Cold hydrogen gas is the raw fuel for star formation in galaxies, and its partition into atomic and molecular phases is a key quantity for galaxy evolution. In this Letter, we combine Atacama Large Millimeter/submillimeter Array and Arecibo single-dish observations to estimate the molecular-to-atomic hydrogen mass ratio for massive star-forming galaxies at $z\sim$ 0.2 extracted from the HIGHz survey, i.e., some of the most massive gas-rich systems currently known. We show that the balance between atomic and molecular hydrogen in these galaxies is similar to that of local main-sequence disks, implying that atomic hydrogen has been dominating the cold gas mass budget of star-forming galaxies for at least the past three billion years. In addition, despite harboring gas reservoirs that are more typical of objects at the cosmic noon, HIGHz galaxies host regular rotating disks with low gas velocity dispersions suggesting that high total gas fractions do not necessarily drive high turbulence in the interstellar medium.
Dynamical Evidence for a Billion Solar Mass Black Hole in Galaxy NGC 4061 from ALMA $^{12}$CO(2-1) Kinematics
University of Michigan（密歇根大学）；Faculty of Physics—Engineering Physics, University of Science, Vietnam National University in Ho Chi Minh City（越南国立大学胡志明市科大学物理-工程物理学院）；Department of Physics, International University, Vietnam National University in Ho Chi Minh City（越南国立大学胡志明市国际大学物理系）；Black Hole Initiative, Harvard University（哈佛大学黑洞倡议项目）
ALMA Imaging of Gas and Dust in a Galaxy Protocluster at Redshift 5.3: [CII] Emission in "Typical" Galaxies and Dusty Starbursts ~1 Billion Years after the Big Bang
The Growth of Dust in Galaxies in the First Billion Years with Applications to Blue Monsters
University of Florida（佛罗里达大学）；Cosmic Dawn Center at the Niels Bohr Institute, University of Copenhagen and DTU-Space, Technical University of Denmark（哥本哈根大学尼尔斯·玻尔研究所黎明中心及丹麦技术大学DTU空间）；University of Virginia（弗吉尼亚大学）；Virginia Institute for Theoretical Astronomy, University of Virginia（弗吉尼亚理论天文学研究所）；The NSF-Simons AI Institute for Cosmic Origins, USA（美国NSF-西蒙斯宇宙起源人工智能研究所）；University of California（加州大学）；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）；University of 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）；Universi（大学）
Highly-ionized gas in lensed z = 6.027 Little Red Dot seen through [OIII] 88$μ$m with ALMA
Chalmers University of Technology（查尔姆斯理工大学）；Durham University（杜伦大学）；University of KwaZulu-Natal（夸祖鲁-纳塔尔大学）；Universidade Federal do Rio de Janeiro（里约热内卢联邦大学）；University of Arizona（亚利桑那大学）；Columbia University（哥伦比亚大学）；Flatiron Institute（平顿研究所）
The ALMA Spectroscopic Survey in the HUDF: Constraining cumulative CO emission at $1 \lesssim z \lesssim 4$ with power spectrum analysis of ASPECS LP data from 84 to 115 GHz
我们提出了一个功率谱分析的ALMA光谱测量大型计划（ASPECS LP）的数据从84到115 GHz。这些数据主要探测小尺度波动（$k=10$ - $100$ h Mpc $^{-1}$）在星系中的CO排放总量在$1 \lesssim z \lesssim 4$。我们放置一个积分约束CO光度函数（LF）在这个红移范围内，通过直接测量其在三维（3D）自功率谱的二阶矩，找到一个总CO散粒噪声功率$P_{\textrm{CO,CO}}(k_{\textrm{CO(2-1)}}) \leq 1.9\times10^2$ $μ$ K $^2$（Mpc h $^{-1}$）$^3$。该上限（$3σ$）与Decarli等人2019年观察到的ASPECS CO LF一致，但排除了从这些LF推断的$P_{\textrm{CO,CO}}(k_{\textrm{CO(2-1)}})$范围内的较大空间，我们将其主要归因于$z > 2$处Schechter型CO LF的归一化$Φ_*$和膝关节$L_*$的较大不确定性。此外，通过功率谱分析的ASPECS LP数据与415个位置的可用的光学光谱红移的星系，我们发现，所观察到的平均CO强度和散粒噪声功率的MUSE星系的贡献主要是由ASPECS盲检测，虽然有$\sim20$ %的贡献CO（2-1）的平均强度由于源先前未检测到的盲线搜索。最后，我们从个人的盲目CO检…
JWST Spectroscopic Census of ALMA Faint Submillimeter Galaxies in the Hubble Ultra Deep Field
The Graduate University for Advanced Studies, SOKENDAI（日本高级研究院）；National Astronomical Observatory of Japan（日本国立天文台）；Institute for Cosmic Ray Research, The University of Tokyo（东京大学宇宙射线研究所）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo（东京大学 Kavli 宇宙物理数学研究所）；David A. Dunlap Department of Astronomy and Astrophysics, University of Toronto（多伦多大学大卫·邓普天文学与天体物理学系）；Dunlap Institute for Astronomy and Astrophysics（邓普天文学与天体物理学研究所）
