  We examine the effects of low-temperature, or $\Delta$$n = 0$, dielectronic
recombination (DR) on the ionization balance of the Fe M-Shell (Fe IX through
Fe XVI). Since $\Delta$$n = 0$ rates are not available for these ions, we have
derived estimates based on the existing rates for the first four ionization
states of the CNO sequence and newly calculated rates for L-shell ions of 3rd
row elements and Fe. For a range of ionization parameter and column density
applicable to the intrinsic absorbers detected in {\it ASCA}, {\it Chandra},
and {\it XMM-Newton} observations of Seyfert galaxies, we generated two grids
of photoionization models, with and without DR. The results show that the
ionization parameter at which the population of an Fe M-shell ion peakscan
increase in some cases by factor $>$ 2 when these rates are included. More
importantly, there are dramatic changes in the range in ionization parameter
over which individual M-shell ions contain significant fractions of the total
Fe (e.g. $>$ 10%) in the plasma. These results may explain the mismatch between
the range of Fe ionization states detected in the X-ray spectra of Seyferts,
identified by the energies of the M-Shell Unresolved Transition Array, and
those predicted by photoionization models of the X-ray absorbers that reproduce
lines of second and third row elements. The results suggest that care should be
taken in using 3rd and 4th row ions to constrain the physical conditions in
photoionized X-ray plasmas until accurate DR rates are available. This
underscores the importance of atomic physics in interpreting astronomical
spectroscopy.
