Spatially Resolved Stellar Populations of $0.3<z<6.0$ Galaxies in WHL0137-08 and MACS0647+70 Clusters as Revealed by JWST: How do Galaxies Grow and Quench Over Cosmic Time?
Abdurro'uf, Dan Coe, Intae Jung, Henry C. Ferguson, Gabriel Brammer, Kartheik G. Iyer, Larry D. Bradley, Pratika Dayal, Rogier A. Windhorst, Adi Zitrin, Ashish … 展开作者
Abdurro'uf, Dan Coe, Intae Jung, Henry C. Ferguson, Gabriel Brammer, Kartheik G. Iyer, Larry D. Bradley, Pratika Dayal, Rogier A. Windhorst, Adi Zitrin, Ashish Kumar Meena, Masamune Oguri, Jose M. Diego, Vasily Kokorev, Paola Dimauro, Angela Adamo, Christopher J. Conselice, Brian Welch, Eros Vanzella, Tiger Yu-Yang Hsiao, Xinfeng Xu, Namrata Roy, Celia R. Mulcahey
We study the spatially resolved stellar populations of 444 galaxies at $0.3<z<6.0$ in two clusters (WHL0137-08 and MACS0647+70) and a blank field, combining imaging data from HST and JWST to perform spatially resolved spectral energy distribution (SED) modeling using pixedfit. The high spatial resolution of the imaging data combined with magnification from gravitational lensing in the cluster fields allows us to resolve some galaxies to sub-kpc scales (for 109 of our galaxies). At redshifts around cosmic noon and higher ($2.5\lesssim z\lesssim 6.0$), we find mass doubling times to be independent of radius, inferred from flat specific star formation rate (sSFR) radial profiles and similarities between the half-mass and half-SFR radii. At lower redshifts ($1.5\lesssim z\lesssim 2.5$), a significant fraction of our star-forming galaxies show evidence for nuclear starbursts, inferred from centrally elevated sSFR, and a much smaller half-SFR radius compared to the half-mass radius. At later epochs, we find more galaxies suppress star formation in their center but are still actively forming stars in the disk. Overall, these trends point toward a picture of inside-out galaxy growth consistent with theoretical models and simulations. We also observe a tight relationship between the central mass surface density and global stellar mass with $\sim 0.38$ dex scatter. Our analysis demonstrates the potential of spatially resolved SED analysis with JWST data. Future analysis with larger samples will be able to further explore the assembly of galaxy mass and the growth of their structures
The JWST EXCELS survey: Insights into the nature of quenching at cosmic noon
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 St Andrews（圣安德鲁斯大学）；University of Edinburgh（爱丁堡大学）；University of Nottingham（诺丁汉大学）
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）
MAGAZ3NE: Spatially Resolved Ages and Chemical Abundances of Ultra-Massive Quiescent Galaxies at z $\sim$ 3.5 using JWST/NIRSpec IFU
York University（约克大学）；University of Toronto（多伦多大学）；Dunlap Institute for Astronomy & Astrophysics, University of Toronto（多伦多大学邓普勒天文学与天体物理研究所）；University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）；University of California Davis（加州大学戴维斯分校）；University of Wisconsin-Madison（威斯康星大学麦迪逊分校）；Observatories of the Carnegie Institution for Science（卡内基科学机构天文台）；Princeton University（普林斯顿大学）
Feeding the Dead: Neutral Gas Inflow in a Long-Quenched Ancient Massive Galaxy at $z\sim 2.7$ Observed with JWST/NIRSpec
Tufts University（塔夫茨大学）；INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）；INAF - Osservatorio Astronomico di Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；Dipartimento di Fisica e Astronomia, Universitá di Bologna（博洛尼塔大学物理与天文学系）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯玻尔研究所）；European Space Research and Technology Centre（欧洲空间研究与技术中心）；Universitá degli studi di Milano-Bicocca（米兰比可卡大学）
