Deciphering the JWST spectrum of a 'little red dot' at $z \sim 4.53$: An obscured AGN and its star-forming host
Meghana Killi, Darach Watson, Gabriel Brammer, Conor McPartland, Jacqueline Antwi-Danso, Rosa Newshore, Dan Coe, Natalie Allen, Johan P. U. Fynbo, Katriona Goul… 展开作者
Meghana Killi, Darach Watson, Gabriel Brammer, Conor McPartland, Jacqueline Antwi-Danso, Rosa Newshore, Dan Coe, Natalie Allen, Johan P. U. Fynbo, Katriona Gould, Kasper E. Heintz, Vadim Rusakov, Simone Vejlgaard
备注：
13 pages, 10 figures. Submitted to A&A. Comments welcome
JWST has revealed a class of numerous, extremely compact sources, with rest-frame red optical/near-infrared (NIR) and blue ultraviolet (UV) colours, nicknamed "little red dots". We present one of the highest signal-to-noise ratio JWST NIRSpec/PRISM spectra of a little red dot, J0647_1045 at $z = 4.5321 \pm 0.0001$, and examine its NIRCam morphology, to differentiate the origin of the UV and optical/NIR emission, and elucidate the nature of the little red dot phenomenon. J0647_1045 is unresolved ($r_e < 0.17$ kpc) in the three NIRCam long-wavelength filters, but significantly extended ($r_e = 0.45 \pm 0.06$ kpc) in the three short-wavelength filters, indicating a red compact source in a blue star-forming galaxy. The spectral continuum shows a clear change in slope, from blue in the optical/UV, to red in the restframe optical/NIR, consistent with two distinct components, fit by power-laws with different attenuation: $A_V = 0.54 \pm 0.01$ (UV) and $A_V = 5.7 \pm 0.2$ (optical/NIR). Fitting the H$α$ line requires both broad (full width at half-maximum $\sim 4300 \pm 300 km s^{-1}$) and narrow components, but none of the other emission lines, including H$β$, show evidence of broadness. We calculate $A_V = 1.1 \pm 0.2$ from the Balmer decrement using narrow H$α$ and H$β$, and $A_V > 4.1 \pm 0.2$ from broad H$α$ and upper limit on broad H$β$, consistent with the blue and red continuum attenuation respectively. Based on single-epoch H$α$ linewidth, the mass of the central black hole is $8 \pm 1 \times 10^8 M_\odot$. Our findings are consistent with a multi-component model, where the optical/NIR and broad lines arise from a highly obscured, spatially unresolved region, likely a relatively massive active galactic nucleus, while the less obscured UV continuum and narrow lines arise, at least partly, from a small but spatially resolved star-forming host galaxy.
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。
Modeling the JWST MIRI Counts, Insights Into the Source Properties and Role of Dust-Obscured AGN
Tufts University（塔夫茨大学）；Université de Strasbourg, CNRS, Observatoire Astronomique de Strasbourg（斯特拉斯堡大学、法国国家科学研究中心、斯特拉斯堡天文台）；Winona State University（威诺纳州立大学）；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）；University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）；University of Arizona（亚利桑那大学）；California Institute of Technology（加州理工学院）
JWST Spectroscopic View of a Rapidly Growing Dust-obscured Quasar at $z \sim 4$: Effect of Dust Extinction Correction on Black Hole Mass and Eddington Ratio Estimation
SHELLQs. Bridging the Gap: JWST Unveils Obscured Quasars in the Most Luminous Galaxies at z > 6
Waseda University（早稻田大学）；The University of Tokyo（东京大学）；Peking University（北京大学）；Johns Hopkins University（约翰斯·霍普金斯大学）；Ritsumeikan University（立命馆大学）；National Astronomical Observatory of Japan（日本国立天文台）；Academia Sinica Institute of Astronomy and Astrophysics（中央研究院天文及天文物理研究所）；Ehime University（爱媛大学）
No hidden monsters: Probing recently-quenched galaxies for obscured AGN with JWST-PRIMER MIRI and NIRCam
University of Nottingham（诺丁汉大学）；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）；University of Edinburgh（爱丁堡大学）；University of St Andrews（圣安德鲁斯大学）
Ultra High-Redshift or Closer-by, Dust-Obscured Galaxies? Deciphering the Nature of Faint, Previously Missed F200W-Dropouts in CEERS
Università di Padova（帕多瓦大学）；INAF, Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Department of Astronomy, The University of Texas at Austin（德克萨斯大学奥斯汀分校天文学系）；NSF’s National Optical-Infrared Astronomy Research Laboratory（美国国家光学-红外天文研究实验室）；INAF, Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Department of Physics and Astronomy, Texas A&M University（得克萨斯农工大学物理与天文系）
The MIRI Early Obscured-AGN Wide Survey (MEOW): A Population of Hidden AGN at $z \gtrsim 5$ Revealed by JWST/MIRI Imaging
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 Physics, Massachusetts Institute of Technology（麻省理工学院物理系）；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）；University of the Pacific（太平洋大学）；Space Telescope Science Institute（太空望远镜科学研究所）；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）
