The bulk of the black hole growth since z~1 occurs in a secular universe: No major merger-AGN connection
Mauricio Cisternas, Knud Jahnke, Katherine J. Inskip, Jeyhan Kartaltepe, Anton M. Koekemoer, Thorsten Lisker, Aday R. Robaina, Marco Scodeggio, Kartik Sheth, Jo… 展开作者
Mauricio Cisternas, Knud Jahnke, Katherine J. Inskip, Jeyhan Kartaltepe, Anton M. Koekemoer, Thorsten Lisker, Aday R. Robaina, Marco Scodeggio, Kartik Sheth, Jonathan R. Trump, Rene Andrae, Takamitsu Miyaji, Elisabeta Lusso, Marcella Brusa, Peter Capak, Nico Cappelluti, Francesca Civano, Olivier Ilbert, Chris D. Impey, Alexie Leauthaud, Simon J. Lilly, Mara Salvato, Nick Z. Scoville, Yoshi Taniguchi
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15 pages, 9 figures, accepted for publication in ApJ
What is the relevance of major mergers and interactions as triggering mechanisms for active galactic nuclei (AGN) activity? To answer this longstanding question, we analyze 140 XMM-selected AGN host galaxies and a matched control sample of 1264 inactive galaxies over z~0.3-1.0 and log(M_*/M_sun)<11.7 with high-resolution HST/ACS imaging from the COSMOS field. The visual analysis of their morphologies by 10 independent human classifiers yields a measure of the fraction of distorted morphologies in the AGN and control samples, i.e. quantifying the signature of recent mergers which might potentially be responsible for fueling/triggering the AGN. We find that (1) the vast majority (>85%) of the AGN host galaxies do not show strong distortions, and (2) there is no significant difference in the distortion fractions between active and inactive galaxies. Our findings provide the best direct evidence that, since z~1, the bulk of black hole accretion has not been triggered by major galaxy mergers, therefore arguing that the alternative mechanisms, i.e., secular processes and minor interactions, are the leading triggers for the episodes of major black hole growth. We also exclude an alternative interpretation of our results: a significant time lag between merging and the observability of the AGN phase could wash out the most significant merging signatures, explaining the lack of enhancement of strong distortions on the AGN hosts. We show that this alternative scenario is unlikely due to: (1) recent major mergers being ruled out for the majority of sources due to the high fraction of disk-hosted AGN, (2) the lack of a significant X-ray signal in merging inactive galaxies as a signature of a potential buried AGN, and (3) the low levels of soft X-ray obscuration for AGN hosted by interacting galaxies, in contrast to model predictions.
Evolution along the sequence of S0 Hubble types induced by dry minor mergers. II - Bulge-disk coupling in the photometric relations through merger-induced internal secular evolution
Recoiling Black Holes in Merging Galaxies: Relationship to AGN Lifetimes and Merger Remnant Properties
