The nucleus of the Seyfert 1 galaxy NGC 7469 - Physical conditions and structure

Details The nucleus of the Seyfert 1 galaxy NGC 7469 - Physical conditions and structure The nucleus of the Seyfert 1 galaxy NGC 7469 - Physical conditions and structure

Oct 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...151..137w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 151, no. 1, Oct. 1985, p. 137-143. Research supported by the Naturvetenskaplig

Astronomy and Astrophysics

Astrophysics

13

Astronomical Spectroscopy, Galactic Nuclei, Galactic Structure, Seyfert Galaxies, Continuous Spectra, Emission Spectra, H Lines, Oxygen Spectra, Ultraviolet Spectra

Scientific paper

Optical data from Osterbrock (1977, 1982), together with data from the literature, including IUE observations, have been used to describe the physical conditions in the nucleus of the Seyfert 1 galaxy NGC 7469. The ultraviolet excess emission over a power-law component cannot be explained by Balmer continuum and Fe II emission alone, suggesting also emission from a blackbody with T = 20,000 K, representing the accretion disk, probably the source of variable X-ray emission, around a black hole of mass 0.7 x 10 to the 9th solar masses in the very center. The blue asymmetry of the forbidden O III lines at 4959 and 5007 A, and their large width compared to other narrow lines, suggest two subregions of the narrow-line region. A two-component model for the broad-line region could explain the differences in line width between the broad Balmer components. Outflow of gas from the center of NGC 7469 seems to be the most probable explanation to the asymmetries of the observed emission-line profiles.

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