The Overdense Environments of WISE-Selected, Ultra-Luminous, High-Redshift AGN in the Submillimeter

Jones, Sarah

doi:10.3389/fspas.2017.00051

Cited by 2 publications

(2 citation statements)

References 89 publications

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“…Studies have increasingly shown that Hot DOGs reside in overdense environments, characterized by a high frequency of galactic mergers (Jones et al 2014;Jones 2017;Assef et al 2015;Díaz-Santos et al 2018;Penney et al 2019;Luo et al 2022;Ginolfi et al 2022;Zewdie et al 2023). Despite hosting powerful AGNs, the host galaxies of high-z Hot DOGs are gasrich (Penney et al 2020;Díaz-Santos et al 2021;L.…”

Section: Optical Emissionmentioning

confidence: 99%

“…By imaging the [C II] emission in extremely luminous DOGs (L bol > 10 14 e ) ALMA, however, Díaz-Santos et al (2021) proposed instead that this short-lived phase may be triggered by a minor merger and might occur recurrently throughout the history of the galaxy. This is particularly plausible if Hot DOGs become the brightest galaxies in clusters once the overdensities they live in (Jones et al 2014;Jones 2017;Assef et al 2015;Luo et al 2022;Ginolfi et al 2022;Zewdie et al 2023) become virialized.…”

Section: Optical Emissionmentioning

confidence: 99%

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Black Hole Mass and Eddington Ratio Distribution of Hot Dust-obscured Galaxies

Li,

Assef,

Tsai

et al. 2024

ApJ

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Hot dust-obscured galaxies (Hot DOGs) are a rare population of hyperluminous infrared galaxies discovered by the Wide-field Infrared Survey Explorer mission. Despite the significant obscuration of the active galactic nucleus (AGN) by dust in these systems, pronounced broad and blueshifted emission lines are often observed. Previous work has shown that eight Hot DOGs, referred to as blue-excess Hot DOGs (BHDs), present a blue excess consistent with type 1 quasar emission in their UV–optical spectral energy distributions (SEDs), which has been shown to originate from the light of the obscured central engine scattered into the line of sight. We present an analysis of the rest-frame optical emission characteristics for 172 Hot DOGs through UV–mid-IR SED modeling and spectroscopic details, with a particular focus on the identification of BHDs. We find that while the optical emission observed in Hot DOGs is in most cases dominated by a young stellar population, 26% of Hot DOGs show a significant enough blue excess emission to be classified as BHDs. Based on their broad C iv and Mg ii lines, we find that the mass of the black hole M BH in a BHD ranges from 108.7 to 1010 M ⊙. When using the same emission lines in regular Hot DOGs, we find the M BH estimates cover the entire range found for BHDs while also extending to somewhat lower values. This agreement may imply that the broad lines in regular Hot DOGs also originate from scattered light from the central engine, just as in BHDs, although a more detailed study would be needed to rule out an outflow-driven nature. Similar to z ∼ 6 quasars, we find that Hot DOGs sit above the local relation between stellar and black hole masses, suggesting either that AGN feedback has not yet significantly suppressed the stellar mass growth in the host galaxies or that they will be outliers of the relation when reaching z = 0.

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Section: Optical Emissionmentioning

confidence: 99%

Section: Optical Emissionmentioning

confidence: 99%

Black Hole Mass and Eddington Ratio Distribution of Hot Dust-obscured Galaxies

Li,

Assef,

Tsai

et al. 2024

ApJ

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The AGN fraction in high-redshift protocluster candidates selected by Planck and Herschel

Gatica,

Demarco,

Dole

et al. 2023

Monthly Notices of the Royal Astronomical Society

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A complete understanding of the mass assembly history of structures in the Universe requires the study of the growth of galaxies and their supermassive black holes (SMBHs) as a function of their local environment over cosmic time. In this context, it is important to quantify the effects that the early stages of galaxy cluster development have on the growth of SMBHs. We used a sample of Herschel/SPIRE sources of ∼ 228 red and compact Planck-selected protocluster (PC) candidates to estimate the active galactic nuclei (AGNs) fraction from a large sample of galaxies within these candidates. We estimate the AGN fraction by using the mid-infrared (mid-IR) photometry provided by the WISE/AllWISE data of ∼650 counterparts at high redshifts. We created an AllWISE mid-IR colour–colour selection using a clustering machine learning algorithm and two WISE colour cuts using the 3.4 $\mu$m (W1), 4.6 $\mu$m (W2), and 12 $\mu$m (W3) passbands, to classify sources as AGN. We also compare the AGN fraction in PCs with that in the field to better understand the influence of the environment on galaxy development. We found an AGN fraction of fAGN = 0.113 ± 0.03 in PC candidates and an AGN fraction of fAGN = 0.095 ± 0.013 in the field. We also selected a subsample of ‘red’ SPIRE subsample with a higher overdensity significance, obtaining fAGN = 0.186 ± 0.044, versus fAGN = 0.037 ± 0.010 of ‘non-red sources’, consistent with higher AGN fractions for denser environments. We conclude that our results point towards a higher AGN fraction in PCs, similar to other studies.

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The Overdense Environments of WISE-Selected, Ultra-Luminous, High-Redshift AGN in the Submillimeter

Cited by 2 publications

References 89 publications

Black Hole Mass and Eddington Ratio Distribution of Hot Dust-obscured Galaxies

Black Hole Mass and Eddington Ratio Distribution of Hot Dust-obscured Galaxies

The AGN fraction in high-redshift protocluster candidates selected by Planck and Herschel

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