Iron K-shell emission from NGC 1068

Details Iron K-shell emission from NGC 1068 Iron K-shell emission from NGC 1068

Oct 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...362...90b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 362, Oct. 10, 1990, p. 90-99. Research supported by NASA.

Astronomy and Astrophysics

Astrophysics

55

Emission Spectra, Extremely High Frequencies, Iron, Line Spectra, X Ray Spectra, Ionized Gases, Polarized Light, Radiative Transfer, Thermodynamic Equilibrium

Scientific paper

The X-ray iron line emission from NGC 1068 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 X-rays passing through the ionized gas induce iron K-alpha line emission. The atomic model was constructed to describe in detail the K-shell ionization and K-alpha line emission, as well as to calculate the ionization state properly. A greater equivalent width than previously predicted is found because the observed K-alpha line is produced not only by fluorescence but also by line scattering of the continuum into the line of sight. The K-alpha 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, 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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