Evidence of a high-velocity ionized outflow in a second narrow-line quasar PG 0844+349

By K. Pounds, A. King, K. Page, P. O’Brien. 2003

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Following the discovery of X-ray absorption in a high-velocity outflow from the bright quasar PG 1211 + 143 we have searched for similar features in XMM–Newton archival data of a second (high accretion rate) quasar PG 0844+349. Evidence is found for several faint absorption lines in both the EPIC and RGS spectra, whose most likely identification with resonance transitions in H-like Fe, S and Ne implies an origin in highly ionized matter with an outflow velocity of order ∼0.2c. The line equivalent widths require a line-of-sight column density of NH∼ 4 × 1023 cm−2, at an ionization parameter of log ξ∼ 3.7. Assuming a radial outflow being driven by radiation pressure from the inner accretion disc, as suggested previously for PG 1211 + 143, the flow in PG 0844+349 is also likely to be optically thick, in this case within ∼25 Schwarzschild radii. Our analysis suggests that a high-velocity, highly ionized outflow is likely to be a significant component in the mass and energy budgets of active galactic nuclei accreting at or above the Eddington rate.

Subfields: Astronomy and Astrophysics, Statistics and Probability

View Paper: https://www.semanticscholar.org/paper/93f538a6b67b8f8ef6d89733d2fc679e700eaddb

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Citations in the corpus

The nature and origin of Seyfert warm absorbers (2004, background): “…et al. (1986); c Santos-Lleo et al. (1995); d Markowitz et al. (2003); e Kriss et al. (2000); f Petrucci et al. (2004); g Bachev & Strigachev (2003); h Pounds et al. (2003c); i Swain et al. (2003); j Yuan et al. (2002); k Gondhalekar et al. (1994); l Turner et al. (2002); m Reynolds (2000); n…”
The multi-phase winds of Markarian 231: from the hot, nuclear, ultra-fast wind to the galaxy-scale, molecular outflow (2015, background): “Furthermore, there is growing evidence for the existence of ultra-fast outflows (UFOs) via the detection of highly ionized Fe K-shell absorption arising from a gas moving at velocities up to 0.2–0.4c (Pounds et al. 2003; Reeves et al. 2009; Tombesi et al. 2011, 2015 and references therein).”
CLEARING OUT A GALAXY (2012, background): “Accordingly the most likely connection is via high–velocity wide–angle winds expelled from the vicinity of the nucleus by radiation pressure (e.g. Pounds et al. 2003a,b).”
On why the iron K-shell absorption in AGN is not a signature of the local warm/hot intergalactic medium (2008, background): “However the deep iron K absorption feature observed at 7 keV in 2001 (Pounds et al. 2003) which is readily apparent even on this broad band spectral plot, is not present at the same strength in either the 2004 or 2005 data.”
The Blast Wave Model for AGN Feedback: Effects on AGN Obscuration (2008, background): “…up to vw 0:1c in the central regions, which yield AGN vw /2c 0:05 bymomentum conservation between photons and particles (see Chartas et al. 2002; Pounds et al. 2003); this value has also been adopted in a number of simulations (e.g., Di Matteo et al. 2005) and semianalytic models of galaxy…”
The physics of galactic winds driven by active galactic nuclei (2012, background): “X-ray observations also find evidence for AGN winds with velocities ∼ 0.1c, albeit with lower significance and with more ambiguous interpretation (e.g., Chartas et al. 2002; Pounds et al. 2003; Tombesi et al. 2010).”
A semi-analytic model for the co-evolution of galaxies, black holes and active galactic nuclei (2008, background): “…broad absorption line (BAL) quasars], high-velocity winds have been detected in a variety of different types of quasar systems (de Kool et al. 2001; Chartas, Brandt & Gallagher 2003; Pounds et al. 2003; Pounds & Page 2006), and are now believed to be quite ubiquitous (Ganguly & Brotherton 2008).”
Supercritical Accretion Flows around Black Holes: Two-dimensional, Radiation Pressure-dominated Disks with Photon Trapping (2005, background): “Moreover, Pounds et al. (2003a, 2003b) and Reeves, O’Brien, & Ward (2003) reported by the blueshifted X-ray absorption lines that the highly ionized matter with outflow velocity of order ∼ 0.1c in quasars, and the flow is likely to be optically thick to the electron scattering within r ∼ 100rg.”
Fueling Low-Level AGN Activity through Stochastic Accretion of Cold Gas (2006, background): “…of typical, narrow-line quasars also find BAL-like outflow velocities for some species accelerating at small radii from the central engine (Pounds et al. 2003a,b), and outflows with large covering angles in central regions of “normal” quasars may even be detected in gravitational lensing…”
Direct Cosmological Simulations of the Growth of Black Holes and Galaxies (2007, background): “These include Seyfert II ULIRGs (e.g., Rupke et al. 2005), the ‘‘warm absorbers’’ seen in soft X-rays that show evidence of outflow (e.g., Laor et al. 1997), and broad absorption line (BAL) systems with intense winds with velocities up to 104 km s 1 (e.g., Pounds et al. 2003a, 2003b).”
Cosmological simulations of the growth of supermassive black holes and feedback from active galactic nuclei: method and tests (2009, background): “For example, absorbers seen in X-rays show evidence of outflow (Laor et al. 1997) and broad absorption line systems show evidence of outflows at very high velocity (e.g. Pounds et al. 2003).”