Fast Outflows in Hot Dust-obscured Galaxies Detected with Keck/NIRES

Finnerty, Luke; Larson, Kirsten L.; Soifer, B. T.; Armus, L.; Matthews, K.; Jun, Hyunsung D.; Moon, D. S.; Melbourne, Jason; Gómez, Percy; Tsai, Chao-Wei; Díaz-Santos, T.; Eisenhardt, Peter; Cushing, Michael C.

doi:10.3847/1538-4357/abc3bf

Cited by 22 publications

(50 citation statements)

References 64 publications

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“…The known prodigious outflows support the hypothesis that ERQs are candidate young quasars, tied to an early, powerful stage of quasar-galaxy evolution, as have been inferred for the hot dustobscured galaxies (hot DOGs, Wu et al 2018;Noboriguchi et al 2019;Finnerty et al 2020). Observations of ERQ host galaxies and their extended environments are needed to test this hypothesis.…”

Section: Introductionsupporting

confidence: 54%

Probing the Inner Circumgalactic Medium and Quasar Illumination around the Reddest `Extremely Red Quasar' (ERQ)

Lau,

Hamann,

Gillette

et al. 2022

Preprint

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Dusty quasars might be in a young stage of galaxy evolution with prominent quasar feedback. We study a population of luminous, extremely red quasars at redshifts 𝑧 ∼ 2-4 that has a suite of extreme spectral properties that may all be related to exceptionally powerful quasar-driven outflows. We present Keck/KCWI observations of the reddest known ERQ, at 𝑧 = 2.3184, with an extremely fast [O ] 𝜆5007 outflow at ∼6000 km s −1 . The Ly𝛼 halo spans ∼100 kpc. The halo is kinematically quiet, with velocity dispersion ∼300 km s −1 and no broadening above the dark matter circular velocity down to the spatial resolution ∼6 kpc from the quasar. We detect spatially-resolved He 𝜆1640 and C 𝜆1549 emissions with kinematics similar to the Ly𝛼 halo and a narrow component in the [O ] 𝜆5007. Quasar reddening acts as a coronagraph allowing views of the innermost halo. A narrow Ly𝛼 spike in the quasar spectrum is inner halo emission, confirming the broad C 𝜆1549 in the unresolved quasar is blueshifted by 2242 km s −1 relative to the halo frame. We propose the inner halo is dominated by past/moderate-speed outflow and the outer halo dominated by inflow. The high central concentration of the surface brightness and the circularly symmetric morphology of the inner halo are consistent with the ERQ being young. The He 𝜆1640/Ly𝛼 ratio of the inner halo and the asymmetry level of the overall halo are dissimilar to Type II quasars, implying central ionizing photons can escape along the line of sight. While quasar dominates the ionization, we find no evidence of mechanical quasar feedback on circumgalactic scales.

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Section: Introductionsupporting

confidence: 54%

Probing the Inner Circumgalactic Medium and Quasar Illumination around the Reddest `Extremely Red Quasar' (ERQ)

Lau,

Hamann,

Gillette

et al. 2022

Preprint

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“…Feedback from luminous active galactic nuclei (AGN), also regularly labeled as "quasar feedback", is currently the preferred physical process with which theoretical models of galaxy evolution and cosmological simulations attempt to reproduce observations (Croton et al 2006;Anglés-Alcázar et al 2017a;cf., Muzzin et al 2012). Quasar-mode feedback, which manifests itself in the form of galactic gas outflows, has been identified in a large number of z 2 optically and infrared-selected quasars (OpQs and IRQs, respectively) via fast-moving (v out ≥ 1000 km s −1 ), ionized-gas ([O iii]λλ4959,5007 Å) winds (Zakamska et al 2016;LaMassa et al 2017;Bischetti et al 2017;Wu et al 2018;Perrotta et al 2019;Temple et al 2019;Jun et al 2020;Finnerty et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Kinematics and star formation of high-redshift hot dust-obscured quasars as seen by ALMA

Díaz-Santos

Assef

Eisenhardt

et al. 2021

A&A

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Hot, dust-obscured galaxies (Hot DOGs) are a population of hyper-luminous obscured quasars identified by WISE. We present ALMA observations of the [C II] 158 μm fine-structure line and underlying dust continuum emission in a sample of seven of the most extremely luminous (EL; Lbol ≥ 1014 L⊙) Hot DOGs, at redshifts of z ≃ 3.0−4.6. The [C II] line is robustly detected in four objects, tentatively in one, and likely to have been red-shifted out of the spectral window in the remaining two, based on additional data. On average, [C II] is red-shifted by ≃780 km s−1 from rest-frame ultraviolet emission lines. EL Hot DOGs consistently exhibit very high [C II] surface densities, with Σ[CII] ≃ 1−2 × 109 L⊙ kpc−2, which is as high as the most extreme cases seen in other high-redshift quasars. As a population, EL Hot DOG hosts seem to be roughly centered on the main sequence of star-forming galaxies, but the uncertainties are substantial and individual sources can fall above and below. The average, intrinsic [C II] and dust continuum sizes (FWHMs) are ≃2.1 kpc and ≃1.6 kpc, respectively, with a very narrow range of line-to-continuum size ratios, 1.61 ± 0.10, suggesting they could be linearly proportional. The [C II] velocity fields of EL Hot DOGs are diverse: from barely rotating structures, to resolved hosts with ordered, circular motions, to complex, disturbed systems that are likely the result of ongoing mergers. In contrast, all sources display large line-velocity dispersions, FWHM[CII] ≳ 500 km s−1, which are, on average, larger than optically and IR-selected quasars at similar or higher redshifts. We argue that one possible hypothesis that explains the lack of a common velocity structure, the systematically large dispersion of the ionized gas, and the presence of nearby companion galaxies, may be that the EL Hot DOG phase could be recurrent, rather than a single event. The dynamical friction from the frequent in-fall of neighbor galaxies and gas clumps, along with the subsequent quasar feedback, would contribute to the high turbulence of the gas within the host in a process that could potentially trigger not only one continuous EL, obscured event –but instead a number of recurrent, shorter-lived episodes as long as external accretion continues.

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“…Yan et al [330] confirm that these sources have huge gas columns (≥ 10 25 cm −2 ), consistent with their having very hard but faint X-ray outputs [313,338]. They are also the sites of large, high-velocity outflows [e.g., 69,89].…”

Section: Hot Dust-obscured Galaxiesmentioning

confidence: 81%

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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Fast Outflows in Hot Dust-obscured Galaxies Detected with Keck/NIRES

Cited by 22 publications

References 64 publications

Probing the Inner Circumgalactic Medium and Quasar Illumination around the Reddest `Extremely Red Quasar' (ERQ)

Probing the Inner Circumgalactic Medium and Quasar Illumination around the Reddest `Extremely Red Quasar' (ERQ)

Kinematics and star formation of high-redshift hot dust-obscured quasars as seen by ALMA

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

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