Using cosmological simulations, we address the properties of high-redshift star-forming galaxies (SFGs) across their main sequence (MS) in the plane of star-formation rate (SFR) versus stellar mass. We relate them to the evolution of galaxies through phases of gas compaction, depletion, possible replenishment, and eventual quenching. We find that the high-SFR galaxies in the upper envelope of the MS are compact, with high gas fractions and short depletion times ("blue nuggets"), while the lower-SFR galaxies in the lower envelope have lower central gas densities, lower gas fractions and longer depletion times, consistent with observed gradients across the MS. Stellar-structure gradients are negligible. The SFGs oscillate about the MS ridge on timescales $\sim0.4~t_{\mathrm{Hubble}}$ ($\sim1$ Gyr at $z\sim3$). The propagation upwards is due to gas compaction, triggered, e.g., by mergers, counter-rotating streams, and/or violent disc instabilities. The downturn at the upper envelope is due to central gas depletion by peak star formation and outflows while inflow from the shrunken gas disc is suppressed. An upturn at the lower envelope can occur once the extended disc has been replenished by fresh gas and a new compaction can be triggered, namely as long as the replenishment time is shorter than the depletion time. The mechanisms of gas compaction, depletion and replenishment confine the SFGs to the narrow ($\pm0.3$ dex) MS. Full quenching occurs in massive haloes ($M_{\mathrm{vir}}>10^{11.5}~M_\odot$) and/or at low redshifts ($z<3$), where the replenishment time is long compared to the depletion time, explaining the observed bending down of the MS at the massive end.
Instituto de Astronomía y Física del Espacio, CONICET–UBA（空间物理与天文学研究所，阿根廷国家科学和技术研究委员会-布宜诺斯艾利斯大学）；Departamento de Fisica Teorica, Universidad Autonoma de Madrid（马德里自治大学理论物理系）；CIAFF, Facultad de Ciencias, Universidad Autonoma de Madrid（马德里自治大学理学院CIAFF）
Molecular gas properties of star-forming brightest group galaxies at $z \sim 0.3$
Alma Mater Studiorum Università di Bologna（博洛尼亚大学）；INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所波伦亚天文台）；Zentrum für Astronomie, Universität Heidelberg（海德堡大学天文中心）；Observatoire de Paris, Collège de France, PSL University, Sorbonne University, CNRS, LUX（巴黎天文台，法兰西学院，PSL大学，索邦大学，法国国家科学研究中心，LUX）；Institut de Radioastronomie Millimétrique (IRAM)（毫米波射电天文研究所）；INFN - Sezione di Bologna（意大利国家核物理研究所博洛尼亚分部）；ITP, Universität Heidelberg（海德堡大学理论物理研究所）
MIGHTEE-HI: Environmental effects of cosmic filaments on extragalactic HI detections in the COSMOS and XMM-LSS fields
University of Oxford（牛津大学）；University of Cambridge（剑桥大学）；University of the Western Cape（西开普敦大学）；University of Bristol（布里斯托大学）；Universiteit Gent（根特大学）；University of Edinburgh（爱丁堡大学）；Inter-University Institute for Data Intensive Astronomy, Department of Astronomy, University of Cape Town（开普敦大学天文学系数据密集型天文跨大学研究所）；Centre for Astrophysics Research, School of Physics, Astronomy and Mathematics, University（大学物理、天文与数学学院天体物理学研究中心）
Sleeping or Dead? Probing the Quenching Mechanism of JWST Dormant Galaxies at z > 3 with ALMA
University of Geneva（日内瓦大学）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；University of Sussex（萨塞克斯大学）；Caltech/IPAC（加州理工学院/IPAC）；Université Paris-Saclay（巴黎萨克雷大学）；Université Paris Cité（巴黎西岱大学）；CEA（法国原子能委员会）；CNRS（法国国家科学研究中心）；AIM（天体物理学、信息与微波实验室）；University of Zurich（苏黎世大学）
JWST spectroscopy of galaxies at $z>10$: Damped Ly$α$ absorbers reveal efficient star formation and hidden redshift biases
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）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；The Kavli Institute for Cosmology (KICC), University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Cavendish Laboratory, University of Cambridge（剑桥大学卡文迪许实验室）；Department of Astronomy, University of Geneva（日内瓦大学天文学系）；David A. Dunlap Department of Astronomy and Astrophysics, University of Toronto（多伦多大学戴维·A·邓普天文学与天体物理学系）
ADF22-WEB: Massive galaxy formation shaped by cosmic web filaments in the z = 3.1 proto-cluster core
Nagoya University（名古屋大学）；The Graduate University for Advanced Studies, SOKENDAI（综合研究大学院大学）；Durham University（杜伦大学）；California Institute of Technology（加州理工学院）；University of Arkansas（阿肯色大学）；National Astronomical Observatory of Japan（日本国立天文台）；Kwansei Gakuin University（关西学院大学）
