Exploring AGN and Star Formation Activity of Massive Galaxies at Cosmic Noon
Jonathan Florez, Shardha Jogee, Sydney Sherman, Matthew L. Stevans, Steven L. Finkelstein, Casey Papovich, Lalitwadee Kawinwanichakij, Robin Ciardullo, Caryl Gr… 展开作者
Jonathan Florez, Shardha Jogee, Sydney Sherman, Matthew L. Stevans, Steven L. Finkelstein, Casey Papovich, Lalitwadee Kawinwanichakij, Robin Ciardullo, Caryl Gronwall, C. Megan Urry, Allison Kirkpatrick, Stephanie M. LaMassa, Tonima Tasnim Ananna, Isak Wold
备注：
27 pages, 15 figures. Accepted for publication in MNRAS
We investigate the relation between AGN and star formation (SF) activity at $0.5 < z < 3$ by analyzing 898 galaxies with X-ray luminous AGN ($L_X > 10^{44}$ erg s$^{-1}$) and a large comparison sample of $\sim 320,000$ galaxies without X-ray luminous AGN. Our samples are selected from a large (11.8 deg$^2$) area in Stripe 82 that has multi-wavelength (X-ray to far-IR) data. The enormous comoving volume ($\sim 0.3$ Gpc$^3$) at $0.5 < z < 3$ minimizes the effects of cosmic variance and captures a large number of massive galaxies ($\sim 30,000$ galaxies with $M_* > 10^{11} \ M_{\odot}$) and X-ray luminous AGN. While many galaxy studies discard AGN hosts, we fit the SED of galaxies with and without X-ray luminous AGN with Code Investigating GALaxy Emission (CIGALE) and include AGN emission templates. We find that without this inclusion, stellar masses and star formation rates (SFRs) in AGN host galaxies can be overestimated, on average, by factors of up to $\sim 5$ and $\sim 10$, respectively. The average SFR of galaxies with X-ray luminous AGN is higher by a factor of $\sim 3$ to $10$ compared to galaxies without X-ray luminous AGN at fixed stellar mass and redshift, suggesting that high SFRs and high AGN X-ray luminosities may be fueled by common mechanisms. The vast majority ($> 95 \%$) of galaxies with X-ray luminous AGN at $z=0.5-3$ do not show quenched SF: this suggests that if AGN feedback quenches SF, the associated quenching process takes a significant time to act and the quenched phase sets in after the highly luminous phases of AGN activity.
In theoretical models of galaxy evolution, AGN and star formation (SF) activity are closely linked and AGN feedback is routinely invoked to regulate galaxy growth. In order to constrain such models, we compare the hydrodynamical simulations IllustrisTNG and SIMBA, and the semi-analytical model SAG to the empirical results on AGN and SF at cosmic noon ($0.75 < z < 2.25$) reported in Florez et al. (2020). The empirical results are based on a large mass-complete sample drawn from 93,307 galaxies with and without high X-ray luminosity AGN ($L_X \gtrsim 10^{44}$ erg s$^{-1}$), selected from a 11.8 …
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）
For over 60 years, the scientific community has studied actively growing central super-massive black holes (active galactic nuclei -- AGN) but fundamental questions on their genesis remain unanswered. Numerical simulations and theoretical arguments show that black hole growth occurs during short-lived periods ($\sim$ 10$^{7}$ -10$^{8}$ yr) of powerful accretion. Major mergers are commonly invoked as the most likely dissipative process to trigger the rapid fueling of AGN. If the AGN-merger paradigm is true, we expect galaxy mergers to coincide with black hole accretion during a heavily obscured…
Gaseous outflows are key phenomena in the evolution of galaxies, as they affect star formation (either positively or negatively), eject gas from the core or disk, and directly cause mixing of pristine and processed material. Active outflows may be detected through searches for broad spectral line emission or high-velocity gas, but it is also possible to determine the presence of past outflows by searching for extended reservoirs of chemically enriched molecular gas in the circumgalactic medium (CGM) around galaxies. In this work, we examine the CO(3-2) emission of a set of seven z~2.0-2.5 AGN …
Context. The formation and evolution of galaxies appear linked to the growth of supermassive black holes, as evidenced by empirical scaling relations in nearby galaxies. Understanding this co-evolution over cosmic time requires the revelation of the dynamical state of galaxies and the measurement of the mass of their central black holes (MBH) at a range of cosmic distances. Bright active galactic nuclei (AGNs) are ideal for this purpose. Aims. The High Angular Resolution Monolithic Optical and Near-infrared Integral field spectrograph (HARMONI), the first light integral-field spectrograph for …
The major merger-active galactic nucleus connection up to the cosmic noon
SRON Netherlands Institute for Space Research（荷兰空间研究所）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）；European Space Agency/ESTEC（欧洲航天局/欧洲空间研究与技术中心）；Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México（墨西哥国立自治大学无线电天文学与天体物理研究所）；School of Physics and Astronomy, University of Nottingham（诺丁汉大学物理与天文学院）
