Clumps as multiscale structures in cosmic noon galaxies
Boris S Kalita, Tomoko L Suzuki, Daichi Kashino, John D Silverman, Emanuele Daddi, Luis C Ho, Xuheng Ding, Wilfried Mercier, Andreas L Faisst, Kartik Sheth, Fra… 展开作者
Boris S Kalita, Tomoko L Suzuki, Daichi Kashino, John D Silverman, Emanuele Daddi, Luis C Ho, Xuheng Ding, Wilfried Mercier, Andreas L Faisst, Kartik Sheth, Francesco Valentino, Annagrazia Puglisi, Toshiki Saito, Darshan Kakkad, Olivier Ilbert, Ali Ahmad Khostovan, Zhaoxuan Liu, Takumi Tanaka, Georgios Magdis, Jorge A Zavala, Qinghua Tan, Jeyhan S Kartaltepe, Lilan Yang, Anton M Koekemoer, Jed McKinney, Brant E Robertson, Shuowen Jin, Christopher C Hayward, Michaela Hirschmann, Maximilien Franco, Marko Shuntov, Ghassem Gozaliasl, Aidan Kaminsky, R Michael Rich
Star-forming clumps have been found to significantly influence the star formation of gas-rich $z>1$ galaxies. Using public data from JWST/NIRCam (COSMOS-Web) and ALMA (FMOS-COSMOS), we study a sample of 32 massive ($>10^{10.5}\,\rm M_{\odot}$) main-sequence galaxies at $z_{\rm spec}\sim1.5$ with $\sim0.3\,\rm kpc$ resolution. We create composite morphological models consisting of bulge, disk, and clumps to fully 'deconstruct' the galaxy images. With the resulting measurements of the flux and size of these components, we find the following: (I)The combined contribution of clumps is $1-30\%$ towards the net star formation rate (SFR) of the host while contributing $1-20\%$ to its stellar mass. The clumps show a correlation between their stellar mass and SFR, but have an increased specific-SFR (sSFR) relative to the star-forming main sequence, with offsets ranging from $0\lesssimΔ\log\rm sSFR\lesssim 0.4$. They feature star formation surface densities of $10^{-2}-10^{2}\,\rm M_{\odot}/yr/kpc^{2}$, consistent with values observed in local star-forming and starburst galaxies. (II)The clumps span a large range of characteristic sizes ($r_{e}\sim0.1-1\,\rm kpc$) and stellar masses ($\sim 10^{8.0-9.5}\,\rm M_{\odot}$). We estimate a mass-size relation ($r_{e}\propto\rm M_{\star}^{\,0.52\pm0.07}$) along with a stellar mass function (slope, $α=-1.85\pm 0.19$), both suggesting a hierarchical nature similar to that expected in star-forming regions in local galaxies. (III)Our measurements agree with the properties of stellar clumps in $z\gtrsim1$ lensed systems, bridging the gap between lensed and unlensed studies by detecting structures at sub-kpc scales.(IV)Clumps are found to be preferentially located along spiral features visible primarily in the residual rest-frame near-IR images. In conclusion, we present an observation-based, coherent picture of star-forming clumps at $z>1$.
The MICADO first light imager for the ELT: Simulated Observations of Star Forming Clumps at Cosmic Noon
INAF - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；INAF - Osservatorio Astronomico d’Abruzzo（意大利国家天体物理研究所阿布鲁佐天文台）；INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛纳天文物理与空间科学观测站）；European Southern Observatory（欧洲南方天文台）
本文评估 ELT 的 MICADO 仪器通过模拟观测表征非透镜 z=2 星系中恒星形成团块的能力，证明其可探测至 R_e~20 pc 的团块，填补关键观测空白。
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）
Metal-Poor Gas Accretion Drives Giant Clump Formation at 0.6 < z < 2.6
University of Colorado（科罗拉多大学）；York University（约克大学）；University of California, Davis（加州大学戴维斯分校）；University of California, Merced（加州大学默塞德分校）；Harvard University（哈佛大学）；University of Toronto（多伦多大学）；Dunlap Institute for Astronomy and Astrophysics（邓普勒天文学与天体物理研究所）
NOEMA3D: Extended CO, [C I] and dust in massive star-forming main-sequence galaxies at cosmic noon
Max-Planck-Institut für extraterrestrische Physik（马克斯·普朗克地外物理研究所）；University of California, Berkeley（加州大学伯克利分校）；Institut de Radioastronomie Millimétrique (IRAM)（毫米波射电天文研究所）；Max-Planck-Institut für Astrophysik (MPA)（马克斯·普朗克天体物理研究所）；University of Bologna（博洛尼亚大学）；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与空间科学观测站）
