Broad Iron Lines in Active Galactic Nuclei

By A. C. Fabian, K. Iwasawa, C. Reynolds, A. Young. 2000

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Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/6cda11c1b75980a7220ac3a960d49166ad05dbe2

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Suzaku observations of 'bare' active galactic nuclei (2012, background): “…broad emission features that can be associated with relativistically broadened iron lines (see e.g. Tanaka et al. 1995; Nandra et al. 1999, 2007; Fabian et al. 2000, 2009), and C© 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society Downloaded from…”
Constraining the mass of dark photons and axion-like particles through black-hole superradiance (2018, methodology): “Both the (massindependent) shape of the iron Kα line seen in reflection [71] and the thermal emission from the inner edge of the disc [72] — assumed to be the ISCO [73, 74] (see also [75] for a discussion on the emission from within the plunging region) — are commonly employed for both stellar mass ”
A high-velocity ionized outflow and XUV photosphere in the narrow emission line quasar PG1211+143 (2003, background): “…this ‘hard’ X-ray continuum in Seyfert galaxies arises by Comptonisation of thermal emission from the accretion disc in a ‘hot’ corona (eg Haardt and Maraschi 1991), and produces additional spectral features by ‘reflection’ from dense matter in the disc (eg Pounds et al. 1990, Fabian et al. 2000).”
Measuring the spins of accreting black holes (2011, methodology): “In the Fe Kα method, one determines rISCO by modeling the profile of the broad and skewed iron line, which is formed in the inner disk by Doppler effects, light bending, relativistic beaming, and gravitational redshift (Fabian et al 2000, Reynolds and Nowak 2003, Miller 2007).”
Compton reflection and iron fluorescence in BeppoSAX observations of Seyfert type 1 galaxies (2002, result): “…variability which typically affects the continuum emission of these objects (in addition to reported cases of variations in the line, e.g. Weaver et al. 2001 and references in Fabian et al. 2000), the comparison of Wα, as measured with ASCA, and of R as measured with Ginga, would lack significance.”
An XMM–Newton survey of broad iron lines in Seyfert galaxies (2007, background): “Reviews of the broad line pheonemenon have been published by, e.g. Fabian et al. (2000), Reynolds & Nowak (2003), Liedahl & Torres (2005) and Miller (2007).”
A systematic look at the Very High and Low/Hard state of GX 339-4: Constraining the black hole spin with a new reflection model (2008, background): “…of an accretion disc the ironKα line shape is distorted by various relativistic effects such as gravitational redshift, light-bending, frame-dragging and Doppler shifts,with the effects becoming more prominent the closer the line is emittd o the event horizon (Fabian et al. 1989, 2000; Laor 1991 ).”
An Extended Scheme for Fitting X-Ray Data with Accretion Disk Spectra in the Strong Gravity Regime (2004, background): “For a recent review for AGNs, see Fabian et al. (2000), Reynolds & Nowak (2003), and references cited therein.”
High-Resolution X-Ray Spectroscopy and Modeling of the Absorbing and Emitting Outflow in NGC 3783 (2001, background): “At least some of the Fe Ka Ñuorescent line emission seen from Seyfert 1 galaxies is often very broad and is generally interpreted as originating from an accretion disk orbiting around a central black hole (e.g., Fabian et al. 2000 and references therein).”
THE NUCLEAR SPECTROSCOPIC TELESCOPE ARRAY (NuSTAR) HIGH-ENERGY X-RAY MISSION (2013, background): “Matter velocities are high, and general and special relativistic effects are very strong in the vicinity of the BH, modifying emission line profiles (Fabian et al. 1989; see Fabian et al. 2000, Miller 2007 for reviews).”
Superradiance (2015, methodology): “Both the (mass-independent) shape of the iron Kα line seen in reflection [628] and the thermal emission from the inner edge of the disc [629] – assumed to be the ISCO [630, 631] – are commonly employed for both stellar mass BHs in binaries and supermassive BHs in active galactic nuclei (although the”
Black hole accretion discs in the canonical low‐hard state (2009, background): “Therefore, the shape of the prominent iron Kα line can give a direct indication of the radius of the reflection material from the black hole (Fabian et al. 1989, 2000; Laor 1991).”
A light bending model for the X-ray temporal and spectral properties of accreting black holes (2003, background): “However, this interpretation conflictswith the observation of broad and redshifted iron lines in some sources that strongly suggests an origin close to the central black hole (e.g Fabian et al. 2000; Reynolds & Nowak 2003 for a review on iron lines).”