远红外（FIR）和亚毫米波观测已证实，在过去120亿年里，尘埃遮蔽的恒星形成在恒星质量组装过程中发挥着核心作用。在红移z介于2到4之间时，大部分恒星形成活动被尘埃包裹，且尘埃恒星形成星系（DSFGs，dusty star forming galaxies）的恒星质量密度约占总恒星质量密度的一半。恒星形成发生在致密分子云中，并受到星系能量收支相关的所有星际介质（ISM）组分间复杂相互作用的调控，这些组分包括气体、尘埃、宇宙射线、星际电磁场、引力场、暗物质。分子气体是恒星形成气体与其复杂环境之间的实际纽带，提供了关于恒星形成过程的最丰富信息。然而，要解释分子谱线，需要对调控分子形成并决定云内分子丰度的天体化学网络进行复杂建模，还需要对分子能级得以布居的气体物理条件进行建模。本文批判性地综述了用于预测DSFGs中分子信号所需的主要天体化学参数。我们回顾了关于DSFGs星际介质的现有认知与未解决的问题，突出了分子气体作为恒星形成过程的示踪物与塑造者的关键作用。
英文摘要：
FIR and submm observations have established the fundamental role of dust-obscured star formation in the assembly of stellar mass over the past 12 billion years. At z between 2 and 4, the bulk of star formation is enshrouded in dust, and dusty star forming galaxies (DSFGs) contain about half of the total stellar mass density. Star formation develops in dense molecular clouds, and is regulated by a complex interplay between all the ISM components that contribute to the energy budget of a galaxy: gas, dust, cosmic rays, interstellar electromagnetic fields, gravitational field, dark matter. Molecular gas is the actual link between star forming gas and its complex environment, providing by far the richest amount of information about the star formation process. However, molecular lines interpretation requires complex modeling of astrochemical networks, which regulate the molecular formation and establishes molecular abundances in a cloud, and a modeling of the physical conditions of the gas in which molecular energy levels become populated. This paper critically reviews the main astrochemical parameters needed to get predictions about molecular signals in DSFGs. We review the current knowledge and the open questions about the interstellar medium of DSFGs, outlying the key role of molecular gas as a tracer and shaper of the star formation process.
Formation of Substructure in Luminous Submillimeter Galaxies (FOSSILS): Initial sample and the discovery of a dusty spiral at cosmic noon
SOKENDAI (The Graduate University for Advanced Studies)（日本综合研究大学院大学）；National Astronomical Observatory of Japan（日本国立天文台）；Hokkai-Gakuen University（北海学园大学）
JWST+ALMA reveal the build up of stellar mass in the cores of dusty star-forming galaxies at Cosmic Noon
University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）；Cosmic Dawn Center (DAWN)（黎明宇宙中心）；Tufts University（塔夫茨大学）；University of Geneva（日内瓦大学）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Technical University of Denmark（丹麦技术大学）
MEGA and SMILES Find Fewer Dusty Galaxies than Expected at Cosmic Noon
University of Kansas（堪萨斯大学）；Texas A&M University（德克萨斯农工大学）；NASA Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）；The University of Texas at Austin（得克萨斯大学奥斯汀分校）；Colby College（科尔比学院）；Rochester Institute of Technology（罗切斯特理工学院）
NIRSpec View of the Appearance and Evolution of Balmer Breaks and the Transition from Bursty to Smooth Star Formation Histories from Deep Within the Epoch of Reionization to Cosmic Noon
Chaotic Molecular Gas in Five Dusty Star-forming Galaxies in the Spiderweb Protocluster at $z = 2.16$
University of Arizona（亚利桑那大学）；University of California, Santa Barbara（加州大学圣塔芭芭拉分校）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；Technical University of Denmark（丹麦技术大学）
PASSAGES: The Discovery of a Strongly Lensed Protocluster Core Candidate at Cosmic Noon
School of Earth & Space Exploration, Arizona State University（亚利桑那州立大学地球与空间探索学院）；Department of Astronomy/Steward Observatory, University of Arizona（亚利桑那大学天文系/斯图尔德天文台）；Joint ALMA Observatory（ALMA联合天文台）；National Astronomical Observatory of Japan（日本国立天文台）；European Southern Observatory（欧洲南方天文台）；Department of Astronomy, University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校天文系）；National Radio Astronomy Observatory（美国国家射电天文台）
An ALMA sub-kiloparsec test of the Kennicutt--Schmidt relation in a strongly lensed dusty star-forming galaxy at $z\sim2.78$
