A pulsar wind nebula in the oxygen-rich supernova remnant G292.0+1.8

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 pointlike source of X-ray emission that is well described by an absorbed power-law spectrum with photon index 1.72+/-0.09. This source appears to be marginally extended; its extent of 1."3 (FWHM) is greater than that of a nearby serendipitous X-ray source with FWHM = 1."1. 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. Both the X-ray and radio luminosity of the pulsar wind nebula imply a spin-down energy-loss rate of (E) over dot similar to 10(37) ergs s(-1) for the still undetected pulsar. The pulsar candidate is 0.'9 from the geometric center of the SNR, which implies a transverse velocity of similar to 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.