  We present simultaneous ASCA and RXTE data on the bright Seyfert 1 galaxy
IC4329a. The iron line is significantly broadened, but not to the extent
expected from an accretion disk which extends down to the last stable orbit
around a black hole. We marginally detect a narrow line component, presumably
from the molecular torus, but even including this gives a line profile from the
accretion disk which is significantly narrower that that seen in MCG-6-30-15,
and is much more like that seen from the low/hard state galactic black hole
candidates. This is consistent with the inner disk being truncated before the
last stable orbit, forming a hot flow at small radii as in the ADAF models.
However, we cannot rule out the presence of an inner disk which does not
contribute to the reflected spectrum, either because of extreme ionisation
suppressing the characteristic atomic features of the reflected spectrum or
because the X-ray source is intrinsically anisotropic, so it does not
illuminate the inner disk.
  The source was monitored by RXTE every 2 days for 2 months, and these
snapshot spectra show that there is intrinsic spectral variability. The data
are good enough to disentangle the power law from the reflected continuum and
we see that the power law softens as the source brightens. The lack of a
corresponding increase in the observed reflected spectrum implies that either
the changes in disk inner radial extent/ionisation structure are small, or that
the variability is actually driven by changes in the seed photons which are
decoupled from the hard X-ray mechanism.