An ALMA Band 7 survey of SDSS/Herschel quasars in Stripe 82: II. The nature of FIR-bright quasars
Instituto de Astrofísica de Canarias（加那利天体物理研究所）；Universidad de La Laguna（拉帕鲁纳大学）；European Southern Observatory（欧洲南方天文台）；Joint ALMA Observatory（ALMA联合天文台）；University of Hawai’i（夏威夷大学）；INAF-Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；SRON Netherlands Institute for Space Research（荷兰空间研究研究所）；University of Groningen（格罗宁根大学）；Universidade de Pernambuco（伯南布哥大学）；Universidade Federal Rural de Pernambuco（伯南布哥联邦农村大学）
ALMA Polarization Study of the Magnetic Fields in Two Massive Clumps in the 20 km s$^{-1}$ Cloud of the Central Molecular Zone
Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；State Key Laboratory of Radio Astronomy and Technology（射电天文与技术国家重点实验室）；National Astronomical Observatory of Japan（日本国立天文台）；School of Astronomy and Space Science, Nanjing University（南京大学天文与空间科学学院）；Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education（教育部现代天文与天体物理重点实验室（南京大学））；Department of Physics, National Sun Yat-Sen University（国立中山大学物理系）；Center of Astronomy and Gravitation, National Taiwan Normal University（国立台湾师范大学天文与重力研究中心）
ALMA观测揭示了中央分子区20 km s$^{-1}$云中两个团块的磁场特性，显示磁场在云尺度占主导，但重力在核心和凝聚尺度起主导作用，且磁场不足以阻止气体坍缩。
The ALMaQUEST Survey XVII: Unveiling Multiple Quenching Pathways in Green Valley Galaxies via Molecular Gas and Quenching Timescale Analyses
Institute of Astronomy & Astrophysics, Academia Sinica（中央研究院天文及天文物理研究所）；Graduate Institute of Astrophysics and Department of Physics, National Taiwan University（国立台湾大学天体物理研究所暨物理系）；Argelander-Institut für Astronomie, Universität Bonn（波恩大学阿尔兰德天文学研究所）；Stocker AstroScience Center, Dept. of Physics, Florida International University（佛罗里达国际大学斯托克天体科学中心物理系）；Department of Physics, Tamkang University（淡江大学物理系）；Department of Physics & Astronomy, University of Victoria（维多利亚大学物理与天文系）；Space Telescope Science Institute（太空望远镜科学研究所）；William H. Miller III Department of Physics and Astronomy, Johns Hopkins University（约翰斯·霍普金斯大学威廉·H·米勒三世物理与天文系）；Instituto de Astronomía, Universidad Nacional Autónoma de México（墨西哥国立自治大学天文学研究所）
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
Unveiling the Chemical Complexity and C/O Ratio of the HD 163296 Protoplanetary Disk: Constraints from Multi-line ALMA Observations of Organics, Nitriles, Sulfur-bearing, and Deuterated Molecules
National Institute of Science Education and Research（印度科学教育研究所）；Homi Bhabha National Institute（霍米·巴巴国立学院）；University of Michigan（密歇根大学）；California Institute of Technology（加州理工学院）；Jet Propulsion Laboratory（喷气推进实验室）；Academia Sinica Institute of Astronomy and Astrophysics（中央研究院天文及天文物理研究所）；Max Planck Institute for Astronomy（马克斯·普朗克天体物理学研究所）；National Astronomical Observatory of Japan（日本国立天文台）；SOKENDAI（综合研究大学院大学）
Net-zero gas inflow: Measurement of the gas consumption history of a massive quiescent galaxy
University of Cambridge（剑桥大学）；University College London（伦敦大学学院）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CAB），西班牙高等科学研究理事会-国家航空航天技术研究所）；European Space Agency (ESA), European Space Astronomy Centre (ESAC)（欧洲空间局（ESA），欧洲空间天文中心（ESAC））；NSF’s National Optical-Infrared Astronomy Research Laboratory（美国国家光学-红外天文研究实验室）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；INAF - Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；University of Oxford（牛津大学）；Scuola Normale Superiore（比萨高等师范学院）
The Baryon Budget of Galaxies across the First Billion Years
INAF-Italian National Institute of Astrophysics（意大利国家天体物理研究所）；Institute for Fundamental Physics of the Universe（基础物理宇宙研究所）；European Southern Observatory（欧洲南方天文台）；Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille)（艾克斯马赛大学、法国国家科学研究中心、马赛天体物理学实验室）
