RUBIES: a complete census of the bright and red distant Universe with JWST/NIRSpec
Anna de Graaff, Gabriel Brammer, Andrea Weibel, Zach Lewis, Michael V. Maseda, Pascal A. Oesch, Rachel Bezanson, Leindert A. Boogaard, Nikko J. Cleri, Olivia R.… 展开作者
Anna de Graaff, Gabriel Brammer, Andrea Weibel, Zach Lewis, Michael V. Maseda, Pascal A. Oesch, Rachel Bezanson, Leindert A. Boogaard, Nikko J. Cleri, Olivia R. Cooper, Rashmi Gottumukkala, Jenny E. Greene, Michaela Hirschmann, Raphael E. Hviding, Harley Katz, Ivo Labbé, Joel Leja, Jorryt Matthee, Ian McConachie, Tim B. Miller, Rohan P. Naidu, Sedona H. Price, Hans-Walter Rix, David J. Setton, Katherine A. Suess, Bingjie Wang, Katherine E. Whitaker, Christina C. Williams
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21 pages, 16 figures; accepted for publication in A&A
We present the Red Unknowns: Bright Infrared Extragalactic Survey (RUBIES), providing JWST/NIRSpec spectroscopy of red sources selected across ~150 arcmin$^2$ from public JWST/NIRCam imaging in the UDS and EGS fields. RUBIES novel observing strategy offers a well-quantified selection function: the survey is optimised to reach high (>70%) completeness for bright and red (F150W-F444W>2) sources that are very rare. To place these rare sources in context, we simultaneously observe a reference sample of the 2<z<7 galaxy population, sampling sources at a rate that is inversely proportional to their number density in the 3D space of F444W magnitude, F150W-F444W colour, and photometric redshift. In total, RUBIES observes ~3000 targets across $1<z_{phot}<10$ with both the PRISM and G395M dispersers, and ~1500 targets at $z_{phot}>3$ using only the G395M disperser. The RUBIES data reveal a highly diverse population of red sources that span a broad redshift range ($z_{spec}\sim1-9$), with photometric redshift scatter and outlier fraction that are 3 times higher than for similarly bright sources that are less red. This diversity is not apparent from the photometric SEDs. Only spectroscopy reveals that the SEDs encompass a mixture of galaxies with dust-obscured star formation, extreme line emission, a lack of star formation indicating early quenching, and luminous active galactic nuclei. As a first demonstration of our broader selection function we compare the stellar masses and rest-frame U-V colours of the red sources and our reference sample: red sources are typically more massive ($M_*\sim10^{10-11.5} M_\odot$) across all redshifts. However, we find that the most massive systems span a wide range in U-V colour. We describe our data reduction procedure and data quality, and publicly release the reduced RUBIES data and vetted spectroscopic redshifts of the first half of the survey through the DJA.
RUBIES: The Evolution of the Ionization Parameter from 0 < z < 9
The Pennsylvania State University（宾夕法尼亚州立大学）；University of Wisconsin-Madison（威斯康星大学麦迪逊分校）；Center for Astrophysics, Harvard & Smithsonian（哈佛-史密森尼天体物理中心）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；EPFL（洛桑联邦理工学院）；University of Chicago（芝加哥大学）
A Comprehensive JWST/NIRSpec Census of Broad-line Active Galactic Nuclei: Faint, Low-mass Accretors and a Population of Little Red Dots
New York University（纽约大学）；Menlo School（门洛学校）；Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA)（天体物理跨学科探索与研究中心）；Northwestern University（西北大学）
An (in)complete NIRSpec census of Balmer absorption in Type 1 AGN -- radiation-driven outflows in little red dots, quasars and variable stars
University of Cambridge（剑桥大学）；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）；University College London（伦敦大学学院）
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）
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）
Blowing Star Formation Away in AGN Hosts (BAH) -- III. Serendipitous discovery of a $z\sim2.9$ star-forming galaxy lensed by the galactic bulge of CGCG 012-070 using JWST NIRSpec
JWST Census for the Mass-Metallicity Star-Formation Relations at z=4-10 with the Self-Consistent Flux Calibration and the Proper Metallicity Calibrators
The Cliff: A Metal-Poor Little Red Dot Hosting an Overmassive Black Hole at $z = 3.55$
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 and Astronomy, University College London（伦敦大学学院物理与天文学系）；Waseda Research Institute for Science and Engineering, Faculty of Science and Engineering, Waseda University（早稻田大学理工学术院理工学研究科）；Centre for Astrophysics Research, Department of Physics, Astronomy and Mathematics, University of Hertfordshire（赫特福德大学物理、天文与数学系天体物理学研究中心）；Centro de Astrobiología (CAB), CSIC–INTA（西班牙国家航空航天技术研究所/西班牙国家研究委员会天体生物学中心）；Weinberg Institute for Theoretical Physics, Texas Center for Cosmology and Astroparticle Physics, University of Texas at Austin（德克萨斯大学奥斯汀分校魏因伯格理论物理研究所宇宙学与高能天体物理中心）；Department of Physics, University of Texas at Austin（德克萨斯大学奥斯汀分校物理系）；Department of Astronomy, University of Texas at Austin（德克萨斯大学奥斯汀分校天文学系）；Department of Physics, University of Oxford（牛津大学物理系）
