Dust Emission from Active Galactic Nuclei

Nenkova, Maia; Ivezić, Željko; Elitzur, Moshe

doi:10.1086/340857

Cited by 491 publications

(672 citation statements)

References 19 publications

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“…When discussing these models, it's important to keep in mind that the accuracy or applicability of these models cannot be tested with data since it simply does not exist in enough detail to disentangle effects of geometry, distribution, optical depth, etc. It's also important to note that many have done work in this area, particularly modeling radiative transfer in local starburst populations to generate SEDs (Efstathiou & Rowan-Robinson, 1995;Efstathiou et al, 2000;Efstathiou & Siebenmorgen, 2009;Nenkova et al, 2002;Dullemond & van Bemmel, 2005;Piovan et al, 2006;Nenkova et al, 2008;Takagi et al, 2003;Fritz et al, 2006;Hönig et al, 2006;Schartmann et al, 2008), but here we try to focus on the techniques which have been most commonly employed for SED fitting of high-z dusty starbursts 11 . Silva et al (1998) developed the Grasil code to model galaxy emission by explicitly accounting for dust absorption and emission from the ultraviolet through to the far-infrared.…”

Section: Employing Dust Radiative Transfer Models and Empirical Templmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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Section: Employing Dust Radiative Transfer Models and Empirical Templmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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“…A power-law extension of the restframe optical disk emission into the NIR is a common assumption for the primary source that is used as input for radiative transfer codes that model the torus emission (e.g. Granato & Danese 1994;Nenkova et al 2002;Fritz et al 2006;Stalevski et al 2012), but it is not universal. In particular, some torus models assume a steep fall of the disk spectrum longwards of 1 µm (e.g.…”

Section: Modelling Of the Continuum Emissionmentioning

confidence: 99%

The near-to-mid infrared spectrum of quasars

Hernán-Caballero

Hatziminaoglou

Alonso‐Herrero

et al. 2016

Mon. Not. R. Astron. Soc.

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We analyse a sample of 85 luminous (log(νL ν (3µm)/erg s −1 )>45.5) quasars with restframe ∼2-11 µm spectroscopy from AKARI and Spitzer. Their high luminosity allows a direct determination of the near-infrared quasar spectrum free from host galaxy emission. A semiempirical model consisting of a single template for the accretion disk and two blackbodies for the dust emission successfully reproduces the 0.1-10 µm spectral energy distributions (SEDs). Excess emission at 1-2 µm over the best-fitting model suggests that hotter dust is necessary in addition to the ∼1200 K blackbody and the disk to reproduce the entire near-infrared spectrum. Variation in the extinction affecting the disk and in the relative strength of the disk and dust components accounts for the diversity of individual SEDs. Quasars with higher dust-to-disk luminosity ratios show slightly redder infrared continua and less prominent silicate emission. We find no luminosity dependence in the shape of the average infrared quasar spectrum. We generate a new quasar template that covers the restframe range 0.1-11 µm, and separate templates for the disk and dust components. Comparison with other infrared quasar composites suggests that previous ones are less reliable in the 2-4 µm range. Our template is the first one to provide a detailed view of the infrared emission on both sides of the 4 µm bump.

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“…All these models consider radiative transfer in an anisotropic, but homogenous dusty torus. Nenkova et al (2002) considered radiative transfer between several clouds of dust along radial rays through the torus, and overcame some difficulties of the former homogeneous models for the description of the spectral energy distributions. More recently, Schartmann et al (2005) described the three dimensional treatment of radiative transfer through dusty tori at hydrostatic equilibrium and succeed in reproducing both the mean large aperture spectra from UV to far-IR of several Seyfert type 1 galaxies, and the recent MIDI observations of two specified Seyfert type 2: Circinus and NGC 1068, except for the 9.7 µm silicate feature.…”

Section: Introductionmentioning

confidence: 99%

A new analysis of the nucleus of NGC 1068 with MIDI observations

Poncelet

Perrin²,

Sol³

2006

A&A

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We present a new analysis of the first mid-infrared N-band long-baseline interferometric observations of an extragalactic source: the nucleus of the Seyfert 2 galaxy NGC 1068, obtained with MIDI (Mid-InfrareD Interferometer), the mid-infrared beamcombiner at the European Southern Observatory (ESO) Very Large Telescope Interferometer (VLTI). The resolution of λ/B ∼ 10 mas allows us to study the compact central core of the galaxy between 8 and 13 µm. Both visibility measurements and MIDI spectrum are well reproduced by a simple radiative transfer model with two concentric spherical components. The derived angular sizes and temperatures are ∼35 and 83 mas, and ∼361 K and 226 K for these two components respectively. Other evidence strongly supports such low temperatures. This modeling also provides the variation of optical depth as a function of wavelength for the extended component across the N-band suggesting the presence of amorphous silicate grains. This shows that MIDI has carried out the first direct observations of the distribution of dust around the central engine.

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Dust Emission from Active Galactic Nuclei

Cited by 491 publications

References 19 publications

Dusty star-forming galaxies at high redshift

Dusty star-forming galaxies at high redshift

The near-to-mid infrared spectrum of quasars

A new analysis of the nucleus of NGC 1068 with MIDI observations

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