Broad emission lines for a negatively spinning black hole

By T. Dauser, J. Wilms, C. Reynolds, L. Brenneman. Proceedings of the International Astronomical Union, 2010

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Abstract We present an extended scheme for the calculation of the profiles of emission lines from accretion disks around rotating black holes. The scheme includes disks with angular momenta which are parallel and antiparallel with respect to the black hole's angular momentum, as both configurations are assumed to be stable (King et al. 2005). Based on a Green's function approach, an arbitrary radius dependence of the disk emissivity and arbitrary limb darkening laws can be easily taken into account, while the amount of precomputed data is significantly reduced with respect to other available models. We discuss line shapes for such disks and present a code for modelling observational data with this scheme in X-ray data analysis programs. A detailed discussion will soon be presented in a forthcoming paper (Dauser et al. 2010).

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/34efc2fe3cd1644850e5f3f087e6f559acc5b6b7

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Citations in the corpus

X-RAY REFLECTED SPECTRA FROM ACCRETION DISK MODELS. III. A COMPLETE GRID OF IONIZED REFLECTION CALCULATIONS (2013, methodology): “This work will combine the general relativistic approach implemented in the relline code (Dauser et al. 2010, 2013) with the model spectra presented in this paper.”
The role of the reflection fraction in constraining black hole spin (2014, background): “As shown, e.g., by Dauser et al. (2010), the main effect of the spin on the observed spectrum is to define the location of the ISCO.”
A public code for general relativistic, polarised radiative transfer around spinning black holes (2016, methodology): “…Luminet 1979) and spectra (e.g., Cunningham 1975) of thin black hole accretion discs (Shakura & Sunyaev 1973; Page & Thorne 1974), including state of the art methods to fit spectra in order to infer parameters such as the black hole spin (Davis & Hubeny 2006; Li et al. 2005; Dauser et al. 2010).”
Suzaku observations of 'bare' active galactic nuclei (2012, methodology): “The key free parameters of RELCONV are the spin of the black hole, the inclination of the disc (i) and the radial emissivity profile of the disc.”
THE EXTREME SPIN OF THE BLACK HOLE IN CYGNUS X-1 (2011, methodology): “20 We performed tests with a newer version of these models,RELLINE and RELCONV (Dauser et al. 2010), which are interpolated on a finer grid, an found that our results presented in Section 4 (and elsewhere) are essentially unchanged.”
Irradiation of an accretion disc by a jet: general properties and implications for spin measurements of black holes (2013, methodology): “This problem has been extensively studied in the past and there are several models available to predictthe relativistic smearing given a certain emissivity of the accretion disc (e.g., Fabian et al. 1989; Laor 1991; Dovčiak, Karas & Yaqoob 2004; Brenneman & Reynolds 2006; Dauser et al. 2010).”
THE SPIN OF THE SUPERMASSIVE BLACK HOLE IN NGC 3783 (2011, methodology): “…data sets from XMM-Newton and Suzaku, combined with the latest models of reflection from an ionized accretion disk (e.g., Ross & Fabian 2005) and variable-spin relativistic smearing models (e.g., Brenneman & Reynolds 2006; Dauser et al. 2010), are giving us our first glimpses at the spins of SMBHs.”
Understanding X‐ray reflection emissivity profiles in AGN: locating the X‐ray source (2012, methodology): “This approach was also taken by Brenneman & Reynolds (2006) using the observed profile of the iron Kα spectral line to measure the spin of the black hole (the kerrdisk model) and in the relline model of Dauser et al. (2010).”
Testing the Kerr Black Hole Hypothesis Using X-Ray Reflection Spectroscopy (2016, methodology): “RELLXIL_NK employs the formalism of the transfer function for geometrically thin and optically thick accretion disks (Cunningham 1975; Speith et al. 1995; Dauser et al. 2010).”
TESTING THE NO-HAIR THEOREM WITH OBSERVATIONS IN THE ELECTROMAGNETIC SPECTRUM. IV. RELATIVISTICALLY BROADENED IRON LINES (2012, background): “…these line profiles can be used to measure the spins of black holes (Fabian et al. 1989; Stella 1990; Laor 1991; Reynolds & Nowak 2003; Dovčiak et al. 2004; Beckwith & Done 2004, 2005; Brenneman & Reynolds 2006; Reynolds & Fabian 2008; Dexter & Agol 2009; Karas & Sochora 2010; Dauser et al. 2010).”
Normalizing a Relativistic Model of X-ray Reflection: The Definition of the Reflection Fraction and its Implementation in relxill (2016, methodology): “…on the relevant and interesting case of relativistic reflection with the spectrum blurred by gravitational redshift and by Doppler and light-bending effects, a subject that has been widely studied (see, e.g., Fabian et al. 1989; Laor 1991; Dauser et al. 2010, and the review by Middleton 2015).”
IMPROVED REFLECTION MODELS OF BLACK HOLE ACCRETION DISKS: TREATING THE ANGULAR DISTRIBUTION OF X-RAYS (2013, methodology): “…redshift skew the Fe line (and the fluorescence lines of other elements) and can, for rapidly spinning black holes, extend the red wing of the line to very low energies (Fabian et al. 1982; Laor 1991; Dabrowski et al. 1997; Dovčiak et al. 2004; Brenneman & Reynolds 2006; Dauser et al. 2010).”
Measuring Black Hole Spin Using X-Ray Reflection Spectroscopy (2013, methodology): “The available and commonly employed disk-line convolution models (e.g., relconv; Dauser et al. 2010) are based on GR ray-tracing calculations within the Kerr metric, assuming a razor thin accretion disk lying in the equator of the rotating black hole.”