最遥远的SPT-SZ星系团中的星系群- I. $1.4\lesssim z\lesssim1.7$大质量星系团的环境猝灭
Galaxy populations in the most distant SPT-SZ clusters - I. Environmental quenching in massive clusters at $1.4\lesssim z\lesssim1.7$
V. Strazzullo, M. Pannella, J. J. Mohr, A. Saro, M. L. N. Ashby, M. B. Bayliss, S. Bocquet, E. Bulbul, G. Khullar, A. B. Mantz, S. A. Stanford, B. A. Benson, L.… 展开作者
V. Strazzullo, M. Pannella, J. J. Mohr, A. Saro, M. L. N. Ashby, M. B. Bayliss, S. Bocquet, E. Bulbul, G. Khullar, A. B. Mantz, S. A. Stanford, B. A. Benson, L. E. Bleem, M. Brodwin, R. E. A. Canning, R. Capasso, I. Chiu, A. H. Gonzalez, N. Gupta, J. Hlavacek-Larrondo, M. Klein, M. McDonald, E. Noordeh, D. Rapetti, C. Reichardt, T. Schrabback, K. Sharon, B. Stalder
备注：
29 pages, 16 figures, A&A in press. Replaced to match published version, results unchanged
We present first results from a galaxy population study in the highest redshift galaxy clusters identified in the 2500 deg$^2$ South Pole Telescope Sunyaev Zel'dovich effect (SPT-SZ) survey. The cluster selection is to first order independent of galaxy properties, making the SPT-SZ sample particularly well suited for cluster galaxy population studies. We carry out a 4-band imaging campaign with the {\it Hubble} and {\it Spitzer} Space Telescopes of the five $z\gtrsim 1.4$, S/N$_{SZE}>$5 clusters, that are among the rarest most massive clusters known at this redshift. All five show clear overdensities of red galaxies whose colors agree with the initial cluster redshift estimates. The highest redshift cluster in this sample, SPT-CLJ0459-4947 at $z\sim1.72$, is the most distant $M_{500}>10^{14}~M_{\odot}$ ICM-selected cluster discovered thus far, and is one of only three known clusters in this mass range at $z\gtrsim 1.7$, regardless of selection. Based on UVJ-like photometric classification of quiescent and star-forming galaxies, the passive fraction in the cluster central regions ($r/r_{500}<0.7$) is higher than in the field at the same redshift, with corresponding environmental quenching efficiencies typically in the range $\sim0.5-0.8$ for stellar masses $\log(M/M_{\odot})>10.85$. We have explored the impact of emission from star formation on the selection of this sample, concluding that all five clusters studied here would still have been detected with S/N$_{SZE}>$5, even if they had the same passive fraction as measured in the field. Our results thus point towards an efficient suppression of star formation in massive galaxies in the central regions of the most massive clusters, occurring already earlier than $z\sim1.5$. [Abridged]
Evolution of spatially resolved star formation main sequence and surface density profiles in massive disc galaxies at $0\lesssim z \lesssim 1$: inside-out stellar mass buildup and quenching
Clues to inside-out quenching in quiescent galaxies at $1.2\lesssim z\lesssim2.2$: Age, Fe-, and Mg-abundance gradients from JWST-SUSPENSE
Leiden University（莱顿大学）；Observatories of the Carnegie Institution for Science（卡内基科学研究所天文台）；University of the Pacific（太平洋大学）；University of Pittsburgh（匹兹堡大学）；Max-Planck-Institut für Astronomie（马克斯·普朗克天体物理学研究所）；Max-Planck-Institut für extraterrestrische Physik（马克斯·普朗克地外物理学研究所）；University of California, Berkeley（加州大学伯克利分校）；Tufts University（塔夫茨大学）；Instituto de Astrofísica de Canarias（加那利群岛天体物理研究所）；Universidad de La Laguna（拉帕尔马大学）；York University（约克大学）
The Massive and Distant Clusters of WISE Survey 2: A Stacking Analysis Investigating the Evolution of Star Formation Rates and Stellar Masses in Groups and Clusters
Large-Scale Structure in COSMOS-Web: Tracing Galaxy Evolution in the Cosmic Web up to $z \sim 7$ with the Largest JWST Survey
University of California, Riverside（加州大学河滨分校）；Rochester Institute of Technology（罗切斯特理工学院）；University of California, Santa Barbara（加州大学圣巴巴拉分校）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；University of Hawaii, Hilo（夏威夷大学希洛分校）；Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM（巴黎萨克雷大学、巴黎西岱大学、法国原子能和替代能源委员会、法国国家科学研究中心、天体物理学信息实验室）；University of Hawai‘i（夏威夷大学）；Aalto University（阿尔托大学）；University of Helsinki（赫尔辛基大学）；Aix Marseille Univ, CNRS, CNES, LAM（艾克斯-马赛大学、法国国家科学研究中心、法国国家太空研究中心、天体物理研究实验室）；Technical University of Denmark（丹麦技术大学）；University of Kentucky（肯塔基大学）；Space Telescope Science Institute（太空望远镜科学研究所）；National Astronomical Observatory of Japan（日本国立天文台）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；Institute for Theoretical Physics（理论物理研究所）；Sorbonne Université（索邦大学）；University of Bologna（博洛尼亚大学）；California Institute of Technology（加州理工学院）；MIT Kavli Institute for Astrophysics and Space Research（麻省理工学院卡弗里天体物理学与空间研究所）
