利用 JWST PRIMER 研究 $z\simeq3-5$ 处明亮 Lyman-break 星系的尺寸
The sizes of bright Lyman-break galaxies at $z\simeq3-5$ with JWST PRIMER
R. G. Varadaraj, R. A. A. Bowler, M. J. Jarvis, N. J. Adams, N. Choustikov, A. M. Koekemoer, A. C. Carnall, D. J. McLeod, J. S. Dunlop, C. T. Donnan, N. A. Grogin
备注：
15 pages, 9 figures, 3 tables. Accepted to MNRAS. 2 figures added in appendix
We use data from the JWST Public Release IMaging for Extragalactic Research (PRIMER) survey to measure the size scaling relations of 1668 rest-frame UV-bright Lyman-break galaxies (LBGs) at $z=3-5$ with stellar masses $\mathrm{log}_{10}(M_{\star}/M_{\odot}) > 9$. The sample was selected from seeing-dominated ground-based data, presenting an unbiased sampling of the morphology and size distributions of luminous sources. We fit Sérsic profiles to eight NIRCam bands and also measure a non-parametric half-light radius. We find that the size distributions with both measurements are well-fit by a log-normal distribution at all redshifts, consistent with disk formation models where size is governed by host dark-matter halo angular momentum. We find a size-redshift evolution of $R_{e} = 3.51(1+z)^{-0.60\pm0.22}$ kpc, in agreement with JWST studies. When considering the typical (modal) size over $z=3-5$, we find little evolution with bright LBGs remaining compact at $R_{e}\simeq0.7-0.9$ kpc. Simultaneously, we find evidence for a build-up of large ($R_{e} > 2$ kpc) galaxies by $z=3$. We find some evidence for a negatively sloped size-mass relation at $z=5$ when Sérsic profiles are used to fit the data in F200W. The intrinsic scatter in our size-mass relations increases at higher redshifts. Additionally, measurements probing the rest-UV (F200W) show larger intrinsic scatter than those probing the rest-optical (F356W). Finally, we leverage rest-UV and rest-optical photometry to show that disky galaxies are well established by $z=5$, but are beginning to undergo dissipative processes, such as mergers, by $z=3$. The agreement of our size-mass and size-luminosity relations with simulations provides tentative evidence for centrally concentrated star formation at high-redshift.
JWST PRIMER: A deep JWST study of all ALMA-detected galaxies in PRIMER COSMOS -- dust-obscured star-formation history back to z $\simeq$ 7
Institute for Astronomy, University of Edinburgh（爱丁堡大学天文研究所）；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）；Department of Physics & Astronomy, University College London（伦敦大学学院物理与天文学系）；Space Telescope Science Institute（太空望远镜科学研究所）；Department of Astronomy and Astrophysics, UCO/Lick Observatory, University of California, Santa Cruz（加州大学圣克鲁兹分校天文学与天体物理学系、UCO/莱克天文台）；INAF - Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Jodrell Bank Centre for Astrophysics, Department of Physics & Astronomy, School of Natural Sciences, The University of Manchester（曼彻斯特大学自然科学学院物理与天文学系乔德雷尔银行天体物理中心）
No hidden monsters: Probing recently-quenched galaxies for obscured AGN with JWST-PRIMER MIRI and NIRCam
University of Nottingham（诺丁汉大学）；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）；University of Edinburgh（爱丁堡大学）；University of St Andrews（圣安德鲁斯大学）
ULTIMATE-deblending I. A 50-band Ultraviolet to Mid-infrared Photometric Catalog Combining Space- and Ground-based Data in the JWST/PRIMER survey
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（南京大学现代天文与天体物理教育部重点实验室）；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、天体物理学信息与方法研究所）；INAF – Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Chinese Academy of Sciences South America Center for Astronomy, National Astronomical Observatories, CAS（中国科学院南美天文中心、中国科学院国家天文台）
JWST PRIMER: Post-starburst galaxies dominate the low-mass quiescent galaxy population since z~2
University of Nottingham（诺丁汉大学）；University of St Andrews（圣安德鲁斯大学）；University of Edinburgh（爱丁堡大学）；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）
The multiwavelength structure of post-starburst galaxies at 0.5 < z < 3 with JWST PRIMER: compact morphologies and residual disturbances