The JWST EXCELS survey: Outflows in 1.5 < z < 5 quiescent and recently quenched galaxies are likely relics from episodic AGN activity
University of Edinburgh（爱丁堡大学）；University of Nottingham（诺丁汉大学）；Universidad de Sevilla（塞维利亚大学）；University of St Andrews（圣安德鲁斯大学）；University of California, Los Angeles（加州大学洛杉矶分校）
利用JWST NIRSpec光谱研究1.8 ≤ z ≤ 4.6红移的13个后星暴和静止星系中的中性气体出流和吸积，发现出流与AGN活动相关，且出流速率远高于恒星形成率。
Sleeping or Dead? Probing the Quenching Mechanism of JWST Dormant Galaxies at z > 3 with ALMA
University of Geneva（日内瓦大学）；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）；Caltech/IPAC（加州理工学院/IPAC）；Université Paris-Saclay（巴黎萨克雷大学）；Université Paris Cité（巴黎西岱大学）；CEA（法国原子能委员会）；CNRS（法国国家科学研究中心）；AIM（天体物理学、信息与微波实验室）；University of Zurich（苏黎世大学）
Lyman continuum leakage versus quenching with the James Webb Space Telescope: The spectral signatures of quenched star formation activity in reionization-epoch galaxies
Clues to inside-out quenching in quiescent galaxies at $1.2\lesssim z\lesssim2.2$: Age, Fe-, and Mg-abundance gradients from JWST-SUSPENSE
Leiden University（莱顿大学）；Observatories of the Carnegie Institution for Science（卡内基科学研究所天文台）；University of the Pacific（太平洋大学）；University of Pittsburgh（匹兹堡大学）；Max-Planck-Institut für Astronomie（马克斯·普朗克天体物理学研究所）；Max-Planck-Institut für extraterrestrische Physik（马克斯·普朗克地外物理学研究所）；University of California, Berkeley（加州大学伯克利分校）；Tufts University（塔夫茨大学）；Instituto de Astrofísica de Canarias（加那利群岛天体物理研究所）；Universidad de La Laguna（拉帕尔马大学）；York University（约克大学）
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）
Interplay of Compaction, Quenching, and Black Hole Growth in the Most Massive Galaxies since $z\sim5$: Insights from JWST and Chandra Data
Tohoku University（东北大学）；Indiana University（印第安纳大学）；Stanford University（斯坦福大学）；SLAC National Accelerator Laboratory（SLAC国家加速器实验室）；Institut Teknologi Bandung（万隆理工学院）；National Astronomical Observatory of Japan（日本国立天文台）；Harvard-Smithsonian Center for Astrophysics（哈佛-史密森尼天体物理中心）；Center for Astrophysics | Harvard & Smithsonian（天体物理中心 | 哈佛与史密森尼）
Dust and PAHs in late-stage galaxy evolution: Imprints of TP-AGB dust injection, grain growth and AGN feedback in high-z quiescent galaxies with JWST and ALMA
National Center for Nuclear Research（国家核研究中心）；SISSA（的里雅斯特国际高等研究学院）；INAF, Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）；INAF - Osservatorio Astronomico d’Abruzzo（意大利国家天体物理研究所阿布鲁佐天文台）；Department of Astronomy, University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校天文学系）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；Department of Physics & Astronomy, University of British Columbia（不列颠哥伦比亚大学物理与天文学系）；Caltech/IPAC（加州理工学院/IPAC）；IFPU – Institute for Fundamental Physics of the Universe（基础物理学宇宙研究所）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Center for Astrophysics and Cosmology, University of Nova Gorica（新戈里察大学天体物理学与宇宙学中心）
GA-NIFS: The interplay between feedback and star formation at 3 < z < 9 probed by JWST/NIRSpec IFU
Centro de Astrobiología (CAB), CSIC–INTA（天体生物学中心）；INAF - Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切里天文台）；Max-Planck-Institut für extraterrestrische Physik (MPE)（马克斯·普朗克地外物理学研究所）；Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Cavendish Laboratory - Astrophysics Group, University of Cambridge（剑桥大学卡文迪许实验室天体物理组）；European Space Agency（欧洲空间局）；Department of Physics, University of Oxford（牛津大学物理系）
JWST Spectroscopic View of a Rapidly Growing Dust-obscured Quasar at $z \sim 4$: Effect of Dust Extinction Correction on Black Hole Mass and Eddington Ratio Estimation
LEGGOS I: The JWST LEGGOS Survey -- LEnsing and Galaxy Growth: Observing Substructures -- Unpacks the Nature of Clumpy Star Formation and Quenching in Gravitationally Lensed Galaxies beyond Cosmic Noon
