  We present a survey of the X-ray emitting ejecta in the Cassiopeia A
supernova remnant based on an extensive analysis of over 6000 spectral regions
extracted on 2.5-10" angular scales using the Chandra 1 Ms observation. We
interpret these results in the context of hydrodynamical models for the
evolution of the remnant. The distributions of fitted temperature and
ionization age, and the implied mass coordinates, are highly peaked and suggest
that the ejecta were subjected to multiple secondary shocks following reverse
shock interaction with ejecta inhomogeneities. Based on the fitted emission
measure and element abundances, and an estimate of the emitting volume, we
derive masses for the X-ray emitting ejecta and also show the distribution of
the mass of various elements over the remnant. An upper limit to the total
shocked Fe mass visible in X-rays appears to be roughly 0.13 M_sun, which
accounts for nearly all of the mass expected in Fe ejecta. We find two
populations of Fe ejecta, that associated with normal Si-burning and that
possibly associated with alpha-rich freeze-out, with a mass ratio of
approximately 2:1. Essentially all of the observed Fe (both components) lies
well outside the central regions of the SNR, possibly having been ejected by
hydrodynamic instabilities during the explosion. We discuss this, and its
implications for the neutron star kick.
