A long hard look at MCG-6-30-15 withXMM-Newton

Abstract

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.

Fluorescent iron lines as a probe of astrophysical black hole systems

“…The first results from a later and very long (400 ks) XMM-Newton observation of MCG-6-30-15 were reported recently by Andy Fabian and collaborators [220]. This observation has produced the best iron line profile yet obtained from any object (Fig.…”

“…15. Continuum subtracted iron line profile from the second XMM-Newton observation of MCG-6-30-15 [220]. This is the highest signal to noise relativistic line profile yet measured.…”

Suzaku observations of iron lines and reflection in AGN

“…The Seyfert 1 galaxy MCG -6-30-15 (z = 0.00775) was observed 3 times by Suzaku in 2006 January, with a total exposure of 347 ks and a mean 2-10 keV flux of 4.0 × 10 −11 erg cm −2 s −1 , similar to the XMM-Newton deep look (Fabian et al 2002). The broad band Suzaku spectrum of MCG -6-30-15 plotted as a ratio to a power-law continuum of Γ = 2.0, is shown in Figure 4.…”

The history of the iron Kαline profile in the Piccinotti AGN ESO 198-G24

“…> ∼ 2 hours, corresponding to a spatial scale of > ∼ 7R S M −1 8 , if M 8 is the black hole mass in units of 10 8 solar masses. Fabian et al (2002) point out similar problems to explain the short time scales variability pattern of the relativistic line in MCG-6-30-15. If the BeppoSAX profile is substantially "contaminated" by a narrow component, the discrepancy between the broad component EWs is obviously even larger.…”

“…In a few objects the existence of a relativistically broadened iron line profile is out of question (Nandra et al 1999;Wilms et al 2001;Turner et al 2002;Fabian et al 2002). However, often the observed profiles do not match the theoretical calculations (Fabian et al 1989;Laor 1991;Matt et al 1992).…”