2002ApJ...564L..39P

We present results from the observation of the young Galactic supernova remnant (SNR) G292.0+1.8 with the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. In the 0.3-8 keV band, the high-resolution ACIS images reveal a complex morphology consisting of knots and filaments as well as the blast wave around the periphery of the SNR. We present equivalent width (EW) maps for the elemental species O, Ne, Mg, and Si, which allow us to identify regions of enhanced metallicity in the SNR. G292.0+1.8 is bright in O, Ne, and Si and weaker in S and Ar, with little Fe. The EW and broadband images indicate that the metal-rich ejecta are distributed primarily around the periphery of the SNR. The central beltlike structure has a normal solar-type composition, strongly suggesting that it is primarily emission from a shocked circumstellar medium rather than metal-rich ejecta. We propose that the belt traces its origin to enhanced mass loss in the star's equatorial plane during the slow, red supergiant phase. We also identify thin filaments with normal composition, centered on and extending nearly continuously around the outer boundary of the SNR. These may originate in a shell caused by the stellar winds from the massive progenitor in the red/blue supergiant phases, overrun by the blast wave.