Over the last decade, the Atacama Large Millimeter Array has revealed massive, dusty star-forming galaxies at $z\gtrsim5$, and the James Webb Space Telescope is primed to uncover even more information about them. These observations need dust evolution theory to provide context and are excellent benchmarks to test this theory. Here, we investigate the evolution of galactic dust budget at cosmic dawn using a suite of cosmological zoom-in simulations of moderately massive, high-redshift ($M_{\rm star}\gtrsim10^9 M_{\odot}$; $z\gtrsim5$) galaxies from the FIRE project, the highest resolution ($m_{\rm b} \approx 7100\, M_{\odot}$) of such simulations to date. Our simulations incorporate a dust evolution model that accounts for the dominant sources of dust production, growth, and destruction and follows the evolution of specific dust species, allowing it to replicate a wide range of present-day observations. We find, similar to other theoretical works, that dust growth via gas-dust accretion is the dominant producer of dust mass for these massive, $z\gtrsim 5$ galaxies. However, our fiducial model produces $M_{\rm dust}$ that fall ${\gtrsim}1$ dex below observations at any given $M_{\rm star}$ (typical uncertainties are ${\sim}1$ dex), which we attribute to reduced accretion efficiencies caused by a combination of low galactic metallicities and extremely bursty star formation. Modest enhancements (i.e., within observational/theoretical uncertainties) to accretion and SNe II dust creation raise $M_{\rm dust}$ by ${\lesssim}1$ dex, but this still falls below observations which assume $T_{\rm dust}\sim25$ K. One possibility is that inferred dust masses for $z\gtrsim4$ galaxies are overestimated, and recent observational/analytical works that find $T_{\rm dust}\sim50$ K along with metallicity constraints tentatively support this.
Quasars and the Intergalactic Medium at Cosmic Dawn
类星体在宇宙黎明提供了强有力的探测宇宙中最早的超大质量黑洞（SMBH）的形成和生长，它们与星系和结构形成的联系，以及星系际介质（IGM）在再电离时期（EoR）的演化。在宇宙历史的头十亿年里，已经发现了数百个类星体，类星体的红移边界扩展到z~7.6。对类星体在宇宙黎明的观测表明：（1）在z>5时，亮类星体的数密度呈指数下降，表明最早的类星体出现在z~10时;它们的平均光谱能量分布没有强烈的演化，表明活动星系核环境的迅速建立。(2)在z>7.5时，已经存在了10亿个太阳质量的黑洞;它们必须在不到7亿年的时间内形成和生长，通过大量早期黑洞种子与高效和持续的吸积相结合。(3)类星体的快速增长伴随着强烈的恒星形成和反馈活动，在其宿主星系，这表现出不同的形态和动力学性质，与典型的动力学质量低于本地BH/星系标度关系所暗示的。(4)类星体光谱中的HI吸收探测到宇宙再电离的尾端在z~5.3-6，并指出EoR的中点在6.9 < z < 7.6，IGM电离的空间起伏很大。重元素吸收线的观测表明，环银河系介质也经历了其电离结构和金属富集在EoR的演变。
Dust evolution across cosmic times as seen through DUSTY-GAEA
INAF – Astronomical Observatory of Trieste（意大利国家天体物理研究所的里雅斯特天文台）；University of Khartoum（喀土穆大学）；IFPU – Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；Tianjin Normal University（天津师范大学）；EPFL（洛桑联邦理工学院）
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）
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）
DeepDive: Simultaneous Formation of Massive Quiescent Galaxies in High-Redshift Galaxy Overdensities
The Graduate University for Advanced Studies, SOKENDAI（高级研究大学）；National Astronomical Observatory of Japan（日本国立天文台）；DTU Space, Technical University of Denmark（丹麦技术大学空间科学中心）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；Institute for Cosmic Ray Research, The University of Tokyo（东京大学宇宙射线研究所）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）
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）
Evidence for inefficient dust production in a massive, metal-rich galaxy at $z=7.13$ uncovered by JWST and ALMA
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）；DTU Space, Technical University of Denmark（丹麦技术大学空间研究所）；Department of Astronomy, University of Florida（佛罗里达大学天文学系）；Centre for Astrophysics Research, University of Hertfordshire（赫特福德大学天体物理研究中心）；Department of Physics, University of Surrey（萨里大学物理系）；Department of Physics and Astronomy, University of California, Riverside（加州大学河滨分校物理与天文系）；MIT Kavli Institute for Astrophysics and Space Research（麻省理工学院卡弗里天体物理与空间研究所）；Institute of Astronomy and Astrophysics, Academia Sinica（中央研究院天文及天文物理研究所）
