A Chandra X‐Ray Study of NGC 1068. I. Observations of Extended Emission

Abstract

We report sub arc-second resolution X-ray imaging-spectroscopy of the archetypal type 2 Seyfert galaxy NGC 1068 with the Chandra X-ray Observatory. The observations reveal the detailed structure and spectra of the 13 kpc-extent nebulosity previously imaged at lower resolution with ROSAT. The Chandra image shows a bright, compact source coincident with the brightest radio and optical emission; this source is extended by \simeq 1.5 arcsec (165 pc) in the same direction as the nuclear optical line and radio continuum emission. Bright X-ray emission extends \simeq 5 arcsec (550 pc) to the NE and coincides with the NE radio lobe and gas in the narrow line region. The large-scale emission shows trailing spiral arms and other structures. Numerous point sources associated with NGC 1068 are seen. There is a very strong correlation between the X-ray emission and the high excitation ionized gas seen in HST and ground-based [O III] \lambda 5007 images. The X-rays to the NE of the nucleus are absorbed by only the Galactic column density and thus originate from the near side of the disk of NGC 1068. In contrast the X-rays to the SW are more highly absorbed and must come from gas in the disk or on the far side of it. This geometry is similar to that inferred for the narrow line region and radio lobes. (Abstract truncated).