JWST/NIRCam Pa$\mathrmβ$ narrow-band imaging reveals ordinary dust extinction for H$\mathrmα$ emitters within the Spiderweb protocluster at z=2.16
Jose Manuel Pérez-Martínez, Helmut Dannerbauer, Yusei Koyama, Pablo G. Pérez-González, Rhythm Shimakawa, Tadayuki Kodama, Yuheng Zhang, Kazuki Daikuhara, Chiara… 展开作者
Jose Manuel Pérez-Martínez, Helmut Dannerbauer, Yusei Koyama, Pablo G. Pérez-González, Rhythm Shimakawa, Tadayuki Kodama, Yuheng Zhang, Kazuki Daikuhara, Chiara D'Eugenio, Abdurrahman Naufal
备注：
21 pages, 8 figures. Accepted for publication in ApJ
We combine JWST/NIRCam and Subaru/MOIRCS dual Pa$\mathrmβ$ + H$\mathrmα$ narrow-band imaging to trace the dust attenuation and the star-formation activities of a sample of 43 H$\mathrmα$ emitters at the core of one of the most massive and best-studied clusters in formation at the cosmic noon: the Spiderweb protocluster at $\mathrm{z=2.16}$. We find that most H$\mathrmα$ emitters display Pa$\mathrmβ$/H$\mathrmα$ ratios compatible with Case B recombination conditions, which translates into nebular extinction values ranging at $\mathrm{A_V\approx0-3}$ magnitudes, and dust corrected $\mathrm{Paβ}$ star formation rates consistent with coeval main sequence field galaxies at fixed stellar mass ($\mathrm{9.4<\log M_*/M_\odot<11.0}$) during this cosmic epoch. Furthermore, we investigate possible environmental impacts on dust extinction across the protocluster large-scale structure and find no correlation between the dustiness of its members and environmental proxies such as phase-space position, clustercentric radius, or local density. These results support the scenario for which dust production within the main galaxy population of this protocluster is driven by secular star formation activities fueled by smooth gas accretion across its large-scale structure. This downplays the role of gravitational interactions in boosting star formation and dust production within the Spiderweb protocluster, in contrast with observations in higher redshift and less evolved protocluster cores.
Spider-Webb: enhanced star formation in low-mass galaxies within the Spiderweb protocluster revealed by JWST Pa$β$ narrow-band imaging
Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency（日本宇宙航空研究开发机构宇宙科学研究所）；Astronomical Institute, Tohoku University（东北大学天文研究所）；National Astronomical Observatory of Japan (NAOJ), National Institutes of Natural Sciences（国立天文台（NAOJ），国立自然科学研究所）；Waseda Institute for Advanced Study (WIAS), Waseda University（早稻田大学高等研究院（WIAS））；Instituto de Astrofísica de Canarias (IAC)（加那利天体物理学研究所（IAC））；Departamento Astrofísica, Universidad de La Laguna（拉古纳大学天体物理系）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CAB），西班牙国家科学技术研究委员会-国家航空航天技术研究所）
Chaotic Molecular Gas in Five Dusty Star-forming Galaxies in the Spiderweb Protocluster at $z = 2.16$
University of Arizona（亚利桑那大学）；University of California, Santa Barbara（加州大学圣塔芭芭拉分校）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；Technical University of Denmark（丹麦技术大学）
The 700 ks Chandra Spiderweb Field I: evidence for widespread nuclear activity in the Protocluster
(Abridged) We present an analysis of the 700 ks Chandra ACIS-S observation of the field around the Spiderweb Galaxy at z=2.156, focusing on the nuclear activity in the associated large-scale environment. We identify unresolved X-ray sources down to flux limits of 1.3X10^{-16} and 3.9X10^{-16} erg/s/cm^2 in the soft and hard band, respectively. We search for counterparts in the optical, NIR and submm bands to identify X-ray sources belonging to the protocluster. We detect 107 X-ray unresolved sources within 5 arcmin (corresponding to 2.5 Mpc) of J1140-2629, among which 13 have optical counterpa…
Spider-Webb: Spatially-Resolved Evidence of Inside-Out Quenching in the Spiderweb Protocluster at $z \sim 2$
National Astronomical Observatory of Japan（日本国立天文台）；The Graduate University for Advanced Studies（高级研究院）；Tohoku University（东北大学）；Waseda University（早稻田大学）
JWST reveals extended stellar disks for ALMA-bright dusty star-forming galaxies in the Spiderweb protocluster
Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；University of Science and Technology of China（中国科学技术大学）；Instituto de Astrofísica de Canarias (IAC)（加那利天体物理研究所）；Universidad de La Laguna（拉各拉纳大学）；National Astronomical Observatory of Japan（日本国立天文台）；Graduate University for Advanced Studies (SOKENDAI)（综合研究大学院大学）；Shanghai Jiao Tong University（上海交通大学）；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）
Mass--size evolution and the emerging passive--density relation revealed by JWST/NIRCam in the Spiderweb protocluster
Adam Mickiewicz University（亚当·密茨凯维奇大学）；Instituto de Astrofísica de Canarias（加那利天体物理研究所）；Universidad de La Laguna（拉帕鲁尼亚大学）；European Southern Observatory（欧洲南方天文台）；Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency（日本宇宙航空研究开发机构宇宙科学研究所）；Tohoku University（东北大学）；National Astronomical Observatory of Japan（日本国立天文台）
