The emergence of the Star Formation Main Sequence with redshift unfolded by JWST
P. Rinaldi, R. Navarro-Carrera, K. I. Caputi, E. Iani, G. Ostlin, L. Colina, S. Alberts, J. Alvarez-Marquez, M. Annunziatella, L. Boogaard, L. Costantin, J. Hjo… 展开作者
P. Rinaldi, R. Navarro-Carrera, K. I. Caputi, E. Iani, G. Ostlin, L. Colina, S. Alberts, J. Alvarez-Marquez, M. Annunziatella, L. Boogaard, L. Costantin, J. Hjorth, D. Langeroodi, J. Melinder, T. Moutard, F. Walter
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16 pages, 5 figures, 1 table. Accepted for publication in ApJ
We investigate the correlation between stellar mass (M*) and star formation rate (SFR) across the stellar mass range log10(M*/Msun)~6-11. We consider almost 50,000 star-forming galaxies at z~3-7, leveraging data from COSMOS/SMUVS, JADES/GOODS-SOUTH, and MIDIS/XDF. This is the first study spanning such a wide stellar mass range without relying on gravitational lensing effects. We locate our galaxies on the SFR-M* plane to assess how the location of galaxies in the star-formation main sequence (MS) and starburst (SB) region evolves with stellar mass and redshift. We find that the two star-forming modes tend to converge at log10(M*/Msun) < 7, with all galaxies found in the SB mode. However, deeper observations will be instrumental for reaching lower SFRs and Msun to further validate this scenario. By dissecting our galaxy sample in stellar mass and redshift, we show that the emergence of the star-formation MS is stellar-mass dependent: while in galaxies with log10(M*/Msun) > 9 the MS is already well in place at z = 5-7, for galaxies with log10(M*/Msun)~7-8 it only becomes significant at z<4. Overall, our results are in line with previous findings that the SB mode dominates amongst low stellar-mass galaxies. The earlier emergence of the MS for massive galaxies is consistent with galaxy downsizing.
The importance of super-Eddington black hole accretion for the emergence of massive quiescent galaxies at high redshift
Institute for Computational Cosmology, Department of Physics, University of Durham（达勒姆大学物理系计算宇宙学研究所）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Lorentz Institute for Theoretical Physics, Leiden University（莱顿大学洛伦兹理论物理研究所）；Department of Astrophysics, University of Vienna（维也纳大学天体物理学系）
MEOW: The increase in the obscured AGN fraction in mid-infrared from 0 < z < 6 with JWST MIRI
Massachusetts Institute of Technology（麻省理工学院）；Kavli Institute for Astrophysics and Space Research（卡弗里天体物理学与空间研究所）；Department of Physics, Massachusetts Institute of Technology（麻省理工学院物理系）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CAB），西班牙国家航空航天技术研究所/西班牙高等科学研究理事会）；Department of Physics, University of the Pacific（太平洋大学物理系）；Department of Astronomy, The University of Texas at Austin（德克萨斯大学奥斯汀分校天文系）；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）
利用JWST MIRI数据，研究发现0 < z < 6范围内 obscured AGN 分数随红移增加而显著上升，揭示了光学/紫外波段无法检测到的大量被尘埃遮蔽的AGN。
Duration and properties of the embedded phase of star formation in 37 nearby galaxies from PHANGS-JWST
Zentrum für Astronomie der Universität Heidelberg（海德堡大学天文中心）；Cosmic Origins Of Life (COOL) Research DAO（生命宇宙起源（COOL）研究DAO）；Kavli Institute for Particle Astrophysics & Cosmology, Stanford University（斯坦福大学卡弗里粒子天体物理与宇宙学研究所）；INAF — Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；European Southern Observatory（欧洲南方天文台）；Department of Physics, University of Arkansas（阿肯色大学物理系）；Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange（蔚蓝海岸大学、蔚蓝海岸天文台、法国国家科学研究中心拉格朗日实验室）；Department of Astronomy, The Ohio State University（俄亥俄州立大学天文学系）
JWST PRIMER: Post-starburst galaxies dominate the low-mass quiescent galaxy population since z~2
