other line features, if needed, or another power law. The latter is usually significant at lower energies (below $\sim$ 5 keV), and is thought to be due to electron scattering in an ionized zone extended on a size scale larger than the obscuring structure, even if its contribution depends on modeling details. To model in a simple manner this physical situation, we tied all the power law parameters to the primary one (i.e. photon index, redshift, normalization), and multiplied it by a constant, namely $f_{\rm s}$, which is a free parameter in the fit which quantifies the fraction of the primary power law scattered at low energies. We will refer to this power law as a “scattered power law”. We explain in detail the general fitting procedure for NGC 1194, while for the remaining eight sources we summarize the most relevant findings, in particular the most precise measurement of the column density available to date. Errors quoted always refer to 90% confidence limits for one interesting parameter, if not stated otherwise.

[l c c c c c c c c c c]{} Name & $z$ & $N_{ \rm H}$ & $\log(L_{2-10})$ & Ref. & $M_{\rm BH}$ & Ref. & $R_{\rm 