All Tables

Table 1: Summary of the power-law index and luminosities ( $\times$ 10⁴⁴ erg s^-1) observed by different X-ray satellites in the 2-10 keV energy range over 16 years (5 observations). For a direct comparison, the luminosities have been re-calculated when needed assuming $H_{\rm0}=75$ km s^-1 Mpc^-1 and q₀=0.5. The references (Col. 5) correspond to: RT00 (Reeves & Turner 2000), LT97 (Lawson & Turner 1997).
Table 2: Best-fit spectral parameters of the time-averaged pn spectrum in the 2-12 keV energy range with an absorbed (Galactic, $N_{\rm H}=6.8\times 10^{20}$ cm^-2) power-law (PL) component plus a line profile: zgauss: Gaussian profile; and DISKLINE and LAOR: line profile emitted by a relativistic accretion disk for a non-rotating black hole (Fabian et al. 1989) and a maximally rotating black hole (Laor 1991), respectively. The line fluxes are expressed in 10^-6 photons cm^-2 s^-1. We assume an emissivity index q equal to -2. (a): $R_{\rm in}=6$ $R_{\rm g}$ and $R_{\rm out}=1000$ $R_{\rm g}$ . (b): $R_{\rm in}=1.235$ $R_{\rm g}$ and $R_{\rm out}=400$ $R_{\rm g}$ .
Table 3: Best-fit spectral parameters for the three pn sub-spectra in the 2-10 keV energy range. Column (1): number of the corresponding sub-spectrum (the extraction time range is reported in Fig. 3). Column (2): model used. PL: power-law; zgauss: Gaussian line ( $\sigma$ fixed to 10 eV); AN: narrow diskline annulus ( $\Delta R=1$ $R_{\rm g}$ ; other diskline parameters are discussed in the text, see Sect. 3.2). Column (3): power-law index. Column (4): unabsorbed 2-10 keV flux ( $\times 10^{-12}$ erg cm^-2 s^-1). Column (5): line parameters.