  We present {\it ASCA} observations of the Seyfert 1 galaxies Mrk~1040 and
MS~0225.5+3121. Mrk~1040 was found to have decreased in flux by almost a factor
of 4 since an {\it EXOSAT} observation 10\,years ago. The energy spectrum of
Mrk~1040 displays complexity both at soft energies (below 0.8\thinspace keV)
and at hard energies (6--7\thinspace keV). The latter is readily interpreted as
fluorescent K$\alpha$ emission from cold iron expected when the primary X-ray
source illuminates cold optically-thick material. This line is both broad (with
FWHM 16\,000--70\,000 km\,s$^{-1}$) and strong (equivalent width $\sim 550\pm
250$\, eV) suggesting that it originates from material close to the compact
object with non-solar abundances. Abundance effects on the equivalent width of
such a line are investigated via Monte Carlo simulations. We find that strong
lines can be produced with physically plausible abundances. The effect of
abundances on the associated reflection continuum is also discussed. The soft
spectral complexity implies either a strong soft excess together with intrinsic
absorption, or a complex absorber. Various models for the nature of such a
complex absorber are discussed. MS~0225.5+3121 shows no evidence for any
variability and has a spectrum that is well described by a power law with
Galactic absorption.