Phylogeny of the Milky Way's inner disk and bulge populations: Implications for gas accretion, (the lack of) inside-out thick disk formation, and quenching
An extreme ram-pressure stripping event in a protocluster at redshift 4.3
University of British Columbia（不列颠哥伦比亚大学）；Dalhousie University（达尔豪斯大学）；National Research Council, Herzberg Astronomy and Astrophysics（国家研究委员会赫茨伯格天文学和天体物理学研究所）；Eureka Scientific Inc（尤里卡科学公司）；Universidad Diego Portales（迭戈·波特莱斯大学）；Inter-University Institute for Data Intensive Astronomy, Department of Astronomy, University of Cape Town（开普敦大学数据密集型天文学跨大学研究所天文学系）；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）；Department of Physics, University of Pretoria（比勒陀利亚大学物理系）；Department of Astronomy, University of Florida（佛罗里达大学天文学系）；Texas A&M University（德克萨斯农工大学）
Anisotropic quenching beyond $z=1$ and its implications for preprocessing around high-redshift galaxy clusters
Institute for Cosmic Ray Research, The University of Tokyo（东京大学宇宙射线研究所）；National Astronomical Observatory of Japan（日本国立天文台）；Department of Astronomy, Graduate School of Science, The University of Tokyo（东京大学理学研究科天文学系）；Research Center for the Early Universe, Graduate School of Science, The University of Tokyo（东京大学理学研究科早期宇宙研究中心）；Cosmic Dawn Center (DAWN), Denmark（丹麦黎明中心）；DTU Space, Technical University of Denmark（丹麦技术大学空间研究中心）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo（东京大学高等研究院理化学宇宙 Kavli 研究所）；Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo（东京大学数据驱动发现中心）
Caught in the act: gas and stellar velocity dispersions in a fast quenching compact star-forming galaxy at z~1.7
我们介绍了GDN-8231的Y和H波段的Mask-I MOSFIRE光谱，GDN-8231是一个大质量、致密的恒星形成星系（SFG），红移为$z\sim1.7$。它的光谱揭示了H $_α$和[NII]发射线以及强的巴耳末吸收线。H $_α$和斯皮策MIPS 24 $μ$ m通量都很弱，因此表明SFR $\lesssim5-10$ M $_{\odot}$ yr $^{-1}$的恒星形成率很低。再加上从吸收线测量到的$\sim700$ Myr相对年轻的年龄，这为遥远的星系在快速关闭其恒星形成过程中被捕获提供了第一个直接证据。这样的淬灭使得GDN-8231成为一个紧凑的，静止的星系，类似于我们样本中的其他3个星系，通过$z\sim1.5$。此外，GDN-8231的颜色分布显示出更蓝的中心，与最近模拟的由内而外淬灭早期阶段的预测一致。它的气体视线速度色散$σ^{\rm{gas}}_{\!_{\rm LOS}}=127\pm32$ km s $^{-1}$比它的恒星$σ^{\star}_{\!_{\rm LOS}}=215\pm35$ km s $^{-1}$小近40%。星系的高分辨率流体模拟解释了这种明显较冷的气体运动学的$\sim1.5$的一个因素与旋转盘被认为是在不同的倾角和/或集中的恒星形成区域。一个明确的预测是，它们紧凑、静止的后代保留了一些来自恒星形成祖先的残余旋转。
Galaxy Morphology Network: A Convolutional Neural Network Used to Study Morphology and Quenching in $\sim 100,000$ SDSS and $\sim 20,000$ CANDELS Galaxies
MAGAZ3NE: Spatially Resolved Ages and Chemical Abundances of Ultra-Massive Quiescent Galaxies at z $\sim$ 3.5 using JWST/NIRSpec IFU
York University（约克大学）；University of Toronto（多伦多大学）；Dunlap Institute for Astronomy & Astrophysics, University of Toronto（多伦多大学邓普勒天文学与天体物理研究所）；University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）；University of California Davis（加州大学戴维斯分校）；University of Wisconsin-Madison（威斯康星大学麦迪逊分校）；Observatories of the Carnegie Institution for Science（卡内基科学机构天文台）；Princeton University（普林斯顿大学）
Connecting galaxy evolution in clusters with their radial profiles and phase space distribution: results from the IllustrisTNG hydrodynamical simulations
Dust and PAHs in late-stage galaxy evolution: Imprints of TP-AGB dust injection, grain growth and AGN feedback in high-z quiescent galaxies with JWST and ALMA
National Center for Nuclear Research（国家核研究中心）；SISSA（的里雅斯特国际高等研究学院）；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）；INAF - Osservatorio Astronomico d’Abruzzo（意大利国家天体物理研究所阿布鲁佐天文台）；Department of Astronomy, University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校天文学系）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；Department of Physics & Astronomy, University of British Columbia（不列颠哥伦比亚大学物理与天文学系）；Caltech/IPAC（加州理工学院/IPAC）；IFPU – Institute for Fundamental Physics of the Universe（基础物理学宇宙研究所）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Center for Astrophysics and Cosmology, University of Nova Gorica（新戈里察大学天体物理学与宇宙学中心）
DeepDive: Tracing the early quenching pathways of massive quiescent galaxies at $z>3$ from their star-formation histories and chemical abundances
University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；DTU Space, Technical University of Denmark（丹麦技术大学空间科学与技术中心）；David A. Dunlap Department of Astronomy & Astrophysics, University of Toronto（多伦多大学戴维·A·邓普尔天文与天体物理系）；Dunlap Institute for Astronomy & Astrophysics, University of Toronto（多伦多大学邓普尔天文与天体物理研究所）；Observatories of the Carnegie Institution for Science（卡内基科学机构天文台）
