  We investigated the optical FeII emission in a sample of about 215
low-redshift AGN (quasars and luminous Seyfert 1 galaxies). We find that a
scaled and broadened FeII template based on the I Zw 1 spectrum can
satisfactorily model the FeII emission in almost all sources in our sample. We
confirm that FWHM H$\beta$ and FeII$\lambda$4570 are strongly correlated. The
correlation is different for sources with FWHM(H$\beta$) greater than or less
than $\sim$4000 km s$^{-1}$. Sources with FWHM H$\beta$$\leq$ 4000 km s$^{-1}$
(Population A) show no difference between FWHM H$\beta$ and FeII while sources
with FWHM(H$\beta$) $\geq$ 4000 km s$^{-1}$ (Population B) show FWHM FeII that
is systematically smaller than FWHM H$\beta$. This may be telling us that FeII
emission in Pop. B sources comes from only the outermost part of the H$\beta$\
emitting region where the degree of ionization is lowest.
