraction peaks at SMBH pair separations $<$10 kpc; specifically, we find that the fraction increases significantly at pair separations of $<$4 kpc. Second, we find that AGNs in mergers are preferentially found in major mergers and that the fraction of AGNs found in mergers follows a logarithmic relation, decreasing as merger mass ratio increases. Third, we do not find that mergers (nor the major or minor merger subpopulations) trigger the most luminous AGNs. Finally, we find that nuclear column density, AGN luminosity, and host galaxy star formation rate have no dependence on SMBH pair separation or merger mass ratio in these systems, nor do the distributions of these values differ significantly from that of the overall AGN population.
