  We present an analysis of the co-added and individual 0.7-40 keV spectra from
seven Suzaku observations of the Sy 1.5 galaxy NGC 5548 taken over a period of
eight weeks. We conclude that the source has a moderately ionized, three-zone
warm absorber, a power-law continuum, and exhibits contributions from cold,
distant reflection. Relativistic reflection signatures are not significantly
detected in the co-added data, and we place an upper limit on the equivalent
width of a relativistically broad Fe K line at EW \leq 26 eV at 90% confidence.
Thus NGC 5548 can be labeled an "weak" type-1 AGN in terms of its observed
inner disk reflection signatures, in contrast to sources with very broad,
strong iron lines such as MCG-6-30-15, which are likely much fewer in number.
We compare physical properties of NGC 5548 and MCG-6-30-15 that might explain
this difference in their reflection properties. Though there is some evidence
that NGC 5548 may harbor a truncated inner accretion disk, this evidence is
inconclusive, so we also consider light bending of the hard X-ray continuum
emission in order to explain the lack of relativistic reflection in our
observation. If the absence of a broad Fe K line is interpreted in the
light-bending context, we conclude that the source of the hard X-ray continuum
lies at <100 gravitational radii. We note, however, that light-bending models
must be expanded to include a broader range of physical parameter space in
order to adequately explain the spectral and timing properties of average AGN,
rather than just those with strong, broad iron lines.
