Table 1: Best-fitting spectral parameters of the PN spectrum (exposure time $\sim $5 ks) in the 2-12 keV energy range for an absorbed (Galactic, $N_{\rm H}=9.31\times 10^{20}$ cm-2) power-law (PL) component plus a line profile: GA: Gaussian profile; and DISKLINE (Fabian et al. 1989) and LAOR (Laor 1991): profile line emitted by a relativistic accretion disk for a non-rotating BH and a maximally rotating BH, respectively. An emissivity law q equal to -2 was assumed. (a): $R_{\rm in}=6~R_{\rm g}$ and $R_{\rm out}=1000~R_{\rm g}$. (b): $R_{\rm in}=1.23~R_{\rm g}$ and $R_{\rm out}=400~R_{\rm g}$. The F-test probability was estimated comparing to the single power-law model (PL).

Model
$\Gamma$ Line parameters $\chi^{2}$/d.o.f. F-test
    E (keV) $\sigma$ (keV) $\theta$ (deg) EW (eV)    

PL
1.83 $\pm$ 0.09 - - - - 145.2/114 -

PL + GA
1.92 $\pm$ 0.11 $\rm 6.51^{+0.16}_{-0.20}$ $\rm0.28^{+0.19}_{-0.17}$ - $\rm 527^{+277}_{-248}$ 127.1/111 99.80$\%$

PL + DISKLINE(A)
$1.93\pm0.10$ $\rm 6.51^{+0.21}_{-0.12}$ - <43 $\rm 631^{+259}_{-243}$ 125.5/111 99.90$\%$

PL + LAOR(b)
$1.95\pm0.11$ $\rm 6.41^{+0.37}_{-0.18}$ - <49 $\rm 765^{+315}_{-338}$ 125.4/111 99.90$\%$


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