IRON K-SHELL EMISSION FROM NGC-1068

We model the X-ray iron line emission from NGC 1068 observed by the Ginga satellite using the new multiline, multilevel, non-LTE radiative transport code ALTAIR and a detailed atomic model for Ne-like through stripped iron (Fe XVI-XXVII). Our calculations are based on the model of NGC 1068 proposed by Antonucci and Miller where the emissions from an obscured type 1 Seyfert engine are scattered into our line of sight by ionized gas. The X-rays passing through the ionized gas induce iron Kα line emission. The atomic model was constructed to describe in detail the K-shell ionization and Kα line emission, as well as to calcula: the ionization state properly. We find a greater equivalent width than previously predicted because the observed Ka line is produced not only by fluorescence but also by line scattering of the continuum into our line of sight. Detailed radiative transfer can have a significant effect on the observed line flux both for the Kα line and for the L-shell emission. The degree of iron ionization increases with temperature; therefore the Kα equivalent width and energy are functions not only of the ionization parameter, but also of the column depth and temperature. For a likely model of NGC 1068 we find that the iron abundance is about twice solar, but that modifications of this model may permit a smaller abundance.