XXL-HSC: Host properties of X-ray detected AGNs in XXL clusters
E. Drigga, E. Koulouridis, E. Pouliasis, Y. Toba, M. Akiyama, C. Vignali, A. Ruiz, I. Georgantopoulos, T. Nagao, S. Paltani, M. Plionis, M. Pierre, B. Vijarnwannaluk
There is compelling evidence that AGNs are strongly influenced by their environment. Therefore, studying the AGN population of clusters is essential, as both large-scale structures and AGN play key roles in galaxy evolution, though the interactions between these elements are still not well understood. The primary objective of this study is to unravel the different factors that may significantly affect the triggering of AGN activity in cluster galaxies, including galaxy merging and interactions with other galaxies, and ram pressure from the hot intracluster medium. For our purposes, we used 82 X-ray detected AGN found within a $4r_{500}$ radius of 164 X-ray detected and spectroscopically confirmed galaxy clusters of the XXL survey, up to a redshift of $z\sim$1. This field is covered by deep optical observations of the Hyper Suprime-Cam, which allows for a reliable morphological classification of galaxies. Furthermore, using the X-ray hardness ratio, the optical spectra and the SEDs of the X-ray sources, we have studied the obscuration and other AGN properties and the SFR of the hosts as further indicators of interactions. We found a moderately significant higher fraction of X-ray AGN in galaxy clusters hosted by merging or disturbed galaxies, compared to non-active cluster galaxies or X-ray AGN in the field. This excess is primarily localised in the cluster outskirts. Also, we discovered a higher number of X-ray-hard AGN (hence, possibly obscured) in clusters than in the field particularly in the outskirts. These findings further support the idea that galaxy mergers and interactions may serve as mechanisms for the triggering and obscuration of AGN activity. The relatively high number of disturbed, merging, and possibly obscured AGN hosts in cluster outskirts suggests that galaxy merging and interactions are key drivers in triggering AGN activity in these outer regions of clusters.
XXL-HSC: An updated catalogue of high-redshift ($z\geqslant3.5$) X-ray AGN in the XMM-XXL northern field. Constraints on the bright end of the soft logN-logS
The XXL survey XXXV. The role of cluster mass in AGN activity
本文介绍了XXL巡天中167个真正的X射线星系团（$0.1<z<0.5$）中活动星系核密度的研究结果。这些结果可以为驱动活动星系核和星系团演化的物理机制提供证据。XXL簇样品主要包括贫和中等富结构（$M=10^{13} - 4\times10^{14} M_{\rm o}$）。我们的目的是统计研究集群AGN的人口统计作为集群质量和宿主星系位置的函数。为了研究环境对活动星系核活动的影响，我们计算了光谱学证实的活动星系核（$L_{\rm X [0.5-10\,keV]}>10^{42}$ erg cm $^{-1}$）在明亮星系团中的比例，直到$6r_{500}$半径。为了研究活动星系核总体的质量依赖性和演化，我们进一步将样本分为低质量和高质量星系团以及两个红移仓（0.1-0.28和0.28-0.5）。在95%的置信水平下，我们在$0.5r_{500}$和2个$r_{500}$之间的低质量星系团中检测到显著过量的X射线活动星系核，其下降到星系团核心（$r<0.5r_{500}$）内的场值。与此相反，高质量的集群呈现出一个减少AGN的分数对集群中心。外围的活动星系核的高部分是由低光度活动星系核引起的。这可以解释为低质量星系团的星系合并率较高，其中速度色散不足以阻止星系相互作用和合并。在我们所有星系团的核心都有可能发生冲压压力剥离，但在更深的引力势中可能更强。与以往对大质量或高红移星系团的…
Peking University（北京大学）；Heidelberg University（海德堡大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；University of Illinois Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）
Great Optically Luminous Dropout Research Using Subaru HSC (GOLDRUSH). I. UV Luminosity Functions at $z \sim 4-7$ Derived with the Half-Million Dropouts on the 100 deg$^2$ Sky
The XXL survey LII : The evolution of radio AGN luminosity function determined via parametric methods from GMRT, ATCA, VLA and Cambridge interferometer observations
DAVOS: Dwarf Active Galactic Nuclei from Variability for the Origins of Seeds: Properties of Variability-Selected Active Galactic Nuclei in the COSMOS Field and Expectations for the Rubin Observatory
Empirical Near-Infrared Spectral Templates from SPHEREx: Disentangling AGN and Host-Galaxy Emission
Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；University of Science and Technology of China（中国科学技术大学）；Guizhou University（贵州大学）
Concordance between observations and simulations in the evolution of the mass relation between supermassive black holes and their host galaxies
我们在$0.2<z<1.7$使用匹配良好的观测和多个最先进的模拟（例如，Massive Black II、Horizon-AGN、Illustris、TNG和半解析模型）。观测样本由646个均匀选择的SDSS类星体（$0.2 < z < 0.8$）和32个宽线活动星系核（AGN; $1.2<z<1.7$）组成，前者由超级超级凸轮（HSC）成像，后者由哈勃太空望远镜（HST）成像。我们首先将现实的观测不确定性添加到模拟数据中，然后以与观测相同的方式构建模拟样本。在整个红移范围内，我们的分析表明，所有的模拟预测的内在散射的标度关系的水平相媲美的观察似乎同意分散的本地关系。在平均关系方面，Horizon-AGN和TNG在低和高红移（分别为$z\sim$ 0.2和1.5）下与观测结果最接近，而其他模拟在不确定性范围内显示出细微的差异。为了深入了解所涉及的物理学，在SAM中看到的标度关系的分散性在采用考虑活动星系核外流几何形状的新反馈模型后减少了两倍，并且更接近观测结果。在我们的分析中，色散与红移的一致性支持了模拟中类星体和无线电模式反馈处方的重要性。最后，我们强调提高灵敏度的重要性（例如，使用詹姆斯韦伯太空望远镜），从而推动更低的质量和最小化由于选择效应造成的偏差。
Using Machine Learning to Determine Morphologies of $z<1$ AGN Host Galaxies in the Hyper Suprime-Cam Wide Survey
Yale University（耶鲁大学）；Dartmouth College（达特茅斯学院）；University of Hawaii（夏威夷大学）；University of Miami（迈阿密大学）；INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚天体物理与空间科学天文台）；Stanford University（斯坦福大学）；Modulos AG（Modulos公司）
