X-ray obscuration and obscured AGN in the local universe

By M. Guainazzi, G. Matt, G. Perola. 2005

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Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/d8ed97f315e61d8ad3b355c8aa5e10c0c18b8719

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An X-ray view of 82 LINERs with Chandra and XMM-Newton data (2009, methodology): “The spectral index shows an asymmetrical distribution with a median value (< Γ >=2.11± 0.52 ), consistent with other AGN as reported by Guainazzi et al. (2005) (see Table 10 and Fig.”
THE SPACE DENSITY OF COMPTON-THICK ACTIVE GALACTIC NUCLEUS AND THE X-RAY BACKGROUND (2009, background): “Based on a sample of 49 local Seyfert 2 galaxies, Guainazzi et al. (2005) estimated that ∼50% of all obscured AGN (NH>10 22 cm−2) are Compton thick, and similar estimates were made by Risaliti et al. (1999) based on much smaller numbers.”
What drives the growth of black holes (2011, result): “The predicted column densities and time-variable obscuration are in good agreement with those measured in nearby obscured AGNs (NH > 1022– 1025 cm−2 with absorbing column changes on < 1 year timescales; e.g., Risaliti et al. 1999, 2002; Guainazzi et al. 2005; Cappi et al. 2006).”
The synthesis of the cosmic X-ray background in the Chandra and XMM-Newton era (2006, background): “In the local Universe Compton-thick AGN are found to be as numerous as moderately obscured AGN (Risaliti et al. 1999; Guainazzi et al. 2005) and are expected to provide a significant contribution to the 30 keV peak in the XRB spectrum (Comastri et al. 1995; Gilli et al. 2001).”
ON THE UNIFICATION OF ACTIVE GALACTIC NUCLEI (2012, background): “…Compton thick AGNs (X-ray obscuring column NH & 1024 cm−2) was determined to be as high as 50% in a pre-selected sample of Seyfert 2 (Risaliti et al. 1999; Guainazzi et al. 2005) but only ∼ 20% in complete X-ray samples without spectroscopic pre-selection (Malizia et al. 2009; Burlon et al. 2011).”
PRECISE BLACK HOLE MASSES FROM MEGAMASER DISKS: BLACK HOLE–BULGE RELATIONS AT LOW MASS (2010, background): “Most are Compton thick (NH > 1024 cm−2; Guainazzi et al. 2005; Madejski et al. 2006; Zhang et al. 2006; Kondratko et al. 2006a; Greenhill et al. 2008; Zhang et al. 2010).”
The soft X-ray/NLR connection: a single photoionized medium? (2005, methodology): “We refer the reader to Guainazzi et al. (2005b) for details on this kind of analysis.”
Suzaku Observations of Active Galactic Nuclei Detected in the Swift BAT Survey: Discovery of a “New Type” of Buried Supermassive Black Holes (2007, background): “In optically selected Seyfert 2 galaxies, the presence of prominent soft X-ray emission is common (e.g., Guainazzi et al. 2005).”
Resolving the mid-infrared cores of local Seyferts (2009, methodology): “This also matches older [Oiii] measurements quoted by Guainazzi et al. (2005), if we correct for extinction using the prescription of Bassani et al.(1999).”
Dust covering factor, silicate emission, and star formation in luminous QSOs (2007, background): “In local AGNs, Compton thick nuclei are about as numerous as Compton thin ones (Risaliti et al., 1999; Guainazzi et al., 2005; Cappi etal., 2006).”
On the origin of soft X-rays in obscured AGN: answers from high-resolution spectroscopy with XMM–Newton (2006, background): “Nearby X-ray obscured Active Galactic Nuclei (AGN) invariably exhibit excess emission above the extrapolation of the absorbed nuclear emission (Turner et al. 1997; Guainazzi et al. 2005).”
AGN Dusty Tori. II. Observational Implications of Clumpiness (2008, background): “This could explain the Guainazzi et al. (2005) finding that at least 50% of Seyfert 2 galaxies are Compton-thick.”