Table 2: Best-fitting spectral parameters in the 2.5-12 keV energy range for an absorbed ( $N_{\rm H}=1.88\times 10^{20}$ cm-2) power-law (PL) component plus a line profile: GA: Gaussian profile; and DISKLINE and LAOR: profile line emitted by a relativistic accretion disk for a non-rotating BH and a maximally rotating BH, respectively (Fabian et al. 1989; Laor 1991). The line fluxes are expressed in erg cm-2 s1. We assume an emissivity law q equal to -2. (a): $R_{\rm in}=6~R_{\rm g}$ and $R_{\rm out}=1~000~R_{\rm g}$, inclination = 30$^{\circ }$. (b): $R_{\rm in}=1.26~R_{\rm g}$ and $R_{\rm out}=400~R_{\rm g}$, inclination = 30$^{\circ }$. (c): The energy of the line has been fixed to 6.4 keV (see text).

Model		 $\Gamma$ Line parameters $\chi^{2}$/d.o.f.
PL $1.98\pm0.08$   152.1/150
PL $2.03\pm0.09$ $E=\rm 6.37^{+0.18}_{-0.13}$ keV 134.9/147

+ GA		   $\sigma=0.23^{+0.19}_{-0.11}$ keV  
    $F=\rm 9.6\pm4.0\times10^{-6}$  
    $EW\rm =275^{+164}_{-113}$ eV  
PL $2.03\pm0.09$ $F=8.4\pm3.6\times10^{-6}$ 137.2/149
+ DISKLINE $^{(\rm a,c)}$   $EW=292\pm124$ eV  
PL $2.02\pm0.09$ $F=6.7\pm3.6\times10^{-6}$ 135.9/149

+ LAOR $^{(\rm b,c)}$		   $EW=229\pm94$ eV  


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