Galaxy mergers play a critical role in galaxy evolution - altering the size, morphology, dynamics and composition of galaxies. So far, galaxy mergers have mostly been identified through visual inspection of their rest-frame optical and NIR emission. But, dust can obscure this emission, resulting in the misclassification of mergers as single galaxies, and the incorrect interpretation of their baryonic properties. Having serendipitously discovered a dust-obscured galaxy merger at z = 1.17, we aim to determine the baryonic properties of the two merging galaxies, including the star formation rate, and stellar, molecular gas, and dust masses. Using Band 3 and 6 observations from the Atacama Large Millimeter and submillimeter Array (ALMA), and ancillary data, we study the morphology of this previously misclassified merger. We deblend the emission, derive the gas masses from CO observations, and model the spectral energy distributions, to determine the properties of each galaxy. Using the rare combination of ALMA CO(2-1), CO(5-4) and dust-continuum (rest-frame 520um) observations, we provide insights into the gas and dust content and ISM properties of each merger component. We find that only one of the two galaxies is highly dust-obscured, whereas both are massive (> 10^10.5 Msun), highly star-forming (SFR = 60-900Msun/yr), have a moderate-to-low depletion time (tdepl < 0.7Gyr) and high gas fraction ( fgas >= 1). These properties can be interpreted as the positive impact of the merger. With this serendipitous discovery, we highlight the power of (sub)millimeter observations to identify and characterise the individual components of obscured galaxy mergers.
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）
ALMA Chemical Evolution (ACE) Survey: Molecular gas properties of low-mass, low-metallicity galaxies at cosmic noon
European Southern Observatory（欧洲南方天文台）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CAB），西班牙国家研究委员会-国家航空航天技术研究所）；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）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；Department of Astronomy, University of Florida（佛罗里达大学天文学系）；Department of Astronomy, University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校天文学系）
ALMA Chemical Evolution (ACE) survey: an overview -- extending dust and gas inference to low metallicities at cosmic noon
Centro de Astrobiología (CAB), CSIC-INTA（西班牙太空生物研究中心）；European Southern Observatory（欧洲南方天文台）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Department of Astronomy, University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校天文学系）；Department of Physics, University of California, Santa Barbara（加州大学圣塔芭芭拉分校物理系）；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·玻尔学院宇宙黎明中心及丹麦技术大学DTU空间）；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）；Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学天体物理学研究学院）；Department of Physics and Astronomy（物理与天文学系）
ALMA Chemical Evolution (ACE) survey: dust-to-gas ratios in sub-solar metallicity galaxies at cosmic noon
European Southern Observatory（欧洲南方天文台）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Centre for Astrobiology, Madrid（马德里天体生物学中心）；Department of Astronomy, University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校天文学系）；Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学天文学与天体物理学研究学院）；Department of Physics and Astronomy, University of California, Riverside（加州大学河滨分校物理与天文学系）；Department of Astronomy, University of Florida（佛罗里达大学天文学系）；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·玻尔研究所宇宙黎明中心及丹麦技术大学DTU空间部）
ALMA Chemical Evolution (ACE) survey: The gas fundamental metallicity relation at cosmic noon
Centro de Astrobiología (CAB), CSIC-INTA（西班牙国家研究委员会-国家航空航天技术研究所 天体生物学中心（CAB））；Leiden University（莱顿大学）；Australian National University（澳大利亚国立大学）；University of Florida（佛罗里达大学）；University of Copenhagen（哥本哈根大学）；Technical University of Denmark（丹麦技术大学）
ALMA High-J CO Spectroscopy of High-Redshift Galaxies. II. 0.03" Resolution CO Kinematics Reveal Super-Eddington Accretion in a Dust-Obscured Galaxy at z=3.111
Faculty of Engineering, Hokkai-Gakuen University（北海道学园大学工学部）
Star Formation and Nebular Attenuation from Pa$α$, Br$α$, and Br$β$ in Massive Dust-obscured Galaxies at Cosmic Noon using JWST
The University of Texas at Austin（德克萨斯大学奥斯汀分校）；University of Maryland, College Park（马里兰大学帕克分校）；University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）；Tufts University（塔夫茨大学）；Space Telescope Science Institute（太空望远镜科学研究所）；University of Arizona（亚利桑那大学）；California Institute of Technology（加州理工学院）
ALMA Chemical Evolution (ACE) survey: the dust content of subsolar metallicity galaxies at cosmic noon
Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心）；European Southern Observatory（欧洲南方天文台）；Leiden Observatory, Leiden University（莱顿大学天文台）；Department of Astronomy, University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校天文学系）；Departamento de Física de la Tierra y Astrofísica, Facultad de Ciencias Físicas, Universidad Complutense de Madrid（马德里康普顿斯大学物理科学学院地球与天体物理学系）；Department of Physics and Astronomy, University of California, Riverside（加州大学河滨分校物理与天文学系）；Department of Astronomy, University of Florida（佛罗里达大学天文学系）
Physical properties of hyperluminous, dust-obscured quasars at $z \sim 3$: multiwavelength Spectral Energy Distribution analysis and cold gas content revealed by ALMA
本文基于 ALMA 观测对 16 个 $z \sim 3$ 超亮尘埃遮挡类星体进行多波段 SED 分析，发现其分子气体含量低且消耗快，恒星形成效率高，表明正处于向未遮挡类星体过渡的短暂阶段。
The JWST Emission Line Survey (JELS): Multi-wavelength properties of Paschen line-emitters at Cosmic Noon
Instituto de Física y Astronomía, Universidad de Valparaíso（瓦尔帕莱索大学物理与天文学研究所）；Millennium Nucleus for Galaxies (MINGAL)（银河系千年核）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天文研究所）；Jodrell Bank Centre for Astrophysics, University of Manchester（曼彻斯特大学乔德雷尔银行天体物理学中心）；Institute of Science and Technology Austria (IS（奥地利科学与理工学院）
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）
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）
Constraining the nature of active galactic nuclei through circumgalactic Lya emission at z=2-3
Tsinghua University（清华大学）；University of Milan Bicocca（米兰比可卡大学）；Universität Heidelberg（海德堡大学）；National Astronomical Observatory of Japan（日本国立天文台）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Xi’an Jiaotong-Liverpool University（西交利物浦大学）
