Gas condensation in Brightest Group Galaxies unveiled with MUSE
V. Olivares, P. Salome, S. L. Hamer, F. Combes, M. Gaspari, K. Kolokythas, E. O'Sullivan, R. S. Beckmann, A. Babul, F. L. Polles, M. Lehnert, S. I. Loubser, M. … 展开作者
V. Olivares, P. Salome, S. L. Hamer, F. Combes, M. Gaspari, K. Kolokythas, E. O'Sullivan, R. S. Beckmann, A. Babul, F. L. Polles, M. Lehnert, S. I. Loubser, M. Donahue, M. -L. Gendron-Marsolais, P. Lagos, G. Pineau des Forets, B. Godard, T. Rose, G. Tremblay, G. Ferland, P. Guillard
备注：
38 pages, and 16 figures. Resubmitted to A&A after referee report
The origin of the cold gas in central galaxies in groups is still a matter of debate. We present Multi-Unit Spectroscopic Explorer (MUSE) observations of 18 optically selected local Brightest Group Galaxies (BGGs) to study the kinematics and distribution of the optical emission-line gas. MUSE observations reveal a distribution of gas morphologies including ten complex networks of filaments extending up to 10 kpc to two compact (<3 kpc) and five extended (>5 kpc) disk-dominated structures. Some rotating disks show rings and elongated structures arising from the central disk. The kinematics of the stellar component is mainly rotation-dominated, which is very different from the disturbed kinematics and distribution found in the filamentary sources. The ionized gas is kinematically decoupled from the stellar component for most systems, suggesting an external origin for the gas. We also find that the Halpha luminosity correlates with the cold molecular mass. By exploring the thermodynamical properties of the hot atmospheres, we find that the filamentary sources and compact disks are found in systems with small central entropy values and tcool/teddy ratios. This suggests that, like for Brightest Cluster Galaxies in cool core clusters, the ionized gas are likely formed from hot halo gas condensations, consistently with the Chaotic Cold Accretion simulations (as shown via the C-ratio, Tat, and k-plot). We note that gaseous rotating disks are more frequent than in BCGs. An explanation for the origin of the gas in those objects is a contribution to gas fueling by mergers or group satellites, as qualitatively hinted by some sources of the present sample. Nonetheless, we discuss the possibility that some extended disks could also be a transition stage in an evolutionary sequence including filaments, extended disks and compact disks, as described by hot gas condensation models of cooling flows.
Towards Precision Cosmology With Improved PNLF Distances Using VLT-MUSE. III. Impact of Stellar Populations in Early-Type Galaxy
Leibniz-Institut für Astrophysik Potsdam (AIP)（波茨坦莱布尼茨天体物理研究所）；Institut für Physik und Astronomie, Universität Potsdam（波茨坦大学物理与天文学研究所）；Universitäts-Sternwarte, Fakultät für Physik, Ludwig-Maximilians Universität München（慕尼黑路德维希-马克西米利安大学大学天文台物理学院）；Department of Astronomy & Astrophysics, The Pennsylvania State University（宾夕法尼亚州立大学天文与天体物理系）；Institute for Gravitation and the Cosmos, The Pennsylvania State University（宾夕法尼亚州立大学引力与宇宙研究所）；NSF’s NOIRLab（美国国家科学基金会NOIR实验室）；European Southern Observatory（欧洲南方天文台）
ALMA visits the QSO MUSEUM: Connecting molecular gas and the cool circumgalactic medium around 37 $z\sim3$ quasars
Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Academia Sinica Institute of Astronomy and Astrophysics (ASIAA)（中央研究院天文及天文物理研究所）；Universität Heidelberg, Interdisziplinäres Zentrum für Wissenschaftliches Rechnen (IWR)（海德堡大学跨学科科学计算中心）；Universität Heidelberg, Zentrum für Astronomie, Institut für Theoretische Astrophysik（海德堡大学天文学中心理论天体物理研究所）；Institut de Radioastronomie Millimétrique (IRAM)（毫米波射电天文研究所）
Resolving circumgalactic gas flows around a z$\approx$3.6 quasar using MUSE and ALMA
Università degli Studi di Milano-Bicocca（米兰比可卡大学）；DTU Space, Technical University of Denmark（丹麦技术大学空间中心）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；INAF–Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）；INAF–Osservatorio di Astrofisica e Scienza dello Spazio（意大利国家天体物理研究所天文与空间科学观测站）；IUCAA（印度天体物理学与宇宙学大学研究中心）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）
Discovery of a diffuse optical line emitting halo in the core of the Centaurus cluster of galaxies: Line emission outside the protection of the filaments
Multi-spin stellar velocity maps of the most massive galaxies
Leibniz-Institut für Astrophysik Potsdam (AIP)（波茨坦莱布尼茨天体物理研究所）；European Southern Observatory（欧洲南方天文台）；Univ Lyon, Univ Lyon1, ENS de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574（里昂大学，里昂第一大学，里昂高等师范学院，法国国家科学研究中心，里昂天体物理研究中心）；Leiden Observatory, Leiden University（莱顿天文台，莱顿大学）
The transient event in NGC 1566 from 2017 to 2019 -- I. An eccentric accretion disk and a turbulent, disk-dominated broad-line region unveiled by double-peaked Ca II and O I lines
本文通过分析 NGC 1566 的光谱变源数据，首次探测到 AGN 中 OI 和 CaII 的宽双峰发射线，揭示其宽线区由相对论偏心吸积盘主导并存在标高湍流分层，蓝移漂移或源于暂现事件期间发射的低光学深度风。
Massive dusty multiphase outflow in local merger shows no sign of slowing on kiloparsec scales
Institute of Theoretical Astrophysics, University of Oslo（奥斯陆大学理论天体物理研究所）；Armagh Observatory and Planetarium（阿马天文台和天文馆）；INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）；Dipartimento di Fisica e Astronomia Augusto Righi, Università degli Studi di Bologna（博洛尼亚大学奥古斯托·里基物理与天文学系）；INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚空间科学与天体物理学观测站）
HARMONI view of the host galaxies of active galactic nuclei around cosmic noon: Resolved stellar morpho-kinematics and the M$_{BH}$-$σ_{\star}$ relation
The headlight cloud in NGC 628: An extreme giant molecular cloud in a typical galaxy disk
分子气体的云尺度调查揭示了分子云性质与恒星形成（SF）之间的联系，在一系列银河系环境中。星系盘中的云量被认为是“正常”SF的代表。然而，在高分辨率下，在正常的磁盘环境中也可以观察到具有特殊气体特性和SF活动的云。本文研究了NGC628星盘中最亮云的CO示踪辐射。这片云在空间上与一个非常明亮的HII区域重合。我们描述了它的分子气体性质，并研究了反馈和大尺度过程如何影响分子气体的性质。高分辨率的COALMA观测被用来描述它的质量和动力学状态，并与NGC628中的其他云进行了比较。一个LVG分析被用来约束束稀释的分子气体的密度和温度。我们使用Starburst 99分析MUSE光谱来表征与HII区域相关的年轻恒星星族。云是巨大的（$1-2\times10^7$ M $_{\odot}$），具有$n_{\rm H_2}=5\times10^4$ cm $^{-3}$的光束稀释密度。它具有较低的维里参数，这表明它的CO排放可能是overluminous由于加热的HII区域。一个年轻的大质量$2-4$ M $_{\odot}$恒星星族与之相伴。我们认为，云目前正在被年轻的大质量恒星的反馈破坏。由于云的质量很大，云演化的这个阶段足够长，可以观察到反馈对气体激发的影响。它的高质量可能与它的位置有关，在螺旋共同旋转半径，与盘的其他区域相比，气体经历减少的银河系剪切，并接受持续的气体流入，可以促进云的…
HST view of NGC 5044: Constraints on Filament Widths, Magnetic Support, Multiphase Structure, and Comparison with Cluster Environments
University of Alabama in Huntsville（阿拉巴马大学亨茨维尔分校）；University of Modena and Reggio Emilia（摩德纳和雷焦艾米利亚大学）；Observatoire de Paris, PSL Univ., Collège de France, CNRS, Sorbonne Univ.（巴黎天文台、巴黎文理研究大学、法兰西公学院、法国国家科学研究中心、索邦大学）；Masaryk University（马萨里克大学）；Center for Astrophysics | Harvard & Smithsonian（哈佛-史密森天体物理中心）；University of Portsmouth（朴茨茅斯大学）；Michigan State University（密歇根州立大学）
