Disentangling the AGN and star-formation contributions to the radio-X-ray emission of radio-loud quasars at $1

Azadi, Mojegan; Wilkes, B. J.; Kuraszkiewicz, Joanna; McDowell, Jonathan; Siebenmorgen, R.; Birkinshaw, Mark; Worrall, D. M.; Abrams, Natasha S.; Barthel, P. D.; Fazio, G. G.; Haas, Martín; Hyman, Sóley; Martínez-Galarza, Rafael; Meyer, Eileen T.

doi:10.48550/arxiv.2011.03130

Cited by 3 publications

(28 citation statements)

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“…This study uses the 20 broad-line radio galaxies (i.e., quasars) from this sample. Azadi et al (2020) compiled radio to X-ray SEDs of the 20 3CRR 1 < z 2 quasars by combining new and archival photometry from multi-frequency radio observation, the SMA, ALMA, Herschel, WISE, Spitzer, 2MASS, UKIRT, SDSS, XMM-Newton, and Chandra. The resulting complete, randomly oriented sample has comprehensive multi-wavelength data from radio to X-ray bands, which we employ in the present work.…”

Section: Radio-loud Sample and Datamentioning

confidence: 99%

“…Recently, Azadi et al (2020) introduced a stateof-the-art AGN radio to X-ray SED fitting model (ARXSED) and characterized the SEDs of 20 radioloud quasars from the Revised-Third Cambridge Catalogue of Radio Galaxies (3CRR; Laing et al 1983) at 1 < z 2 . ARXSED significantly improves on other SED models (e.g., Elvis et al 1994;Richards et al 2006;Shang et al 2011;Podigachoski et al 2015) by including 1) a broader range of photometry spanning radio to X-ray wavelengths, 2) improved AGN component models for the emission from the accretion disk (Kubota & Done 2018) and torus (Siebenmorgen et al 2015), 3) a radio component to account for emission from complex radio structures (lobes, jets, cores, and hot spots) and reproduce a high-energy turnover or cutoff due to the aging of the electron populations, 4) a host galaxy component that replicates galaxy emission from radio to UV wavelengths (da Cunha et al 2008(da Cunha et al , 2015, and 5) estimates for the intrinsic AGN SED obtained by correcting the photometry for reddening and absorption occurring in the torus, the host galaxy, and the Milky Way.…”

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

“…In this contribution we use the SED modeling approach of Azadi et al (2020) and present the bolometric luminosity correction of both non-rotating and maximally-rotating AGN. We first use the Azadi et al (2020) SED fits (ARXSED) to individual radio-loud quasars (20 quasars) from the 3CRR sample at 1 < z 2 to determine their bolometric luminosities and correction factors. ARXSED allows us to overcome the gaps in the photometry, the viewing angle correction, including/excluding MIR data, and thereby accurately estimate the bolometric correction factors.…”

Section: Introductionmentioning

confidence: 99%

“…ARXSED allows us to overcome the gaps in the photometry, the viewing angle correction, including/excluding MIR data, and thereby accurately estimate the bolometric correction factors. We then expand our analysis to more general samples, building upon the Azadi et al (2020) approach. We create ∼11000 artifi-cial accretion disk templates utilizing QSOSED model of Kubota & Done (2018) by varying BH mass (from 10 7 to 10 10 M ⊙ ), Eddington ratio (from 0.03 to 1.0 in dex) and spin (from 0 to 1) within the acceptable range by the model.…”

Section: Introductionmentioning

confidence: 99%

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The Bolometric Luminosity Correction of Radio-Quiet and Radio-Loud Quasars at 1

Azadi¹,

Wilkes²,

Kuraszkiewicz³

et al. 2022

Preprint

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To understand the impact of active galactic nuclei (AGN) on their host galaxies and large scale environment it is crucial to determine their total radiative power across all wavelengths (i.e., bolometric luminosity). In this contribution we describe how quasar accretion disk spectral energy distribution (SED) templates, parameterized by the black hole (BH) mass, Eddington ratio, and spin can be used to estimate their total radiated luminosity. To estimate the bolometric luminosity of AGN, we integrate the accretion disk SEDs from 1 µm to 10 keV. Our approach self-consistently covers any gaps in observations and does not include reprocessed emission from the torus. The accretion disk SED, and consequently the bolometric correction inferred from it, strongly depend on the BH mass, the Eddington ratio, and spin. In particular, the bolometric correction in the visible bands (5000 Å and 3000 Å) strongly depends on BH mass, and at X-ray strongly depends on the Eddington ratio. At wavelengths closer to the peak of the accretion disk SED the dependence becomes weaker. Additionally, maximally-rotating (spin = 1) quasars require a higher bolometric correction than their non-rotating (spin = 0) counterparts at all wavelengths. The SEDs and the bolometric correction presented in this work can determine the radiative power of any sample of radio-quiet to radio-loud Type 1 AGN with observations in the range from 1 µm to 10 keV provided the observations are corrected for extinction.

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Section: Radio-loud Sample and Datamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

The Bolometric Luminosity Correction of Radio-Quiet and Radio-Loud Quasars at 1

Azadi¹,

Wilkes²,

Kuraszkiewicz³

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

show abstract

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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AGN Selection and Demographics in GOODS-S/HUDF from X-Ray to Radio

Lyu

Alberts

Rieke

et al. 2022

ApJ

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We present a comprehensive census of the active galactic nuclei (AGNs) in the GOODS-S/HUDF region from the X-ray to the radio, covering both the obscured and unobscured populations. This work includes a robust analysis of the source optical to mid-IR spectral energy distributions (SEDs) featuring (semi)empirical AGN and galaxy dust emission models and Bayesian fitting techniques, ultra-deep Very Large Array 3 and 6 GHz observations, and an integrated analysis of various AGN selection techniques, including X-ray properties, UV to mid-IR SED analysis, optical spectral features, mid-IR colors, radio-loudness and spectral slope, and AGN variability. In total, we report ∼900 AGNs over the ∼170 arcmin2 3D-HST GOODS-S footprint, which has doubled the AGN number identified in the previous X-ray sample, with ∼26% of our sample undetected in the deepest Chandra image. With a summary of AGN demographics from different selection methods, we find that no one single band or technique comes close to selecting a complete AGN sample despite the great depth of the data in GOODS-S/HUDF. We estimate the yields of various approaches and explore the reasons for incompleteness. We characterize the statistical properties, such as source number density, obscuration fraction, and luminosity function of the AGN sample in this field, and discuss their immediate implications. We also provide some qualitative predictions of the AGN sample that might be discovered by the upcoming JWST surveys.

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Disentangling the AGN and star-formation contributions to the radio-X-ray emission of radio-loud quasars at $1

Cited by 3 publications

References 0 publications

The Bolometric Luminosity Correction of Radio-Quiet and Radio-Loud Quasars at 1

The Bolometric Luminosity Correction of Radio-Quiet and Radio-Loud Quasars at 1

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

AGN Selection and Demographics in GOODS-S/HUDF from X-Ray to Radio

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