JWST+ALMA reveal the build up of stellar mass in the cores of dusty star-forming galaxies at Cosmic Noon
University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）；Cosmic Dawn Center (DAWN)（黎明宇宙中心）；Tufts University（塔夫茨大学）；University of Geneva（日内瓦大学）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Technical University of Denmark（丹麦技术大学）
An ALMA study of the massive molecular clump N159W-North in the Large Magellanic Cloud: A possible gas flow penetrating one of the most massive protocluster systems in the Local Group
MEGATRON: the impact of non-equilibrium effects and local radiation fields on the circumgalactic medium at cosmic noon
Sorbonne Université（索邦大学）；University of Chicago（芝加哥大学）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理学研究所）；University of Bath（巴斯大学）；Lund University（隆德大学）；Univ Lyon 1, ENS de Lyon（里昂第一大学，里昂高等师范学院）；University of Oxford（牛津大学）；University of Cambridge（剑桥大学）
LEGGOS II: A Strong Lens Model and Source-Plane Projection of the Clumpy Star-Forming Galaxy SGASJ111020.0+645950.8 at z=2.48
University of Michigan（密歇根大学）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；University of Maryland（马里兰大学）；Center for Research and Exploration in Space Science and Technology, NASA/GSFC（NASA/戈达德太空飞行中心空间科学与技术研究探索中心）；University of Cincinnati（辛辛那提大学）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Eureka Scientific（尤里卡科学公司）；University of Washington（华盛顿大学）
An ALMA sub-kiloparsec test of the Kennicutt--Schmidt relation in a strongly lensed dusty star-forming galaxy at $z\sim2.78$
Universidad de Valparaíso（瓦尔帕莱索大学）；Millenium Nucleus for Galaxies (MINGAL)（星系千年核（MINGAL））；STAR Institute（STAR研究所）；Université Côte d’Azur（蔚蓝海岸大学）；University of Florida（佛罗里达大学）；Universidad Nacional Autónoma de México（墨西哥国立自治大学）；Instituto Nacional de Astrofísica Óptica y Electrónica (INAOE)（国家天体物理学、光学和电子学研究所）；Universidad Central de Chile（智利中央大学）
The ALMA Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE): Core Growth, Cluster Contraction, and Primordial Mass Segregation
A first GLIMPSE into star clusters populations across cosmic time
Univ Lyon, Univ Lyon1, Ens de Lyon, CNRS, CRAL UMR5574（里昂大学）；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宇宙前沿中心）；Centre for Extragalactic Astronomy, Department of Physics, Durham University（杜伦大学物理系河外天文研究中心）；Institute for Computational Cosmology, Department of Physics, Durham University（杜伦大学物理系计算宇宙学研究所）；Department of Astronomy, University of Geneva（日内瓦大学天文学系）；Institut d’Astrophysique de Paris, CNRS, Sorbonne Université（巴黎天体物理研究所）
Evidence for Shallow Nebular Attenuation Curves and Patchy Dust Geometry at z~2 with Pa-beta/H-alpha Measurements from JWST-MegaScience Medium Band Photometry
University of California, Berkeley（加州大学伯克利分校）；University of Colorado, Boulder（科罗拉多大学博尔德分校）；Leiden University（莱顿大学）；Space Telescope Science Institute（太空望远镜科学研究所）；The Pennsylvania State University（宾夕法尼亚州立大学）；Institut d’Astrophysique de Paris, CNRS, Sorbonne Université（巴黎天体物理研究所，法国国家科学研究中心，索邦大学）；University of Pittsburgh（匹兹堡大学）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）
The Stellar Population of NGC 346 in the Small Magellanic Cloud with JWST
Maynooth University（梅努斯大学）；Dublin Institute for Advanced Studies（都柏林高等研究院）；European Space Research and Technology Centre（欧洲空间研究与技术中心）；University of Edinburgh（爱丁堡大学）；Royal Observatory（皇家天文台）；California Institute of Technology（加州理工学院）；AURA for the European Space Agency, ESA Office, STScI（美国大学研究协会（代表欧洲航天局，ESA办公室，STScI））；Space Telescope Science Institute（太空望远镜科学研究所）；Morgan State University（摩根州立大学）；INAF, Astronomical Observatory of Rome（意大利国家天体物理研究所，罗马天文台）
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）
