The Ultraviolet Spectra of Active Galaxies With Double-Peaked Emission Lines

Details The Ultraviolet Spectra of Active Galaxies With Double-Peaked Emission Lines The Ultraviolet Spectra of Active Galaxies With Double-Peaked Emission Lines

2004-04-26

arxiv.org/abs/astro-ph/0404506v1

Astronomy and Astrophysics

Astrophysics

To appear in "The Interplay among Black Holes, Stars and ISM in Galactic Nuclei," IAU Coll. 222, eds. Storchi Bergmann, Ho, an

Scientific paper

10.1017/S1743921304001383

We present the results of UV spectroscopy of AGNs with double-peaked Balmer emission lines. In 2/3 of the objects, the far-UV resonance lines are strong, with single-peaked profiles resembling those of Seyfert galaxies. The Mg II line is the only UV line with a double-peaked profile. In the remaining objects, the far-UV resonance lines are relatively weak but still single-peaked. The latter group also displays prominent UV absorption lines, indicative of a low-ionization absorber. We interpret the difference in the profiles of the emission lines as resulting from two different regions: a dense, low-ionization accretion disk (the predominant source of the Balmer and Mg II lines), and a lower density, higher-ionization wind (the predominant source of the far-UV resonance lines). These results suggest a way of connecting the double-peaked emitters with the greater AGN population: in double-peaked emitters the accretion rate onto the black hole is low, making the wind feeble and allowing the lines from the underlying disk to shine through. This scenario also implies that in the majority of AGNs, the wind is the source of the broad emission lines.

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