An Absence of Radio-Loud Active Galactic Nuclei in Geometrically Flat Quiescent Galaxies: Implications for Maintenance-Mode Feedback Models
Ivana Barišić, Arjen van der Wel, Josha van Houdt, Michael V. Maseda, Eric F. Bell, Rachel Bezanson, Yu-Yen Chang, Huub Röttgering, Glenn van de Ven, Po-Feng Wu
备注：
7 pages, 5 figures, accepted for publication in ApJ Letters
Maintenance-mode feedback from low-accretion rate AGN, manifesting itself observationally through radio-loudness, is invoked in all cosmological galaxy formation models as a mechanism that prevents excessive star-formation in massive galaxies (M$_*$ $\gtrsim$ 3$\times$10$^{10}$ M$_{\odot}$). We demonstrate that at a fixed mass the incidence of radio-loud AGN (L $>$ 10$^{23}$ WHz$^{- 1}$) identified in the FIRST and NVSS radio surveys among a large sample of quiescent (non-star forming) galaxies selected from the SDSS is much higher in geometrically round galaxies than in geometrically flat, disk-like galaxies. As found previously, the RL AGN fraction increases steeply with stellar velocity dispersion $σ_*$ and stellar mass, but even at a fixed velocity dispersion of 200-250 kms$^{-1}$ this fraction increases from 0.3% for flat galaxies (projected axis ratio of q $<$ 0.4) to 5% for round galaxies (q $>$ 0.8). We rule out that this strong trend is due to projection effects in the measured velocity dispersion. The large fraction of radio-loud AGN in massive, round galaxies is consistent with the hypothesis that such AGN deposit energy into their hot gaseous halos, preventing cooling and star-formation. However, the absence of such AGN in disk-like quiescent galaxies -- most of which are not satellites in massive clusters, raises important questions: is maintenance-mode feedback a generally valid explanation for quiescence; and, if so, how does that feedback avoid manifesting at least occasionally as a radio-loud galaxy?
Link between radio-loud AGNs and host-galaxy shape
静止星系的形态与其中心超大质量黑洞的活动有关。在这项工作中，我们使用LOFAR两个$-$米制巡天（LoTSS DR 1）和斯隆数字巡天数据发布7（SDSS DR 7）的第一个数据发布的数据，选择超过15 000个静止星系在$z<0.3$调查射电大声活动星系核（RLAGN）和它们的宿主星系的形态之间的连接。利用LoTSS的深度，我们发现，在固定的恒星质量，速度色散，或表面质量密度与$L_{\rm 150\,MHz}>10^{21}\rm\,W\,Hz^{-1}$的RLAGN的分数不依赖于星系投影轴比（$q$）。然而，高功率（$L_{\rm 150\,MHz}>10^{23}\rm\,W\,Hz^{-1}$）RLAGN更有可能在大质量的圆形星系中发现，而低功率和中功率（$L_{\rm 150\,MHz}\leq10^{23}\rm\,W\,Hz^{-1}$）RLAGN具有与非RLAGN星系相似的$q$分布。我们认为，我们的研究结果支持的图片，高功率RLAGNs更容易被触发的星系合并丰富的历史，而低功率RLAGNs可以被触发的星系增长主要通过长期的过程。我们的工作也支持这样的想法，即低光度RLAGN可能是足够的低质量的静止星系与盘状形态，这是基于一个简单的外推从观察到的能量平衡之间的冷却和RLAGN诱导腔大规模集群的维持模式反馈。我们发现，在控制了两个样本的射电光度和恒星质量后，可能在星…
First detection of ultra-fast outflows in a quiescent galaxy
Institute of Space Sciences (ICE, CSIC)（空间科学研究所）；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究学院）；Instituto de Astrofísica de Canarias (IAC)（加那利天体物理研究所）；Universidad de La Laguna (ULL)（拉帕鲁纳大学）；Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；INAF - IASF Palermo（意大利国家天体物理研究所巴勒莫分所）；The Catholic University of America（美利坚天主教大学）；INAF, Osservatorio Astronomico di Brera（意大利国家天体物理研究所布拉耶天文台）；Università degli Studi Roma Tre（罗马第三大学）
There and back again? Neutral outflows in z~3.5 quiescent galaxies
Cosmic Dawn Center (DAWN)（黎明中心）；DTU Space, Technical University of Denmark（丹麦技术大学空间部）；INAF-Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；Department of Astronomy, University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校天文学系）；The Graduate University for Advanced Studies, SOKENDAI（日本综合研究大学院大学）；National Astronomical Observatory of Japan（日本国立天文台）；DARK, Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所暗物质研究中心）
Active galactic nucleus activity in brightest cluster galaxies at intermediate redshifts in Sunyaev-Zel'dovich--selected clusters
South African Astronomical Observatory（南非天文台）；Department of Astronomy, University of Cape Town（开普敦大学天文学系）；Wits Centre for Astrophysics, School of Physics, University of the Witwatersrand（威特沃特斯兰德大学物理学院天体物理中心）；School of Mathematics, Statistics & Computer Science, University of KwaZulu-Natal（夸祖鲁-纳塔尔大学数学、统计与计算机科学学院）；Centre for Space Research, North-West University（西北大学空间研究中心）；National Institute for Theoretical and Computational Sciences (NITheCS)（国家理论与计算科学研究所）；Inter-University Centre for Astronomy and Astrophysics（大学间天文学与天体物理学中心）
Tracing Radio AGN-Driven Quenching in Post-Starburst Galaxies at Cosmic Noon
Johns Hopkins University（约翰斯·霍普金斯大学）；Space Telescope Science Institute（太空望远镜科学研究所）；AURA for ESA, Space Telescope Science Institute（欧洲空间局阿雷西博大学协会太空望远镜科学研究所）；University of Nottingham（诺丁汉大学）；University of St Andrews（圣安德鲁斯大学）；University of Edinburgh（爱丁堡大学）；European Southern Observatory (ESO)（欧洲南方天文台）
J-HERTz: J-PLUS Heritage Exploration of Radio Targets at z $<$ 5
Centro de Estudios de Física del Cosmos de Aragón (CEFCA)（阿拉贡宇宙物理学研究中心）；Instituto de Astrofísica de Andalucía (CSIC)（安达卢西亚天体物理研究所）；Departamento de Física, Faculdade de Ciências, Universidade de Lisboa（里斯本大学理学院物理系）；BNP Paribas Corporate & Institutional Banking（法国巴黎银行企业与机构银行业务）
PEARLS: NuSTAR and XMM-Newton Extragalactic Survey of the JWST North Ecliptic Pole Time Domain Field VI: Multiwavelength SED Analysis
Arizona State University（亚利桑那州立大学）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Center for Astrophysics | Harvard & Smithsonian（天体物理中心 | 哈佛与史密森尼学会）；University of Utah（犹他大学）