University of Nottingham（诺丁汉大学）；University of St Andrews（圣安德鲁斯大学）；University of Edinburgh（爱丁堡大学）；Johns Hopkins University（约翰斯·霍普金斯大学）；Space Telescope Science Institute（太空望远镜科学研究所）
Probing the Cosmic Reionization History with JWST: Gunn-Peterson and Ly$α$ Damping Wing Absorption at $4.5 < z < 13$
The University of Tokyo（东京大学）；National Astronomical Observatory of Japan（日本国立天文台）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo（东京大学宇宙物理数学研究所（WPI））
From stardust to interstellar grain growth in the first galaxies: a cosmological transition in dust evolution near z ~ 8.9
Aix Marseille Université, CNRS, CNES, LAM（艾克斯马赛大学）；Chalmers University of Technology（查尔姆斯理工大学）；Dipartimento di Fisica, “Sapienza” Università di Roma（罗马智慧大学物理系）；INAF/Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；INFN, Sezione di Roma I（意大利国家核物理研究所罗马第一分部）；Sapienza School for Advanced Studies（罗马智慧大学高等研究院）；Institute of Astronomy and Astrophysics, Academia Sinica（中央研究院天文及天文物理学研究所）
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 ））
Mass regulates the emerging timescale of young star clusters
Stockholm University（斯德哥尔摩大学）；University of Massachusetts（马萨诸塞大学）；Queen Mary University of London（伦敦玛丽女王大学）；Australian National University（澳大利亚国立大学）；University of Arizona（亚利桑那大学）；Space Telescope Science Institute（太空望远镜科学研究所）
The Cosmic Rush Hour: Rapid Formation of Bright, Massive, Disky, Star-Forming Galaxies as Signatures of Early-Universe Physics
Massachusetts Institute of Technology（麻省理工学院）；Center for Astrophysics | Harvard & Smithsonian（天体物理中心 | 哈佛与史密森尼学会）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；University of Cambridge（剑桥大学）
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）
To high redshift and low mass: exploring the emergence of quenched galaxies and their environments at $3<z<6$ in the ultra-deep JADES MIRI F770W parallel
An emerging baryon cycle in a galaxy 500 million years after the Big Bang
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）；Department of Astronomy, Tsinghua University（清华大学天文系）；School of Astronomy and Space Science, Nanjing University（南京大学天文与空间科学学院）；Department of Astronomy, School of Physics, Peking University（北京大学物理学院天文系）；Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学科维理天文与天体物理研究所）
The MandelZoom project II: the impact of stellar feedback on black hole accretion through an $α$-disc in dwarf galaxies with a resolved interstellar medium
Institute of Astronomy, University of Cambridge（剑桥大学天文学研究所）；Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）；Centre for Astrophysics Research, Department of Physics, Astronomy and Mathematics, University of Hertfordshire（赫特福德大学物理、天文与数学系天体物理研究中心）；St Catharine’s College, University of Cambridge（剑桥大学圣凯瑟琳学院）
Intense and extended CIII] emission suggests a strong outflow in JADES-GS-z14-0
Scuola Normale Superiore（高等师范学院）；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）；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）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Centro de Astrobiología (CAB), CSIC-INTA（西班牙国家航空航天技术研究所/西班牙国家研究委员会天体生物学中心）；Department of Physics, University of Oxford（牛津大学物理系）；Sorbonne Université, CNRS（索邦大学法国国家科学研究中心）
Hunting the first Cosmic Giants: formation and detectability of Direct Collapse Black Holes around high-redshift quasars
University of Edinburgh（爱丁堡大学）；Università degli Studi dell’Insubria（因苏布利亚大学）；INAF/Osservatorio Astronomico di Roma（罗马天文台国家 Astrophysics 研究所）；INFN, Sezione di Milano-Bicocca（米兰比可卡大学 INFN 分部）；Institute of Science and Technology Austria (ISTA)（奥地利科学与理工学院）；Columbia University（哥伦比亚大学）；Institut d’Astrophysique de Paris, Sorbonne Université（巴黎天体物理研究所，索邦大学）
