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）
Xiaojing Lin, Eiichi Egami, Fengwu Sun, Haowen Zhang, Xiaohui Fan, Jakob M. Helton, Feige Wang, Andrew J. Bunker, Zheng Cai, Daniel J. Eisenstein, Daniel T. Jaf… 展开作者
Xiaojing Lin, Eiichi Egami, Fengwu Sun, Haowen Zhang, Xiaohui Fan, Jakob M. Helton, Feige Wang, Andrew J. Bunker, Zheng Cai, Daniel J. Eisenstein, Daniel T. Jaffe, Zhiyuan Ji, Xiangyu Jin, Maria Anne Pudoka, Sandro Tacchella, Wei Leong Tee, Pierluigi Rinaldi, Brant Robertson, Yang Sun, Christopher N. A. Willmer, Chris Willott, Junyu Zhang, Yongda Zhu
We study the luminosity function (LF) and clustering properties of 888 H$α$ emitters (HAEs) at $3.75 < z < 6$ in the GOODS-N field. The sample, built from JWST CONGRESS and FRESCO NIRCam grism surveys using a novel redshift assignment algorithm, spans $\sim$62 arcmin$^2$ and reaches $L_{\rm Hα} \sim 10^{41.2} {\rm erg s^{-1}}$. We identify two prominent filamentary protoclusters at $z \approx 4.41$ and $z \approx 5.19$, hosting 98 and 144 HAEs, respectively. The observed H$α$ LFs show similar shallow faint-end slopes for both protocluster and field galaxies at $z=3.75-5$, and for the protocluster at $z=5-6$ ($α\approx 1.2$ to $-1.3$). In contrast, the field LF at $z=5-6$ is much steeper ($α=-1.87_{-0.23}^{+0.30}$), suggesting that protocluster galaxies at $z > 5$ are more evolved, resembling those at $z=3.75-5$. The observed star formation rate density from H$α$, integrated down to 0.45 ${\rm M_\odot yr^{-1}}$, is $0.050^{+0.002}_{-0.003}$ and $0.046^{+0.006}_{-0.004} M_\odot {\rm yr}^{-1} {\rm Mpc}^{-3}$ at $z=3.75-5$ and $z=5-6$, with protoclusters contributing $\sim$25% and 55%, respectively. This implies that a large fraction of star formation at $z > 4$ occurs in protoclusters. We conduct the first star-formation-rate-limited 3D clustering analysis at $z > 4$. We find the filamentary protocluster geometry flattens the power-law shape of the HAE auto-correlation functions, with slopes much shallower than typically assumed. The auto-correlation function of field HAEs have correlation lengths of $r_0 = 4.61^{+1.00}_{-0.68} h^{-1}{\rm Mpc}$ at $z \approx 4-5$ and $r_0 = 6.23^{+1.68}_{-1.13} h^{-1}{\rm Mpc}$ at $z=5-6$. Comparing the observed correlation functions with the UniverseMachine simulation, we infer the dark matter (sub-)halo masses of HAEs to be $\log (M_h/M_\odot)=11.0-11.2$ at $z\approx 4-6$, with a scatter of 0.4 dex.
