Hostname: page-component-cd9895bd7-lnqnp Total loading time: 0 Render date: 2024-12-25T04:39:07.488Z Has data issue: false hasContentIssue false
  • English
  • Français

The ultraviolet spectra of active galaxies with double-peaked emission lines

Published online by Cambridge University Press:  24 November 2004

M. Eracleous ,
J. P. Halpern ,
T. Storchi-Bergmann ,
A. V. Filippenko ,
A. S. Wilson  and
M. Livio
M. Eracleous
Affiliation:
Deptartment of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA
J. P. Halpern
Affiliation:
Departt of Astronomy, Columbia University, 550 West 120th Street, New York, NY 10027
T. Storchi-Bergmann
Affiliation:
Instituto de Fisica, UFRGS, Campus do Vale, Porto Alegre, RS, Brazil
A. V. Filippenko
Affiliation:
Dept. of Astronomy, University of California, Berkeley, CA 94720, USA
A. S. Wilson
Affiliation:
Dept. of Astronomy, University of Maryland, College Park, MD 20742, USA
M. Livio
Affiliation:
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
ORAL CONTRIBUTIONS
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS222 , March 2004 , pp. 29 - 32
Copyright
© 2004 International Astronomical Union