The GlimmIr: Spectroscopic Variability in a z~7 LRD Indicates Rapid Changes in Both the Narrow and Broad Line Regions
NASA Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）；University of Maryland, College Park（马里兰大学帕克分校）；Center for Research and Exploration in Space Science and Technology, NASA/GSFC（NASA/GSFC空间科学与技术探索研究中心）；Space Telescope Science Institute（太空望远镜科学研究所）；Center for Space Sciences and Technology, UMBC（马里兰大学巴尔的摩县分校空间科学与技术中心）
How much gas and dust is in the $z=5.7$ Lyman Break Galaxy HZ10? An ALMA Band 10 to 4 and JWST/NIRSpec study of its interstellar medium
Academia Sinica（中央研究院）；Universidad de Concepción（康塞普西翁大学）；Millennium Institute for Galaxies (MINGAL)（银河系千年研究所）；Universidad Diego Portales（迭戈·波特莱斯大学）；Chalmers University of Technology（查尔姆斯理工大学）；University of Maryland, College Park（马里兰大学帕克分校）；Leiden University（莱顿大学）；University of Western Australia（西澳大学）；University of Toronto（多伦多大学）；Ghent University（根特大学）；Foundation for Research and Technology Hellas (FORTH)（希腊研究与技术基金会）；European University Cyprus（塞浦路斯欧洲大学）；Caltech/IPAC（加州理工学院/IPAC）；Scuola Normale Superiore（比萨高等师范学院）；Space Telescope Science Institute（太空望远镜科学研究所）；SOKENDAI (The Graduate University for Advanced Studies)（综合研究大学院大学）；National Astronomical Observatory of Japan（日本国立天文台）；Hiroshima University（广岛大学）；University of Cambridge（剑桥大学）；National Radio Astronomy Observatory（美国国家无线电天文台）；Universidad de Granada（格拉纳达大学）；INAF – Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Flatiron Institute（平托研究所）；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台）；University of Sussex（萨塞克斯大学）
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）
DeepDive: A deep dive into the physics of the first massive quiescent galaxies in the Universe
Cosmic Dawn Center (DAWN)（宇宙黎明中心）；DTU Space, Technical University of Denmark（丹麦技术大学空间科学部）；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 Massachusetts, Amherst（马萨诸塞大学阿默斯特分校天文学系）；Department of Astronomy, The University of Texas at Austin（德克萨斯大学奥斯汀分校天文学系）；Department of Astronomical Science, The Graduate University for Advanced Studies, SOKENDAI（国立天文台大学校天文学研究科）；National Astronomical Observatory of Japan（日本国立天文台）；Institute of Astrophysics, National Taiwan University（台湾大学天体物理研究所）；David A. Dunlap Department of Astronomy and Astrophysics, University of Toronto（多伦多大学大卫A.邓普林天文学与天体物理学系）
The AGN nature of strong CIII emitters in the Early Universe with JWST
INAF – Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Dipartimento di Fisica, Università di Roma Sapienza（罗马第一大学物理系）；Physics Department, Tor Vergata University of Rome（罗马托尔维加塔大学物理系）；Institute of Physics, Laboratory for Galaxy Evolution and Spectral Modelling, EPFL（洛桑联邦理工学院星系演化与光谱建模实验室物理研究所）；University of the Pacific（太平洋大学）；Instituto de Astrofísica de Andalucía (IAA-CSIC)（安达卢西亚天体物理研究所）；Department of Physics and Astronomy, University of Kansas（堪萨斯大学物理与天文学系）；Department of Astronomy and Astrophysics, The Pennsylvania（宾夕法尼亚大学天文学与天体物理学系）
The Blue Jay Survey: Deep JWST Spectroscopy for a Representative Sample of Galaxies at Cosmic Noon
Università di Bologna（博洛尼亚大学）；INAF, Osservatorio di Astrofisica e Scienza dello Spazio（意大利国家天体物理研究所天文与空间科学观测站）；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）；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）；ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D)（ARC三维全天空天体物理卓越研究中心（ASTRO 3D））；Centre for Astrophysics and Supercomputing, Swinburne University of Technology（斯威本科技大学天体物理与超级计算中心）；Department of Astronomy and Astrophysics, The Pennsylvania State University（宾夕法尼亚州立大学天文与天体物理系）；Institute for Gravitation and the Cosmos, The Pennsylvania State University（宾夕法尼亚州立大学引力与宇宙学研究所）
The JWST Ultramassive Galaxy Sample -- I. Overview, Photometry, and Stellar Kinematics: Selecting Optimal Template Subsets via Non-Negative Matrix Factorization
University of Oxford（牛津大学）；University of Michigan（密歇根大学）；Space Telescope Science Institute（太空望远镜科学研究所）
Near-infrared emission line diagnostics for AGN from the local Universe to redshift 3
INAF - Osservatorio Astronomico di Roma（罗马天文台）；INAF - Osservatorio Astrofisico di Arcetri（阿切尔菲西天文台）；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 Padova（帕多瓦天文台）；Aix Marseille Univ, CNRS, CNES, LAM Marseille（艾克斯马赛大学）；Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM（巴黎萨克雷大学、巴黎西岱大学）；Instituto de Investigación Multidisciplinar en Ciencia y Tecnología, Universidad de La Serena（拉塞雷纳大学多学科科学技术研究所）；Departamento de Astronomía, Universidad de La Serena（拉塞雷纳大学天文学系）；Department of Astronomy, The University of Texas at Austin（德克萨斯大学奥斯汀分校天文学系）；Dipartimento di Fisica e Astronomia “G.Galilei”, Universitá di Padova（帕多瓦大学伽利略物理与天文学系）
The ionizing properties of JWST's compact broad-line emitters
Institute of Science and Technology Austria (ISTA)（奥地利科学技术研究所）；Princeton University（普林斯顿大学）；Massachusetts Institute of Technology（麻省理工学院）；MIT Kavli Institute for Astrophysics and Space Research（麻省理工学院卡弗里天体物理学与空间研究研究所）；University of Hawai’i（夏威夷大学）
