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~10³⁷ 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 ~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.