A soft X-ray study of type I active galactic nuclei observed with Chandra high-energy transmission grating spectrometer

By B. McKernan, T. Yaqoob, C. Reynolds. 2007

133 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/43ee1bd1b3808c8b3a4b9e43f42b5fdbb43b2904

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Citations in the corpus

DISCOVERY OF ULTRA-FAST OUTFLOWS IN A SAMPLE OF BROAD-LINE RADIO GALAXIES OBSERVED WITH SUZAKU (2010, methodology): “Following McKernan et al. (2007), we can derive a simple relation for the ratio between the mass outflow rate and the mass accretion rate, i.e. Ṁout/Ṁacc ≃ 6000C(v0.”
The Suzaku View of Highly Ionized Outflows in AGN. 1; Statistical Detection and Global Absorber Properties (2012, background): “…for discrete absorption lines and photoelectric edges in their soft-band (E < 3 keV) spectra (e.g. Reynolds 1997; Crenshaw et al. 2003; Blustin et al. 2005), with typical lineof-sight velocities ranging from a few hundred to around a thousand km s−1 (Blustin et al. 2005; McKernan et al. 2007).”
EVIDENCE FOR ULTRA-FAST OUTFLOWS IN RADIO-QUIET ACTIVE GALACTIC NUCLEI. II. DETAILED PHOTOIONIZATION MODELING OF Fe K-SHELL ABSORPTION LINES (2011, background): “In fact, these absorbers are usually less ionized, are outflowing with velocities lower than∼1000 km/s and are supposed to have a different physical origin (e.g., Blustin et al. 2005; McKernan et al. 2007).”
Evidence for ultra-fast outflows in radio-quiet AGNs - I. Detection and statistical incidence of Fe K-shell absorption lines (2010, methodology): “…parameters can not be constrained with the 4–10 keV EPIC pn spectra, we used the typical parameters already reported in the literature, i.e. a column density in the rangeNH≃1021– 1022 cm−2 and an ionization parameter in the interval logξ≃0– 3 erg s−1 cm (Blustin et al. 2005; McKernan et al. 2007).”
DRIVING OUTFLOWS WITH RELATIVISTIC JETS AND THE DEPENDENCE OF ACTIVE GALACTIC NUCLEUS FEEDBACK EFFICIENCY ON INTERSTELLAR MEDIUM INHOMOGENEITY (2012, background): “From observational estimates of the energetics of AGN outflows, one would expect this factor to be of order 0.001–0.01 (e.g., McKernan et al. 2007; Moe et al. 2009; Tombesi et al. 2010), which is also found in disk-wind simulations (Kurosawa et al. 2009; Takeuchi et al. 2010; Ohsuga & Mineshige…”
Unification of X-ray winds in Seyfert galaxies: from ultra-fast outflows to warm absorbers (2012, methodology): “The number of sources having papers reporting the detection of WAs is 21/35, therefore the fraction of objects with WAs is at least &60%, consistent with previous studies (Reynolds 1997; George et al. 1998; Blustin et al. 2005; McKernan et al. 2007; Winter 2010).”
The multi-phase winds of Markarian 231: from the hot, nuclear, ultra-fast wind to the galaxy-scale, molecular outflow (2015, background): “In X-rays mildly ionized warm absorbers with velocities of ∼500-1000 km s−1 are observed in more than half of AGN (Piconcelli et al. 2005; Blustin et al. 2005; McKernan et al. 2007).”
Powerful Outflows and Feedback from Active Galactic Nuclei (2015, background): “L, with outflow velocities of several hundred km s−1 (Blustin et al. 2005, McKernan et al. 2007).”
Intermediate mass black holes in AGN discs – I. Production and growth (2012, background): “This is a very high accretion rate for a black hole, exceeding inferred accretion rates from gas disks in most Seyfert AGN (McKernan et al. 2007).”