The radial gradient of gas-phase metallicity is a powerful probe of the chemical and structural evolution of star-forming galaxies, closely tied to disk formation and gas kinematics in the early universe. We present spatially resolved chemical and dynamical properties for a sample of 25 galaxies at $0.5 \lesssim z \lesssim 1.7$ from the \msasd survey. These innovative observations provide 3D spectroscopy of galaxies at a spatial resolution approaching JWST's diffraction limit and a high spectral resolution of $R\simeq2700$. The metallicity gradients measured in our galaxy sample range from $-$0.03 to 0.02 dex~kpc$^{-1}$. Most galaxies exhibit negative or flat radial gradients, indicating lower metallicity in the outskirts or uniform metallicity throughout the entire galaxy. We confirm a tight relationship between stellar mass and metallicity gradient at $z\sim1$ with small intrinsic scatter of 0.02 dex~kpc$^{-1}$. Our results indicate that metallicity gradients become increasingly negative as stellar mass increases, likely because the more massive galaxies tend to be more ``disky". This relationship is consistent with the predictions from cosmological hydrodynamic zoom-in simulations with strong stellar feedback. This work presents the effort to harness the multiplexing capability of JWST NIRSpec/MSA in slit-stepping mode to map the chemical and kinematic profiles of high-redshift galaxies in large samples and at high spatial and spectral resolution.
The James Webb Space Telescope (JWST) will be an exquisite new near-infrared observatory with imaging and multi-object spectroscopy through ESA's NIRspec instrument with its unique Micro-Shutter Array (MSA), allowing for slits to be positioned on astronomical targets by opening specific 0.002"-wide micro shutter doors. To ensure proper target acquisition, the on-sky position of the MSA needs to be verified before spectroscopic observations start. An onboard centroiding program registers the position of pre-identified guide stars in a Target Acquisition (TA) image, a short pre-spectroscopy expo…
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）
NEXUS: Abundance, Environments, and Spectral Diversity of Little Red Dots from the NIRSpec MSA Sample
Department of Astronomy, University of Illinois Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校天文学系）；National Center for Supercomputing Applications, University of Illinois Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校国家超级计算应用中心）；Department of Astronomy, University of Michigan（密歇根大学天文学系）；Department of Astrophysical Sciences, Princeton University（普林斯顿大学天体物理学系）；UC San Diego（加州大学圣地亚哥分校）
The Near InfraRed Spectrograph (NIRSpec) on the James Webb Space Telescope (JWST) includes a novel micro shutter array (MSA) to perform multi object spectroscopy. While the MSA is mainly targeting galaxies across a larger field, it can also be used for studying star formation in crowded fields. Crowded star formation regions typically feature strong nebular emission, both in emission lines and continuum. In this work, nebular emission is referred to as nebular contamination. Nebular contamination can obscure the light from the stars, making it more challenging to obtain high quality spectra. T…
MSA-3D: Rotation Curves and Dark Matter Fractions at z~0.5-1.7 with JWST/NIRSpec
Max-Planck-Institut für extraterrestrische Physik (MPE)（马克斯·普朗克地外物理学研究所）；International Centre for Radio Astronomy Research, University of Western Australia（西澳大学国际射电天文研究中心）；Centre for Astrophysics & 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 Physics and Astronomy, University of California, Davis（加州大学戴维斯分校物理与天文学系）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo（东京大学宇宙学前沿研究 Kavli 研究所）；School of Astronomy and Space Science, University of Chinese Academy of Sciences (UCAS)（中国科学院大学天文与空间科学学院）；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）
JADES Dark Horse: demonstrating high-multiplex observations with JWST/NIRSpec dense-shutter spectroscopy in the JADES Origins Field
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 for Astrophysical and Planetary Science, University of Colorado, Boulder（科罗拉多大学博尔德分校天体物理学与行星科学系）；Center for Astrophysics | Harvard & Smithsonian（哈佛史密森尼天体物理中心）；Department of Physics and Astronomy, University College London（伦敦大学学院物理与天文系）；Scuola Normale Superiore（比萨高等师范学院）；European Southern Observatory（欧洲南方天文台）；Steward Observatory, University of Arizona（亚利桑那大学斯图沃德天文台）；Department of Physics, University of Oxford（牛津大学物理系）；Department of Astronomy & Astrophysics, The Pennsylvania State University（宾夕法尼亚州立大学天文与天体物理系）
Early Results from GLASS-JWST. XXV. Electron Density in the Interstellar Medium at $0.7\lesssim z\lesssim 9.3$ with NIRSpec High-resolution Spectroscopy
The Evolution of Low-Ionization Electron Densities in Galaxies Across Cosmic Epochs
