An absorption origin for the X-ray spectral variability of MCG-6-30-15

By L. Miller, T. Turner, J. Reeves. 2008

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Context. The Seyfert I galaxy MCG–6-30-15 shows one of the best examples of a broad “red wing” of emission in its X-ray spectrum at energies 2 20 keV. Methods. We compiled all the available long-exposure, high-quality data for MCG–6-30-15: 522 ks of Chandra hetgs, 282 ks of XMM-Newton pn/rgs and 253 ks of Suzaku xis/pin data. This is the first analysis of this full dataset. We investigated the spectral variability on timescales >20 ks using principal components analysis and fitted spectral models to “flux state” and mean spectra over the energy range 0.5−45 keV (depending on detector). The absorber model was based on the zones previously identified in the highresolution grating data. Joint fits were carried out to any data that were simultaneous. Results. Multiple absorbing zones covering a wide range of ionisation are required by the grating data, including a highly ionised outflowing zone. A variable partial-covering zone plus absorbed low-ionisation reflection, distant from the source, provides a complete description of the variable X-ray spectrum. A single model fits all the data. We conclude that these zones are responsible for the red wing, its apparent lack of variability, the absorption structure around the Fe Kα line, the soft-band “excess” and the high flux seen in the hard X-ray band. A relativistically-blurred Fe line is not required in this model. We suggest the partial covering zone is a clumpy wind from the accretion disk.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/33125ca994458f1fdca3b1c9d653797c14a67228

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The role of the reflection fraction in constraining black hole spin (2014, background): “…et al. 2012), or NGC 1365, (Risaliti et al. 2013), Galactic Black Holes, such as Cyg X-1 (Fabian et al. 1989; Duro et al. 2011; Tomsick et al. 2014), GRS 1915+10 (Miller et al. 2013b), or GX 339−4 (Miller et al. 2008; Reis et al. 2008), and neutron stars (e.g., Serpens X-1; Miller et al. 2013a).”
Stellar and Quasar Feedback in Concert: Effects on AGN Accretion, Obscuration, and Outflows (2015, background): “…(v ∼ 102− 103 kms−1) associated with the narrow line region and the “warm absorber” (Laor et al. 1997; Crenshaw et al. 2000; Steenbrugge et al. 2005; Krongold et al. 2007), as well as quasar absorption and occultation systems (e.g. McKernan & Yaqoob 1998; Turner et al. 2008; Miller et al. 2008).”
The Suzaku View of Highly Ionized Outflows in AGN. 1; Statistical Detection and Global Absorber Properties (2012, background): “Furthermore, in some sources (e.g. Mrk 766, Miller et al. 2007; MCG -6-30-15, Miller et al. 2008) the ‘excess’ could simply be a product of complex absorption and just be the manifestation of opacity around ∼1–2 keV.”
IMPROVED REFLECTION MODELS OF BLACK HOLE ACCRETION DISKS: TREATING THE ANGULAR DISTRIBUTION OF X-RAYS (2013, background): “…USA; alohfink@astro.umd.edu, chris@astro.umd.edu, ftombesi@astro.umd.edu 4 NASA Goddard Space Flight Center, Greenbelt, MD 20771 USA; timothy.r.kallman@nasa.gov these relativistic effects (e.g., Miller et al. 2008; Steiner et al. 2011; Reynolds et al. 2012; Fabian et al. 2012a; Dauser et al. 2012).”
X-RAY REFLECTED SPECTRA FROM ACCRETION DISK MODELS. III. A COMPLETE GRID OF IONIZED REFLECTION CALCULATIONS (2013, background): “…a skewed line profile with a red wing that can extend to very low energies, particularly in the case of high spin (e.g., Fabian et al. 2000; Fabian & Vaughan 2003; Reynolds & Nowak 2003; Dovčiak et al. 2004; Miller et al. 2008; Steiner et al. 2011; Reynolds et al. 2012; Dauser et al. 2012).”