Rapid quenching and early gas depletion in the core of a galaxy protocluster at z=2.2
Instituto de Astrofísica de Canarias (IAC)（加那利天体物理研究所）；Universidad de La Laguna（拉古纳大学）；Université Paris-Saclay（巴黎萨克雷大学）；Université Paris Cité（巴黎西岱大学）；CEA（法国原子能和替代能源委员会）；CNRS（法国国家科学研究中心）；AIM（宇宙学、物质与星际介质实验室）；Institut de physique du globe de Paris（巴黎地球物理研究所）；IGN（法国国家地理与森林信息研究所）；Academia Sinica Institute of Astronomy and Astrophysics (ASIAA)（中央研究院天文及天文物理研究所）；The Graduate University for Advanced Studies（综合研究大学院大学）；Subaru Telescope（昴星团望远镜）；National Astronomical Observatory of Japan（日本国立天文台）；National Institutes of Natural Sciences（自然科学研究机构）；Centro de Astrobiología (CAB)（天体生物学中心）；CSIC（西班牙国家科学研究委员会）；INTA（西班牙航空航天技术研究所）；Nanjing University（南京大学）
The Luminosity Function and Clustering of H$α$ Emitting Galaxies at $z\approx4-6$ from a Complete NIRCam Grism Redshift Survey
Tsinghua University（清华大学）；University of Arizona（亚利桑那大学）；University of Michigan（密歇根大学）；University of Oxford（牛津大学）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；University of Cambridge（剑桥大学）；University of California, Santa Cruz（加州大学圣克鲁兹分校）
Discovery of a $z\simeq 4.9$ Lyman-$α$ Emitter Protocluster: Wavelength-Dependent Environmental Effects on Galaxy Structure
National Astronomical Observatory of Japan（日本国立天文台）；The Graduate University for Advanced Studies（日本综合研究大学院大学）；The University of Tokyo（东京大学）；Tohoku University（东北大学）
Before its time: a remarkably evolved protocluster core at z=7.88
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）；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）；Chiba University（千叶大学）；Institute of Astronomy, University of Cambridge（剑桥大学天文学研究所）；Aix Marseille Univ, CNRS, CNES, LAM（艾克斯-马赛大学）；Center for Astrophysics, Harvard University（哈佛大学天体物理中心）
Early Emergence of Environmental Effects: Accelerated Galaxy Assembly in a z=2.96 Protocluster in the COSMOS Field
Tsinghua University（清华大学）；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所（ Kavli IPMU ））
Not all protoclusters host evolved galaxies: Evidence for reduced environmental effects in a lower halo mass protocluster at $z = 7.66$
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）；DARK, Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所 DARK 研究中心）；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）
A large overdensity of LRD-like galaxies discovered by JWST in the SPT2349-56 protocluster at z=4.30
Dalhousie University（达尔豪斯大学）；University of British Columbia（不列颠哥伦比亚大学）；NRC Herzberg Astronomy and Astrophysics（加拿大国家研究委员会赫茨伯格天文学与天体物理学研究所）；Eureka Scientific Inc（尤里卡科学公司）；University of Illinois（伊利诺伊大学）；National Center for Supercomputing Applications（超级计算应用国家中心）；Max-Planck-Institut fur Radioastronomie（马克斯·普朗克射电天文研究所）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；Universidad Diego Portales（迭戈·波特莱斯大学）；Millenium Nucleus for Galaxies (MINGAL)（星系千年核心（MINGAL））；University of Victoria（维多利亚大学）
Galaxy Protoclusters as Drivers of Cosmic Reionization: II. Te-Based Metallicities of Lyman-α Emitters
Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学）；Las Campanas Observatory, Carnegie Science（拉斯坎帕纳斯天文台，卡内基科学）；University of California Santa Barbara（加州大学圣塔芭芭拉分校）；Instituto de Astrofísica de la Facultad de Ingeniería y Ciencias, Universidad Diego Portales（迭戈·波特莱斯大学工程与科学学院天体物理研究所）；Texas A&M University（德克萨斯农工大学）；George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A&M University（德克萨斯农工大学乔治·P和辛西娅·伍兹基础物理与天文学研究所）；Caltech/IPAC（加州理工学院/IPAC）；Institute for Cosmic Ray Research, The University of Tokyo（东京大学宇宙射线研究所）；Space Telescope Science Institute（太空望远镜科学研究所）
The Koi Pond: A Strongly Lensed Protocluster Core hosting a Diverse Population of DSFGs
Arizona State University（亚利桑那州立大学）；Joint ALMA Observatory（ALMA联合天文台）；National Astronomical Observatory of Japan（日本国立天文台）；European Southern Observatory（欧洲南方天文台）；Universidad Diego Portales（迭戈·波特莱斯大学）；University of Arizona（亚利桑那大学）；Chalmers University of Technology（查尔姆斯理工大学）
JADES: Discovery of Large Reservoirs of Small Dust Grains in the Circumgalactic Medium of Massive Galaxies at $z\sim3.5$ through Deep JWST/NIRCam Imaging and Grism Spectroscopy
University of Cambridge（剑桥大学）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；The Pennsylvania State University（宾夕法尼亚州立大学）；Tsinghua University（清华大学）
RIOJA. Environmental Effects on Stellar Populations and Ionized Gas in a Protocluster at $z=7.88$
University of Tsukuba（筑波大学）；Tsukuba Institute for Advanced Research (TIAR), University of Tsukuba（筑波大学先进研究院）；Tomonaga Center for the History of the Universe (TCHoU), Faculty of Pure and Applied Sciences, University of Tsukuba（筑波大学纯应用科学学部朝永中心宇宙历史研究中心）；Centro de Astrobiología (CAB), CSIC-INTA（西班牙国家航空航天技术研究所/西班牙高等科学研究委员会天体生物学中心）；Waseda Research Institute for Science and Engineering, Faculty of Science and Engineering, Waseda University（早稻田大学理工学部的理工学研究科）；Department of Pure and Applied Physics, School of Advanced 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纯应用物理系）
