Detailed non-LTE calculations of the iron emission from NGC 1068

Details Detailed non-LTE calculations of the iron emission from NGC 1068 Detailed non-LTE calculations of the iron emission from NGC 1068

Nov 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989esasp.296..885b&link_type=abstract

In ESA, The 23rd ESLAB Symposium on Two Topics in X Ray Astronomy. Volume 2: AGN and the X Ray Background p 885-889 (SEE N90-258

Astronomy and Astrophysics

Astronomy

1

Emission Spectra, Iron, K Lines, Radiative Transfer, Stellar Models, X Ray Spectra, Abundance, Background Radiation, Galactic Nuclei, Ionization, Scattering, Seyfert Galaxies, Temperature Dependence, Temperature Effects, X Ray Sources

Scientific paper

The X-ray iron line emission from NGC 1068 observed by the Ginga satellite is modeled using the new multiline, multilevel, non-LTE radiative transport code ALTAIR and a detailed atomic model for Ne-like through stripped iron. The parameter space of the obscured type 1 Seyfert nucleus model for this object is studied. The equivalent width is greater than previously predicted. It is found that detailed radiative transfer can have a significant effect on the observed line flux both for the K alpha line and for the L-shell emission. The ionization of the iron increases with temperature. Therefore the K alpha equivalent width and energy is a function not only of the ionization parameter, but also of the column depth and temperature. For a likely model of NGC 1068 it is found that the iron abundance is about twice solar, but that modifications of this model may permit a smaller abundance.

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