University of Washington（华盛顿大学）；University of Pittsburgh（匹兹堡大学）；University of Arizona（亚利桑那大学）；Eureka Scientific（尤里卡科学公司）；University of Cincinnati（辛辛那提大学）；NASA Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）
Mature but Still Growing: JWST Detection of the Earliest Intracluster Light at z ~ 2
Yonsei University（延世大学）；University of California, Davis（加州大学戴维斯分校）；California Institute of Technology（加州理工学院）；University of Oxford（牛津大学）；University of California, Los Angeles（加州大学洛杉矶分校）；Korea Astronomy and Space Science Institute（韩国天文学与空间科学研究所）
A census of quiescent galaxies across $0.5 < z < 8$ with JWST/MIRI: Mass-dependent number density evolution of quiescent galaxies in the early Universe
Nanjing University（南京大学）；Tianjin Normal University（天津师范大学）
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
Witnessing the rapid growth of disk galaxies over cosmic time using JWST and HST
Universidad de Valladolid（巴利亚多利德大学）；Laboratory for Disruptive Interdisciplinary Science (LaDIS), Universidad de Valladolid（巴利亚多利德大学颠覆性跨学科科学实验室）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所（ICE，CSIC））；Instituto de Astrofísica de Canarias（加那利天体物理研究所）；Departamento de Astrofísica, Universidad de La Laguna（拉帕拉塔大学天体物理学系）；Instituto de Astrofísica e Ciéncia do Espaço, Universidad de Lisboa（里斯本大学天体物理学与空间科学研究所）
Reconstruction of Cosmic Black Hole Growth and Mass Distribution from Quasar Luminosity Functions at $z>4$: Implications for Faint and Low-mass Populations in JWST
Caught Napping by JWST UNCOVER+MegaScience: Constraining bursty star formation histories and number densities of mini-quenched galaxies at redshifts 4-7
University of Washington（华盛顿大学）；University of Pittsburgh（匹兹堡大学）；University of Colorado, Boulder（科罗拉多大学博尔德分校）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；Princeton University（普林斯顿大学）
Cosmic Stillness: High Quiescent Galaxy Fractions Across Upper Mass Scales in the Early Universe to z = 7 with JWST
University of Manchester（曼彻斯特大学）；University of Victoria（维多利亚大学）；Arizona State University（亚利桑那州立大学）；University of Louisville（路易斯维尔大学）；University of the Basque Country UPV/EHU（巴斯克自治大学）；DIPC, Basque Country UPV/EHU（巴斯克基础科学中心，巴斯克自治大学）；Ikerbasque, Basque Foundation for Science（伊卡巴斯基，巴斯克科学基金会）；Space Telescope Science Institute（太空望远镜科学研究所）；Association of Universities for Research in Astronomy (AURA) for the European Space Agency (ESA), STScI（欧洲空间局太空望远镜科学研究所大学研究协会）；The Johns Hopkins University（约翰斯·霍普金斯大学）；International Centre for Radio Astronomy Research (ICRAR) and the International Space Centre (ISC), The University of Western Australia（西澳大利亚大学国际射电天文研究中心和国际太空中心）；University of Arizona（亚利桑那大学）；National Research Council of Canada, Herzberg Astronomy & Astrophysics Research Centre（加拿大国家研究委员会赫茨伯格天体物理学与天文学研究中心）；ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D)（ARC三维全天空天体物理学卓越中心）；University of Missouri（密苏里大学）
JWST Reveals a Candidate Jellyfish Galaxy at z=1.156
University of Waterloo（滑铁卢大学）；Waterloo Centre for Astrophysics, University of Waterloo（滑铁卢大学天体物理中心）；York University（约克大学）；Perimeter Institute for Theoretical Physics（基础物理研究所）；École Polytechnique Fédérale de Lausanne (EPFL)（洛桑联邦理工学院）
Dynamical properties and star formation history of a low-mass quenched galaxy at Cosmic Noon
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）；DARK, Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Department of Astronomical Science, The Graduate University for Advanced Studies, SOKENDAI（国立天文台高等研究院天文学研究科）；National Astronomical Observatory of Japan（日本国立天文台）；ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D)（ARC三维全天空天体物理学卓越中心）；Subaru Telescope（昴星团望远镜）
