The time-averaged ``Deep Minimum'' spectrum

In this section, we present a detailed re-analysis of the time-averaged EPIC-pn spectrum first presented in Paper I. The purpose of this re-analysis is two-fold. Firstly, we wish to test the robustness of the results from Paper I to the application of more realistic models. We will demonstrate that one still requires extreme broadening/redshifting of the X-ray reflection features, even when one uses self-consistent ionized reflection models (that include Compton broadening of the iron line), complex absorption, and a curved continuum derived from thermal Comptonisation. With that fact established, the second purpose of this section is to apply physically motivated relativistic smearing laws to these data, allowing us to test directly particular accretion disk models.

Table 1: First set of spectral fits to the time-averaged EPIC-pn data for the July 2000 observation of MCG$-$6-30-15. Spectral models are denoted as follows: ABS = neutral absorption with the Galactic column density of $N_{\rm H}=4.1\times 10^{20}\hbox{${\rm cm}^{-2}\,$}$; cRECO = cold reflection continuum (described by the PEXRAV model within the xspec fitting package; Magdziarz & Zdziarski 1995) with a relative reflection strength of ${\cal R}$; iREFL = ionized reflection model (Ballantyne, Ross & Fabian 2001) with an ionization parameter $\xi$; KDISK = relativistic smearing convolution model for a thin disk around a near-extremal Kerr black hole (spin parameter $a=0.998$) viewed at an inclination of $i$ with a surface emissivity varying as $\epsilon \propto r^{-\beta }$ between radii $r=r_{\rm in}$ and $r=400r_{\mathrm g}$; NFE = narrow emission line of iron with rest-frame energy $E_{\rm narrow}$ and equivalent width $W_{\rm K\alpha}$; PCABS = partial covering neutral absorber in which a column density $N_{\rm H}$ covers a fraction $f$ of the X-ray source; PO = power-law continuum with photon index $\Gamma$

Model Parameters 2-10keV fitting 0.5-10keV fitting 0.5-10keV fitting

(pure warm absorber) (absorber+emitter)

$$N_{\rm H} 4.1^{+0.1}_{-0} 4.1^{+0.1}_{-0}$$ ABS(PO) =4.1

$$\Gamma 1.795^{+0.015}_{-0.015} 2.04\pm 0.01 1.82\pm 0.01$$

$$\chi^2$$ 2514/2109 5092/2905 3595/2902

$$N_{\rm H} 4.1^{+0.1}_{-0} 4.1^{+0.1}_{-0}$$ ABS(PO+NFE) =4.1

$$\Gamma 1.81^{+0.01}_{-0.02} 2.05\pm 0.01 1.83\pm 0.01$$

$$E_{\rm narrow} 6.40^{+0.01}_{-0.02} 6.40\pm 0.01 6.39\pm 0.01$$

$$W_{\rm K\alpha } 96\pm 10 65\pm 15$$ 65

$$\chi^2$$ 2401/2107 4870/2903 3474/2900

$$N_{\rm H,1} =4.1 4.1^{+0.01}_{-0} 4.4^{+1.3}_{-0.3}$$ ABS*PCABS*(PO+NFE)

$$N_{\rm H,2} 940^{+150}_{-160} 740^{+40}_{-30} 680\pm 50$$

$$f 0.53\pm 0.03 0.47^{+0.01}_{-0.02} 0.41\pm 0.03$$

$$\Gamma 2.32^{+0.07}_{-0.06} 2.26\pm 0.01 2.17\pm 0.04$$

$$E_{\rm narrow} 6.40\pm 0.01 6.40\pm 0.01 6.40\pm 0.01$$

$$W_{\rm K\alpha } 56\pm 10 60\pm 10 60\pm 12$$

$$\chi^2$$ 2063/2105 3077/2901 3041/2898

$$N_{\rm H} 4.1^{+0.1}_{-0} 4.1^{+0.1}_{-0}$$ ABS(PO+NFE+cRECO) =4.1

$$\Gamma 1.79^{+0.01}_{-0.02} 2.17\pm 0.01 1.88^{+0.01}_{-0.03}$$

$$E_{\rm narrow} 6.39^{+0.01}_{-0.01} 6.39^{+0.01}_{-0.03} 6.39^{+0.01}_{-0.03}$$

$$W_{\rm K\alpha } 66^{+6}_{-12} 37\pm 9 56\pm 11$$

$${\cal R} <0.1 5.9^{+0.5}_{-0.4} 0.89^{+0.21}_{-0.43}$$

$$\chi^2$$ 2384/2106 3840/2902 3457/2898

$$\Gamma 1.76^{+0.04}_{-0.02} 1.85\pm 0.01 1.81^{+0.04}_{0.03}$$ ABS(PO+NFE+KDISK[iREFL])

$$E_{\rm narrow} 6.40\pm 0.01 6.39\pm 0.01 6.39\pm 0.01$$

$$W_{\rm K\alpha } 101\pm 25 96\pm 19 96\pm 18$$

$$\log(\xi_{\rm broad}) 3.10^{+0.15}_{-0.20} 2.97^{+0.05}_{-0.03} 3.08^{+0.08}_{-0.09}$$

$$r_{\rm in} 1.30^{+0.21}_{-0.06} 1.47^{+0.14}_{-0.08} 1.49^{+0.20}_{-0.10}$$

$$\beta 7.70\pm 0.15 5.7^{+1.3}_{-0.7} 5.5^{+1.2}_{-0.8}$$

$$i 56\pm 4 44\pm 6 43^{+6}_{-10}$$

$$\chi^2$$ 2060/2102 2983/2895 2976/2892

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