  We present results from fitting ionized accretion disc models to three long
ASCA observations of the Seyfert 1 galaxy MCG--6-30-15. All three datasets can
be fit by a model consisting of ionized reflection from the inner region of the
accretion disc (with twice solar Fe abundance) and a separate diskline
component from farther out on the the disc. The diskline is required to fit the
height of the observed Fe K line profile. However, we show that a much simpler
model of reflection from a very weakly ionized constant density disc also fits
the data. In this case only a single cold Fe K line at 6.4 keV is required to
fit the observed line. The ionized disc models predict that O VIII K, C VI K,
Fe XVII L, and Fe XVIII L lines will appear in the soft X-ray region of the
reflection spectrum, but are greatly blurred due to Compton scattering. The
equivalent width (EW) of O VIII K is estimated to be about 10 eV and seems to
be as strong as the blend of the Fe L lines. This result creates difficulty for
the claim of a strong relativistic O VIII line in the XMM-Newton grating
spectrum of MCG--6-30-15, although we can not strictly rule it out since
MCG--6-30-15 was in an anomalously low state during that observation. We find
that increasing the O abundance or breaking the continuum below 2 keV will not
significantly strengthen the line. The second Fe K line component in the
ionized disc model may arise from neutral reflection from a flared disc, or
from a second illumination event. The data cannot distinguish between the two
cases, and we conclude that single zone ionized disc models have difficulty
fitting these hard X-ray data of MCG--6-30-15.
