By tracing the orbital and star formation histories of galaxies within the Coma cluster, we seek to understand the role of the high-density cluster environment in quenching these galaxies. We combine star formation histories extracted from high-signal-to-noise spectra of 11 early-type galaxies around the center of the Coma cluster with probability distributions for their orbital parameters obtained using an N-body simulation to connect their orbital and star formation histories. We find that all 11 galaxies likely quenched near their first pericentric approach. Higher stellar mass galaxies ($\log(M_\star/\mathrm{M}_\odot)>10$) had formed a higher fraction of their stellar mass (more than $\sim90\%$) than their lower mass counterparts ($\sim 80$-$90\%$) by the time they fell into the cluster (when they cross $2.5r_\mathrm{vir}$). We find that the expected infall occurred around $z\sim0.6$, followed by the first pericentric passage $\sim4\,\mathrm{Gyr}$ later. Galaxies in our sample formed a significant fraction of their stellar mass, up to $15\%$, between infall and first pericenter, and had assembled more than $\sim98\%$ of their cumulative stellar mass by first pericenter. Unlike previous low-redshift studies that suggest that star formation continues until about first apocenter or later, the high percentage of stellar mass already formed by first pericenter in our sample galaxies points to star formation ceasing within a gigayear after the first pericentric passage. We consider the possible physical mechanisms driving quenching and find that our results resemble the situation in clusters at $z\sim1$, where active stripping of gas (ram-pressure or tidally driven) seems to be required to quench satellites by their first pericentric passage. However, a larger sample will be required to conclusively account for the unknown fraction of preprocessed satellites in the Coma cluster.
ALMA-JELLY II. Constraining the radial profiles of the quenching timescales in ram-pressure-stripped galaxies
Università di Milano-Bicocca（米兰比可卡大学）；INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）；Aix Marseille Univ, CNRS, CNES, LAM（艾克斯-马赛大学、法国国家科学研究中心、法国国家空间研究中心、天体物理与行星学实验室）；INAF - Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）；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）；Yale University（耶鲁大学）；Astronomical Institute of the Czech Academy of Sciences（捷克科学院天文研究所）；The University of Alabama in Huntsville（阿拉巴马大学亨茨维尔分校）；University of Hertfordshire Centre for Astrophysics Research（赫特福德大学天体物理学研究中心）；Observatoire de Paris, LUX, Collège de France, CNRS, PSL University, Sorbonne Uni（巴黎天文台、卢克瑟姆实验室、法兰西学院、法国国家科学研究中心、巴黎文理研究大学、索邦大学）
The role of bars in quenching star formation from z = 3 to the present epoch. Halpha3: an Halpha imaging survey of HI selected galaxies from ALFALFA, VI
Ram-pressure-induced star formation in low-mass galaxies infalling on-to the Coma cluster: insights from DESI
Universite Paris Cite（巴黎西岱大学）；CNRS（法国国家科学研究中心）；Astroparticule et Cosmologie（亚原子粒子与宇宙学）；Sternberg Astronomical Institute（斯滕伯格天文研究所）；M.V. Lomonosov Moscow State University（莫斯科罗蒙诺索夫国立大学）；Center for Astrophysics | Harvard & Smithsonian（哈佛史密森尼天体物理中心）；Institut d’Astrophysique de Paris (UMR 7095: CNRS & Sorbonne Université)（巴黎天体物理学研究所）；Sorbonne Université（索邦大学）；INAF Osservatorio Astronomico di Trieste（的里雅斯特天文台）；IFPU: Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；Faculty of Space Research, M.V. Lomonosov Moscow State University（莫斯科罗蒙诺索夫国立大学空间研究学院）
Evolution of Galaxy Shapes from Prolate to Oblate through Compaction Events
我们使用宇宙学模拟研究星系整体形状的演化。这些形状是指暗物质、恒星和气体在恒星半质量半径处的组成部分。大多数星系在$z\sim2-4$经历了一个特征性的压缩事件，成为一个蓝块，这标志着从DM主导的中心体到自引力重子核的转变。我们发现，在高- $z$，DM占主导地位的阶段，恒星和DM系统往往是三轴，优先长轴和相互对齐。伸长是由各向异性的速度分散，起源于沿占主导地位的大尺度灯丝星系的组装支持。我们估计，扭矩的主导晕是能够诱导伸长的恒星系统和它的晕对齐。然后，与过渡到自引力，小近心轨道膨胀和DM和恒星系统演变成一个更球形和扁圆形的配置，与气体盘对齐，并与旋转相关。这种转变通常发生在恒星质量为$\sim 10^9$ M $_\odot$，核心逃逸速度为$\sim 100$ km s $^{-1}$时，这表明超新星反馈可能有效地保持核心DM主导和系统长扁。早期的拉长相本身可能是压实事件的原因，而向扁圆相的转变可能与随后的核心淬火有关。
Connecting galaxy evolution in clusters with their radial profiles and phase space distribution: results from the IllustrisTNG hydrodynamical simulations
Why the Northern Hemisphere Needs a 30-40m Telescope and the Science at Stake: Ultra-Low-Mass Dwarf Galaxies Across the Boreal Cosmic Web
Instituto de Astrofísica de Canarias（加那利群岛天体物理学研究所）；Universidad de La Laguna（拉戈亚大学）；Universidad de Granada（格拉纳达大学）；Universidad Autónoma de Madrid（马德里自治大学）；Universidad de La Serena（拉塞雷纳大学）；Canada-France-Hawaii Telescope（加拿大-法国-夏威夷望远镜）；Planetarium La Enseñanza（La Enseñanza 天文馆）；Instituto de Astrofisica de Andalucía（安达卢西亚天体物理学研究所）；INAF – Astronomical Observatory of Brera（意大利国家天体物理研究所布雷拉天文台）；Leiden Observatory（莱顿天文台）
