X-ray line emission from photo-ionized gas in a Seyfert nucleus

Details X-ray line emission from photo-ionized gas in a Seyfert nucleus X-ray line emission from photo-ionized gas in a Seyfert nucleus

Mar 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981mnras.194p..29f&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 194, Mar. 1981, p. 29P-32P. Research supported by the Radcliffe Trust

Astronomy and Astrophysics

Astronomy

7

Galactic Nuclei, Galactic Radiation, Gas Ionization, Photoionization, Seyfert Galaxies, X Ray Spectra, Ariel 5 Satellite, Compton Effect, Emission Spectra

Scientific paper

It is shown that the strong iron line observed in the Ariel V X-ray spectrum of the Seyfert galaxy NGC 5548 may be due to recombination-line emission in a highly photo-ionized gas. This gas must lie within 3 x 10 to the 16th cm of the source of the continuum emission, and provides a direct handle on conditions deep within the broad-line region of the nucleus. The iron line is the closest feature yet observed to the continuum source.

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