The origin of coronal lines in Seyfert galaxies

Details The origin of coronal lines in Seyfert galaxies The origin of coronal lines in Seyfert galaxies

Aug 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...343..678k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 343, Aug. 15, 1989, p. 678-685.

Astronomy and Astrophysics

Astronomy

73

Galactic Radiation, Interstellar Matter, Line Spectra, Seyfert Galaxies, Abundance, Active Galactic Nuclei, Photoionization, Spiral Galaxies, X Ray Astronomy

Scientific paper

This paper examines the possibility that the coronal line region in Seyfert galaxies may be the result of an interstellar medium (ISM) exposed to, and subsequently photoionized by, a 'bare' Seyfert nucleus. It is shown that a 'generic' AGN continuum illuminating the warm-phase of the ISM of a spiral galaxy can produce the observed emission. In this picture the same UV-radiation cone that is responsible for the high-excitation extended narrow-line emission clouds observed out to 1-2 kpc or farther from the nuclei of some Seyfert galaxies also produces the coronal lines. Soft X-rays originating in the nucleus are Compton-scattered off the ISM, thus producing extended soft X-ray emission, as observed in NGC 4151. The results of the calculations show a basic insensitivity to the ISM density, which explains why similar coronal line spectra are found in many Seyfert galaxies of varying physical environments.

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