A comprehensive range of X-ray ionized-reflection models

By R. Ross, A. Usa, UK InstituteofAstronomy. 2005

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X-ray ionized reflection occurs when a surface is irradiated with X-rays so intense that its ionization state is determined by the ionization parameter ξ ∝ F/n, where F is the incident flux and n the gas density. It occurs in accretion, on to compact objects including black holes in both active galaxies and stellar-mass binaries, and possibly in gamma-ray bursts. Computation of model reflection spectra is often time consuming. Here we present the results from a comprehensive grid of models computed with our code, which has now been extended to include what we consider to be all energetically important ionization states and transitions. This grid is being made available as an ionized-reflection model, REFLION, for XSPEC. Ke yw ords: accretion, accretion discs ‐ line: formation ‐ radiative transfer ‐ galaxies: active ‐ X-rays: general.

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Citations in the corpus

Multidimensional modelling of X-ray spectra for AGN accretion disc outflows (2008, background): “As one would expect, this scattered/reprocessed spectrum is qualitatively similarto that obtained from standard disk reflection models (e.g. Ross & Fabian 2005).”
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, methodology): “Figure 10 (right) shows the best-fit REFLIONX model, prior to (top) and after blurring (bottom), for the LHS.”
Broad iron L line and X-ray reverberation in 1H0707-495 (2009, methodology): “The flux ratio between the K and L features is 1:20, measured as the ratio of equivalent widths of two laor lines, is consistent with the value expected from atomic physics (Ross & Fabian 2005).”
An absorption origin for the X-ray spectral variability of MCG-6-30-15 (2008, methodology): “(1999) and Ross & Fabian (2005) and calculated by the extended model made available by those authors.”
Black hole accretion discs in the canonical low‐hard state (2009, methodology): “When using the reflection model REFLIONX, the Fe Kα line, as well as the Compton hump, is modelled self-consistently.”
Suzaku observations of 'bare' active galactic nuclei (2012, methodology): “This was also modelled with REFLIONX, with ξ = 1.0 (the lowest ionization state accepted by the model), while we required the iron abundance to be the same as that of the disc reflection component, and we again required that the photon index of the ionizing continuum to be the same as that of the PL”
Normalizing a Relativistic Model of X-ray Reflection: The Definition of the Reflection Fraction and its Implementation in relxill (2016, methodology): “In the nonrelativistic case, this is the standard assumption built into such widely used reflection models such as pexrav (Magdziarz & Zdziarski 1995), reflionx (Ross & Fabian 2005), and xillver (García et al. 2013).”
Broad Iron-Kα Emission Lines as a Diagnostic of Black Hole Spin (2007, background): “The ionized reflection models of Ross & Fabian (2005) show that distinguishable iron line features are lost when > 3 ; 103 erg cm s 1.”
IMPROVED REFLECTION MODELS OF BLACK HOLE ACCRETION DISKS: TREATING THE ANGULAR DISTRIBUTION OF X-RAYS (2013, methodology): “The reflection model that has been most widely used by observers, for both general application and for measuring black hole spin via the Fe-line method, is REFLIONX (Ross & Fabian 2005).”
Measuring the spins of accreting black holes (2011, methodology): “In order to determine the spin using the Fe-line method, one must model the reflection spectrum in detail (Ross and Fabian 2005, 2007).”
An Explanation for the soft X-ray excess in AGN (2005, methodology): “We fit them with the relativistically blurred photoionized disc model of Ross & Fabian (2005).”
X-RAY REFLECTED SPECTRA FROM ACCRETION DISK MODELS. I. CONSTANT DENSITY ATMOSPHERES (2010, methodology): “…1993; Czerny & Zycki 1994; Krolik et al. 1994; Magdziarz & Zdziarski 1995; Ross et al. 1996; Matt et al. 1996; Poutanen et al. 1996; Blackman 1999; Ross & Fabian 2005), while hydrostatic calculations have been carried out by Rozanska & Czerny (1996); Nayakshin et al. (2000); Nayakshin & Kallman…”
A quasi-periodic modulation of the iron line centroid energy in the black hole binary H1743−322 (2016, background): “An increase in disc ionization increases the iron line energy and suppresses the flux in the reflection hump relative to the line (e.g. Ross & Fabian 2005; Garcı́a et al. 2013), in conflict with what we observe (Fig.”
Relativistic iron K X-ray reverberation in NGC 4151 (2011, methodology): “In order to further understand the differences between the low and high flux intervals, we fitted the spectra with an absorbed power-law plus cold reflection modelled with the reflection table reflionx (Ross & Fabian 2005).”
Measuring Black Hole Spin Using X-Ray Reflection Spectroscopy (2013, methodology): “In practice, all of these measurements have employed the Ross & Fabian (2005) model reflionx.”
Going with the Flow: Can the Base of Jets Subsume the Role of Compact Accretion Disk Coronae? (2005, background): “…point, the coronal models themselves describe a continuum spectrum more complicated than a simple, 2 The pexriv model, incorporated into the eqpairmodel, tends to have an unnaturally sharp ionized Fe edge structure, especially when compared to the more sophisticated models of Ross & Fabian (2005).”
Suzaku Observations of the Hard X-ray Variability of MCG-6-30-15: the Effects of Strong Gravity Around a Kerr Black Hole (2006, methodology): “We use a grid of models from Ross & Fabian (2005) to obtain the X–ray reflection spectrum.”
THE EXTREME SPIN OF THE BLACK HOLE IN CYGNUS X-1 (2011, methodology): “Effect of using a different reflection model We replace IREFLECT⊗SIMPLC+KERRDISK with REFLIONX23 (Ross & Fabian 2005), which is widely used in measuring spin via the Fe Kα line.”