Piercing through Highly Obscured and Compton-thick AGNs in the Chandra Deep Fields. II. Are Highly Obscured AGNs the Missing Link in the Merger-triggered AGN–Galaxy Coevolution Models?

Li, Junyao; Xue, Yongquan; Brandt, W. N.; Yang, Guang; Vito, F.; Tozzi, P.; Vignali, C.; Comastri, A.; Shu, Xinwen; Fang, Guanwen; Fan, Lulu; Chen, Chien-Ting; Zheng, Xuechen

doi:10.3847/1538-4357/abb6e7

Cited by 13 publications

(7 citation statements)

References 160 publications

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“…Moreover, depending upon the selection criteria, the resulting MIR AGN sample may be contaminated by star-forming galaxies, especially for the criterion in Lacy et al (2007). The criterion in Donley et al (2012) is generally more reliable in avoiding the misclassification of star-forming galaxies as AGNs, but it may miss the highly obscured AGNs (e.g., Li et al 2020). In this work, we select MIR AGN candidates if a source is detected in all four IRAC bands with a signal-to-noise ratio (S/N) above three and meets any criterion in Stern et al (2005), Lacy et al (2007), or Donley et al (2012) so that the resulting MIR AGN sample is as complete as possible.…”

Section: An Overview Of Different Selection Methodsmentioning

confidence: 99%

Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties

Zou

Brandt

Chen

et al. 2022

ApJS

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W-CDF-S, ELAIS-S1, and XMM-LSS will be three Deep-Drilling Fields (DDFs) of the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST), but their extensive multiwavelength data have not been fully utilized as done in the COSMOS field, another LSST DDF. To prepare for future science, we fit source spectral energy distributions (SEDs) from X-ray to far-infrared in these three fields mainly to derive galaxy stellar masses and star formation rates. We use CIGALE v2022.0, a code that has been regularly developed and evaluated, for the SED fitting. Our catalog includes 0.8 million sources covering 4.9 deg2 in W-CDF-S, 0.8 million sources covering 3.4 deg2 in ELAIS-S1, and 1.2 million sources covering 4.9 deg2 in XMM-LSS. Besides fitting normal galaxies, we also select candidates that may host active galactic nuclei (AGNs) or are experiencing recent star formation variations and use models specifically designed for these sources to fit their SEDs; this increases the utility of our catalog for various projects in the future. We calibrate our measurements by comparison with those in well-studied smaller regions and briefly discuss the implications of our results. We also perform detailed tests of the completeness and purity of SED-selected AGNs. Our data can be retrieved from a public website.

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Section: An Overview Of Different Selection Methodsmentioning

confidence: 99%

Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties

Zou

Brandt

Chen

et al. 2022

ApJS

Self Cite

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“…With these observations, accurate estimates of N H and intrinsic X-ray luminosity can be made. Li et al (2020) improved this analysis for the most heavily obscured AGNs within CDF-N/S. Estimates of the intrinsic X-ray luminosity and column density are taken from Li et al (2020) when available.…”

Section: Goodsmentioning

confidence: 99%

The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei

Auge,

Sanders,

Treister

et al. 2023

ApJ

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Spectral energy distributions (SEDs) from X-ray to far-infrared (FIR) wavelengths are presented for a sample of 1246 X-ray-luminous active galactic nuclei (AGNs; L 0.5–10 keV > 1043 erg s−1), with z spec < 1.2, selected from Stripe 82X, COSMOS, and GOODS-N/S. The rest-frame SEDs show a wide spread (∼2.5 dex) in the relative strengths of broad continuum features at X-ray, ultraviolet (UV), mid-infrared (MIR), and FIR wavelengths. A linear correlation (log–log slope of 0.7 ± 0.04) is found between L MIR and L X. There is significant scatter in the relation between the L UV and L X owing to heavy obscuration; however, the most luminous and unobscured AGNs show a linear correlation (log–log slope of 0.8 ± 0.06) in the relation above this scatter. The relation between L FIR and L X is predominantly flat, but with decreasing dispersion at L X > 1044 erg s−1. The ratio between the “galaxy-subtracted” bolometric luminosity and the intrinsic L X increases from a factor of ∼10 to 70 from log L bol/(erg s−1) = 44.5 to 46.5. Characteristic SED shapes have been determined by grouping AGNs based on relative strengths of the UV and MIR emission. The average L 1μm is constant for the majority of these SED shapes, while AGNs with the strongest UV and MIR emission have elevated L 1μm, consistent with the AGN emission dominating their SEDs at optical and near-infrared wavelengths. A strong correlation is found between the SED shape and both the L X and L bol, such that L bol/L X = 20.4 ± 1.8, independent of the SED shape. This is consistent with an evolutionary scenario of increasing L bol with decreasing obscuration as the AGN blows away circumnuclear gas.

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“…SFRs estimated from far-IR luminosities have been used to conclude that quasar host galaxies tend to lie on or near to the star-forming galaxy main sequence [25,49,91,158,198,251,258,328,339]. However, Xie et al [326] recently concluded that AGN hosts predominantly lie above the main sequence.…”

Section: Star Formationmentioning

confidence: 99%

Infrared Spectral Energy Distribution and Variability of Active Galactic Nuclei: Clues to the Structure of Circumnuclear Material

Lyu

Rieke

2022

Universe

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The active galactic nucleus (AGN) phenomenon results from a supermassive black hole accreting its surrounding gaseous and dusty material. The infrared (IR) regime provides most of the information to characterize the dusty structures that bridge from the galaxy to the black hole, providing clues to the black hole growth and host galaxy evolution. Over the past several decades, with the commissioning of various ground, airborne and space IR observing facilities, our interpretations of the AGN circumnuclear structures have advanced significantly through an improved understanding of how their dust emission changes as a function of wavelength and how the heating of the dusty structures responds to variations in the energy released from the central engine. In this review, we summarize the current observational knowledge of the AGN IR broad-band spectral energy distributions (SEDs) and the IR time variability behavior covering large ranges of AGN luminosity and redshift, and discuss some first-order insights into the obscuring structures and host galaxy IR properties that can be obtained by integrating the relevant observations into a coherent picture.

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Piercing through Highly Obscured and Compton-thick AGNs in the Chandra Deep Fields. II. Are Highly Obscured AGNs the Missing Link in the Merger-triggered AGN–Galaxy Coevolution Models?

Abstract: By using a large, highly obscured ( > -N 10 cm H 23

Cited by 13 publications

References 160 publications

Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties

Spectral Energy Distributions in Three Deep-drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time: Source Classification and Galaxy Properties

The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei

Infrared Spectral Energy Distribution and Variability of Active Galactic Nuclei: Clues to the Structure of Circumnuclear Material

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