AGN Dusty Tori. II. Observational Implications of Clumpiness

By M. Nenkova, M. Sirocky, R. Nikutta, Željko Ivezic´, M. Elitzur. 2008

625 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/fb1b78c3ba5395be253321bea21e11d19e9a93d3

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Citations in the corpus

The origin of the broad line region in active galactic nuclei (2010, methodology): “The distance is smaller than the distance to the dusty torus Rdust ∼ 0.4L 1/2 45 pc (Nenkova et al. 2008; where L45 stands for the bolometric luminosity in 1045 erg s−1) since in our case the temperature results only from the local disk dissipation instead of the irradiation by the central parts of…”
TESTING THE UNIFICATION MODEL FOR ACTIVE GALACTIC NUCLEI IN THE INFRARED: ARE THE OBSCURING TORI OF TYPE 1 AND 2 SEYFERTS DIFFERENT? (2011, methodology): “The latter can be represented in terms of the escape probability Pesc (see equation 4 in Nenkova et al. 2008a).”
Cosmic X-ray surveys of distant active galaxies (2015, background): “AGNs of higher luminosities may be able to evacuate or destroy, via radiative feedback, circumnuclear gas and dust more effectively, leading to a so-called “receding torus” with larger opening angle (e.g., Menci et al 2008; Nenkova et al 2008).”
Revisiting the Unified Model of Active Galactic Nuclei (2015, methodology): “This approach was later used by Mor & Netzer (2012) who combined the Nenkova et al. (2008b) clumpy torus model with two additional components, one containing pure graphite grains and the other a dusty NLR.”
OUTFLOWS FROM ACTIVE GALACTIC NUCLEI: KINEMATICS OF THE NARROW-LINE AND CORONAL-LINE REGIONS IN SEYFERT GALAXIES, (2011, methodology): “The clumpy distribution is also supported by theoretical models (Schartmann et al. 2005; Elitzur & Shlossman 2006; Nenkova et al. 2008) and observations of thermal dust emission (e.g., Jaffe et al. 2004), silicate absorption (e.g., Deo et al. 2007), and molecular gas (MS06; H09).”
OBSCURATION-DEPENDENT EVOLUTION OF ACTIVE GALACTIC NUCLEI (2015, background): “In the context of clumpy torus models (Hönig & Beckert 2007; Nenkova et al. 2008), a more intense radiation field leads to the (partial) ionisation of individual dust and gas clouds thereby increasing the effective solid angle of unobscured sight-lines.”
The incidence of obscuration in active galactic nuclei (2013, methodology): “…explored models for the BLR and/or for the obscuring torus which naturally account for their disappearance at lower luminosities (Nicastro 2000; Nenkova et al. 2008; Elitzur & Ho 2009), even if in most models this effect sets in at much lower luminosities and/or Eddington ratios than those…”
Evolution of broad-line emission from active galactic nuclei (2013, background): “Accounting for the change in composition across the dust sublimation radius Rd ' 0.4L1/245 pc, (1) where L45 = Lbol/1045 erg s−1 (Nenkova et al. 2008), the BLR and torus were unified in a single outflow: At radii beyond Rd the clouds are dusty and comprise the AGN obscuring torus, while the wind…”
Discovery of extreme [O III] λ5007 Å outflows in high-redshift red quasars (2015, background): “…2006; Hönig et al. 2006; Schartmann et al. 2008) and in SEDs of type 2 quasars which are notably redder than type 1 SEDs even in the mid-infrared (Liu et al. 2013b), though anisotropy of infrared emission can be strongly suppressed if the obscuring material is clumpy (Nenkova et al. 2008).”
THE SPACE DENSITY OF COMPTON-THICK ACTIVE GALACTIC NUCLEUS AND THE X-RAY BACKGROUND (2009, background): “This lack of CT AGN can be interpreted either in the context of a clumpy torus (e.g., Krolik & Begelman 1988; Nenkova et al. 2008a) or a smooth distribution (e.g., Pier & Krolik 1992).”
First X-ray-based statistical tests for clumpy-torus models: eclipse events from 230 years of monitoring of Seyfert AGN (2014, methodology): “For instance, if N0 is between 5 and 15 (see, e.g., Nenkova et al. 2008b), it is clear from Fig.”
THE QUASAR OUTFLOW CONTRIBUTION TO AGN FEEDBACK: VLT MEASUREMENTS OF SDSS J0318-0600 (2009, background): “See Pier & Voit (1995); Nenkova et al. (2008) for a more extensive discussion of the properties of illuminated dusty tori associated with AGNs.”
A systematic search for changing-look quasars in SDSS (2015, background): “Another possibility is that the entire UV/continuum emitting region and BLR is obscured; this might be expected if the distribution of dust lying at the outskirts of the BLR is patchy (e.g., Nenkova et al. 2008a,b; Elitzur 2012).”
THREE-YEAR SWIFT–BAT SURVEY OF ACTIVE GALACTIC NUCLEI: RECONCILING THEORY AND OBSERVATIONS? (2010, background): “Recently (see Hönig & Beckert 2007; Nenkova et al. 2008) F% was interpreted in the framework of a radiation-limited clumpy dust torus in which F% ∝ L−0.25, which is much closer to our findings.”
Active galactic nuclei: what’s in a name? (2017, methodology): “…and van Bemmel 2005; Fritz et al. 2006), whether it is clumpy in the form of optically and geometrically thick clouds (Krolik and Begelman 1988; Nenkova et al. 2002, 2008; Elitzur and Shlosman 2006; Tristram et al. 2007), or a combination of the two (Stalevski et al. 2012; Assef et al. 2013).”
Three-dimensional radiative transfer modeling of AGN dusty tori as a clumpy two-phase medium (2011, methodology): “According to the unification model, the different appearance of type 1 and type 2 active galactic nuclei (AGN) is only a matter of orientation (Antonucci 1993; Urry & Padovani 1995).”
Stellar Population Inference with Prospector (2020, methodology): “Circumstellar dust around AGB stars is implemented via the Villaume et al. (2015) templates, while dust associated with AGN is modeled using a simplified implementation of the Nenkova et al. (2008b) templates.”
Discovery of 21 New Changing-look AGNs in the Northern Sky (2017, background): “…] 4 J un 2 01 8 2 movement of obscuring material, in a scenario that the dusty toroidal structure obscuring the BLR has a patchy distribution (e.g., Nenkova et al. 2008a,b; Elitzur 2012) or an accelerating outflow (e.g., Shapovalova et al. 2010); (2) variable accretion rate, in an evolutionary…”