See text for a general description of the figure. NGC 3245: for HST/STIS spectra, emission lines are modeled with a single narrow Gaussian component. The residuals were improved by adding a broad component to Hα. [O I] lines are not visible. In the Palomar spectrum, the double-peaked line profiles are modeled with two Gaussian components. As the [O I] line is rather faint, [S II] lines have been used for the modeling. Hα does not require any BLR-originated component.