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 Ė ∼ 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.