Universidad de Valparaíso（瓦尔帕莱索大学）；Millenium Nucleus for Galaxies (MINGAL)（星系千年核（MINGAL））；STAR Institute（STAR研究所）；Université Côte d’Azur（蔚蓝海岸大学）；University of Florida（佛罗里达大学）；Universidad Nacional Autónoma de México（墨西哥国立自治大学）；Instituto Nacional de Astrofísica Óptica y Electrónica (INAOE)（国家天体物理学、光学和电子学研究所）；Universidad Central de Chile（智利中央大学）
PAHSPECS: JWST/MIRI Spectroscopy of PAHs at Cosmic Noon
Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CAB），西班牙国家航空航天技术研究所/西班牙国家研究委员会）；Institute of Astrophysics, Foundation for Research and Technology–Hellas (FORTH)（希腊研究与技术基金会天体物理研究所）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Department of Astronomy & Astrophysics, University of California San Diego（加州大学圣地亚哥分校天文与天体物理系）；Instituto de Estudios Astrofícos, Facultad de Ingeniería y Ciencias, Universidad Diego Portales（迭戈帕托莱斯大学工程与科学学院天体物理研究所）；Millenium Nucleus for Galaxies (MINGAL)（星系千年核心（MINGAL））；INAF Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（博洛尼亚空间天体物理学与科学国家研究院）
The DAWN JWST Archive: A spectroscopically-informed population study of the physical properties of galaxies at z>2
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）；Department of Astronomy, University of Geneva（日内瓦大学天文学系）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；DTU Space, Technical University of Denmark（丹麦技术大学空间科学部）
The Koi Pond: A Strongly Lensed Protocluster Core hosting a Diverse Population of DSFGs
Arizona State University（亚利桑那州立大学）；Joint ALMA Observatory（ALMA联合天文台）；National Astronomical Observatory of Japan（日本国立天文台）；European Southern Observatory（欧洲南方天文台）；Universidad Diego Portales（迭戈·波特莱斯大学）；University of Arizona（亚利桑那大学）；Chalmers University of Technology（查尔姆斯理工大学）
Evolution of the infrared luminosity function and its corresponding dust-obscured star formation rate density out to z~6
Institute of Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University（尼古拉·哥白尼大学物理、天文与信息学学院天体物理研究所）；National Centre for Nuclear Research（国家核研究中心）；Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh（爱丁堡大学天体物理研究所皇家天文台）；Astronomical Observatory Institute, Faculty of Physics and Astronomy, Adam Mickiewicz University（亚当·密茨凯维奇大学物理与天文学学院天文台研究所）
Outflows in the Early Universe: Neutral gas Absorption in Galaxies at z > 3 from low-resolution JWST Spectroscopy
Università di Bologna（博洛尼亚大学）；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与空间科学观测站）；University of Copenhagen（哥本哈根大学）；Swinburne University of Technology（斯威本科技大学）；University of Toronto（多伦多大学）
JWST Catches a Strongly Gravitationally Lensed AGN In Transition from Type II to Type I
Eureka Scientific（尤里卡科学）；University of Chicago（芝加哥大学）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理学研究所）；University of Washington（华盛顿大学）；Institute for Data-Intensive Research in Astrophysics and Cosmology (DiRAC), University of Washington（华盛顿大学天体物理学与宇宙学数据密集型研究所）；eScience Institute, University of Washington（华盛顿大学eScience研究所）；University of Michigan（密歇根大学）；University of Massachusetts（马萨诸塞大学）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；International Space Science Institute（国际空间科学研究所）
Gravitationally Lensed View of DSFG-1 in PLCK G165.7+67.0: Strong Dust Emission and Spatially Resolved Stellar Population Analysis with JWST and SMA
Chinese Academy of Sciences South America Center for Astronomy (CASSACA), National Astronomical Observatories(NAOC)（中国科学院南美天文中心（CASSACA），国家天文台）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；State Key Laboratory of Radio Astronomy and Technology, Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台射电天文与技术国家重点实验室）；Department of Physics and Astronomy, Chalmers University of Technology（查尔姆斯理工大学物理与天文系）；Sorbonne Université, UPMC Paris 6 and CNRS, UMR 7095, Institut d’Astrophysique de Paris（索邦大学，巴黎第六大学及法国国家科学研究中心，UMR 7095，巴黎天文研究所）；Department of Astronomy/Steward Observatory, University of Arizona（亚利桑那大学天文学系/斯图尔德天文台）
