Bren E. Backhaus, Jonathan R. Trump, Nikko J. Cleri, Raymond Simons, Ivelina Momcheva, Casey Papovich, Vicente Estrada-Carpenter, Steven L. Finkelstein, Jasleen… 展开作者
Bren E. Backhaus, Jonathan R. Trump, Nikko J. Cleri, Raymond Simons, Ivelina Momcheva, Casey Papovich, Vicente Estrada-Carpenter, Steven L. Finkelstein, Jasleen Matharu, Zhiyuan Ji, Benjamin Weiner, Mauro Giavalisco, Intae Jung
We use Hubble Space Telescope WFC3 G102 and G141 grism spectroscopy to measure rest-optical emission-line ratios of 533 galaxies at $z\sim1.5$ in the CANDELS Ly$α$ Emission at Reionization (CLEAR) survey. We compare $\frac{[OIII]}{Hβ}$ vs. $\frac{[SII]}{(Hα+[NII])}$ as an "unVO87" diagram for 461 galaxies and $\frac{[OIII]}{Hb}$ vs. $\frac{[NeIII]}{[OII]}$ as an "OHNO" diagram for 91 galaxies. The unVO87 diagram does not effectively separate active galactic nuclei (AGN) and $[NeV]$ sources from star-forming galaxies, indicating that the unVO87 properties of star-forming galaxies evolve with redshift and overlap with AGN emission-line signatures at $z>1$. The OHNO diagram effectively separates X-ray AGN and $[NeV]$-emitting galaxies from the rest of the population. We find that the $\frac{[OIII]}{Hβ}$ line ratios are significantly anti-correlated with stellar mass and significantly correlated with $\log(L_{Hβ})$, while $\frac{[SII]}{(Hα+[NII])}$ is significantly anti-correlated with $\log(L_{Hβ})$. Comparison with MAPPINGS~V photoionization models indicates that these trends are consistent with lower metallicity and higher ionization in low-mass and high-SFR galaxies. We do not find evidence for redshift evolution of the emission-line ratios outside of the correlations with mass and SFR.Our results suggest that the OHNO diagram of $\frac{[OIII]}{Hb}$ vs. $\frac{[NeIII]}{[OII]}$ will be a useful indicator of AGN content and gas conditions in very high-redshift galaxies to be observed by the James Webb Space Telescope.
HARMONI view of the host galaxies of active galactic nuclei around cosmic noon: Resolved stellar morpho-kinematics and the M$_{BH}$-$σ_{\star}$ relation
Molecular Clouds Resolved at the Onset of Cosmic Noon
National Radio Astronomy Observatory（国家射电天文台）；Université Lyon 1（里昂第一大学）；ENS de Lyon（巴黎高等师范学院里昂分校）；CNRS UMR5574, Centre de Recherche Astrophysique de Lyon（法国国家科学研究中心联合研究实验室5574，里昂天体物理研究中心）；Tsinghua University（清华大学）；Agnes Scott College（阿格尼丝·斯科特学院）；Victoria University of Wellington（惠灵顿维多利亚大学）；Centro de Astrobiología, CSIC-INTA（天体生物学中心，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）；ASTRON, the Netherlands Institute for Radio Astronomy（荷兰射电天文研究所）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）；Sorbonne Université（索邦大学）；CNRS UMR 7095, Institut d’Astrophysique de Paris（法国国家科学研究中心联合研究实验室7095，巴黎天体物理学研究所）
PAHSPECS: Spatially Resolved PAH Spectroscopy at cosmic noon with JWST MIRI MRS
University of California San Diego（加州大学圣地亚哥分校）；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）；Leiden Observatory, Leiden University（莱顿天文台，莱顿大学）；Institute of Astrophysics, Foundation for Research and Technology-Hellas (FORTH)（希腊基础与研究基金会天体物理研究所）；School of Sciences, European University Cyprus（塞浦路斯欧洲大学理学院）；Instituto de Estudios Astrofísicos, 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）；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空间科学与天体物理观测站）；Hiroshima Astrophysical Science Center, Hiroshima University（广岛大学广岛天体科学中心）
The BRIDGE Survey. I. Metallicities and Physical Properties of Gas Probing the Circumgalactic Medium at Cosmic Noon
University of Notre Dame（圣母大学）；W.M. Keck Observatory（W.M.凯克天文台）；European Southern Observatory（欧洲南方天文台）；Aix Marseille Université（艾克斯-马赛大学）；CNRS（法国国家科学研究中心）；Laboratoire d’Astrophysique de Marseille（马赛天体物理学实验室）；University of California（加利福尼亚大学）；UCO/Lick Observatory（加州大学/利克天文台）；Kavli Institute for the Physics and Mathematics of the Universe（Kavli宇宙物理与数学研究所）；National Astronomical Observatory of Japan（日本国立天文台）
Do galaxy mergers increase star formation and turbulence at cosmic noon?
