A long hard look at MCG–6-30-15 with XMM-Newton

By A. C. Fabian, S. Vaughan, K. Nandra, K. Iwasawa, D. Ballantyne, J. Lee, A. Rosa, A. Turner, A. J. Y. IoA, Cambridge and 5 more. 2002

380 citations recorded by the source corpus.

We present the first results from a 325-ks observation of the Seyfert 1 galaxy MCG–6-30-15 with XMM-Newton and BeppoSAX. The strong, broad, skewed iron line is clearly detected and is well characterized by a steep emissivity profile within 6rg (i.e. 6GM/c2) and a flatter profile beyond. The inner radius of the emission appears to lie at about 2rg, consistent with results reported from both an earlier XMM-Newton observation of MCG–6-30-15 by Wilms et al. and part of an ASCA observation by Iwasawa et al. when the source was in a lower flux state. The radius and steep emissivity profile do depend however on an assumed incident power-law continuum and a lack of complex absorption above 2.5 keV. The blue wing of the line profile is indented, either by absorption at about 6.7 keV or by a hydrogenic iron emission line. The broad iron line flux does not follow the continuum variations in a simple manner.

Subfields: Astronomy and Astrophysics, Computational Mechanics

View Paper: https://www.semanticscholar.org/paper/180ceb4bacb312e86599093017fc4a1b83036104

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Computational Mechanics

Citations in the corpus

An XMM–Newton survey of broad iron lines in Seyfert galaxies (2007, background): “On the other hand, there are numerous examples where a relativistic accretion disk line is the preferred interpretation (e.g. Reeves et a. 2001; Gondoin et al. 2002; Longinotti et al. 2003), including the seemingly cast–iron case of MCG-6-30-15 (Fabian et al. 2002; Vaughan & Fabian 2004).”
Modeling Kicks from the Merger of Generic Black Hole Binaries (2008, result): “Low spin magnitudes would lower kicks, but this is contrary to spin inferences from Fe Kα lines; see Iwasawa (1996); Fabian et al. (2002); Reynolds & Nowak (2003); Brenneman & Reynolds (2006).”
IMPROVED REFLECTION MODELS OF BLACK HOLE ACCRETION DISKS: TREATING THE ANGULAR DISTRIBUTION OF X-RAYS (2013, background): “Differences to the Angle-Average (relxill_lp) Recent measurements (Wilms et al. 2001; Fabian et al. 2002; Brenneman & Reynolds 2006; Dauser et al. 2012; Fabian et al. 2012b; Gallo et al. 2011; Ponti et al. 2010; Brenneman et al. 2011, 2013; Duro et al. 2011; Miller et al. 2006; Reis et al. 2008)…”
Understanding X‐ray reflection emissivity profiles in AGN: locating the X‐ray source (2012, background): “Weaker variation of the reflection component that is uncorrelated with the variation in the primary continuum was observed by Vaughan & Edelson (2001) and Fabian & Vaughan (2003) in MCG–6-30-15.”
General relativistic magnetohydrodynamic simulations of the jet formation and large-scale propagation from black hole accretion systems (2006, background): “Observations of MCG 6-30-15 show an iron line feature consistent with emission from a relativistic disk with v/c ∼ 0.2 (Tanaka et al. 1995; Fabian et al. 2002), although the lack of a temporal correlation between the continuum emission and iron-line emission may suggest the basic fluorescence model…”
On characterizing the variability properties of X-ray light curves from active galaxies (2003, background): “(2002), Fabian et al. (2002) and Schurch & Warwick (2002) for some examples of rms spectra from AGN.”
Broad iron L line and X-ray reverberation in 1H0707-495 (2009, background): “Another way to explore the variability is through fluxresolved spectra (e.g. Vaughan & Fabian 2004).”
Black holes in astrophysics (2005, background): “The data confirm that the emission comes from a relativistic disk (e.g., Vaughan & Fabian 2004) and at least some of the datasets can be interpreted in terms of a rapidly spinning BH, e.g., assuming that there is no emission from within the ISCO, Reynolds et al. (2004b) estimate a∗ > 0.93.”
The Suzaku View of Highly Ionized Outflows in AGN. 1; Statistical Detection and Global Absorber Properties (2012, background): “Furthermore, weak hard-band absorption has been noted in the XMM–Newton spectra of MCG -6-30-15 by several authors (e.g. Fabian et al. 2002; Vaughan & Fabian 2004; Nandra et al. 2007; Miller et al. 2008).”
An absorption origin for the X-ray spectral variability of MCG-6-30-15 (2008, methodology): “…for this work is that it has been recognised for some time that the red wing component is surprisingly constant in amplitude (Iwasawa et al., 1996; Vaughan & Fabian, 2004) (although Ponti et al. 2004 did find evidence for additional variability around 5 keV in the 2000XMM-Newton ob- servation).”
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): “Such RMS spectra have previously been determined for MCG–6-30-15 (Matsumoto et al 2003; Fabian et al 2002; Ponti et al 2004).”
Fluorescent iron lines as a probe of astrophysical black hole systems (2002, background): “Continuum subtracted iron line proHle from the second XMM-Newton observation of MCG–6-30-15 [220].”
Evidence for ultra-fast outflows in radio-quiet AGNs - I. Detection and statistical incidence of Fe K-shell absorption lines (2010, background): “For instance,Fabian et al. (2002) and Vaughan & Fabian (2004) found hints for a narrow absorption feature at∼6.7 keV probably due to Fe XXV Heα in the EPIC pn spectrum of this source.”
The iron line in MCG—6-30-15 from XMM—Newton: evidence for gravitational light bending? (2003, neutral): “2 A NA LY S I S Fabian et al. (2002a) discuss details of the observation and basic data reduction.”
An Extended Scheme for Fitting X-Ray Data with Accretion Disk Spectra in the Strong Gravity Regime (2004, methodology): “Note that an alternative interpretation of the data (as pointed out by Fabian et al. 2002) is that there is not an emission line at ∼ 6.9 keV, but He-like resonance absorption at ∼ 6.7 keV.”
Constraining Black Hole Spin via X-Ray Spectroscopy (2006, methodology): “This absorption feature was also preferentially used in the MCG 06-30-15 work of Vaughan & Fabian (2004) and was consistent with the prediction of Sako et al. (2003) based on a Reflection Grating Spectrometer (RGS) observation of this source in 2001.”
Black Hole Spin Evolution (2003, background): “Some SMBHs and GBHCs show broad, skewed Fe K lines, for example in MCG 6-30-15 (Tanaka et al. 1995; Fabian et al. 2002), Cyg X-1 (Miller et al. 2002b), and XTE J1650 500 (Miller et al. 2002a; for a review see Reynolds & Nowak 2003).”
Combined long and short timescale X-ray variability of NGC 4051 with RXTE and XMM-Newton (2003, background): “Zero lag, asymetric, CCFs: As the bulk of the X-rays will be produced, in all bands, close to the black hole (eg Fabian et al. 2002 require a highly centrally peaked emission profile in the disc to explain the shape of the iron line in MCG-6-30-15) we do not expect large lags between bands on short…”