A Morphology Catalog of Galaxies in CEERS: Evolution in the Size and Color Gradients of Galaxies Since Cosmic Dawn
Colby College（科尔比学院）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；University of the Pacific（太平洋大学）；Columbia University（哥伦比亚大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Rochester Institute of Technology（罗切斯特理工学院）；Universidad de La Serena（拉塞雷纳大学）；Instituto de Astrofísica de Andalucía (CSIC)（安达卢西亚天体物理学研究所（西班牙国家科学研究委员会））；ARAID Foundation. Centro de Estudios de Física del Cosmos de Aragón (CEFCA)（阿拉贡宇宙物理研究中心基金会）；University of Kansas（堪萨斯大学）
Elizabeth J. McGrath, Steven L. Finkelstein, Guillermo Barro, Viraj Pandya, Jeyhan S. Kartaltepe, Dale D. Kocevski, Ricardo O. Amorín, Bren E. Backhaus, Fernand… 展开作者
Elizabeth J. McGrath, Steven L. Finkelstein, Guillermo Barro, Viraj Pandya, Jeyhan S. Kartaltepe, Dale D. Kocevski, Ricardo O. Amorín, Bren E. Backhaus, Fernando Buitrago, Antonello Calabrò, Yingjie Cheng, Luca Costantin, Isa G. Cox, Kelcey Davis, Giovanni Gandolfi, Yuchen Guo, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Marc Huertas-Company, Anton M. Koekemoer, Ray A. Lucas, Bahram Mobasher, Fabio Pacucci, Casey Papovich, Pablo G. Pérez-González, Jonathan R. Trump, L. Y. Aaron Yung, Pablo Arrabal Haro, Micaela B. Bagley, Mark Dickinson, Adriano Fontana, Andrea Grazian, Norman A. Grogin, Lisa J. Kewley, Allison Kirkpatrick, Jennifer M. Lotz, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Stephen M. Wilkins, Guang Yang, Lise-Marie Seillé, Xin Wang
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22 pages, 9 figures. Accepted for publication in ApJ Letters, CEERS focus issue
We present measurements of morphological parameters from fitting 53,885 galaxies detected to a magnitude limit of F356W$< 28.5$ in the CEERS NIRCam imaging with galfit in six broadband filters: F115W, F150W, F200W, F277W, F356W, and F444W. We provide a public catalog of Sérsic index, effective semi-major axis, axis ratio, integrated magnitude, and position angle for these galaxies in each of the filters. Uncertainties in the measured parameters are estimated from simulated galaxies that have similar noise and background properties as the observed galaxies. We compare our measurements with those in the CANDELS/EGS field measured with HST/WFC3 and find that the sizes agree to within 0.09 dex and the Sérsic indices agree to within 0.13 dex. We further present the evolution in the size-mass relation, and find that the evolution to $z\sim9$ is consistent with previous results derived at lower redshift. Finally, we look at the color gradients of galaxies at $1<z<5$ and find that for late-type galaxies ($n<2.5$), there is a strong dependence on mass, but no apparent evolution with redshift, indicating that the stellar populations and dust attenuation in more massive galaxies vary substantially with radius and contribute to significant morphological $k-$corrections. For early type galaxies ($n>2.5$), the color gradients are nearly flat with no dependence on mass, indicating that the stellar populations are more uniform throughout. The structural measurements presented are accurate to $20\%$ or better for most galaxies with F356W $<27.0$ mag and will enable further studies of galaxy morphology to $z\sim10$.
