A model for the infrared emission of FSC 10214+4724

Efstathiou, A.

doi:10.1111/j.1745-3933.2006.00210.x

Cited by 37 publications

(49 citation statements)

References 58 publications

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“…The estimated SFRs are consistent with those estimated in other radio-quiet obscured QSOs at high-z (e.g. Ivison et al 1998;Efstathiou 2006;Stevens et al 2005;Polletta et al 2008;Sajina et al 2007b). …”

Section: Sed Modeling and Star Formation Ratesupporting

confidence: 87%

“…The number of well studied composite systems is still low, and it is often difficult to separate and quantify the contribution from different energy sources (see e.g. the variety of models proposed to explain the properties of F 10214+4724; Rowan-Robinson et al 1993;Teplitz et al 2006;Efstathiou 2006). In order to quantify their contribution to the bolometric luminosity, the multiwavelength spectral energy distributions (SEDs) of such systems need to be measured and modeled.…”

Section: Introductionmentioning

confidence: 99%

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Obscured and powerful AGN and starburst activities at z ~ 3.5

Polletta¹,

Omont²,

Berta³

et al. 2008

A&A

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Aims. Short phases of coeval powerful starburst and AGN activity during the lifetimes of the most massive galaxies are predicted by various models of galaxy formation and evolution. In spite of their recurrence and high luminosity, such events are rarely observed. Finding such systems, understanding their nature, and constraining their number density can provide key constraints to galaxy evolutionary models and insights into the interplay between starburst and AGN activities. Methods. We report the discovery of two sources at z = 3.867 and z = 3.427 that exhibit both powerful starburst and AGN activities. They benefit from multi-wavelength data from radio to X rays from the CFHTLS-D1/SWIRE/XMDS surveys. Follow-up optical and near-infrared spectroscopy, and millimeter IRAM/MAMBO observations are also available. We performed a multi-wavelength analysis of their spectral energy distributions with the aim of understanding the origin of their emission and constraining their luminosities. A comparison with other composite systems at similar redshifts from the literature is also presented. Results. The AGN and starburst bolometric luminosities are ∼1013 L . The AGN emission dominates at X ray, optical, mid-infrared wavelengths, and probably also in the radio. The starburst emission dominates in the far-infrared. The estimated star formation rates range from 500 to 3000 M /yr. The AGN near-infrared and X ray emissions are heavily obscured in both sources with an estimated dust extinction A V ≥ 4, and Compton-thick gas column densities. The two sources are the most obscured and most luminous AGNs detected at millimeter wavelengths currently known. Conclusions. The sources presented in this work are heavily obscured QSOs, but their properties are not fully explained by the standard AGN unification model. In one source, the ultraviolet and optical spectra suggest the presence of outflowing gas and shocks, and both sources show emission from hot dust, most likely in the vicinity of the nucleus. Evidence of moderate, AGN-driven radio activity is also found in both sources. Based on the estimated stellar and black hole masses, the two sources lie on the local M BH −M bulge relation. To remain on this relation as they evolve, their star formation rate has to decrease or stop. Our results support evolutionary models that invoke radio feedback such as the star formation quenching mechanism, and suggest that such a mechanism might play a major role also in powerful AGNs.

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Section: Sed Modeling and Star Formation Ratesupporting

confidence: 87%

Section: Introductionmentioning

confidence: 99%

Obscured and powerful AGN and starburst activities at z ~ 3.5

Polletta¹,

Omont²,

Berta³

et al. 2008

A&A

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“…The torus geometry assumed in the Efstathiou & RowanRobinson (1995) models means that the mid-IR emission is anisotropic, with viewing angles closer to edge-on tending to suppress the mid-IR emission (Efstathiou 2006;Efstathiou et al 2014). The derived combination of torus geometry and viewing angle of IRAS 09104+4109 thus impliesa (multiplicative) anisotropy correction to the AGN luminosity of ) IR spectral energy distribution for IRAS 09104 +4109.…”

