  We present the preliminary results of a Chandra X-ray study of N132D, a young
shell-like supernova remnant (SNR) in the Large Magellanic Cloud. The
equivalent width maps of emissions from O, Ne, Mg, Si, and S are provided.
Spatially resolved spectral analysis for the small-scale regions were
tentatively performed. The X-ray spectra of the interior can be described with
a single-thermal model. The faint interior regions have lower density and
higher temperature (above 1keV) than those of bright interior regions. The
X-ray spectra along the shell can be phenomenally fitted with either a
double-vpshock model or a vpshock + powerlaw model. If the non-thermal
component is true, N132D would be listed as another X-ray synchrotron SNR.
