using a 20-radius circle for the source and four circles around the source region for the background. All [*XMM-Newton*]{} and [*Chandra*]{} spectra were rebinned to have a minimum of 5 counts in each energy bin after background subtraction, and they were fit simultaneously with the same models using [Xspec]{} (Arnaud 1996). In view of the low source counts, we fit the spectra using the Cash-statistic instead of $\chi^2$.

We first fit the spectra over the energy range 0.2–10 keV using a single absorbed power-law model with the minimum absorption set to the Galactic value of ${\ensuremath{N_\mathrm{H}}}= 4.04\times10^{20} \, \rm cm^{-2}$ (Kalberla et al. 2005). The fit yields a column density equal to the Galactic value, a photon index $\Gamma_{1} = 2.65_{-0.15}^{+0.15}$, and C-statistic = 145 (125 degrees of freedom). The residuals, however, clearly show a flat, hard excess above 3 keV, which implies that an obscured component exists. We then added an absorbed power-law component with a photon index fixed to $\Gamma_{2} = 1.90$, typical of AGNs (Shemmer et al. 2008; Constantin et al. 2009). As shown in Figure 6, the fit is improved significantly, resulting in C-statistic = 116 (123 degrees of freedom). The soft-band power law, with $\Gamma_1 