Australian National University（澳大利亚国立大学）；ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D)（三维全天空天体物理学卓越研究中心）；Max-Planck-Institut für extraterrestrische Physik (MPE)（马克斯·普朗克地外物理研究所）；Laboratoire de Physique de l’École Normale Supérieure, ENS, Université PSL, CNRS, Sorbonne Université, Université Paris Cité, Observatoire de Paris（巴黎高等师范学校物理实验室）
INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所-布拉拉天文台）；Como Lake centre for AstroPhysics (CLAP)（科莫湖天体物理中心）；INFN, Sezione di Milano-Bicocca（意大利国家核物理研究所-米兰比可卡分校分部）
Formation of Substructure in Luminous Submillimeter Galaxies (FOSSILS): Initial sample and the discovery of a dusty spiral at cosmic noon
SOKENDAI (The Graduate University for Advanced Studies)（日本综合研究大学院大学）；National Astronomical Observatory of Japan（日本国立天文台）；Hokkai-Gakuen University（北海学园大学）
Spatially Resolved AGN Ionization and Star Formation at Cosmic Noon with JWST/JEMS
Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；NSF NOIRLab（美国国家科学基金会NOIR天文台）；International Gemini Observatory/NSF NOIRLab（国际Gemini天文台/美国国家科学基金会NOIR天文台）；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, Cambridge（剑桥卡弗里宇宙学研究所）
PAHSPECS: Polycyclic aromatic hydrocarbon properties at cosmic noon with JWST/MIRI MRS
University of Crete（克里特大学）；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）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CAB），西班牙国家科学研究委员会-国家航空航天技术研究所）；Leiden Observatory, Leiden University（莱顿天文台，莱顿大学）；University of California San Diego（加州大学圣地亚哥分校）；Universidad Diego Portales（迭戈·波特莱斯大学）；Millenium Nucleus for Galaxies (MINGAL)（星系千年核心（MINGAL））
MAMMOTH-Grism: Gas-phase Metallicity Gradients of Star-forming Galaxies in Protocluster Environments at Cosmic Noon
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；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）；Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University（北京师范大学天文与空间科学学院前沿科学研究院）；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 Astronomy, Tsinghua University（清华大学天文系）；Infrared Processing and Analysis Center, Caltech（加州理工学院红外处理与分析中心）
The Extremely Luminous Quasar Survey in the Sloan Digital Sky Survey footprint. III. The South Galactic Cap Sample and the Quasar Luminosity Function at Cosmic Noon
A nuclear disc at Cosmic Noon: evidence of early bar-driven galaxy evolution
Durham University（杜伦大学）；University of Manchester（曼彻斯特大学）；Universidade Federal do Rio Grande（里奥格兰德联邦大学）；Kyungpook National University（庆北国立大学）；European Southern Observatory（欧洲南方天文台）；Aix Marseille Univ, CNRS, CNES, LAM（艾克斯马赛大学、法国国家科学研究中心、法国国家空间研究中心、天体物理与行星学实验室）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）
CECILIA: Gas-Phase Physical Conditions and Multi-Element Chemistry at Cosmic Noon
Northwestern University（西北大学）；California Institute of Technology（加州理工学院）；University of Wisconsin-Madison（威斯康星大学麦迪逊分校）；The Chinese University of Hong Kong（香港中文大学）；Space Telescope Science Institute（太空望远镜科学研究所）
