Inner shell of optically thin gas in active galactic nuclei

Details Inner shell of optically thin gas in active galactic nuclei Inner shell of optically thin gas in active galactic nuclei

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...385..127z&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 385, Jan. 20, 1992, p. 127-131.

Astronomy and Astrophysics

Astrophysics

25

Active Galactic Nuclei, Balmer Series, Lyman Alpha Radiation, Lyman Beta Radiation, Optical Thickness, Seyfert Galaxies, Emission Spectra, Line Shape, Quasars

Scientific paper

The Ly-alpha and Balmer line profiles in more than 50 Seyfert 1 galaxies and QSOs are studied. Approximately 60 percent of the objects show similar profiles, 25 percent show smaller FWHM of H-beta or H-alpha. In five objects the Ly-alpha profiles have stronger wings than the Balmer lines. The Ly-alpha Balmer ratio increases along both wings, suggesting an inner envelope of a very broad-line region. This region accounts for up to 10 percent of the total Balmer line emission and 50 percent of the Ly-alpha emission. The far wings are often fitted with a power-law curve better than logarithmic. The optically thin gas in these objects is in Keplerian motion, and therefore is accreted rather than ejected.

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