An optically-dark merging system at z~6 detected by JWST
Giulia Rodighiero, Andrea Enia, Laura Bisigello, Giorgia Girardi, Giovanni Gandolfi, Mahsa Kohandel, Andrea Pallottini, Nicolo' Badinelli, Andrea Grazian, Andre… 展开作者
Giulia Rodighiero, Andrea Enia, Laura Bisigello, Giorgia Girardi, Giovanni Gandolfi, Mahsa Kohandel, Andrea Pallottini, Nicolo' Badinelli, Andrea Grazian, Andrea Ferrara, Benedetta Vulcani, Alessandro Bianchetti, Antoninto Marasco, Francesco Sinigaglia, Marco Castellano, Paola Santini, Paolo Cassata, Enrico Maria Corsini, Carlotta Gruppioni
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Accepted for publication in Astronomy & Astrophysics
Near- to mid-Infrared observations (from Spitzer and JWST) have revealed a hidden population of galaxies at redshift z=3-6, called optically-dark objects, which are believed to be massive and dusty star-formers. While optically-dark sources are widely recognized as a significant component of the stellar mass function, the history of their stellar mass assembly remains unexplored. However, they are thought to be the progenitors of the more massive early-type galaxies found in present-day groups and clusters. It is thus important to examine the possible connection between dark sources and merging events, in order to understand the environment in which they live. Here, we report our search for close companions in a sample of 19 optically-dark objects identified in the SMACS0723 JWST deep field. They were selected in the NIRCam F444W band and undetected below 2mu. We restrict our analysis to the reddest (i.e. F277W-F444W> 1.3) and brightest (F444W< 26 mag) objects. We have identified an optically-dark source showing a very close companion (<0.5"). The spatially resolved SED fitting procedure indicates that all components lying within 1.5" from the dark source are indeed at z~5.7. Tidal features (leading to a whale shaped morphology) corroborate the hypothesis that the dark source is the most massive (log(M/Msun)>10.3) and dusty (Av~3 at the core) system of an ongoing merger with a mass ratio of ~10. Similar merging systems are identified in the SERRA simulations, allowing us to reconstruct their stellar mass assembly history and predict their molecular gas properties The discovery of mergers within dark galaxies at the end of the Epoch of Reionization underscores the importance of conducting a statistical search for additional candidates in deep NIRCam fields. Such research will aid in understanding the role of merging processes during the obscured phase of stellar mass accumulation.
Stellar Morphology of Optically Dark or Faint Galaxies at $z>3$ with JWST
University of Geneva（日内瓦大学）；Heidelberg University（海德堡大学）；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）；University of Sussex（萨塞克斯大学）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）
Mergers Drive Structural Complexity but Not Starbursts in Lyman-$α$ Emitters at $3 < z < 4$: A JWST Spatially Resolved View
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台光学天文重点实验室）；School of Astronomy and Space Science, University of Chinese Academy of Science（中国科学院大学天文与空间科学学院）；Key Laboratory of Space Astronomy and Technology, National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台空间天文与技术重点实验室）；College of Physical Science and Technology, Shenyang Normal University（沈阳师范大学物理科学与技术学院）
研究发现3 < z < 4的Lyman-α发射体中合并驱动结构复杂性，但未引发显著恒星爆发，通过JWST空间分辨分析揭示合并对LAEs特性的影响。
A cosmic collision in the making: JWST/NIRISS reveals a merging and maturing protocluster core at z~3 around a red quasar
Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut（海德堡大学天文学中心，天文计算研究所）；Space Telescope Science Institute（太空望远镜科学研究所）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Department of Physics, Rhodes College（罗德学院物理系）；Department of Physics and Astronomy, Bloomberg Center, Johns Hopkins University（约翰斯·霍普金斯大学彭博中心物理与天文学系）；Institute for Advanced Study（高等研究院）；Department of Astronomy and Joint Space-Science Institute, University of Maryland, College Park（马里兰大学帕克分校天文学系及联合空间科学研究所）；Departamento de Astronomia, Instituto de Física, Universidade Federal do Rio Grande do Sul（南里奥格兰德联邦大学物理研究所天文学系）
Tracing the earliest stages of star and cluster formation in 19 nearby galaxies with PHANGS-JWST and HST: compact 3.3 $μ$m PAH emitters and their relation to the optical census of star clusters
GA-NIFS: interstellar medium properties and tidal interactions in the evolved massive merging system B14-65666 at z=7.152
University of Cambridge（剑桥大学）；University of Oxford（牛津大学）；The University of Manchester（曼彻斯特大学）；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）；Scuola Normale Superiore（比萨高等师范学院）；Sorbonne Université（索邦大学）
The Cosmic Owl: Twin Active Collisional Ring Galaxies with Starburst Merging Front at $z=1.14$