The Large-scale Environments of Low-luminosity AGNs at $3.9 < z < 6$ and Implications for Their Host Dark Matter Halos 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）；University of Cambridge（剑桥大学）；University College London（伦敦大学学院）；University of California, Santa Cruz（加利福尼亚大学圣克鲁兹分校）
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）
Rapid, out of equilibrium metal enrichment indicated by a flat mass-metallicity relation at z~6 from NIRCam grism spectroscopy
Institute of Science and Technology Austria（奥地利科学技术学院）；National Astronomical Observatory of Japan（日本国立天文台）；Astronomy Centre, University of Sussex（萨塞克斯大学天文学中心）；Department of Physics, North Carolina State University（北卡罗来纳州立大学物理系）；Institute for Computational & Data Sciences, The Pennsylvania State University（宾夕法尼亚州立大学计算与数据科学研究所）；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）；Department of Astronomy, University of Wisconsin-Madison（威斯康星大学麦迪逊分校天文学系）；Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）
Medium-band Astrophysics with the Grism of NIRCam In Frontier fields (MAGNIF): Spectroscopic Census of H$α$ Luminosity Functions and Cosmic Star Formation at $z\sim 4.5$ and 6.3
SAPPHIRES: Extremely Metal-Poor Galaxy Candidates with $12+{\rm log(O/H)}<7.0$ at $z\sim5-7$ from Deep JWST/NIRCam Grism Observations
Space Telescope Science Institute (STScI)（太空望远镜科学研究所）；The Johns Hopkins University（约翰斯·霍普金斯大学）；Association of Universities for Research in Astronomy (AURA), Inc.（大学天文研究协会）；University of Texas at Austin（德克萨斯大学奥斯汀分校）；Ben-Gurion University of the Negev（内盖夫本-古里安大学）；University of Groningen（格罗宁根大学）；University of Cambridge（剑桥大学）；University College London（伦敦大学学院）；University of Arizona（亚利桑那大学）；Tsinghua University（清华大学）；Chiba University（千叶大学）；The University of Tokyo（东京大学）；National Astronomical Observatory of Japan（日本国立天文台）；SOKENDAI (The Graduate University for Advanced Studies)（综合研究大学院大学）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；University of Copenhagen（哥本哈根大学）；University of Oxford（牛津大学）；Westlake University（西湖大学）；University of Michigan（密歇根大学）
Slitless Areal Pure-Parallel HIgh-Redshift Emission Survey (SAPPHIRES): Early Data Release of Deep JWST/NIRCam Images and Spectra in MACS J0416 Parallel Field
Probing Direct Contributions of Galaxies and AGN to Cosmic Reionization in a Quasar Field J0226+0302 with JWST NIRCam and NIRSpec
University of Michigan（密歇根大学）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Cosmic Dawn Center (DAWN), Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所黎明中心）；Kavli IPMU (WPI), UTIAS, The University of Tokyo（东京大学宇宙起源研究核心理论研究中心）；Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo（东京大学宇宙起源研究核心理论中心数据驱动发现中心）；Department of Physics & Astronomy, University of California, Riverside（加州大学河滨分校物理与天文学系）
The Number Density Evolution of Extreme Emission Line Galaxies in 3D-HST: Results from a Novel Automated Line Search Technique for Slitless Spectroscopy
From Grism to IFU: Revising the Redshift and Nature of the Massive Dusty Galaxy S1 with JWST and ALMA
University of Geneva（日内瓦大学）；University of Sussex（萨塞克斯大学）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Université Paris-Saclay, Université Paris Cité（巴黎萨克雷大学、巴黎西岱大学）；Leiden University（莱顿大学）
Quantifying the escape of Ly$α$ at $z\approx 5-6$: a census of Ly$α$ escape fraction with H$α$ emitting galaxies spectroscopically confirmed by JWST and VLT/MUSE
Beyond the stars: Linking H$α$ sizes, kinematics, and star formation in galaxies at $z\approx 4-6$ with JWST grism surveys and $\texttt{geko}$
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 Astronomy and Astrophysics, University of California, Santa Cruz（加州大学圣克鲁斯分校天文学与天体物理学系）；Scuola Normale Superiore（比萨高等师范学院）；Steward Observatory, University of Arizona（亚利桑那大学斯蒂沃德天文台）；Department of Physics, University of Oxford（牛津大学物理系）
JWST observes the assembly of a massive galaxy at z~4
