  We present high spatial resolution X-ray spectroscopy of supernova remnant
G292.0+1.8 with the {\sl Chandra} observations. The X-ray emitting region of
this remnant was divided into 25 $\times$ 25 pixels with a scale of 20$\arcsec$
$\times$ 20$\arcsec$ each. Spectra of 324 pixels were created and fitted with
an absorbed one component non-equilibrium ionization model. With the spectral
analysis results we obtained maps of absorbing column density, temperature,
ionization age, and the abundances for O, Ne, Mg, Si, S, and Fe. The abundances
of O, Ne and Mg show tight correlations between each other in the range of
about two orders of magnitude, suggesting them all from explosive C/Ne burning.
Meanwhile, the abundances of Si and S are also well correlated, indicating them
to be the ashes of explosive explosive O-burning or incomplete Si-burbing. The
Fe emission lines are not prominent among the whole remnant, and its abundance
are significantly deduced, indicating that the reverse shock may have not
propagated to the Fe-rich ejecta. Based on relative abundances of O, Ne, Mg, Si
and Fe to Si, we suggest a progenitor mass of $25-30 M_{\odot}$ for this
remnant.