Tsinghua University（清华大学）；National Radio Astronomy Observatory（国家射电天文台）；The University of Tokyo（东京大学）；Kavli Institute for the Physics and Mathematics of the Universe (WPI)（宇宙物理与数学研究 Kavli 研究所（WPI））；Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS（数据驱动发现中心，Kavli IPMU（WPI），UTIAS）；Aix Marseille Univ.（艾克斯马赛大学）；CNRS（法国国家科学研究中心）；CNES（法国国家空间研究中心）；LAM（拉格朗日天体物理学实验室）；European Southern Observatory（欧洲南方天文台）
Cloud-Cloud Collisions Induce Filament-Mediated Super Star Cluster Formation in the Antennae Overlap Region: Evidence from ALMA and JWST
Shunan University（周南大学）；Shizuoka University（静冈大学）；National Astronomical Observatory of Japan, National Institutes of Natural Sciences（日本国立天文台，国立自然科学研究院）；The Graduate University for Advanced Studies, SOKENDAI（综合研究大学院大学）；Kagawa University（香川大学）；Gifu University（岐阜大学）
NGDEEP Epoch 1: Spatially Resolved H$α$ Observations of Disk and Bulge Growth in Star-Forming Galaxies at $z \sim$ 0.6-2.2 from JWST NIRISS Slitless Spectroscopy
Reionization and the ISM/Stellar Origins with JWST and ALMA (RIOJA): The core of the highest redshift galaxy overdensity at $z = 7.88$ confirmed by NIRSpec/JWST
The descendants of $z \gtrsim 10$ JWST galaxies in the COLIBRE simulations
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；University of Chinese Academy of Sciences（中国科学院大学）；Durham University（杜伦大学）；Leiden University（莱顿大学）；Leibniz-Institut für Astrophysik Potsdam (AIP)（波茨坦阿斯特罗物理研究所）
The ALPINE-CRISTAL-JWST Survey: Chemical Abundance Comparison Between the ISM and CGM of Main-Sequence Galaxies at z=4-6
Caltech/IPAC（加州理工学院/IPAC）；INAF – Osservatorio di Astrofisica e Scienza dello Spazio di 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）；Dipartimento di Fisica “Enrico Fermi”, Universitá di Pisa（比萨大学恩里科·费米物理系）；Scuola Internazionale Superiore Studi Avanzati (SISSA)（国际高等研究院）；Istituto Nazionale di Fisica Nucleare (INFN)-Sezione di Trieste（意大利国家核物理研究所的里雅斯特分部）；Istituto di Radioastronomia dell’Istituto Nazionale di Astrofisica (IRA-INAF)（意大利国家天体物理研究所射电天文研究所）；Department of Physics and Astronomy, University of California, Riverside（加州大学河滨分校物理与天文学系）
Spatially resolved metallicity and ionization in the merging system Gz9p3 at z=9.3
Stockholm University（斯德哥尔摩大学）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CAB），西班牙国家研究委员会-国家航空技术研究所）；Space Telescope Science Institute (STScI)（太空望远镜科学研究所）；University of Copenhagen（哥本哈根大学）；UK Astronomy Technology Centre, Royal Observatory Edinburgh（英国天文学技术中心，爱丁堡皇家天文台）
The Hidden Life of Stars: Embedded Beginnings to AGB Endings in the PHANGS-JWST Sample. I. Catalog of Mid-IR Sources
University of Alberta（阿尔伯塔大学）；The Ohio State University（俄亥俄州立大学）；Center for Cosmology and Astroparticle Physics (CCAPP)（宇宙学与亚原子物理中心）；UCSD（加州大学圣地亚哥分校）；Université Côte d’Azur（蔚蓝海岸大学）；Observatoire de la Côte d’Azur（蔚蓝海岸天文台）；CNRS, Laboratoire Lagrange（法国国家科学研究中心，拉格朗日实验室）；The Johns Hopkins University（约翰斯·霍普金斯大学）；Space Telescope Science Institute（太空望远镜科学研究所）；European Southern Observatory（欧洲南方天文台）；Max-Planck-Institut für Extraterrestrische Physik (MPE)（马克斯·普朗克地外物理学研究所）
Tianjin Astrophysics Center, Tianjin Normal University（天津师范大学天体物理中心）；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））；National Astronomical Observatory, Chinese Academy of Sciences（中国科学院国家天文台）；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）
Comprehensive JWST+ALMA Study on the Extended Ly$α$ Emitters, Himiko and CR7 at $z\sim 7$: Blue Major Merger Systems in Stark Contrast to Submillimeter Galaxies
JWST and Keck observations of the off-nuclear tidal disruption event TDE 2025abcr: An evolving reprocessing layer
UC Santa Cruz（加州大学圣克鲁兹分校）；University of California Observatories（加州大学天文台）；University of California, Berkeley（加州大学伯克利分校）；University of Illinois at Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；Center for Astrophysics | Harvard & Smithsonian（哈佛史密森尼天体物理中心）；University of Texas Austin（德克萨斯大学奥斯汀分校）
Stellar masses of optically dark galaxies: uncertainty introduced by the attenuation law and star-formation histories
Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Cavendish Laboratory, University of Cambridge（剑桥大学卡文迪许实验室）；Department of Physics, University of Oxford（牛津大学物理系）
A SPectroscopic survey of biased halos In the Reionization Era (ASPIRE): Impact of Galaxies on the CGM Metal Enrichment at z > 6 Using the JWST and VLT
Early steps in the hierarchical assembly of a Milky Way-mass galaxy 1 Gyr after the Big Bang
Dunlap Institute for Astronomy and Astrophysics（邓拉普天体物理与天文研究所）；Department of Astronomy and Physics and Institute for Computational Astrophysics, Saint Mary’s University（圣玛丽大学天文物理系及计算天体物理研究所）；Waseda Research Institute for Science and Engineering, Faculty of Science and Engineering, Waseda University（早稻田大学理工学部理工学研究科）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡佩恩天文研究所）；Faculty of Mathematics and Physics, University of Ljubljana（卢布尔雅那大学数学物理学院）；Department of Physics and Astronomy, University of California Davis（加州大学戴维斯分校物理与天文学系）
