A$^{3}$COSMOS: A census on the molecular gas mass and extent of main-sequence galaxies across cosmic time
Tsan-Ming Wang, Benjamin Magnelli, Eva Schinnerer, Daizhong Liu, Ziad Aziz Modak, Eric Faustino Jiménez-Andrade, Christos Karoumpis, Vasily Kokorev, Frank Bertoldi
第一次限制在$0.4<z<3.6$的$>10^{10}$ M $_{\odot}$主序星（MS）星系的质量完整样本的分子气体的平均质量和范围。我们应用一个创新的$uv$为基础的叠加分析，一个大的档案阿塔卡玛大型毫米/亚毫米阵列（ALMA）的意见。这种叠加分析提供了星系群分子气体的平均质量和范围的测量。MS星系的分子气体质量随红移和恒星质量的变化而变化。在所有恒星质量下，分子气体分数从$z\sim3.2$到$z\sim0$减少了24倍。在给定的红移下，MS星系的分子气体比例随着恒星质量的减少而减少，其速度与它们的特定恒星形成率的减少大致相同。MS星系的分子气体耗尽时间大致保持在$z>0.5$，值为3亿~ 5亿r，但从$z\sim0.5$到$z\sim0$增加了3倍。MS星系的分子气体耗尽时间的这种演化可以从它们的分子气体表面密度的演化和一个似乎普遍的仅MS的$Σ_{M_{\rm mol}}-Σ_{\rm SFR}$关系来预测，其推断斜率为1.13，即，所谓的KS关系。MS星系的远红外尺寸没有随红移或恒星质量的显著变化，平均圆化半光半径为2.2 kpc。最后，我们的平均分子气体质量低于以前的估计，可能是由于文献研究偏向于单独检测的MS星系与大量的气体水库。一阶，分子气体含量的MS星系调节其恒星形成整个宇宙时间，而其恒星形成效率的变化起着次要的作用。尽管它们的气体含量和SFR有很大的演变，MS星系沿着一个似乎普遍的MS-唯一KS关系演变。
英文摘要：
To constrain for the first time the mean mass and extent of the molecular gas of a mass-complete sample of $>10^{10}$M$_{\odot}$ main-sequence (MS) galaxies at $0.4<z<3.6$. We apply an innovative $uv$-based stacking analysis to a large set of archival Atacama Large Millimeter/submillimeter Array (ALMA) observations. This stacking analysis provides measurements of the mean mass and extent of the molecular gas of galaxy populations. The molecular gas mass of MS galaxies evolves with redshift and stellar mass. At all stellar masses, the molecular gas fraction decreases by a factor of 24 from $z\sim3.2$ to $z\sim0$. At a given redshift, the molecular gas fraction of MS galaxies decreases with stellar mass, at roughly the same rate as their specific star formation rate decreases. The molecular gas depletion time of MS galaxies remains roughly constant at $z>0.5$ with a value of 300--500 Myr, but increases by a factor of 3 from $z\sim0.5$ to $z\sim0$. This evolution of the molecular gas depletion time of MS galaxies can be predicted from the evolution of their molecular gas surface density and a seemingly universal MS-only $Σ_{M_{\rm mol}}-Σ_{\rm SFR}$ relation with an inferred slope of 1.13, i.e., the so-called KS relation. The far-infrared size of MS galaxies shows no significant evolution with redshift or stellar mass, with a mean circularized half-light radius of 2.2 kpc. Finally, our mean molecular gas masses are lower than previous estimates, likely caused by the fact that literature studies were biased towards individually-detected MS galaxies with massive gas reservoirs. To first order, the molecular gas content of MS galaxies regulates their star formation across cosmic time, while variation of their star formation efficiency plays a secondary role. Despite a large evolution of their gas content and SFRs, MS galaxies evolved along a seemingly universal MS-only KS relation.
COSMOS2025: A Machine Learning Census of Massive Quiescent Galaxies at $2.5 < \text{z} < 5$
Institute for Advanced Studies in Basic Sciences (IASBS)（基础科学高等研究所）；Universität Bonn（波恩大学）；Institute for Research in Fundamental Sciences (IPM)（伊朗基本科学研究中心）
The Large Early Galaxy Astrophysics Census (LEGA-C) Data Release II: dynamical and stellar population properties of z ~< 1 galaxies in the COSMOS field
CHAMPS: The COSMOS High-Redshift ALMA-MIRI Population Survey - A New Census of the Dusty Early Universe
California Institute of Technology（加州理工学院）；Rochester Institute of Technology（罗切斯特理工学院）；Universidad Diego Portales（迭戈帕托莱斯大学）；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）；The University of Tokyo（东京大学）
A census of star-formation and gas mass tracers in two lensed $z \sim 4$ dusty star-forming galaxies
University of Illinois（伊利诺伊大学）；National Center for Supercomputing Applications（国家超级计算应用中心）；Texas A&M University（德克萨斯农工大学）；Stony Brook University（石溪大学）；Universidad Diego Portales（迭戈·波特莱斯大学）
An ALMA survey of submillimetre galaxies in the COSMOS field: The extent of the radio-emitting region revealed by 3 GHz imaging with the Very Large Array
A GLIMPSE of the 99%: a census of the faintest galaxies during the epoch of reionization and its implications for galaxy formation models
Sorbonne Université（索邦大学）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；Univ Lyon, Univ Lyon1, Ens de Lyon（里昂大学，里昂第一大学，巴黎高等师范学校里昂分校）；University of Geneva（日内瓦大学）；Tufts University（塔夫茨大学）；Leiden Observatory（莱顿天文台）；Space Telescope Science Institute（太空望远镜科学研究所）；Rutgers University（罗格斯大学）