High redshift JWST predictions from IllustrisTNG: III. Infrared luminosity functions, obscured star formation and dust temperature of high-redshift galaxies
JWST observations and a model for the extremely luminous obscured quasar W2246-0526 at z=4.6
School of Sciences, European University Cyprus（塞浦路斯欧洲大学理学院）；CaSToRC, The Cyprus Institute（塞浦路斯研究所）；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）；Department of Physics and Astronomy, University of Hawaii（夏威夷大学物理与天文学系）；Institute for Astronomy, University of Hawaii（夏威夷大学天文研究所）
JWST PRIMER: A deep JWST study of all ALMA-detected galaxies in PRIMER COSMOS -- dust-obscured star-formation history back to z $\simeq$ 7
Institute for Astronomy, University of Edinburgh（爱丁堡大学天文研究所）；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）；Department of Physics & Astronomy, University College London（伦敦大学学院物理与天文学系）；Space Telescope Science Institute（太空望远镜科学研究所）；Department of Astronomy and Astrophysics, UCO/Lick Observatory, University of California, Santa Cruz（加州大学圣克鲁兹分校天文学与天体物理学系、UCO/莱克天文台）；INAF - Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Jodrell Bank Centre for Astrophysics, Department of Physics & Astronomy, School of Natural Sciences, The University of Manchester（曼彻斯特大学自然科学学院物理与天文学系乔德雷尔银行天体物理中心）
Kinematic Stratification in Extremely Red Quasars Revealed by JWST
The Johns Hopkins University（约翰斯·霍普金斯大学）；Florida Gulf Coast University（佛罗里达海湾海岸大学）；California Institute of Technology（加州理工学院）；University of California, Riverside（加利福尼亚大学河滨分校）；University of California, San Diego（加利福尼亚大学圣地亚哥分校）；University of Maryland, College Park（马里兰大学帕克分校）；Zentrum für Astronomie der Universität Heidelberg（海德堡大学天文中心）
Aether-SHELLQs: JWST integral-field spectroscopy of candidate obscured quasars at z ~ 6
Ehime University（爱媛大学）；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天文与空间科学观测站）；Gemini Observatory, NSF’s NOIRLab（吉米尼天文台，美国国家光学红外天文研究实验室）；Max Planck Institut für Astronomie（马克斯·普朗克天文学研究所）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）；Massachusetts Institute of Technology（麻省理工学院）；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）；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）；Princeton University（普林斯顿大学）；Observatoire de Paris, PSL University, Sorbonne Université, CNRS（巴黎天文台，巴黎文理研究大学，索邦大学，法国国家科学研究中心）
ALESS--JWST: Dust-driven Morphologies and Hidden Stellar Mass in $z\sim3$ Sub-millimeter Galaxies
International Center for Radio Astronomy Research (ICRAR), The University of Western Australia（西澳大利亚大学国际射电天文研究中心）；International Space Center (ISC), The University of Western Australia（西澳大利亚大学国际太空中心）；Leiden Observatory, Leiden University（莱顿大学莱登天文台）；Centre for Extragalactic Astronomy, Department of Physics, Durham University（杜伦大学物理系河外天文中心）；European Space Agency (ESA), ESA Office, Space Telescope Science Institute（欧洲空间局（ESA）欧洲空间局办公室太空望远镜科学研究所）；Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学天文学与天体物理学研究学院）；Space Telescope Science Institute（太空望远镜科学研究所）
Star Formation and Nebular Attenuation from Pa$α$, Br$α$, and Br$β$ in Massive Dust-obscured Galaxies at Cosmic Noon using JWST
The University of Texas at Austin（德克萨斯大学奥斯汀分校）；University of Maryland, College Park（马里兰大学帕克分校）；University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）；Tufts University（塔夫茨大学）；Space Telescope Science Institute（太空望远镜科学研究所）；University of Arizona（亚利桑那大学）；California Institute of Technology（加州理工学院）
The JWST Emission Line Survey (JELS): Multi-wavelength properties of Paschen line-emitters at Cosmic Noon
Instituto de Física y Astronomía, Universidad de Valparaíso（瓦尔帕莱索大学物理与天文学研究所）；Millennium Nucleus for Galaxies (MINGAL)（银河系千年核）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天文研究所）；Jodrell Bank Centre for Astrophysics, University of Manchester（曼彻斯特大学乔德雷尔银行天体物理学中心）；Institute of Science and Technology Austria (IS（奥地利科学与理工学院）
A SPectroscopic survey of biased halos In the Reionization Era (ASPIRE): Spectroscopically Complete Census of Obscured Cosmic Star Formation Rate Density at $z=4-6$
A JWST MIRI LRS Survey of 37 Massive Star-Forming Galaxies and AGN at Cosmic Noon -- Overview and First Results
The University of Texas at Austin（德克萨斯大学奥斯汀分校）；University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）；Tufts University（塔夫茨大学）；Space Telescope Science Institute（太空望远镜科学研究所）；University of Arizona（亚利桑那大学）；University of Kansas（堪萨斯大学）；California Institute of Technology（加州理工学院）；University of California Santa Barbara（加州大学圣巴巴拉分校）；Foundation for Research and Technology-Hellas (FORTH)（希腊研究基金会）；European University Cyprus（塞浦路斯欧洲大学）；NASA-Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；University of Washington（华盛顿大学）
