  We present X-ray emission line equivalent width images of the bright Galactic
supernova remnant Cassiopeia A for the elements Si, S, Ar, Ca, and Fe using a
50,000 s observation with the Advanced CCD Imaging Spectrometer on the Chandra
X-ray Observatory. The images essentially identify the bulk of detectable
ejecta of these elements over a wide range of surface brightness, and show
morphologies distinctly different from that of the broadband X-ray emission and
of the 4-6 keV continuum emission. The Si, S, Ar, and Ca maps, while different
in turn from those of Fe, show that these X-ray emitting ejecta are distributed
similarly to the fast optical ejecta knots, and clearly delineate the X-ray
counterpart of the northeast optical jet. Low surface brightness regions just
outside the bright shell in the north and west are also shown to have strong
line emission. The strong Fe emission is exterior to that of other elements in
the east, as previously noted, but is generally coincident elsewhere. The
projected interior has relatively little emission traced by high line
equivalent widths.
