= 
2.86_{-0.16}^{+0.17}$, is slightly steeper than the previous fit. The absorption column density of the absorbed power-law component is ${\ensuremath{N_\mathrm{H}}}= 
9.7_{-5.8}^{+18}\times10^{22} \, \rm cm^{-2}$. The observed 0.5–2 keV and 2–10 keV fluxes are $2.5_{-0.2}^{+0.2}\times10^{-14}$ and $4.6_{-0.4}^{+0.4}\times10^{-14}$ [erg s$^{-1}$ cm$^{-2}$]{}, corresponding to $4.0_{-0.3}^{+0.4}\times10^{40}$ and $6.5_{-0.6}^{+0.6}\times10^{40}$ [erg s$^{-1}$]{}, respectively. Assuming that the obscured power-law component is the intrinsic emission from the corona, the unabsorbed 2–10 keV flux is $6.7\times10^{-14}$ [erg s$^{-1}$ cm$^{-2}$]{}, corresponding to $9.5\times10^{40}$ [erg s$^{-1}$]{}. The monochromatic flux at 2 keV is $7.8\times10^{-32}$ . As the spectra are cut off above 10 keV and no variations are detected in each single exposure or among the four exposures, we cannot exclude the possibility that the absorption is Compton-thick.

If we link the spectral slope of the hard component to the soft one, we obtain $\Gamma = 2.84\pm0.16$, ${\ensuremath{N_\mathrm{H}}}= 14.6_{-7.8}^{+23}\times10^{42} \,\rm cm^{-2}$, and a scattering fraction of $10\%$ if we attribute the soft component to scattered nuclear emission. We note that this fraction is consistent with those commonly reported in other obscured AGNs ($0.1\% - 10\%$; Noguchi et al . 2010).

Ultraviolet Observations
------------------------

The Optical Monitor (OM) on [*XMM-Newton*]{} took data for UM 625 in the UVW1 (2910 Å) and UVW2 