Early thin-disc assembly revealed by JWST edge-on galaxies
Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）
Marloes van Asselt, Francesca Rizzo, Luca Di Mascolo
备注：
20 pages, 17 figures 2 tables (plus 5 pages, 7 figures and 2 tables as appendix). Accepted for publication in Monthly Notices of the Royal Astronomical Society
The vertical structure of stellar discs provides key constraints on their formation and evolution. Nearby spirals, including the Milky Way, host thin and thick components that may arise either from an early turbulent phase or from the subsequent dynamical heating of an initially thin disc; measuring disc thickness across cosmic time therefore offers a direct test of these scenarios. We present a new methodology to measure the thickness of edge-on galaxies that explicitly accounts for departures from perfectly edge-on orientations by fitting a full three-dimensional model with forward modelling. This improves on traditional approaches that assume an inclination of $90^\circ$ and can bias thicknesses high. Applying the method to JWST imaging of galaxies at $1<z<3$ with stellar masses $\gtrsim 10^9~M_\odot$ from four major surveys, we measure a median scale height of $z_0 = 0.25\pm0.14$~kpc and a median ratio $h_r/z_0=8.4\pm3.7$. These values are consistent with the Milky Way and local thin discs, and indicate scale heights $\sim 1.6$ times smaller than those inferred for local galaxies from single-disc fits. This result implies that thin discs are already present at $z\sim3$. We further show that a thick disc contributing 10\% of the thin-disc luminosity would be detectable in the data considered in this work, implying that any thick disc present must be fainter and favouring a scenario in which thick discs build up progressively through dynamical heating at $z<1$.
RIOJA. A Clumpy Galaxy Assembly at Redshift 6.81 Revealed by JWST
Waseda University（早稻田大学）；University of Tsukuba（筑波大学）；Flatiron Institute（平顿研究所）；The University of Tokyo（东京大学）；Nagoya University（名古屋大学）；Kyoto University（京都大学）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), UT Institute for Advanced Study, The University of Tokyo（东京大学宇宙起源研究核心（WPI）/ 基础宇宙物理学宇宙论前沿中心）；Chalmers University of Technology（查尔姆斯理工大学）；National Astronomical Observatory of Japan（日本国立天文台）；Chiba University（千叶大学）；Space Telescope Science Institute (STScI)（太空望远镜科学研究所）；Graduate University for Advanced Studies (SOKENDAI)（综合研究大学院大学）
Supermassive Black Hole Assembly from Heavy Seeds with Dynamical Friction in the BRAHMA Simulations: Implications for JWST, LISA, and the Local Universe
University of Virginia（弗吉尼亚大学）；Virginia Institute for Theoretical Astronomy, University of Virginia（弗吉尼亚大学理论天体物理研究所）；University of California Berkeley（加州大学伯克利分校）；Center for Computational Astrophysics, Flatiron institute（西蒙斯基金会平顿计算天体物理中心）；Leibniz Institute for Astrophysics Potsdam (AIP)（波茨坦阿基米德天体物理研究所）；Yale University（耶鲁大学）；Black Hole Initiative, Harvard University（哈佛大学黑洞倡议计划）
JWST observes the assembly of a massive galaxy at z~4
University of Oxford（牛津大学）；University of Leiden（莱顿大学）；Observatório Nacional/MCTI（国家天文台/科技部）；TNO（荷兰组织应用科学研究所）；Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理研究所）；Steward Observatory, University of Arizona（亚利桑那大学斯蒂沃德天文台）；Instituto de Astrofísica de La Plata, CONICET-UNLP（拉普拉塔天体物理研究所/阿根廷国家科学技术研究委员会/拉普拉塔国立大学）；Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata（拉普拉塔国立大学天文与地球科学学院）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心/西班牙国家技术研究委员会/国家航空航天技术研究所）；ELTE Eoẗovös Loránd University（罗兰大学）