University of Oxford（牛津大学）；University of Leiden（莱顿大学）；Observatório Nacional/MCTI（国家天文台/科技部）；TNO（荷兰组织应用科学研究所）；Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理研究所）；Steward Observatory, University of Arizona（亚利桑那大学斯蒂沃德天文台）；Instituto de Astrofísica de La Plata, CONICET-UNLP（拉普拉塔天体物理研究所/阿根廷国家科学技术研究委员会/拉普拉塔国立大学）；Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata（拉普拉塔国立大学天文与地球科学学院）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心/西班牙国家技术研究委员会/国家航空航天技术研究所）；ELTE Eoẗovös Loránd University（罗兰大学）
Quasar Radiative Feedback May Suppress Galaxy Growth on Intergalactic Scales at $z = 6.3$
Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；School of Earth and Space Exploration, Arizona State University（亚利桑那州立大学地球与空间探索学院）；Augustana Campus, University of Alberta（阿尔伯塔大学奥古斯都校区）；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）；Department of Physics, Massachusetts Institute of Technology（麻省理工学院物理系）；Center for Frontier Science, Chiba University（千叶大学前沿科学中心）；Department of Physics, University of Oxford（牛津大学物理系）；Department of Astronomy, Tsinghua University（清华大学天文系）；Division of Particle and Astrophysical Science, Nagoya University（名古屋大学粒子与天体物理科学分部）；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）；Department of Physics and Astronomy, University College London（伦敦大学学院物理与天文系）；AURA for the European Space Agency (ESA), Space Telescope Science Institute（欧洲航天局（ESA）授权机构AURA，太空望远镜科学研究所）；Department of Astronomy, University of Michigan（密歇根大学天文系）
Diversity and Evolution of Dust Attenuation Curves from Redshift z ~ 1 to 9
Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心）；MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院卡弗里天体物理学与空间研究所）；Kavli Institute for Cosmological Physics (KICP), University of Chicago（芝加哥大学卡弗里宇宙物理研究所）；Department of Astronomy & Astrophysics, University of Chicago（芝加哥大学天文与天体物理系）；Sterrenkundig Observatorium Department of Physics and Astronomy Universiteit Gent（根特大学物理与天文学系天文台）；Institute for Computational & Data Sciences, The Pennsylvania State University（宾夕法尼亚州立大学计算与数据科学研究所）；Institute of Science and Technology Austria（奥地利科学与技术研究所）；Center for Astrophysics | Harvard & Smithsonian（哈佛史密森尼天体物理中心）；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）；Department of Physics, University of Oxford（牛津大学物理系）；Department of Astronomy, Oskar Klein Centre, Stockholm University（斯德哥尔摩大学奥斯卡克莱因中心天文学系）
All the Massive Galaxy Overdensities during Reionization: JWST Rest-Frame Optical Selection Reveals Young, Chemically Evolved Galaxies Embedded in Dense, Neutral Gas at z > 5
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）；DTU Space, Technical University of Denmark（丹麦技术大学空间科学中心）；Institute of Science and Technology Austria (ISTA)（奥地利科学技术研究院）；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）；Department of Astronomy, University of Geneva（日内瓦大学天文系）；National Astronomical Observatory of Japan（日本国立天文台）；INAF/Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）
JWST ASPIRE: How Did Galaxies Complete Reionization? Evidence for Excess IGM Transmission around ${\rm [O\,{\scriptstyle III}]}$ Emitters during Reionization
The Impact of Cosmic Variance and Satellites on JWST Clustering Measurements at Redshift around 6
University of California, Santa Barbara（加州大学圣塔芭芭拉分校）；Center for Astrophysics | Harvard & Smithsonian（哈佛-史密森天体物理中心）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）
Testing the inference of kinematics from mock JWST NIRSpec/MSA observations of TNG50 galaxies at $z\sim2-6$
Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Fakultät für Physik und Astronomie, Universität Heidelberg（海德堡大学物理与天文学院）；Space Telescope Science Institute（太空望远镜科学研究所）
Stellar masses of optically dark galaxies: uncertainty introduced by the attenuation law and star-formation histories
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, University of Oxford（牛津大学物理系）
ASPIRE: The Environments and Dark Matter Halos of Luminous Quasars in the Epoch of Reionization
University of Michigan（密歇根大学）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Space Telescope Science Institute（太空望远镜科学研究所）；University of California, Santa Barbara（加州大学圣塔芭芭拉分校）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Newcastle University（纽卡斯尔大学）；INAF–Osservatorio di Astrofisica e Scienza dello Spazio（意大利国家天体物理研究所空间科学与天体物理观测站）；Department of Astronomy, University of Geneva（日内瓦大学天文学系）
