  We present theoretical iron emission line strengths for physical conditions
typical of Active Galactic Nuclei with Broad-Line Regions. The non-local
thermodynamic equilibrium (NLTE) models include a new and extensive treatment
of radiative transfer in the FeIII ion, complementing the FeII emission line
strengths predicted in our earlier works. We also briefly present preliminary
results for the FeI emission from AGN using a reduced atom model. We can
satisfactorily reproduce the empirical UV FeIII emission line template of
Vestergaard & Wilkes (2001) for the prototypical narrow-line Seyfert 1 galaxy I
Zw 1, both in terms of the general FeIII flux distribution and the relative
strength of the FeIII and FeII emission. However, a number of detailed features
are still not matched; the most prominent example is the strongest single FeIII
feature observed in the I Zw 1 spectrum, UV47: it is predicted to be strong
only in models suppressing Fe-H charge exchange reactions. We examine the role
of variations in cloud turbulent velocity and iron abundance and carry out
Monte Carlo simulations to demonstrate the effect of uncertainties in atomic
data on the computed spectra.