Birds of a Feather: Resolving Stellar Mass Assembly With JWST/NIRCam in a Pair of Kindred $z \sim 2$ Dusty Star-forming Galaxies Lensed by the PLCK G165.7+67.0 Cluster
The Role of Environment in Shaping the Assembly Timelines of Massive Quiescent Galaxies at Cosmic Noon
ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D)（ARC三维全天空天体物理学卓越中心）；INAF, Astrophysics and Space Science Observatory Bologna（意大利国家天体物理研究所博洛尼亚天文台）；Cavendish Laboratory - Astrophysics Group, University of Cambridge（剑桥大学卡文迪许实验室）；Institute for Computational & Data Sciences, The Pennsylvania State University（宾夕法尼亚州立大学计算与数据科学研究所）；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）；Departamento de Astronomía, Universidad de Chile（智利大学天文学系）；Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学天文与天体物理研究学院）；Dipartimento di Fisica e Astronomia, Università di Bologna（博洛尼亚大学物理与天文学系）
A Lower Bound of Star Formation Activity in Ultra-high Redshift Galaxies Detected with JWST: Implications for Stellar Populations and Radiation Sources
Massive Galaxies Form Early and Gray: Stellar Assembly and Dust Attenuation at $\mathbf{z>3.5}$ from CAPERS
The University of Texas at Austin（德克萨斯大学奥斯汀分校）；Cosmic Frontier Center, The University of Texas at Austin（德克萨斯大学奥斯汀分校宇宙前沿中心）；NSF’s National Optical-Infrared Astronomy Research Laboratory（美国国家光学-红外天文研究实验室）；Space Telescope Science Institute（太空望远镜科学研究所）
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）
The JWST-PRIMAL Legacy Survey. A JWST/NIRSpec reference sample for the physical properties and Lyman-$α$ absorption and emission of $\sim 500$ galaxies at $z=5.5-13.4$
A Census of the 200 Most Massive Galaxies Spectroscopically Observed with JWST at zspec $\sim$3-15
University of Geneva（日内瓦大学）；Cosmic Dawn Center (DAWN)（黎明宇宙中心）；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）；Université Paris-Saclay（巴黎萨克雷大学）；Université Paris Cité（巴黎西岱大学）；CEA（法国原子能和替代能源委员会）；CNRS（法国国家科学研究中心）
Simulation-based inference of galaxy properties from JWST pixels
Instituto de Astrofísica de Canarias（加那利天体物理研究所）；Universidad de La Laguna（拉古纳大学）；Observatoire de Paris, LERMA, PSL University（巴黎天文台，PSL大学）；Université Paris-Cité（巴黎西岱大学）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CSIC-INTA））；University of Arizona（亚利桑那大学）；Space Telescope Science Institute（太空望远镜科学研究所）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）
GA-NIFS view of LAP1: Assembly of Pop~III stellar clusters during EoR
Kavli Institute for Cosmology, 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 Physics and Astronomy, University College London（伦敦大学学院物理与天文系）；Scuola Normale Superiore（比萨高等师范学院）；INAF – OAS, 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观测台）；Instituto Nacional de Astrofísica, Óptica y Electrónica（墨西哥国家天体物理学、光学和电子研究所）；Institute of Astronomy, University of Cambridge（剑桥大学天文学研究所）；Facultad de Astronomía y Geofísica, Universidad de La Plata（拉普拉塔大学天文与地球物理学院）；Max-Planck-Institut für extraterrestrische Physik（马克斯·普朗克地外物理研究所）；Centro de Astrobiología (CAB), CSIC–INTA（西班牙国家技术研究与应用中心-国家航空太空技术研究所天体生物学中心）；INAF — Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）
Spatially Resolved Stellar Populations of $0.3<z<6.0$ Galaxies in WHL0137-08 and MACS0647+70 Clusters as Revealed by JWST: How do Galaxies Grow and Quench Over Cosmic Time?