中心超大质量黑洞（SMBH）是局部观测星系的普遍特征，大量证据表明SMBH及其宿主星系的生长密切相关。然而，在合并的情况下，引力波（GW）的反冲可能会将SMBH从银河系中心移开，或者将其完全弹出。为了探索这种现象的后果，我们使用气体星系合并，包括一系列BH反冲速度的流体动力学模拟。我们已经生成了一套超过200个模拟与超过60个合并模型，使我们能够识别反冲BH的行为的系统趋势-特别是（i）他们的动态，（ii）他们的可观察到的签名，（iii）他们对BH/星系共同进化的影响。(i)反冲BH轨迹在很大程度上取决于宿主星系的气体含量; BH距中心的最大位移可能在富含气体和缺乏气体的合并之间变化高达一个数量级。在某些情况下，反冲轨道还取决于BH合并相对于星系合并残余形成的时间。(ii)通过运动学偏移量（v> 800 km s ^-1）或空间偏移量（R> 1 kpc），可以观测到存在于1~1亿年寿命的活动星系核（AGN）。此外，反冲事件影响活动星系核的总寿命。GW反冲一般会减少明亮活动星系核的寿命，但可能会延长低光度活动星系核的寿命。(iii)快速反冲的黑洞的质量可能比静止的黑洞小5倍。这些质量缺陷降低了M-σ关系的归一化，并有助于内在和整体散射。此外，反冲事件取代了来自星系中心的AGN反馈，这提高了中心恒星的形成率。这导致了更长的星爆阶段和合并残留物中更高的中心恒星密度。
Merger-driven Fueling of Active Galactic Nuclei: Six Dual and Offset Active Galactic Nuclei Discovered with Chandra and Hubble Space Telescope Observations
Galaxy pairs in the Sloan Digital Sky Survey - IX: Merger-induced AGN activity as traced by the Wide-field Infrared Survey Explorer
星系之间的相互作用预计会导致气体流入，可能引发核活动。由于流入的物质可以掩盖相互作用星系的中心区域，以前的光学研究的一个潜在的限制是，被掩盖的活动星系核（AGN）可以错过在合并序列的各个阶段。我们提出了第一个大的中红外研究活动星系核合并和星系对，以量化的相互作用所引发的模糊活动星系核的发病率。样本由斯隆数字巡天（Sloan Digital Sky Survey）绘制的星系对和合并后的星系组成，这些星系对和宽视场红外天空探测器（WISE）的探测结果相匹配。我们发现，在对活动星系核的分数，相对于质量，红移和环境匹配的控制样本，增加作为一个功能，减少预计分离。这种增强是最引人注目的合并后的样本，在那里我们发现一个因素的10-20过剩的活动星系核部分相比，控制。虽然这种趋势是在定性协议的基础上的光学活动星系核选择的结果，中红外选择活动星系核过剩增加更显着地在合并后比光学活动星系核。我们的研究结果表明，积极占主导地位的光学遮蔽活动星系核变得更加普遍，在最先进的合并，与理论预测一致。
Cool-Core Destruction in Merging Clusters with AGN Feedback and Radiative Cooling
National Taiwan University（台湾大学）；California Institute of Technology（加州理工学院）；National Tsing Hua University（清华大学）；National Center for Theoretical Sciences（国家理论科学中心）；Harvard-Smithsonian Center for Astrophysics（哈佛-史密松天体物理中心）；University of Modena and Reggio Emilia（摩德纳和雷焦艾米利亚大学）
Halo Occupation Distributions of Moderate X-ray AGNs through Major and Minor Mergers in a $Λ$-CDM Cosmology
受Allevato et al.（2012）在COSMOS领域中最近推断的X射线选定活动星系核晕占据分布（HOD）形式的启发，我们使用一个基于$Λ$ -CDM宇宙学中暗物质晕（DMH）之间合并活动的简单模型，研究了中等亮度X射线活动星系核（mXAGN）的HOD性质。在上述情况下，在$z=0.5$模拟的mXAGN的HOD和数密度与Allevato等人（2012）的结果进行比较。我们发现，模拟的HOD的主要和次要合并，和观察到的mXAGN是一致的。我们的主要结果是，未成年人合并，相反，人们可能会期望，可以发挥重要作用的活动mAGN。
Electromagnetic Counterparts of Stellar-mass Binary Black Hole Mergers in AGN Accretion Disks: Theoretical Models and Observational Status
University of Science and Technology of China（中国科学技术大学）；Institute of High Energy Physics, Chinese Academy of Sciences（中国科学院高能物理研究所）；Guizhou University（贵州大学）
Black hole populations and hierarchical growth across the AGN parameter space
Institut für Theoretische Astrophysik, ZAH, Universität Heidelberg（海德堡大学理论天体物理研究所）；Interdisziplinäres Zentrum für Wissenschaftliches Rechnen, Universität Heidelberg（海德堡大学跨学科科学计算中心）；Physics and Astronomy Department Galileo Galilei, University of Padova（帕多瓦大学伽利略物理与天文系）；INFN, Sezione di Padova（意大利国家核物理研究所帕多瓦分部）；Department of Astronomy, University of Concepción（康塞普西翁大学天文学系）；INFN, Sezione di Trieste（意大利国家核物理研究所的里雅斯特分部）
