Using the Chandra X-ray Observatory we have discovered a diffuse , center-filled region of hard X-ray emission within the young , oxygen-rich supernova remnant ( SNR ) G292.0+1.8 .
Near the peak of this diffuse emission lies a point-like source of X-ray emission that is well described by an absorbed power-law spectrum with photon index 1.72 \pm 0.09 .
This source appears to be marginally extended ; its extent of 1.3 ^ { \prime \prime } ( FWHM ) is greater than that of a nearby serendipitous X-ray source with FWHM = 1.1 ^ { \prime \prime } .
This is strong evidence for the presence within SNR G292.0+1.8 of a young rapidly-rotating pulsar and its associated pulsar wind nebula .
From the unabsorbed , 0.2-4 keV band X-ray luminosity of the pulsar wind nebula ( L _ { X } \sim 4 \times 10 ^ { 34 } ergs s ^ { -1 } ) , we infer a spin-down energy loss rate of \dot { E } \sim 7 \times 10 ^ { 36 } ergs s ^ { -1 } for the still undetected pulsar .
The pulsar candidate is 0.9 ^ { \prime } from the geometric center of the SNR which implies a transverse velocity of \sim 770 ( D / 4.8 { kpc } ) ( t / 1600 { yr } ) ^ { -1 } km s ^ { -1 } assuming currently accepted values for the distance and age of G292.0+1.8 .