Ultra High-Redshift or Closer-by, Dust-Obscured Galaxies? Deciphering the Nature of Faint, Previously Missed F200W-Dropouts in CEERS
Università di Padova（帕多瓦大学）；INAF, Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Department of Astronomy, The University of Texas at Austin（德克萨斯大学奥斯汀分校天文学系）；NSF’s National Optical-Infrared Astronomy Research Laboratory（美国国家光学-红外天文研究实验室）；INAF, Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Department of Physics and Astronomy, Texas A&M University（得克萨斯农工大学物理与天文系）
Beyond the Monsters: A More Complete Census of Black Hole Activity at Cosmic Dawn
Providence College（普罗维登斯学院）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；University of Connecticut（康涅狄格大学）；The Pennsylvania State University（宾夕法尼亚州立大学）；University of Massachusetts Amherst（马萨诸塞大学阿默斯特分校）；Space Telescope Science Institute（空间望远镜科学研究所）；Ecole Polytechnique Fédérale de Lausanne (EPFL)（洛桑联邦理工学院）；University of Louisville（路易斯维尔大学）；Rochester Institute of Technology（罗切斯特理工学院）；Colby College（科尔比学院）；Harvard University（哈佛大学）；University of Chinese Academy of Sciences (UCAS)（中国科学院大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Beijing Normal University（北京师范大学）
Skyfire: A Spectroscopic Census of Little Red Dots and Broad-Line AGN in the CEERS Field
Colby College（科尔比学院）；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（宇宙前沿中心，德克萨斯大学奥斯汀分校）；Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), The University of Tokyo（东京大学宇宙物理与数学研究所（Kavli IPMU，WPI））；Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学科维理天文与天体物理研究所）；University of the Pacific（太平洋大学）；Peking University（北京大学）；Astrophysics Science Division, NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心天体物理学部）；University of Connecticut（康涅狄格大学）；Space Telescope Science Institute（空间望远镜科学研究所）
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）
Witnessing downsizing in the making: quiescent and breathing galaxies at the dawn of the Universe
University of Southampton（南安普顿大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Harvard University（哈佛大学）；University of California, Irvine（加州大学尔湾分校）；EPFL（洛桑联邦理工学院）；University of the Pacific（太平洋大学）；NSF's National Optical-Infrared Astronomy Research Laboratory（美国国家光学-红外天文研究实验室）；University of Chinese Academy of Sciences (UCAS)（中国科学院大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Beijing Normal University（北京师范大学）
PANORAMIC: The Dawn of Massive Quiescent Galaxies I. Number Density and Cosmic Variance from 1000 arcmin$^2$ NIRCam Imaging
University of Arizona（亚利桑那大学）；NSF–DOE Vera C. Rubin Observatory/NSF NOIRLab（美国国家科学基金会-能源部维拉·C·鲁宾天文台/美国国家光学红外天文研究实验室）；University of Geneva（日内瓦大学）；Princeton University（普林斯顿大学）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；University of Pittsburgh（匹兹堡大学）；University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）；Cosmic DAWN Center, Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所宇宙黎明中心）
No evolution in the number density of little red dots from cosmic dawn to cosmic noon
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 e Astronomia, Università di Bologna（博洛尼亚大学物理与天文系）；Space Telescope Science Institute for the European Space Agency (ESA), ESA Office（欧洲空间局太空望远镜科学研究所）；The 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）；INAF – Arcetri Astrophysical Observatory（意大利国家天体物理研究所阿切尔奇天文台）
Cosmic Vine: High abundance of massive galaxies and dark matter halos in a forming cluster at z=3.44
Cosmic Dawn Center (DAWN)（宇宙黎明中心）；DTU Space, Technical University of Denmark（丹麦技术大学空间研究所）；CEA, IRFU, DAp, AIM, Université Paris-Saclay, Université Paris Cité, Sorbonne Paris Cité, CNRS（法国原子能和替代能源委员会、法国研究与发展创新局、达普实验室、天体物理与成像实验室、巴黎萨克雷大学、巴黎西岱大学、索邦巴黎西岱大学、法国国家科学研究中心）；Instituto de Física, Pontificia Universidad Católica de Valparaíso（天主教瓦莱帕尔索大学物理研究所）；Instituto de Física y Astronomía, Universidad de Valparaíso（瓦尔帕莱索大学物理与天文研究所）；Millennium Nucleus for Galaxies (MINGAL)（星系千年核）；School of Astronomy and Space Science, Nanjing University（南京大学天文与空间科学学院）
Euclid preparation: TBD. Cosmic Dawn Survey: evolution of the galaxy stellar mass function across 0.2<z<6.5 measured over 10 square degrees
Institute for Astronomy, University of Hawaii（夏威夷大学天文研究所）；Department of Astronomy, University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校天文学系）；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）；Caltech/IPAC（加州理工学院/IPAC）
Pushing JWST to the extremes: search and scrutiny of bright galaxy candidates at z$\simeq$15-30
INAF（意大利国家天体物理研究所）；Sapienza, Università di Roma（罗马第一大学）；Centro de Astrobiología (CAB), CSIC–INTA（西班牙国家航空航天技术研究所与西班牙高等科学研究中心联合天文生物学家中心）；University of Massachusetts（马萨诸塞大学）；NSF’s NOIRLab（美国国家科学基金会地下光学红外天文实验室）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；University of California, Los Angeles（加州大学洛杉矶分校）