The University of Texas at Austin（德克萨斯大学奥斯汀分校）；Stockholm University（斯德哥尔摩大学）；Institute of Science and Technology Austria (ISTA)（奥地利科学技术研究所）；Space Telescope Science Institute（太空望远镜科学研究所）；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学院）
MSA-3D: Connecting the Chemical and Kinematic Structures of Galaxies at $z \sim 1$
School of Astronomy and Space Science, University of Chinese Academy of Sciences (UCAS)（中国科学院大学天文与空间科学学院）；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空间前沿研究院）；Department of Physics and Astronomy, University of California, Davis（加州大学戴维斯分校物理与天文学系）；Max-Planck-Institut für Extraterrestrische Physik (MPE)（马克斯·普朗克地外物理研究所）；Centre for Astrophysics and Supercomputing, Swinburne University of Technology（斯威本科技大学天体物理学与超级计算中心）；Astronomical Institute, Tohoku University（东北大学天文学研究所）
MSA-3D: A Diversity of Dust Attenuation Profiles Across the Epoch of Thin Disk Emergence
University of California, Davis（加州大学戴维斯分校）；University of California, Riverside（加州大学河滨分校）；University of California Los Angeles（加州大学洛杉矶分校）；University of Kentucky（肯塔基大学）；Space Telescope Science Institute（太空望远镜科学研究所）；INAF – Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；Max-Planck-Institut für extraterrestische Physik (MPE)（马克斯·普朗克地外物理学研究所）；Swinburne University of Technology（斯威本科技大学）；University of Sydney（悉尼大学）
JADES: Detecting [OIII]$λ4363$ Emitters and Testing Strong Line Calibrations in the High-$z$ Universe with Ultra-deep JWST/NIRSpec Spectroscopy up to $z \sim 9.5$
Source--Line Associations in JWST/NIRSpec Dense-Shutter Spectroscopy
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 for Astrophysical and Planetary Science, University of Colorado, Boulder（科罗拉多大学博尔德分校天文与行星科学系）；Department of Physics, University of Oxford（牛津大学物理系）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Department of Astronomy, The University of Texas at Austin（德克萨斯大学奥斯汀分校天文学系）；Cosmic Frontier Center, The University of Texas at Austin（德克萨斯大学奥斯汀分校前沿宇宙中心）；Department of Astronomy and Astrophysics, University of California, Santa Cruz（加州大学圣克鲁兹分校天文与天体物理学系）
Direct Abundance Maps and Radial Metallicity Gradients of two Galaxies at z~4-5 in the GARDEN Survey
NSF’s National Optical-Infrared Astronomy Research Laboratory（美国国家光学红外天文研究实验室）；Space Telescope Science Institute（太空望远镜科学研究所）；The William H. Miller III Department of Physics & Astronomy, Johns Hopkins University（约翰斯·霍普金斯大学威廉·H·米勒三世物理与天文学系）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）
BlackTHUNDER: Shedding light on a dormant and extreme little red dot at z=8.50
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）；Max-Planck-Institut für extraterrestrische Physik（马克斯·普朗克地外物理学研究所）；Department of Physics and Astronomy, University College London（伦敦大学学院物理与天文系）；Università degli Studi di Firenze（佛罗伦萨大学）；Dipartimento di Fisica e Astronomia, Università degli Studi di Firenze（佛罗伦萨大学物理与天文系）；INAF - Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切尔蒂天文台）
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）
DREAMS. JWST Spectroscopy of a $z=8.3$ Galaxy with an ALMA Dust Continuum Detection: Early Dust, Very High $T_{\rm dust}$, and a Multi-wavelength [OIII] Ratio Discrepancy
Institute for Cosmic Ray Research, The University of Tokyo（宇宙射线研究所，东京大学）；Department of Physics, Graduate School of Science, The University of Tokyo（理学研究科物理学系，东京大学）；National Astronomical Observatory of Japan（日本国立天文台）；Astronomical Science Program, Graduate Institute for Advanced Studies, SOKENDAI（综合研究大学院大学天文学研究科，SOKENDAI）；Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), The University of Tokyo（宇宙线起源研究宇宙前沿中心（Kavli IPMU），东京大学）；Institute of Liberal Arts and Science, Kanazawa University（金泽大学教养部）
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）
A first look at quasar-galaxy clustering at $z\simeq7.3$
Hamburger Sternwarte, Universität Hamburg（汉堡天文台，汉堡大学）；Leiden Observatory, Leiden University（莱顿天文台，莱顿大学）；Max-Planck-Institut für Astronomie（马克斯·普朗克天体物理学研究所）；Institute for Theoretical Physics, Heidelberg University（海德堡大学理论物理研究所）；Department of Astronomy, University of Michigan（密歇根大学天文学系）；Department of Physics, Massachusetts Institute of Technology（麻省理工学院物理系）；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）；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·玻尔学院宇宙黎明中心）
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）
Resolving stellar populations, star formation, and interstellar medium conditions with JWST in a large spiral galaxy at $z\approx2$
Max-Planck-Institut für extraterrestrische Physik (MPE)（马克斯·普朗克地外物理学研究所）；Scuola Normale Superiore（比萨高等师范学院）；Department of Physics and Astronomy “Augusto Righi”, University of Bologna（博洛尼亚大学物理与天文学“奥古斯托·里吉”系）；INAF – Astrophysics and Space Science Observatory of Bologna（意大利国家天体物理研究所博洛尼亚天文台）；Max-Planck-Institut für Astrophysik (MPA)（马克斯·普朗克天体物理研究所）；Department of Astronomy, University of Geneva（日内瓦大学天文学系）；Cosmic Dawn Center (DAWN), Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔学院宇宙黎明中心）
