  We present high spatial resolution X-ray spectroscopy of supernova remnant
Cassiopeia A with the {\sl Chandra} observations. The X-ray emitting region of
this remnant was divided into 38 $\times$ 34 pixels with a scale of 10$\arcsec$
$\times$ 10$\arcsec$ each. Spectra of 960 pixels were created and fitted with
an absorbed two component non-equilibrium ionization model. With the spectral
analysis results we obtained maps of absorbing column density, temperatures,
ionization ages, and the abundances for Ne, Mg, Si, S, Ca and Fe. The Si, S and
possibly Ca abundance maps show obviously jet structures, while Fe doesn't
follow the jet but seems to be distributed perpendicular to it. In the range of
about two orders of magnitude, the abundances of Si, S and Ca show tight
correlations between each other, suggesting them to be ejecta from explosive
O-burning and incomplete Si-burning. Meanwhile, Ne abundance is well correlated
with that of Mg, indicating them to be the ashes of explosive C/Ne burning. The
Fe abundance is positively correlated with that of Si when Si abundance is
lower than 3 solar abundances, but a negative correlation appears when the Si
abundance is higher. We suggest that such a two phase correlation is the
results of different ways in which Fe is synthesized.
