A high-velocity ionized outflow and XUV photosphere in the narrow emission line quasar PG1211+143

By K. Pounds, J. Reeves, A. King, K. Page, P. O’Brien, M. W. D. O. PhysicsAstronomy, U. Leicester, Lab. for High Energy Astrophysics, Nasa Gsfc. 2003

349 citations recorded by the source corpus.

The definitive version is available from www.blackwell-synergy.com. Erratum published in Monthly Notices of the Royal Astronomical Society, 2005, 356, p.1599

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/80bafc172b3323ff8789eb201804a4ff90ae9193

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Citations in the corpus

Global Radiation-Magnetohydrodynamic Simulations of Black-Hole Accretion Flow and Outflow: Unified Model of Three States (2009, background): “…outflows with velocity of ∼0.25c in model A will explain the X-ray observations of bright quasars exhibiting blue-shifted absorption lines, which are interpreted as the absorption by the outflow material moving with velocity on the order of 0.1c (Pounds et al. 2003; Reeves et al. 2003).”
Relativistic X-Ray Lines from the Inner Accretion Disks Around Black Holes (2007, background): “Pounds et al. (2003a) analyzed an XMM-Newton observation of NGC 5548, and report no evidence of a broad disk line (though an upper limit on such a feature is not given).”
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…”
Heating cooling flows with jets (2003, background): “1 shows that the dynamical time of the ICM exceeds 200 Myr at all radii, the large-scale structure of the ICM will be unaffected by fluctuations in the AGN’s power on short time-scales.”
An Explanation for the soft X-ray excess in AGN (2005, background): “This has implications for the energetics and cosmological evolution of these systems, as some measured outflows can involve similar amounts of power as the radiation e.g. Pounds et al. (2003).”
Quasar feedback revealed by giant molecular outflows (2010, background): “…and nearby Seyfert nuclei prominent outflows are observed, but generally only i the ionized gas component (e.g. Crenshaw et al. 2003; Turnshek 1984; Pounds et al. 2003), which accounts only for a minor fraction of the gas mass in the host galaxy, and are generally confined in the nuclear region on…”
Powerful Outflows and Feedback from Active Galactic Nuclei (2015, methodology): “A decade after the first reports (Pounds et al. 2003, Reeves et al. 2003), high-velocity (v∼0.1c), highly-ionized winds are now established to be common in low redshift AGN.”
Modelling feedback from stars and black holes in galaxy mergers (2004, background): “…of a number of quasars (mostly broad absorption line systems) reveal significant absorption, implying large outflows with a kinetic power corresponding to a significant fraction of the AGN bolometric luminosity (Chartas, Brandt & Gallagher 2003; Crenshaw, Kraemer & George 2003; Pounds et al. 2003).”
A unified model for AGN feedback in cosmological simulations of structure formation (2007, background): “The presence of quasar induced outflows has been observationally confirmed in a number of cases (e.g. Chartas et al., 2003; Crenshaw et al., 2003; Pounds et al., 2003), and has first been demonstrated in simulations of merging galaxy pairs by Di Matteo et al. (2005).”
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…”
EVIDENCE FOR ULTRA-FAST OUTFLOWS IN RADIO-QUIET ACTIVE GALACTIC NUCLEI. II. DETAILED PHOTOIONIZATION MODELING OF Fe K-SHELL ABSORPTION LINES (2011, background): “The detection in this observation was already reported by Pounds et al. (2003).”
Evidence for ultra-fast outflows in radio-quiet AGNs - I. Detection and statistical incidence of Fe K-shell absorption lines (2010, methodology): “Mrk 766: a detailed analysis of the XMM-Newton EPIC pn spectra of the source has already been reported by Pounds et al. (2003c), Miller et al. (2007) and Turner et al. (2007).”
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).”
DISCOVERY OF ULTRA-FAST OUTFLOWS IN A SAMPLE OF BROAD-LINE RADIO GALAXIES OBSERVED WITH SUZAKU (2010, methodology): “…de- tection of blue-shifted Fe K absorption lines at rest-frame energies of ∼7–10 keV in the X-ray spectra of radio-quiet AGN (e.g., Chartas et al. 2002; Chartas et al. 2003; Pounds et al. 2003; Dadina et al. 2005; Markowitz et al. 2006; Braito et al. 2007; Cappi et al. 2009; Reeves et al. 2009a).”
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).”
An XMM–Newton survey of broad iron lines in Seyfert galaxies (2007, background): “Individual cases have been found in which no broadening seems to be required (e.g. Gondoin et al. 2001, 2003; Pounds et al. 2003; Bianchi et al. 2004), or where alternative, physically plausible explanations can account for the broad features (e.g. Reeves et al. 2004).”
Evidence of a high-velocity ionized outflow in a second narrow-line quasar PG 0844+349 (2003, methodology): “As shown in the analysis of PG 1211+143 (Pounds et al. 2003), for a radial outflow with constant (coasting) speed v, occupying a solid angle of 4πb steradians, mass conservation implies the outflow is optically thick at a radius Rph, where Rph Rs = 1 2ηb c v Ṁout ṀEdd .”