Dust covering factor, silicate emission, and star formation in luminous QSOs

By R. Maiolino, O. Shemmer, M. Imanishi, H. Netzer, E. Oliva, D. Lutz, E. Sturm. 2007

208 citations recorded by the source corpus.

This article presents Spitzer IRS low resolution, mid-IR spectra of a sample of 25 high luminosity QSOs at 2 < z < 3.5.

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In Astronomy and Astrophysics

Citations in the corpus

Hot graphite dust and the infrared spectral energy distribution of active galactic nuclei (2011, result): “Several earlier studies suggested a similar trend (e.g., Wang et al. 2005; Maiolino et al. 2007; Treister et al. 2008), however these were based on the total MIR emission which translates to the covering factor of the entir dusty structure, and not just the hot dust.”
Spitzer Quasar and ULIRG Evolution Study (QUEST). II. The Spectral Energy Distributions of Palomar-Green Quasars (2007, background): “This is now confirmed by the recent work of Maiolino et al. (2007) who studied much higher luminosity QSOs.”
The dust covering factor in active galactic nuclei (2016, methodology): “We recover similar values as Maiolino et al. (2007) and Lusso et al. (2013) around LAGN ≈ 1045 erg/s, and have significant deviations at low and high LAGN ends.”
CAIXA: a catalogue of AGN in the XMM-Newton archive - II. Multiwavelength correlations (2009, background): “…with the recent discovery of a non-linear relation between thermal emission from dust and optical luminosity in AGN, which implies a decrease of the covering factor of dust with luminosity, with a slope of −0.18 (Maiolino et al. 2007), i.e. very close to the one which characterises the IT effect.”
AGN Dusty Tori. I. Handling of Clumpy Media (2008, background): “(9) In a recent study Maiolino et al. (2007) defined the “dust covering factor” as the ratio of thermal infrared emission to the primary AGN radiation.”
Enhanced star formation rates in AGN hosts with respect to inactive galaxies from PEP-Herschel observations (2012, background): “(5) of Maiolino et al. (2007) and adopting a ratio of 7 between bolometric and 5100 Å luminosity. trol sample.”
Star Formation in the Hosts of High-z QSOs: Evidence from Spitzer PAH Detections (2008, background): “The effect becomes clear by inclusion of the PAH upper limit which has been derived for the sample of Maiolino et al. (2007) that is not selected to be mm-bright (Fig.”
IDENTIFYING LUMINOUS ACTIVE GALACTIC NUCLEI IN DEEP SURVEYS: REVISED IRAC SELECTION CRITERIA (2012, background): “X-ray/MIR Relation The observed X-ray to MIR luminosity ratio, a proxy for AGN obscuration, allows us to place an independent constraint on the column densities of the α ≤ −1.0 power-law sources (Lutz et al. 2004; Maiolino et al. 2007; Gandhi et al. 2009; Park et al. 2010).”
The mean star formation rate of X-ray selected active galaxies and its evolution from z~2.5: results from PEP-Herschel (2012, background): “5 from Maiolino et al. (2007) and taking a ratio of 7 between the luminosity at 5100Å andLAGN (Netzer & Trakhtenbrot 2007). logLAGN = (logLX − 11.78) 0.721 + 0.845 (1) whereLX (the 2-10 keV band X-ray luminosity) andLAGN are in erg s−1.”
AGN Dusty Tori. II. Observational Implications of Clumpiness (2008, background): “This has been verified in a large number of observations that estimate the luminosity dependence of either f2 or f1 (the fraction of unobscured sources), or differences between the luminosity functions of type 1 and 2 AGNs (see Hao et al. 2005; Simpson 2005; Maiolino et al. 2007).”
THE XMM-NEWTON WIDE-FIELD SURVEY IN THE COSMOS FIELD (XMM-COSMOS): DEMOGRAPHY AND MULTIWAVELENGTH PROPERTIES OF OBSCURED AND UNOBSCURED LUMINOUS ACTIVE GALACTIC NUCLEI (2010, background): “…the finding, mainly from X–ray surveys, that absorption is much more common at low luminosities (see e.g. Ueda et al. 2003, la Franca et al. 2005, Maiolino et al. 2007, Hasinger 2008) and, possibly, at high redshift (La Franca et al. 2005; Ballantyne et al. 2006; Treister & Urry 2006; Hasinger…”
CHASING HIGHLY OBSCURED QSOs IN THE COSMOS FIELD (2008, background): “…population is large at low AGN luminosities and decreases at high luminosities, as it is indeed observed (Lawrence & Elvis 1982, Ueda et al. 2003, Steffen et al. 2003, La Franca et al. 2005, Treister & Urry 2005, 2006, Maiolino et al. 2007, Hasinger 2008, Trump et al. 2008, Della Ceca et al. 2008).”
THREE-YEAR SWIFT–BAT SURVEY OF ACTIVE GALACTIC NUCLEI: RECONCILING THEORY AND OBSERVATIONS? (2010, result): “From the results of Della Ceca et al. (2008), they found a slope of 0.22, in very good agreement with the IT effect, with the slope ( 0.18) presented in Maiolino et al. (2007), and eventually with our findings ( 0.26).”
New Spectral Model for Constraining Torus Covering Factors from Broadband X-Ray Spectra of Active Galactic Nuclei (2018, methodology): “Studies in the infrared band indicate that the torus covering factor may be a function of luminosity (e.g., Maiolino et al. 2007, Treister et al. 2008, Assef et al. 2013), and may correlate with other measurable properties (e.g., presence of broad lines in optical spectra; Mateos et al. 2016).”
Resolving the mid-infrared cores of local Seyferts (2009, result): “…– in other words, a decrease ofLMIR /LBol – with increasingLBol is qualitatively similar to that inferred in the quasar regime by other authors (e.g. Maiolino et al. 2007; Treister et al. 2008) and may be int rpreted in terms of a decrease of covering factor ofdust for more powerful sources.”
What broad emission lines tell us about how active galactic nuclei work (2009, background): “The covering factor of the torus can be calculated statistically from the ratio of type-1 (faceon) to type-2 (edge-on) AGNs, and directly for in- dividual objects from the strength of the thermal emission (e.g., Maiolino et al. 2007).”
Star formation in AGN hosts in GOODS-N (2010, background): “(5) of Maiolino et al. (2007) and a ratio 7 between bolometric and 5100 Å luminosity.”
Revisiting the Unified Model of Active Galactic Nuclei (2015, methodology): “Covering factors for a large number of type-I AGNs have been obtained by using the Ldust/LAGN method (Maiolino et al. 2007; Treister, Krolik & Dullemond 2008; Mor & Trakhtenbrot 2011; Mor & Netzer 2012; Roseboom et al. 2013; Lusso et al. 2013).”