Rapid Compton-thick/Compton-thin Transitions in the Seyfert 2 Galaxy NGC 1365

By G. Risaliti, M. Elvis, G. Fabbiano, A. Baldi, A. Zezas. 2005

198 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/4f0e067fdc99e3c54e2549e9cec5ac303473aa91

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In Astronomy and Astrophysics

Citations in the corpus

An XMM–Newton survey of broad iron lines in Seyfert galaxies (2007, background): “We exclude one case of a Seyfert 1.8, NGC 1365, which has been shown to have a highly complex spectrum which at least at times is Compton thick (Risaliti et al. 2005), severely complicating analysis of the iron line.”
Occultation Measurement of the Size of the X-Ray-emitting Region in the Active Galactic Nucleus of NGC 1365 (2007, methodology): “The spectral analysis revealed the presence of a highly ionized, compact absorber (Risaliti et al. 2005B), while the timing analysis revealed column density variability of ∆(NH) ∼ 10 23 cm−2 on time scales of ∼ 50 ks (Risaliti 2006, Risaliti et al. 2007, in prep.).”
The FIRST-2MASS Red Quasar Survey (2007, background): “This is an especially important caveat in the case of dust-obscured quasars, as the obscuring material close to the nucleus may cross the line of sight over these timescales, leading to different measurements of the source’s extinction (e.g., Risaliti et al. 2005).”
First X-ray-based statistical tests for clumpy-torus models: eclipse events from 230 years of monitoring of Seyfert AGN (2014, background): “1 d) eclipse events observed in other objects, namely NGC 1365 and Mkn 766 (Risaliti et al. 2005, 2007, 8 This may not be true for Cen A, whose continuum emission is likely mildly beamed.”
Faint high-redshift AGN in the Chandra deep field south: the evolution of the AGN luminosity function and black hole demography (2011, background): “Compact absorbers have been discovered in local Seyferts (e.g. Risaliti et al. 2005), but they might be more common at high redshift.”
Active galactic nuclei: what’s in a name? (2017, background): “…have shown that the X-ray and optical spectral properties of AGN can vary on relatively short timescales as a result of changes in the absorbing column density along the line of sight (e.g. Risaliti et al. 2002, 2005; Matt et al. 2003; MacLeod et al. 2016; Ruan et al. 2016; see also Sect.”
The AGN-obscuring Torus: The End of the “Doughnut” Paradigm? (2006, unknown): “From time variations of X-ray obscuration that indicate cloud motions across the line of sight, Risaliti et al. (2002, 2005) ﬁnd that some of the obscuring clouds are at radii considered typical of the AGN broad-line region (BLR).”
TESTING THE UNIFICATION MODEL FOR ACTIVE GALACTIC NUCLEI IN THE INFRARED: ARE THE OBSCURING TORI OF TYPE 1 AND 2 SEYFERTS DIFFERENT? (2011, unknown): “…Levenson et al. (2006); (f) Jiménez-Bailón et al. (2005); (g) Vignali & Comastri (2002); (h) Elvis et al. (2004); (i) Awaki et al. (2006); (j) Turner et al. (2000); (k) Risaliti et al. (2005); (l) Yaqoob et al. (2007); (m) Lamer et al. (2000); (n) Lamer et al. (2003); (o) Beckmann et al. (2005).”
X-RAY SPECTRAL PROPERTIES OF THE BAT AGN SAMPLE (2008, methodology): “The source has been observed extensively by XMM-Newton and Chandra with relevant papers – for instance Risaliti (2007) and Risaliti et al. (2005).”
The Blast Wave Model for AGN Feedback: Effects on AGN Obscuration (2008, background): “These are the regions where the Compton-thick absorbers are presumably located, according to several observational indications, from the local abundance of Compton-thick sources (favoring large covering factors and consequently compact sizes; Risaliti et al. 1999), to the direct limits from Chandra ”