Section: Infrared and Optical Analysismentioning

confidence: 95%

The Geometry of the Infrared and X-Ray Obscurer in a Dusty Hyperluminous Quasar

Farrah

Baloković

Stern

et al. 2016

ApJ

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We study the geometry of the active galactic nucleus (AGN) obscurer in IRAS 09104+4109, an IR-luminous, radio-intermediate FR-I source at z = 0.442, using infrared data from Spitzer and Herschel, X-ray data from NuSTAR, Swift, Suzaku, and Chandra, and an optical spectrum from Palomar. The infrared data imply a total restframe 1-1000 μm luminosity of 5.5×10 46 erg s −1 and require both an AGN torus and a starburst model. The AGN torus has an anisotropy-corrected IR luminosity of 4.9×10 46 erg s −1 and a viewing angle and half-opening angle both of approximately 36°from pole-on. The starburst has a star formation rate of (110±34) M e yr −1 and an age of <50 Myr. These results are consistent with two epochs of luminous activity in IRAS 09104+4109: one approximately 150 Myr ago, and one ongoing. The X-ray data suggest a photon index of Γ ; 1.8 and a line-ofsight column density of N H ; 5×10 23 cm −2 . This argues against a reflection-dominated hard X-ray spectrum, which would have implied a much higher N H and luminosity. The X-ray and infrared data are consistent with a bolometric AGN luminosity of L bol ∼(0.5-2.5)×10 47 erg s −1. The X-ray and infrared data are further consistent with coaligned AGN obscurers in which the line of sight "skims" the torus. This is also consistent with the optical spectra, which show both coronal iron lines and broad lines in polarized but not direct light. Combining constraints from the X-ray, optical, and infrared data suggestthat the AGN obscurer is within a vertical height of 20 pc, and a radius of 125 pc, of the nucleus.

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“…It is generally accepted that the enormous luminosity of this galaxy at redshift z = 2.224 is due to gravitational lensing by a foreground galaxy with magnification between 50 and 100 (Broadhurst & Lehar 1995;Serjeant et al 1995) or 15−20 (Deane et al 2013). Following the detection of a silicate emission feature (Teplitz et al 2006) in this narrow-lined object, Efstathiou (2006) and Efstathiou et al (2013) proposed that the emission feature is due to emission from narrow-line region clouds at a temperature of 210 K.…”

Section: Fit To the Hyperluminous Ir Galaxy Iras F10214+4724mentioning

confidence: 98%

Self-consistent two-phase AGN torus models

Siebenmorgen

Heymann

Efstathiou

2015

A&A

131

189

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We assume that dust near active galactic nuclei (AGNs) is distributed in a torus-like geometry, which can be described as a clumpy medium or a homogeneous disk, or as a combination of the two (i.e. a two-phase medium). The dust particles considered are fluffy and have higher submillimeter emissivities than grains in the diffuse interstellar medium. The dust-photon interaction is treated in a fully self-consistent three-dimensional radiative transfer code. We provide an AGN library of spectral energy distributions (SEDs). Its purpose is to quickly obtain estimates of the basic parameters of the AGNs, such as the intrinsic luminosity of the central source, the viewing angle, the inner radius, the volume filling factor and optical depth of the clouds, and the optical depth of the disk midplane, and to predict the flux at yet unobserved wavelengths. The procedure is simple and consists of finding an element in the library that matches the observations. We discuss the general properties of the models and in particular the 10 µm silicate band. The AGN library accounts well for the observed scatter of the feature strengths and wavelengths of the peak emission. AGN extinction curves are discussed and we find that there is no direct one-to-one link between the observed extinction and the wavelength dependence of the dust cross sections. We show that objects in the library cover the observed range of mid-infrared colors of known AGNs. The validity of the approach is demonstrated by matching the SEDs of a number of representative objects: Four Seyferts and two quasars for which we present new Herschel photometry, two radio galaxies, and one hyperluminous infrared galaxy. Strikingly, for the five luminous objects we find that pure AGN models fit the SED without needing to postulate starburst activity.

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A model for the infrared emission of FSC 10214+4724

Cited by 37 publications

References 58 publications

Obscured and powerful AGN and starburst activities at z ~ 3.5

Obscured and powerful AGN and starburst activities at z ~ 3.5

The Geometry of the Infrared and X-Ray Obscurer in a Dusty Hyperluminous Quasar

Self-consistent two-phase AGN torus models

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