The AGN-obscuring Torus: The End of the “Doughnut” Paradigm?

2006

301 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/2b66c740dfaadc298bc851e10a1c9a4c3e95af7d

Citations in the corpus

What drives the growth of black holes (2011, unknown): “However, these results are consistent with clumpy torus models (e.g., Nenkova et al., 2002; Elitzur & Shlosman, 2006; Nenkova et al., 2008; Schartmann et al., 2008; Hönig et al., 2006; Hönig & Kishimoto, 2010), which predict no inclination-angle dependence on the strength of the mid-IR emission…”
MID-INFRARED SELECTION OF ACTIVE GALACTIC NUCLEI WITH THE WIDE-FIELD INFRARED SURVEY EXPLORER. II. PROPERTIES OF WISE-SELECTED ACTIVE GALACTIC NUCLEI IN THE NDWFS BOÖTES FIELD (2012, unknown): “For example, several authors (e.g., Krolik & Begelman 1988; Nenkova et al. 2002, 2008; Elitzur & Shlosman 2006; Tristram et al. 2007) have argued that the dust in the torus must be in optically and geometrically thick clumps to reproduce observations, while others (e.g., Dullemond & van Bemmel…”
TESTING THE UNIFICATION MODEL FOR ACTIVE GALACTIC NUCLEI IN THE INFRARED: ARE THE OBSCURING TORI OF TYPE 1 AND 2 SEYFERTS DIFFERENT? (2011, unknown): “The first results of radiative transfer calculations of a clumpy rather than a smooth medium were reported by Nenkova et al. (2002) and Elitzur & Shlosman (2006), and further work was done by Dullemond & van Bemmel (2005).”
AGN Dusty Tori. II. Observational Implications of Clumpiness (2008, unknown): “If the black hole mass is M 7 ; 107 M then it dominates the gravitational motions within a radius 35(M 7/ 2)1/3 pc, where , typically of order unity, is the rotation velocity (in km s 1 pc 1) induced by the galactic bulge in its interior (Elitzur & Shlosman 2006).”
First X-ray-based statistical tests for clumpy-torus models: eclipse events from 230 years of monitoring of Seyfert AGN (2014, unknown): “Clouds are possibly supported vertically by, e.g., radiation pressure (Krolik 2007) or disk winds (Elitzur & Shlosman 2006).”
OBSCURATION-DEPENDENT EVOLUTION OF ACTIVE GALACTIC NUCLEI (2015, unknown): “However, under this model, the critical luminosity below which the obscurer can not be sustained is strictly 18 Buchner et al. determined by the black hole mass (Elitzur & Shlosman 2006; Elitzur 2008).”
ON THE DISAPPEARANCE OF THE BROAD-LINE REGION IN LOW-LUMINOSITY ACTIVE GALACTIC NUCLEI (2009, unknown): “The derivation of the BLR / TOR disappearance presented here is more general than the original one in Elitzur & Shlosman (2006).”
Nuclear Activity in Nearby Galaxies (2008, unknown): “For example, the clumpy torus model of Elitzur & Shlosman (2006) predicts that the BLR can no longer be sustained for Lbol ∼ 10 42 ergs s−1.”
High-Resolution Mid-Infrared Spectroscopy of Ultraluminous Infrared Galaxies (2007, unknown): “…a strong dependence of observed properties on viewing angle, as nearly all lines of evidence suggest that the dust in AGNs is arranged in a planar structure, whether that structure is a torus (Schartmann et al. 2005), a flared disk (Fritz et al. 2006), or discrete clouds (Elitzur & Shlosman 2006).”
Cosmic X-ray surveys of distant active galaxies (2015, unknown): “In recent years, for example, it has become possible to obtain direct estimates of the (luminosity dependent) extent of the torus (e.g., Burtscher et al 2013; Koshida et al 2014) and to ascertain its apparently clumpy nature (e.g., Elitzur and Shlosman 2006; Mor et al 2009).”
A diversity of dusty AGN tori - Data release for the VLTI/MIDI AGN Large Program and first results for 23 galaxies (2013, unknown): “Current dynamical models of the torus see it either made up from outflowing (e.g. Elitzur & Shlosman, 2006; Czerny & Hryniewicz, 2011; Gallagher et al., 2013) material that is part of a wind blown off from the accretion disk or as an inflowing structure whose scale-height may be provided by…”
Evolution of broad-line emission from active galactic nuclei (2013, unknown): “…of the wind launch velocity is comparable to the local turbulence velocity in the disc, which is roughly 10 per cent of the local Keplerian velocity (Elitzur & Shlosman 2006); that is, vw vK close to the disc (in the Blandford & Payne solution, the launch velocity of the cold wind is taken as 0).”
The WISE AGN Catalog (2017, unknown): “…geometrically and optically thick clouds, toroidally distributed around the central engine (e.g., Krolik & Begelman 1988; Nenkova et al. 2002, 2008; Elitzur & Shlosman 2006; Tristram et al. 2007), although a number of uncertainties remain about the exact properties and distribution of the dust…”
Revisiting the Unified Model of Active Galactic Nuclei (2015, unknown): “Several of its aspects were described in Laor (2003), Elitzur & Shlosman (2006) and Elitzur & Ho (2009).”