Statistical studies of X-ray selected Active Galactic Nuclei (AGN) indicate that the fraction of obscured AGN increases with increasing redshift, and the results suggest that a significant part of the accretion growth occurs behind obscuring material in the early universe. We investigate the obscured fraction of highly accreting X-ray AGN at around the peak epoch of supermassive black hole growth utilizing the wide and deep X-ray and optical/IR imaging datasets. A unique sample of luminous X-ray selected AGNs above $z>2$ was constructed by matching the XMM-SERVS X-ray point-source catalog with…
SUNRISE-3D: Sharp UNveiling of AGN feedback Regulation and its Impact on Star-formation at the cosmic noon Epoch
INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica Milano（意大利国家天体物理研究所空间天体物理与宇宙学米兰研究所）；INAF - Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Department of Mathematics and Physics, Roma Tre University（罗马第三大学数学与物理系）
We present the high-mass end of the galaxy stellar mass function using the largest sample to date (5,352) of star-forming galaxies with $M_{\star} > 10^{11} M_{\odot}$ at cosmic noon, $1.5 < z < 3.5$. This sample is uniformly selected across 17.2 deg$^2$ ($\sim$0.44 Gpc$^3$ comoving volume from $1.5 < z < 3.5$), mitigating the effects of cosmic variance and encompassing a wide range of environments. This area, a factor of 10 larger than previous studies, provides robust statistics at the high-mass end. Using multi-wavelength data in the Spitzer/HETDEX Exploratory Large Area (SHELA) footprint w…
Tracing Radio AGN-Driven Quenching in Post-Starburst Galaxies at Cosmic Noon
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）；AURA for ESA, Space Telescope Science Institute（欧洲空间局阿雷西博大学协会太空望远镜科学研究所）；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）；European Southern Observatory (ESO)（欧洲南方天文台）
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 re…
Ever deeper and wider lookback surveys have led to a fairly robust outline of the cosmic star formation history, which culminated around z~2 -- a period often nicknamed "cosmic noon." Our knowledge about star-forming galaxies at these epochs has dramatically advanced from increasingly complete population censuses and detailed views of individual galaxies. We highlight some of the key observational insights that influenced our current understanding of galaxy evolution in the equilibrium growth picture: $\bullet$ scaling relations between galaxy properties are fairly well established among massi…
Feedback from AGN is thought to be key in shaping the life cycle of their host galaxies by regulating star-formation activity. Therefore, to understand the impact of AGN on star formation, it is essential to trace the molecular gas out of which stars form. In this paper we present the first systematic study of the CO properties of AGN hosts at z~2 for a sample of 27 X-ray selected AGN spanning two orders of magnitude in AGN bolometric luminosity (Lbol= 10^44.7-10^46.9 erg/s) by using ALMA Band 3 observations of the CO(3-2) transition (~1" angular resolution). To search for evidence of AGN feed…
We use the SPace Infrared telescope for Cosmology and Astrophysics (SPICA) project as a template to demonstrate how deep spectrophotometric surveys covering large cosmological volumes over extended fields (1-15 square degrees) with a mid-IR imaging spectrometer (17-36 micron) in conjunction with deep 70 micron photometry with a far-IR camera, at wavelengths which are not affected by dust extinction can answer the most crucial questions in current galaxy evolution studies. A SPICA-like mission will be able for the first time to provide an unobscured three dimensional (3-D, i.e. x, y and redshif…
We present spatially resolved H$α$ properties of 21 type 1 AGN host galaxies at z$\sim$2 derived from the SUPER survey. These targets were observed with the adaptive optics capabilities of the SINFONI spectrograph, a near-infrared integral field spectrograph, that provided a median spatial resolution of 0.3 arcsec ($\sim$2 kpc). We model the H$α$ emission line profile in each pixel to investigate whether it traces gas in the narrow line region or if it is associated with star formation. To do this, we first investigate the presence of resolved H$α$ emission by removing the contribution of the …
The onset of stellar bars at Cosmic Noon. Bar-driven quenching and AGN co-evolution in a mature disc galaxy
Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心）；Departamento de Astronomía, Universidad de La Serena（拉塞雷纳大学天文系）；Instituto de Astrofísica de Canarias（加那利群岛天体物理学研究所）；Departamento de Astrofísica de la Universidad de La Laguna（拉古纳大学天体物理学系）；Department of Physics, Faculty of Science, Ferdowsi University of Mashhad（马什哈德菲尔道西大学理学院物理系）；INAF – Osservatorio Astronomico di Padova（帕多瓦天文台）；Dipartimento di Fisica e Astronomia “G. Galilei”, Università di Padova（帕多瓦大学伽利略物理与天文学系）
