We find the X-ray ionization parameter for the ionized material is strongly peaked at Ux approx 0.1. The column densities of ionized material are typically in the range N_{H,z} approx 10^{21}--10^{23} cm^{-2}, although highly ionized (and hence psuedo-transparent) column densities up to 10^{24} cm^{-2} cannot be excluded in some cases. We also investigate the importance of the emission-spectrum from the ionized gas, finding that it significantly improves the fit to many sources with an intensity consistent with material subtending a large solid angle at the central source. Allowing a fraction of the continuum to be observed without attenuation also improves the fit to many sources, and is definitely required in the case of NGC 4151. A deficit of counts is observed at approx 1 keV in the sources exhibiting the strongest absorption features. We suggest this is likely to be the signature of a second zone of (more highly) ionized gas, which might have been seen previously in the deep Fe K-shell edges observed in some Ginga observations. We find evidence that the ionized material in NGC 3227 and MCG-6-30-15 contains embedded dust, whilst there is no such evidence in the other sources
We discuss these results in the context of previous studies and briefly explore the implications in other wavebands.