School of Physics and Astronomy, University of Nottingham（诺丁汉大学物理与天文学学院）；School of Physics and Astronomy, University of St Andrews（圣安德鲁斯大学物理与天文学学院）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天文研究所）；William H. Miller III Department of Physics and Astronomy, Johns Hopkins University（约翰霍普金斯大学威廉·H·米勒三世物理与天文学系）；AURA for ESA, Space Telescope Science Institute（欧洲空间局AURA太空望远镜科学研究所）
Validating z > 7.5 Lyman Break Galaxy candidates in the COSMOS field with JWST/PASSAGE
Minnesota Institute for Astrophysics, University of Minnesota（明尼苏达大学天体物理研究所）；INAF, Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；International Centre for Radio Astronomy Research, University of Western Australia（西澳大利亚大学国际射电天文研究中心）；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）；Space Telescope Science Institute（太空望远镜科学研究所）；Stockholm University, Department of Astronomy（斯德哥尔摩大学天文学系）；University of California, Los Angeles, Department of Physics and Astronomy（加州大学洛杉矶分校物理与天文学系）；IPAC, California Institute of Technology（加州理工学院IPAC）
The Sunburst Arc with JWST. IV. The importance of interaction, turbulence, and feedback for Lyman-continuum escape
Stockholm University（斯德哥尔摩大学）；International Space Science Institute（国际空间科学研究所）；Center for Research and Exploration in Space Science and Technology, NASA/GSFC（NASA戈达德太空飞行中心空间科学与技术研究实验中心）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；California Institute of Technology（加州理工学院）；Steward Observatory, University of Arizona（亚利桑那大学斯蒂沃德天文台）
Lyman-$α$ Visibility During the Epoch of Reionization: Combining JWST FRESCO Grism Data with Keck Archival Spectroscopy
Anton Pannekoek Institute for Astronomy（安顿·潘内科克天文学研究所）；Institute of High-Energy Physics（高能物理研究所）；University of Amsterdam（阿姆斯特丹大学）；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所）；Department of Astronomy, University of Geneva（日内瓦大学天文学系）；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）；Institute of Science and Technology Austria (ISTA)（奥地利科学与技术研究所）
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。
The Size Evolution and the Size-Mass Relation of Lyman-Alpha Emitters across $3 \lesssim z < 7$ as Observed by JWST
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）；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）；Shanghai Key Lab for Astrophysics, Shanghai Normal University（上海师范大学天文与空间科学上海市重点实验室）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台星系与宇宙学重点实验室）；Dipartimento di Fisica G. Occhialini, Università degli Studi di Milano-Bicocca（米兰比可卡大学G. Occhialini物理系）
Confirmation and Refutation of Lyman Continuum Leakers at $z\sim3$ with JWST NIRSpec/IFU
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）；Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University（北京师范大学天文与前沿科学研究院）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）
Lyman-alpha emission at the end of reionization: line strengths and profiles from MMT and JWST observations at z~5-6
Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；MIT Kavli Institute for Astrophysics and Space Research（麻省理工学院卡弗里天体物理与空间研究所）；Departement d’Astronomie, University of Geneva（日内瓦大学天文学系）；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）
Constraints on the $z\sim6-13$ intergalactic medium from JWST spectroscopy of Lyman-alpha damping wings in galaxies
Cosmic Dawn Center (DAWN)（黎明宇宙中心）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Department of Astronomy, University of California, Berkeley（加州大学伯克利分校天文学系）
Rest-Frame UV and Optical Structural Evolution of Narrowband-Selected Lyman-alpha Emitters at z = 2-7 with JWST/NIRCam
National Astronomical Observatory of Japan（日本国立天文台）；The University of Tokyo（东京大学）；Nara Prefectural University（奈良县立大学）；The Graduate University for Advanced Studies（综合研究大学院大学）；Tohoku University（东北大学）；EPFL（洛桑联邦理工学院）；Alma Mater Studiorum Università di Bologna（博洛尼亚大学）；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）；Universität Heidelberg（海德堡大学）
Lyman continuum leakage versus quenching with the James Webb Space Telescope: The spectral signatures of quenched star formation activity in reionization-epoch galaxies
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）
The JWST-PRIMAL Legacy Survey. A JWST/NIRSpec reference sample for the physical properties and Lyman-$α$ absorption and emission of $\sim 500$ galaxies at $z=5.5-13.4$