Cosmic Duets II. Growth and accretion in Gaia Multi-Peak dual AGN at Cosmic Noon
University of Trento（特伦托大学）；INAF – Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所（西班牙高等科研理事会））；INAF – Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）；Institut d’Astrophysique de Paris（巴黎天体物理研究所）；INAF - Istituto di Astrofisica e Planetologia Spaziali（意大利国家天体物理研究所天文与行星物理学研究所）；Max Planck Institute for extraterrestrial Physics（马克斯·普朗克地外物理研究所）；Centro de Astrobiología (CAB), CSIC–INTA（天体生物学中心（西班牙高等科研理事会-国家航空航天技术研究所））
Varstrometry for Off-nucleus and Dual Subkiloparsec AGN (VODKA): Three Quadruply Lensed Quasars at Cosmic Noon in HST and JWST
Johns Hopkins University（约翰斯·霍普金斯大学）；University of Illinois at Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；Wuhan University（武汉大学）；Institute for Advanced Study（普林斯顿高等研究院）；Massachusetts Institute of Technology（麻省理工学院）
We investigate the presence of ionised gas outflows in a sample of 141 main-sequence star-forming galaxies at $1.2<z<2.6$ from the KLEVER (KMOS Lensed Emission Lines and VElocity Review) survey. Our sample covers an exceptionally wide range of stellar masses, $8.1<\log(M_\star/M_{\odot})<11.3$, pushing outflow studies into the dwarf regime thanks to gravitationally lensed objects. We stack optical rest-frame emission lines (H$β$, [OIII], H$α$ and [NII]) in different mass bins and seek for tracers of gas outflows by using a novel, physically motivated method that improves over the widely used, …
JWST MIRI color classification of mid-infrared selected galaxies: MIRI color classification toward cosmic noon
Department of Astronomy and Space Sciences, Science Faculty, İstanbul University（伊斯坦布尔大学理学院天文学与空间科学系）；Institute of Astronomy, National Tsing Hua University（国立清华大学天文研究所）；Department of Physics and Astronomy, University of California Los Angeles（加州大学洛杉矶分校物理与天文学系）；Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies)（日本综合研究大学院大学天文学科学系）；National Astronomical Observatory of Japan（日本国立天文台）；Department of Physics, National Chung Hsing University（国立中兴大学物理系）；Research School of Astronomy and Astrophysics, The Australian National University（澳大利亚国立大学天文与天体物理研究学院）；Sabancı University, Faculty of Engineering and Natural Sciences（萨班哲大学工程与自然科学学院）
We analyse the star formation rates (SFRs), colours, and dust extinctions of galaxies in massive (10^12.5-10^13.5 Msun) haloes at z~2 in high-resolution, cosmological zoom-in simulations as part of the Feedback in Realistic Environments (FIRE) project. The simulations do not model feedback from active galactic nuclei (AGN) but reproduce well the observed relations between stellar and halo mass and between stellar mass and SFR. About half (a third) of the simulated massive galaxies (massive central galaxies) at z~2 have broad-band colours classifying them as 'quiescent', and the fraction of qui…
Emission-line Variable Active Galactic Nuclei at Cosmic Noon from HETDEX
Department of Astronomy, The University of Texas at Austin（德克萨斯大学奥斯汀分校天文学系）；McDonald Observatory, The University of Texas at Austin（德克萨斯大学奥斯汀分校麦克唐纳天文台）；Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台光学天文重点实验室）；Department of Astronomy & Astrophysics, The Pennsylvania State University（宾夕法尼亚州立大学天文学与天体物理学系）；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）；Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences（中国科学院天体结构与演化重点实验室）
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））
We analyze by detailed modelling the spectra observed from the sample galaxies at z$\sim$0.8 presented by Ly et al (2015), constraining the models by the [OIII]5007+4959/[OIII]4363 line ratios. Composite models accounting for shock and photoionization by AGN or starburst are adopted. O/H are about solar for all the objects, except for a few AGN clouds with O/H= 0.3 -0.5 solar. Starburst models reproduce most of the data within the observational errors. About half of the object spectra are well fitted by an accreting AGN. Some galaxies show multiple radiation sources, such as starburst+AGN, or …
A jet-gas interaction beyond the host galaxy: detection of a neutral hydrogen outflow at cosmic noon
Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；School of Chemical and Physical Sciences, Victoria University of Wellington（惠灵顿维多利亚大学化学与物理科学学院）；First Light Fusion Ltd.（第一缕光融合有限公司）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天体物理研究所）；Inter-University Institute for Data Intensive Astronomy, Department of Astronomy, University of Cape Town（开普敦大学天文学系数据密集型天文跨大学研究所）；International Centre for Radio Astronomy Research (ICRAR), Curtin University（科廷大学国际射电天文研究中心）；ATNF, CSIRO Space and Astronomy（澳大利亚联邦科学与工业研究组织空间与天文台射电天文国家设施）；State Key Laboratory of Radio Astronomy and Technology（射电天文与技术国家重点实验室）；College of Physics, Guizhou University（贵州大学物理学院）
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）