Early steps in the hierarchical assembly of a Milky Way-mass galaxy 1 Gyr after the Big Bang
Dunlap Institute for Astronomy and Astrophysics（邓拉普天体物理与天文研究所）；Department of Astronomy and Physics and Institute for Computational Astrophysics, Saint Mary’s University（圣玛丽大学天文物理系及计算天体物理研究所）；Waseda Research Institute for Science and Engineering, Faculty of Science and Engineering, Waseda University（早稻田大学理工学部理工学研究科）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡佩恩天文研究所）；Faculty of Mathematics and Physics, University of Ljubljana（卢布尔雅那大学数学物理学院）；Department of Physics and Astronomy, University of California Davis（加州大学戴维斯分校物理与天文学系）
Reionization and the ISM/Stellar Origins with JWST and ALMA (RIOJA): The core of the highest redshift galaxy overdensity at $z = 7.88$ confirmed by NIRSpec/JWST
Early Emergence of Environmental Effects: Accelerated Galaxy Assembly in a z=2.96 Protocluster in the COSMOS Field
Tsinghua University（清华大学）；The University of Tokyo（东京大学）；Kavli Institute for the Physics and Mathematics of the Universe (WPI)（宇宙物理与数学研究所（ Kavli IPMU ））
A large overdensity of LRD-like galaxies discovered by JWST in the SPT2349-56 protocluster at z=4.30
Dalhousie University（达尔豪斯大学）；University of British Columbia（不列颠哥伦比亚大学）；NRC Herzberg Astronomy and Astrophysics（加拿大国家研究委员会赫茨伯格天文学与天体物理学研究所）；Eureka Scientific Inc（尤里卡科学公司）；University of Illinois（伊利诺伊大学）；National Center for Supercomputing Applications（超级计算应用国家中心）；Max-Planck-Institut fur Radioastronomie（马克斯·普朗克射电天文研究所）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；Universidad Diego Portales（迭戈·波特莱斯大学）；Millenium Nucleus for Galaxies (MINGAL)（星系千年核心（MINGAL））；University of Victoria（维多利亚大学）
Two-phase formation of galaxies: the coevolution between galaxies and dark matter halos
Tsinghua University（清华大学）；Nanjing University（南京大学）；University of Science and Technology of China（中国科学技术大学）；University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）
Early Results from GLASS-JWST. XXV. Electron Density in the Interstellar Medium at $0.7\lesssim z\lesssim 9.3$ with NIRSpec High-resolution Spectroscopy
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）
Supermassive Dark Stars and their remnants as a possible solution to three recent cosmic dawn puzzles
Colgate University（科尔盖特大学）；University of Pennsylvania（宾夕法尼亚大学）；Space Telescope Science Institute (STScI)（太空望远镜科学研究所）；Johns Hopkins University（约翰斯·霍普金斯大学）；University of Texas（德克萨斯大学）；Stockholm University（斯德哥尔摩大学）；Nordic Institute for Theoretical Physics (NORDITA)（北欧理论物理研究所）
Insights on Metal Enrichment and Environmental Effect at $z\approx5-7$ with JWST ASPIRE/EIGER and Chemical Evolution Model
Cosmic Dawn Center (DAWN)（黎明中心）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Tsinghua University（清华大学）；The Hebrew University（希伯来大学）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；University of Arizona（亚利桑那大学）；International Gemini Observatory/NSF NOIRLab（国际双子座天文台/美国国家光学红外天文实验室）；Northwestern College（西北学院）；Observatoire de Paris, Université PSL, Sorbonne Université, CNRS（巴黎天文台，巴黎文理研究大学，索邦大学，法国国家科学研究中心）；University of Michigan（密歇根大学）；Huazhong University of Science and Technology（华中科技大学）；Chinese Academy of Sciences South America Center for Astronomy, National Astronomical Observatories, CAS（中国科学院南京天文光学技术研究所（南美天文中心））；Universidad de Chile（智利大学）
