We present high spatial resolution X-ray spectroscopy of supernova remnant G292.0+1.8 with the 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 .